Author: "MARSHALL, J. L." / Topic: astrophysics - astrophysics of galaxies - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"MARSHALL, J. L."' showing total 47 results

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47 results on '"MARSHALL, J. L."'

1. Characterizing the intracluster light over the redshift range 0.2 < z < 0.8 in the DES-ACT overlap

Author: Golden-Marx, Jesse B., Zhang, Y., Ogando, R. L. C., Allam, S., Tucker, D. L., Miller, C. J., Hilton, M., Mutlu-Pakdil, B., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Bellido, J. García, Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Marshall, J. L., Melchior, P., Mena-Fernández, J., Miquel, R., Mohr, J. J., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Sifón, C., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vincenzi, M., Weaverdyck, N., Yanny, B., and Collaboration, DES
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We characterise the properties and evolution of Bright Central Galaxies (BCGs) and the surrounding intracluster light (ICL) in galaxy clusters identified in overlapping regions of the Dark Energy Survey and Atacama Cosmology Telescope Survey (DES-ACT), covering the redshift range $0.20$14.4. We also measure the stellar mass - halo mass (SMHM) relation for the BCG+ICL system and find that the slope, $\beta$, which characterises the dependence of $M_{\rm 200m,SZ}$ on the BCG+ICL stellar mass, increases with radius. The outskirts are more strongly correlated with the halo than the core, which supports that the BCG+ICL system follows a two-phase growth, where recent growth ($z, Comment: 19 pages, 12 Figures, 3 Tables. Submitted to MNRAS on 9/7/2022 -- Metadata typo corrected
Published: 2023

2. Ultracool dwarfs candidates based on six years of the Dark Energy Survey data

Author: Ponte, M. dal, Santiago, B., Rosell, A. Carnero, De Paris, L., Pace, A. B., Bechtol, K., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., Desai, S., De Vicente, J., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Malagón, A. A. Plazas, Pieres, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Weaverdyck, N.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present a sample of 19,583 ultracool dwarf candidates brighter than z $\leq 23$ selected from the Dark Energy Survey DR2 coadd data matched to VHS DR6, VIKING DR5 and AllWISE covering $\sim$ 4,800 $deg^2$. The ultracool candidates were first pre-selected based on their (i-z), (z-Y), and (Y-J) colours. They were further classified using a method that compares their optical, near-infrared and mid-infrared colours against templates of M, L and T dwarfs. 14,099 objects are presented as new L and T candidates and the remaining objects are from the literature, including 5,342 candidates from our previous work. Using this new and deeper sample of ultracool dwarf candidates we also present: 20 new candidate members to nearby young moving groups (YMG) and associations, variable candidate sources and four new wide binary systems composed of two ultracool dwarfs. Finally, we also show the spectra of twelve new ultracool dwarfs discovered by our group and presented here for the first time. These spectroscopically confirmed objects are a sanity check of our selection of ultracool dwarfs and photometric classification method., Comment: 18 pages, 10 figures, 7 tables. Accepted for publication in MNRAS
Published: 2023
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3. The Dark Energy Survey Year 3 high redshift sample: Selection, characterization and analysis of galaxy clustering

Author: Sánchez, C., Alarcon, A., Bernstein, G. M., Sanchez, J., Pandey, S., Raveri, M., Prat, J., Weaverdyck, N., Sevilla-Noarbe, I., Chang, C., Baxter, E., Omori, Y., Jain, B., Alves, O., Amon, A., Bechtol, K., Becker, M. R., Blazek, J., Choi, A., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Crocce, M., Cross, D., Derose, J., Diehl, H. T., Dodelson, S., Drlicawagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Xiao Fang, Fosalba, P., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Maccrann, N., Mccullough, J., Myles, J., Krause, E., Porredon, A., Rodriguezmonroy, M., Rykoff, E. S., Secco, L. F., Sheldon, E., Troxel, M. A., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M. E. S., Desai, S., Doel, P., Doux, C., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gutierrez, G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., and HEP, INSPIRE
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The fiducial cosmological analyses of imaging galaxy surveys like the Dark Energy Survey (DES) typically probe the Universe at redshifts $z < 1$. This is mainly because of the limited depth of these surveys, and also because such analyses rely heavily on galaxy lensing, which is more efficient at low redshifts. In this work we present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around $z \sim 0.9$, $1.2$ and $1.5$, which significantly extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions. The analysis of galaxy clustering measurements, with a total signal-to-noise $S/N \sim 70$ after scale cuts, yields robust cosmological constraints on a combination of the fraction of matter in the Universe $\Omega_m$ and the Hubble parameter $h$, $\Omega_m h = 0.195^{+0.023}_{-0.018}$, and 2-3% measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, $b \sigma_8$. A companion paper $\textit{(in preparation)}$ will present the cross-correlations of these high-$z$ samples with CMB lensing from Planck and SPT, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work., Comment: 28 pages, 25 figures. To be submitted to MNRAS. Comments welcome
Published: 2022

4. The Observed Evolution of the Stellar Mass-Halo Mass Relation for Brightest Central Galaxies

Author: Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F. [UNESP], Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Costanzi, M., Crocce, M., Costa, L. N. da, Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I, Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V, Schubnell, M., Serrano, S., Sevilla-Noarbe, I, Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Varga, T. N., DES Collaboration, Golden-Marx, JB [0000-0002-6394-045X], Zhang, Y [0000-0001-5969-4631], Ogando, RLC [0000-0003-2120-1154], Palmese, A [0000-0002-6011-0530], Abbott, TMC [0000-0003-1587-3931], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], Castander, FJ [0000-0001-7316-4573], Costanzi, M [0000-0001-8158-1449], Crocce, M [0000-0002-9745-6228], Da Costa, LN [0000-0002-7731-277X], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Diehl, HT [0000-0002-8357-7467], Drlica-Wagner, A [0000-0001-8251-933X], Evrard, AE [0000-0002-4876-956X], Ferrero, I [0000-0002-1295-1132], Fosalba, P [0000-0002-1510-5214], García-Bellido, J [0000-0002-9370-8360], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Gruen, D [0000-0003-3270-7644], Gruendl, RA [0000-0002-4588-6517], Gschwend, J [0000-0003-3023-8362], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Jeltema, T [0000-0001-6089-0365], Kuehn, K [0000-0003-0120-0808], Kuropatkin, N [0000-0003-2511-0946], Marshall, JL [0000-0003-0710-9474], Melchior, P [0000-0002-8873-5065], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Morgan, R [0000-0002-7016-5471], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Romer, AK [0000-0002-9328-879X], Sanchez, E [0000-0002-9646-8198], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Soares-Santos, M [0000-0001-6082-8529], Tarle, G [0000-0003-1704-0781], Apollo - University of Cambridge Repository, National Science Foundation (US), Ministerio de Ciencia e Innovación (España), European Commission, UAM. Departamento de Física Teórica, A Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Castander, F. J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares- Santos, M., Suchyta, E., Tarle, G., Varga, T. N., Shanghai Jiao Tong Univ, Univ Michigan, Fermilab Natl Accelerator Lab, Lab Interinst E Astron LIneA, Observ Nacl, Univ Chicago, NSFs Natl Opt Infrared Astron Res Lab, Universidade Estadual Paulista (UNESP), Univ Portsmouth, Inst Astrophys Paris, UPMC Univ Paris 06, UCL, Inst Astrofis Canarias, Univ La Laguna, Natl Ctr Supercomp Applicat, Univ Illinois, Inst Estudis Espacials Catalunya IEEC, CSIC, Univ Trieste, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Ctr Invest Energet Medioambientales & Tecnol CIEM, IIT Hyderabad, Santa Cruz Inst Particle Phys, Univ Oslo, Univ Autonoma Madrid, Stanford Univ, SLAC Natl Accelerator Lab, Univ Geneva, Univ Queensland, Ohio State Univ, Ludwig Maximilians Univ Munchen, Ctr Astrophys Harvard & Smithsonian, Lawrence Berkeley Natl Lab, Univ Arizona, Macquarie Univ, Lowell Observ, Universidade de São Paulo (USP), Texas A&M Univ, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Barcelona Inst Sci & Technol, Max Planck Inst Extraterr Phys, Univ Wisconsin, Univ Cambridge, Univ Sussex, Univ Fed Rio Grande do Sul, Univ Southampton, and Oak Ridge Natl Lab
Subjects: Galaxy clusters, Galaxy evolution, Brightest cluster galaxies, astro-ph.GA, FOS: Physical sciences, Física, Galaxy cluster, Astronomy and Astrophysics, GALÁXIAS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics
Abstract: Golden-Marx; J. B. et al. (DES Collaboration), We quantify evolution in the cluster-scale stellar mass-halo mass (SMHM) relation's parameters using 2323 clusters and brightest central galaxies (BCGs) over the redshift range 0.03 ≤ z ≤ 0.60. The precision on the inferred SMHM parameters is improved by including the magnitude gap (m gap) between the BCG and fourth-brightest cluster member (M14) as a third parameter in the SMHM relation. At fixed halo mass, accounting for m gap, through a stretch parameter, reduces the SMHM relation's intrinsic scatter. To explore this redshift range, we use clusters, BCGs, and cluster members identified using the Sloan Digital Sky Survey C4 and redMaPPer cluster catalogs and the Dark Energy Survey redMaPPer catalog. Through this joint analysis, we detect no systematic differences in BCG stellar mass, m gap, and cluster mass (inferred from richness) between the data sets. We utilize the Pareto function to quantify each parameter's evolution. We confirm prior findings of negative evolution in the SMHM relation's slope (3.5σ), and detect negative evolution in the stretch parameter (4.0σ) and positive evolution in the offset parameter (5.8σ). This observed evolution, combined with the absence of BCG growth, when stellar mass is measured within 50 kpc, suggests that this evolution results from changes in the cluster's m gap. For this to occur, late-term growth must be in the intracluster light surrounding the BCG. We also compare the observed results to IllustrisTNG 300-1 cosmological hydrodynamic simulations and find modest qualitative agreement. However, the simulations lack the evolutionary features detected in the real data., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciênciae Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

5. Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies

Author: A Mau, S., Nadler, E. O., Wechsler, R. H., Drlica-Wagner, A., Bechtol, K., Green, G., Huterer, D., Li, T. S., Mao, Y. -Y., Martínez-Vázquez, C. E., McNanna, M., Mutlu-Pakdil, B., Pace, A. B., Peter, A., Riley, A. H., Strigari, L., Wang, M. -Y., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., Davis, T. M., Vicente, J. De, Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Maia, M. A. G., Marshall, J. L., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Paz-Chinchón, F., Pieres, A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Weller, J., DES Collaboration, Mau, S [0000-0003-3519-4004], Nadler, EO [0000-0002-1182-3825], Wechsler, RH [0000-0003-2229-011X], Drlica-Wagner, A [0000-0001-8251-933X], Bechtol, K [0000-0001-8156-0429], Green, G [0000-0001-5417-2260], Huterer, D [0000-0001-6558-0112], Li, TS [0000-0002-9110-6163], Mao, YY [0000-0002-1200-0820], Martínez-Vázquez, CE [0000-0002-9144-7726], McNanna, M [0000-0001-5435-7820], Mutlu-Pakdil, B [0000-0001-9649-4815], Pace, AB [0000-0002-6021-8760], Peter, A [0000-0002-8040-6785], Riley, AH [0000-0001-5805-5766], Strigari, L [0000-0001-5672-6079], Wang, MY [0000-0002-8226-6237], Aguena, M [0000-0001-5679-6747], Allam, S [0000-0002-7069-7857], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Bocquet, S [0000-0002-4900-805X], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Rosell, AC [0000-0003-3044-5150], Kind, MC [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], Crocce, M [0000-0002-9745-6228], Davis, TM [0000-0002-4213-8783], Vicente, JD [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Ferrero, I [0000-0002-1295-1132], Flaugher, B [0000-0002-2367-5049], Frieman, J [0000-0003-4079-3263], García-Bellido, J [0000-0002-9370-8360], Giannini, G [0000-0002-3730-1750], Gruen, D [0000-0003-3270-7644], Gruendl, RA [0000-0002-4588-6517], Gschwend, J [0000-0003-3023-8362], Gutierrez, G [0000-0003-0825-0517], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Kuehn, K [0000-0003-0120-0808], Lahav, O [0000-0002-1134-9035], Maia, MAG [0000-0001-9856-9307], Marshall, JL [0000-0003-0710-9474], Miquel, R [0000-0002-6610-4836], Morgan, R [0000-0002-7016-5471], Ogando, RLC [0000-0003-2120-1154], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Sanchez, E [0000-0002-9646-8198], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Tucker, DL [0000-0001-7211-5729], Weller, J [0000-0002-8282-2010], Apollo - University of Cambridge Repository, UAM. Departamento de Física Teórica, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Kavli Institute for Particle Astrophysics and Cosmology, Science and Technology Facilities Council (UK), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministerio de Economía y Competitividad (España), German Research Foundation, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, A Mau, S., Nadler, E. O., Wechsler, R. H., Drlica-Wagner, A., Bechtol, K., Green, G., Huterer, D., T. S., Li, Mao, Y. -Y., Martínez-Vázquez, C. E., Mcnanna, M., Mutlu-Pakdil, B., Pace, A. B., Peter, A., Riley, A. H., Strigari, L., Wang, M. -Y., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., Davis, T. M., Vicente, J. De, Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Maia, M. A. G., Marshall, J. L., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Paz-Chinchón, F., Pieres, A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Física, Astronomy and Astrophysics, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy abundances, High Energy Physics - Phenomenology, Halo, High Energy Physics - Phenomenology (hep-ph), Dwarf Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark matter, astro-ph.CO, Dark Matter, Milky Way dark matter halo, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Mau et al., We use a recent census of the Milky Way (MW) satellite galaxy population to constrain the lifetime of particle dark matter (DM). We consider two-body decaying dark matter (DDM) in which a heavy DM particle decays with lifetime τ comparable to the age of the universe to a lighter DM particle (with mass splitting epsilon) and to a dark radiation species. These decays impart a characteristic "kick velocity," Vkick = epsilonc, on the DM daughter particles, significantly depleting the DM content of low-mass subhalos and making them more susceptible to tidal disruption. We fit the suppression of the present-day DDM subhalo mass function (SHMF) as a function of τ and Vkick using a suite of high-resolution zoom-in simulations of MW-mass halos, and we validate this model on new DDM simulations of systems specifically chosen to resemble the MW. We implement our DDM SHMF predictions in a forward model that incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk using an empirical model for the galaxy–halo connection. By comparing to the observed MW satellite population, we conservatively exclude DDM models with τ < 18 Gyr (29 Gyr) for Vkick = 20 kms−1 (40 kms−1) at 95% confidence. These constraints are among the most stringent and robust small-scale structure limits on the DM particle lifetime and strongly disfavor DDM models that have been proposed to alleviate the Hubble and S8 tensions., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant No. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

6. The DECam Local Volume Exploration Survey Data Release 2

Author: Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, and Fundação de Amparo à Pesquisa do Estado de São Paulo
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Surveys, Astrophysics - Astrophysics of Galaxies, Catalogs, Local Group, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Catalog, Survey, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Full list of authors: Drlica-Wagner, A.; Ferguson, P. S.; Adamow, M.; Aguena, M.; Allam, S.; Andrade-Oliveira, F.; Bacon, D.; Bechtol, K.; Bell, E. F.; Bertin, E.; Bilaji, P.; Bocquet, S.; Bom, C. R.; Brooks, D.; Burke, D. L.; Carballo-Bello, J. A.; Carlin, J. L.; Carnero Rosell, A.; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cerny, W.; Chang, C.; Choi, Y.; Conselice, C.; Costanzi, M.; Crnojevic, D.; da Costa, L. N.; De Vicente, J.; Desai, S.; Esteves, J.; Everett, S.; Ferrero, I; Fitzpatrick, M.; Flaugher, B.; Friedel, D.; Frieman, J.; Garcia-Bellido, J.; Gatti, M.; Gaztanaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Hartley, W. G.; Hernandez-Lang, D.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hughes, A. K.; Jacques, A.; James, D. J.; Johnson, M. D.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lidman, C.; Lin, H.; March, M.; Marshall, J. L.; Martinez-Delgado, D.; Martinez-Vazquez, C. E.; Massana, P.; Mau, S.; McNanna, M.; Melchior, P.; Menanteau, F.; Miller, A. E.; Miquel, R.; Mohr, J. J.; Morgan, R.; Mutlu-Pakdil, B.; Munoz, R. R.; Neilsen, E. H.; Nidever, D. L.; Nikutta, R.; Nilo Castellon, J. L.; Noel, N. E. D.; Ogando, R. L. C.; Olsen, K. A. G.; Pace, A. B.; Palmese, A.; Paz-Chinchon, F.; Pereira, M. E. S.; Pieres, A.; Malagon, A. A. Plazas; Prat, J.; Riley, A. H.; Rodriguez-Monroy, M.; Romer, A. K.; Roodman, A.; Sako, M.; Sakowska, J. D.; Sanchez, E.; Sanchez, F. J.; Sand, D. J.; Santana-Silva, L.; Santiago, B.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I; Simon, J. D.; Smith, M.; Soares-Santos, M.; Stringfellow, G. S.; Suchyta, E.; Suson, D. J.; Tan, C. Y.; Tarle, G.; Tavangar, K.; Thomas, D.; To, C.; Tollerud, E. J.; Troxel, M. A.; Tucker, D. L.; Varga, T. N.; Vivas, A. K.; Walker, A. R.; Weller, J.; Wilkinson, R. D.; Wu, J. F.; Yanny, B.; Zaborowski, E.; Zenteno, A.; DELVE Collaboration; DES Collaboration; Astro Data Lab.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We present the second public data release (DR2) from the DECam Local Volume Exploration survey (DELVE). DELVE DR2 combines new DECam observations with archival DECam data from the Dark Energy Survey, the DECam Legacy Survey, and other DECam community programs. DELVE DR2 consists of ∼160,000 exposures that cover >21,000 deg2 of the high-Galactic-latitude (∣b∣ > 10°) sky in four broadband optical/near-infrared filters (g, r, i, z). DELVE DR2 provides point-source and automatic aperture photometry for ∼2.5 billion astronomical sources with a median 5σ point-source depth of g = 24.3, r = 23.9, i = 23.5, and z = 22.8 mag. A region of ∼17,000 deg2 has been imaged in all four filters, providing four-band photometric measurements for ∼618 million astronomical sources. DELVE DR2 covers more than 4 times the area of the previous DELVE data release and contains roughly 5 times as many astronomical objects. DELVE DR2 is publicly available via the NOIRLab Astro Data Lab science platform. © 2022. The Author(s). Published by the American Astronomical Society., The DELVE project is partially supported by Fermilab LDRD project L2019-011, the NASA Fermi Guest Investigator Program Cycle 9 grant 91201, and the National Science Foundation (NSF) under grant AST-2108168. This work is supported by the Fermilab Visiting Scholars Award Program from the Universities Research Association. A.B.P. acknowledges support from NSF grant AST-1813881. J.L.C. acknowledges support from NSF grant AST-1816196. J.D.S. acknowledges support from NSF grant AST-1714873. S.R.M. acknowledges support from NSF grant AST-1909497. D.J.S. acknowledges support from NSF grants AST-1821967 and AST-1813708. D.C. acknowledges support from NSF grant AST-1814208. B.M.P. acknowledges support from the NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2001663. S.M. acknowledges support from the NSF Graduate Research Fellowship under grant DGE-1656518. D.M.D. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Centre of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). C.P.M.B. and M.R.L.C. acknowledge support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement no. 682115). L.S.S. acknowledges the financial support from FAPESP through the grant #2020/03301-5. J.A.C.B. acknowledges support from ANID FONDECYT Regular 1220083. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo á Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2022

7. Identification of Galaxy-Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning

Author: Zaborowski, E., Drlica-Wagner, A., Ashmead, F., Wu, J. F., Morgan, R., Bom, C. R., Shajib, A. J., Birrer, S., Cerny, W., Buckley-Geer, L., Mutlu-Pakdil, B., Ferguson, P. S., Glazebrook, K., Lozano, S. J. Gonzalez, Gordon, Y., Martinez, M., Manwadkar, V., O'Donnell, J., Poh, J., Riley, A., Sakowska, J. D., Santana-Silva, L., Santiago, B. X., Sluse, D., Tan, C. Y., Tollerud, E. J., Verma, A., Carballo-Bello, J. A., Choi, Y., James, D. J., Kuropatkin, N., Martínez-Vázquez, C. E., Nidever, D. L., Castellon, J. L. Nilo, Noël, N. E. D., Olsen, K. A. G., Pace, A. B., Mau, S., Yanny, B., Zenteno, A., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Conselice, C. J., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Lin, H., Marshall, J. L., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., To, C., and Weaverdyck, N.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We perform a search for galaxy-galaxy strong lens systems using a convolutional neural network (CNN) applied to imaging data from the first public data release of the DECam Local Volume Exploration Survey (DELVE), which contains $\sim 520$ million astronomical sources covering $\sim 4,000$ $\mathrm{deg}^2$ of the southern sky to a $5σ$ point-source depth of $g=24.3$, $r=23.9$, $i=23.3$, and $z=22.8$ mag. Following the methodology of similar searches using DECam data, we apply color and magnitude cuts to select a catalog of $\sim 11$ million extended astronomical sources. After scoring with our CNN, the highest scoring 50,000 images were visually inspected and assigned a score on a scale from 0 (definitely not a lens) to 3 (very probable lens). We present a list of 617 strong lens candidates, 599 of which are previously unreported. We categorize our candidates using their human-assigned scores, resulting in 60 Grade A candidates, 160 Grade B candidates, and 397 Grade C candidates. We additionally highlight 8 potential quadruply lensed quasars from this sample. Due to the location of our search footprint in the northern Galactic cap ($b > 10$ deg) and southern celestial hemisphere (${\rm Dec.}, 27 pages; added machine-readable table
Published: 2022
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8. Dark Energy Survey Year 3 Results: Constraints on cosmological parameters and galaxy bias models from galaxy clustering and galaxy-galaxy lensing using the redMaGiC sample

Author: Pandey, S., Krause, E., DeRose, J., MacCrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., DES Collaboration, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, European Commission, European Research Council, Pandey, S., Krause, E., Derose, J., Maccrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysic, combination, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Astrophysics of Galaxies, FOS: Physical sciences, marginalization, Astrophysics, Cosmology and Nongalactic Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics - Astrophysics of Galaxies, efficient, Astrophysic, scale dependence, Astrophysics of Galaxies (astro-ph.GA), halo-mass, evolution, impact, redshift distributions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: S. Pandey et al., We constrain cosmological parameters and galaxy-bias parameters using the combination of galaxy clustering and galaxy-galaxy lensing measurements from the Dark Energy Survey (DES) year-3 data. We describe our modeling framework and choice of scales analyzed, validating their robustness to theoretical uncertainties in small-scale clustering by analyzing simulated data. Using a linear galaxy-bias model and redMaGiC galaxy sample, we obtain 10% constraints on the matter density of the Universe. We also implement a nonlinear galaxy-bias model to probe smaller scales that includes parametrization based on hybrid perturbation theory and find that it leads to a 17% gain in cosmological constraining power. We perform robustness tests of our methodology pipeline and demonstrate stability of the constraints to changes in the theory model. Using the redMaGiC galaxy sample as foreground lens galaxies and adopting the best-fitting cosmological parameters from DES year-1 data, we find the galaxy clustering and galaxy-galaxy lensing measurements to exhibit significant signals akin to decorrelation between galaxies and mass on large scales, which is not expected in any current models. This likely systematic measurement error biases our constraints on galaxy bias and the S8 parameter. We find that a scale-, redshift- and sky-area-independent phenomenological decorrelation parameter can effectively capture this inconsistency between the galaxy clustering and galaxy-galaxy lensing. We trace the source of this correlation to a color-dependent photometric issue and minimize its impact on our result by changing the selection criteria of redMaGiC galaxies. Using this new sample, our constraints on the S8 parameter are consistent with previous studies and we find a small shift in the Ωm constraints compared to the fiducial redMaGiC sample. We infer the constraints on the mean host-halo mass of the redMaGiC galaxies in this new sample from the large-scale bias constraints, finding the galaxies occupy halos of mass approximately 1.6×1013M⊙/h., E. K. is supported by the Department of Energy Grant No. DE-SC0020247 and the David and Lucile Packard Foundation. S. P. and B.J. are supported in part by the U.S. Department of Energy Grant No. DE-SC0007901 and NASA ATP Grant No. NNH17ZDA001N. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at The OhioStateUniversity, theMitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ´eticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität MünchenandtheassociatedExcellenceCluster Universe,the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-20160597, and No. MDM-2015-0509, some of which include ERDFfundsfromtheEuropean Union. I.F.A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/ 2007-2013) including ERC Grant Agreements No. 240672, No.291329,andNo.306478.Weacknowledgesupportfrom the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through Project No. CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office ofScience,OfficeofHighEnergyPhysics.
Published: 2021

9. Dwarf AGNs from Optical Variability for the Origins of Seeds (DAVOS): Insights from the Dark Energy Survey Deep Fields

Author: Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., Collaboration, DES, Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., and Des, Collaboration
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies active, galaxies dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, black hole physic, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We present a sample of 706, $z < 1.5$ active galactic nuclei (AGNs) selected from optical photometric variability in three of the Dark Energy Survey (DES) deep fields (E2, C3, and X3) over an area of 4.64 deg$^2$. We construct light curves using difference imaging aperture photometry for resolved sources and non-difference imaging PSF photometry for unresolved sources, respectively, and characterize the variability significance. Our DES light curves have a mean cadence of 7 days, a 6 year baseline, and a single-epoch imaging depth of up to $g \sim 24.5$. Using spectral energy distribution (SED) fitting, we find 26 out of total 706 variable galaxies are consistent with dwarf galaxies with a reliable stellar mass estimate ($M_{\ast}, 21 pages, 22 figures incl. 3 appendices; accepted for publication in MNRAS
Published: 2021
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10. Shadows in the Dark: Low-Surface-Brightness Galaxies Discovered in the Dark Energy Survey

Author: Tanoglidis, D., Drlica-Wagner, A., Wei, K., Li, T. S., Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., DeRose, J., Conselice, C., Gagnon, L., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), UAM. Departamento de Física Teórica, Tanoglidis, D., Drlica-Wagner, A., Wei, K., T. S., Li, Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., Derose, J., Conselice, C., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., and Walker, A. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, Sky surveys, 01 natural sciences, Imaging data, Luminosity, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Coma Cluster, Surface brightness, Sky survey, Global Air Sampling Program, education, 010303 astronomy & astrophysics, STFC, Low surface brightness galaxie, Physics, education.field_of_study, 010308 nuclear & particles physics, Física, RCUK, Astronomy and Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Star Formation, Dark energy, Low surface brightness galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a catalog of 23,790 extended low-surface-brightness galaxies (LSBGs) identified in $\sim 5000 ��^2$ from the first three years of imaging data from the Dark Energy Survey (DES). Based on a single-component S��rsic model fit, we define extended LSBGs as galaxies with $g$-band effective radii $R_{eff}(g) > 2.5''$ and mean surface brightness $\bar��_{eff}(g) > 24.2 \,mag ��rcsec^{-2}$. We find that the distribution of LSBGs is strongly bimodal in $(g-r)$ vs.\ $(g-i$) color space. We divide our sample into red ($g-i \geq 0.60$) and blue ($g-i 1.5 \,kpc$ and central surface brighthness $��_0(g) > 24.0\, mag \,arcsec^{-2}$. The wide-area sample of LSBGs in DES can be used to test the role of environment on models of LSBG formation and evolution., 31 pages, 19 figures. Version accepted for publication in ApJS. Data products related to this work can be found in: https://des.ncsa.illinois.edu/releases/other/y3-lsbg
Published: 2020
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11. OzDES Reverberation Mapping Program: The first Mg II lags from five years of monitoring

Author: Yu, Zhefu, Martini, Paul, Penton, A., Davis, T. M., Malik, U., Lidman, C., Tucker, B. E., Sharp, R., Kochanek, C. S., Peterson, B. M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Asorey, J., Bertin, E., Brooks, D., Burke, D. L., Calcino, J., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Costanzi, M., da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kim, A. G., Kron, R., Kuehn, K., Kuropatkin, N., Lewis, G. F., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Möller, A., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., and Tucker, D. L.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: Reverberation mapping is a robust method to measure the masses of supermassive black holes (SMBHs) outside of the local Universe. Measurements of the radius -- luminosity ($R-L$) relation using the Mg II emission line are critical for determining these masses near the peak of quasar activity at $z \approx 1 - 2$, and for calibrating secondary mass estimators based on Mg II that can be applied to large samples with only single-epoch spectroscopy. We present the first nine Mg II lags from our five-year Australian Dark Energy Survey (OzDES) reverberation mapping program, which substantially improves the number and quality of Mg II lag measurements. As the Mg II feature is somewhat blended with iron emission, we model and subtract both the continuum and iron contamination from the multi-epoch spectra before analyzing the Mg II line. We also develop a new method of quantifying correlated spectroscopic calibration errors based on our numerous, contemporaneous observations of F-stars. The lag measurements for seven of our nine sources are consistent with both the H$\beta$ and Mg II $R-L$ relations reported by previous studies. Our simulations verify the lag reliability of our nine measurements, and we estimate that the median false positive rate of the lag measurements is $4\%$., Comment: 18 pages, 12 figures. MNRAS, Volume 507, Issue 3, November 2021, Pages 3771-3788
Published: 2021
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12. Milky Way Satellite Census. III. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies

Author: Nadler, E. O., Drlica-Wagner, A., Bechtol, K., Mau, S., Wechsler, R. H., Gluscevic, V., Boddy, K., Pace, A. B., Li, T. S., McNanna, M., Riley, A. H., Garc��a-Bellido, J., Mao, Y. -Y., Green, G., Burke, D. L., Peter, A., Jain, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Brooks, D., Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Walker, A. R., and Wester, W.
Subjects: High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At $95\%$ confidence, we report limits on (i) the mass of thermal relic warm DM, $m_{\rm WDM} > 6.5\ \mathrm{keV}$ (free-streaming length, $\lambda_{\rm{fs}} \lesssim 10\,h^{-1}\ \mathrm{kpc}$), (ii) the velocity-independent DM-proton scattering cross section, $\sigma_{0} < 8.8\times 10^{-29}\ \mathrm{cm}^{2}$ for a $100\ \mathrm{MeV}$ DM particle mass (DM-proton coupling, $c_p \lesssim (0.3\ \mathrm{GeV})^{-2}$), and (iii) the mass of fuzzy DM, $m_{\phi}> 2.9 \times 10^{-21}\ \mathrm{eV}$ (de Broglie wavelength, $\lambda_{\rm{dB}} \lesssim 0.5\ \mathrm{kpc}$). These constraints are complementary to other observational and laboratory constraints on DM properties., Comment: 15 pages, 5 figures, 2 tables. Updated to published version
Published: 2020

13. The Host Galaxies of Rapidly Evolving Transients in the Dark Energy Survey

Author: Wiseman, P., Pursiainen, M., Childress, M., Swann, E., Smith, M., Galbany, L., Lidman, C., Davis, T. M., Gutiérrez, C. P., Möller, A., Thomas, B. P., Frohmaier, C., Foley, R. J., Hinton, S. R., Kelsey, L., Kessler, R., Lewis, G. F., Sako, M., Scolnic, D., Sullivan, M., Vincenzi, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, B. E., Tucker, D. L., Varga, T. N., Walker, A. R., Wiseman, P, Pursiainen, M, Childress, M, Swann, E, Smith, M, Galbany, L, Lidman, C, M Davis, T, P Gutiérrez, C, Möller, A, P Thomas, B, Frohmaier, C, J Foley, R, R Hinton, S, Kelsey, L, Kessler, R, F Lewis, G, Sako, M, Scolnic, D, Sullivan, M, Vincenzi, M, T M, C Abbott, Aguena, M, Allam, S, Annis, J, Bertin, E, Bhargava, S, Brooks, D, L Burke, D, A Carnero Rosell, Carollo, D, M Carrasco Kind, Carretero, J, Costanzi, M, N da Costa, L, T Diehl, H, Doel, P, Everett, S, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Glazebrook, K, Gruen, D, A Gruendl, R, Gschwend, J, Gutierrez, G, L Hollowood, D, Honscheid, K, J James, D, Kuehn, K, Kuropatkin, N, Lima, M, M A, G Maia, L Marshall, J, Martini, P, Menanteau, F, Miquel, R, Palmese, A, Paz-Chinchón, F, A Plazas, A, K Romer, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, E Sommer, N, Suchyta, E, M E, C Swanson, Tarle, G, E Tucker, B, L Tucker, D, N Varga, T, and R Walker, A
Subjects: abundances – galaxies: photometry – galaxies: star formation – transients: supernovae [galaxies], endocrine system, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), galaxies: abundances – galaxies: photometry – galaxies: star formation – transients: supernovae, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Rapidly evolving transients (RETs), also termed fast blue optical transients (FBOTs), are a distinct class of astrophysical event. They are characterised by lightcurves that decline much faster than common classes supernovae (SNe), span vast ranges in peak luminosity and can be seen to redshifts greater than 1. Their evolution on fast timescales has hindered high quality follow-up observations, and thus their origin and explosion/emission mechanism remains unexplained. In this paper we define the largest sample of RETs to date, comprising 106 objects from the Dark Energy Survey, and perform the most comprehensive analysis of RET host galaxies. Using deep-stacked photometry and emission-lines from OzDES spectroscopy, we derive stellar masses and star-formation rates (SFRs) for 49 host galaxies, and metallicities for 37. We find that RETs explode exclusively in star-forming galaxies and are thus likely associated with massive stars. Comparing RET hosts to samples of host galaxies of other explosive transients as well as field galaxies, we find that RETs prefer galaxies with high specific SFRs, indicating a link to young stellar populations, similar to stripped-envelope SNe. RET hosts appear to show a lack of chemical enrichment, their metallicities akin to long duration gamma-ray bursts and superluminous SN host galaxies. There are no clear relationships between properties of the host galaxies and the peak magnitudes or decline rates of the transients themselves., Comment: 16 pages, 15 figures, submitted to MNRAS
Published: 2020

14. Observation and Confirmation of Six Strong Lensing Systems in The Dark Energy Survey Science Verification Data

Author: Nord, B., Buckley-Geer, E., Lin, H., Diehl, H. T., Helsby, J., Kuropatkin, N., Amara, A., Collett, T., Allam, S., Caminha, G. B., de Bom, C., Desai, S., Dúmet-Montoya, H., Pereira, M. Elidaiana da S., Finley, D. A., Flaugher, B., Furlanetto, C., Gaitsch, H., Gill, M., Merritt, K. W., More, A., Tucker, D., Saro, A., Rykoff, E. S., Rozo, E., Birrer, S., Abdalla, F. B., Agnello, A., Auger, M., Brunner, R. J., Carrasco Kind, M., Castander, F. J., Cunha, C. E., da Costa, L. N., Foley, R. J., Gerdes, D. W., Glazebrook, K., Gschwend, J., Hartley, W., Kessler, R., Lagattuta, D., Lewis, G., Maia, M. A. G., Makler, M., Menanteau, F., Niernberg, A., Scolnic, D., Vieira, J. D., Gramillano, R., Abbott, T. M. C., Banerji, M., Benoit-Lévy, A., Brooks, D., Burke, D. L., Capozzi, D., Carnero Rosell, A., Carretero, J., d'Andrea, C. B., Dietrich, J. P., Doel, P., Evrard, A. E., Frieman, J., Gaztanaga, E., Gruen, D., Honscheid, K., James, D. J., Kuehn, K., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Neilsen, E., Nichol, R. C., Ogando, R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Walker, A. R., Wester, W., Zhang, Y., Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Nord, B., Buckley-Geer, E., Lin, H., Diehl, H. T., Helsby, J., Kuropatkin, N., Amara, A., Collett, T., Allam, S., Caminha, G. B., De Bom, C., Desai, S., Dumet-Montoya, H., Da Pereira, M. Elidaiana S., Finley, D. A., Flaugher, B., Furlanetto, C., Gaitsch, H., Gill, M., Merritt, K. W., More, A., Tucker, D., Saro, A., Rykoff, E. S., Rozo, E., Birrer, S., Abdalla, F. B., Agnello, A., Auger, M., Brunner, R. J., Kind, M. Carrasco, Castander, F. J., Cunha, C. E., Da Costa, L. N., Foley, R. J., Gerdes, D. W., Glazebrook, K., Gschwend, J., Hartley, W., Kessler, R., Lagattuta, D., Lewis, G., Maia, M. A. G., Makler, M., Menanteau, F., Niernberg, A., Scolnic, D., Vieira, J. D., Gramillano, R., Abbott, T. M. C., Banerji, M., Benoit-Lévy, A., Brooks, D., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Carretero, J., D'Andrea, C. B., Dietrich, J. P., Doel, P., Evrard, A. E., Frieman, J., Gaztanaga, E., Gruen, D., Honscheid, K., James, D. J., Kuehn, K., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Neilsen, E., Nichol, R. C., Ogando, R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Walker, A. R., Wester, W., and Zhang, Y.
Subjects: Strong gravitational lensing, observational [methods], Astrophysics, 01 natural sciences, cosmology: observations, galaxies: clusters: general, galaxies: distances and redshifts, gravitational lensing: strong, methods: observational, techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Einstein radius, law.invention, law, clusters: general [galaxies], Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, QB, Physics, Solar mass, Astrophysics::Instrumentation and Methods for Astrophysics, observations [cosmology], strong [gravitational lensing], astro-ph.CO, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, 0103 physical sciences, distances and redshift [galaxies], Spectrograph, distances and reshifts [galaxies], Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [SDU]Sciences of the Universe [physics], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), uploaded-in-3-months-elsewhere
Abstract: We report the observation and confirmation of the first group- and cluster-scale strong gravitational lensing systems found in Dark Energy Survey (DES) data. Through visual inspection of data from the Science Verification (SV) season, we identified 53 candidate systems. We then obtained spectroscopic follow-up of 21 candidates using the Gemini Multi-Object Spectrograph (GMOS) at the Gemini South telescope and the Inamori-Magellan Areal Camera and Spectrograph (IMACS) at the Magellan/Baade telescope. With this follow-up, we confirmed six candidates as gravitational lenses: Three of the systems are newly discovered, and the remaining three were previously known. Of the 21 observed candidates, the remaining 15 were either not detected in spectroscopic observations, were observed and did not exhibit continuum emission (or spectral features), or were ruled out as lensing systems. The confirmed sample consists of one group-scale and five galaxy cluster-scale lenses. The lensed sources range in redshift z ~ 0.80-3.2, and in i-band surface brightness i_{SB} ~ 23-25 mag/sq.-arcsec. (2" aperture). For each of the six systems, we estimate the Einstein radius and the enclosed mass, which have ranges ~ 5.0 - 8.6" and ~ 7.5 x 10^{12} - 6.4 x 10^{13} solar masses, respectively., 17 pages, 7 figures, 4 tables; submitted to ApJ
Published: 2015

15. OzDES multifibre spectroscopy for the Dark Energy Survey: Three year results and first data release

Author: Childress, M. J., Lidman, C., Davis, T. M., Tucker, B. E., Asorey, J., Yuan, F., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Banerji, M., Benoit-Levy, A., Stephanie Bernard, Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Cunha, C. E., Da Costa, L. N., D Andrea, C. B., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Foley, R. J., Fosalba, P., Frieman, J., Garcia-Bellido, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hinton, S. R., Hoormann, J. K., James, D. J., Kessler, R., Kim, A. G., King, A. L., Kovacs, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lagattuta, D. J., Lewis, G. F., Li, T. S., Lima, M., Lin, H., Macaulay, E., Maia, M. A. G., Marriner, J., March, M., Marshall, J. L., Martini, P., Mcmahon, R. G., Menanteau, F., Miquel, R., Moller, A., Morganson, E., Mould, J., Mudd, D., Muthukrishna, D., Nichol, R. C., Nord, B., Ogando, R. L. C., Ostrovski, F., Parkinson, D., Plazas, A. A., Reed, S. L., Reil, K., Romer, A. K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Seymour, N., Sharp, R., Smith, M., Soares-Santos, M., Sobreira, F., Sommer, N. E., Spinka, H., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Uddin, S. A., Walker, A. R., Wester, W., and Zhang, B. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results for the first three years of OzDES, a six-year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multi-year baseline, and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17,000 objects, including the redshifts of 2,566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise, magnitude, and exposure time, finding that our redshift success rate increases significantly at a signal-to-noise of 2 to 3 per 1-Angstrom bin. We also find that the change in signal-to-noise with exposure time closely matches the Poisson limit for stacked exposures as long as 10 hours. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as the 4m Multi-Object Spectroscopic Telescope (4MOST), the Subaru Prime Focus Spectrograph (PFS), and the Maunakea Spectroscopic Explorer (MSE). This work marks the first OzDES data release, comprising 14,693 redshifts. OzDES is on target to obtain over a yield of approximately 5,700 supernova host-galaxy redshifts., Accepted for publication in MNRAS. Redshift data release is available at http://www.mso.anu.edu.au/ozdes/DR1
Published: 2017

16. A Study of Quasar Selection in the Dark Energy Survey Supernova fields

Author: Tie, S. S., Martini, P., Mudd, D., Ostrovski, F., Reed, S. L., Lidman, C., Kochanek, C., Davis, T. M., Sharp, R., Uddin, S., King, A., Wester, W., Tucker, B. E., Tucker, D. L., Buckley-Geer, E., Carollo, D., Childress, M., Glazebrook, K., Hinton, S. R., Lewis, G., Macaulay, E., O Neill, C. R., Abbott, T. M. C., Filipe Abdalla, Annis, J., Benoit-L Evy, A., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., Da Costa, L. N., Depoy, D. L., Desai, S., Doel, P., Eifler, T. F., Evrard, A. E., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miller, C. J., Miquel, R., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., and Des, The Collaboration
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We present a study of quasar selection using the DES supernova fields. We used a quasar catalog from an overlapping portion of the SDSS Stripe 82 region to quantify the completeness and efficiency of selection methods involving color, probabilistic modeling, variability, and combinations of color/probabilistic modeling with variability. We only considered objects that appear as point sources in the DES images. We examine color selection methods based on the WISE mid-IR W1-W2 color, a mixture of WISE and DES colors (g-i and i-W1) and a mixture of VHS and DES colors (g-i and i-K). For probabilistic quasar selection, we used XDQSOz, an algorithm that employs an empirical multi-wavelength flux model of quasars to assign quasar probabilities. Our variability selection uses the multi-band chi2-probability that sources are constant in the DES Year 1 griz-band light curves. The completeness and efficiency are calculated relative to an underlying sample of point sources that are detected in the required selection bands and pass our data quality and photometric error cuts. We conduct our analyses at two magnitude limits, i85% for both i-band magnitude limits and efficiencies of >80% to the bright limit and >60% to the faint limit; however, the giW1 and giW1+variability methods give the highest quasar surface densities. The XDQSOz method and combinations of W1W2/giW1/XDQSOz with variability are among the better selection methods when both high completeness and high efficiency are desired. We also present the OzDES Quasar Catalog of 1,263 spectroscopically-confirmed quasars taken by the OzDES survey. The catalog includes quasars with redshifts up to z~4 and brighter than i=22 mag, although the catalog is not complete up this magnitude limit., 16 pages, 12 figures, 3 tables; Submitted to ApJ. The OzDES Quasar Catalog can be downloaded at http://bit.ly/2fWsK9t . For a video summary of the paper, please see https://www.youtube.com/watch?v=JeQNdUATze0
Published: 2016
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17. COSMOGRAIL XVI: Time delays for the quadruply imaged quasar DES J0408-5354 with high-cadence photometric monitoring

Author: Courbin, F., Bonvin, V., Buckley-Geer, E., Fassnacht, C. D., Frieman, J., Lin, H., Marshall, P. J., Suyu, S. H., Treu, T., Anguita, T., Motta, V., Meylan, G., Paic, E., Tewes, M., Agnello, A., Chao, D. C. -Y, Chijani, M., Gilman, D., Rojas, K., Williams, P., Hempel, A., Kim, S., Lachaume, R., Rabus, M., Abbott, T. M. C., Allam, S., Annis, J., Banerji, M., Bechtol, K., Benoit-Lévy, A., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., D Andrea, C. B., Da Costa, L. N., Davis, C., Depoy, D. L., Desai, S., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Richard McMahon, Menanteau, F., Miquel, R., Nord, B., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Tucker, D. L., Walker, A. R., and Wester, W.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies
Abstract: We present time-delay measurements for the new quadruply imaged quasar DES J0408-5354, the first quadruply imaged quasar found in the Dark Energy Survey (DES). Our result is made possible by implementing a new observational strategy using almost daily observations with the MPIA 2.2m telescope at La Silla observatory and deep exposures reaching a signal-to-noise ratio of about 1000 per quasar image. This data quality allows us to catch small photometric variations (a few mmag rms) of the quasar, acting on temporal scales much shorter than microlensing, hence making the time delay measurement very robust against microlensing. In only 7 months we measure very accurately one of the time delays in DES J0408-5354: Dt(AB) = -112.1 +- 2.1 days (1.8%) using only the MPIA 2.2m data. In combination with data taken with the 1.2m Euler Swiss telescope, we also measure two delays involving the D component of the system Dt(AD) = -155.5 +- 12.8 days (8.2%) and Dt(BD) = -42.4 +- 17.6 days (41%), where all the error bars include systematics. Turning these time delays into cosmological constraints will require deep HST imaging or ground-based Adaptive Optics (AO), and information on the velocity field of the lensing galaxy., 9 pages, 5 figures, accepted for publication in Astronomy & Astrophysics

18. Physical properties of star clusters in the outer LMC as observed by the Dark Energy Survey

Author: Pieres, A., Santiago, B., Balbinot, E., Luque, E., Queiroz, A. B. A., Da Costa, L. N., Maia, M. A. G., Drlica-Wagner, A., Roodman, A., Abbott, C., Allam, S., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., Desai, S., Diehl, H. T., Eifler, T. F., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Marshall, J. L., Martini, P., Miller, C. J., Miquel, R., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Douglas Tucker, and Walker, A. R.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: The Large Magellanic Cloud (LMC) harbors a rich and diverse system of star clusters, whose ages, chemical abundances, and positions provide information about the LMC history of star formation. We use Science Verification imaging data from the Dark Energy Survey to increase the census of known star clusters in the outer LMC and to derive physical parameters for a large sample of such objects using a spatially and photometrically homogeneous data set. Our sample contains 255 visually identified cluster candidates, of which 109 were not listed in any previous catalog. We quantify the crowding effect for the stellar sample produced by the DES Data Management pipeline and conclude that the stellar completeness is < 10% inside typical LMC cluster cores. We therefore develop a pipeline to sample and measure stellar magnitudes and positions around the cluster candidates using DAOPHOT. We also implement a maximum-likelihood method to fit individual density profiles and colour-magnitude diagrams. For 117 (from a total of 255) of the cluster candidates (28 uncatalogued clusters), we obtain reliable ages, metallicities, distance moduli and structural parameters, confirming their nature as physical systems. The distribution of cluster metallicities shows a radial dependence, with no clusters more metal-rich than [Fe/H] ~ -0.7 beyond 8 kpc from the LMC center. The age distribution has two peaks at ~ 1.2 Gyr and ~ 2.7 Gyr., 41 pages, 16 figures, 1 appendix

19. Evolution of Galaxy Luminosity and Stellar-Mass Functions since $z=1$ with the Dark Energy Survey Science Verification Data

Author: Capozzi, D., Etherington, J., Thomas, D., Maraston, C., Rykoff, E. S., Sevilla-Noarbe, I., Bechtol, K., Carrasco Kind, M., Drlica-Wagner, A., Pforr, J., Gschwend, J., Carnero Rosell, A., Pellegrini, P., Maia, M. A. G., Da Costa, L. N., Benoit-Lévy, A., Swanson, M. E. C., Wechsler, R. H., Banerji, M., Papovich, C., Morice-Atkinson, X., Abdalla, F., Brooks, D., Carretero, J., Cunha, C., D Andrea, C., Desai, S., Diehl, T. H., Evrards, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., James, D., Jeltema, T., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Nord, B., Ogando, R. L. C., Plazas Malagòn, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Soares-Santos, M., Sobreira, F., Eric Suchyta, and Tarle, G.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first study of the evolution of the galaxy luminosity and stellar-mass functions (GLF and GSMF) carried out by the Dark Energy Survey (DES). We describe the COMMODORE galaxy catalogue selected from Science Verification images. This catalogue is made of $\sim 4\times 10^{6}$ galaxies at $0, Comment: 27 pages, 15 figures, 4 tables. Submitted for publication. Comments are welcome

20. Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey Data II: Hierarchical Bayesian Modeling of Red-Sequence Galaxy Luminosity Function

Author: Zhang, Y., Miller, C. J., Rooney, P., Bermeo, A., Romer, A. K., Vergara Cervantes, C., Rykoff, E. S., Hennig, C., Das, R., Mckay, T., Song, J., Wilcox, H., Bacon, D., Bridle, S. L., Collins, C., Conselice, C., Hilton, M., Hoyle, B., Kay, S., Liddle, A. R., Mann, R. G., Mehrtens, N., Mayers, J., Nichol, R. C., Sahlén, M., Stott, J., Viana, P. T. P., Wechsler, R. H., Abbott, T., Abdalla, F. B., Allam, S., Benoit-Lévy, A., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Matias Carrasco Kind, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D Andrea, C. B., Da Costa, L. N., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Walker, A. R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using $\sim 100$ X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function of cluster red sequence galaxies in the redshift range of $0.1

21. From the fire: a deeper look at the Phoenix stream

Author: K. Tavangar, P. Ferguson, N. Shipp, A. Drlica-Wagner, S. Koposov, D. Erkal, E. Balbinot, J. García-Bellido, K. Kuehn, G. F. Lewis, T. S. Li, S. Mau, A. B. Pace, A. H. Riley, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, H. T. Diehl, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, N. Kuropatkin, M. A. G. Maia, J. L. Marshall, F. Menanteau, R. Miquel, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, M. Rodriguez-Monroy, E. Sanchez, V. Scarpine, S. Serrano, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, T. N. Varga, A. R. Walker, UAM. Departamento de Física Teórica, Tavangar, K [0000-0001-6584-6144], Ferguson, P [0000-0001-6957-1627], Shipp, N [0000-0003-2497-091X], Drlica-Wagner, A [0000-0001-8251-933X], Koposov, S [0000-0003-2644-135X], Erkal, D [0000-0002-8448-5505], Balbinot, E [0000-0002-1322-3153], García-Bellido, J [0000-0002-9370-8360], Kuehn, K [0000-0003-0120-0808], Lewis, GF [0000-0003-3081-9319], Li, TS [0000-0002-9110-6163], Mau, S [0000-0003-3519-4004], Pace, AB [0000-0002-6021-8760], Riley, AH [0000-0001-5805-5766], Aguena, M [0000-0001-5679-6747], Allam, S [0000-0002-7069-7857], Annis, J [0000-0002-0609-3987], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], De Vicente, J [0000-0001-8318-6813], Diehl, HT [0000-0002-8357-7467], Flaugher, B [0000-0002-2367-5049], Frieman, J [0000-0003-4079-3263], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Gruen, D [0000-0003-3270-7644], Gschwend, J [0000-0003-3023-8362], Gutierrez, G [0000-0003-0825-0517], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Kuropatkin, N [0000-0003-2511-0946], Maia, MAG [0000-0001-9856-9307], Marshall, JL [0000-0003-0710-9474], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Ogando, RLC [0000-0003-2120-1154], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Plazas Malagón, AA [0000-0002-2598-0514], Sanchez, E [0000-0002-9646-8198], Sevilla-Noarbe, I [0000-0002-1831-1953], Smith, M [0000-0002-3321-1432], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Walker, AR [0000-0002-7123-8943], Apollo - University of Cambridge Repository, Astronomy, University of Chicago, University of Wisconsin-Madison, Texas AandM University, MIT Kavli Institute for Astrophysics and Space Research, Fermi National Accelerator Laboratory, Royal Observatory, University of Cambridge, University of Surrey, University of Groningen, Universidad Autonoma de Madrid, Lowell Observatory, Macquarie University, The University of Sydney, University of Toronto, Observatories of the Carnegie Institution for Science, Princeton University, Stanford University, Carnegie Mellon University, NSF's National Optical-Infrared Astronomy Research Laboratory, Laboratório Interinstitucional de E-Astronomia-LIneA, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, University College London, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Trieste, Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Universität Hamburg, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Ludwig-Maximilians-Universität, University of Queensland, The Ohio State University, Center for Astrophysics | Harvard and Smithsonian, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, National Science Foundation (US), Department of Energy (US), German Research Foundation, Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Generalitat de Catalunya, Tavangar, K., Ferguson, P., Shipp, N., Drlica-Wagner, A., Koposov, S., Erkal, D., Balbinot, E., García-Bellido, J., Kuehn, K., Lewis, G. F., T. S., Li, Mau, S., Pace, A. B., Riley, A. H., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., and Walker, A. R.
Subjects: Galaxy structure, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar stream, Stellar streams, FOS: Physical sciences, Física, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxies and Cosmology, Cosmology, Dark matter, Astronomy data modeling, Milky Way dynamics, Milky way dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Tavangar et al., We use 6 yr of data from the Dark Energy Survey to perform a detailed photometric characterization of the Phoenix stellar stream, a 15° long, thin, dynamically cold, low-metallicity stellar system in the Southern Hemisphere. We use natural splines, a nonparametric modeling technique, to simultaneously fit the stream track, width, and linear density. This updated stream model allows us to improve measurements of the heliocentric distance (17.4 ± 0.1 (stat.) ±0.8 (sys.) kpc) and distance gradient (−0.009 ± 0.006 kpc deg−1) of Phoenix, which corresponds to a small change of 0.13 ± 0.09 kpc in heliocentric distance along the length of the stream. We measure linear intensity variations on degree scales, as well as deviations in the stream track on ∼2° scales, suggesting that the stream may have been disturbed during its formation and/or evolution. We recover three peaks and one gap in linear intensity along with fluctuations in the stream track. Compared to other thin streams, the Phoenix stream shows more fluctuations and, consequently, the study of Phoenix offers a unique perspective on gravitational perturbations of stellar streams. We discuss possible sources of perturbations to Phoenix, including baryonic structures in the Galaxy and dark matter subhalos., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at The Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the LudwigMaximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-20160597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007–2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project No. CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2022

22. DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc

Author: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny, Ferguson, PS [0000-0001-6957-1627], Shipp, N [0000-0003-2497-091X], Drlica-Wagner, A [0000-0001-8251-933X], Li, TS [0000-0002-9110-6163], Cerny, W [0000-0003-1697-7062], Tavangar, K [0000-0001-6584-6144], Pace, AB [0000-0002-6021-8760], Marshall, JL [0000-0003-0710-9474], Riley, AH [0000-0001-5805-5766], Adamów, M [0000-0002-6904-359X], Carlin, JL [0000-0002-3936-9628], Choi, Y [0000-0003-1680-1884], James, DJ [0000-0001-5160-4486], Koposov, SE [0000-0003-2644-135X], Kuropatkin, N [0000-0003-2511-0946], Martínez-Vázquez, CE [0000-0002-9144-7726], Mau, S [0000-0003-3519-4004], Mutlu-Pakdil, B [0000-0001-9649-4815], Olsen, KAG [0000-0002-7134-8296], Sakowska, JD [0000-0002-1594-1466], Stringfellow, GS [0000-0003-1479-3059], Yanny, B [0000-0002-9541-2678], Apollo - University of Cambridge Repository, Ferguson, P. S. [0000-0001-6957-1627], Shipp, N. [0000-0003-2497-091X], Drlica-Wagner, A. [0000-0001-8251-933X], Li, T. S. [0000-0002-9110-6163], Cerny, W. [0000-0003-1697-7062], Tavangar, K. [0000-0001-6584-6144], Pace, A. B. [0000-0002-6021-8760], Marshall, J. L. [0000-0003-0710-9474], Riley, A. H. [0000-0001-5805-5766], Adamów, M. [0000-0002-6904-359X], Carlin, J. L. [0000-0002-3936-9628], Choi, Y. [0000-0003-1680-1884], James, D. J. [0000-0001-5160-4486], Koposov, Sergey E. [0000-0003-2644-135X], Kuropatkin, N. [0000-0003-2511-0946], Martínez-Vázquez, C. E. [0000-0002-9144-7726], Mau, S. [0000-0003-3519-4004], Mutlu-Pakdil, B. [0000-0001-9649-4815], Olsen, K. A. G. [0000-0002-7134-8296], Sakowska, J. D. [0000-0002-1594-1466], Stringfellow, G. S. [0000-0003-1479-3059], and Yanny, B. [0000-0002-9541-2678]
Subjects: astro-ph.GA, FOS: Physical sciences, Astronomy and Astrophysics, 5109 Space Sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxies and Cosmology, Space and Planetary Science, Clinical Research, Astrophysics of Galaxies (astro-ph.GA), Computer Science::Multimedia, 51 Physical Sciences, Astrophysics::Galaxy Astrophysics
Abstract: We perform a detailed photometric and astrometric analysis of stars in the Jet stream using data from the first data release of the DECam Local Volume Exploration Survey (DELVE) DR1 and \emph{Gaia} EDR3. We discover that the stream extends over $\sim 29 ^{\circ}$ on the sky (increasing the known length by $18^{\circ}$), which is comparable to the kinematically cold Phoenix, ATLAS, and GD-1 streams. Using blue horizontal branch stars, we resolve a distance gradient along the Jet stream of 0.2 kpc/deg, with distances ranging from $D_\odot \sim 27-34$ kpc. We use natural splines to simultaneously fit the stream track, width, and intensity to quantitatively characterize density variations in the Jet stream, including a large gap, and identify substructure off the main track of the stream. Furthermore, we report the first measurement of the proper motion of the Jet stream and find that it is well-aligned with the stream track suggesting the stream has likely not been significantly perturbed perpendicular to the line of sight. Finally, we fit the stream with a dynamical model and find that the stream is on a retrograde orbit, and is well fit by a gravitational potential including the Milky Way and Large Magellanic Cloud. These results indicate the Jet stream is an excellent candidate for future studies with deeper photometry, astrometry, and spectroscopy to study the potential of the Milky Way and probe perturbations from baryonic and dark matter substructure., 19 pages, 10 figures, Accepted in ApJ
Published: 2022

23. The Evolution of AGN Activity in Brightest Cluster Galaxies

Author: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, R. D. Wilkinson, National Aeronautics and Space Administration (US), National Science Foundation (US), Department of Energy (US), Somboonpanyakul, T., Mcdonald, M., Noble, A., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Bacon, D., Bayliss, M. B., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Calzadilla, M., Canning, R., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Doel, P., Eisenhardt, P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Floyd, B., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gonzalez, A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, N., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Khullar, G., Kim, K. J., Klein, M., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Romer, A. K., Ruppin, F., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Singh, P., Smith, M., Soares-Santos, M., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Tucker, D. L., Wilkinson, R. D., UAM. Departamento de Física Teórica, Massachusetts Institute of Technology, Stanford University, Arizona State University, Laboratório Interinstitucional de E-Astronomia - LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), University of Portsmouth, University of Cincinnati, Institut d'Astrophysique de Paris, University of Sussex, University College London, University of Chicago, SLAC National Accelerator Laboratory, Instituto de Astrofisica de Canarias, Dpto. Astrofìsica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Trieste, Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, IObservatório Nacional, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), California Institute of Technology, Santa Cruz Institute for Particle Physics, University of Oslo, University of Missouri-Kansas City, Universidad Autonoma de Madrid, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Florida, Ludwig-Maximilians-Universität, CSIRO Astronomy and Space Science, University of Queensland, The Ohio State University, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, University of Wisconsin-Madison, National Institute for Nuclear Physics, University of Southampton, Osservatorio Astronomico di Brera, and Oak Ridge National Laboratory
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Física, Active Galactic Nuclei, Astronomy and Astrophysics, GALÁXIAS, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, cluster fo galaxies, AGN, Radio Jets (Astronomy), cluster fo galaxie, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics
Abstract: Somboonpanyakul et al., We present the results of an analysis of Wide-field Infrared Survey Explorer (WISE) observations of the full 2500 deg2 South Pole Telescope (SPT)-Sunyaev–Zel'dovich cluster sample. We describe a process for identifying active galactic nuclei (AGN) in brightest cluster galaxies (BCGs) based on WISE mid-IR color and redshift. Applying this technique to the BCGs of the SPT-SZ sample, we calculate the AGN-hosting BCG fraction, which is defined as the fraction of BCGs hosting bright central AGNs over all possible BCGs. Assuming an evolving single-burst stellar population model, we find statistically significant evidence (>99.9%) for a mid-IR excess at high redshift compared to low redshift, suggesting that the fraction of AGN-hosting BCGs increases with redshift over the range of 0 < z < 1.3. The best-fit redshift trend of the AGN-hosting BCG fraction has the form (1 + z)4.1±1.0. These results are consistent with previous studies in galaxy clusters as well as as in field galaxies. One way to explain this result is that member galaxies at high redshift tend to have more cold gas. While BCGs in nearby galaxy clusters grow mostly by dry mergers with cluster members, leading to no increase in AGN activity, BCGs at high redshift could primarily merge with gas-rich satellites, providing fuel for feeding AGNs. If this observed increase in AGN activity is linked to gas-rich mergers rather than ICM cooling, we would expect to see an increase in scatter in the Pcav versus Lcool relation at z > 1. Last, this work confirms that the runaway cooling phase, as predicted by the classical cooling-flow model, in the Phoenix cluster is extremely rare and most BCGs have low (relative to Eddington) black hole accretion rates., T.S. and M.M. acknowledge support from the Kavli Research Investment Fund at MIT, and from NASA through Chandra grant GO5-16143. F.R. acknowledges financial support provided by NASA through SAO Award Number SV2-82023 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientìfico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Enérgeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Fìsica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians-Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the OzDES Membership Consortium, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.
Published: 2022

24. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1

Author: Nikhel Gupta, Tesla E. Jeltema, X. Shao, C. Lidman, Santiago Avila, Vinu Vikram, Michael McDonald, E. Buckley-Geer, David J. Brooks, R. L. C. Ogando, Joseph J. Mohr, M. E. C. Swanson, D. L. Hollowood, V. Scarpine, Shantanu Desai, Maurilio Pannella, Peter Doel, S. Serrano, V. Strazzullo, I-Non Chiu, Matthias Klein, John P. Stott, Enrique Gaztanaga, Robert A. Gruendl, Michael Schubnell, Basilio X. Santiago, J. P. Dietrich, Juan Garcia-Bellido, E. Suchyta, Ramon Miquel, E. J. Sanchez, August E. Evrard, Marcos Lima, Rafe Schindler, J. Annis, Kyler Kuehn, Federico Bianchini, M. Costanzi, J. Gschwend, G. Gutierrez, Christian L. Reichardt, David J. James, A. Saro, Antonella Palmese, A. A. Plazas, L. N. da Costa, M. Smith, I. Sevilla-Noarbe, Daniel Gruen, M. A. G. Maia, S. Everett, F. Paz-Chinchón, J. de Vicente, Jennifer L. Marshall, Esra Bulbul, M. Carrasco Kind, Alfredo Zenteno, J. Carretero, Eli S. Rykoff, A. Carnero Rosell, K. Honscheid, Felipe Menanteau, Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chiu, I., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Mcdonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., and Zenteno, A.
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, galaxies [submillimeter], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, Intracluster medium, 0103 physical sciences, clusters: general [galaxies], 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Luminosity function (astronomy), Physics, Astronomy and Astrophysics, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies: luminosity function, galaxies: clusters: general, mass function, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], galaxies: luminosity function, mass function, High Energy Physics::Experiment, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843~MHz radio AGN population in galaxy clusters from two large catalogs created using the Dark Energy Survey (DES): $\sim$11,800 optically selected RM-Y3 and $\sim$1,000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGN are highly concentrated around cluster centers to $z\sim1$. We measure the halo occupation number for cluster radio AGN above a threshold luminosity, finding that the number of radio AGN per cluster increases with cluster halo mass as $N\propto M^{1.2\pm0.1}$ ($N\propto M^{0.68\pm0.34}$) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad band colors and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGN luminosity function (LF). The LF exhibits a redshift trend of the form $(1+z)^\gamma$ in density and luminosity, respectively, of $\gamma_{\rm D}=3.0\pm0.4$ and $\gamma_{\rm P}=0.21\pm0.15$ in the RM-Y3 sample, and $\gamma_{\rm D}=2.6\pm0.7$ and $\gamma_{\rm P}=0.31\pm0.15$ in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGN, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core ($, Comment: 20 pages, 15 figures Replaced with published version
Published: 2020

25. Dark energy survey year 3 results: Photometric data set for cosmology

Author: Tesla E. Jeltema, Samuel Hinton, I. Ferrero, Matt J. Jarvis, G. Gutierrez, C.Pond, Ramon Miquel, C. Lidman, E. M. Huff, Michel Aguena, Risa H. Wechsler, Eric H. Neilsen, Martin Crocce, R. D. Wilkinson, A. Benoit-Lévy, Daniel Thomas, David J. James, J. De Vicente, Boris Leistedt, D. J. Brout, E. Suchyta, August E. Evrard, Jochen Weller, Douglas L. Tucker, Matthew R. Becker, Eric Morganson, G. Tarle, Sunayana Bhargava, F. J. Castander, Tianjun Li, V. Scarpine, Ian Harrison, Peter Doel, J. Carretero, Tamara M. Davis, Jennifer L. Marshall, Keith Bechtol, T. M. C. Abbott, A. A. Plazas, Ami Choi, Ben Hoyle, K. M. Stringer, C. J. Conselice, Huan Lin, H. T. Diehl, M. Carrasco Kind, Chun-Hao To, E. J. Sanchez, Ofer Lahav, K. Kuehn, M.E.E.Pereira, Robert Morgan, Erin Sheldon, R. Cawthon, Peter Melchior, E. S. Rykoff, Alex Drlica-Wagner, D. L. Burke, I. Sevilla-Noarbe, A. Alarcon, Y.-H. Zhang, David J. Brooks, Dragan Huterer, J. Gschwend, Brian Yanny, Antonella Palmese, N. Kuropatkin, Michael Troxel, W. C. Wester, Gary Bernstein, J. Annis, A. Roodman, M. A. G. Maia, M. Rodriguez-Monroy, S. Allam, Robert A. Gruendl, Tommaso Giannantonio, K. D. Eckert, T. N. Varga, A. K. Romer, Adriano Pieres, L. N. da Costa, P. Martini, Enrique Gaztanaga, R. L. C. Ogando, Sarah Bridle, Santiago Avila, Chihway Chang, S. Everett, S. Desai, J.Allyn-Smith, E. Bertin, D. L. Hollowood, S. Serrano, Richard Kessler, Michael Schubnell, Marcos Lima, Joseph J. Mohr, Alexandra Amon, Felipe Menanteau, Richard G. Kron, A. Carnero Rosell, K. Honscheid, F. Paz-Chinchón, M. Smith, Daniel Gruen, D. W. Gerdes, M. Costanzi, B. Flaugher, M. D. Johnson, P. Fosalba, W. G. Hartley, J. P. Dietrich, Juan Garcia-Bellido, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Instituto Nacional de Ciência e Tecnologia (Brasil), European Commission, Generalitat de Catalunya, Department of Energy (US), Sevilla-Noarbe, I., Bechtol, K., Carrasco Kind, M., Carnero Rosell, A., Becker, M. R., Drlica-Wagner, A., Gruendl, R. A., Rykoff, E. S., Sheldon, E., Yanny, B., Alarcon, A., Allam, S., Amon, A., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Burke, D. L., Carretero, J., Choi, A., Diehl, H. T., Everett, S., Flaugher, B., Gaztanaga, E., Gschwend, J., Harrison, I., Hartley, W. G., Hoyle, B., Jarvis, M., Johnson, M. D., Kessler, R., Kron, R., Kuropatkin, N., Leistedt, B., T. S., Li, Menanteau, F., Morganson, E., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Pond, C., Rodriguez-Monroy, M., Allyn-Smith, J., Stringer, K. M., Troxel, M. A., Tucker, D. L., de Vicente, J., Wester, W., Zhang, Y., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bhargava, S., Bridle, S. L., Brooks, D., Brout, D., Castander, F. J., Cawthon, R., Chang, C., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. E., Davis, T. M., Desai, S., Dietrich, J. P., Doel, P., Eckert, K., Evrard, A. E., Ferrero, I., Fosalba, P., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huff, E. M., Huterer, D., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Mohr, J. J., Morgan, R., Neilsen, E., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wechsler, R. H., Weller, J., Wilkinson, R. D., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, and UAM. Departamento de Física Teórica
Subjects: Observational cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Surveys, 7. Clean energy, 01 natural sciences, Cosmology, Photometric calibration, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Survey, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Catalogs, 1671, 205, 1146, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, 010308 nuclear & particles physics, Image (category theory), Física, Astronomy and Astrophysics, Galaxy, Data set, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Catalog, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data release, Quality information
Abstract: Sevilla-Noarbe, I., et al. (DES Collaboration), We describe the Dark Energy Survey (DES) photometric data set assembled from the first three years of science operations to support DES Year 3 cosmologic analyses, and provide usage notes aimed at the broad astrophysics community. Y3 GOLD improves on previous releases from DES, Y1 GOLD, and Data Release 1 (DES DR1), presenting an expanded and curated data set that incorporates algorithmic developments in image detrending and processing, photometric calibration, and object classification. Y3 GOLD comprises nearly 5000 deg of grizY imaging in the south Galactic cap, including nearly 390 million objects, with depth reaching a signal-to-noise ratio ∼10 for extended objects up to i ∼ 23.0, and top-of-the-atmosphere photometric uniformity 98% and purity >99% for galaxies with 19 < i < 22.5. Additionally, it includes per-object quality information, and accompanying maps of the footprint coverage, masked regions, imaging depth, survey conditions, and astrophysical foregrounds that are used to select the cosmologic analysis samples., K.B. acknowledges support from the U. S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Nos. DE-SC0020278 and DE-SC0017647. The DES data management system is supported by the NSF under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union?s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ci?ncia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). A.C.R. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under grant AYA2017-84061-P, co-financed by FEDER (European Regional Development Funds) and by the Spanish Space Research Program ?Participation in the NISP instrument and preparation for the science of EUCLID? (ESP2017-84272-C2-1-R). This manuscript has been authored by Fermi Research Alliance, LLC under contract No. DE-AC02-07CH11359 with the U. S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021

26. Constraints on dark matter properties from observations of Milky Way satellite galaxies

Author: A. K. Romer, J. Carretero, Annika H. G. Peter, P. Doel, Antonella Palmese, M. A. G. Maia, Vera Gluscevic, Tenglin Li, Ethan O. Nadler, David J. James, A. R. Walker, Marcelle Soares-Santos, S. Desai, Gregory M. Green, Keith Bechtol, Josh Frieman, S. Everett, V. Scarpine, H. T. Diehl, Alex Drlica-Wagner, Dragan Huterer, W. C. Wester, B. Flaugher, Samuel Hinton, J. De Vicente, G. Gutierrez, S. Serrano, J. Annis, D. L. Burke, Douglas L. Tucker, Kyler Kuehn, J. Gschwend, I. Sevilla-Noarbe, Kimberly K. Boddy, M. Smith, Jennifer L. Marshall, Salcedo Romero de Ávila, N. Kuropatkin, L. N. da Costa, S. Allam, Robert A. Gruendl, S. Mau, T. M. C. Abbott, M. Costanzi, M. Carrasco Kind, Daniel Gruen, A. A. Plazas, E. J. Sanchez, M. McNanna, Michel Aguena, M. E. C. Swanson, K. Honscheid, Juan Garcia-Bellido, Andrew B. Pace, Yao-Yuan Mao, Felipe Menanteau, D. W. Gerdes, F. Paz-Chinchón, Elisabeth Krause, A. H. Riley, David J. Brooks, G. Tarle, Ramon Miquel, E. Suchyta, August E. Evrard, Risa H. Wechsler, Bhuvnesh Jain, Ofer Lahav, UAM. Departamento de Física Teórica, Nadler, E. O., Drlica-Wagner, A., Bechtol, K., Mau, S., Wechsler, R. H., Gluscevic, V., Boddy, K., Pace, A. B., T. S., Li, Mcnanna, M., Riley, A. H., García-Bellido, J., Mao, Y. -Y., Green, G., Burke, D. L., Peter, A., Jain, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Brooks, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Walker, A. R., Wester, W., Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), and Department of Energy (US)
Subjects: Scattering cross-section, Milky Way, Dark matter, General Physics and Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo, Particle dark matter, Dwarf Galaxies, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Thermal, Satellite galaxy, Dark Matter, Astrophysics - Cosmology and Nongalactic Astrophysic, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, Física, Astrophysics - Astrophysics of Galaxies, Galaxy, High Energy Physics - Phenomenology, Astrophysics - Cosmology and Nongalactic Astrophysics, Matter wave
Abstract: Nadler, Ethan O, et al. DES Collaboration, We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At 95% confidence, we report limits on (i) the mass of thermal relic warm DM, mWDM>6.5 keV (free-streaming length, λfs≲10h-1 kpc), (ii) the velocity-independent DM-proton scattering cross section, σ02.9×10-21 eV (de Broglie wavelength, λdB≲0.5 kpc). These constraints are complementary to other observational and laboratory constraints on DM properties., The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021

27. OzDES Reverberation Mapping Program: Lag recovery reliability for 6-year CIV analysis

Author: G. Tarle, Maria E. S. Pereira, E. Suchyta, R. D. Wilkinson, Daniela Carollo, I. Ferrero, A. Carnero Rosell, Samuel Hinton, J. Gschwend, Tim Eifler, Kyler Kuehn, M. E. C. Swanson, G. Gutierrez, Juan Garcia-Bellido, J. Carretero, Tamara M. Davis, Rob Sharp, Sunayana Bhargava, David J. Brooks, Antonella Palmese, M. A. G. Maia, M. Smith, D. L. Hollowood, Daniel Gruen, J. K. Hoormann, C. Lidman, B. E. Tucker, S. Serrano, Jennifer L. Marshall, A. K. Romer, Daniel Scolnic, Paul Martini, Josh Frieman, Enrique Gaztanaga, Anais Möller, E. Bertin, S. A. Uddin, D. W. Gerdes, J. Calcino, David J. James, A. A. Plazas, H. T. Diehl, David Bacon, A. Penton, A. G. Kim, Pablo Fosalba, M. Carrasco Kind, Ramon Miquel, M. Costanzi, K. Honscheid, J. Annis, J. De Vicente, W. C. Wester, S. Everett, S. Allam, Robert A. Gruendl, F. Paz-Chinchón, Felipe Menanteau, V. Scarpine, U. Malik, Chun-Hao To, Michel Aguena, E. J. Sanchez, Jacobo Asorey, N. Kuropatkin, Zhefu Yu, T. N. Varga, L. N. da Costa, Robert Morgan, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), DES, Penton, A, Malik, U, Davis, T M, Martini, P, Yu, Z, Sharp, R, Lidman, C, Tucker, B E, Hoormann, J K, Aguena, M, Allam, S, Annis, J, Asorey, J, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Calcino, J, Carnero&nbsp, Rosell, A, Carollo, D, Carrasco&nbsp, Kind, M, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, De&nbsp, Vicente, J, Diehl, H T, Eifler, T F, Everett, S, Ferrero, I, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hinton, S R, Hollowood, D L, Honscheid, K, James, D J, Kim, A G, Kuehn, K, Kuropatkin, N, Maia, M A G, Marshall, J L, Menanteau, F, Miquel, R, Morgan, R, Möller, A, Palmese, A, Paz-Chinchón, F, Plazas, A A, Romer, A K, Sanchez, E, Scarpine, V, Scolnic, D, Serrano, S, Smith, M, Suchyta, E, Swanson, M E C, Tarle, G, To, C, Uddin, S A, Varga, T N, Wester, W, Wilkinson, R D, Lewis, G, National Science Foundation (US), Ministerio de Ciencia e Innovación (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), and UAM. Departamento de Física Teórica
Subjects: galaxies: active, quasars: emission lines, quasars: general, Astrophysics - Astrophysics of Galaxies, Lag, FOS: Physical sciences, 01 natural sciences, emission lines [Quasars], statistical analysis, (Galaxies:) Quasars: Emission Lines, 0103 physical sciences, quasar, silver, AGN, 010303 astronomy & astrophysics, Reliability (statistics), Physics, [PHYS]Physics [physics], general [quasars], 010308 nuclear & particles physics, ) Quasars: Emission Lines [(Galaxies], Física, Astronomy and Astrophysics, gold, (Galaxies:) Quasars: Supermassive Black Holes, Nuclei, Reliability engineering, emission line [quasars], Space and Planetary Science, quality, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], slope, Reverberation mapping, dispersion, galaxy, statistical, ) Quasars: Supermassive Black Holes [(Galaxies]
Abstract: Penton, A. et al (DES Collaboration), We present the statistical methods that have been developed to analyse the OzDES reverberation mapping sample. To perform this statistical analysis we have created a suite of customizable simulations that mimic the characteristics of each source in the OzDES sample. These characteristics include: the variability in the photometric and spectroscopic light curves, the measurement uncertainties, and the observational cadence. By simulating the sources in the OzDES sample that contain the C iv emission line, we developed a set of criteria that rank the reliability of a recovered time-lag depending on the agreement between different recovery methods, the magnitude of the uncertainties, and the rate at which false positives were found in the simulations. These criteria were applied to simulated light curves and these results used to estimate the quality of the resulting Radius-Luminosity relation. We grade the results using three quality levels (gold, silver, and bronze). The input slope of the R-L relation was recovered within 1σ for each of the three quality samples, with the gold standard having the lowest dispersion with a recovered a R-L relation slope of 0.454 ± 0.016 with an input slope of 0.47. Future work will apply these methods to the entire OzDES sample of 771 AGN., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2021

28. Rates and delay times of Type Ia supernovae in the Dark Energy Survey

Author: Geraint F. Lewis, A. R. Walker, A. A. Plazas Malagón, J. Annis, Brodie Popovic, M. E. C. Swanson, Enrique Gaztanaga, Josh Frieman, G. Tarle, Anais Möller, E. Bertin, Samuel Hinton, C. Lidman, B. E. Tucker, G. Gutierrez, Jennifer L. Marshall, B. Flaugher, R. L. C. Ogando, V. Scarpine, Daniel Scolnic, M. Carrasco Kind, F. Andrade-Oliveira, Robert C. Nichol, D. J. Brout, Daniel Thomas, J. Gschwend, Kyler Kuehn, Daniela Carollo, K. Honscheid, J. Carretero, David J. James, Tamara M. Davis, Ramon Miquel, Maria E. S. Pereira, M. Costanzi, Pablo Fosalba, Juan Garcia-Bellido, Peter Doel, E. Buckley-Geer, I. Ferrero, I. Sevilla-Noarbe, Karl Glazebrook, H. T. Diehl, Felipe Menanteau, David Bacon, Benjamin Rose, M. Soares-Santos, Chris Frohmaier, M. Vincenzi, N. Kuropatkin, Robert Morgan, Mark Sullivan, A. K. Romer, Elisabeth Krause, T. N. Varga, Tommaso Giannantonio, L. N. da Costa, M. Toy, Paul Martini, A. Carnero Rosell, O. Graur, D. L. Burke, P. Wiseman, S. Allam, Robert A. Gruendl, Michael Schubnell, S. Everett, David J. Brooks, D. L. Hollowood, Adriano Pieres, S. Serrano, Richard Kessler, Michel Aguena, M. Smith, Daniel Gruen, E. Suchyta, Zoe Zontou, F. Paz-Chinchón, Lluís Galbany, L. Kelsey, P. Armstrong, Don Petravick, S. Desai, Jacobo Asorey, Antonella Palmese, M. A. G. Maia, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, Ben Hoyle, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Wiseman, P., Sullivan, M., Smith, M., Frohmaier, C., Vincenzi, M., Graur, O., Popovic, B., Armstrong, P., Brout, D., Davis, T. M., Galbany, L., Hinton, S. R., Kelsey, L., Kessler, R., Lidman, C., Möller, A., Nichol, R. C., Rose, B., Scolnic, D., Toy, M., Zontou, Z., Asorey, J., Carollo, D., Glazebrook, K., Lewis, G. F., Tucker, B. E., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Varga, T. N., Walker, A. R., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Stellar mass, FOS: Physical sciences, Context (language use), Astrophysics, Type (model theory), 01 natural sciences, 7. Clean energy, Luminosity, supernovae: general, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, white dwarf, 010303 astronomy & astrophysics, STFC, evolution [galaxies], 0105 earth and related environmental sciences, white dwarfs, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), RCUK, White dwarf, Astronomy and Astrophysics, galaxies: evolution, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Redshift, Galaxy, ST/R000506/1, Supernova, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 8. Economic growth, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae]
Abstract: Wiseman, P., et al. DES Collaboration, We use a sample of 809 photometrically classified Type Ia supernovae (SNe Ia) discovered by the Dark Energy Survey (DES) along with 40 415 field galaxies to calculate the rate of SNe Ia per galaxy in the redshift range 0.2 < z < 0.6. We recover the known correlation between SN Ia rate and galaxy stellar mass across a broad range of scales 8.5 ≤ log (M*/M⊙) ≤ 11.25. We find that the SN Ia rate increases with stellar mass as a power law with index 0.63 ± 0.02, which is consistent with the previous work. We use an empirical model of stellar mass assembly to estimate the average star formation histories (SFHs) of galaxies across the stellar mass range of our measurement. Combining the modelled SFHs with the SN Ia rates to estimate constraints on the SN Ia delay time distribution (DTD), we find that the data are fit well by a power-law DTD with slope index β = −1.13 ± 0.05 and normalization A = 2.11 ± 0.05 × 10−13 SNe M⊙−1 yr−1, which corresponds to an overall SN Ia production efficiency NIa/M∗=0.9 +4.0−0.7×10−3 SNe M−1⊙⁠. Upon splitting the SN sample by properties of the light curves, we find a strong dependence on DTD slope with the SN decline rate, with slower-declining SNe exhibiting a steeper DTD slope. We interpret this as a result of a relationship between intrinsic luminosity and progenitor age, and explore the implications of the result in the context of SN Ia progenitors., The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007–2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2021

29. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author: Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H., Battaglia, Nick, Bond, J. Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K., Devlin, Mark, Dunkley, Jo, Evrard, August E., Ferraro, Simone, Hill, J. Colin, Hughes, John P., Gallardo, Patricio A., Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S., Nati, Frederico, Newburgh, Laura B., Niemack, Michael D., Page, Lyman A., Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sif��n, Crist��bal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L., Rosell, Aurelio C., Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, da Costa, Luiz N., De Vicente, Juan, Desai, Shantanu, Diehl, Thomas H., Doel, Peter, Everett, Spencer, Ferrero, Ismael, Fert��, Agn��s, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garc��a-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G., Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klaus, James, David J., Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo L. C., Paz-Chinch��n, Francisco, Malag��n, Andr��s Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Varga, Tamas N., Wilkinson, Reese D., Zhang, Yuanyuan, Austermann, Jason E., Beall, James A., Becker, Daniel T., Denison, Edward V., Duff, Shannon M., Hilton, Gene C., Hubmayr, Johannes, Ullom, Joel N., Van Lanen, Jeff, Vale, Leila R., Collaboration, DES, Collaboration, ACT, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari, S., Shin, T. -H., Jain, B., Hilton, M., Baxter, E., Chang, C., Wechsler, R. H., Battaglia, N., Bond, J. R., Bocquet, S., Choi, S. K., Derose, J., Devlin, M., Dunkley, J., Evrard, A. E., Ferraro, S., Hill, J. C., Hughes, J. P., Gallardo, P. A., Lokken, M., Macinnis, A., Madhavacheril, M. S., Mcmahon, J., Nati, F., Newburgh, L. B., Niemack, M. D., Page, L. A., Palmese, A., Partridge, B., Rozo, E., Rykoff, E., Salatino, M., Schillaci, A., Sehgal, N., Sifon, C., C. -H., To, Wollack, E., H. -Y., Wu, Xu, Z., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Da Costa, L. N., Vicente, J. D., Desai, S., Diehl, T. H., Doel, P., Everett, S., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., L. C. Ogando R., Paz-Chinchon, F., Malagon, A. P., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., E. C. Swanson M., Varga, T. N., Wilkinson, R. D., Zhang, Y., Austermann, J. E., Beall, J. A., Becker, D. T., Denison, E. V., Duff, S. M., Hilton, G. C., Hubmayr, J., Ullom, J. N., Lanen, J. V., and Vale, L. R.
Subjects: Galaxy dark matter halos, 010308 nuclear & particles physics, FOS: Physical sciences, Cold dark matter, Astronomy and Astrophysics, Galaxy clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, SZ effect, Galaxy cluster, Surveys, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy evolution, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy kinematics
Abstract: Adhikari, S., et al. (DES and ACT Collaboration), We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr., The DES Data Management System is supported by the NSF under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Unionʼs Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2)
Published: 2021

30. The STRong lensing Insights into the Dark Energy Survey (STRIDES) 2017/2018 follow-up campaign: discovery of 10 lensed quasars and 10 quasar pairs

Author: A. A. Plazas, C. Lemon, Antonella Palmese, M. Smith, M. A. G. Maia, G C-F Chen, J. Carretero, Anowar J. Shajib, Marcos Lima, Adriano Agnello, Frederic Courbin, Ramon Miquel, Shantanu Desai, D. L. Burke, G. Gutierrez, G. Tarle, Daniel Gruen, M. March, Ofer Lahav, Paul L. Schechter, Tim Eifler, Enrique Gaztanaga, Thomas E. Collett, A. Carnero Rosell, M. Costanzi, Yordanka Apostolovski, Kyler Kuehn, Juan Garcia-Bellido, Richard G. McMahon, Christopher D. Fassnacht, S. Allam, Robert A. Gruendl, Elisabeth Krause, David J. Brooks, A. Melo, Simon Birrer, Motta, David J. James, D. W. Gerdes, Matthew W. Auger, Michael Schubnell, Tommaso Treu, Josh Frieman, Cristian E. Rusu, Felipe Menanteau, M. Carrasco Kind, A. Roodman, B. Flaugher, J. Annis, Alistair R. Walker, Marcelle Soares-Santos, Timo Anguita, E. Suchyta, S. Serrano, K. Honscheid, N. Kuropatkin, F. Paz-Chinchón, Santiago Avila, Jennifer L. Marshall, L. N. da Costa, A. G. Kim, J. De Vicente, Huan Lin, E. Buckley-Geer, T. M. C. Abbott, E. Bertin, E. J. Sanchez, J. Gschwend, Lemon, C., Auger, M. W., Mcmahon, R., Anguita, T., Apostolovski, Y., Chen, G. C. -F., Fassnacht, C. D., Melo, A. D., Motta, V., Shajib, A., Treu, T., Agnello, A., Buckley-Geer, E., Schechter, P. L., Birrer, S., Collett, T., Courbin, F., Rusu, C. E., Abbott, T. M. C., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Eifler, T. F., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kim, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Walker, A. R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, McMahon, Richard [0000-0001-8447-8869], and Apollo - University of Cambridge Repository
Subjects: candidates, observational [methods], time-delay, Astrophysics, 01 natural sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, sky, Physics, Faint Object Spectrograph, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational lensing: strong, gravitational lenses, strong [gravitational lensing], Astrophysics::Earth and Planetary Astrophysics, methods: observational, sextractor, Astronomical and Space Sciences, astro-ph.GA, FOS: Physical sciences, selection, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Photometry (optics), quasars: general, Gravitational Lenses, 0103 physical sciences, Quasars, Spectrograph, STFC, Astrophysics::Galaxy Astrophysics, general [quasars], 010308 nuclear & particles physics, variability, Near-infrared spectroscopy, RCUK, Astronomy and Astrophysics, Quasar, Galaxies, Light curve, redshift, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), gaia, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmograil
Abstract: We report the results of the STRong lensing Insights from the Dark Energy Survey (STRIDES) follow-up campaign of the late 2017/early 2018 season. We obtained spectra of 65 lensed quasar candidates either with EFOSC2 on the NTT or ESI on Keck, which confirm 10 new gravitationally lensed quasars and 10 quasar pairs with similar spectra, but which do not show a lensing galaxy in DES images. Eight lensed quasars are doubly imaged with source redshifts between 0.99 and 2.90, one is triply imaged by a group (DESJ0345-2545, $z=1.68$), and one is quadruply imaged (quad: DESJ0053-2012, $z=3.8$). Singular isothermal ellipsoid models for the doubles, based on high-resolution imaging from SAMI on SOAR or NIRC2 on Keck, give total magnifications between 3.2 and 5.6, and Einstein radii between 0.49 and 1.97 arcseconds. After spectroscopic follow-up, we extract multi-epoch $grizY$ photometry of confirmed lensed quasars and contaminant quasar+star pairs from the first 4 years of DES data using parametric multi-band modelling, and compare variability in each system's components. By measuring the reduced ${\chi}^2$ associated with fitting all epochs to the same magnitude, we find a simple cut on the less variable component that retains all confirmed lensed quasars, while removing 94 per cent of contaminant systems with stellar components. Based on our spectroscopic follow-up, this variability information can improve selection of lensed quasars and quasar pairs from 34-45 per cent to 51-70 per cent, with the majority of remaining contaminants being compact star-forming galaxies. Using mock lensed quasar lightcurves we demonstrate that selection based only on variability will over-represent the quad fraction by 10 per cent over a complete DES magnitude-limited sample (excluding microlensing differences), explained by the magnification bias and hence lower luminosity (more variable) sources in quads., Comment: 22 pages, 16 figures, submitted to MNRAS
Published: 2020

31. Perturbation theory for modeling galaxy bias: Validation with simulations of the Dark Energy Survey

Author: Ramon Miquel, Elisabeth Krause, Martin Crocce, I. Ferrero, A. Roodman, M. E. C. Swanson, J. DeRose, E. Suchyta, D. L. Burke, S. Serrano, Niall MacCrann, J. Annis, Jochen Weller, Felipe Menanteau, Bhuvnesh Jain, Xiao Fang, M. Costanzi, A. Carnero Rosell, Jack Elvin-Poole, G. Tarle, Jennifer L. Marshall, S. Allam, Robert A. Gruendl, Josh Frieman, M. Carrasco Kind, K. Honscheid, Juan Garcia-Bellido, Michael Schubnell, F. Paz-Chinchón, S. Pandey, Oliver Friedrich, J. Gschwend, A. A. Plazas, J. Carretero, M. Smith, Antonella Palmese, Michel Aguena, Daniel Gruen, Gary Bernstein, M. A. G. Maia, Pablo Fosalba, V. Scarpine, S. Everett, David J. Brooks, E. J. Sanchez, Shantanu Desai, Jonathan Blazek, G. Gutierrez, Santiago Avila, J. De Vicente, I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, Kyler Kuehn, L. N. da Costa, Pandey, S., Krause, E., Jain, B., Maccrann, N., Blazek, J., Crocce, M., Derose, J., Fang, X., Ferrero, I., Friedrich, O., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Elvin-Poole, J., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, growth, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, estimators, 01 natural sciences, Measure (mathematics), evolution, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, Statistical physics, Perturbation theory, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, survey cosmological implications, 010308 nuclear & particles physics, Matter power spectrum, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, halo occupation distribution, Galaxy, Nonlinear system, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Configuration space, constraints
Abstract: We describe perturbation theory (PT) models of galaxy bias for applications to photometric galaxy surveys. We model the galaxy-galaxy and galaxy-matter correlation functions in configuration space and validate against measurements from mock catalogs designed for the Dark Energy Survey (DES). We find that an effective PT model with five galaxy bias parameters provides a good description of the 3D correlation functions above scales of 4 Mpc/$h$ and $z < 1$. Our tests show that at the projected precision of the DES-Year 3 analysis, two of the non-linear bias parameters can be fixed to their co-evolution values, and a third (the $k^2$ term for higher derivative bias) set to zero. The agreement is typically at the 2 percent level over scales of interest, which is the statistical uncertainty of our simulation measurements. To achieve this level of agreement, our {\it fiducial} model requires using the full non-linear matter power spectrum (rather than the 1-loop PT one). We also measure the relationship between the non-linear and linear bias parameters and compare them to their expected co-evolution values. We use these tests to motivate the galaxy bias model and scale cuts for the cosmological analysis of the Dark Energy Survey; our conclusions are generally applicable to all photometric surveys., 19 pages, 14 figures, 1 table
Published: 2020

32. Identifying RR Lyrae Variable Stars in Six Years of the Dark Energy Survey

Author: H. T. Diehl, A. R. Walker, David Bacon, A. Roodman, M. Smith, Samuel Hinton, G. Gutierrez, Daniel Gruen, David J. James, Tenglin Li, Michael Schubnell, J. De Vicente, G. Tarle, J. Gschwend, D. L. Hollowood, Maria E. S. Pereira, S. Serrano, Michel Aguena, R. L. C. Ogando, D. W. Gerdes, Jennifer L. Marshall, A. Carnero Rosell, D. L. Burke, S. Desai, M. Costanzi, David J. Brooks, I. Ferrero, P. S. Ferguson, Yanxi Zhang, S. Allam, Robert A. Gruendl, Daniel Thomas, Eric H. Neilsen, Lucas M. Macri, Antonella Palmese, Martin Crocce, W. C. Wester, T. M. C. Abbott, R. D. Wilkinson, Alex Drlica-Wagner, C. E. Martínez-Vázquez, M. A. G. Maia, Juan Garcia-Bellido, E. Bertin, Chun-Hao To, Robert Morgan, F. Paz-Chinchón, Keith Bechtol, Felipe Menanteau, E. J. Sanchez, K. M. Stringer, E. Suchyta, Ben Hoyle, A. K. Vivas, Kyler Kuehn, Ramon Miquel, K. Honscheid, A. A. Plazas, I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, T. N. Varga, L. N. da Costa, K. Tavangar, J. Carretero, Enrique Gaztanaga, Andrew B. Pace, M. Carrasco Kind, Peter Doel, UAM. Departamento de Física Teórica, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Stringer, K. M., Drlica-Wagner, A., Macri, L., Martínez-Vázquez, C. E., Vivas, A. K., Ferguson, P., Pace, A. B., Walker, A. R., Neilsen, E., Tavangar, K., Wester, W., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Ferrero, I., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., T. S., Li, Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., Zhang, Y., the DES Collaboration, National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), and Australian Research Council
Subjects: Proper motion, Milky Way stellar halo, 010504 meteorology & atmospheric sciences, RR Lyrae variable stars, Milky Way, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, RR Lyrae variable, 01 natural sciences, Milky Way Galaxy, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Satellite galaxy, Astrophysics::Solar and Stellar Astrophysics, Eridanus, RRab variable star, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Dwarf galaxy, Physics, RRab variable stars, the Milky Way, 1410, 1413, 1060, 1054, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Física, Astronomy and Astrophysics, RR Lyrae variable star, Stars, Space and Planetary Science, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Stringer, K. M., et al. (DES Collaboration), We present a search for RR Lyrae stars using the full six-year data set from the Dark Energy Survey covering ∼5000 deg2 of the southern sky. Using a multistage multivariate classification and light-curve template-fitting scheme, we identify RR Lyrae candidates with a median of 35 observations per candidate. We detect 6971 RR Lyrae candidates out to ∼335 kpc, and we estimate that our sample is >70% complete at ∼150 kpc. We find excellent agreement with other wide-area RR Lyrae catalogs and RR Lyrae studies targeting the Magellanic Clouds and other Milky Way satellite galaxies. We fit the smooth stellar halo density profile using a broken-power-law model with fixed halo flattening (q = 0.7), and we find strong evidence for a break at = - R 32.1+ kpc 0 0.9 1.1 with an inner slope of = - - n 2.54+ 1 0.09 0.09 and an outer slope of = - - n 5.42+ 2 0.14 0.13. We use our catalog to perform a search for Milky Way satellite galaxies with large sizes and low luminosities. Using a set of simulated satellite galaxies, we find that our RR Lyrae-based search is more sensitive than those using resolved stellar populations in the regime of large (rh 500 pc), low-surface-brightness dwarf galaxies. A blind search for large, diffuse satellites yields three candidate substructures. The first can be confidently associated with the dwarf galaxy Eridanus II. The second has a distance and proper motion similar to the ultrafaint dwarf galaxy Tucana II but is separated by ∼5 deg. The third is close in projection to the globular cluster NGC 1851 but is ∼10 kpc more distant and appears to differ in proper motion., The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007- 2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2020
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33. OzDES multi-object fibre spectroscopy for the Dark Energy Survey: Results and second data release

Author: Enrique Gaztanaga, C. Lidman, J. Carretero, Tim Eifler, B. E. Tucker, E. Swann, Tamara M. Davis, Lluís Galbany, Sara Webb, J. Gschwend, S. Allam, Robert A. Gruendl, Samuel Hinton, Eli S. Rykoff, J. K. Hoormann, Krzysztof Bolejko, W. G. Hartley, G. Gutierrez, M. E. C. Swanson, Mark Sullivan, Edward Macaulay, Anais Möller, Paul Martini, Michael Schubnell, A. Carnero Rosell, Douglas L. Tucker, Kyler Kuehn, Ryan J. Foley, R. D. Wilkinson, Peter Doel, I. Sevilla-Noarbe, Daniel Scolnic, Andrew J. King, N. Kuropatkin, N. E. Sommer, Bonnie Zhang, Felipe Menanteau, M. Pursiainen, G. Tarle, Zhefu Yu, A. Kremin, Fang Yuan, V. Scarpine, Anthony Carr, M. Carrasco Kind, Sunayana Bhargava, David Parkinson, T. N. Varga, L. N. da Costa, S. A. Uddin, A. R. Walker, Robert C. Nichol, A. Roodman, M. Childress, Daniela Carollo, M. Costanzi, K. Honscheid, Juan Garcia-Bellido, E. Bertin, D. Lagattuta, Antonella Palmese, Jennifer L. Marshall, J. De Vicente, Joshua A. Frieman, M. A. G. Maia, D. Mudd, W. C. Wester, Fiona H. Panther, U. Malik, M. March, Basilio X. Santiago, Geraint F. Lewis, Peter Melchior, Richard Scalzo, J. Annis, Rob Sharp, M. Sako, D. L. Hollowood, S. Serrano, Richard Kessler, P. Wiseman, S. Everett, David J. Brooks, Marcos Lima, E. Suchyta, A. A. Plazas, F. J. Castander, Jacobo Asorey, T. M. C. Abbott, D. J. Brout, Michel Aguena, Huan Lin, J. Calcino, David J. James, Pablo Fosalba, E. J. Sanchez, Karl Glazebrook, Ramon Miquel, F. Paz-Chinchón, M. Smith, Daniel Gruen, Tenglin Li, Santiago Avila, A. G. Kim, Lidman, C., Tucker, B. E., Davis, T. M., Uddin, S. A., Asorey, J., Bolejko, K., Brout, D., Calcino, J., Carollo, D., Carr, A., Childress, M., Hoormann, J. K., Foley, R. J., Galbany, L., Glazebrook, K., Hinton, S. R., Kessler, R., Kim, A. G., King, A., Kremin, A., Kuehn, K., Lagattuta, D., Lewis, G. F., Macaulay, E., Malik, U., March, M., Martini, P., Moller, A., Mudd, D., Nichol, R. C., Panther, F., Parkinson, D., Pursiainen, M., Sako, M., Swann, E., Scalzo, R., Scolnic, D., Sharp, R., Smith, M., Sommer, N. E., Sullivan, M., Webb, S., Wiseman, P., Yu, Z., Yuan, F., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., Da Costa, L. N., De Vicente, J., Doel, P., Eifler, T. F., Everett, S., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., T. S., Li, Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Laboratoire de Physique de Clermont (LPC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Australian Research Council, and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS)
Subjects: transients: supernovae, Astrophysics, dark energy [cosmology], 01 natural sciences, 7. Clean energy, law.invention, cosmology: dark energy, supermassive black hole [quasars], law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010303 astronomy & astrophysics, catalogues, Physics, quasars: supermassive black holes, Astrophysics::Instrumentation and Methods for Astrophysics, GALÁXIAS, Supernova, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, surveys, techniques: spectroscopic, catalogue, Astrophysics - Cosmology and Nongalactic Astrophysics, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, supermassive black holessurveys [Quasars], 0103 physical sciences, survey, Spectrograph, Astrophysics::Galaxy Astrophysics, STFC, 010308 nuclear & particles physics, supermassive black holes [quasars], RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Photometry (astronomy), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Quasars: supermassive black holessurveys, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], supernovae [transients]
Abstract: We present a description of the Australian Dark Energy Survey (OzDES) and summarize the results from its 6 years of operations. Using the 2dF fibre positioner and AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope, OzDES has monitored 771 active galactic nuclei, classified hundreds of supernovae, and obtained redshifts for thousands of galaxies that hosted a transient within the 10 deep fields of the Dark Energy Survey. We also present the second OzDES data release, containing the redshifts of almost 30 000 sources, some as faint as r = 24 mag, and 375 000 individual spectra. These data, in combination with the time-series photometry from the Dark Energy Survey, will be used to measure the expansion history of the Universe out to z ∼1.2 and the masses of hundreds of black holes out to z ∼4. OzDES is a template for future surveys that combine simultaneous monitoring of targets with wide-field imaging cameras and wide-field multi-object spectrographs., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Fi-nanciadora de Estudos e Projetos, Fundac¸ão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemein-schaft, and the Collaborating Institutions in the DES. LG was funded by the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement no. 839090. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). Parts of this research were supported by the Australian Research Council under grants DP160100930, FL180100168, and FT140101270.
Published: 2020

34. First cosmology results using type Ia supernovae from the Dark Energy Survey: the effect of host galaxy properties on supernova luminosity

Author: Geraint F. Lewis, C. Frohmaier, David J. Brooks, Samuel Hinton, G. Gutierrez, Sunayana Bhargava, Jennifer L. Marshall, Brad E. Tucker, Eli S. Rykoff, Michel Aguena, A. R. Walker, Josh Frieman, Mark Sullivan, B. Flaugher, Elisabeth Krause, A. Carnero Rosell, M. Pursiainen, G. Tarle, R. R. Gupta, Tim Eifler, D. L. Burke, David J. James, Lluís Galbany, M. E. C. Swanson, Michael Schubnell, Pablo Fosalba, E. Macaulay, R. C. Thomas, S. Allam, Robert A. Gruendl, M. Carrasco Kind, I. Sevilla-Noarbe, J. De Vicente, Robert C. Nichol, Ramon Miquel, E. Suchyta, C. B. D'Andrea, K. Honscheid, Karl Glazebrook, Douglas L. Tucker, Antonella Palmese, N. Kuropatkin, Kyler Kuehn, M. A. G. Maia, Marcus Lima, P. Wiseman, T. N. Varga, L. N. da Costa, Tamara M. Davis, Juan Garcia-Bellido, Daniela Carollo, Peter Melchior, Peter Nugent, Claudia P. Gutiérrez, Felipe Menanteau, Daniel Scolnic, M. Costanzi, A. Roodman, M. Vincenzi, Enrique Gaztanaga, Ryan J. Foley, V. Scarpine, S. Everett, M. Sako, D. L. Hollowood, S. Serrano, Richard Kessler, A. A. Plazas, L. Kelsey, D. J. Brout, W. G. Hartley, N. E. Sommer, A. K. Romer, Paul Martini, F. Paz-Chinchón, M. Smith, Daniel Gruen, Anais Möller, E. Bertin, Peter Doel, H. T. Diehl, Niall MacCrann, J. Gschwend, C. Lidman, E. Swann, Daniel Thomas, E. Buckley-Geer, Santiago Avila, S. Desai, T. M. C. Abbott, E. J. Sanchez, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Smith, M., Sullivan, M., Wiseman, P., Kessler, R., Scolnic, D., Brout, D., D'Andrea, C. B., Davis, T. M., Foley, R. J., Frohmaier, C., Galbany, L., Gupta, R. R., Gutiérrez, C. P., Hinton, S. R., Kelsey, L., Lidman, C., Macaulay, E., Möller, A., Nichol, R. C., Nugent, P., Palmese, A., Pursiainen, M., Sako, M., Swann, E., Thomas, R. C., Tucker, B. E., Vincenzi, M., Carollo, D., Lewis, G. F., Sommer, N. E., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maccrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Walker, A. R., Des, Collaboration, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)
Subjects: transients: supernovae, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Cosmology, Luminosity, surveys, supernovae: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, survey, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Equation of state (cosmology), RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Dark energy, Astrophysics::Earth and Planetary Astrophysics, supernovae [transients], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae], observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present improved photometric measurements for the host galaxies of 206 spectroscopically confirmed type Ia supernovae discovered by the Dark Energy Survey Supernova Program (DES-SN) and used in the first DES-SN cosmological analysis. Fitting spectral energy distributions to the $griz$ photometric measurements of the DES-SN host galaxies, we derive stellar masses and star-formation rates. For the DES-SN sample, when considering a 5D ($z$, $x_1$, $c$, $\alpha$, $\beta$) bias correction, we find evidence of a Hubble residual `mass step', where SNe Ia in high mass galaxies ($>10^{10} \textrm{M}_{\odot}$) are intrinsically more luminous (after correction) than their low mass counterparts by $\gamma=0.040\pm0.019$mag. This value is larger by $0.031$mag than the value found in the first DES-SN cosmological analysis. This difference is due to a combination of updated photometric measurements and improved star formation histories and is not from host-galaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with $\gamma=0.066\pm0.020$mag. The 1D-5D $\gamma$ difference for DES-SN is $0.026\pm0.009$mag. We show that this difference is due to a strong correlation between host galaxy stellar mass and the $x_1$ component of the 5D distance-bias correction. To better understand this effect, we include an intrinsic correlation between light-curve width and stellar mass in simulated SN Ia samples. We show that a 5D fit recovers $\gamma$ with $-9$mmag bias compared to a $+2$mmag bias for a 1D fit. This difference can explain part of the discrepancy seen in the data. Improvements in modeling correlations between galaxy properties and SN is necessary to determine the implications for $\gamma$ and ensure unbiased precision estimates of the dark energy equation-of-state as we enter the era of LSST., Comment: 27 pages, 13 figures; Submitted to MNRAS
Published: 2020
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35. The impact of spectroscopic incompleteness in direct calibration of redshift distributions for weak lensing surveys

Author: Marcos Lima, J. Gschwend, J. DeRose, E. Suchyta, Gary Bernstein, Peter Melchior, R. Cawthon, D. L. Burke, A. Roodman, Felipe Menanteau, Michael Schubnell, David J. James, Joshua A. Frieman, I. Sevilla-Noarbe, Antonella Palmese, R. Miquel, S. Samani, Ofer Lahav, Pablo Fosalba, M. A. G. Maia, W. G. Hartley, M. Smith, J. Carretero, D. L. Hollowood, N. Kuropatkin, David J. Brooks, T. N. Varga, Tamara M. Davis, Jochen Weller, Samuel Hinton, F. J. Castander, Eli S. Rykoff, Risa H. Wechsler, M. Carrasco Kind, Daniel Gruen, L. N. da Costa, Jacobo Asorey, H. T. Diehl, J. Annis, S. Allam, Robert A. Gruendl, G. Gutierrez, S. Serrano, A. Carnero Rosell, R. L. C. Ogando, Elisabeth Krause, T. M. C. Abbott, V. Scarpine, Markus Rau, K. Honscheid, E. Bertin, E. J. Sanchez, Jennifer L. Marshall, A. L. King, Enrique Gaztanaga, D. W. Gerdes, Ben Hoyle, C. Lidman, Michel Aguena, S. Kent, A. A. Plazas, F. Paz-Chinchón, Sarah Bridle, Santiago Avila, L. Whiteway, Chihway Chang, Douglas L. Tucker, Kyler Kuehn, S. Desai, G. Tarle, Marcelle Soares-Santos, Michael Troxel, M. Costanzi, B. Flaugher, R. D. Wilkinson, J. P. Dietrich, Juan Garcia-Bellido, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Generalitat de Catalunya, Hartley, W. G., Chang, C., Samani, S., Carnero Rosell, A., Davis, T. M., Hoyle, B., Gruen, D., Asorey, J., Gschwend, J., Lidman, C., Kuehn, K., King, A., Rau, M. M., Wechsler, R. H., Derose, J., Hinton, S. R., Whiteway, L., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Bertin, E., Bridle, S. L., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Kent, S., Krause, E., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Troxel, M. A., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, media_common.quotation_subject, Large-scale structure of universe, FOS: Physical sciences, Astrophysics, Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Cosmology, Photometry (optics), gravitational lensing: weak, statistics [Galaxies], Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, distances and redshifts [Galaxies], Hardware_INTEGRATEDCIRCUITS, distances and redshift [galaxies], statistic [galaxies], 010303 astronomy & astrophysics, Weak gravitational lensing, galaxies: statistics, media_common, Selection bias, Physics, galaxies: distances and redshifts, large-scale structure of Universe, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysics, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Galaxy, Redshift, Weighting, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: DES Collaboration: et al., Obtaining accurate distributions of galaxy redshifts is a critical aspect of weak lensing cosmology experiments. One of the methods used to estimate and validate redshift distributions is to apply weights to a spectroscopic sample, so that their weighted photometry distribution matches the target sample. In this work, we estimate the selection bias in redshift that is introduced in this procedure. We do so by simulating the process of assembling a spectroscopic sample (including observer-assigned confidence flags) and highlight the impacts of spectroscopic target selection and redshift failures. We use the first year (Y1) weak lensing analysis in Dark Energy Survey (DES) as an example data set but the implications generalize to all similar weak lensing surveys. We find that using colour cuts that are not available to the weak lensing galaxies can introduce biases of up to Δz ∼ 0.04 in the weighted mean redshift of different redshift intervals (Δz ∼ 0.015 in the case most relevant to DES). To assess the impact of incompleteness in spectroscopic samples, we select only objects with high observer-defined confidence flags and compare the weighted mean redshift with the true mean. We find that the mean redshift of the DES Y1 weak lensing sample is typically biased at the Δz = 0.005−0.05 level after the weighting is applied. The bias we uncover can have either sign, depending on the samples and redshift interval considered. For the highest redshift bin, the bias is larger than the uncertainties in the other DES Y1 redshift calibration methods, justifying the decision of not using this method for the redshift estimations. We discuss several methods to mitigate this bias., The DES data management system is supported by the National Science Foundation under grants AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2020

36. The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Author: A. R. Walker, Michel Aguena, Devon L. Hollowood, David J. Brooks, J. Gschwend, Samuel Hinton, Mark Sullivan, G. Gutierrez, J. Carretero, C. Lidman, Santiago Avila, Tamara M. Davis, Antonella Palmese, G. Tarle, A. A. Plazas, A. K. Romer, Paul Martini, David J. James, I. Sevilla-Noarbe, Lluís Galbany, Peter Doel, Daniel Thomas, D. L. Burke, N. Kuropatkin, H. T. Diehl, David Bacon, Agnès Ferté, Pablo Fosalba, M. Costanzi, S. Desai, E. Suchyta, Matthew Grayling, P. Wiseman, T. N. Varga, Juan Garcia-Bellido, F. J. Castander, C. Frohmaier, L. N. da Costa, J. Annis, R. L. C. Ogando, S. Allam, Robert A. Gruendl, F. Paz-Chinchón, S. A. Uddin, T. M. C. Abbott, Kyler Kuehn, D. J. Brout, I. Ferrero, S. Everett, A. G. Kim, K. Honscheid, Lisa Kelsey, Chun-Hao To, Anais Möller, E. Bertin, Jennifer L. Marshall, E. J. Sanchez, Maria Vincenzi, Mathew Smith, R. D. Wilkinson, Claudia P. Gutiérrez, M. Sako, Felipe Menanteau, A. Carnero Rosell, Daniel Scolnic, S. Serrano, Ramon Miquel, Richard Kessler, Ofer Lahav, Robert Morgan, Marcos Lima, Daniel Gruen, Carlos Solans Sanchez, D. W. Gerdes, B. Flaugher, M. Carrasco Kind, UAM. Departamento de Física Teórica, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), Kelsey, L., Sullivan, M., Smith, M., Wiseman, P., Brout, D., Davis, T. M., Frohmaier, C., Galbany, L., Grayling, M., Gutiérrez, C. P., Hinton, S. R., Kessler, R., Lidman, C., Möller, A., Sako, M., Scolnic, D., Uddin, S. A., Vincenzi, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Kim, A. G., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sánchez, C., Sanchez, E., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Walker, A. R., and Wilkinson, R. D.
Subjects: Length scale, Distance Scale, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, general [Supernovae], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Cosmology: Observations, Photometry (optics), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, survey, Astrophysics - Cosmology and Nongalactic Astrophysic, observations [Cosmology], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Distance scale, 010308 nuclear & particles physics, 4. Education, surveys, supernovae: general, distance scale, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Física, Astronomy and Astrophysics, Light curve, Galaxy, Supernovae: General, Supernova, 13. Climate action, Space and Planetary Science, Homogeneous, Astrophysics of Galaxies (astro-ph.GA), Dark energy, ESTRUTURA DO UNIVERSO, Astrophysics::Earth and Planetary Astrophysics, observation [cosmology]
Abstract: This work was supported by the Science and Technology Facilities Council (grant number ST/P006760/1) through the DISCnet Centre forDoctoral Training. M.Sullivan and M.Smith acknowledge support from EU/FP7-ERC grant 615929, and PW acknowledges support from STFC grant ST/R000506/1. LG was funded by the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio StateUniversity, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen ossische Technische Hochschule (ETH) Z urich, Fermi National Accelerator Laboratory, theUniversity of Illinois at Urbana Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit at M unchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2)., This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics., The data underlying this paper are available in the DES3YR data release, available at https://www.darkenergysurvey.org/des-year-3- supernova-cosmology-results/, and in the online supplementary material., Supplementary data are available at MNRAS online. Table 1. Seeing-optimized image stack parameters., Analyses of Type Ia supernovae (SNe Ia) have found puzzling correlations between their standardized luminosities and host galaxy properties: SNe Ia in high-mass, passive hosts appear brighter than those in lower mass, star-forming hosts. We examine the host galaxies of SNe Ia in the Dark Energy Survey 3-yr spectroscopically confirmed cosmological sample, obtaining photometry in a series of 'local' apertures centred on the SN, and for the global host galaxy. We study the differences in these host galaxy properties, such as stellar mass and rest-frame U - R colours, and their correlations with SN Ia parameters including Hubble residuals. We find all Hubble residual steps to be >3 sigma in significance, both for splitting at the traditional environmental property sample median and for the step of maximum significance. For stellar mass, we find a maximal local step of 0.098 +/- 0.018mag; similar to 0.03mag greater than the largest global stellar mass step in our sample (0.070 +/- 0.017mag). When splitting at the sample median, differences between local and global U - R steps are small, both similar to 0.08mag, but are more significant than the global stellar mass step (0.057 +/- 0.017mag). We split the data into sub-samples based on SN Ia light-curve parameters: stretch (x(1)) and colour (c), finding that redder objects (c > 0) have larger Hubble residual steps, for both stellar mass and U - R, for both local and global measurements, of similar to 0.14mag. Additionally, the bluer (star-forming) local environments host a more homogeneous SN Ia sample, with local U - R rms scatter as low as 0.084 +/- 0.017mag for blue (c < 0) SNe Ia in locally blue U - R environments., Science and Technology Facilities Council through the DISCnet Centre forDoctoral Training ST/P006760/1, EU/FP7-ERC grant 615929, UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC) ST/R000506/1, European Commission 839090, Spanish grant within the European Funds for Regional Development (FEDER) PGC2018-095317-B-C21, United States Department of Energy (DOE), National Science Foundation (NSF), Spanish Government, UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC), Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Ohio State University, Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University, Ciencia Tecnologia e Inovacao (FINEP), Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, National Council for Scientific and Technological Development (CNPq), Ministerio da Ciencia, Tecnologia e Inovacao, German Research Foundation (DFG), University of California at Santa Cruz, University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, ETH Zurich, United States Department of Energy (DOE) University of Chicago, University of Illinois at Urbana Champaign, Institut de Ciencies de l'Espai (IEEC/CSIC), Institut de Fisica d'Altes Energies, Ludwig-Maximilians Universit at Munchen and the associated Excellence Cluster Universe, University of Michigan System, National Science Foundation (NSF) NSF - Directorate for Mathematical & Physical Sciences (MPS), University of Nottingham, University of Pennsylvania, University of Portsmouth, Stanford University, University of Sussex, Texas AM University, OzDES Membership Consortium, National Science Foundation (NSF) AST-1138766 AST-1536171, MINECO AYA2015-71825 ESP2015-66861 FPA2015-68048 SEV-2016-0588 SEV-2016-0597 MDM-2015-0509, ERDF funds from the European Union, CERCA program of the Generalitat de Catalunya, European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013), European Research Council (ERC) European Commission 240672 291329 306478, National Council for Scientific and Technological Development (CNPq) 465376/2014-2, Kavli Institute of Cosmological Physics at the University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh
Published: 2020
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37. Chemical Analysis of the Ultrafaint Dwarf Galaxy Grus II. Signature of High-mass Stellar Nucleosynthesis

Author: David J. Brooks, R. A. Bernstein, Jennifer L. Marshall, J. Gschwend, A. Carnero Rosell, N. Kuropatkin, V. Scarpine, E. Buckley-Geer, D. L. Hollowood, S. Serrano, K. D. Eckert, T. N. Varga, L. N. da Costa, M. Carrasco Kind, Peter Doel, H. T. Diehl, S. Everett, J. D. Simon, K. Honscheid, Daniela Carollo, Marla Geha, D. Q. Nagasawa, J. Carretero, Marcelle Soares-Santos, Shantanu Desai, E. Bertin, Kyler Kuehn, E. J. Sanchez, Joshua A. Frieman, E. Suchyta, Gregory Tarle, I. Ferrero, P. Ferguson, Terese T. Hansen, Tenglin Li, Santiago Avila, Enrique Gaztanaga, Andrew B. Pace, Tim Eifler, M. E. C. Swanson, A. A. Plazas, David J. James, M. Costanzi, D. L. Burke, Juan Garcia-Bellido, S. Allam, Robert A. Gruendl, R. D. Wilkinson, Antonella Palmese, Ramon Miquel, M. A. G. Maia, Michel Aguena, M. March, Basilio X. Santiago, A. R. Walker, J. De Vicente, Samuel Hinton, G. Gutierrez, M. Smith, Daniel Gruen, D. W. Gerdes, F. Paz-Chinchón, Hansen, T. T., Marshall, J. L., Simon, J. D., Li, T. S., Bernstein, R. A., Pace, A. B., Ferguson, P., Nagasawa, D. Q., Kuehn, K., Carollo, D., Geha, M., James, D., Walker, A., Diehl, H. T., Aguena, M., Allam, S., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Costanzi Alunno Cerbolini, M., Da Costa, L. N., Desai, S., Vicente, J. D., Doel, P., Eckert, K., Eifler, T. F., Everett, S., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuropatkin, N., Maia, M. A. G., March, M., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Wilkinson, R., National Science Foundation (US), National Aeronautics and Space Administration (US), Kavli Institute for Particle Astrophysics and Cosmology, Department of Energy (US), Higher Education Funding Council for England, Ministerio de Ciencia y Tecnología (España), University of Illinois, University of Chicago, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), German Research Foundation, Ministerio de Economía y Competitividad (España), European Commission, University of California, University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (España), University of Edinburgh, University of Michigan, National Optical Astronomy Observatory (US), University of Nottingham, The Ohio State University, University of Pennsylvania, University of Sussex, and Texas A&M University
Subjects: Initial mass function, 010504 meteorology & atmospheric sciences, Milky Way, Chemical abundances, Dwarf galaxies, Chemically peculiar stars, Stellar abundances, FOS: Physical sciences, GALÁXIA (VIA LÁCTEA), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Stellar nucleosynthesis, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, Physics, Chemically peculiar star, Astronomy and Astrophysics, Chemical abundance, Astrophysics - Astrophysics of Galaxies, Abundance of the chemical elements, Galaxy, Astrophysics - Solar and Stellar Astrophysics, Dwarf galaxie, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: We present a detailed abundance analysis of the three brightest member stars at the top of the giant branch of the ultrafaint dwarf (UFD) galaxy Grus II. All stars exhibit a higher than expected [Mg/Ca] ratio compared to metal-poor stars in other UFD galaxies and in the Milky Way (MW) halo. Nucleosynthesis in high-mass (20 M o) core-collapse supernovae has been shown to create this signature. The abundances of this small sample (three) stars suggests the chemical enrichment of Grus II could have occurred through substantial high-mass stellar evolution, and is consistent with the framework of a top-heavy initial mass function. However, with only three stars it cannot be ruled out that the abundance pattern is the result of a stochastic chemical enrichment at early times in the galaxy. The most metal-rich of the three stars also possesses a small enhancement in rapid neutron-capture (r-process) elements. The abundance pattern of the r-process elements in this star matches the scaled r-process pattern of the solar system and r-process enhanced stars in other dwarf galaxies and in the MW halo, hinting at a common origin for these elements across a range of environments. All current proposed astrophysical sites of r-process element production are associated with high-mass stars, thus the possible top-heavy initial mass function of Grus II would increase the likelihood of any of these events occurring. The time delay between the and r-process element enrichment of the galaxy favors a neutron star merger as the origin of the r-process elements in Grus II., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The collaborating institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo InterAmerican Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. I.F.A.E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007- 2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). T.T.H and J.D.S acknowledge support from NSF grant AST1714873. T.S.L. is supported by NASA through Hubble Fellowship grant HST-HF2-51439.001, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2020

38. STRIDES: Spectroscopic and photometric characterization of the environment and effects of mass along the line of sight to the gravitational lenses DES J0408-5354 and WGD 2038-4008

Author: F. J. Castander, B. Flaugher, Peter Doel, H. T. Diehl, Josh Frieman, Samuel Hinton, E. J. Sanchez, G. Gutierrez, I. Sevilla-Noarbe, N. Kuropatkin, T. N. Varga, L. N. da Costa, Peter Melchior, Douglas L. Tucker, Kyler Kuehn, Sunayana Bhargava, Huan Lin, M. E. C. Swanson, K. Honscheid, J. Carretero, F. Paz-Chinchón, V. Scarpine, Jennifer L. Marshall, M. Costanzi, Tim Eifler, Santiago Avila, Michael Schubnell, Lise Christensen, Antonella Palmese, G. Tarle, E. Buckley-Geer, G. Meylan, M. Smith, David J. James, Daniel Gruen, M. A. G. Maia, Marcelle Soares-Santos, S. Desai, Cristian Rusu, Felipe Menanteau, E. Bertin, S. Serrano, David J. Brooks, Pablo Fosalba, Tommaso Treu, J. Poh, Anowar J. Shajib, Michel Aguena, J. Gschwend, A. Carnero Rosell, S. Allam, Robert A. Gruendl, A. A. Plazas, E. Suchyta, Simon Birrer, A. Agnello, S. Everett, Ramon Miquel, Thomas E. Collett, R. L. C. Ogando, Christopher D. Fassnacht, Juan Garcia-Bellido, Kenneth C. Wong, M. Carrasco Kind, Sampath Mukherjee, Enrique Gaztanaga, Timo Anguita, J. De Vicente, Buckley-Geer, E J, Lin, H, Rusu, C E, Poh, J, Palmese, A, Agnello, A, Christensen, L, Frieman, J, Shajib, A J, Treu, T, Collett, T, Birrer, S, Anguita, T, Fassnacht, C D, Meylan, G, Mukherjee, S, Wong, K C, Aguena, M, Allam, S, Avila, S, Bertin, E, Bhargava, S, Brooks, D, Carnero&nbsp, Rosell, A, Carrasco&nbsp, Kind, M, Carretero, J, Castander, F J, Costanzi, M, da&nbsp, Costa, L N, De&nbsp, Vicente, J, Desai, S, Diehl, H T, Doel, P, Eifler, T F, Everett, S, Flaugher, B, Fosalba, P, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hinton, S R, Honscheid, K, James, D J, Kuehn, K, Kuropatkin, N, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Ogando, R L C, Paz-Chinchón, F, Plazas, A A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Tucker, D L, Varga, T N, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, European Space Agency, National Aeronautics and Space Administration (US), European Research Council, European Commission, and Ministerio de Economía y Competitividad (España)
Subjects: Software_OPERATINGSYSTEMS, redshifts, ANGULAR MASKS, h-0, quasars: individual: des j0408-5354, wgd 2038-4008, Astrophysics, I, 7. Clean energy, 01 natural sciences, Spectral line, Gravitation, individual: DES J0408-5354, WGD 2038-4008 [quasars], galaxies: groups: general, clusters, 010303 astronomy & astrophysics, Physics, galaxy-group identification, Line-of-sight, individual: DES J0408-5354 [quasars], gravitational lensing: strong, Velocity dispersion, ComputerSystemsOrganization_PROCESSORARCHITECTURES, i, WGD 2038–4008, STELLAR POPULATION SYNTHESIS, strong [gravitational lensing], quasars: individual: DES J0408–5354, stellar population synthesis, quasars: individual: DES J0408-5354, WGD 2038-4008, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), QUASARES, ComputingMethodologies_SIMULATIONANDMODELING, FOS: Physical sciences, Probability density function, Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, REDSHIFTS, Astrophysics - Astrophysics of Galaxie, evolution, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, GALAXY-GROUP IDENTIFICATION, STFC, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, groups: general [galaxies], H-0, RCUK, resolution, Astronomy and Astrophysics, Quasar, angular masks, Redshift, Galaxy, EVOLUTION, RESOLUTION, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CLUSTERS
Abstract: The DES Collaboration: et al., In time-delay cosmography, three of the key ingredients are (1) determining the velocity dispersion of the lensing galaxy, (2) identifying galaxies and groups along the line of sight with sufficient proximity and mass to be included in the mass model, and (3) estimating the external convergence κext from less massive structures that are not included in the mass model. We present results on all three of these ingredients for two time-delay lensed quad quasar systems, DES J0408–5354 and WGD 2038–4008 . We use the Gemini, Magellan, and VLT telescopes to obtain spectra to both measure the stellar velocity dispersions of the main lensing galaxies and to identify the line-of-sight galaxies in these systems. Next, we identify 10 groups in DES J0408–5354 and two groups in WGD 2038–4008 using a group-finding algorithm. We then identify the most significant galaxy and galaxy-group perturbers using the ‘flexion shift’ criterion. We determine the probability distribution function of the external convergence κext for both of these systems based on our spectroscopy and on the DES-only multiband wide-field observations. Using weighted galaxy counts, calibrated based on the Millennium Simulation, we find that DES J0408–5354 is located in a significantly underdense environment, leading to a tight (width ∼3 per cent⁠), negative-value κext distribution. On the other hand, WGD 2038–4008 is located in an environment of close to unit density, and its low source redshift results in a much tighter κext of ∼1 per cent⁠, as long as no external shear constraints are imposed., JP would like to thank Gourav Khullar for his help and insightful discussions that helped improve the analysis in this paper. This work made use of computing resources and support provided by the Research Computing Center at the University of Chicago. JP is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. AJS was supported by the National Aeronautics and Space Administration (NASA) through the Space Telescope Science Institute (STScI) grant HST-GO-15320. AJS was also supported by the Dissertation Year Fellowship from the University of California, Los Angeles (UCLA) graduate division. TA acknowledges support from Proyecto FONDECYT N: 1190335. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. CDF acknowledges support for this work from the National Science Foundation under Grant No. AST-1715611. SM acknowledges the funding from the European Research Council (ERC) under the EUs Horizon 2020 research and innovation program (COSMICLENS; grant agreement No. 787886). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-88861, FPA2015-68048, SEV-2012-0234, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.
Published: 2020
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39. Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution?

Author: R. L. C. Ogando, Brian Yanny, Enrique Gaztanaga, Antonella Palmese, E. Suchyta, S. Everett, August E. Evrard, M. A. G. Maia, Matt Hilton, Tesla E. Jeltema, A. Choi, J. Carretero, Douglas L. Tucker, Kyler Kuehn, G. Tarle, K. Honscheid, M. Costanzi, Michel Aguena, J. Gschwend, David J. James, M. Carrasco Kind, Ofer Lahav, D. L. Burke, Pablo Fosalba, Scarpine, Markus Rau, Chang Chihway, B. Flaugher, S. Allam, Robert A. Gruendl, T. M. C. Abbott, D. L. Hollowood, David J. Brooks, A. A. Plazas, M. March, Basilio X. Santiago, Ben Hoyle, Josh Frieman, Jesse B. Golden-Marx, J. Annis, J. De Vicente, E. J. Sanchez, Mohr Joe, N. Kuropatkin, T. N. Varga, L. N. da Costa, Santiago Avila, Chihway Chang, Jennifer L. Marshall, F. Paz-Chinchón, Michael Schubnell, H. Sampaio-Santos, Pagul Amanda, Joe Zuntz, M. Smith, Daniel Gruen, T. Shin, D. W. Gerdes, M. Gatti, Samuel Hinton, G. Gutierrez, Risa H. Wechsler, Matt J. Jarvis, Yanxi Zhang, Ramon Miquel, E. Bertin, Peter Doel, K. Herner, H. T. Diehl, Juan Garcia-Bellido, Sampaio-Santos, H., Zhang, Y., Ogando, R. L. C., Shin, T., Golden-Marx, Jesse B., Yanny, B., Herner, K., Hilton, M., Choi, A., Gatti, M., Gruen, D., Hoyle, B., Rau, M. M., De Vicente, J., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Marshall, J. L., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Tucker, D. L., Varga, T. N., Wechsler, R. H., UAM. Departamento de Física Teórica, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: galaxies: clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Evolution, galaxies: photometry, dark matter, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Optical Light, Luminosity, Clusters, Photometry, Astrophysics - Astrophysics of Galaxie, Clusters: General [Galaxies], Stellar Haloes, 0103 physical sciences, Cluster (physics), Galaxy formation and evolution, Satellite galaxy, Galaxies: Photometry, Dark Matter, Surface brightness, General, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Dark Energy Survey, Física, Astronomy and Astrophysics, Illustristng Simulations, Mass, Galaxies, Galaxy, Space and Planetary Science, cluster [galaxies], Astrophysics of Galaxies (astro-ph.GA), Calibration, photometry [galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: Clusters: General
Abstract: We explore the relation between diffuse intracluster light (central galaxy included) and the galaxy cluster (baryonic and dark) matter distribution using a sample of 528 clusters at $0.2\leq z \leq 0.35$ found in the Dark Energy Survey (DES) Year 1 data. The surface brightness of the diffuse light shows an increasing dependence on cluster total mass at larger radius, and appears to be self-similar with a universal radial dependence after scaling by cluster radius. We also compare the diffuse light radial profiles to the cluster (baryonic and dark) matter distribution measured through weak lensing and find them to be comparable. The IllustrisTNG galaxy formation simulation, TNG300, offers further insight into the connection between diffuse stellar mass and cluster matter distributions -- the simulation radial profile of the diffuse stellar component does not have a similar slope with the total cluster matter content, although that of the cluster satellite galaxies does. Regardless of the radial trends, the amount of diffuse stellar mass has a low-scatter scaling relation with cluster's total mass in the simulation, out-performing the total stellar mass of cluster satellite galaxies. We conclude that there is no consistent evidence yet on whether or not diffuse light is a faithful radial tracer of the cluster matter distribution. Nevertheless, both observational and simulation results reveal that diffuse light is an excellent indicator of the cluster's total mass., Comment: Accepted on MNRAS
Published: 2020
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40. Milky Way Satellite Census -- II. Galaxy-Halo Connection Constraints Including the Impact of the Large Magellanic Cloud

Author: Nadler, E.O., Wechsler, R.H., Bechtol, K., Mao, Y.-Y., Green, G., Drlica-Wagner, A., McNanna, M., Mau, S., Pace, A.B., Simon, J.D., Kravtsov, A., Dodelson, S., Li, T.S., Riley, A.H., Wang, M.Y., Abbott, T.M.C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G.M., Bertin, E., Brooks, D., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L.N., De Vicente, J., Desai, S., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W.G., Hinton, S.R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M.A.G., Marshall, J.L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A.A., Romer, A.K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T.N., Walker, A.R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Kavli Institute for Particle Astrophysics and Cosmology, National Aeronautics and Space Administration (US), Department of Energy (US), Ministerio de Ciencia e Innovación (España), Science and Technology Facilities Council (UK), University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Generalitat de Catalunya, Nadler, E. O., Wechsler, R. H., Bechtol, K., Mao, Y. -Y., Green, G., Drlica-Wagner, A., Mcnanna, M., Mau, S., Pace, A. B., Simon, J. D., Kravtsov, A., Dodelson, S., T. S., Li, Riley, A. H., Wang, M. Y., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T. N., and Walker, A. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Virial theorem, Galactic halo, Galaxy abundances, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Milky Way dark matter halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, Physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The population of Milky Way (MW) satellites contains the faintest known galaxies and thus provides essential insight into galaxy formation and dark matter microphysics. Here we combine a model of the galaxy-halo connection with newly derived observational selection functions based on searches for satellites in photometric surveys over nearly the entire high Galactic latitude sky. In particular, we use cosmological zoom-in simulations of MW-like halos that include realistic Large Magellanic Cloud (LMC) analogs to fit the position-dependent MW satellite luminosity function. We report decisive evidence for the statistical impact of the LMC on the MW satellite population due to an estimated 6 ± 2 observed LMC-associated satellites, consistent with the number of LMC satellites inferred from Gaia proper-motion measurements, confirming the predictions of cold dark matter models for the existence of satellites within satellite halos. Moreover, we infer that the LMC fell into the MW within the last 2 Gyr at high confidence. Based on our detailed full-sky modeling, we find that the faintest observed satellites inhabit halos with peak virial masses below 3.2× 10 M· at 95% confidence, and we place the first robust constraints on the fraction of halos that host galaxies in this regime. We predict that the faintest detectable satellites occupy halos with peak virial masses above 10 M·, highlighting the potential for powerful galaxy formation and dark matter constraints from future dwarf galaxy searches., This research received support from the National Science Foundation (NSF) under grant No. NSF AST-1517422, grant No. NSF PHY17-48958 through the Kavli Institute for Theoretical Physics program “The Small-Scale Structure of Cold(?) Dark Matter,” and grant No. NSF DGE-1656518 through the NSF Graduate Research Fellowship received by E.O.N. Support for Y.-Y.M. was provided by the Pittsburgh Particle Physics, Astrophysics and Cosmology Center through the Samuel P. Langley PITT PACC Postdoctoral Fellowship and NASA through NASA Hubble Fellowship grant No. HST-HF2-51441.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Part of this work was performed at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. This research made use of computational resources at SLAC National Accelerator Laboratory, a U.S. Department of Energy Office; the authors are thankful for the support of the SLAC computational team. This research made use of the Sherlock cluster at the Stanford Research Computing Center (SRCC); the authors are thankful for the support of the SRCC team. This research made use of https://arXiv.org and NASA’s Astrophysics Data System for bibliographic information. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the NSFʼs National Optical-Infrared Astronomy Laboratory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This work is based in part on observations at Cerro Tololo Inter-American Observatory, NSFʼs National Optical-Infrared Astronomy Laboratory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. The IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/ 2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by the Fermi Research Alliance, LLC, under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2019

41. Milky Way Satellite Census. I. The Observational Selection Function for Milky Way Satellites in DES Y3 and Pan-STARRS DR1

Author: Elisabeth Krause, Shantanu Desai, Ramon Miquel, Tim Eifler, S. Everett, Peter Melchior, Alex Drlica-Wagner, J. D. Simon, I. Sevilla-Noarbe, J. L. Marshall, D. H. Brooks, Sahar S. Allam, Kyler Kuehn, Peter Doel, K. Honscheid, H. T. Diehl, D. Gruen, J. Frieman, Alistair R. Walker, M. Carrasco Kind, M. A. G. Maia, James Annis, Antonella Palmese, E. Bertin, Adriano Pieres, Juan Garcia-Bellido, Felipe Menanteau, Enrique Gaztanaga, Eduardo Rozo, Gregory Tarle, B. Flaugher, Andrew B. Pace, Robert A. Gruendl, D. L. Burke, G. Gutierrez, David James, J. De Vicente, Risa H. Wechsler, J. Gschwend, E. Suchyta, Keith Bechtol, M. S. Schubnell, M. Costanzi, M. McNanna, N. P. Kuropatkin, M. Smith, J. Carretero, Tenglin Li, E. J. Sanchez, L. N. da Costa, A. A. Plazas, A. Carnero Rosell, S. Mau, Ethan O. Nadler, V. Scarpine, Santiago Serrano, Ofer Lahav, T. M. C. Abbott, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), National Aeronautics and Space Administration (US), Department of Energy (US), Ministerio de Ciencia e Innovación (España), Science and Technology Facilities Council (UK), University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Drlica-Wagner, A., Bechtol, K., Mau, S., Mcnanna, M., Nadler, E. O., Pace, A. B., T. S., Li, Pieres, A., Rozo, E., Simon, J. D., Walker, A. R., Wechsler, R. H., Abbott, T. M. C., Allam, S., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. C., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Palmese, A., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., and Tarle, G.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Higher education, Milky way galaxy, Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Milky Way Galaxy, 0103 physical sciences, Dark matter, media_common.cataloged_instance, Local group, European union, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Government, business.industry, European research, Astronomy and Astrophysics, Dwarf spheroidal galaxie, Dwarf spheroidal galaxies, Census, Astrophysics - Astrophysics of Galaxies, Graduate research, Alliance, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Local Group, National laboratory, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the results of a systematic search for ultra-faint Milky Way satellite galaxies using data from the Dark Energy Survey (DES) and Pan-STARRS1 (PS1). Together, DES and PS1 provide multi-band photometry in optical/near-infrared wavelengths over ∼80% of the sky. Our search for satellite galaxies targets ∼25,000 deg of the high-Galactic-latitude sky reaching a 10σ point-source depth of ⪆22.5 mag in the g and r bands. While satellite galaxy searches have been performed independently on DES and PS1 before, this is the first time that a self-consistent search is performed across both data sets. We do not detect any new high-significance satellite galaxy candidates, recovering the majority of satellites previously detected in surveys of comparable depth. We characterize the sensitivity of our search using a large set of simulated satellites injected into the survey data. We use these simulations to derive both analytic and machine-learning models that accurately predict the detectability of Milky Way satellites as a function of their distance, size, luminosity, and location on the sky. To demonstrate the utility of this observational selection function, we calculate the luminosity function of Milky Way satellite galaxies, assuming that the known population of satellite galaxies is representative of the underlying distribution. We provide access to our observational selection function to facilitate comparisons with cosmological models of galaxy formation and evolution., This research was supported in part by the National Science Foundation (NSF) under Grant No. NSF PHY-1748958 through the Kavli Institute for Theoretical Physics program “The SmallScale Structure of Cold(?) Dark Matter,” and grant no. NSF DGE1656518 through the NSF Graduate Research Fellowship received by E.O.N. This research made use of computational resources at SLAC National Accelerator Laboratory, a U.S. Department of Energy Office; the authors thank the support of the SLAC computational team. This research has made use of the WEBDA database, operated at the Department of Theoretical Physics and Astrophysics of the Masaryk University. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the NSFs National Optical-Infrared Astronomy Laboratory, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This work is based in part on observations at Cerro Tololo Inter-American Observatory, NSFs National Optical-Infrared Astronomy Laboratory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016- 0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC, under contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The U.S. Government retains—and the publisher, by accepting the article for publication, acknowledges that the U.S. government retains—a non-exclusive, paidup, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for U.S. government purposes.
Published: 2019

42. Dark Energy Surveyed Year 1 results: calibration of cluster mis-centring in the redMaPPer catalogues

Author: W. G. Hartley, C. Stern, Devon L. Hollowood, John P. Stott, Ramon Miquel, A. Bermeo, B. Flaugher, Martin Sahlén, Chris A. Collins, Eli S. Rykoff, Elisabeth Krause, Tesla E. Jeltema, Yanxi Zhang, Shantanu Desai, C. J. Miller, Arya Farahi, A. A. Plazas, J. Gschwend, Marcelle Soares-Santos, M. E. C. Swanson, M. Costanzi, Xi Chen, Vinu Vikram, J. P. Dietrich, R. H. Schindler, Juan Garcia-Bellido, W. C. Wester, E. Bertin, David J. Brooks, M. Klein, A. Carnero Rosell, J. Carretero, Peter Melchior, Sunayana Bhargava, M. Smith, Eduardo Rozo, Jennifer L. Marshall, Daniel Gruen, G. Gutierrez, S. W. Allen, D. L. Burke, Peter Doel, R. D. Wilkinson, Maria Manolopoulou, S. Allam, Robert A. Gruendl, Pablo Fosalba, K. Honscheid, H. T. Diehl, V. Scarpine, S. Everett, G. Tarle, August E. Evrard, Ricardo L. C. Ogando, Julian A. Mayers, J. De Vicente, Ben Hoyle, Daniel Thomas, Felipe Menanteau, Robert G. Mann, M. A. G. Maia, A. von der Linden, G. Morris, Risa H. Wechsler, E. Suchyta, Matt Hilton, S. Serrano, M. Carrasco Kind, C. Vergara Cervantes, Marcos Lima, I. Sevilla-Noarbe, Enrique Gaztanaga, N. Kuropatkin, M. Splettstoesser, Adam Mantz, L. N. da Costa, Joshua A. Frieman, Douglas L. Tucker, Kyler Kuehn, Paul Giles, A. K. Romer, Santiago Avila, Keith Bechtol, F. J. Castander, Pedro T. P. Viana, E. J. Sanchez, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Zhang, Y., Jeltema, T., Hollowood, D. L., Everett, S., Rozo, E., Farahi, A., Bermeo, A., Bhargava, S., Giles, P., Romer, A. K., Wilkinson, R., Rykoff, E. S., Mantz, A., Diehl, H. T., Evrard, A. E., Stern, C., Gruen, D., von der Linden, A., Splettstoesser, M., Chen, X., Costanzi, M., Allen, S., Collins, C., Hilton, M., Klein, M., Mann, R. G., Manolopoulou, M., Morris, G., Mayers, J., Sahlen, M., Stott, J., Vergara Cervantes, C., Viana, P. T. P., Wechsler, R. H., Allam, S., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., Hoyle, B., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Wester, W., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: general, dark energy, X-rays: galaxies: clusters, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, media_common.cataloged_instance, clusters: general [galaxies], European union, Astronomy observatory, 010303 astronomy & astrophysics, media_common, QB, Physics, 010308 nuclear & particles physics, European research, GALÁXIAS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Research council, Astrophysics of Galaxies (astro-ph.GA), Fundamental physics, Christian ministry, galaxies: clusters [X-rays], National laboratory, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The center determination of a galaxy cluster from an optical cluster finding algorithm can be offset from theoretical prescriptions or $N$-body definitions of its host halo center. These offsets impact the recovered cluster statistics, affecting both richness measurements and the weak lensing shear profile around the clusters. This paper models the centering performance of the \RM~cluster finding algorithm using archival X-ray observations of \RM-selected clusters. Assuming the X-ray emission peaks as the fiducial halo centers, and through analyzing their offsets to the \RM~centers, we find that $\sim 75\pm 8 \%$ of the \RM~clusters are well centered and the mis-centered offset follows a Gamma distribution in normalized, projected distance. These mis-centering offsets cause a systematic underestimation of cluster richness relative to the well-centered clusters, for which we propose a descriptive model. Our results enable the DES Y1 cluster cosmology analysis by characterizing the necessary corrections to both the weak lensing and richness abundance functions of the DES Y1 redMaPPer cluster catalog., Code used in this analysis is available from https://github.com/yyzhang/center_modeling_y1
Published: 2019

43. Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters

Author: Peter Doel, Elisabeth Krause, David J. James, Alistair R. Walker, Pablo Fosalba, H. T. Diehl, Douglas L. Tucker, J. Carretero, Jochen Weller, Pedro T. P. Viana, Kyler Kuehn, E. J. Sanchez, Paul Giles, I. Sevilla-Noarbe, Eli S. Rykoff, David Brooks, M. E. C. Swanson, N. Kuropatkin, Shantanu Desai, J. P. Dietrich, Ramon Miquel, Adam Mantz, L. N. da Costa, Mathew Smith, M. Carrasco Kind, A. Bermeo, C. Vergara Cervantes, Daniel Thomas, Marcos Lima, E. Buckley-Geer, Xi Chen, V. Scarpine, R. L. C. Ogando, Tesla E. Jeltema, Sunayana Bhargava, Michael Schubnell, Joshua A. Frieman, G. Gutierrez, Robert G. Mann, Jennifer L. Marshall, J. Gschwend, K. Honscheid, Enrique Gaztanaga, M. Costanzi, Yanxi Zhang, Julian A. Mayers, A. K. Romer, August E. Evrard, Arya Farahi, Flavia Sobreira, S. Serrano, Felipe Menanteau, B. Flaugher, John P. Stott, Gregory Tarle, R. D. Wilkinson, A. Carnero Rosell, S. Everett, P. Rooney, D. L. Burke, Juan Garcia-Bellido, Martin Sahlén, Chris A. Collins, Eduardo Rozo, J. Annis, Robert A. Gruendl, Vinu Vikram, J. De Vicente, E. Suchyta, Matt Hilton, Santiago Avila, Devon L. Hollowood, Andrew R. Liddle, Francisco J. Castander, A. A. Plazas, Daniel Gruen, D. W. Gerdes, M. A. G. Maia, Peter Melchior, Farahi, A., Chen, X., Evrard, A. E., Hollowood, D. L., Wilkinson, R., Bhargava, S., Giles, P., Romer, A. K., Jeltema, T., Hilton, M., Bermeo, A., Mayers, J., Vergara Cervantes, C., Rozo, E., Rykoff, E. S., Collins, C., Costanzi, M., Everett, S., Liddle, A. R., Mann, R. G., Mantz, A., Rooney, P., Sahlen, M., Stott, J., Viana, P. T. P., Zhang, Y., Annis, J., Avila, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., da Costa, L. N., de Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, 0103 physical sciences, 010306 general physics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, Scaling, STFC, ComputingMilieux_MISCELLANEOUS, QC, Galaxy cluster, QB, Confidence region, Physics, clusters: general - X-rays: galaxies: clusters [Galaxies], RCUK, Astronomy and Astrophysics, Covariance, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Log-normal distribution, astro-ph.CO, Galaxies: clusters: general - X-rays: galaxies: clusters, galaxies: clusters [X-rays], Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using archival X-ray observations and a log-normal population model, we estimate constraints on the intrinsic scatter in halo mass at fixed optical richness for a galaxy cluster sample identified in Dark Energy Survey Year-One (DES-Y1) data with the redMaPPer algorithm. We examine the scaling behavior of X-ray temperatures, $T_X$, with optical richness, $\lambda_{RM}$, for clusters in the redshift range $0.2 50\%$ complete for clusters with $\lambda_{RM} > 130$. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, $\sigma_{\ln Tx | \lambda} = 0.275 \pm 0.019$. Joined with constraints for $T_X$ scaling with halo mass from the Weighing the Giants program and richness--temperature covariance estimates from the LoCuSS sample, we derive the richness-conditioned scatter in mass, $\sigma_{\ln M | \lambda} = 0.30 \pm 0.04\, _{({\rm stat})} \pm 0.09\, _{({\rm sys})}$, at an optical richness of approximately 70. Uncertainties in external parameters, particularly the slope and variance of the $T_X$--mass relation and the covariance of $T_X$ and $\lambda_{RM}$ at fixed mass, dominate the systematic error. The $95\%$ confidence region from joint sample analysis is relatively broad, $\sigma_{\ln M | \lambda} \in [0.14, \, 0.55]$, or a factor ten in variance., Comment: 14 pages. Main results are Figure 3, 5, and 6, Table 2, and Equation 9. Submitted to MNRAS. Comments welcome
Published: 2019

44. Supernova Siblings: Assessing the Consistency of Properties of Type Ia Supernovae that Share the Same Parent Galaxies

Author: W. G. Hartley, V. Scarpine, N. E. Sommer, I. Sevilla-Noarbe, David J. Brooks, David J. James, G. Tarle, N. Kuropatkin, A. A. Plazas, Jennifer L. Marshall, Ramon Miquel, K. D. Eckert, Ryan J. Foley, T. N. Varga, L. N. da Costa, L. Kelsey, K. Kuehn, Karl Glazebrook, Lluís Galbany, C. Lidman, Samuel Hinton, Robert Morgan, Anais Möller, E. Bertin, E. Suchyta, Marcus Lima, G. Gutierrez, Edward Macaulay, P. Doel, Geraint F. Lewis, Alex Drlica-Wagner, M. Costanzi, J. Gschwend, D. J. Brout, Daniela Carollo, Salcedo Romero de Ávila, A. Massiah, T. F. Eifler, Tianjun Li, Michael Schubnell, P. Wiseman, J. Annis, Brodie Popovic, Joshua A. Frieman, T. M. C. Abbott, P. Fosalba, R. D. Wilkinson, M. Pursiainen, S. Everett, E. J. Sanchez, H. T. Diehl, K. Honscheid, M. Carrasco Kind, M. Sako, Robert C. Nichol, D. L. Hollowood, M. E. C. Swanson, B. Flaugher, S. Serrano, Richard Kessler, S. Desai, Enrique Gaztanaga, M. N. K. Smith, Mark Sullivan, Felipe Menanteau, K. Bechtol, Juan Garcia-Bellido, A. Carnero Rosell, A. R. Walker, J. De Vicente, Antonella Palmese, Daniel Gruen, D. L. Burke, M. A. G. Maia, Daniel Scolnic, B. P. Thomas, D. W. Gerdes, S. Allam, Robert A. Gruendl, B. E. Tucker, Michel Aguena, J. Carretero, R. Hounsell, Tamara M. Davis, F. Paz-Chinchón, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), National Aeronautics and Space Administration (US), European Commission, European Research Council, Department of Energy (US), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Scolnic, D., Smith, M., Massiah, A., Wiseman, P., Brout, D., Kessler, R., Davis, T. M., Foley, R. J., Galbany, L., Hinton, S. R., Hounsell, R., Kelsey, L., Lidman, C., Macaulay, E., Morgan, R., Nichol, R. C., Moller, A., Popovic, B., Sako, M., Sullivan, M., Thomas, B. P., Tucker, B. E., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. C., Carollo, D., Kind, M. C., Carretero, J., Costanzi Alunno Cerbolini, M., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lewis, G. F., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Pursiainen, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Walker, A. R., and Wilkinson, R.
Subjects: Observational cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), 01 natural sciences, 7. Clean energy, Consistency (statistics), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation), Physics, Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Distance modulus, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: et al. arXiv:2002.00974v2, While many studies have shown a correlation between properties of the light curves of SNe Ia and properties of their host galaxies, it remains unclear what is driving these correlations. We introduce a new direct method to study these correlations by analyzing "parent" galaxies that host multiple SNe Ia "siblings." Here, we search the Dark Energy Survey SN sample, one of the largest samples of discovered SNe, and find eight galaxies that hosted two likely SNe Ia. Comparing the light-curve properties of these SNe and recovered distances from the light curves, we find no better agreement between properties of SNe in the same galaxy as any random pair of galaxies, with the exception of the SN light-curve stretch. We show at 2.8σ significance that at least one-half of the intrinsic scatter of SNe Ia distance modulus residuals is not from common host properties. We also discuss the robustness with which we could make this evaluation with LSST, which will find 100× more pairs of galaxies, and pave a new line of study on the consistency of SNe Ia in the same parent galaxies. Finally, we argue that it is unlikely that some of these SNe are actually single, lensed SN with multiple images., D.S. is supported by DOE grant DE-SC0010007, the David and Lucile Packard Foundation. D.S. and R.K. are supported in part by NASA under Contract No. NNG17PX03C issued through the WFIRST Science Investigation Teams Programme. D.B. and M.S. were supported by DOE grant DE-FOA0001358 and NSF grant AST-1517742. L.G. was funded by the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 839090. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We are grateful for the support of the University of Chicago Research Computing Center for assistance with the calculations carried out in this work. R.F. is supported in part by NSF grants AST-1518052 and AST1815935, the Gordon & Betty Moore Foundation, the HeisingSimons Foundation, and by fellowships from the David and Lucile Packard Foundation, as well as the NASA contract above. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo InterAmerican Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). We acknowledge support from EU/FP7-ERC grant No. 615929. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2020

45. The Dark Energy Survey Data Release 1

Author: M. W. G. Johnson, M. Baumer, Tesla E. Jeltema, Eric H. Neilsen, Peter Nugent, Martin Crocce, S. Hamilton, M. Smith, Antonella Palmese, Nora Shipp, Eli S. Rykoff, F. Nogueira, L. Baruah, Daniel Gruen, Daniel Scolnic, Brian Nord, M. A. G. Maia, Brian Yanny, Matthias Klein, J. Song, R. R. Gupta, Yanxi Zhang, Arya Farahi, J. Carretero, M. March, Basilio X. Santiago, Tamara M. Davis, Shantanu Desai, Gary S. Da Costa, Jochen Weller, T. F. Eifler, Daniel A. Goldstein, J. M. Hislop, Joseph J. Mohr, R. C. Thomas, Erin Sheldon, David Brooks, M. E. C. Swanson, A. Porredon, A. Carnero Rosell, A. Saro, D. W. Gerdes, Xi Chen, Attila Kovács, Eric Morganson, R. C. Wolf, J. P. Dietrich, A. Kremin, T. M. C. Abbott, Richard G. McMahon, Jeremy Mould, J. D. Maloney, Jacobo Asorey, A. Benoit-Lévy, Hiranya V. Peiris, Ofer Lahav, Vinu Vikram, J. Lasker, E. J. Sanchez, B. Flaugher, S. Juneau, Risa H. Wechsler, Ricardo L. C. Ogando, Alistair R. Walker, A. A. Plazas, Ryan J. Foley, M. Carrasco Kind, W. C. Wester, Jennifer L. Marshall, D. L. Burke, Adam Amara, A. Scott, M.L. Sánchez, Jonathan Blazek, C. B. D'Andrea, Marcelle Soares-Santos, R. C. Smith, S. E. Kuhlmann, Ashley J. Ross, Robert C. Nichol, Ben Hoyle, G. Daues, M. Gower, C. J. Miller, M. D. Johnson, Wayne A. Barkhouse, Samuel Hinton, Felipe Menanteau, Kevin Reil, L. Nunes, F. Paz-Chinchón, David J. James, Tenglin Li, Scott Dodelson, Santiago Avila, Ann Elliott, Chihway Chang, T. Kacprzak, G. Tarle, Knut Olsen, R. Das, Ramon Miquel, Lyndsay Old, Juan Garcia-Bellido, E. Bertin, A. Roodman, Tommaso Giannantonio, Carlos E. Cunha, J. Poh, Pablo Fosalba, Enrique Gaztanaga, G. Gutierrez, J. DeRose, J. J. Thaler, Enrique Fernández, Will J. Percival, S. Allam, Paul M. Ricker, A. Pujol, Robert A. Gruendl, V. Scarpine, Andrew B. Pace, R. P. Rollins, K. Honscheid, Timothy A. McKay, Darren L. DePoy, G. Khullar, R. T. Li, Joe Zuntz, Alex Drlica-Wagner, R. Nikutta, Francisco J. Castander, C. Pond, Douglas L. Tucker, Don Petravick, W. G. Hartley, A. K. Vivas, R. Cawthon, Riccardo Campisano, D. A. Finley, D. Brout, Karl Glazebrook, Dragan Huterer, Peter Melchior, Elisabeth Krause, Mark Sullivan, Kyler Kuehn, V. C. Busti, P. Rooney, C. J. Conselice, Huan Lin, Marc Manera, J. Annis, Sebastian Bocquet, A. M. G. Koziol, M. L. Silveira, M. Fitzpatrick, Andrew R. Liddle, Alfredo Zenteno, O. Ballester, Steve Kent, Daniel Thomas, E. Buckley-Geer, Michael Troxel, A. K. Romer, Paul Martini, A. Fausti Neto, Keith Bechtol, C. Davis, J. Gschwend, Gary Bernstein, Hao-Yi Wu, Peter Doel, H. T. Diehl, J. De Vicente, J. P. Marriner, M. S. S. Gill, E. Suchyta, Niall MacCrann, August E. Evrard, Alexandre Refregier, Douglas N. Friedel, Albert Stebbins, M. Banerji, Joshua A. Frieman, I. Sevilla-Noarbe, J. A. Smith, T. McClintock, N. Kuropatkin, L. N. da Costa, Laia Cardiel-Sas, M. Sako, D. L. Hollowood, S. Serrano, David L. Nidever, Marcos Lima, Richard G. Kron, P. Lopez-Reyes, Filipe B. Abdalla, Bhuvnesh Jain, Matthew R. Becker, Flavia Sobreira, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), DES, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), NOAO Data Lab, Abbott, T. M. C., Abdalla, F. B., Allam, S., Amara, A., Annis, J., Asorey, J., Avila, S., Ballester, O., Banerji, M., Barkhouse, W., Baruah, L., Baumer, M., Bechtol, K., Becker, M. R., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Blazek, J., Bocquet, S., Brooks, D., Brout, Buckley-Geer, E., Burke, D. L., Busti, V., Campisano, R., Cardiel-Sas, L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, X., Conselice, C., Costa, G., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., Daues, G., Davis, T. M., Davis, C., De Vicente, J., Depoy, D. L., Derose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elliott, A. E., Evrard, A. E., Farahi, A., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fosalba, P., Friedel, D. N., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gower, M., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Hislop, J. M., Hollowood, D., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kacprzak, T., Kent, S., Khullar, G., Klein, M., Kovacs, A., Koziol, A. M. G., Krause, E., Kremin, A., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lasker, J., Li, T. S., Li, R. T., Liddle, A. R., Lima, M., Lin, H., López-Reyes, P., Maccrann, N., Maia, M. A. G., Maloney, J. D., Manera, M., March, M., Marriner, J., Marshall, J. L., Martini, P., Mcclintock, T., Mckay, T., Mcmahon, R. G., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morganson, E., Mould, J., Neilsen, E., Nichol, R. C., Nogueira, F., Nord, B., Nugent, P., Nunes, L., Ogando, R. L. C., Old, L., Pace, A. B., Palmese, A., Paz-Chinchón, F., Peiris, H. V., Percival, W. J., Petravick, D., Plazas, A. A., Poh, J., Pond, C., Porredon, A., Pujol, A., Refregier, A., Reil, K., Ricker, P. M., Rollins, R. P., Romer, A. K., Roodman, A., Rooney, P., Ross, A. J., Rykoff, E. S., Sako, M., Sanchez, M. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shipp, N., Silveira, M. L., Smith, M., Smith, R. C., Smith, J. A., Soares-Santos, M., Sobreira, F., Song, J., Stebbins, A., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Vivas, A. K., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Wu, H., Yanny, B., Zenteno, A., Zhang, Y., Zuntz, J., Des, Collaboration, Juneau, S., Fitzpatrick, M., Nikutta, R., Nidever, D., Olsen, K., Scott, A., and NOAO Data, Lab
Subjects: Astronomical Objects, catalog, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], techniques: image processing, Astrophysics, astronomical databases: miscellaneous, 01 natural sciences, law.invention, photometric [techniques], techniques: photometric, law, Observatory, Astrophysics - Cosmology and Nongalactic Astrophysic, 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics, image processing [techniques], observations [cosmology], sky survey, Astrophysics - Solar and Stellar Astrophysics, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, sextractor, Data release, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.SR, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, astro-ph.GA, FOS: Physical sciences, Astronomy & Astrophysics, miscellaneou [astronomical databases], Telescope, surveys, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, survey, Astronomical And Space Sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Physical Chemistry (Incl. Structural), 010308 nuclear & particles physics, Organic Chemistry, representations, Astronomy and Astrophysics, miscellaneous [astronomical databases], angular masks, Astrophysics - Astrophysics of Galaxies, Galaxy, Data set, catalogs, cosmology: observations, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: We describe the first public data release of the Dark Energy Survey, DES DR1, consisting of reduced single epoch images, coadded images, coadded source catalogs, and associated products and services assembled over the first three years of DES science operations. DES DR1 is based on optical/near-infrared imaging from 345 distinct nights (August 2013 to February 2016) by the Dark Energy Camera mounted on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. We release data from the DES wide-area survey covering ~5,000 sq. deg. of the southern Galactic cap in five broad photometric bands, grizY. DES DR1 has a median delivered point-spread function of g = 1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.90 arcsec FWHM, a photometric precision of < 1% in all bands, and an astrometric precision of 151 mas. The median coadded catalog depth for a 1.95" diameter aperture at S/N = 10 is g = 24.33, r = 24.08, i = 23.44, z = 22.69, and Y = 21.44 mag. DES DR1 includes nearly 400M distinct astronomical objects detected in ~10,000 coadd tiles of size 0.534 sq. deg. produced from ~39,000 individual exposures. Benchmark galaxy and stellar samples contain ~310M and ~ 80M objects, respectively, following a basic object quality selection. These data are accessible through a range of interfaces, including query web clients, image cutout servers, jupyter notebooks, and an interactive coadd image visualization tool. DES DR1 constitutes the largest photometric data set to date at the achieved depth and photometric precision., 30 pages, 20 Figures. Release page found at this url https://des.ncsa.illinois.edu/releases/dr1
Published: 2018

46. Galaxy Populations in Massive Galaxy Clusters to z=1.1: Color Distribution, Concentration, Halo Occupation Number and Red Sequence Fraction

Author: Alistair R. Walker, Marcelle Soares-Santos, J. Carretero, A. Fausti-Neto, A. Benoit-Lévy, Ofer Lahav, Peter Doel, Joseph J. Mohr, J. P. Dietrich, A. Saro, Shantanu Desai, R. L. C. Ogando, A. Carnero, G. Tarle, H. T. Diehl, Eduardo Rozo, C. Hennig, G. Gutierrez, Ramon Miquel, A. Zenteno, Nikhel Gupta, Jennifer L. Marshall, Brian Nord, R. C. Smith, I-Non Chiu, Sebastian Bocquet, V. Strazzullo, Eric H. Neilsen, K. Honscheid, B. Stalder, T. M. C. Abbott, Daniel Thomas, Daniel Gruen, M. Carrasco Kind, Michael McDonald, Yanxi Zhang, Tim Eifler, Vinu Vikram, David J. Brooks, S. A. Stanford, E. J. Sanchez, R. Capasso, Michael Schubnell, M. E. C. Swanson, David J. James, R. A. Bernstein, C. B. D'Andrea, Pablo Fosalba, Christian L. Reichardt, L. N. daCosta, Julie Hlavacek-Larrondo, Anthony H. Gonzalez, A. A. Plazas, E. Suchyta, August E. Evrard, E. Bertin, C. Gangkofner, F. B. Abdalla, Matthew B. Bayliss, Eli S. Rykoff, Diego Capozzi, A. K. Romer, Peter Melchior, Paul Martini, Flavia Sobreira, C. J. Miller, M. March, Basilio X. Santiago, Kyler Kuehn, I. Sevilla-Noarbe, N. Kuropatkin, Joshua A. Frieman, Robert A. Gruendl, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Hennig, C., Mohr, J. J., Zenteno, A., Desai, S., Dietrich, J. P., Bocquet, S., Strazzullo, V., Saro, A., Abbott, T. M. C., Abdalla, F. B., Bayliss, M., Benoit-Levy, A., Bernstein, R. A., Bertin, E., Brooks, D., Capasso, R., Capozzi, D., Carnero, A., Carrasco Kind, M., Carretero, J., Chiu, I., D'Andrea, C. B., Dacosta, L. N., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Fausti-Neto, A., Fosalba, P., Frieman, J., Gangkofner, C., Gonzalez, A., Gruen, D., Gruendl, R. A., Gupta, N., Gutierrez, G., Honscheid, K., Hlavacek-Larrondo, J., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., March, M., Marshall, J. L., Martini, P., Mcdonald, M., Melchior, P., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R., Plazas, A. A., Reichardt, C., Romer, A. K., Rozo, E., Rykoff, E. S., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Stalder, B., Stanford, S. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Walker, A. R., Zhang, Y., MIT Kavli Institute for Astrophysics and Space Research, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: galaxies: clusters: individual, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Virial theorem, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, clusters: general [galaxies], galaxies: formation, education, 010303 astronomy & astrophysics, evolution [galaxies], STFC, Galaxy cluster, luminosity function [galaxies], QB, Luminosity function (astronomy), Physics, education.field_of_study, clusters: individual [galaxies], 010308 nuclear & particles physics, RCUK, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies: luminosity function, South Pole Telescope, Space and Planetary Science, mass function, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), Baryon acoustic oscillations, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the galaxy populations in 74 Sunyaev Zeldovich Effect (SZE) selected clusters from the South Pole Telescope (SPT) survey that have been imaged in the science verification phase of the Dark Energy Survey (DES). The sample extends up to $z\sim 1.1$ with $4 \times 10^{14} M_{\odot}\le M_{200}\le 3\times 10^{15} M_{\odot}$. Using the band containing the 4000~\AA\ break and its redward neighbor, we study the color-magnitude distributions of cluster galaxies to $\sim m_*+2$, finding: (1) the intrinsic rest frame $g-r$ color width of the red sequence (RS) population is $\sim$0.03 out to $z\sim0.85$ with a preference for an increase to $\sim0.07$ at $z=1$ and (2) the prominence of the RS declines beyond $z\sim0.6$. The spatial distribution of cluster galaxies is well described by the NFW profile out to $4R_{200}$ with a concentration of $c_{\mathrm{g}} = 3.59^{+0.20}_{-0.18}$, $5.37^{+0.27}_{-0.24}$ and $1.38^{+0.21}_{-0.19}$ for the full, the RS and the blue non-RS populations, respectively, but with $\sim40$\% to 55\% cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region $N_{200}$ exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The red sequence (RS) fraction within $R_{200}$ is $(68\pm3)$\% at $z=0.46$, varies from $\sim$55\% at $z=1$ to $\sim$80\% at $z=0.1$, and exhibits intrinsic variation among clusters of $\sim14$\%. We discuss a model that suggests the observed redshift trend in RS fraction favors a transformation timescale for infalling field galaxies to become RS galaxies of 2 to 3~Gyr., Comment: 22 pages, 14 figures, submitted to MNRAS
Published: 2016

47. Dark Energy Survey Year 3 results: galaxy-halo connection from galaxy-galaxy lensing

Author: Martin Crocce, R. D. Wilkinson, Maria E. S. Pereira, Joe Zuntz, Alex Drlica-Wagner, K. Honscheid, J. Blazek, Elisabeth Krause, Scott Dodelson, Chihway Chang, Matthew R. Becker, S. Desai, F. J. Castander, T. M. C. Abbott, Marcos Lima, Antonella Palmese, C. Doux, Chun-Hao To, E. J. Sanchez, Stella Seitz, I. Tutusaus, E. Bertin, M. A. G. Maia, J. Annis, A. Alarcon, I. Ferrero, Matt J. Jarvis, Eli S. Rykoff, Peter Doel, Brian Yanny, Yanxi Zhang, P. F. Leget, Josh Frieman, David J. Brooks, W. G. Hartley, J. P. Dietrich, Juan Garcia-Bellido, Ramon Miquel, Bhuvnesh Jain, H. T. Diehl, David Bacon, A. Roodman, G. Zacharegkas, J. McCullough, M. Costanzi, E. M. Huff, R. Chen, M Gatti, Niall MacCrann, Jennifer L. Marshall, Carlos Solans Sanchez, Samuel Hinton, Michel Aguena, Adriano Pieres, C. Davis, G. Gutierrez, B. Yin, B. Flaugher, Alexandra Amon, R. P. Rollins, J. Myles, J. Gschwend, Gary Bernstein, K. Herner, A. Navarro-Alsina, Keith Bechtol, Enrique Gaztanaga, Ami Choi, Ben Hoyle, J. Carretero, G. Giannini, J. DeRose, E. Suchyta, August E. Evrard, Felipe Menanteau, David J. James, A. Carnero Rosell, S. Everett, Jack Elvin-Poole, A. Porredon, Youngsoo Park, Pablo Fosalba, Risa H. Wechsler, Daniel Thomas, Peter Melchior, R. Cawthon, Agnès Ferté, J. Cordero, D. L. Burke, D. L. Hollowood, R. L. C. Ogando, S. Serrano, A. Campos, F. Paz-Chinchón, I. Harrison, S. Allam, Robert A. Gruendl, M. Smith, Daniel Gruen, T. Shin, M. Carrasco Kind, F. Andrade-Oliveira, Marco Raveri, L. F. Secco, G. Tarle, Erin Sheldon, Ashley J. Ross, I. Sevilla-Noarbe, Kyler Kuehn, N. Kuropatkin, K. D. Eckert, T. N. Varga, L. N. da Costa, Michael Troxel, S. Pandey, J. Muir, J. Prat, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Zacharegkas, G., Chang, C., Prat, J., Pandey, S., Ferrero, I., Blazek, J., Jain, B., Crocce, M., Derose, J., Palmese, A., Seitz, S., Sheldon, E., Hartley, W. G., Wechsler, R. H., Dodelson, S., Fosalba, P., Krause, E., Park, Y., Sanchez, C., Alarcon, A., Amon, A., Bechtol, K., Becker, M. R., Bernstein, G. M., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Davis, C., Diehl, H. T., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Herner, K., Huff, E. M., Jarvis, M., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Myles, J., Navarro-Alsina, A., Porredon, A., Raveri, M., Rollins, R. P., Roodman, A., Ross, A. J., Rykoff, E. S., Secco, L. F., Sevilla-Noarbe, I., Shin, T., Troxel, M. A., Tutusaus, I., Varga, T. N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Muir, J., Ogando, R. L. C., Paz-Chinchon, F., Pieres, A., Sanchez, E., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Wilkinson, R. D., Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, National Aeronautics and Space Administration (US), University of Chicago, University of Pennsylvania, University of Oslo, Northeastern University, Observatoire de Sauverny, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Lawrence Berkeley National Laboratory, Fermi National Accelerator Laboratory, Giessenbachstrasse, Ludwig-Maximilians Universität München, Brookhaven National Laboratory, University of Geneva, Stanford University, Slac National Accelerator Laboratory, Carnegie Mellon University, University of Arizona, University of Tokyo, Argonne National Laboratory, University of Wisconsin-Madison, la Laguna, Laboratório Interinstitucional de E-Astronomia-LIneA, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, Ohio State University, University of Manchester, Santa Cruz Institute for Particle Physics, California Institute of Technology, Barcelona Institute of Science and Technology, Denys Wilkinson Building, University of Cambridge, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnológicas (CIEMAT), University of Edinburgh, Casilla, Universidade Estadual Paulista (UNESP), University of Portsmouth, Institut d'Astrophysique de Paris, University College London, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Iit Hyderabad, Ludwig-Maximilians-Universität, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, University of Sussex, and UAM. Departamento de Física Teórica
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo occupation distribution, Cosmology, matter haloes, Galactic halo, gravitational lensing: weak, dark matter [cosmology], weak [gravitational lensing], 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, large-scale structure of universe, occupation distribution, massive galaxies, model, 010308 nuclear & particles physics, 100 square degrees, Física, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, cosmology: dark matter, large-scale structure of Universe, Galaxy, Redshift, radial-distribution, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, cosmological constraints, cfhtlens, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: G. Zacharegkas et al., Galaxy–galaxy lensing is a powerful probe of the connection between galaxies and their host dark matter haloes, which is important both for galaxy evolution and cosmology. We extend the measurement and modelling of the galaxy–galaxy lensing signal in the recent Dark Energy Survey Year 3 cosmology analysis to the highly non-linear scales (∼100 kpc). This extension enables us to study the galaxy–halo connection via a Halo Occupation Distribution (HOD) framework for the two lens samples used in the cosmology analysis: a luminous red galaxy sample (REDMAGIC) and a magnitude-limited galaxy sample (MAGLIM). We find that REDMAGIC (MAGLIM) galaxies typically live in dark matter haloes of mass log10(Mh/M⊙) ≈ 13.7 which is roughly constant over redshift (13.3−13.5 depending on redshift). We constrain these masses to ∼15 per cent ⁠, approximately 1.5 times improvement over the previous work. We also constrain the linear galaxy bias more than five times better than what is inferred by the cosmological scales only. We find the satellite fraction for REDMAGIC (MAGLIM) to be ∼0.1−0.2 (0.1−0.3) with no clear trend in redshift. Our constraints on these halo properties are broadly consistent with other available estimates from previous work, large-scale constraints, and simulations. The framework built in this paper will be used for future HOD studies with other galaxy samples and extensions for cosmological analyses., CC is supported by the Henry Luce Foundation. JP is supported by DOE grant DE-SC0021429. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773,PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

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