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41 results on '"cosmology observations"'

1. Cosmological Inference from within the Peculiar Local Universe.

Author

Mohayaee, Roya, Rameez, Mohamed, and Sarkar, Subir

Subjects
*TYPE I supernovae, *N-body simulations (Astronomy), *COSMOLOGICAL constant, *ACCELERATION (Mechanics), UNIVERSE
Abstract

The existence of 'peculiar' velocities due to the formation of cosmic structure marks a point of discord between the real universe and the usually assumed Friedmann–Lemaítre–Robertson–Walker metric, which accommodates only the smooth Hubble expansion on large scales. In the standard Λ CDM model framework, Type Ia supernovae data are routinely "corrected" for the peculiar velocities of both the observer and the supernova host galaxies relative to the cosmic rest frame, in order to infer evidence for acceleration of the expansion rate from their Hubble diagram. However, observations indicate a strong, coherent local bulk flow that continues outward without decaying out to a redshift z ≳ 0.1 , contrary to the Λ CDM expectation. By querying the halo catalogue of the Dark Sky Hubble-volume N-body simulation, we find that an observer placed in an unusual environment like our local universe should see correlations between supernovae in the JLA catalogue that are 2–8 times stronger than seen by a typical or Copernican observer. This accounts for our finding that peculiar velocity corrections have a large impact on the value of the cosmological constant inferred from supernova data. We also demonstrate that local universe-like observers will infer a downward biased value of the clustering parameter S 8 from comparing the density and velocity fields. More realistic modelling of the peculiar local universe is thus essential for correctly interpreting cosmological data. [ABSTRACT FROM AUTHOR]

Published
2024
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6. Does the GRB Duration Depend on Redshift?

Author

Horvath, Istvan, Racz, Istvan I., Bagoly, Zsolt, Balázs, Lajos G., and Pinter, Sandor

Subjects
*GAMMA ray bursts, *REDSHIFT, *LARGE scale structure (Astronomy)
Abstract

Several hundred gamma-ray burst (GRB) redshifts have been determined to date. One of the other important properties—besides the distance—of the GRBs is the duration of the burst. In this paper, we analyse these two important quantities of the phenomena. In this paper, we map the two-dimensional distribution and explore some suspicious areas. As it is well known that the short GRBs are closer than the others, we search for parts in the Universe where the GRB duration is different from the others. We also analyse whether there are any ranges in the duration where the redshifts differ. We find some suspicious areas, however, no other significant region was found than the short GRB region. [ABSTRACT FROM AUTHOR]

Published
2022
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9. Constraining the baryonic feedback with cosmic shear using the DES Year-3 small-scale measurements

Author

Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Des, Collaboration

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Nuclear Theory, High Energy Physics::Phenomenology, cosmology observations, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics Cosmology and Nongalactic Astrophysics, Space and Planetary Science, gravitational lensing weak, large-scale structure of Universe, cosmology observation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package \texttt{Baccoemu} to accelerate the evaluation of the baryonic nonlinear matter power spectrum. We design our analysis pipeline to focus on the constraints of the baryonic suppression effects, utilizing the implication given by a principal component analysis on the Fisher forecasts. Our constraint on the baryonic effects can then be used to better model and ameliorate the effects of baryons in producing cosmological constraints from the next generation large-scale structure surveys. We detect the baryonic suppression on the cosmic shear measurements with a $\sim 2 \sigma$ significance. The characteristic halo mass for which half of the gas is ejected by baryonic feedback is constrained to be $M_c > 10^{13.2} h^{-1} M_{\odot}$ (95\% C.L.). The best-fit baryonic suppression is $\sim 5\%$ at $k=1.0 {\rm Mpc}\ h^{-1}$ and $\sim 15\%$ at $k=5.0 {\rm Mpc} \ h^{-1}$. Our findings are robust with respect to the assumptions about the cosmological parameters, specifics of the baryonic model, and intrinsic alignments., Comment: 20 pages, 10 figures. DES Collaboration, Year-3 analysis

Published
2022
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10. Using host galaxy spectroscopy to explore systematics in the standardization of Type Ia supernovae

Author

M Dixon, C Lidman, J Mould, L Kelsey, D Brout, A Möller, P Wiseman, M Sullivan, L Galbany, T M Davis, M Vincenzi, D Scolnic, G F Lewis, M Smith, R Kessler, A Duffy, E N Taylor, C Flynn, T M C Abbott, M Aguena, S Allam, F Andrade-Oliveira, J Annis, J Asorey, E Bertin, S Bocquet, D Brooks, D L Burke, A Carnero Rosell, D Carollo, M Carrasco Kind, J Carretero, M Costanzi, L N da Costa, M E S Pereira, P Doel, S Everett, I Ferrero, B Flaugher, D Friedel, J Frieman, J García-Bellido, M Gatti, D W Gerdes, K Glazebrook, D Gruen, J Gschwend, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D Huterer, D J James, K Kuehn, N Kuropatkin, U Malik, M March, F Menanteau, R Miquel, R Morgan, B Nichol, R L C Ogando, A Palmese, F Paz-Chinchón, A Pieres, A A Plazas Malagón, M Rodriguez-Monroy, A K Romer, E Sanchez, V Scarpine, I Sevilla-Noarbe, M Soares-Santos, E Suchyta, G Tarle, C To, B E Tucker, D L Tucker, T N Varga, Dixon, M., Lidman, C., Mould, J., Kelsey, L., Brout, D., Möller, A., Wiseman, P., Sullivan, M., Galbany, L., Davis, T. M., Vincenzi, M., Scolnic, D., Lewis, G. F., Smith, M., Kessler, R., Duffy, A., Taylor, E. N., Flynn, C., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Asorey, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gerdes, D. W., Glazebrook, K., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Kuropatkin, N., Malik, U., March, M., Menanteau, F., Miquel, R., Morgan, R., Nichol, B., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Tucker, B. E., Tucker, D. L., Varga, T. N., Australian Research Council, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Generalitat de Catalunya, European Commission, and European Research Council

Subjects
Galaxies: general, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: observations, cosmology observations, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, surveys, galaxies general, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, survey, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

M. Dixon et al., We use stacked spectra of the host galaxies of photometrically identified Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) to search for correlations between Hubble diagram residuals and the spectral properties of the host galaxies. Utilizing full spectrum fitting techniques on stacked spectra binned by Hubble residual, we find no evidence for trends between Hubble residuals and properties of the host galaxies that rely on spectral absorption features (, MD would like to acknowledge support through an Australian Government Research Training Program Scholarship. This research was supported by the Australian Research Council The Centre of Excellence for Dark Matter Particle Physics (CDM; project number CE200100008) and the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav; project number CE170100004). This project/publication was made possible through the support of a grant from the John Templeton Foundation. The authors gratefully acknowledge this grant ID 61807, Two Standard Models Meet. The opinions expressed in this publication are those of the author(s) and do not necessarily reflect the views of the John Templeton Foundation. 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 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). 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. Based on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional custodians of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present.

Published
2022
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11. Independent cosmological constraints from high-z H  ii  galaxies.

Author

González-Morán, Ana Luisa, Chávez, Ricardo, Terlevich, Roberto, Terlevich, Elena, Bresolin, Fabio, Fernández-Arenas, David, Plionis, Manolis, Basilakos, Spyros, Melnick, Jorge, and Telles, Eduardo

Subjects
*COSMIC background radiation, *GALAXIES, *TYPE I supernovae, *DARK energy, *PHYSICAL cosmology, *EQUATIONS of state
Abstract

We present new high spectral resolution observations of 15 high-z (1.3 ≤ z ≤2.5) H  ii galaxies (H  ii  G) obtained with MOSFIRE at the Keck Observatory. These data, combined with already published data for another 31 high-z and 107 z ≤0.15 H  ii  G, are used to obtain new independent cosmological results using the distance estimator based on the established correlation between the Balmer emission line velocity dispersion and luminosity for H  ii  G. Our results are in excellent agreement with the latest cosmological concordance model (ΛCDM) published results. From our analysis, we find a value for the mass density parameter of |$\Omega _m=0.290^{+0.056}_{-0.069}$| (stat). For a flat universe, we constrain the plane |$\lbrace \Omega _m;w_0\rbrace = \lbrace 0.280^{+0.130}_{-0.100} ; -1.12^{+0.58}_{-0.32}\rbrace$| (stat). The joint likelihood analysis of H  ii  G with other complementary cosmic probes (cosmic microwave background and baryon acoustic oscillations) provides tighter constraints for the parameter space of the equation of state of dark energy that are also in excellent agreement with those of similar analyses using Type Ia supernovae instead as the geometrical probe. [ABSTRACT FROM AUTHOR]

Published
2019
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12. Consistent lensing and clustering in a low-S8 Universe with BOSS, DES Year 3, HSC Year 1, and KiDS-1000

Author

A Amon, N C Robertson, H Miyatake, C Heymans, M White, J DeRose, S Yuan, R H Wechsler, T N Varga, S Bocquet, A Dvornik, S More, A J Ross, H Hoekstra, A Alarcon, M Asgari, J Blazek, A Campos, R Chen, A Choi, M Crocce, H T Diehl, C Doux, K Eckert, J Elvin-Poole, S Everett, A Ferté, M Gatti, G Giannini, D Gruen, R A Gruendl, W G Hartley, K Herner, H Hildebrandt, S Huang, E M Huff, B Joachimi, S Lee, N MacCrann, J Myles, A Navarro-Alsina, T Nishimichi, J Prat, L F Secco, I Sevilla-Noarbe, E Sheldon, T Shin, T Tröster, M A Troxel, I Tutusaus, A H Wright, B Yin, M Aguena, S Allam, J Annis, D Bacon, M Bilicki, D Brooks, D L Burke, A Carnero Rosell, J Carretero, F J Castander, R Cawthon, M Costanzi, L N da Costa, M E S Pereira, J de Jong, J De Vicente, S Desai, J P Dietrich, P Doel, I Ferrero, J Frieman, J García-Bellido, D W Gerdes, J Gschwend, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D Huterer, A Kannawadi, K Kuehn, N Kuropatkin, O Lahav, M Lima, M A G Maia, J L Marshall, F Menanteau, R Miquel, J J Mohr, R Morgan, J Muir, F Paz-Chinchón, A Pieres, A A Plazas Malagón, A Porredon, M Rodriguez-Monroy, A Roodman, E Sanchez, S Serrano, H Shan, E Suchyta, M E C Swanson, G Tarle, D Thomas, C To, Y Zhang, Amon, A., Robertson, N. C., Miyatake, H., Heymans, C., White, M., Derose, J., Yuan, S., Wechsler, R. H., Varga, T. N., Bocquet, S., Dvornik, A., More, S., Ross, A. J., Hoekstra, H., Alarcon, A., Asgari, M., Blazek, J., Campos, A., Chen, R., Choi, A., Crocce, M., Diehl, H. T., Doux, C., Eckert, K., Elvin-Poole, J., Everett, S., Ferté, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Hartley, W. G., Herner, K., Hildebrandt, H., Huang, S., Huff, E. M., Joachimi, B., Lee, S., Maccrann, N., Myles, J., Navarro-Alsina, A., Nishimichi, T., Prat, J., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Tröster, T., Troxel, M. A., Tutusaus, I., Wright, A. H., Yin, B., Aguena, M., Allam, S., Annis, J., Bacon, D., Bilicki, M., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., de Jong, J., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Frieman, J., García-Bellido, J., Gerdes, D. W., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Kannawadi, A., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Porredon, A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Serrano, S., Shan, H., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Zhang, Y.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmology observations, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, gravitational lensing weak, large-scale structure of Universe, Cosmology and Nongalactic Astrophysics, Astrophysic, Space and Planetary Science, cosmology observation, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We evaluate the consistency between lensing and clustering probes of large-scale structure based on measurements of projected galaxy clustering from BOSS combined with overlapping galaxy-galaxy lensing from three surveys: DES Y3, HSC Y1, and KiDS-1000. An intra-lensing-survey study finds good agreement between these lensing data. We model the observations using the Dark Emulator and fit the data at two fixed cosmologies: Planck, with $S_8=0.83$, and a Lensing cosmology with $S_8=0.76$. For a joint analysis limited to scales with $R>5.25h^{-1}$Mpc, we find that both cosmologies provide an acceptable fit to the data. Full utilisation of the small-scale clustering and lensing measurements is hindered by uncertainty in the impact of baryon feedback and assembly bias, which we account for with a reasoned theoretical error budget. We incorporate a systematic scaling parameter for each redshift bin, $A$, that decouples the lensing and clustering to capture any inconsistency. When a wide range of scales ($0.15, Comment: 28 pages, 11 figures

Published
2023

13. The Dark Energy Survey supernova program: cosmological biases from supernova photometric classification

Author

Vincenzi, M., Sullivan, M., Möller, A., Armstrong, P., Bassett, B. A., Brout, D., Carollo, D., Carr, A., Davis, T. M., Frohmaier, C., Galbany, L., Glazebrook, K., Graur, O., Kelsey, L., Kessler, R., Kovacs, E., Lewis, G. F., Lidman, C., Malik, U., Nichol, R. C., Popovic, B., Sako, M., Scolnic, D., Smith, M., Taylor, G., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Annis, J., Asorey, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., Des, Collaboration, Vincenzi, M., Sullivan, M., Möller, A., Armstrong, P., Bassett, B. A., Brout, D., Carollo, D., Carr, A., Davis, T. M., Frohmaier, C., Galbany, L., Glazebrook, K., Graur, O., Kelsey, L., Kessler, R., Kovacs, E., Lewis, G. F., Lidman, C., Malik, U., Nichol, R. C., Popovic, B., Sako, M., Scolnic, D., Smith, M., Taylor, G., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Annis, J., Asorey, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., Des, Collaboration, UAM. Departamento de Física Teórica, 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), and DES

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmology observations, FOS: Physical sciences, Física, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Astrophysics Cosmology and Nongalactic Astrophysics, Cosmology: Observations, Supernovae: General, surveys, supernovae general, Space and Planetary Science, survey, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology observation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Artículo escrito por un elevado número de autores, solo se referencian el que aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere, This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society Volume 518.1 (2023): 1106-1127 is available online at: https://academic.oup.com/mnras/article-abstract/518/1/1106/6601453, Cosmological analyses of samples of photometrically identified type Ia supernovae (SNe Ia) depend on understanding the effects of ‘contamination’ from core-collapse and peculiar SN Ia events. We employ a rigorous analysis using the photometric classifier SuperNNova on state-of-the-art simulations of SN samples to determine cosmological biases due to such ‘non-Ia’ contamination in the Dark Energy Survey (DES) 5-yr SN sample. Depending on the non-Ia SN models used in the SuperNNova training and testing samples, contamination ranges from 0.8 to 3.5 per cent, with a classification efficiency of 97.7–99.5 per cent. Using the Bayesian Estimation Applied to Multiple Species (BEAMS) framework and its extension BBC (‘BEAMS with Bias Correction’), we produce a redshift-binned Hubble diagram marginalized over contamination and corrected for selection effects, and use it to constrain the dark energy equation-of-state, w. Assuming a flat universe with Gaussian ΩM prior of 0.311 ± 0.010, we show that biases on w are, This work was supported by the Science and Technology Facilities Council [grant number ST/P006760/1] through the DISCnet Cen¬tre for Doctoral Training. MS acknowledges support from EU/FP7¬ERC grant 615929, and PW acknowledges support from STFC grant ST/R000506/1. TMD acknowledges support from ARC grant FL180100168. LG acknowledges financial support from the Span¬ish Ministry of Science, Innovation and Universities (MICIU) un¬der the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. RH and MS were supported by DOE grant DE-FOA-0001781 and NASA grant NNH15ZDA001N-WFIRST. The material is based upon work sup¬ported by NASA under award number 80GSFC17M0002. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. This paper has gone through internal review by the DES collab¬oration. 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 Uni¬versity of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fun¬damental Physics and Astronomy at Texas A&M University, Finan¬ciadora 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 Forschungsgemein¬schaft 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 Cam¬bridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University Col¬lege London, the DES-Brazil Consortium, the University of Edin¬burgh, 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 Uni-versity, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the Uni¬versity of Sussex, Texas A&M University, and the OzDES Member¬ship 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 Na¬tional 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 re¬sults 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 Ciên¬cia 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. De¬partment of Energy, Office of Science, Office of High Energy Physics. This work was completed in part with resources provided by the University of Chicago’s Research Computing Center. Finally, this work was based in part on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present

Published
2023
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14. Dark energy survey year 3 results: weak lensing shape catalogue

Author

Peter Doel, Alexandra Amon, Joe Zuntz, Jack Elvin-Poole, M. Smith, Daniel Gruen, V. Scarpine, J. Carretero, Tamara M. Davis, H. T. Diehl, David Bacon, Niall MacCrann, I. Tutusaus, Tesla E. Jeltema, A. Navarro-Alsina, J. De Vicente, D. W. Gerdes, J. Gschwend, Daniel Thomas, Gary Bernstein, Marcos Lima, E. M. Huff, M. Gatti, W. C. Wester, Josh Frieman, R. Chen, Michel Aguena, Samuel Hinton, G. Gutierrez, David J. Brooks, R. P. Rollins, Matthew R. Becker, J. Prat, Ami Choi, Ben Hoyle, S. Samuroff, F. Paz-Chinchón, Santiago Avila, Chihway Chang, Antonella Palmese, M. A. G. Maia, E. Bertin, M. E. C. Swanson, S. Serrano, S. Pandey, S. Desai, Michael Schubnell, J. McCullough, M. Costanzi, D. L. Burke, J. P. Dietrich, Juan Garcia-Bellido, E. Suchyta, W. G. Hartley, Carlos Solans Sanchez, Christopher J. Conselice, S. Allam, Robert A. Gruendl, Ramon Miquel, Eli S. Rykoff, Jochen Weller, F. J. Castander, Richard G. Kron, T. Shin, D. L. Hollowood, T. M. C. Abbott, Elisabeth Krause, C. Doux, Chun-Hao To, E. J. Sanchez, A. A. Plazas, I. Ferrero, Matt J. Jarvis, K. Honscheid, S. Everett, L. F. Secco, M. Carrasco Kind, Martin Crocce, R. D. Wilkinson, Sunayana Bhargava, Risa H. Wechsler, J. Myles, David J. James, Jennifer L. Marshall, Agnès Ferté, Michael Troxel, I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, Alex Drlica-Wagner, K. D. Eckert, T. N. Varga, Dragan Huterer, L. N. da Costa, Bhuvnesh Jain, J. Annis, Douglas L. Tucker, Erin Sheldon, Robert Morgan, G. Tarle, Ian Harrison, A. Roodman, Tommaso Giannantonio, A. Carnero Rosell, Gatti, M., Sheldon, E., Amon, A., Becker, M., Troxel, M., Choi, A., Doux, C., Maccrann, N., Navarro Alsina, A., Harrison, I., Gruen, D., Bernstein, G., Jarvis, M., Secco, L. F., Ferté, A., Shin, T., Mccullough, J., Rollins, R. P., Chen, R., Chang, C., Pandey, S., Tutusaus, I., Prat, J., Elvin-Poole, J., Sanchez, C., Plazas, A. A., Roodman, A., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., da Costa, L. N., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jeltema, T., Krause, E., Kron, R., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Myles, J., Palmese, A., Paz-Chinchón, F., Rykoff, E. S., Samuroff, S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Wechsler, R. H., Weller, J., Wester, W., Wilkinson, R. D., National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), 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
Effective Area, Point spread function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Techniques: image processing, FOS: Physical sciences, Astrophysics, Surveys, 01 natural sciences, surveys, weak [gravitational lensing], Gravitational lensing: weak, Methods: data analysis, 0103 physical sciences, data analysis [methods], survey, Spurious relationship, weak [ravitational lensing], 010303 astronomy & astrophysics, catalogues, Weak gravitational lensing, media_common, Physics, Energy Surveys, Number density, image processing [techniques], 010308 nuclear & particles physics, Cosmology: observations, Física, Astronomy and Astrophysics, Catalogues, Dark Energy, observations [cosmology], Galaxy, Weak Lensing, Space and Planetary Science, Sky, data analysi [methods], Dark energy, ravitational lensing: weak, Catalog, methods: data analysis, techniques: image processing, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology Observations, catalogue, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], observation [cosmology]
Abstract

Gatti, M., et al. (DES Collaboration), We present and characterize the galaxy shape catalogue from the first 3 yr of Dark Energy Survey (DES) observations, over an effective area of 4143 deg2 of the southern sky. We describe our data analysis process and our self-calibrating shear measurement pipeline metacalibration, which builds and improves upon the pipeline used in the DES Year 1 analysis in several aspects. The DES Year 3 weak-lensing shape catalogue consists of 100 204 026 galaxies, measured in the riz bands, resulting in a weighted source number density of neff = 5.59 gal arcmin-2 and corresponding shape noise σe = 0.261. We perform a battery of internal null tests on the catalogue, including tests on systematics related to the point spread function (PSF) modelling, spurious catalogue B-mode signals, catalogue contamination, and galaxy properties., 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 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 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) e-Universe (CNPq grant 465376/2014-2).

Published
2021
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15. Tracing Galaxy Evolution by Their Present-Day Luminosity Function

Author

Tempel E.

Subjects
cosmology observations, large scale structure of the universe, galaxies luminosity function, clusters, formation, Astronomy, QB1-991
Abstract

Galaxy luminosity functions are derived for different morphological types and various colors of galaxies, to trace the evolutionary effects which a priori should be different for void and supercluster galaxies. We also analyse how the galaxy group content changes in the large-scale environment. One of the principal results is the conclusion that the evolution of spiral galaxies is almost independent of the global environment. Meanwhile, the luminosity function of elliptical galaxies depends strongly on the environment. This shows that the global environmental density is an important factor in the formation of elliptical galaxies. The results of the present study clearly show that, except the local/group environment, the global (supercluster-void) environment plays an important role in the formation and evolution of galaxies.

Published
2011
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16. A galaxy-driven model of type Ia supernova luminosity variations

Author

Wiseman, P., Vincenzi, M., Sullivan, M., Kelsey, L., Popovic, B., Rose, B., Brout, D., Davis, T. M., Frohmaier, C., Galbany, L., Lidman, C., Möller, A., Scolnic, D., Smith, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., March, M., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Varga, T. N., DES Collaboration, Wiseman, P., Vincenzi, M., Sullivan, M., Kelsey, L., Popovic, B., Rose, B., Brout, D., Davis, T. M., Frohmaier, C., Galbany, L., Lidman, C., Möller, A., Scolnic, D., Smith, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., March, M., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Varga, T. N., Des, Collaboration, Science and Technology Facilities Council (UK), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Consejo Superior de Investigaciones Científicas (España), European Research Council, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), and Generalitat de Catalunya

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), supernovae general, dust, extinction, galaxies evolution, cosmology observations, Cosmology: observations, Supernovae: general, Galaxies: evolution, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DES Collaboration: P. Wiseman et al., Type Ia supernovae (SNe Ia) are used as standardizable candles to measure cosmological distances, but differences remain in their corrected luminosities which display a magnitude step as a function of host galaxy properties such as stellar mass and rest-frame U−R colour. Identifying the cause of these steps is key to cosmological analyses and provides insight into SN physics. Here we investigate the effects of SN progenitor ages on their light-curve properties using a galaxy-based forward model that we compare to the Dark Energy Survey 5-yr SN Ia sample. We trace SN Ia progenitors through time and draw their light-curve width parameters from a bimodal distribution according to their age. We find that an intrinsic luminosity difference between SNe of different ages cannot explain the observed trend between step size and SN colour. The data split by stellar mass are better reproduced by following recent work implementing a step in total-to-selective dust extinction ratio (RV) between low- and high-mass hosts, although an additional intrinsic luminosity step is still required to explain the data split by host galaxy U−R. Modelling the RV step as a function of galaxy age provides a better match overall. Additional age versus luminosity steps marginally improve the match to the data, although most of the step is absorbed by the width versus luminosity coefficient α. Furthermore, we find no evidence that α varies with SN age., P.W. acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. MS acknowledges support from EU/FP7-ERC grant 615929. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Social Fund (ESF) ‘Investing in your future’ under the 2019 Ramón y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement number 759194 - USNAC). 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 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). 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

17. The mass and galaxy distribution around SZ-selected clusters

Author

Edward J. Wollack, S. Goldstein, Erin S. Sheldon, Jochen Weller, L. N. da Costa, J. Elvin-Poole, Suzanne T. Staggs, Simone Ferraro, Marco Raveri, Mark J. Devlin, J. P. Dietrich, Sahar S. Allam, T. N. Varga, David Brooks, S. Pandey, M. Lokken, Brian Yanny, Maria E. S. Pereira, A. Amsellem, J. DeRose, Maria Salatino, J. McCullough, M. E. C. Swanson, M. Costanzi, C. Doux, Chun-Hao To, Cristóbal Sifón, E. J. Sanchez, Joseph J. Mohr, I. Tutusaus, I. Sevilla-Noarbe, Gary Bernstein, B. Partridge, John P. Hughes, Carlos Solans Sanchez, G. Tarle, Scott Dodelson, Chihway Chang, V. Scarpine, Keith Bechtol, Ian Harrison, Enrique Gaztanaga, B. Flaugher, Peter Doel, Nick Battaglia, Alex Drlica-Wagner, J. Myles, David J. James, N. P. Kuropatkin, H. T. Diehl, David Bacon, Kavilan Moodley, Niall MacCrann, T. M. C. Abbott, David H. Weinberg, Kyler Kuehn, M. Gatti, J. Prat, Adriano Pieres, Samuel Hinton, Bhuvnesh Jain, K. Eckert, J. De Vicente, T. Dacunha, Marcelle Soares-Santos, E. Suchyta, E. J. Baxter, D. Gruen, A. Carnero Rosell, J. Carretero, Matt Hilton, M. Belyakov, Michael Troxel, J. C. Hill, F. Paz-Chinchón, A. Alarcon, Richard P. Rollins, Antonio Campos, Ramon Miquel, S. Desai, Federico Nati, Michael D. Niemack, Sebastian Bocquet, M. Smith, M. Aguena, A. K. Romer, Daniel Thomas, E. Buckley-Geer, L. A. Page, Emmanuel Bertin, Antonella Palmese, Andrés N. Salcedo, Jeff McMahon, Agnès Ferté, Blake D. Sherwin, M. A. G. Maia, D. W. Gerdes, Ofer Lahav, I. Ferrero, Mathew S. Madhavacheril, Robert Morgan, M. Rodriguez-Monroy, Yanxi Zhang, A. A. Plazas Malagón, Andrey V. Kravtsov, S. Everett, Marco A. P. Lima, S. Adhikari, Patricio A. Gallardo, Matthew R. Becker, Basilio X. Santiago, D. L. Burke, J. Frieman, J. R. Bond, Robert A. Gruendl, M. Carrasco Kind, F. Andrade-Oliveira, Tesla E. Jeltema, Ricardo L. C. Ogando, M. Jarvis, R. Chen, Ami Choi, Elisabeth Krause, Peter Melchior, Eli S. Rykoff, Eve M. Vavagiakis, G. Gutierrez, A. Navarro-Alsina, Santiago Serrano, B. Yin, Alexandra Amon, Felipe Menanteau, James Annis, Brian J. Koopman, L. F. Secco, W. G. Hartley, Alessandro Schillaci, Devon L. Hollowood, T. Shin, University of Pennsylvania, University of Chicago, University of Hawaii, The Ohio State University, Cornell University, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians-Universität, NSF’s National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), Laboratório Interinstitucional de e-Astronomia – LIneA, Argonne National Laboratory, Fermi National Accelerator Laboratory, Stanford University, Universidade Estadual Paulista (UNESP), University of Portsmouth, University of Wisconsin-Madison, Institut d’Astrophysique de Paris, University of Toronto, University College London, Carnegie Mellon University, Duke University, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Lawrence Berkeley National Laboratory, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, California Institute of Technology, Institut d’Estudis Espacials de Catalunya (IEEC), CSIC), University of Michigan, SLAC National Accelerator Laboratory, Denys Wilkinson Building, University of Manchester, University of Geneva, Columbia University, Flatiron Institute, Westville Campus, University of Queensland, The State University of New Jersey, Center for Astrophysics | Harvard & Smithsonian, Yale University, University of Arizona, Macquarie University, Lowell Observatory, Dunlap Institute of Astronomy & Astrophysics, University of Cambridge, Perimeter Institute for Theoretical Physics, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Milano-Bicocca, Universidade Estadual de Campinas (UNICAMP), Princeton University, Haverford College, University of Sussex, UFRGS, Brookhaven National Laboratory, Pontificia Universidad Católica de Valparaíso, University of Southampton, Oak Ridge National Laboratory, NASA/Goddard Space Flight Center, Shin, T, Jain, B, Adhikari, S, Baxter, E, Chang, C, Pandey, S, Salcedo, A, Weinberg, D, Amsellem, A, Battaglia, N, Belyakov, M, Dacunha, T, Goldstein, S, Kravtsov, A, Varga, T, Abbott, T, Aguena, M, Alarcon, A, Allam, S, Amon, A, Andrade-Oliveira, F, Annis, J, Bacon, D, Bechtol, K, Becker, M, Bernstein, G, Bertin, E, Bocquet, S, Bond, J, Brooks, D, Buckley-Geer, E, Burke, D, Campos, A, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chen, R, Choi, A, Costanzi, M, da Costa, L, Derose, J, Desai, S, de Vicente, J, Devlin, M, Diehl, H, Dietrich, J, Dodelson, S, Doel, P, Doux, C, Drlica-Wagner, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferraro, S, Ferrero, I, Ferte, A, Flaugher, B, Frieman, J, Gallardo, P, Gatti, M, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Harrison, I, Hartley, W, Hill, J, Hilton, M, Hinton, S, Hollowood, D, Hughes, J, James, D, Jarvis, M, Jeltema, T, Koopman, B, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Lokken, M, Maccrann, N, Madhavacheril, M, Maia, M, Mccullough, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Myles, J, Nati, F, Navarro-Alsina, A, Niemack, M, Ogando, R, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Pereira, M, Pieres, A, Plazas Malagon, A, Prat, J, Raveri, M, Rodriguez-Monroy, M, Rollins, R, Romer, A, Rykoff, E, Salatino, M, Sanchez, C, Sanchez, E, Santiago, B, Scarpine, V, Schillaci, A, Secco, L, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Sherwin, B, Sifon, C, Smith, M, Soares-Santos, M, Staggs, S, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Troxel, M, Tutusaus, I, Vavagiakis, E, Weller, J, Wollack, E, Yanny, B, Yin, B, Zhang, Y, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Univ Penn, Univ Chicago, Univ Hawaii, Ohio State Univ, Cornell Univ, Max Planck Inst Extraterr Phys, Ludwig Maximilians Univ Munchen, NSFs Natl Opt Infrared Astron Res Lab, Lab Interinst E Astron LIneA, Argonne Natl Lab, Fermilab Natl Accelerator Lab, Stanford Univ, Univ Portsmouth, Univ Wisconsin, Inst Astrophys Paris, Sorbonne Univ, Univ Toronto, UCL, Carnegie Mellon Univ, Duke Univ, Inst Astrofis Canarias, Univ La Laguna, Natl Ctr Supercomp Applicat, Univ Illinois, Barcelona Inst Sci & Technol, Lawrence Berkeley Natl Lab, Univ Trieste, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Observ Nacl, Ctr Invest Energet Medioambientales & Tecnol CIEM, Santa Cruz Inst Particle Phys, Univ Oslo, CALTECH, Inst Estudis Espacials Catalunya IEEC, CSIC, Univ Michigan, SLAC Natl Accelerator Lab, Univ Oxford, Univ Manchester, Univ Geneva, Columbia Univ, Flatiron Inst, Univ KwaZulu Natal, Univ Queensland, Rutgers State Univ, Ctr Astrophys Harvard & Smithsonian, Yale Univ, Univ Arizona, Macquarie Univ, Lowell Observ, Dunlap Inst Astron & Astrophys, Univ Cambridge, Perimeter Inst Theoret Phys, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Univ Milano Bicocca, Haverford Coll, Univ Sussex, Univ Fed Rio Grande do Sul, Brookhaven Natl Lab, Pontificia Univ Catolica Valparaiso, Univ Southampton, Oak Ridge Natl Lab, NASA, Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., Derose, J., Desai, S., de Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferte, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., Maccrann, N., Madhavacheril, M. S., Maia, M. A. G., Mccullough, J., Mcmahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchon, F., Pereira, M. E. S., Pieres, A., Plazas Malagon, A. A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sanchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifon, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., and Zhang, Y.

Subjects
Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmology: observation, Cosmology, Galaxies clusters general, observations [Cosmology], Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Cosmology observation, Physics, Cosmology: observations, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Cosmology observations, Galaxies evolution, Galaxy, Redshift, Galaxies: clusters: general, Space and Planetary Science, Atacama Cosmology Telescope, Dark energy, Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Shin, T., et al., We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev–Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 data set. With signal-to-noise ratio of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2–20 h Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: (1) The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. (2) The full mass profile is also consistent with the simulations. (3) The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift, and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology, and astrophysics are discussed., 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 no. 465376/2014-2).

Published
2021

18. The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Large-scale structure catalogs for cosmological analysis

Author

Axel de la Macorra, Eric Jullo, Jeremy L. Tinker, J. N. McLane, Faizan G. Mohammad, Aurelio Carnero Rosell, Sylvain de la Torre, Hélion du Mas des Bourboux, Arnaud de Mattia, Peter Doohyun Choi, V. Ruhlmann-Kleider, Stephanie Escoffier, Hui Kong, S. Fromenteau, Stephen Bailey, Hee-Jong Seo, Solène Chabanier, Eva-Maria Mueller, Alex Smith, Jean-Paul Kneib, Joel R. Brownstein, Gong-Bo Zhao, Richard Neveux, Jonathan Brinkmann, Irene Cruz-González, Alexandra N. Higley, Kyle S. Dawson, Yucheng Zhang, Chia-Hsun Chuang, Andrea Muñoz-Gutiérrez, John Moustakas, Etienne Burtin, Johan Comparat, Will J. Percival, Christian Nitschelm, Shadab Alam, Donald P. Schneider, Graziano Rossi, Julian E. Bautista, Nathalie Palanque-Delabrouille, Anthony R. Pullen, Cheng Zhao, Adam D. Myers, Pauline Zarrouk, Jiamin Hou, Romain Paviot, Mehdi Rezaie, Jeffrey A. Newman, Ashley J. Ross, M. Vivek, Rita Tojeiro, Mariana Vargas Magaña, Brad W. Lyke, Anand Raichoor, Héctor Gil-Marín, Dmitry Bizyaev, Center for Cosmology & AstroParticle Physics, Ohio State University [Columbus] (OSU), Institute of Cosmology and Gravitation [Portsmouth] (ICG), University of Portsmouth, University of St Andrews [Scotland], Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, University of Utah, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Institute for Space Studies of Catalonia [Barcelona] (IEEC-CSIC), Department of Physics and Astronomy [Laramie], University of Wyoming (UW), Department of Physics and Astronomy [Waterloo], University of Waterloo [Waterloo], Siena College [Loudonville], Department of Physics [Oxford], University of Oxford, Perimeter Institute for Theoretical Physics [Waterloo], Ecole Polytechnique Fédérale de Lausanne (EPFL), Ohio University - Athens (OU), Physics & Astronomy Department [Ohio University], Department of Physics [New York], New York University [New York] (NYU), NYU System (NYU)-NYU System (NYU), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), New Mexico State University, Centro de Investigaciones Energéticas Medioambientales y Tecnológicas [Madrid] (CIEMAT), Sejong University, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Instituto de Ciencias Físicas, Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Centro de Astronomia [Antofagasta] (CITEVA), Universidad de Antofagasta, Center for Computational Astrophysics [New York], Flatiron Institute, Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Indian Institute of Astrophysics (IIA), ANR-16-CE31-0021,eBOSS,Sondes cosmologiques de la gravitation et de l'énergie noire(2016), ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project: 670193,H2020,ERC-2014-ADG,COSFORM(2015), University of Oxford [Oxford], Universidad Nacional Autónoma de México (UNAM), University of St Andrews. School of Physics and Astronomy, Alfred P. Sloan Foundation, Department of Energy (US), European Commission, Centre National de la Recherche Scientifique (France), and National Research Foundation of Korea

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), reconstruction, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, spiders, galaxies, emission, 0103 physical sciences, QB Astronomy, observations [Cosmology], 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, catalogues, power-spectrum analysis, QB, media_common, Physics, 010308 nuclear & particles physics, Oscillation, Null (mathematics), Astrophysics::Instrumentation and Methods for Astrophysics, Sampling (statistics), DAS, Astronomy and Astrophysics, Quasar, acoustic-oscillations, calibration, Catalogues, Galaxy, Redshift, Baryon, QC Physics, 13. Climate action, Space and Planetary Science, Sky, cosmology: observations, digital sky survey, Cosmology Observations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present large-scale structure catalogs from the completed extended Baryon Oscillation Spectroscopic Survey (eBOSS). Derived from Sloan Digital Sky Survey (SDSS) -IV Data Release 16 (DR16), these catalogs provide the data samples, corrected for observational systematics, and random positions sampling the survey selection function. Combined, they allow large-scale clustering measurements suitable for testing cosmological models. We describe the methods used to create these catalogs for the eBOSS DR16 Luminous Red Galaxy (LRG) and Quasar samples. The quasar catalog contains 343,708 redshifts with $0.8 < z < 2.2$ over 4,808\,deg$^2$. We combine 174,816 eBOSS LRG redshifts over 4,242\,deg$^2$ in the redshift interval $0.6 < z < 1.0$ with SDSS-III BOSS LRGs in the same redshift range to produce a combined sample of 377,458 galaxy redshifts distributed over 9,493\,deg$^2$. Improved algorithms for estimating redshifts allow that 98 per cent of LRG observations result in a successful redshift, with less than one per cent catastrophic failures ($��z > 1000$ ${\rm km~s}^{-1}$). For quasars, these rates are 95 and 2 per cent (with $��z > 3000$ ${\rm km~s}^{-1}$). We apply corrections for trends between the number densities of our samples and the properties of the imaging and spectroscopic data. For example, the quasar catalog obtains a $��^2$/DoF$= 776/10$ for a null test against imaging depth before corrections and a $��^2$/DoF$=6/8$ after. The catalogs, combined with careful consideration of the details of their construction found here-in, allow companion papers to present cosmological results with negligible impact from observational systematic uncertainties., Matches version accepted by MNRAS, very minor changes. A summary of all SDSS BAO and RSD measurements with accompanying legacy figures can be found here: https://www.sdss.org/science/final-bao-and-rsd-measurements/ . The full cosmological interpretation of these measurements can be found here: https://sdss.org/science/cosmology-results-from-eboss/

Published
2020
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19. MODELING TIME-VARYING DARK ENERGY WITH CONSTRAINTS FROM LATEST OBSERVATIONS.

Author

ZHANG, QING-JUN and WU, YUE-LIANG

Subjects
*DARK energy, *EQUATIONS of state, *TIME-varying systems, *REDSHIFT, *VARIATIONAL principles, *METAPHYSICAL cosmology, *SCIENTIFIC observation
Abstract

We introduce a set of two-parameter models for the dark energy equation of state (EOS) w(z) to investigate time-varying dark energy. The models are classified into two types according to their boundary behaviors at the redshift z = (0, ∞) and their local extremum properties. A joint analysis based on four observations (SNe + BAO + CMB + H0) is carried out to constrain all the models. It is shown that all models get almost the same $\chi^2_{\min}\simeq 469$ and the cosmological parameters (ΩM, h, Ωbh2) with the best-fit results (0.28, 0.70, 2.24), although the constraint results on two parameters (w0, w1) and the allowed regions for the EOS w(z) are sensitive to different models and a given extra model parameter. For three of Type I models which have similar functional behaviors with the so-called CPL model, the constrained two parameters w0 and w1 have negative correlation and are compatible with the ones in CPL model, and the allowed regions of w(z) get a narrow node at z~0.2. The best-fit results from the most stringent constraints in Model Ia give $(w_0, w_1) = (-0.96^{+0.26}_{-0.21}, -0.12^{+0.61}_{-0.89})$ which may compare with the best-fit results $(w_0, w_1) = (-0.97^{+0.22}_{-0.18}, -0.15^{+0.85}_{-1.33})$ in the CPL model. For four of Type II models which have logarithmic function forms and an extremum point, the allowed regions of w(z) are found to be sensitive to different models and a given extra parameter. It is interesting to obtain two models in which two parameters w0 and w1 are strongly correlative and appropriately reduced to one parameter by a linear relation w1∝(1+w0). [ABSTRACT FROM AUTHOR]

Published
2012
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20. THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS.

Author

Barbary, K., Aldering, G., Amanullah, R., Brodwin, M., Connolly, N., Dawson, K. S., Doi, M., Eisenhardt, P., Faccioli, L., Fadeyev, V., Fakhouri, H. K., Fruchter, A. S., Gilbank, D. G., Gladders, M. D., Goldhaber, G., Goobar, A., Hattori, T., Hsiao, E., Huang, X., and Ihara, Y.

Subjects
*TYPE I supernovae, *REDSHIFT, *STAR clusters, *WHITE dwarf stars
Abstract

We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < ɀ < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected ɀ > 0.9 SNe. Finding 8 ± 1 cluster SNe Ia, we determine an SN Ia rate of 0.50 Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. (stat) Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. (sys) Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. SNuB (SNUB ≡ 10-12 SNe Lʘ-1 yr-1). In units of stellar mass, this translates to. 0.13 Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. (stat) Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. (sys) Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. SNuM (SNuM ≡ 10-12 SNe Mʘ-1 yr-1 ). This represents a factor of ≈5 ± 2 increase over measurements of the cluster rate at ɀ < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: ψ (t) t Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. 5 Under the approximation of a single-burst cluster formation redshift of ɀf = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = - 1.41 Due to image rights restrictions, multiple line equation(s) cannot be graphically displayed. consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the "double degenerate" scenario and inconsistent with some models for the "single degenerate" scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts. [ABSTRACT FROM AUTHOR]

Published
2012
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21. Limitations of Bayesian Evidence applied to cosmology.

Author

Efstathiou, G.

Subjects
*METAPHYSICAL cosmology, *BAYESIAN analysis, *PARAMETER estimation, *DARK energy, *ASTRONOMY, *STATISTICAL physics
Abstract

There has been increasing interest by cosmologists in applying Bayesian techniques, such as Bayesian Evidence, for model selection. A typical example is in assessing whether observational data favour a cosmological constant over evolving dark energy. In this paper, the example of dark energy is used to illustrate limitations in the application of Bayesian Evidence associated with subjective judgements concerning the choice of model and priors. An analysis of recent cosmological data shows a statistically insignificant preference for a cosmological constant over simple dynamical models of dark energy. It is argued that for nested problems, as considered here, Bayesian parameter estimation can be more informative than computing Bayesian Evidence for poorly motivated physical models. [ABSTRACT FROM AUTHOR]

Published
2008
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22. The completed SDSS-IV extended baryon oscillation spectroscopic survey: geometry and growth from the anisotropic void–galaxy correlation function in the luminous red galaxy sample

Author

Stephanie Escoffier, Kyle S. Dawson, Alex Woodfinden, J. Rich, Mariana Vargas Magaña, J. Bautista, Ashley J. Ross, Seshadri Nadathur, Graziano Rossi, Marie Aubert, Will J. Percival, Joel R. Brownstein, S. Fromenteau, Donald P. Schneider, Héctor Gil-Marín, Agence Nationale de la Recherche (France), National Research Foundation of Korea, Ministry of Education, Science and Technology (South Korea), Sejong University, Institute of Cosmology and Gravitation [Portsmouth] (ICG), University of Portsmouth, Department of Physics and Astronomy [Waterloo], University of Waterloo [Waterloo], Perimeter Institute for Theoretical Physics [Waterloo], Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Utah, Instituto de Ciencias Físicas, Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Institute for Space Studies of Catalonia [Barcelona] (IEEC-CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Center for Cosmology & AstroParticle Physics, Ohio State University [Columbus] (OSU), Instituto de Matematicas (UNAM), Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Institute for Gravitation and the Cosmos [PennState], ANR-16-CE31-0021,eBOSS,Sondes cosmologiques de la gravitation et de l'énergie noire(2016), ANR-11-LABX-0060,OCEVU,Origines, Constituants et EVolution de l'Univers(2011), and Universidad Nacional Autónoma de México (UNAM)

Subjects
Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Cosmological parameters, FOS: Physical sciences, Large scale structure of Universe, Large-scale structure of universe, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (astronomy), Parameter space, 01 natural sciences, observations [Cosmological], 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Oscillation, Cosmological: observations, Astronomy and Astrophysics, Cosmology observations, Galaxy, Redshift, Baryon, Space and Planetary Science, Sky, astro-ph.CO, Multipole expansion, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an analysis of the anisotropic redshift-space void–galaxy correlation in configuration space using the Sloan Digital Sky Survey extended Baryon Oscillation Spectroscopic Survey (eBOSS) Data Release 16 luminous red galaxy (LRG) sample. This sample consists of LRGs between redshifts 0.6 and 1.0, combined with the high redshift z > 0.6 tail of the Baryon Oscillation Spectroscopic Survey Data Release 12 CMASS sample. We use a reconstruction method to undo redshift-space distortion (RSD) effects from the galaxy field before applying a watershed void-finding algorithm to remove bias from the void selection. We then perform a joint fit to the multipole moments of the correlation function for the growth rate fσ8 and the geometrical distance ratio DM/DH, finding fσ8(zeff)=0.356±0.079 and DM/DH(zeff)=0.868±0.017 at the effective redshift zeff=0.69 of the sample. The posterior parameter degeneracies are orthogonal to those from galaxy clustering analyses applied to the same data, and the constraint achieved on DM/DH is significantly tighter. In combination with the consensus galaxy BAO and full-shape analyses of the same sample, we obtain fσ8 = 0.447 ± 0.039, DM/rd = 17.48 ± 0.23, and DH/rd = 20.10 ± 0.34. These values are in good agreement with the ΛCDM model predictions and represent reductions in the uncertainties of 13 per cent⁠, 23 per cent⁠, and 28 per cent⁠, respectively, compared to the combined results from galaxy clustering, or an overall reduction of 55 per cent in the allowed volume of parameter space., MA and SE acknowledge support from the French National Research Agency by the eBOSS ANR grant (ANR-16-CE31-0021) and the OCEVU Labex (ANR-11-LABX-0060). GR acknowledges support from the National Research Foundation of Korea (NRF) through Grants No. 2017R1E1A1A01077508 and No. 2020R1A2C1005655 funded by the Korean Ministry of Education, Science and Technology (MoEST), and from the faculty research fund of Sejong University.

Published
2020
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23. Systematic effects induced by half-wave plate precession into measurements of the cosmic microwave background polarization

Author

F. Piacentini, Giuseppe D'Alessandro, L. Mele, L. Pagano, F. Columbro, Silvia Masi, P. de Bernardis, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Istituto Nazionale di Fisica Nucleare [Ferrara] (INFN), and Istituto Nazionale di Fisica Nucleare (INFN)

Subjects
cosmological model, dimension: 3, Cosmic microwave background, satellite, Cosmic background radiation, cosmic background radiation: polarization, Astrophysics, Cosmology -Polarization -Half Wave Plate -Instrument systematics, cosmic background radiation, 01 natural sciences, rotation, NO, 010309 optics, symbols.namesake, polarimeters, cosmology observations, polarimetric, Observational cosmology, precession, 0103 physical sciences, Stokes parameters, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, 010303 astronomy & astrophysics, Physics, beam: polarization, Linear polarization, instrumentation: polarimeters, Astronomy and Astrophysics, Polarimeter, Moment of inertia, Polarization (waves), sensitivity, Cosmology: observations, Instrumentation: polarimeters, Techniques: polarimetric, Computational physics, electric field, modulation, techniques: polarimetric, B-mode, Space and Planetary Science, cosmology: observations, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Context. The primordial B-mode signal in the cosmic microwave background (CMB) represents the smoking gun of cosmic inflation, and measuring it is the main goal of current experimental effort. The most accessible method for measuring polarization features of the CMB radiation is a Stokes polarimeter based on the rotation of a half-wave plate (HWP). Aims. Current observational cosmology is starting to be limited by systematic effects. A Stokes polarimeter with a rotating HWP has the advantage of mitigating a long list of potential systematics by modulating the linearly polarized component of the radiation, but the rotating HWP itself may introduce new systematic effects that must be under control. This represents one of the most critical parts in the design of a B-mode experiment. It is therefore mandatory to take all the systematic effects into account that the instrumentation can induce. We here present, simulate, and analyze the spurious signal arising from the precession of a rotating HWP. Methods. We first derived an analytical formula to describe the systematic effect that is induced by the HWP precession on the propagating radiation, using the 3D generalization of the Müller formalism. We then performed several numerical simulations that show the effect induced on the Stokes parameters by this systematic. We also derived and discuss the effect on B-modes as measured by a satellite experiment. Results. We derive the analytical formula for the Stokes parameters from a Stokes polarimeter where the HWP follows a precessional motion with an angle θ0. We show the result depending on the HWP inertia tensor, spinning speed, and on θ0. The result of numerical simulations is reported as a simple time-line of the electric fields. Finally, assuming that the entire sky is observed with a satellite mission, we analyze the effect on B-mode measurements. Conclusions. The effect is not negligible at the sensitivity of current B-mode experiments, therefore this systematic needs to be carefully considered for future experiments.

Published
2019
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24. Probing Cosmology with the homogeneity scale of the Universe through large scale structure surveys

Author

Ntelis, Pierros, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, CNRS, Paris Diderot University, Astroparticule and Cosmology Group, Physics Department, Paris Diderot University, Jean-Christophe Hamilton(hamilton@APC.UNIV-PARIS7.FR), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Ntelis, Pierros

Subjects
[SDU] Sciences of the Universe [physics], [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmologie observationnelles, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmology Observations, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract

This thesis exposes my contribution to the measurement of homogeneity scale using galaxies, with the cosmological interpretation of results.In physics, any model is characterized by a set of principles. Most models in cosmology are based on the Cosmological Principle, which states that the universe is statistically homogeneous and isotropic on a large scales. Today, this principle is considered to be true since it is respected by those cosmological models that accurately describe the observations. However, while the isotropy of the universe is now confirmed by many experiments, it is not the case for the homogeneity. To study cosmic homogeneity, we propose to not only test a model but to test directly one of the postulates of modern cosmology. Since 1998 the measurements of cosmic distances using type Ia supernovae, we know that the universe is now in a phase of accelerated expansion. This phenomenon can be explained by the addition of an unknown energy component, which is called dark energy. Since dark energy is responsible for the expansion of the universe, we can study this mysterious fluid by measuring the rate of expansion of the universe. The universe has imprinted in its matter distribution a standard ruler, the Baryon Acoustic Oscillation (BAO) scale. By measuring this scale at different times during the evolution of our universe, it is then possible to measure the rate of expansion of the universe and thus characterize this dark energy. Alternatively, we can use the homogeneity scale to study this dark energy. Studying the homogeneity and the BAO scale requires the statistical study of the matter distribution of the universe at large scales, superior to tens of Megaparsecs. Galaxies and quasars are formed in the vast overdensities of matter and they are very luminous: these sources trace the distribution of matter. By measuring the emission spectra of these sources using large spectroscopic surveys, such as BOSS and eBOSS, we can measure their positions. It is thus possible to reconstruct the distribution of matter in 3 dimensions in gigantic volumes. We can then extract various statistical observables to measure the BAO scale and the scale of homogeneity of the universe. Using Data Release 12 CMASS galaxy catalogs, we obtained precision on the homogeneity scale reduced by 5 times compared to WiggleZ measurement.At large scales, the universe is remarkably well described in linear order by the ΛCDM-model, the standard model of cosmology. In general, it is not necessary to take into account the nonlinear effects which complicate the model at small scales. On the other hand, at large scales, the measurement of our observables becomes very sensitive to the systematic effects. This is particularly true for the analysis of cosmic homogeneity, which requires an observational method so as not to bias the measurement. In order to study the homogeneity principle in a model independent way, we explore a new way to infer distances using cosmic clocks and type Ia SuperNovae. This establishes the Cosmological Principle using only a small number of a priori assumption, i.e. the theory of General Relativity and astrophysical assumptions that are independent from Friedmann Universes and in extend the homogeneity assumption.This manuscript is as follows. After a short presentation of the knowledge in cosmology necessary for the understanding of this manuscript, presented in Chapter 1, Chapter 2 will deal with the challenges of the Cosmological Principle as well as how to overcome those. In Chapter 3, we will discuss the technical characteristics of the large scale structure surveys, in particular focusing on BOSS and eBOSS galaxy surveys. Chapter 4 presents the detailed analysis of the measurement of cosmic homogeneity and the various systematic effects likely to impact our observables. Chapter 5 will discuss how to use the cosmic homogeneity as a standard ruler to constrain dark energy models from current and future surveys. In Chapter 6, we present our results on the determination of the homogeneity of the universe model independently. Finally in chapter 7, we draw our conclusions., Cette th\`ese pr\'esente ma contribution \`a la mesure de l'\'echelle d'homog\'en\'eit\'e \`a l'aide de galaxies, avec l'interpr\'etation cosmologique des r\`esultats.En physique, tout mod\`ele est constitu\'e par un ensemble de principes. La plupart des mod\`eles de cosmologie sont bas\'es sur le principe cosmologique, qui indique que l'univers est statistiquement homog\`ene et isotrope \`a grande \'echelle. Aujourd'hui, ce principe est consid\'er\'e comme vrai car il est respect\'e par ces mod\`eles cosmologiques qui d\'ecrivent avec pr\'ecision les observations. Cependant, l'isotropie de l'univers est maintenant confirm\'ee par de nombreuses exp\'eriences, mais ce n'est pas le cas pour l'homog\'en\'eit\'e. Pour \'etudier l'homog\'en\'eit\'e cosmique, nous proposons un postulat d'homog\'en\'eit\'e cosmique.Depuis 1998, les mesures des distances cosmiques \`a l'aide de supernovae de type Ia, nous savons que l'univers est maintenant en phase d'expansion acc\'el\'er\'ee. Ce ph\'enom\`ene s'explique par l'ajout d'une composante \'energ\'etique inconnue, appel\'ee \'energie sombre. Puisque l'\'energie noire est responsable de l'expansion de l'univers, nous pouvons \'etudier ce fluide myst\'erieux en mesurant le taux d'expansion de l'univers. L'\'echelle d'oscillation acoustique Baryon (BAO). En mesurant cette \'echelle \`a diff\'erents moments de la vie de notre univers, il est alors possible de mesurer le taux d'expansion de l'univers et donc de caract\'eriser cette \'energie sombre. Alternativement, nous pouvons utiliser l'\'echelle d'homog\'en\'eit\'e pour \'etudier cette \'energie sombre.L'\'etude l'echelle de l'homog\'en\'eit\'e et l'\'echelle BAO reclament l\`etude statistique de la regroupement de la mati\`ere de l'univers \`a grandes \'echelles, sup\'erieure \`a plusieurs dizaines de Megaparsecs. Les galaxies et les quasars sont form\'es dans les vastes surdensit\'es de la mati\`ere et ils sont tr\`es lumineuses: ces sources tracent la distribution de la mati\`ere. En mesurant les spectres d'\'emission de ces sources en utilisant de larges \'etudes spectroscopiques, telles que BOSS et eBOSS, nous pouvons mesurer leurs positions. Il est possible de reconstruire la distribution de la mati\`ere en trois dimensions en volumes gigantesques. Nous pouvons ensuite extraire divers observables statistiques pour mesurer l'\'echelle BAO et l'\'echelle d'homog\'en\'eit\'e de l'univers. En utilisant les catalogues de diffusion de donn\'ees 12 de la version 12 de donn\'ees, nous avons obtenu une pr\'ecision sur l'\'echelle d'homog\'en\'eit\'e r\'eduite de $5$ par rapport la mesure de WiggleZ.\`A grande \'echelle, l'univers est remarquablement bien d\'ecrit en ordre lin\'eaire selon le mod\`ele $ \ LCDM $, le mod\'ele standard de la cosmologie. En g\'en\'eral, il n'est pas n\'ecessaire de prendre en compte les effets non lin\'eaires qui compliquent le mod\`ele \`a petites \'echelles. D'autre part, \`a grande \'echelle, la mesure de nos observables devient tr\`es sensible aux effets syst\'ematiques. Ceci est particuli\`erement vrai pour l'analyse de l'homog\'en\'eit\'e cosmique, qui n\'ecessite une m\`ethode d'observation.Afin d'\'etudier le principe d'homog\'en\'eit\'e d'une mani\`ere ind\'ependante du mod\`ele, nous explorons une nouvelle fa\c{c}on d'inf\'erer des distances en utilisant des horloges cosmiques et SuperNovae de type Ia. C'est la th\'eorie la plus couramment utilis\'ee dans le domaine des hypoth\`eses astrophysiques.Ce manuscrit est le suivant. Apr\`es une courte pr\'esentation des connaissances en cosmologie n'ecessaires \`a la compr\'ehension de ce manuscrit, pr\'esent\'ee au chapitre 1, le chapitre 2 traitera des d\'efis du principe cosmologique ainsi que de la mani\`ere de les surmonter. Au chapitre 3, nous discuterons des caract\'eristiques techniques de la structure \`a grande \'echelle dans les enqu\^etes de BOSS et de eBOSS. Le chapitre 4 pr\'esente l'analyse d\'etaill'ee de la mesure de l'homog\'en\'eit\'e cosmique et des diff\'erents effets syst\'ematiques. Le chapitre 5 traitera de l'utilisation de l'homog\'en\'eit\'e cosmique comme r\`egle standard pour limiter les mod\`eles d'\'energie sombre des enqu\^etes actuelles et futures. Dans le chapitre 6, nous pr\'esentons nos r\'esultats sur la d\'etermination de l'homog\'en\'eit\'e du mod\`ele universel de mani\`ere ind\'ependante. Enfin, au chapitre 7, nous tirons nos conclusions.

Published
2017

25. The 2dF QSO Redshift Survey - IV. The QSO Power Spectrum from the 10k Catalogue

Author

Fiona Hoyle, P.J. Outram, T. Shanks, S.M. Croom, B.J. Boyle, N.S. Loaring, L. Miller, and R.J. Smith

Subjects
QSOS, Physics, Astrophysics (astro-ph), Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Cosmology observations, Lambda, Redshift survey, Omega, Redshift, Cosmology, Galaxy, Large-scale structure of Universe, Space and Planetary Science, Quasars, Astrophysics::Galaxy Astrophysics
Abstract

(ABRIDGED) We present a power spectrum analysis of the 10K catalogue from the 2dF QSO Redshift Survey. We compare the redshift-space power spectra of QSOs to those measured for galaxies and Abell clusters at low redshift and find that they show similar shapes in their overlap range, 50-150h^{-1}Mpc, with P_QSO(k)\propto k^{-1.4}. The amplitude of the QSO power spectrum at z~1.4 is almost comparable to that of galaxies at the present day if Omega_m=0.3 and Omega_Lambda=0.7 (the Lambda cosmology), and a factor of ~3 lower if Omega_m=1 (the EdS cosmology) is assumed. The amplitude of the QSO power spectrum is a factor of ~10 lower than that measured for Abell clusters at the present day. At larger scales, the QSO power spectra continue to rise robustly to ~400 h^{-1}Mpc, implying more power at large scales than in the APM galaxy power spectrum measured by Baugh & Efstathiou. We split the QSO sample into two redshift bins and find little evolution in the amplitude of the power spectrum. The QSO power spectrum may show a spike feature at ~90h^{-1}Mpc assuming the Lambda cosmology or ~65 h^{-1}Mpc assuming an EdS cosmology. Although the spike appears to reproduce in both the North and South strips and in two independent redshift ranges, its statistical significance is still marginal and more data is needed to test further its reality. We compare the QSO power spectra to CDM models to obtain a constraint on the shape parameter, Gamma. For two choices of cosmology (Omega_m=1, Omega_Lambda=0 and Omega_m=0.3, Omega_Lambda=0.7), we find the best fit model has Gamma~0.1 +-0.1., MNRAS Accepted

Published
2016

26. Redshift-space distortions

Author

Charles Shapiro, Ashley J. Ross, Lado Samushia, Alvise Raccanelli, and Will J. Percival

Subjects
Cosmology, Cosmology observations, Large-scale structure of Universe, General relativity, General Mathematics, General Engineering, General Physics and Astronomy, Astronomy, Astrophysics, Galaxy, Metric expansion of space, Redshift-space distortions, Statistical precision, Limit (mathematics), Mathematics
Abstract

Comparing measurements of redshift-space distortions (RSDs) with geometrical observations of the expansion of the Universe offers tremendous potential for testing general relativity on very large scales. The basic linear theory of RSDs in the distant-observer limit has been known for 25 years and the effect has been conclusively observed in numerous galaxy surveys. The next generation of galaxy survey will observe many millions of galaxies over volumes of many tens of Gpc 3 . They will provide RSD measurements of such exquisite precision that we will have to carefully analyse and correct for many systematic deviations from this simple picture in order to fully exploit the statistical precision obtained. We review RSD theory and show how ubiquitous RSDs actually are, and then consider a number of potential systematic effects, shamelessly highlighting recent work in which we have been involved. This review ends by looking ahead to the future surveys that will make the next generation of RSD measurements.

Published
2011
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27. Galaxy clusters and groups in the ALHAMBRA survey

Author

J. M. Quintana, Narciso Benítez, A. J. Cenarro, David Cristóbal-Hornillos, Emilio J. Alfaro, Carlos López-Sanjuan, R. A. Dupke, Alberto Molino, Ll. Hurtado-Gil, Jesús A. Varela, Vicent J. Martínez, C. Husillos, Marc Huertas-Company, B. Ascaso, Francisco Prada, Jesús Cabrera-Caño, L. Nieves-Seoane, Tom Broadhurst, Kerttu Viironen, Yolanda Jiménez-Teja, A. del Olmo, Mirjana Pović, Jaime Perea, J. Masegosa, Leopoldo Infante, T. Aparício-Villegas, A. Fernández-Soto, Pablo Arnalte-Mur, J. A. L. Aguerri, L. A. Díaz-García, R. M. González Delgado, J. Cepa, Francisco J. Castander, Alex Merson, I. Márquez, Miguel Cerviño, William Schoenell, Mariano Moles, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Spanish National Research Council (CSIC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 'Federico II' University of Naples Medical School, Department of Chemistry and Institute for Nanoscale Physics and chemistry (INPAC), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), AUTRES, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Gobierno de Aragón, Generalitat Valenciana, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), European Research Council, and Junta de Andalucía

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Astrophysics, X-rays galaxies clusters, clusters: general [Galaxies], Galaxies clusters general, observations [Cosmology], Galaxy cluster, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Cosmology: observations, Física, Astronomy, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Cosmology observations, Catalogues, Galaxies evolution, Space and Planetary Science, [SDU]Sciences of the Universe [physics], X-rays: galaxies: clusters, galaxies: clusters [X-rays], Galaxies: clusters: general, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Ascaso, Begoña et al., We present a catalogue of 348 galaxy clusters and groups with 0.2 < z < 1.2 selected in the 2.78 deg2 Advanced Large, Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The high precision of our photometric redshifts, close to 1 per cent, and the wide spread of the seven ALHAMBRA pointings ensure that this catalogue has better mass sensitivity and is less affected by cosmic variance than comparable samples. The detection has been carried out with the Bayesian Cluster Finder, whose performance has been checked in ALHAMBRA-like light-cone mock catalogues. Great care has been taken to ensure that the observable properties of the mocks photometry accurately correspond to those of real catalogues. From our simulations, we expect to detect galaxy clusters and groups with both 70 per cent completeness and purity down to dark matter halo masses of Mh ∼ 3 × 1013 M⊙ for z < 0.85. Cluster redshifts are expected to be recovered with ∼0.6 per cent precision for z < 1. We also expect to measure cluster masses with σMh|M∗CL∼0.25-0.35dexσMh|MCL∗∼0.25-0.35dex precision down to ∼ 3 × 1013 M⊙, masses which are 50 per cent smaller than those reached by similar work. We have compared these detections with previous optical, spectroscopic and X-rays work, finding an excellent agreement with the rates reported from the simulations. We have also explored the overall properties of these detections such as the presence of a colour–magnitude relation, the evolution of the photometric blue fraction and the clustering of these sources in the different ALHAMBRA fields. Despite the small numbers, we observe tentative evidence that, for a fixed stellar mass, the environment is playing a crucial role at lower redshifts (z < 0.5)., We acknowledge support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-22111-C03-02, AYA2010-15169, AYA2012-30789, AYA2013-48623-C2-2, AYA2013-42227-P, AYA2013-40611-P, AYA2011-29517-C03-01, AYA2014-58861-C3-1, AYA2010-15081, Generalitat Valenciana projects PROMETEOII/2014/060, Junta de Andalucia grant TIC114, JA2828, Aragon Gorvernment-Research Group E103. MP acknowledges financial support from JAE-Doc program of the Spanish National Research Council (CSIC), co-funded by the European Social Fund. PAM acknowledges support from ERC StG Grant DEGAS-259586 and from the Science and Technology Facilities Council grants ST/K003305/1 and ST/L00075X/1.

Published
2015
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28. Planck 2015 results. III. LFI systematic uncertainties

Author

Planck Collaboration, Ade, P. A. R., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Battaglia, P., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., BURIGANA, CARLO, Butler, R. C., Calabrese, E., Catalano, A., Christensen, P. R., Colombo, L. P. L., Cruz, M., Curto, A., CUTTAIA, FRANCESCO, Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., De Rosa, A., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Doré, O., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., FINELLI, FABIO, FRAILIS, Marco, Franceschet, C., FRANCESCHI, ENRICO, GALEOTTA, Samuele, Galli, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., GRUPPUSO, ALESSANDRO, Hansen, F. K., Harrison, D. L., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., MARIS, Michele, Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Meinhold, P. R., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., MORGANTE, GIANLUCA, Mortlock, D., Munshi, D., Murphy, J. A., Nati, F., Natoli, P., Noviello, F., Paci, F., Pagano, L., Pajot, F., PAOLETTI, DANIELA, Partridge, B., Pasian, F., Pearson, T. J., Perdereau, O., Pettorino, V., Piacentini, F., Pointecouteau, E., Polenta, G., Pratt, G. W., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., SANDRI, MAURA, Santos, D., Savelainen, M., Scott, D., Stolyarov, V., Stompor, R., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., TERENZI, LUCA, Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., UMANA, Grazia Maria Gloria, VALENZIANO, LUCA, Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., VILLA, FABRIZIO, Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Yvon, D., ZACCHEI, Andrea, Zibin, J. P., Zonca, A., Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Planck, Ade, P. A. R., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Battaglia, PAOLA MARIA, Battaner, E., Benabed, K., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Burigana, C., Butler, R. C., Calabrese, E., Catalano, A., Christensen, P. R., Colombo, L. P. L., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Doré, O., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., Finelli, F., Frailis, M., Franceschet, C., Franceschi, E., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Harrison, D. L., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Meinhold, P. R., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Nati, F., Natoli, P., Noviello, F., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Partridge, B., Pasian, F., Pearson, T. J., Perdereau, O., Pettorino, V., Piacentini, F., Pointecouteau, E., Polenta, G., Pratt, G. W., Puget, J. L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Stolyarov, V., Stompor, R., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Yvon, D., Zacchei, A., Zibin, J. P., Zonca, A., Ade, P, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartolo, N, Basak, S, Battaglia, P, Battaner, E, Benabed, K, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Burigana, C, Butler, R, Calabrese, E, Catalano, A, Christensen, P, Colombo, L, Cruz, M, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, de Rosa, A, de Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Doré, O, Ducout, A, Dupac, X, Elsner, F, Enßlin, T, Eriksen, H, Finelli, F, Frailis, M, Franceschet, C, Franceschi, E, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Giraud Héraud, Y, Gjerløw, E, González Nuevo, J, Górski, K, Gregorio, A, Gruppuso, A, Hansen, F, Harrison, D, Hernández Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Hornstrup, A, Hovest, W, Huffenberger, K, Hurier, G, Jaffe, A, Jaffe, T, Keihänen, E, Keskitalo, R, Kiiveri, K, Kisner, T, Knoche, J, Krachmalnicoff, N, Kunz, M, Kurki Suonio, H, Lagache, G, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leahy, J, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, Lindholm, V, López Caniego, M, Lubin, P, Macías Pérez, J, Maffei, B, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martínez González, E, Masi, S, Matarrese, S, Meinhold, P, Mennella, A, Migliaccio, M, Mitra, S, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Nati, F, Natoli, P, Noviello, F, Paci, F, Pagano, L, Pajot, F, Paoletti, D, Partridge, B, Pasian, F, Pearson, T, Perdereau, O, Pettorino, V, Piacentini, F, Pointecouteau, E, Polenta, G, Pratt, G, Puget, J, Rachen, J, Reinecke, M, Remazeilles, M, Renzi, A, Ristorcelli, I, Rocha, G, Rosset, C, Rossetti, M, Roudier, G, Rubiño Martín, J, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Scott, D, Stolyarov, V, Stompor, R, Suur Uski, A, Sygnet, J, Tauber, J, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vassallo, T, Vielva, P, Villa, F, Wade, L, Wandelt, B, Watson, R, Wehus, I, Yvon, D, Zacchei, A, Zibin, J, and Zonca, A

Subjects
Astronomy, Cosmic microwave background, cosmic microwave background radiation, cosmology observations, space vehicles, instruments, methods data analysis, Astrophysics, Cosmic background radiation, Cosmology: observation, 01 natural sciences, Space vehicles: instruments, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, QC, QB, media_common, Physics, Settore FIS/05, Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, Planck temperature, Methods: data analysis, Astronomy and Astrophysics, Space and Planetary Science, Amplitude, symbols, cosmic background radiation, cosmology: observations, space vehicles: instruments, methods: data analysis, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, Space vehicles: instrument, NO, instruments [Space vehicles], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, instrument [Space vehicles], 0103 physical sciences, Planck, Reionization, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysic, data analysi [Methods], Sky, Multipole expansion, Methods: data analysi
Abstract

CSIC, Consejo Superior de Investigaciones Científicas; ERC, European Research Council; MINECO, Ministerio de Economía y Competitividad; MPG, Max-Planck-Gesellschaft; NASA, National Aeronautics and Space Administration; etc., Ade, P.A.R., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Battaglia, P., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Burigana, C., Butler, R.C., Calabrese, E., Catalano, A., Christensen, P.R., Colombo, L.P.L., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J.M., Doré, O., Ducout, A., Dupac, X., Elsner, F., Enßlin, T.A., Eriksen, H.K., Finelli, F., Frailis, M., Franceschet, C., Franceschi, E., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K.M., Gregorio, A., Gruppuso, A., Hansen, F.K., Harrison, D.L., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Hornstrup, A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T.S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leahy, J.P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lubin, P.M., Macías-Pérez, J.F., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P.G., Martínez-González, E., Masi, S., Matarrese, S., Meinhold, P.R., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J.A., Nati, F., Natoli, P., Noviello, F., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Partridge, B., Pasian, F., Pearson, T.J., Perdereau, O., Pettorino, V., Piacentini, F., Pointecouteau, E., Polenta, G., Pratt, G.W., Puget, J.-L., Rachen, J.P., Reinecke, M., Remazeilles, M., Renzi, A., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J.A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Stolyarov, V., Stompor, R., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Watson, R., Wehus, I.K., Yvon, D., Zacchei, A., Zibin, J.P., Zonca, A.

Published
2015
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29. Galaxy clusters and groups in the ALHAMBRA survey

Author

Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Ascaso, Begoña, Benitez, N., Fernandez-Soto, Alberto, Arnalte-Mur, P., López-Sanjuán, Carlos, Molino, Alberto, Schoenell, W., Jiménez-Teja, Yolanda, Merson, Alexander I., Huertas-Company, Marc, Díaz-García, Luis A., Martínez, Vicent J., Cenarro, Andres Javier, Dupke, Renato A., Márquez, I., Masegosa, J., Nieves-Seoane, L., Pović, Mirjana, Varela, Jesús, Viironen, Kerttu, Aguerri, José Alfonso López, Olmo, A. del, Moles, Mariano, Perea, Jaime D., Alfaro, Emilio J., Aparicio-Villegas, T., Broadhurst, Tom J., Cabrera Caño, Jesús María, Castander, Francisco Javier J., Cepa, Jordi P., Cerviño, Miguel, González Delgado, R. M., Cristóbal-Hornillos, David, Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Ascaso, Begoña, Benitez, N., Fernandez-Soto, Alberto, Arnalte-Mur, P., López-Sanjuán, Carlos, Molino, Alberto, Schoenell, W., Jiménez-Teja, Yolanda, Merson, Alexander I., Huertas-Company, Marc, Díaz-García, Luis A., Martínez, Vicent J., Cenarro, Andres Javier, Dupke, Renato A., Márquez, I., Masegosa, J., Nieves-Seoane, L., Pović, Mirjana, Varela, Jesús, Viironen, Kerttu, Aguerri, José Alfonso López, Olmo, A. del, Moles, Mariano, Perea, Jaime D., Alfaro, Emilio J., Aparicio-Villegas, T., Broadhurst, Tom J., Cabrera Caño, Jesús María, Castander, Francisco Javier J., Cepa, Jordi P., Cerviño, Miguel, González Delgado, R. M., and Cristóbal-Hornillos, David

Abstract

We present a catalogue of 348 galaxy clusters and groups with 0.2 < z < 1.2 selected in the 2.78 deg2 Advanced Large, Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The high precision of our photometric redshifts, close to 1 per cent, and the wide spread of the seven ALHAMBRA pointings ensure that this catalogue has better mass sensitivity and is less affected by cosmic variance than comparable samples. The detection has been carried out with the Bayesian Cluster Finder, whose performance has been checked in ALHAMBRA-like light-cone mock catalogues. Great care has been taken to ensure that the observable properties of the mocks photometry accurately correspond to those of real catalogues. From our simulations, we expect to detect galaxy clusters and groups with both 70 per cent completeness and purity down to dark matter halo masses of Mh ~ 3 × 1013M* for z < 0.85. Cluster redshifts are expected to be recovered with ~0.6 per cent precision for z < 1. We also expect to measure cluster masses with σMh|MCL * ~ 0.25-0.35 precision down to ~ 3 × 1013M⊙, masses which are 50 per cent smaller than those reached by similar work. We have compared these detections with previous optical, spectroscopic and X-rays work, finding an excellent agreement with the rates reported from the simulations. We have also explored the overall properties of these detections such as the presence of a colour-magnitude relation, the evolution of the photometric blue fraction and the clustering of these sources in the different ALHAMBRA fields. Despite the small numbers, we observe tentative evidence that, for a fixed stellar mass, the environment is playing a crucial role at lower redshifts (z < 0.5). © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Published
2015

31. The Instituto de Astrofisica de Canarias–Bartol Cosmic Microwave Background Anisotropy Experiment: Results of the 1994 Campaign

Author

Michele Limon, C. M. Gutierrez, Rafael Rebolo, Lucio Piccirillo, and B. Femenia

Subjects
Physics, cosmic microwave background, Cold dark matter, Cosmic microwave background, cosmology observations, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Atmospheric noise, Likelihood analysis, Space and Planetary Science, Content (measure theory), statistical methods, Anisotropy, Multipole expansion, Noise (radio)
Abstract

We present the results of a Cosmic Microwave Background (CMB) anisotropy ground-based millimetric experiment sensitive to fluctuations on angular scales of $\sim 2\degg$. Four independent bands centered at 3.3, 2.1, 1.3 and 1.1 mm collected $\sim 550$ hours of observation during the Summer of 1994. The instrument was located on the island of Tenerife at an altitude of 2400 m. The low water-vapor content and the atmospheric stability of the site, combined with new techniques to subtract atmospheric noise, result in the reduction of atmospheric contamination in the lowest frequency channel to a level of $\sim 1.5$~times the instrument noise. Detailed estimations of Galactic foreground contamination show that this contribution is negligible at $|b| \stackrel{>}{_\sim} 12\degg$. Two different multipole bands ($\ell=53^{+22}_{-13}$ and $33^{+24}_{-13}$) are analyzed showing that our technique to subtract the atmospheric contribution is more effective in the multipole band at $\ell=53$. A likelihood analysis of these data reveals the presence of a common signal between the channels at 3.3, 2.1 and 1.3 mm corresponding to a band power estimate of $ \sqrt{\lla (\lla+1) C_{\lla}/(2 \pi)} = 2.0^{+1.0}_{-0.8} \cdot 10^{-5}$ and $\sqrt{\lla (\lla+1) C_{\lla}/(2 \pi)} = 4.1^{+2.4}_{-2.2} \cdot 10^{-5}$ for the $\ell =53$ and 33 multipole bands respectively. Calibration uncertainty has been treated as a systematic effect. The level of fluctuations in the $\ell =53$ band is in good agreement with our preliminary analysis presented in Piccirillo \et 1997, with measurements by other experiments working at similar angular scales, and with the predictions of standard Cold Dark Matter (CDM) models.

Published
1998
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32. Planck intermediate results I. Further validation of new Planck clusters with XMM-Newton

Author

Planck Collaboration: N. Aghanim54, M. Arnaud69⋆, M. Ashdown66, 5, F. Atrio Barandela17, J. Aumont54, C. Baccigalupi79, A. Balbi34, A. J. Banday87, 8, R. B. Barreiro62, J. G. Bartlett1, E. Battaner89, K. Benabed55, J. P. Bernard8, M. Bersanelli31, H. Bo ̈hringer75, A. Bonaldi65, J. R. Bond7, J. Borrill13, F. R. Bouchet55, H. Bourdin34, M. L. Brown65, C. Burigana47, R. C. Butler47, P. Cabella35, J. F. Cardoso70, 1, 55, P. Carvalho5, A. Catalano71, L. Cayo ́n24, A. Chamballu52, R. R. Chary53, L. Y. Chiang58, G. Chon75, P. R. Christensen76, D. L. Clements52, S. Colafrancesco44, S. Colombi55, A. Coulais68, B. P. Crill64, F. Cuttaia47, A. Da Silva11, H. Dahle60, R. J. Davis65, P. de Bernardis30, G. de Gasperis34, G. de Zotti43, J. Delabrouille1, J. De ́mocle`s69, F. X. De ́sert51, J. M. Diego62, K. Dolag88, H. Dole54, S. Donzelli48, O. Dore ́64, 9, M. Douspis54, X. Dupac40, T. A. Enßlin74, H. K. Eriksen60, F. Finelli47, I. Flores Cacho8, O. Forni87, P. Fosalba56, M. Frailis45, S. Fromenteau1, S. Galeotta45, K. Ganga1, R. T. Ge ́nova Santos61, M. Giard87, J. Gonza ́lez Nuevo62, R. Gonza ́lez Riestra39, K. M. Go ́rski64, A. Gruppuso47, F. K. Hansen60, D. Harrison59, A. Hempel61, C. Herna ́ndez Monteagudo12, D. Herranz62, S. R. Hildebrandt9, A. Hornstrup16, K. M. Huffenberger90, G. Hurier71, T. Jagemann40, J. Jasche4, M. Juvela23, E. Keiha ̈nen23, R. Keskitalo64, T. S. Kisner73, R. Kneissl38, 6, J. Knoche74, L. Knox26, H. Kurki Suonio23, G. Lagache54, A. La ̈hteenma ̈ki2, J. M. Lamarre68, A. Lasenby5, C. R. Lawrence64, S. Leach79, R. Leonardi40, A. Liddle22, P. B. Lilje60, M. Lo ́pez Caniego62, G. Luzzi67, J. F. Mac ́ıas Pe ́rez71, D. Maino31, N. Mandolesi47, R. Mann80, F. Marleau19, D. J. Marshall87, E. Mart ́ınez Gonza ́lez62, S. Masi30, M. Massardi46, S. Matarrese29, F. Matthai74, P. Mazzotta34, P. R. Meinhold27, A. Melchiorri30, J. B. Melin15, L. Mendes40, A. Mennella31, M. A. Miville Descheˆnes54, 7, A. Moneti55, L. Montier87, G. Morgante47, D. Mortlock52, D. Munshi81, P. Naselsky76, P. Natoli33, 3, 47, H. U. Nørgaard Nielsen16, F. Noviello65, S. Osborne84, F. Pasian45, G. Patanchon1, O. Perdereau67, F. Perrotta79, F. Piacentini30, E. Pierpaoli21, S. Plaszczynski67, P. Platania63, E. Pointecouteau87, G. Polenta3, N. Ponthieu54, L. Popa57, T. Poutanen42, 23, 2, G. W. Pratt69, J. L. Puget54, J. P. Rachen74, R. Rebolo61, 14, 37, M. Reinecke74, M. Remazeilles54, 1, C. Renault71, S. Ricciardi47, T. Riller74, I. Ristorcelli87, G. Rocha64, C. Rosset1, M. Rossetti31, J. . A. . R. u. b. i. n. ̃ o. M. a. r. t. ́ı n. 6 1, 3 7 , B. . R. u. s. h. o. l. m. e. 5 3, M. . S. a. n. d. r. i. 4 7 , G. . S. a. v. i. n. i. 7 8, B. . M. . S. c. h. a. e. f. e. r. 8 6 , D. . S. c. o. t. t. 2 0, G. . F. . S. m. o. o. t. 2 5 , 7 3, 1 , J. . L. . S. t. a. r. c. k. 6 9, F. . S. t. i. v. o. l. i. 5 0, R. Sunyaev74, D. Sutton59, J. F. Sygnet55, J. A. Tauber41, L. Terenzi47, L. Toffolatti18, M. Tomasi48, M. Tristram67, L. Valenziano47, B. Van Tent72, P. Vielva62, F. Villa47, N. Vittorio34, B. D. Wandelt55, 85, 28, J. Weller88, S. D. M. White74, D. Yvon15, A. Zacchei45, A. Zonca27, GREGORIO, ANNA, Universidad de Cantabria, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), 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), AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Traitement et Communication de l'Information (LTCI), Télécom ParisTech-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), PLANCK, European Space Agency, Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), Agenzia Spaziale Italiana, Consiglio Nazionale delle Ricerche, Istituto Nazionale di Fisica Nucleare, National Aeronautics and Space Administration (US), Department of Energy (US), Science and Technology Facilities Council (UK), UK Space Agency, Consejo Superior de Investigaciones Científicas (España), Ministerio de Ciencia e Innovación (España), Junta de Andalucía, Academy of Finland, Ministry of Education and Culture (Finland), German Centre for Air and Space Travel, Max Planck Society, National Space Institute (Denmark), Research Council of Norway, Science Foundation Ireland, Fundação para a Ciência e a Tecnologia (Portugal), Planck Collaboration: N., Aghanim54, M., Arnaud69⋆, M., Ashdown66, F., Atrio Barandela17, J., Aumont54, C., Baccigalupi79, A., Balbi34, A. J., Banday87, R. B., Barreiro62, J. G., Bartlett1, E., Battaner89, K., Benabed55, J. P., Bernard8, M., Bersanelli31, H., Bo ̈hringer75, A., Bonaldi65, J. R., Bond7, J., Borrill13, F. R., Bouchet55, H., Bourdin34, M. L., Brown65, C., Burigana47, R. C., Butler47, P., Cabella35, J. F., Cardoso70, 1, 55, P., Carvalho5, A., Catalano71, L., Cayo ́n24, A., Chamballu52, R. R., Chary53, L. Y., Chiang58, G., Chon75, P. R., Christensen76, D. L., Clements52, S., Colafrancesco44, S., Colombi55, A., Coulais68, B. P., Crill64, F., Cuttaia47, A., Da Silva11, H., Dahle60, R. J., Davis65, P., de Bernardis30, G., de Gasperis34, G., de Zotti43, J., Delabrouille1, J., De ́mocle`s69, F. X., De ́sert51, J. M., Diego62, K., Dolag88, H., Dole54, S., Donzelli48, O., Dore ́64, M., Douspis54, X., Dupac40, T. A., Enßlin74, H. K., Eriksen60, F., Finelli47, I., Flores Cacho8, O., Forni87, P., Fosalba56, M., Frailis45, S., Fromenteau1, S., Galeotta45, K., Ganga1, R. T., Ge ́nova Santos61, M., Giard87, J., Gonza ́lez Nuevo62, R., Gonza ́lez Riestra39, K. M., Go ́rski64, Gregorio, Anna, A., Gruppuso47, F. K., Hansen60, D., Harrison59, A., Hempel61, C., Herna ́ndez Monteagudo12, D., Herranz62, S. R., Hildebrandt9, A., Hornstrup16, K. M., Huffenberger90, G., Hurier71, T., Jagemann40, J., Jasche4, M., Juvela23, E., Keiha ̈nen23, R., Keskitalo64, T. S., Kisner73, R., Kneissl38, J., Knoche74, L., Knox26, H., Kurki Suonio23, G., Lagache54, A., La ̈hteenma ̈ki2, J. M., Lamarre68, A., Lasenby5, C. R., Lawrence64, S., Leach79, R., Leonardi40, A., Liddle22, P. B., Lilje60, M., Lo ́pez Caniego62, G., Luzzi67, J. F., Mac ́ıas Pe ́rez71, D., Maino31, N., Mandolesi47, R., Mann80, F., Marleau19, D. J., Marshall87, E., Mart ́ınez Gonza ́lez62, S., Masi30, M., Massardi46, S., Matarrese29, F., Matthai74, P., Mazzotta34, P. R., Meinhold27, A., Melchiorri30, J. B., Melin15, L., Mendes40, A., Mennella31, M. A., Miville Descheˆnes54, A., Moneti55, L., Montier87, G., Morgante47, D., Mortlock52, D., Munshi81, P., Naselsky76, P., Natoli33, 3, 47, H. U., Nørgaard Nielsen16, F., Noviello65, S., Osborne84, F., Pasian45, G., Patanchon1, O., Perdereau67, F., Perrotta79, F., Piacentini30, E., Pierpaoli21, S., Plaszczynski67, P., Platania63, E., Pointecouteau87, G., Polenta3, N., Ponthieu54, L., Popa57, T., Poutanen42, 23, 2, G. W., Pratt69, J. L., Puget54, J. P., Rachen74, R., Rebolo61, 14, 37, M., Reinecke74, M., Remazeilles54, C., Renault71, S., Ricciardi47, T., Riller74, I., Ristorcelli87, G., Rocha64, C., Rosset1, M., Rossetti31, J. . A. . R. u. b. i. n. ̃ o. M. a. r. t. ́ı n., 6 1, 3 7, B. . R. u. s. h. o. l. m. e. 5 3, M. . S. a. n. d. r. i. 4 7, G. . S. a. v. i. n. i. 7 8, B. . M. . S. c. h. a. e. f. e. r. 8 6, D. . S. c. o. t. t. 2 0, G. . F. . S. m. o. o. t. 2 5, 7 3, 1, J. . L. . S. t. a. r. c. k. 6 9, F. . S. t. i. v. o. l. i., 5 0, R., Sunyaev74, D., Sutton59, J. F., Sygnet55, J. A., Tauber41, L., Terenzi47, L., Toffolatti18, M., Tomasi48, M., Tristram67, L., Valenziano47, B., Van Tent72, P., Vielva62, F., Villa47, N., Vittorio34, B. D., Wandelt55, 85, 28, J., Weller88, S. D. M., White74, D., Yvon15, A., Zacchei45, A., Zonca27, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Department of Physics, and Helsinki Institute of Physics

Subjects
galaxies: clusters: intracluster medium, galaxies: clusters: general, cosmology: observations, cosmic background radiation, x-rays: galaxies: clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, education, Cosmology: observations − Galaxies: cluster: general − Galaxies: clusters: intracluster medium − Cosmic background radiation, cosmology observations, Flux, FOS: Physical sciences, Astrophysics, clusters: intracluster medium [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmic background radiation, 01 natural sciences, 7. Clean energy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, galaxies, X-rays, 0103 physical sciences, Cluster (physics), Cosmology: observations, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, X-rays: galaxies: clusters, Planck, observations − Galaxies: cluster: general − Galaxies: clusters: intracluster medium − Cosmic background radiation [Cosmology], Spectroscopy, observations [Cosmology], intracluster medium, 010303 astronomy & astrophysics, Malmquist bias, Physics, Astrophysics - Cosmology and Extragalactic Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysics, 115 Astronomy, Space science, Redshift, Space and Planetary Science, symbols, galaxies: clusters [X-rays], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 < S/N < 5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 < z < 0.94, demonstrating Planck's capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using Y X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y SZ-Y X relation, with a turnover at Y SZ ~ 4 × 10 -4 arcmin 2. We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the Y X vs. Y SZ and X-ray flux F X vs. Y SZ relations. © 2012 ESO., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU).

Published
2012
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33. Initial LOFAR observations of epoch of reionization windows : II. Diffuse polarized emission in the ELAIS-N1 field

Author

Jelić, V., de Bruyn, A. G., Mevius, M., Abdalla, F. B., Asad, K. M. B., Bernardi, G., Brentjens, M. A., Bus, S., Chapman, E., Ciardi, B., Daiboo, S., Fernandez, E. R., Ghosh, A., Harker, G., Jensen, H., Kazemi, S., Koopmans, L. V. E., Labropoulos, P., Martinez-Rubi, O., Mellema, G., Offringa, A. R., Pandey, V. N., Patil, A. H., Thomas, R. M., Vedantham, H. K., Veligatla, V., Yatawatta, S., Zaroubi, S., Alexov, A., Anderson, J., Avruch, I. M., Beck, R., Bell, M. E., Bentum, M. J., Best, P., Bonafede, A., Bregman, J., Breitling, F., Broderick, J., Brouw, W. N., Brüggen, M., Butcher, H. R., Conway, J. E., de Gasperin, F., de Geus, E., Deller, A., Dettmar, R. -J, Duscha, S., Eislöffel, J., Engels, D., Falcke, H., Fallows, R. A., Fender, R., Ferrari, C., Frieswijk, W., Garrett, M. A., Grießmeier, J., Gunst, A. W., Hamaker, J. P., Hassall, T. E., Haverkorn, M., Heald, G., Hessels, J. W. T., Hoeft, M., Hörandel, J., Horneffer, A., van der Horst, A., Iacobelli, M., Juette, E., Karastergiou, A., Kondratiev, V. I., Kramer, M., Kuniyoshi, M., Kuper, G., van Leeuwen, J., Maat, P., Mann, G., McKay-Bukowski, D., McKean, J. P., Munk, H., Nelles, A., Norden, M. J., Paas, H., Pandey-Pommier, M., Pietka, G., Pizzo, R., Polatidis, A. G., Reich, W., Röttgering, H., Rowlinson, A., Scaife, A. M. M., Schwarz, D., Serylak, M., Smirnov, O., Steinmetz, M., Stewart, A., Tagger, M., Tang, Y., Tasse, C., ter Veen, S., Thoudam, Satyendra, Toribio, C., Vermeulen, R., Vocks, C., van Weeren, R. J., Wijers, R. A. M. J., Wijnholds, S. J., Wucknitz, O., Zarka, P., Jelić, V., de Bruyn, A. G., Mevius, M., Abdalla, F. B., Asad, K. M. B., Bernardi, G., Brentjens, M. A., Bus, S., Chapman, E., Ciardi, B., Daiboo, S., Fernandez, E. R., Ghosh, A., Harker, G., Jensen, H., Kazemi, S., Koopmans, L. V. E., Labropoulos, P., Martinez-Rubi, O., Mellema, G., Offringa, A. R., Pandey, V. N., Patil, A. H., Thomas, R. M., Vedantham, H. K., Veligatla, V., Yatawatta, S., Zaroubi, S., Alexov, A., Anderson, J., Avruch, I. M., Beck, R., Bell, M. E., Bentum, M. J., Best, P., Bonafede, A., Bregman, J., Breitling, F., Broderick, J., Brouw, W. N., Brüggen, M., Butcher, H. R., Conway, J. E., de Gasperin, F., de Geus, E., Deller, A., Dettmar, R. -J, Duscha, S., Eislöffel, J., Engels, D., Falcke, H., Fallows, R. A., Fender, R., Ferrari, C., Frieswijk, W., Garrett, M. A., Grießmeier, J., Gunst, A. W., Hamaker, J. P., Hassall, T. E., Haverkorn, M., Heald, G., Hessels, J. W. T., Hoeft, M., Hörandel, J., Horneffer, A., van der Horst, A., Iacobelli, M., Juette, E., Karastergiou, A., Kondratiev, V. I., Kramer, M., Kuniyoshi, M., Kuper, G., van Leeuwen, J., Maat, P., Mann, G., McKay-Bukowski, D., McKean, J. P., Munk, H., Nelles, A., Norden, M. J., Paas, H., Pandey-Pommier, M., Pietka, G., Pizzo, R., Polatidis, A. G., Reich, W., Röttgering, H., Rowlinson, A., Scaife, A. M. M., Schwarz, D., Serylak, M., Smirnov, O., Steinmetz, M., Stewart, A., Tagger, M., Tang, Y., Tasse, C., ter Veen, S., Thoudam, Satyendra, Toribio, C., Vermeulen, R., Vocks, C., van Weeren, R. J., Wijers, R. A. M. J., Wijnholds, S. J., Wucknitz, O., and Zarka, P.

Abstract

Aims. This study aims to characterise the polarized foreground emission in the ELAIS-N1 field and to address its possible implications for extracting of the cosmological 21 cm signal from the LOw-Frequency ARray – Epoch of Reionization (LOFAR-EoR) data. Methods. We used the high band antennas of LOFAR to image this region and RM-synthesis to unravel structures of polarized emission at high Galactic latitudes. Results. The brightness temperature of the detected Galactic emission is on average ~4 K in polarized intensity and covers the range from –10 to + 13 rad m-2 in Faraday depth. The total polarized intensity and polarization angle show a wide range of morphological features. We have also used the Westerbork Synthesis Radio Telescope (WSRT) at 350 MHz to image the same region. The LOFAR and WSRT images show a similar complex morphology at comparable brightness levels, but their spatial correlation is very low. The fractional polarization at 150 MHz, expressed as a percentage of the total intensity, amounts to ≈1.5%. There is no indication of diffuse emission in total intensity in the interferometric data, in line with results at higher frequencies Conclusions. The wide frequency range, high angular resolution, and high sensitivity make LOFAR an exquisite instrument for studying Galactic polarized emission at a resolution of ~1–2 rad m-2 in Faraday depth. The different polarized patterns observed at 150 MHz and 350 MHz are consistent with different source distributions along the line of sight wring in a variety of Faraday thin regions of emission. The presence of polarized foregrounds is a serious complication for epoch of reionization experiments. To avoid the leakage of polarized emission into total intensity, which can depend on frequency, we need to calibrate the instrumental polarization across the field of view to a small fraction of 1%.

Published
2014
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34. Erratum: The Herschel PEP/HerMES Luminosity Function – I. Probing the Evolution of PACS selected Galaxies to z ≃ 4

Author

Domínguez Sánchez, Helena and Domínguez Sánchez, Helena

Abstract

© 2013 The Authors Published by Oxford University Press. Artículo firmado por 102 autores., This is an erratum to the paper ‘The Herschel PEP/HerMES Luminosity Function – I: Probing the Evolution of PACS selected Galaxies to z ≃ 4’, by Gruppioni et al., published in MNRAS, 432, 23 (2013)., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2013

35. The White Mountain polarimeter telescope and an upper limit on cosmic microwave background polarization

Author

Fabrizio Villa, Maarten van der Heide, Ocleto D'Arcangelo, Fabrizio Stavola, G. Vietor Davis, Joshua Marvil, Jeffery Childers, Philip Lubin, Thyrso Villela, Hugh O`Neill, Terrence D. Cole, Alan R. Levy, Brian Williams, Markus Ansmann, Rodrigo Leonardi, Peter T. Timbie, Peter Meinhold, Gerald Miller, Marco Bersanelli, Nathan Stebor, and Carlos Alexandre Wuensche

Subjects
White Mountain, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Physics::Geophysics, law.invention, Telescope, Celestial pole, law, 0103 physical sciences, 010303 astronomy & astrophysics, media_common, Instrumentation polarimeters, Physics, geography, Plateau, geography.geographical_feature_category, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Polarimeter, Cosmology observations, Polarization (waves), geography.mountain, Space and Planetary Science, Sky
Abstract

The White Mountain Polarimeter (WMPol) is a dedicated ground-based microwave telescope and receiver system for observing polarization of the Cosmic Microwave Background. WMPol is located at an altitude of 3880 meters on a plateau in the White Mountains of Eastern California, USA, at the Barcroft Facility of the University of California White Mountain Research Station. Presented here is a description of the instrument and the data collected during April through October 2004. We set an upper limit on $E$-mode polarization of 14 $\mu\mathrm{K}$ (95% confidence limit) in the multipole range $170

Published
2008
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36. Population III stars: hidden or disappeared?

Author

Tornatore, Luca, Ferrara, Andrea, Schneider, Raffaella, Tornatore, Luca, Ferrara, A, and Raffaella, S.

Subjects
Cosmology: observations, Astrophysics (astro-ph), cosmology observations, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Astrophysics, galaxy formation, cosmology theory, Space and Planetary Science, intergalactic medium, Cosmology: theory, cosmology observation, Astrophysics::Galaxy Astrophysics, Intergalactic medium
Abstract

A PopIII/Pop II transition from massive to normal stars is predicted to occur when the metallicity of the star forming gas crosses the critical range Z_cr = 10^(-5 +/- 1) Z_sun. To investigate the cosmic implications of such process we use numerical simulations which follow the evolution, metal enrichment and energy deposition of both Pop III and Pop II stars. We find that: (i) due to inefficient heavy element transport by outflows and slow "genetic" transmission during hierarchical growth, large fluctuations around the average metallicity arise; as a result Pop III star formation continues down to z=2.5, but at a low peak rate of 10^-5 M_sun yr^-1 Mpc^-3 occurring at z~6 (about 10^-4 of the PopII one); (ii) Pop III star formation proceeds in a "inside-out" mode in which formation sites are progressively confined at the periphery of collapsed structures, where the low gas density and correspondingly long free-fall timescales result in a very inefficient astration. These conclusions strongly encourage deep searches for pristine star formation sites at moderate (2, Comment: to appear in MNRAS

Published
2007

37. Galactic Foreground Contribution to the BEAST Cosmic Microwave Background Anisotropy Maps

Author

Marco Bersanelli, Miikka Kangas, P. Platania, Carlo Burigana, Josh Marvil, Thyrso Villela, Carlos Alexandre Wuensche, Benjamin D. Wandelt, Nazzareno Mandolesi, Jorge Mejia, Philip Lubin, Davide Maino, Nathan Stebor, Jeff Childers, Camilo Tello, Michael Seiffert, N. Figueiredo, Peter Meinhold, Hugh O’Neill, and I. J. O'Dwyer

Subjects
ISM structure, Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, 02 engineering and technology, Astrophysics, 01 natural sciences, Declination, Lower limit, law.invention, Telescope, law, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Anisotropy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Coupling constant, Order (ring theory), 020206 networking & telecommunications, Astronomy and Astrophysics, Scale height, Cosmology observations, 13. Climate action, Space and Planetary Science
Abstract

We report limits on the Galactic foreground emission contribution to the Background Emission Anisotropy Scanning Telescope (BEAST) Ka- and Q-band CMB anisotropy maps. We estimate the contribution from the cross-correlations between these maps and the foreground emission templates of an H alpha map, a destriped version of the Haslam et al. 408 MHz map, and a combined 100 mu m IRAS DIRBE map. Our analysis samples the BEAST similar to 10 degrees declination band into 24 one-hour (R. A.) wide sectors with similar to 7900 pixels each, where we calculate (1) the linear correlation coefficient between the anisotropy maps and the templates; (2) the coupling constants between the specific intensity units of the templates and the antenna temperature at the BEAST frequencies; and (3) the individual foreground contributions to the BEAST anisotropy maps. The peak sector contributions of the contaminants in the Ka-band are of 56.5% free-free with a coupling constant of 8.3 +/- 0.4 mu K R-1, and 67.4% dust with 45.0 +/- 2.0 mu K MJy(-1) sr(-1). In the Q band the corresponding values are of 64.4% free-free with 4.1 +/- 0.2 mu K R-1 and 67.5% dust with 24.0 +/- 1.0 mu K MJy(-1) sr(-1). Using a lower limit of 10% in the relative uncertainty of the coupling constants, we can constrain the sector contributions of each contaminant in both maps to

Published
2005
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38. GRB 030227: The first multiwavelength afterglow of an INTEGRAL GRB

Author

Sylvio Klose, Sandro Mereghetti, Sofia Feltzing, Victor Reglero, A. J. Castro-Tirado, Henrik D. Pedersen, J. M. Castro Cerón, E.P.J. van den Heuvel, M. D. Perez-Ramirez, Chryssa Kouveliotou, S. Brandt, A. S. Fruchter, Nial R. Tanvir, José M. Vílchez, A. de Ugarte Postigo, Shashi B. Pandey, Michael I. Andersen, James E. Rhoads, Vijay Mohan, Filippo Mannucci, Ralph A. M. J. Wijers, B. L. Jensen, Niels Lund, Jens Hjorth, Sergei Guziy, Lex Kaper, Ram Sagar, J. P. U. Fynbo, Ingemar Lundström, C. Riess, Javier Gorosabel, N. Masetti, D. Reverte, S. A. Trushkin, Andrea Tiengo, Elena Pian, J. Buckle, Evert Rol, Paul Vreeswijk, S. Martínez Núñez, Jochen Greiner, Eliana Palazzi, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, Spectral index, Bursts, Astrophysics (astro-ph), Gamma rays, Compton scattering, bursts [gamma rays], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Photometric, Cosmology observations, UNESCO::ASTRONOMÍA Y ASTROFÍSICA, Power law, ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia [UNESCO], observations [cosmology], Afterglow, photometric [techniques], Space and Planetary Science, Astronomy, Astrophysics and Cosmology, UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia, Gamma-ray burst, ASTRONOMÍA Y ASTROFÍSICA [UNESCO]
Abstract

We present multiwavelength observations of a gamma-ray burst detected by INTEGRAL (GRB 030227) between 5.3 hours and ~1.7 days after the event. Here we report the discovery of a dim optical afterglow (OA) that would not have been detected by many previous searches due to its faintess (R~23). This OA was seen to decline following a power law decay with index Alpha_R= -0.95 +/- 0.16. The spectral index Beta_opt/NIR yielded -1.25 +/- 0.14. These values may be explained by a relativistic expansion of a fireball (with p = 2.0) in the cooling regime. We also find evidence for inverse Compton scattering in X-rays., Comment: 5 pages, 5 figures, accepted for publication in A&A

Published
2003

39. Systematic Uncertainties Associated with the Cosmological Analysis of the First Pan-STARRS1 Type Ia Supernova Sample

Author

Scolnic, D., Rest, A., Riess, A., Huber, M. E., Foley, R. J., Brout, D., Chornock, R., Narayan, G., Tonry, J. L., Berger, Edo, Soderberg, Alicia M., Stubbs, Christopher William, Kirshner, Robert P., Rodney, S., Smartt, S. J., Schlafly, E., Botticella, M. T., Challis, P., Czekala, I., Drout, M., Hudson, M. J., Kotak, R., Leibler, C., Lunnan, R., Marion, G. H., McCrum, M., Milisavljevic, Danny, Pastorello, A., Sanders, Nathan Edward, Smith, K., Stafford, E., Thilker, D., Valenti, S., Wood-Vasey, W. M., Zheng, Z., Burgett, W. S., Chambers, K. C., Denneau, L., Draper, P. W., Flewelling, H., Hodapp, K. W., Kaiser, N., Kudritzki, R.-P., Magnier, E. A., Metcalfe, N., Price, P. A., Sweeney, W., Wainscoat, R., and Waters, C.

Subjects
supernova general, cosmology observations, cosmological parameters
Abstract

We probe the systematic uncertainties from the 113 Type Ia supernovae (SN Ia) in the Pan-STARRS1 (PS1) sample along with 197 SN Ia from a combination of low-redshift surveys. The companion paper by Rest et al. (2013) describes the photometric measurements and cosmological inferences from the PS1 sample. The largest systematic uncertainty stems from the photometric calibration of the PS1 and low-z samples. We increase the sample of observed Calspec standards from 7 to 10 used to define the PS1 calibration system. The PS1 and SDSS-II calibration systems are compared and discrepancies up to ∼ 0.02 mag are recovered. We find uncertainties in the proper way to treat intrinsic colors and reddening produce differences in the recovered value of w up to 3%. We estimate masses of host galaxies of PS1 supernovae and detect an insignificant difference in distance residuals of the full sample of 0.037±0.031 mag for host galaxies with high and low masses. Assuming flatness and including systematic uncertainties in our analysis of only SNe measurements, we find w =−1.120+0.360 −0.206(Stat)+0.269 −0.291(Sys). With additional constraints from BAO, CMB (Planck) and H0 measurements, we find w = −1.166+0.072 −0.069 and Ωm = 0.280+0.013 −0.012 (statistical and systematic errors added in quadrature). Significance of the inconsistency with w = −1 depends on whether we use Planck or WMAP measurements of the CMB: wBAO+H0+SN+WMAP = −1.124+0.083−0.065., Astronomy

Published
2014
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40. The completed SDSS-IV extended baryon oscillation spectroscopic survey: growth rate of structure measurement from anisotropic clustering analysis in configuration space between redshift 0.6 and 1.1 for the emission-line galaxy sample

Author

Santiago Avila, Yuting Wang, Violeta Gonzalez-Perez, Arnaud de Mattia, Kyle S. Dawson, Shadab Alam, Gong-Bo Zhao, Will J. Percival, Anand Raichoor, Romain Paviot, Claudio Gorgoni, Jiamin Hou, Faizan G. Mohammad, Cheng Zhao, Eva Maria Mueller, Ashley J. Ross, Graziano Rossi, Jean-Paul Kneib, V. Ruhlmann-Kleider, Hélion du Mas des Bourboux, Amélie Tamone, Sylvain de la Torre, Etienne Burtin, Stephanie Escoffier, Donald P. Schneider, Chia-Hsun Chuang, Johan Comparat, Michael J. Chapman, Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Center for Cosmology & AstroParticle Physics, Ohio State University [Columbus] (OSU), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Perimeter Institute for Theoretical Physics [Waterloo], Department of Physics and Astronomy [Waterloo], University of Waterloo [Waterloo], Universidad Autonoma de Madrid (UAM), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Max-Planck-Institut für Extraterrestrische Physik (MPE), University of Utah, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institute of Cosmology and Gravitation [Portsmouth] (ICG), University of Portsmouth, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Department of Physics [Oxford], University of Oxford [Oxford], Sejong University, Institute for Gravitation and the Cosmos [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Chinese Academy of Sciences [Beijing] (CAS), ANR-16-CE31-0021,eBOSS,Sondes cosmologiques de la gravitation et de l'énergie noire(2016), ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project: 670193,H2020,ERC-2014-ADG,COSFORM(2015), European Project: 290975,EC:FP7:ERC,ERC-2011-ADG_20110209,LIDA(2012), Universidad Autónoma de Madrid (UAM), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and University of Oxford

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Galaxies distances and redshift, reconstruction, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Large scale structure of Universe, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Correlation function (quantum field theory), distance scale, 01 natural sciences, large-scale structure, efficient, 0103 physical sciences, evolution, quasar sample, Emission spectrum, Perturbation theory, dark energy, 010303 astronomy & astrophysics, Legendre polynomials, power-spectrum analysis, Physics, large-scale structure of universe, model, 010308 nuclear & particles physics, Angular diameter distance, Astronomy and Astrophysics, Cosmology observations, acoustic-oscillations, Galaxy, Redshift, Baryon, Space and Planetary Science, cosmology: observations, digital sky survey, galaxies: distances and redshifts, cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the anisotropic clustering of emission line galaxies (ELGs) from the Sloan Digital Sky Survey IV (SDSS-IV) extended Baryon Oscillation Spectroscopic Survey (eBOSS) Data Release 16 (DR16). Our sample is composed of 173,736 ELGs covering an area of 1170 deg$^2$ over the redshift range $0.6 \leq z \leq 1.1$. We use the Convolution Lagrangian Perturbation Theory in addition to the Gaussian Streaming Redshift-Space Distortions to model the Legendre multipoles of the anisotropic correlation function. We show that the eBOSS ELG correlation function measurement is affected by the contribution of a radial integral constraint that needs to be modelled to avoid biased results. To mitigate the effect from unknown angular systematics, we adopt a modified correlation function estimator that cancels out the angular modes from the clustering. At the effective redshift, $z_{\rm eff}=0.85$, including statistical and systematical uncertainties, we measure the linear growth rate of structure $f\sigma_8(z_{\rm eff}) = 0.35\pm0.10$, the Hubble distance $D_H(z_{\rm eff})/r_{\rm drag} = 19.1^{+1.9}_{-2.1}$ and the comoving angular diameter distance $D_M(z_{\rm eff})/r_{\rm drag} = 19.9\pm1.0$. These results are in agreement with the Fourier space analysis, leading to consensus values of: $f\sigma_8(z_{\rm eff}) = 0.315\pm0.095$, $D_H(z_{\rm eff})/r_{\rm drag} = 19.6^{+2.2}_{-2.1}$ and $D_M(z_{\rm eff})/r_{\rm drag} = 19.5\pm1.0$, consistent with $\Lambda$CDM model predictions with Planck parameters., Comment: A summary of all SDSS BAO and RSD measurements with accompanying legacy figures can be found here: https://www.sdss.org/science/final-bao-and-rsd-measurements/ . The full cosmological interpretation of these measurements can be found here: https://www.sdss.org/science/cosmology-results-from-eboss/

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