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2. Emission line predictions for mock galaxy catalogues: a new differentiable and empirical mapping from DESI.

Author

Khederlarian, Ashod, Newman, Jeffrey A, Andrews, Brett H, Dey, Biprateep, Moustakas, John, Hearin, Andrew, Juneau, Stéphanie, Tortorelli, Luca, Gruen, Daniel, Hahn, ChangHoon, Canning, Rebecca E A, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Fanning, Kevin, Ferraro, Simone, and Forero-Romero, Jaime

Subjects
SPECTRAL energy distribution, AUTOMATIC differentiation, GALAXIES, STELLAR populations, DARK energy
Abstract

We present a simple, differentiable method for predicting emission line strengths from rest-frame optical continua using an empirically determined mapping. Extensive work has been done to develop mock galaxy catalogues that include robust predictions for galaxy photometry, but reliably predicting the strengths of emission lines has remained challenging. Our new mapping is a simple neural network implemented using the JAX Python automatic differentiation library. It is trained on Dark Energy Spectroscopic Instrument Early Release data to predict the equivalent widths (EWs) of the eight brightest optical emission lines (including H α, H β, [O ii ], and [O iii ]) from a galaxy's rest-frame optical continuum. The predicted EW distributions are consistent with the observed ones when noise is accounted for, and we find Spearman's rank correlation coefficient ρ s > 0.87 between predictions and observations for most lines. Using a non-linear dimensionality reduction technique, we show that this is true for galaxies across the full range of observed spectral energy distributions. In addition, we find that adding measurement uncertainties to the predicted line strengths is essential for reproducing the distribution of observed line-ratios in the BPT diagram. Our trained network can easily be incorporated into a differentiable stellar population synthesis pipeline without hindering differentiability or scalability with GPUs. A synthetic catalogue generated with such a pipeline can be used to characterize and account for biases in the spectroscopic training sets used for training and calibration of photo- z 's, improving the modelling of systematic incompleteness for the Rubin Observatory LSST and other surveys. [ABSTRACT FROM AUTHOR]

Published
2024
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4. Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I.Sample from the Early Data

Author

Guo, Wei-Jian, Zou, Hu, Fawcett, Victoria Anne, Canning, Rebecca, Juneau, Stephanie, Davis, Tamara M., Alexander, David M., Jiang, Linhua, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Fanning, Kevin, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Honscheid, Klaus, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Pan, Zhiwei, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Siudek, Małgorzata, Sanchez, Eusebio, Schubnell, Michael, Seo, Hee-Jong, Sui, Jipeng, Tarlé, Gregory, and Zhou, Zhiming

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

Changing-look Active Galactic Nuclei (CL AGN) can be generally confirmed by the emergence (turn-on) or disappearance (turn-off) of broad emission lines, associated with a transient timescale (about $100\sim5000$ days) that is much shorter than predicted by traditional accretion disk models. We carry out a systematic CL AGN search by cross-matching the spectra coming from the Dark Energy Spectroscopic Instrument and the Sloan Digital Sky Survey. Following previous studies, we identify CL AGN based on $\rm{H}\alpha $, $\rm{H}\beta$, and Mg\,{\sc ii} at $z\leq0.75$ and Mg\,{\sc ii}, C\,{\sc iii}], and C\,{\sc iv} at $z>0.75$. We present 130 CL AGN based on visual inspection and three selection criteria, including 2 $\rm{H}\alpha$, 45 $\rm{H}\beta$, 38 Mg\,{\sc ii}, 61 C\,{\sc iii}], and 10 C\,{\sc iv} CL AGN. Twenty cases show simultaneous appearances/disappearances of two broad emission lines while three AGN exhibit the concurrent appearance of three broad emission lines. We also present 91 CL AGN candidates with significant flux variation of broad emission lines but remaining strong broad components. In the confirmed CL AGN, 42 cases show additional CL candidate features for different lines. In this paper, we find 1) a 95:35 ratio of a turn-on to turn-off CL AGN; 2) the highest redshift CL AGN ($z=3.56$) ever discovered; 3) an upper limit transition timescale ranging from 244 to 5762 days in the rest-frame; 4) the majority of CL AGN follow the bluer-when-brighter trend. Our results greatly increase the current CL census ($30\sim50\%$) and would be conducive to explore the underlying physical mechanism.

Published
2023

5. The DESI One-Percent Survey: Exploring A Generalized SHAM for Multiple Tracers with the UNIT Simulation

Author

Yu, Jiaxi, Zhao, Cheng, Gonzalez-Perez, Violeta, Chuang, Chia-Hsun, Brodzeller, Allyson, de Mattia, Arnaud, Kneib, Jean-Paul, Krolewski, Alex, Rocher, Antoine, Ross, Ashley, Wang, Yunchong, Yuan, Sihan, Zhang, Hanyu, Zhou, Rongpu, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Dawson, Kyle, de la Macorra, Alex, Doel, Peter, Fanning, Kevin, Font-Ribera, Andreu, Forero-Romero, Jaime, Gontcho, Satya Gontcho A, Honscheid, Klaus, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Manera, Marc, Martini, Paul, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Percival, Will, Poppett, Claire, Raichoor, Anand, Rossi, Graziano, Seo, Hee-Jong, Tarlé, Gregory, Zhou, Zhimin, Zou, Hu, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

International audience; We perform a SubHalo Abundance Matching (SHAM) study with two algorithms: {$\sigma, V_{\rm ceil}, v_{\rm smear}$}-SHAM and {$\sigma, V_{\rm ceil},f_{\rm sat}$}-SHAM. These are designed to reproduce the clustering on 5--30$\,h^{-1}\,{\rm Mpc}$ of DESI One Percent Survey targets: Luminous Red Galaxies (LRGs), Emission Line Galaxies (ELGs) and Quasi-Stellar Objects (QSOs) at $0.4

Published
2023

6. Analysis of the impact of broad absorption lines on quasar redshift measurements with synthetic observations.

Author

García, Luz Ángela, Martini, Paul, Gonzalez-Morales, Alma X, Font-Ribera, Andreu, Herrera-Alcantar, Hiram K, Aguilar, Jessica Nicole, Ahlen, Steve, Brooks, David, de la Macorra, Axel, Doel, Peter, Forero-Romero, Jaime E, Guy, Julien, Kisner, Theodore, Landriau, Martin, Miquel, Ramon, Moustakas, John, Nie, Jundan, Poppett, Claire, Tarlé, Gregory, and Zhou, Zhimin

Subjects
REDSHIFT, DARK energy, QUASARS, SIGNAL-to-noise ratio, ABSORPTION, GALAXIES, PHYSICAL cosmology
Abstract

Accurate quasar classifications and redshift measurements are increasingly important to precision cosmology experiments. Broad absorption line (BAL) features are present in 15–20 per cent of all quasars, and these features can introduce systematic redshift errors, and in extreme cases produce misclassifications. We quantitatively investigate the impact of BAL features on quasar classifications and redshift measurements with synthetic spectra that were designed to match observations by the Dark Energy Spectroscopic Instrument (DESI) survey. Over the course of 5 yr, DESI aims to measure spectra for 40 million galaxies and quasars, including nearly three million quasars. Our synthetic quasar spectra match the signal-to-noise ratio and redshift distributions of the first year of DESI observations, and include the same synthetic quasar spectra both with and without BAL features. We demonstrate that masking the locations of the BAL features decreases the redshift errors by about 1 per cent and reduces the number of catastrophic redshift errors by about 80 per cent. We conclude that identifying and masking BAL troughs should be a standard part of the redshift determination step for DESI and other large-scale spectroscopic surveys of quasars. [ABSTRACT FROM AUTHOR]

Published
2023
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7. Siena Galaxy Atlas 2020.

Author

Moustakas, John, Lang, Dustin, Dey, Arjun, Juneau, Stéphanie, Meisner, Aaron, Myers, Adam D., Schlafly, Edward F., Schlegel, David J., Valdes, Francisco, Weaver, Benjamin A., and Zhou, Rongpu

Published
2023
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8. The Optical Corrector for the Dark Energy Spectroscopic Instrument

Author

Miller, Timothy N., Doel, Peter, Gutierrez, Gaston, Besuner, Robert, Brooks, David, Gallo, Giuseppe, Heetderks, Henry, Jelinsky, Patrick, Kent, Stephen M., Lampton, Michael, Levi, Michael, Liang, Ming, Meisner, Aaron, Sholl, Michael J., Silber, Joseph Harry, Sprayberry, David, Aguilar, Jessica Nicole, de la Macorra, Axel, Eisenstein, Daniel, Fanning, Kevin, Font-Ribera, Andreu, Gaztanaga, Enrique, Gontcho, Satya Gontcho A, Honscheid, Klaus, Jimenez, Jorge, Joyce, Dick, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Guillou, Laurent Le, Magneville, Christophe, Martini, Paul, Miquel, Ramon, Moustakas, John, Nie, Jundan, Percival, Will, Poppett, Claire, Prada, Francisco, Rossi, Graziano, Schlegel, David, Schubnell, Michael, Seo, Hee-Jong, Sharples, Ray, Tarle, Gregory, Vargas-Magana, Mariana, Zhou, Zhimin, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and DESI

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Dark Energy Spectroscopic Instrument (DESI) is currently measuring the spectra of 40\,million galaxies and quasars, the largest such survey ever made to probe the nature of cosmological dark energy. The 4-meter Mayall telescope at Kitt Peak National Observatory has been adapted for DESI, including the construction of a 3.2-degree diameter prime focus corrector that focuses astronomical light onto a 0.8-meter diameter focal surface with excellent image quality over the DESI bandpass of 360-980nm. The wide-field corrector includes six lenses, as large as 1.1-meters in diameter and as heavy as 237\,kilograms, including two counter-rotating wedged lenses that correct for atmospheric dispersion over Zenith angles from 0 to 60 degrees. The lenses, cells, and barrel assembly all meet precise alignment tolerances on the order of tens of microns. The barrel alignment is maintained throughout a range of observing angles and temperature excursions in the Mayall dome by use of a hexapod, which is itself supported by a new cage, ring, and truss structure. In this paper we describe the design, fabrication, and performance of the new corrector and associated structure, focusing on how they meet DESI requirements. In particular we describe the prescription and specifications of the lenses, design choices and error budgeting of the barrel assembly, stray light mitigations, and integration and test at the Mayall telescope. We conclude with some validation highlights that demonstrate the successful corrector on-sky performance, and list some lessons learned during the multi-year fabrication phase., Comment: 68 pages, 56 figures, 22 tables. Submitted to the Astronomical Journal

Published
2023

9. GTC Follow-up Observations of Very Metal-Poor Star Candidates from DESI

Author

Prieto, Carlos Allende, Aguado, David S., Hernández, Jonay I. González, Rebolo, Rafael, Najita, Joan, Manser, Christopher J., Rockosi, Constance, Slepian, Zachary, Mezcua, Mar, Valluri, Monica, Ezzeddine, Rana, Koposov, Sergey E., Cooper, Andrew P., Dey, Arjun, Gänsicke, Boris T., Li, Ting S., Cunha, Katia, Zou, Siwei, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, Cole, Shaun, Eftekharzadeh, Sarah, Fanning, Kevin, Forero-Romero, Jaime, Gontcho, Satya Gontcho A, Honscheid, Klaus, Jablonka, Pascale, Kehoe, Robert, Kisner, Theodore, Landriau, Martin, de la Macorra, Axel, Meisner, Aaron, Miquel, Ramón, Moustakas, John, Nie, Jundan, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Sánchez, Eusebio, Schubnell, Michael, Sharples, Ray, Siudek, Malgorzata, Smith, Verne V., Tarlé, Gregory, Vincenzo, Fiorenzo, Weaver, Benjamin Alan, Zhou, Zhimin, and Zou, Hu

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The observations from the Dark Energy Spectroscopic Instrument (DESI) will significantly increase the numbers of known extremely metal-poor stars by a factor of ~ 10, improving the sample statistics to study the early chemical evolution of the Milky Way and the nature of the first stars. In this paper we report high signal-to-noise follow-up observations of 9 metal-poor stars identified during the DESI commissioning with the Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy (OSIRIS) instrument on the 10.4m Gran Telescopio Canarias (GTC). The analysis of the data using a well-vetted methodology confirms the quality of the DESI spectra and the performance of the pipelines developed for the data reduction and analysis of DESI data., 13 pages, 4 figures, to be submitted to ApJ, data available from https://doi.org/10.5281/zenodo.8020841

Published
2023

10. PROVABGS: The Probabilistic Stellar Mass Function of the BGS One-Percent Survey

Author

Hahn, ChangHoon, Aguilar, Jessica Nicole, Alam, Shadab, Ahlen, Steven, Brooks, David, Cole, Shaun, de la Macorra, Axel, Doel, Peter, Font-Ribera, Andreu A., Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Honscheid, Klaus, Huang, Song, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Poppett, Claire, Rossi, Graziano, Saintonge, Amélie, Sanchez, Eusebio, Saulder, Christoph, Schubnell, Michael, Seo, Hee-Jong, Siudek, Małgorzata, Speranza, Federico, Tarlé, Gregory, Weaver, Benjamin A., Wechsler, Risa H., Yuan, Sihan, Zhou, Zhimin, and Zou, Hu

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the probabilistic stellar mass function (pSMF) of galaxies in the DESI Bright Galaxy Survey (BGS), observed during the One-Percent Survey. The One-Percent Survey was one of DESI's survey validation programs conducted from April to May 2021, before the start of the main survey. It used the same target selection and similar observing strategy as the main survey and successfully observed the spectra and redshifts of 143,017 galaxies in the $r < 19.5$ magnitude-limited BGS Bright sample and 95,499 galaxies in the fainter surface brightness and color selected BGS Faint sample over $z < 0.6$. We derive pSMFs from posteriors of stellar mass, $M_*$, inferred from DESI photometry and spectroscopy using the Hahn et al. (2022a; arXiv:2202.01809) PRObabilistic Value-Added BGS (PROVABGS) Bayesian SED modeling framework. We use a hierarchical population inference framework that statistically and rigorously propagates the $M_*$ uncertainties. Furthermore, we include correction weights that account for the selection effects and incompleteness of the BGS observations. We present the redshift evolution of the pSMF in BGS as well as the pSMFs of star-forming and quiescent galaxies classified using average specific star formation rates from PROVABGS. Overall, the pSMFs show good agreement with previous stellar mass function measurements in the literature. Our pSMFs showcase the potential and statistical power of BGS, which in its main survey will observe >100$\times$ more galaxies. Moreover, we present the statistical framework for subsequent population statistics measurements using BGS, which will characterize the global galaxy population and scaling relations at low redshifts with unprecedented precision., 25 pages, 12 figures; data used to generate figures is available at https://doi.org/10.5281/zenodo.8018936; submitted to ApJ

Published
2023

11. Target Selection for the DESI Peculiar Velocity Survey

Author

Saulder, Christoph, Howlett, Cullan, Douglass, Kelly A., Said, Khaled, BenZvi, Segev, Ahlen, Steven, Aldering, Greg, Bailey, Stephen, Brooks, David, Davis, Tamara, de la Macorra, Axel, Dey, Arjun, Font-Ribera, Andreu, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Honscheid, Klaus, Kim, Alex G., Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Levi, Michael E., Lucey, John, Meisner, Aaron M., Miquel, Ramon, Moustakas, John, Myers, Adam D., Palanque-Delabrouille, Nathalie, Percival, Will, Poppett, Claire, Prada, Francisco, Qin, Fei, Schubnell, Michael, Tarlé, Gregory, Magaña, Mariana Vargas, Weaver, Benjamin Alan, Zhou, Rongpu, Zhou, Zhimin, Zou, Hu, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the target selection and characteristics of the DESI Peculiar Velocity Survey, the largest survey of peculiar velocities (PVs) using both the fundamental plane (FP) of galaxies and the Tully-Fisher (TF) relationship planned to date. We detail how we identify suitable early-type galaxies for the FP and suitable late-type galaxies for the TF relation using the photometric data provided by the DESI Legacy Imaging Survey DR9. Subsequently, we provide targets for 373 533 early-type galaxies and 118 637 late-type galaxies within the DESI 5-year footprint. We validate these photometric selections using existing morphological classifications. Furthermore, we demonstrate using survey validation data that DESI is able to measure the spectroscopic properties to sufficient precision to obtain PVs for our targets. Based on realistic DESI fiber assignment simulations and spectroscopic success rates, we predict the final DESI Peculiar Velocity Survey will obtain $\sim$133 000 FP-based and $\sim$53 000 TF-based PV measurements over an area of 14 000 $\mathrm{deg^{2}}$. Each of these components will be a factor of 4--5 larger than other recent samples. We forecast the ability of using these data to measure the clustering of galaxy positions and peculiar velocities from the combined DESI PV and Bright Galaxy Surveys (BGS), which allows for cancellation of cosmic variance at low redshifts. With these forecasts, we anticipate a $4\%$ statistical measurement on the growth rate of structure at $z, 20 pages, 15 figures, 14 tables; submitted to MNRAS

Published
2023

12. DESI z >~ 5 Quasar Survey. I. A First Sample of 400 New Quasars at z ~ 4.7-6.6

Author

Yang, Jinyi, Fan, Xiaohui, Gupta, Ansh, Myers, Adam, Palanque-Delabrouille, Nathalie, Wang, Feige, Yèche, Christophe, Aguilar, Jessica Nicole, Ahlen, Steven, Alexander, David, Brooks, David, Dawson, Kyle, de la Macorra, Axel, Dey, Arjun, Dhungana, Govinda, Fanning, Kevin, Font-Ribera, Andreu, Gontcho, Satya, Guy, Julien, Honscheid, Klaus, Juneau, Stephanie, Kisner, Theodore, Kremin, Anthony, Le Guillou, Laurent, Levi, Michael, Magneville, Christophe, Martini, Paul, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Percival, Will, Poppett, Claire, Prada, Francisco, Schlafly, Edward, Tarlé, Gregory, Magana, Mariana Vargas, Weaver, Benjamin Alan, Wechsler, Risa, Zhou, Rongpu, Zhou, Zhimin, Zou, Hu, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the first results of a high-redshift ($z$ >~ 5) quasar survey using the Dark Energy Spectroscopic Instrument (DESI). As a DESI secondary target program, this survey is designed to carry out a systematic search and investigation of quasars at $z$ >~ 5, up to redshift 6.8. The target selection is based on the DESI Legacy Imaging Surveys (the Legacy Surveys) DR9 photometry, combined with the Pan-STARRS1 data and $J$-band photometry from public surveys. A first quasar sample has been constructed from the DESI Survey Validation 3 (SV3) and first-year observations until May 2022. This sample includes more than 400 new quasars at redshift 4.7 = 5, more than one third of existing quasars previously published at this redshift. The observations so far result in an average success rate of 23% at $z$ > 4.7. The current spectral dataset has already allowed analysis of interesting individual objects (e.g., quasars with damped Ly$\alpha$ absorbers and broad absorption line features), and statistical analysis will follow the survey's completion. A set of science projects will be carried out leveraging this program, including quasar luminosity function, quasar clustering, intergalactic medium, quasar spectral properties, intervening absorbers, and properties of early supermassive black holes. Additionally, a sample of 38 new quasars at $z$ ~ 3.8-5.7 discovered from a pilot survey in the DESI SV1 is also published in this paper., Comment: 28 pages, 9 figures, and 2 tables; submitted to AAS

Published
2023

13. Target Selection and Sample Characterization for the DESI LOW-Z Secondary Target Program

Author

Darragh-Ford, Elise, Wu, John F., Mao, Yao-Yuan, Wechsler, Risa H., Geha, Marla, Forero-Romero, Jaime E., Hahn, Changhoon, Kallivayalil, Nitya, Moustakas, John, Nadler, Ethan O., Nowotka, Marta, Peek, J.E.G., Tollerud, Erik J., Weiner, Benjamin, Aguilar, J., Ahlen, S., Brooks, D., Cooper, A.P., de la Macorra, A., Dey, A., Fanning, K., Font-Ribera, A., Gontcho A. Gontcho, S., Honscheid, K., Kisner, T., Kremin, Anthony, Landriau, M., Levi, Michael E., Martini, P., Meisner, Aaron M., Miquel, R., Myers, Adam D., Nie, Jundan, Palanque-Delabrouille, N., Percival, W.J., Prada, F., Schlegel, D., Schubnell, M., Tarlé, Gregory, Vargas-Magaña, M., Zhou, Zhimin, Zou, And H., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and HEP, INSPIRE

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies
Abstract

We introduce the DESI LOW-Z Secondary Target Survey, which combines the wide-area capabilities of the Dark Energy Spectroscopic Instrument (DESI) with an efficient, low-redshift target selection method. Our selection consists of a set of color and surface brightness cuts, combined with modern machine learning methods, to target low-redshift dwarf galaxies ($z$ < 0.03) between $19 < r < 21$ with high completeness. We employ a convolutional neural network (CNN) to select high-priority targets. The LOW-Z survey has already obtained over 22,000 redshifts of dwarf galaxies (M$_* < 10^9$ M$_\odot$), comparable to the number of dwarf galaxies discovered in SDSS-DR8 and GAMA. As a spare fiber survey, LOW-Z currently receives fiber allocation for just ~50% of its targets. However, we estimate that our selection is highly complete: for galaxies at $z < 0.03$ within our magnitude limits, we achieve better than 95% completeness with ~1% efficiency using catalog-level photometric cuts. We also demonstrate that our CNN selections $z, 24 pages, 14 figures, data to reproduce figures: https://zenodo.org/record/7422591

Published
2023

14. Extending the Dynamic Range of Galaxy Outflow Scaling Relations: Massive Compact Galaxies with Extreme Outflows.

Author

Davis, Julie D., Tremonti, Christy A., Swiggum, Cameren N., Moustakas, John, Diamond-Stanic, Aleksandar M., Coil, Alison L., Geach, James E., Hickox, Ryan C., Perrotta, Serena, Petter, Grayson C., Rudnick, Gregory H., Rupke, David S. N., Sell, Paul H., and Whalen, Kelly E.

Subjects
GALAXIES, STAR formation, BLACK holes, WIND speed, OPTICAL spectra, STELLAR mass, GALAXY mergers
Abstract

We investigate galactic winds in the HizEA galaxies, a collection of 46 late-stage galaxy mergers at z = 0.4–0.8, with stellar masses of log (M * / M ⊙) = 10.4 – 11.5 , star formation rates (SFRs) of 20–500 M ⊙ yr−1, and ultra-compact (a few 100 pc) central star-forming regions. We measure their gas kinematics using the Mg ii λ λ 2796,2803 absorption lines in optical spectra from MMT, Magellan, and Keck. We find evidence of outflows in 90% of targets, with maximum outflow velocities of 550–3200 km s−1. We combine these data with ten samples from the literature to construct scaling relations for outflow velocity versus SFR, star formation surface density (ΣSFR), M *, and SFR/ M *. The HizEA galaxies extend the dynamic range of the scaling relations by a factor of ∼2–4 in outflow velocity and an order of magnitude in SFR and ΣSFR. The ensemble scaling relations exhibit strong correlations between outflow velocity, SFR, SFR/ R, and ΣSFR, and weaker correlations with M * and SFR/ M *. The HizEA galaxies are mild outliers on the SFR and M * scaling relations, but they connect smoothly with more typical star-forming galaxies on plots of outflow velocity versus SFR/ R and ΣSFR. These results provide further evidence that the HizEA galaxies' exceptional outflow velocities are a consequence of their extreme star formation conditions rather than hidden black hole activity, and they strengthen previous claims that ΣSFR is one of the most important properties governing the velocities of galactic winds. [ABSTRACT FROM AUTHOR]

Published
2023
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15. Spectroscopic needs for imaging dark energy experiments

Author

Newman, Jeffrey A., Abate, Alexandra, Abdalla, Filipe B., Allam, Sahar, Allen, Steven W., Ansari, Réza, Bailey, Stephen, Barkhouse, Wayne A., Beers, Timothy C., Blanton, Michael R., Brodwin, Mark, Brownstein, Joel R., Brunner, Robert J., Carrasco Kind, Matias, Cervantes-Cota, Jorge L., Cheu, Elliott, Chisari, Nora Elisa, Colless, Matthew, Comparat, Johan, Coupon, Jean, Cunha, Carlos E., de la Macorra, Axel, Dell’Antonio, Ian P., Frye, Brenda L., Gawiser, Eric J., Gehrels, Neil, Grady, Kevin, Hagen, Alex, Hall, Patrick B., Hearin, Andew P., Hildebrandt, Hendrik, Hirata, Christopher M., Ho, Shirley, Honscheid, Klaus, Huterer, Dragan, Ivezić, Željko, Kneib, Jean-Paul, Kruk, Jeffrey W., Lahav, Ofer, Mandelbaum, Rachel, Marshall, Jennifer L., Matthews, Daniel J., Ménard, Brice, Miquel, Ramon, Moniez, Marc, Moos, H.W., Moustakas, John, Myers, Adam D., Papovich, Casey, Peacock, John A., Park, Changbom, Rahman, Mubdi, Rhodes, Jason, Ricol, Jean-Stephane, Sadeh, Iftach, Slozar, Anže, Schmidt, Samuel J., Stern, Daniel K., Anthony Tyson, J., von der Linden, Anja, Wechsler, Risa H., Wood-Vasey, W.M., and Zentner, Andrew R.

Published
2015
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16. A Spectroscopic Road Map for Cosmic Frontier: DESI, DESI-II, Stage-5

Author

Schlegel, David J., Ferraro, Simone, Aldering, Greg, Baltay, Charles, Benzvi, Segev, Besuner, Robert, Blanc, Guillermo A., Bolton, Adam S., Bonaca, Ana, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, Derose, Joseph, Dey, Arjun, Doel, Peter, Drlica-Wagner, Alex, Fan, Xiaohui, Gutierrez, Gaston, Green, Daniel, Guy, Julien, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kollmeier, Juna A., Kremin, Anthony, Lahav, Ofer, Landriau, Martin, Lang, Dustin, Leauthaud, Alexie, Levi, Michael E., Linder, Eric V., Magneville, Christophe, Martini, Paul, Mcdonald, Patrick, Miller, Christopher J., Myers, Adam D., Newman, Jeffrey A., Nugent, Peter E., Palanque-Delabrouille, Nathalie, Padmanabhan, Nikhil, Palmese, Antonella, Poppett, Claire, Prochaska, Jason X., Raichoor, Anand, Ramirez, Solange, Sailer, Noah, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Soares-Santos, Marcelle, Tarlé, Greg, Valluri, Monica, Weaverdyck, Noah J., Wechsler, Risa H., White, Martin, Yèche, Christophe, Zhou, Rongpu, Finkbeiner, Douglas, Gontcho A. Gontcho, Satya, Moustakas, John, Ross, Ashley J., Samushia, Lado, Zaritsky, Dennis, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and DESI

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), dimension: 3, lens, redshift: high, FOS: Physical sciences, dark matter: density, cosmic background radiation, inflation: model, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), DESI, star, dark energy: density, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], density: high, quasar, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this white paper, we present an experimental road map for spectroscopic experiments beyond DESI. DESI will be a transformative cosmological survey in the 2020s, mapping 40 million galaxies and quasars and capturing a significant fraction of the available linear modes up to z=1.2. DESI-II will pilot observations of galaxies both at much higher densities and extending to higher redshifts. A Stage-5 experiment would build out those high-density and high-redshift observations, mapping hundreds of millions of stars and galaxies in three dimensions, to address the problems of inflation, dark energy, light relativistic species, and dark matter. These spectroscopic data will also complement the next generation of weak lensing, line intensity mapping and CMB experiments and allow them to reach their full potential., Contribution to Snowmass 2021

Published
2022

17. The MegaMapper: A Stage-5 Spectroscopic Instrument Concept for the Study of Inflation and Dark Energy

Author

Schlegel, David J., Kollmeier, Juna A., Aldering, Greg, Bailey, Stephen, Baltay, Charles, Bebek, Christopher, BenZvi, Segev, Besuner, Robert, Blanc, Guillermo, Bolton, Adam S., Bonaca, Ana, Bouri, Mohamed, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, Crane, Jeffrey, Demina, Regina, DeRose, Joseph, Dey, Arjun, Doel, Peter, Fan, Xiaohui, Ferraro, Simone, Finkbeiner, Douglas, Font-Ribera, Andreu, Gontcho, Satya Gontcho A, Green, Daniel, Gutierrez, Gaston, Guy, Julien, Heetderks, Henry, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kremin, Anthony, Kronig, Luzius, Konidaris, Nick, Lahav, Ofer, Lampton, Michael L., Landriau, Martin, Lang, Dustin, Leauthaud, Alexie, Levi, Michael E., Liguori, Michele, Linder, Eric V., Magneville, Christophe, Martini, Paul, Mateo, Mario, McDonald, Patrick, Miller, Christopher J., Moustakas, John, Myers, Adam D., Mulchaey, John, Newman, Jeffrey A., Nugent, Peter E., Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Piro, Antonella Palmese Anthony L., Poppett, Claire, Prochaska, Jason X., Pullen, Anthony R., Rabinowitz, David, Raichoor, Anand, Ramirez, Solange, Rix, Hans-Walter, Ross, Ashley J., Samushia, Lado, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Shectman, Stephen A., Schlafly, Edward F., Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Slosar, Anže, Soares-Santos, Marcelle, Tarlé, Greg, Thompson, Ian, Valluri, Monica, Wechsler, Risa H., White, Martin, Wilson, Michael J., Yèche, Christophe, Zaritsky, Dennis, Zhou, Rongpu, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
High Energy Physics - Experiment (hep-ex), DESI, galaxy: redshift, target: density, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, Astrophysics - Instrumentation and Methods for Astrophysics, dark energy, Instrumentation and Methods for Astrophysics (astro-ph.IM), High Energy Physics - Experiment
Abstract

In this white paper, we present the MegaMapper concept. The MegaMapper is a proposed ground-based experiment to measure Inflation parameters and Dark Energy from galaxy redshifts at $2, Comment: Contributed White Paper to Snowmass 2021. arXiv admin note: substantial text overlap with arXiv:1907.11171. text overlap with arXiv:2209.03585

Published
2022

18. Intrinsic alignment as an RSD contaminant in the DESI survey.

Author

Lamman, Claire, Eisenstein, Daniel, Aguilar, Jessica Nicole, Brooks, David, de la Macorra, Axel, Doel, Peter, Font-Ribera, Andreu, Gontcho A Gontcho, Satya, Honscheid, Klaus, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Levi, Michael, Miquel, Ramon, Moustakas, John, Palanque-Delabrouille, Nathalie, Poppett, Claire, Schubnell, Michael, and Tarlé, Gregory

Subjects
DARK energy, STATISTICAL correlation, LARGE scale structure (Astronomy), LENGTH measurement, QUADRUPOLES
Abstract

We measure the tidal alignment of the major axes of luminous red galaxies (LRGs) from the Legacy Imaging Survey and use it to infer the artificial redshift-space distortion signature that will arise from an orientation-dependent, surface-brightness selection in the Dark Energy Spectroscopic Instrument (DESI) survey. Using photometric redshifts to downweight the shape–density correlations due to weak lensing, we measure the intrinsic tidal alignment of LRGs. Separately, we estimate the net polarization of LRG orientations from DESI's fibre-magnitude target selection to be of order 10−2 along the line of sight. Using these measurements and a linear tidal model, we forecast a 0.5 per cent fractional decrease on the quadrupole of the two-point correlation function for projected separations of 40–80 h −1 Mpc. We also use a halo catalogue from the Abacussummit cosmological simulation suite to reproduce this false quadrupole. [ABSTRACT FROM AUTHOR]

Published
2023
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19. Kinematics, Structure, and Mass Outflow Rates of Extreme Starburst Galactic Outflows.

Author

Perrotta, Serena, Coil, Alison L., Rupke, David S. N., Tremonti, Christy A., Davis, Julie D., Diamond-Stanic, Aleksandar M., Geach, James E., Hickox, Ryan C., Moustakas, John, Rudnick, Gregory H., Sell, Paul H., Swiggum, Cameren N., and Whalen, Kelly E.

Subjects
KINEMATICS, STAR formation, STARBURSTS, TURBULENT mixing, GALACTIC evolution, COLUMNS
Abstract

We present results on the properties of extreme gas outflows in massive (M * ∼ 1011 M ⊙), compact, starburst (star formation rate, SFR∼ 200 M ⊙ yr−1) galaxies at z = 0.4–0.7 with very high star formation surface densities (ΣSFR ∼ 2000 M ⊙ yr−1 kpc−2). Using optical Keck/HIRES spectroscopy of 14 HizEA starburst galaxies, we identify outflows with maximum velocities of 820–2860 km s−1. High-resolution spectroscopy allows us to measure precise column densities and covering fractions as a function of outflow velocity and characterize the kinematics and structure of the cool gas outflow phase (T ∼ 104 K). We find substantial variation in the absorption profiles, which likely reflects the complex morphology of inhomogeneously distributed, clumpy gas and the intricacy of the turbulent mixing layers between the cold and hot outflow phases. There is not a straightforward correlation between the bursts in the galaxies' star formation histories and their wind absorption line profiles, as might naively be expected for starburst-driven winds. The lack of strong Mg ii absorption at the systemic velocity is likely an orientation effect, where the observations are down the axis of a blowout. We infer high mass outflow rates of ∼50–2200 M ⊙ yr−1, assuming a fiducial outflow size of 5 kpc, and mass loading factors of η ∼ 5 for most of the sample. While these values have high uncertainties, they suggest that starburst galaxies are capable of ejecting very large amounts of cool gas that will substantially impact their future evolution. [ABSTRACT FROM AUTHOR]

Published
2023
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20. DESI Survey Validation Spectra Reveal an Increasing Fraction of Recently Quenched Galaxies at z ∼ 1.

Author

Setton, David J., Dey, Biprateep, Khullar, Gourav, Bezanson, Rachel, Newman, Jeffrey A., Aguilar, Jessica N., Ahlen, Steven, Andrews, Brett H., Brooks, David, de la Macorra, Axel, Dey, Arjun, Eftekharzadeh, Sarah, Font-Ribera, Andreu, A Gontcho, Satya Gontcho, Kremin, Anthony, Juneau, Stephanie, Landriau, Martin, Meisner, Aaron, Miquel, Ramon, and Moustakas, John

Published
2023
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21. H??-based star formation rates in and around z ? 0.5 EDisCS clusters

Author

Cooper, Jennifer R., Rudnick, Gregory H., Brammer, Gabriel G., Desjardins, Tyler, Mann, Justin L., Weiner, Benjamin J., De Lucia, Gabriella, Desai, Vandana, Finn, Rose A., Jablonka, Pascale, Moustakas, John, Teplitz, Harry I., Vulcani, Benedetta, and Zaritsky, Dennis

Subjects
Space and Planetary Science, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We investigate the role of environment on star formation rates (SFRs) of galaxies at various cosmic densities in well-studied clusters. We present the star-forming main sequence for 163 galaxies in four EDisCS clusters in the range 0.4 < z < 0.7. We use Hubble Space Telescope/Wide Field Camera 3 observations of the H?? emission line to span three distinct local environments: the cluster core, infall region, and external field galaxies. The main sequence defined from our observations is consistent with other published H?? distributions at similar redshifts but differs from those derived from star formation tracers such as 24 ?m. We find that the H?-derived SFRs for the 67 galaxies with stellar masses greater than the mass-completeness limit of M* > 109.75?M? show little dependence on environment. At face value, the similarities in the SFR distributions in the three environments may indicate that the process of finally shutting down star formation is rapid, however, the depth of our data and size of our sample make it difficult to conclusively test this scenario. Despite having significant H?? emission, 21 galaxies are classified as UVJ-quiescent and may represent a demonstration of the quenching of star formation caught in the act.

Published
2022

22. The Target Selection Pipeline for the Dark Energy Spectroscopic Instrument

Author

Myers, Adam D., Moustakas, John, Bailey, Stephen, Weaver, Benjamin A., Cooper, Andrew P., Forero-Romero, Jaime E., Abolfathi, Bela, Alexander, David M., Brooks, David, Chaussidon, Edmond, Chuang, Chia-Hsun, Dawson, Kyle, Dey, Arjun, Dey, Biprateep, Dhungana, Govinda, Doel, Peter, Fanning, Kevin, Gaztanaga, Enrique, Gontcho, Satya Gontcho A., Gonzalez-Morales, Alma X., Hahn, Changhoon, Herrera-Alcantar, Hiram K., Honscheid, Klaus, Ishak, Mustapha, Karim, Tanveer, Kirkby, David, Kisner, Theodore, Koposov, Sergey E., Kremin, Anthony, Lan, Ting-Wen, Landriau, Martin, Levi, Michael E., Magneville, Christophe, Martini, Paul, Meisner, Aaron, Napolitano, Lucas, Newman, Jeffrey A., Palanque-Delabrouille, Nathalie, Percival, Will, Poppett, Claire, Prada, Francisco, Raichoor, Anand, Ross, Ashley J., Schlafly, Edward F., Schubnell, Michael, Tan, Ting, Tarle, Gregory, Wilson, Michael J., Yeche, Christophe, Zhou, Rongpu, Zhou, Zhimin, Zou, Hu, and HEP, INSPIRE

Subjects
[PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract

In May, 2021, the Dark Energy Spectroscopic Instrument (DESI) began a five-year survey of approximately 50 million total extragalactic and Galactic targets. The primary DESI dark-time targets are Emission Line Galaxies (ELGs), Luminous Red Galaxies (LRGs) and quasars (QSOs). In bright time, DESI will focus on two surveys known as the Bright Galaxy Survey (BGS) and the Milky Way Survey (MWS). DESI also observes a selection of "secondary" targets for bespoke science goals. This paper gives an overview of the publicly available pipeline (desitarget) used to process targets for DESI observations. Highlights include details of the different DESI survey targeting phases, the targeting ID (TARGETID) used to define unique targets, the bitmasks used to indicate a particular type of target, the data model and structure of DESI targeting files, and examples of how to access and use the desitarget codebase. This paper will also describe "supporting" DESI target classes, such as standard stars, sky locations, and random catalogs that mimic the angular selection function of DESI targets. The DESI target selection pipeline is complex and sizable -- this paper attempts to summarize the most salient information required to understand and work with DESI targeting data.

Published
2022

23. Hidden depths in the local Universe: The Stellar Stream Legacy Survey.

Author

Martínez-Delgado, David, Cooper, Andrew P., Román, Javier, Pillepich, Annalisa, Erkal, Denis, Pearson, Sarah, Moustakas, John, Laporte, Chervin F. P., Laine, Seppo, Akhlaghi, Mohammad, Lang, Dustin, Makarov, Dmitry, Borlaff, Alejandro S., Donatiello, Giuseppe, Pearson, William J., Miró-Carretero, Juan, Cuillandre, Jean-Charles, Domínguez, Helena, Roca-Fàbrega, Santi, and Frenk, Carlos S.

Subjects
MILKY Way, UNIVERSE, DWARF galaxies, TIDAL currents, STELLAR orbits, GALAXY formation
Abstract

Context. Mergers and tidal interactions between massive galaxies and their dwarf satellites are a fundamental prediction of the Lambda-cold dark matter cosmology. These events are thought to provide important observational diagnostics of non-linear structure formation. Stellar streams in the Milky Way and Andromeda are spectacular evidence for ongoing satellite disruption. However, constructing a statistically meaningful sample of tidal streams beyond the Local Group has proven a daunting observational challenge, and the full potential for deepening our understanding of galaxy assembly using stellar streams has yet to be realised. Aims. Here we introduce the Stellar Stream Legacy Survey, a systematic imaging survey of tidal features associated with dwarf galaxy accretion around a sample of ∼3100 nearby galaxies within z ∼ 0.02, including about 940 Milky Way analogues. Methods. Our survey exploits public deep imaging data from the DESI Legacy Imaging Surveys, which reach surface brightness as faint as ∼29 mag arcsec−2 in the r band. As a proof of concept of our survey, we report the detection and broad-band photometry of 24 new stellar streams in the local Universe. Results. We discuss how these observations can yield new constraints on galaxy formation theory through comparison to mock observations from cosmological galaxy simulations. These tests will probe the present-day mass assembly rate of galaxies, the stellar populations and orbits of satellites, the growth of stellar halos, and the resilience of stellar disks to satellite bombardment. [ABSTRACT FROM AUTHOR]

Published
2023
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24. The DESI PRObabilistic Value-added Bright Galaxy Survey (PROVABGS) Mock Challenge.

Author

Hahn, ChangHoon, Kwon, K. J., Tojeiro, Rita, Siudek, Malgorzata, Canning, Rebecca E. A., Mezcua, Mar, Tinker, Jeremy L., Brooks, David, Doel, Peter, Fanning, Kevin, Gaztañaga, Enrique, Kehoe, Robert, Landriau, Martin, Meisner, Aaron, Moustakas, John, Poppett, Claire, Tarle, Gregory, Weiner, Benjamin, and Zou, Hu

Subjects
SPECTRAL energy distribution, GALAXIES, PHOTOMETRY, STELLAR mass, DARK energy, STAR formation, GALAXY spectra
Abstract

The PRObabilistic Value-added Bright Galaxy Survey (PROVABGS) catalog will provide measurements of galaxy properties, such as stellar mass (M *), star formation rate (SFR), stellar metallicity (Z), and stellar age (t age), for >10 million galaxies of the Dark Energy Spectroscopic Instrument (DESI) Bright Galaxy Survey. Full posterior distributions of the galaxy properties will be inferred using state-of-the-art Bayesian spectral energy distribution (SED) modeling of DESI spectroscopy and Legacy Surveys photometry. In this work, we present the SED model, the neural emulator for the model, and the Bayesian inference framework of PROVABGS. Furthermore, we apply the PROVABGS SED modeling on realistic synthetic DESI spectra and photometry, constructed using the L-Galaxies semi-analytic model. We compare the inferred galaxy properties to the true values of the simulation using a hierarchical Bayesian framework to quantify accuracy and precision. Overall, we accurately infer the true M *, SFR, Z, and t age of the simulated galaxies. However, the priors on galaxy properties induced by the SED model have a significant impact on the posteriors, which we characterize in detail. This work also demonstrates that a joint analysis of spectra and photometry significantly improves the constraints on galaxy properties over photometry alone and is necessary to mitigate the impact of the priors. With the methodology presented and validated in this work, PROVABGS will maximize information extracted from DESI observations and extend current galaxy studies to new regimes and unlock cutting-edge probabilistic analyses. https://github.com/changhoonhahn/provabgs/ [ABSTRACT FROM AUTHOR]

Published
2023
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25. H$\alpha$-based Star Formation Rates in and around z $\sim$ 0.5 EDisCS clusters

Author

Cooper, Jennifer R., Rudnick, Gregory H., Brammer, Gabriel G., Desjardins, Tyler, Mann, Justin L., Weiner, Benjamin J., Aragón-Salamanca, Alfonso, De Lucia, Gabriella, Desai, Vandana, Finn, Rose A., Jablonka, Pascale, Jaffé, Yara L., Moustakas, John, Spérone-Longin, Damien, Teplitz, Harry I., Vulcani, Benedetta, and Zaritsky, Dennis

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We investigate the role of environment on star-formation rates of galaxies at various cosmic densities in well-studied clusters. We present the star-forming main sequence for 163 galaxies in four EDisCS clusters in the range 0.4 $$ 10$^{9.75}$M\textsubscript{\(\odot\)} show little dependence on environment. At face value, the similarities in the star-formation rate distributions in the three environments may indicate that the process of finally shutting down star formation is rapid, however, the depth of our data and size of our sample make it difficult to conclusively test this scenario. Despite having significant H$\alpha$ emission, 21 galaxies are classified as {\em UVJ}-quiescent and may represent a demonstration of the quenching of star formation caught in the act., Comment: 25 pages, 15 figures, 5 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2021

26. Reaching for the Edge I: probing the outskirts of massive galaxies with HSC, DECaLS, SDSS, and Dragonfly.

Author

((李嘉轩)), Jiaxuan Li, ((黄崧)), Song Huang, Leauthaud, Alexie, Moustakas, John, Danieli, Shany, Greene, Jenny E, Abraham, Roberto, Ardila, Felipe, Kado-Fong, Erin, Lokhorst, Deborah, Lupton, Robert, and Price, Paul

Subjects
GALAXIES, DRAGONFLIES, PHOTOMETRY, STELLAR mass, DARK energy, SURFACE brightness (Astronomy), GALAXY clusters
Abstract

The outer light (stellar haloes) of massive galaxies has recently emerged as a possible low scatter tracer of dark matter halo mass. To test the robustness of outer light measurements across different data sets, we compare the 1D azimuthally averaged surface brightness profiles of massive galaxies using four independent data sets: the Hyper Suprime-Cam survey (HSC), the Dark Energy Camera Legacy Survey (DECaLS), the Sloan Digital Sky Survey (SDSS), and the Dragonfly Wide Field Survey (Dragonfly). We test the sky subtraction and proposed corrections for HSC and DECaLS. For galaxies at z < 0.05, Dragonfly has the best control of systematics, reaching surface brightness levels of μ r ≈ 30 mag arcsec−2. At 0.19 < z < 0.50, HSC can reliably recover individual surface brightness profiles to μ r ≈ 28.5 mag arcsec−2 (R  = 100–150 kpc in semimajor axis). In a statistical sense, DECaLS agrees with HSC to R > 200 kpc. DECaLS and HSC measurements of the stellar mass contained within 100 kpc agree within 0.05 dex. Finally, we use weak lensing to show that measurements of outer light with DECaLS at 0.19 < z < 0.50 show a similar promise as HSC as a low scatter proxy of halo mass. The tests and results from this paper represent an important step forward for accurate measurements of the outer light of massive galaxies and demonstrate that outer light measurements from DECam imaging will be a promising method for finding galaxy clusters. [ABSTRACT FROM AUTHOR]

Published
2022
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27. Overview of the DESI Legacy Imaging Surveys

Author

Dey, Arjun, Schlegel, David J., Lang, Dustin, Blum, Robert, Burleigh, Kaylan, Fan, Xiaohui, Findlay, Joseph R., Finkbeiner, Doug, Herrera, David, Juneau, Stephanie, Landriau, Martin, Levi, Michael, McGreer, Ian, Meisner, Aaron, Myers, Adam D., Moustakas, John, Nugent, Peter, Patej, Anna, Schlafly, Edward F., Walker, Alistair R., Valdes, Francisco, Weaver, Benjamin A., Yèche, Christophe, Zou, Hu, Zhou, Xu, Abareshi, Behzad, Abbott, T. M. C., Abolfathi, Bela, Aguilera, C., Alam, Shadab, Allen, Lori, Alvarez, A., Annis, James, Ansarinejad, Behzad, Aubert, Marie, Beechert, Jacqueline, Bell, Eric F., BenZvi, Segev Y., Beutler, Florian, Bielby, Richard M., Bolton, Adam S., Briceño, César, Buckley-Geer, Elizabeth J., Butler, Karen, Calamida, Annalisa, Carlberg, Raymond G., Carter, Paul, Casas, Ricard, Castander, Francisco J., Choi, Yumi, Comparat, Johan, Cukanovaite, Elena, Delubac, Timothee, DeVries, Kaitlin, Dey, Sharmila, Dhungana, Govinda, Dickinson, Mark, Ding, Zhejie, Donaldson, John B., Duan, Yutong, Duckworth, Christopher J., Eftekharzadeh, Sarah, Eisenstein, Daniel J., Etourneau, Thomas, Fagrelius, Parker A., Farihi, Jay, Fitzpatrick, Mike, Font-Ribera, Andreu, Fulmer, Leah, Gansicke, Boris T., Gaztanaga, Enrique, George, Koshy, Gerdes, David W., Gontcho, Satya Gontcho A., Gorgoni, Claudio, Green, Gregory, Guy, Julien, Harmer, Diane, Hernandez, M., Honscheid, Klaus, Lijuan, Huang, W., James, David, Jannuzi, Buell T., Jiang, Linhua, Joyce, Richard, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kneib, Jean-Paul, Kueter-Young, Andrea, Lan, Ting-Wen, Lauer, Tod, Guillou, Laurent Le, Suu, Auguste Le Van, Lee, Jae Hyeon, Lesser, Michael, Levasseur, Laurence Perreault, Li, Ting S., Mann, Justin L., Marshall, Bob, Martinez-Vazquez, C. E., Martini, Paul, Bourboux, Helion du Mas des, McManus, Sean, Meier, Tobias Gabriel, Menard, Brice, Metcalfe, Nigel, Munoz-Gutierrez, Andrea, Najita, Joan, Napier, Kevin, Narayan, Gautham, Newman, Jeffrey A., Nie, Jundan, Nord, Brian, Norman, Dara J., Olsen, Knut A. G., Paat, Anthony, Palanque-Delabrouille, Nathalie, Peng, Xiyan, Poppett, Claire L., Poremba, Megan R., Prakash, Abhishek, Rabinowitz, David, Raichoor, Anand, Rezaie, Mehdi, Robertson, A. N., Roe, Natalie A., Ross, Ashley J., Ross, Nicholas P., Rudnick, Gregory, Safonova, Sasha, Saha, Abhijit, Sanchez, F. Javier, Savary, Elodie, Schweiker, Heidi, Scott, Adam, Seo, Hee-Jong, Shan, Huanyuan, Silva, David R., Slepian, Zachary, Soto, Christian, Sprayberry, David, Staten, Ryan, Stillman, Coley M., Stupak, Robert J., Summers, David L., Tie, Suk Sien, Tirado, H., Vargas-Magana, Mariana, Vivas, A. Katherina, Wechsler, Risa H., Williams, Doug, Yang, Jinyi, Yang, Qian, Yapici, Tolga, Zaritsky, Dennis, Zenteno, A., Zhang, Kai, Zhang, Tianmeng, Zhou, Rongpu, Zhou, Zhimin, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Universidad Antonio Nariño (UAN), 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, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, National University of Defense Technology [China], 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), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), National Optical Astronomy Observatory (NOAO), Columbia University [New York], Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Biologie des Interactions Neurones / Glie, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), University of Arizona, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), 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), Sorbonne Université (SU), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), 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), Institut Lagrange de Paris, Chimie, Modélisation et Imagerie pour la Biologie [Orsay], Université Paris-Sud - Paris 11 (UP11)-Institut Curie [Paris]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Computer Vision Center (Centre de visio per computador) (CVC), Universitat Autònoma de Barcelona (UAB), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), 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, Ministry of Education Key Laboratory of Protein Sciences, Center for Structural Biology, Laboratoire de Tribologie et Dynamique des Systèmes (LTDS), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE)-Ecole Nationale d'Ingénieurs de Saint Etienne (ENISE)-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), Universidad Autonoma de Madrid (UAM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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)-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 de Lyon-Université de Lyon-École Nationale des Travaux Publics de l'État (ENTPE)-Ecole Nationale d'Ingénieurs de Saint Etienne-Centre National de la Recherche Scientifique (CNRS), National Natural Science Foundation of China, Department of Energy (US), National Energy Research Scientific Computing Center (US), National Science Foundation (US), National Optical Astronomy Observatory (US), Lawrence Berkeley National Laboratory, Harvard University, Dey, Arjun, Schlegel, David J., Lang, Dustin, Blum, Robert, Fan, Xiaohui, Finkbeiner, Douglas, Herrera, David, Juneau, Stephanie, Landriau, Martin, Levi, Michael, McGreer, Ian, Meisner, Aaron, Moustakas, John, Nugent, Peter, Schlafly, Edward F., Walker, Alistair, Valdés, Francisco, Zou, Hu, Abolfathi, Bela, Allen, Lori, Annis, James, Ansarinejad, Behzad, Bell, Eric F., BenZvi, Segev, Beutler, Florian, Calamida, Annalisa, Carlberg, Raymond G., Casas, Richard, Castander, Francisco J., Choi, Yumi, Dickinson, Mark, Duan, Yutong, Fagrelius, Parker, Farihi, Jay, Fulmer, Leah, Gaztañaga, Enrique, George, Koshy, Gerdes, David W., Green, Gregory, James, David J., Jannuz, Buell T., Jiang, Linhua, Joyce, Richard, Karkar, Sonia, Kehoe, Robert, Lan, Ting-Wen, Lauer, Tod R., Le Guillou, Laurent, Lesser, Michael, Marshall, Robert, Martini, Paul, Mas des Bourboux, Hélion du, Metcalfe, Nigel, Narayan, Gautham, Newman, Jeffrey A., Nord, Brian, Olsen, Knut, Prakash, Abhishek, Ross, Nicholas P., Rudnick, Gregory, Safonova, Sasha, Saha, Abhijit, Schweiker, Heidi, Silva, David R., Sien, Suk, Vivas, Kathy, Yang, Jinyi, Yang, Qian, Yapici, Tolga, Zaritsky, Dennis, Zhang, Kai, Zhang, Tianmeng, Zhou, Rongpu, University of St Andrews. School of Physics and Astronomy, Dey, Arjun [0000-0002-4928-4003], Schlegel, David J. [0000-0002-5042-5088], Lang, Dustin [0000-0002-1172-0754], Blum, Robert [0000-0002-8622-4237], Fan, Xiaohui [0000-0003-3310-0131], Finkbeiner, Douglas [0000-0003-2808-275X], Herrera, David [0000-0003-2092-6727], Juneau, Stephanie [0000-0002-0000-2394], Landriau, Martin [0000-0003-1838-8528], Levi, Michael [0000-0003-1887-1018], McGreer, Ian [0000-0002-3461-5228], Meisner, Aaron [0000-0002-1125-7384], Moustakas, John [0000-0002-2733-4559], Nugent, Peter [0000-0002-3389-0586], Schlafly, Edward F. [0000-0002-3569-7421], Walker, Alistair [0000-0002-7123-8943], Valdés, Francisco [0000-0001-5567-1301], Zou, Hu [0000-0002-6684-3997], Abolfathi, Bela [0000-0003-1820-8486], Allen, Lori [0000-0002-7789-5119], Annis, James [0000-0002-0609-3987], Ansarinejad, Behzad [0000-0002-6443-3396], Bell, Eric F. [0000-0002-5564-9873], BenZvi, Segev [0000-0001-5537-4710], Beutler, Florian [0000-0003-0467-5438], Calamida, Annalisa [0000-0002-0882-7702], Carlberg, Raymond G. [0000-0002-7667-0081], Casas, Richard [0000-0002-8165-5601], Castander, Francisco J. [0000-0001-7316-4573], Choi, Yumi [0000-0003-1680-1884], Dickinson, Mark [0000-0001-5414-5131], Duan, Yutong [0000-0002-2611-0895], Fagrelius, Parker [0000-0001-6974-5826], Farihi, Jay [0000-0003-1748-602X], Fulmer, Leah [0000-0001-9247-7794], Gaztañaga, Enrique [0000-0001-9632-0815], George, Koshy [0000-0002-1734-8455], Gerdes, David W. [0000-0001-6942-2736], Green, Gregory [0000-0001-5417-2260], James, David J. [0000-0001-5160-4486], Jannuz, Buell T. [0000-0002-1578-6582], Jiang, Linhua [0000-0003-4176-6486], Joyce, Richard [0000-0003-0201-5241], Karkar, Sonia [0000-0003-2832-777X], Kehoe, Robert [0000-0002-7101-697X], Lan, Ting-Wen [0000-0001-8857-7020], Lauer, Tod R. [0000-0003-3234-7247], Le Guillou, Laurent [0000-0001-7178-8868], Lesser, Michael [0000-0002-7199-0537], Marshall, Robert [0000-0002-6880-9987], Martini, Paul [0000-0002-4279-4182], Mas des Bourboux, Hélion du [0000-0001-8955-3573], Metcalfe, Nigel [0000-0001-9034-4402], Narayan, Gautham [0000-0001-6022-0484], Newman, Jeffrey A. [0000-0001-8684-2222], Nord, Brian [0000-0001-6706-8972], Olsen, Knut [0000-0002-7134-8296], Prakash, Abhishek [0000-0003-4451-4444], Ross, Nicholas P. [0000-0003-1830-6473], Rudnick, Gregory [0000-0001-5851-1856], Safonova, Sasha [0000-0002-2240-7421], Saha, Abhijit [0000-0002-6839-4881], Schweiker, Heidi [0000-0001-9580-4869], Silva, David R. [0000-0002-7678-2155], Sien, Suk [0000-0002-5249-1353], Vivas, Kathy [0000-0003-4341-6172], Yang, Jinyi [0000-0001-5287-4242], Yang, Qian [0000-0002-6893-3742], Yapici, Tolga [0000-0002-5306-4804], Zaritsky, Dennis [0000-0002-5177-727X], Zhang, Kai [0000-0002-9808-3646], Zhang, Tianmeng [0000-0002-8531-5161], Zhou, Rongpu [0000-0001-5381-4372], Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and 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)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, halo, FOS: Physical sciences, Surveys, 01 natural sciences, milky-way tomography, Footprint, Software, surveys, Observatory, 0103 physical sciences, QB Astronomy, redshift distributions, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, dark energy survey, STFC, QB, 0105 earth and related environmental sciences, Remote sensing, media_common, business.industry, RCUK, Astronomy and Astrophysics, cosmos, 3rd-DAS, Probabilistic inference, Galactic plane, streams, Photometry (astronomy), Space and Planetary Science, Sky, Satellite, digital sky survey, galaxy, Catalogs, Astrophysics - Instrumentation and Methods for Astrophysics, business, sdss, sextractor, catalogs, Geology, astro-ph.IM
Abstract

The DESI Legacy Imaging Surveys (http://legacysurvey.org/) are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image ≈14,000 deg2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamically adjusting the exposure times and pointing selection during observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering a catalog, constructed by using a probabilistic inference-based approach to estimate source shapes and brightnesses. The catalog includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4, 4.6, 12, and 22 μm) observed by the Wide-field Infrared Survey Explorer satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project., The BASS is also supported by the External Cooperation Program of Chinese Academy of Sciences (Grant # 114A11KYSB20160057), and Chinese National Natural Science Foundation (Grant # 11433005). The Legacy Surveys imaging of the DESI footprint is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under Contract No. DE-AC02- 05CH11231, by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract; and by the U.S. National Science Foundation, Division of Astronomical Sciences under Contract No. AST-0950945 to NOAO. Travel and other support for the DECaLS and MzLS projects is provided by the National Optical Astronomy Observatory, the Lawrence Berkeley National Laboratory, and the DESI Project. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013) / ERC Grant Agreement n. 320964 (WDTracer). J. Moustakas gratefully acknowledges support from the National Science Foundation grant AST1616414. A. Dey thanks the Radcliffe Institute for Advanced Study for their generous support during the year these surveys were initiated. A. Dey, D. J. Schlegel, and D. Lang thank the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293, for their hospitality and support during summer 2015 during which part of this work was conducted.

Published
2019

28. Three Gravitationally Lensed Supernovae Behind Clash Galaxy Clusters

Author

Patel, Brandon, McCully, Curtis, Jha, Saurbh W, Rodney, Steven A, Jones, David O, Graur, Or, Merten, Julian, Zitrin, Adi, Riess, Adam G, Matheson, Thomas, Sako, Masao, Holoien, Thomas W. -S, Postman, Marc, Coe, Dan, Bartelmann, Matthias, Balestra, Italo, Benitez, Narciso, Bouwens, Rychard, Bradley, Larry, Broadhurst, Tom, Cenko, Stephen Bradley, Donahue, Megan, Filippenko, Alexei V, Ford, Holland, Garnavich, Peter, Grillo, Claudio, Infante, Leopoldo, Jouvel, Stephanie, Kelson, Daniel, Koekemoer, Anton, Lahav, Ofer, Lemze, Doron, Maoz, Dan, Medezinski, Elinor, Melchior, Peter, Meneghetti, Massimo, Molino, Alberto, Moustakas, John, Moustakas, Leonidas A, Nonino, Mario, Rosati, Piero, Seitz, Stella, Strolger, Louis G, Umetsu, Keiichi, and Zheng, Wei

Subjects
Astronomy, Astrophysics
Abstract

We report observations of three gravitationally lensed supernovae (SNe) in the Cluster Lensing And Supernova survey with Hubble (CLASH) Multi-Cycle Treasury program. These objects, SN CLO12Car (z = 1.28), SN CLN12Did (z = 0.85), and SN CLA11Tib (z = 1.14), are located behind three different clusters, MACSJ1720.2+3536 (z = 0.391), RXJ1532.9+3021 (z = 0.345), and A383 (z = 0.187), respectively. Each SN was detected in Hubble Space Telescope optical and infrared images. Based on photometric classification, we find that SNe CLO12Car and CLN12Did are likely to be Type Ia supernovae (SNe Ia), while the classification of SN CLA11Tib is inconclusive. Using multi-color light-curve fits to determine a standardized SN Ia luminosity distance, we infer that SN CLO12Car was approx. 1.0 +/- 0.2 mag brighter than field SNe Ia at a similar redshift and ascribe this to gravitational lens magnification. Similarly, SN CLN12Did is approx. 0.2 +/- 0.2 mag brighter than field SNe Ia. We derive independent estimates of the predicted magnification from CLASH strong+weak-lensing maps of the clusters (in magnitude units, 2.5 log10 μ): 0.83 +/- 0.16 mag for SN CLO12Car, 0.28 +/- 0.08 mag for SN CLN12Did, and 0.43 +/- 0.11 mag for SN CLA11Tib. The two SNe Ia provide a new test of the cluster lens model predictions: we find that the magnifications based on the SN Ia brightness and those predicted by the lens maps are consistent. Our results herald the promise of future observations of samples of cluster-lensed SNe Ia (from the ground or space) to help illuminate the dark-matter distribution in clusters of galaxies, through the direct determination of absolute magnifications.

Published
2014
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29. Preliminary clustering properties of the DESI BGS bright targets using DR9 Legacy Imaging Surveys.

Author

Zarrouk, Pauline, Ruiz-Macias, Omar, Cole, Shaun, Norberg, Peder, Baugh, Carlton, Brooks, David, Gaztañaga, Enrique, Kitanidis, Ellie, Kehoe, Robert, Landriau, Martin, Moustakas, John, Prada, Francisco, and Tarlé, Gregory

Subjects
DARK energy, LARGE scale structure (Astronomy), ORDER statistics, DATA release, GALAXIES
Abstract

We characterize the selection cuts and clustering properties of a magnitude-limited sample of bright galaxies that is part of the Bright Galaxy Survey (BGS) of the Dark Energy Spectroscopic Instrument (DESI) using the ninth data release of the Legacy Imaging Surveys (DR9). We describe changes in the DR9 selection compared to the DR8 one and we also compare the DR9 selection in three distinct regions: BASS/MzLS in the north Galactic Cap (NGC), DECaLS in the NGC, and DECaLS in the south Galactic Cap (SGC). We investigate the systematics associated with the selection and assess its completeness by matching the BGS targets with the Galaxy and Mass Assembly (GAMA) survey. We measure the angular clustering for the overall bright sample (r mag ≤ 19.5) and as function of apparent magnitude and colour. This enables to determine the clustering strength r 0 and slope γ by fitting a power-law model that can be used to generate accurate mock catalogues for this tracer. We use a counts-in-cells technique to explore higher order statistics and cross-correlations with external spectroscopic data sets in order to check the evolution of the clustering with redshift and the redshift distribution of the BGS targets using clustering redshifts. While this work validates the properties of the BGS bright targets, the final target selection pipeline and clustering properties of the entire DESI BGS will be fully characterized and validated with the spectroscopic data of Survey Validation. [ABSTRACT FROM AUTHOR]

Published
2022
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30. A magnified young galaxy from about 500 million years after the Big Bang

Author

Zheng, Wei, Postman, Marc, Zitrin, Adi, Moustakas, John, Shu, Xinwen, Jouvel, Stephanie, Høst, Ole, Molino, Alberto, Bradley, Larry, Coe, Dan, Moustakas, Leonidas A., Carrasco, Mauricio, Ford, Holland, Benítez, Narciso, Lauer, Tod R., Seitz, Stella, Bouwens, Rychard, Koekemoer, Anton, Medezinski, Elinor, Bartelmann, Matthias, Broadhurst, Tom, Donahue, Megan, Grillo, Claudio, Infante, Leopoldo, Jha, Saurabh W., Kelson, Daniel D., Lahav, Ofer, Lemze, Doron, Melchior, Peter, Meneghetti, Massimo, Merten, Julian, Nonino, Mario, Ogaz, Sara, Rosati, Piero, Umetsu, Keiichi, and van der Wel, Arjen

Published
2012
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31. Inflation and Dark Energy from spectroscopy at z > 2

Author

Ferraro, Simone, Wilson, Michael J., Abidi, Muntazir, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bavdhankar, Chetan, Bernal, Jos�� Luis, Beutler, Florian, Biagetti, Matteo, Blanc, Guillermo A., Blazek, Jonathan, Bolton, Adam S., Borrill, Julian, Frye, Brenda, Buckley-Geer, Elizabeth, Bull, Philip, Burgess, Cliff, Byrnes, Christian T., Cai, Zheng, Castander, Francisco J, Castorina, Emanuele, Chang, Tzu-Ching, Chaves-Montero, Jon��s, Chen, Shi-Fan, Chen, Xingang, Balland, Christophe, Y��che, Christophe, Cohn, J. D., Coulton, William, Courtois, Helene, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D'Amico, Guido, Dawson, Kyle, Delabrouille, Jacques, Dey, Arjun, Dor��, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Fan, Xiaohui, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, Garc��a-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Green, Daniel, Guy, Julien, Hahn, ChangHoon, Hanany, Shaul, Handley, Will, Hathi, Nimish, Hawken, Adam J., Hern��ndez-Aguayo, C��sar, Hlo��ek, Ren��e, Huterer, Dragan, Ishak, Mustapha, Kamionkowski, Marc, Karagiannis, Dionysios, Keeley, Ryan E., Kehoe, Robert, Khatri, Rishi, Kim, Alex, Kneib, Jean-Paul, Kollmeier, Juna A., Kovetz, Ely D., Krause, Elisabeth, Krolewski, Alex, L'Huillier, Benjamin, Landriau, Martin, Levi, Michael, Liguori, Michele, Linder, Eric, Luki��, Zarija, de la Macorra, Axel, Plazas, Andr��s A., Marshall, Jennifer L., Martini, Paul, Masui, Kiyoshi, McDonald, Patrick, Meerburg, P. Daniel, Meyers, Joel, Mirbabayi, Mehrdad, Moustakas, John, Myers, Adam D., Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niz, Gustavo, Padmanabhan, Hamsa, Palunas, Povilas, Percival, Will J., Piacentini, Francesco, Pieri, Matthew M., Piro, Anthony L., Prakash, Abhishek, Rhodes, Jason, Ross, Ashley J., Rossi, Graziano, Rudie, Gwen C., Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Simon, Joshua D., Simon, Sara, Slepian, Zachary, Slosar, An��e, Sridhar, Srivatsan, Stebbins, Albert, Escoffier, Stephanie, Switzer, Eric R., Tarl��, Gregory, Trodden, Mark, Uhlemann, Cora, Uren��a-L��pez, L. Arturo, Di Valentino, Eleonora, Vargas-Maga��a, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Hong-Ming

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), astro-ph.GA, astro-ph.CO, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

The expansion of the Universe is understood to have accelerated during two epochs: in its very first moments during a period of Inflation and much more recently, at $z < 1$, when Dark Energy is hypothesized to drive cosmic acceleration. The undiscovered mechanisms behind these two epochs represent some of the most important open problems in fundamental physics. The large cosmological volume at $2 < z < 5$, together with the ability to efficiently target high-$z$ galaxies with known techniques, enables large gains in the study of Inflation and Dark Energy. A future spectroscopic survey can test the Gaussianity of the initial conditions up to a factor of ~50 better than our current bounds, crossing the crucial theoretical threshold of $��(f_{NL}^{\rm local})$ of order unity that separates single field and multi-field models. Simultaneously, it can measure the fraction of Dark Energy at the percent level up to $z = 5$, thus serving as an unprecedented test of the standard model and opening up a tremendous discovery space., Science white paper submitted to the Astro2020 Decadal Survey

Published
2019

32. Dark Matter Science in the Era of LSST

Author

Bechtol, Keith, Drlica-Wagner, Alex, Abazajian, Kevork N., Abidi, Muntazir, Adhikari, Susmita, Ali-Haïmoud, Yacine, Annis, James, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Baccigalupi, Carlo, Banerjee, Arka, Banik, Nilanjan, Bennett, Charles, Beutler, Florian, Bird, Simeon, Birrer, Simon, Biswas, Rahul, Biviano, Andrea, Blazek, Jonathan, Boddy, Kimberly K., Bonaca, Ana, Borrill, Julian, Bose, Sownak, Bovy, Jo, Frye, Brenda, Brooks, Alyson M., Buckley, Matthew R., Buckley-Geer, Elizabeth, Bulbul, Esra, Burchat, Patricia R., Burgess, Cliff, Calore, Francesca, Caputo, Regina, Castorina, Emanuele, Chang, Chihway, Chapline, George, Charles, Eric, Chen, Xingang, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert Ac, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D Amico, Guido, Davis, Tamara M., Dawson, William A., Macorra, Axel La, Valentino, Eleonora Di, Rivero, Ana Díaz, Digel, Seth, Dodelson, Scott, Doré, Olivier, Dvorkin, Cora, Eckner, Christopher, Ellison, John, Erkal, Denis, Farahi, Arya, Fassnacht, Christopher D., Ferreira, Pedro G., Flaugher, Brenna, Foreman, Simon, Friedrich, Oliver, Frieman, Joshua, García-Bellido, Juan, Gawiser, Eric, Gerbino, Martina, Maurizio Giannotti, Gill, Mandeep Ss, Gluscevic, Vera, Golovich, Nathan, Gontcho, Satya Gontcho A., González-Morales, Alma X., Grin, Daniel, Gruen, Daniel, Hearin, Andrew P., Hendel, David, Hezaveh, Yashar D., Hirata, Christopher M., Hložek, Renee, Horiuchi, Shunsaku, Jain, Bhuvnesh, Jee, M. James, Jeltema, Tesla E., Kamionkowski, Marc, Kaplinghat, Manoj, Keeley, Ryan E., Keeton, Charles R., Khatri, Rishi, Koposov, Sergey E., Koushiappas, Savvas M., Kovetz, Ely D., Lahav, Ofer, Lam, Casey, Lee, Chien-Hsiu, Li, Ting S., Liguori, Michele, Lin, Tongyan, Lisanti, Mariangela, Loverde, Marilena, Lu, Jessica R., Mandelbaum, Rachel, Mao, Yao-Yuan, Mcdermott, Samuel D., Mcnanna, Mitch, Medford, Michael, Meerburg, P. Daniel, Meyer, Manuel, Mirbabayi, Mehrdad, Mishra-Sharma, Siddharth, Marc, Moniez, More, Surhud, Moustakas, John, Muñoz, Julian B., Murgia, Simona, Myers, Adam D., Nadler, Ethan O., Necib, Lina, Newburgh, Laura, Newman, Jeffrey A., Nord, Brian, Nourbakhsh, Erfan, Nuss, Eric, O Connor, Paul, Pace, Andrew B., Padmanabhan, Hamsa, Palmese, Antonella, Peiris, Hiranya V., Peter, Annika Hg, Piacentni, Francesco, Piacentini, Francesco, Plazas, Andrés, Polin, Daniel A., Prakash, Abhishek, Prescod-Weinstein, Chanda, Read, Justin I., Ritz, Steven, Robertson, Brant E., Rose, Benjamin, Rosenfeld, Rogerio, Rossi, Graziano, Samushia, Lado, Sánchez, Javier, Sánchez-Conde, Miguel A., Schaan, Emmanuel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Shipp, Nora, Simon, Joshua D., Simon, Sara, Slatyer, Tracy R., Slosar, Anže, Sridhar, Srivatsan, Stebbins, Albert, Straniero, Oscar, Strigari, Louis E., Tait, Tim Mp, Tollerud, Erik, Troxel, Ma, Tyson, J. Anthony, Uhlemann, Cora, Urenña-López, L. Arturo, Verma, Aprajita, Vilalta, Ricardo, Walter, Christopher W., Wang, Mei-Yu, Watson, Scott, Wechsler, Risa H., Wittman, David, Xu, Weishuang, Yanny, Brian, Young, Sam, Yu, Hai-Bo, Zaharijas, Gabrijela, Zentner, Andrew R., Zuntz, Joe, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-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), 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), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, 01 natural sciences, Standard Model, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Particle mass, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, hep-ex, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, 13. Climate action, Fundamental physics, astro-ph.CO, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Particle Physics - Experiment, dark matter: parameter space, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Astrophysical observations currently provide the only robust, empirical measurements of dark matter. In the coming decade, astrophysical observations will guide other experimental efforts, while simultaneously probing unique regions of dark matter parameter space. This white paper summarizes astrophysical observations that can constrain the fundamental physics of dark matter in the era of LSST. We describe how astrophysical observations will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational interactions with the Standard Model, and compact object abundances. Additionally, we highlight theoretical work and experimental/observational facilities that will complement LSST to strengthen our understanding of the fundamental characteristics of dark matter., 11 pages, 2 figures, Science Whitepaper for Astro 2020, more information at https://lsstdarkmatter.github.io

Published
2019

33. Inflation and Dark Energy from Spectroscopy at $z > 2$

Author

Ferraro, Simone, Wilson, Michael J., Abidi, Muntazir, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bavdhankar, Chetan, Bernal, Joséluis, Beutler, Florian, Matteo Biagetti, Blanc, Guillermo A., Blazek, Jonathan, Bolton, Adam S., Borrill, Julian, Frye, Brenda, Buckley-Geer, Elizabeth, Bull, Philip, Burgess, Cliff, Byrnes, Christian T., Cai, Zheng, Castander, Francisco J., Castorina, Emanuele, Chang, Tzu-Ching, Chaves-Montero, Jonás, Chen, Shi-Fan, Chen, Xingang, Balland, Christophe, Yèche, Christophe, Cohn, J. D., Coulton, William, Courtois, Helene, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D Amico, Guido, Dawson, Kyle, Delabrouille, Jacques, Dey, Arjun, Doré, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Fan, Xiaohui, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A., Green, Daniel, Guy, Julien, Hahn, Changhoon, Hanany, Shaul, Handley, Will, Hathi, Nimish, Hawken, Adam J., Hernández-Aguayo, César, Hložek, Renée, Huterer, Dragan, Ishak, Mustapha, Kamionkowski, Marc, Karagiannis, Dionysios, Keeley, Ryan E., Kehoe, Robert, Khatri, Rishi, Kim, Alex, Kneib, Jean-Paul, Kollmeier, Juna A., Kovetz, Ely D., Krause, Elisabeth, Krolewski, Alex, L Huillier, Benjamin, Landriau, Martin, Levi, Michael, Liguori, Michele, Linder, Eric, Lukić, Zarija, La Macorra, Axel, Plazas, Andrés A., Marshall, Jennifer L., Martini, Paul, Masui, Kiyoshi, Mcdonald, Patrick, Daniel Meerburg, P., Meyers, Joel, Mirbabayi, Mehrdad, Moustakas, John, Myers, Adam D., Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niz, Gustavo, Padmanabhan, Hamsa, Palunas, Povilas, Percival, Will J., Piacentini, Francesco, Pieri, Matthew M., Piro, Anthony L., Prakash, Abhishek, Rhodes, Jason, Ross, Ashley J., Rossi, Graziano, Rudie, Gwen C., Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Simon, Joshua D., Simon, Sara, Slepian, Zachary, Slosar, Anže, Sridhar, Srivatsan, Stebbins, Albert, Escoffier, Stephanie, Switzer, Eric R., Tarlé, Gregory, Trodden, Mark, Uhlemann, Cora, Arturo Urenña-López, L., Di Valentino, Eleonora, Vargas-Magaña, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, Zhu, Hong-Ming, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), 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), Département d'Astrophysique (ex SAP) (DAP), 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, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
cosmological model, non-Gaussianity, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxy, expansion: acceleration, inflation, dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, boundary condition, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The expansion of the Universe is understood to have accelerated during two epochs: in its very first moments during a period of Inflation and much more recently, at $z < 1$, when Dark Energy is hypothesized to drive cosmic acceleration. The undiscovered mechanisms behind these two epochs represent some of the most important open problems in fundamental physics. The large cosmological volume at $2 < z < 5$, together with the ability to efficiently target high-$z$ galaxies with known techniques, enables large gains in the study of Inflation and Dark Energy. A future spectroscopic survey can test the Gaussianity of the initial conditions up to a factor of ~50 better than our current bounds, crossing the crucial theoretical threshold of $\sigma(f_{NL}^{\rm local})$ of order unity that separates single field and multi-field models. Simultaneously, it can measure the fraction of Dark Energy at the percent level up to $z = 5$, thus serving as an unprecedented test of the standard model and opening up a tremendous discovery space., Comment: Science white paper submitted to the Astro2020 Decadal Survey

Published
2019

34. Astro2020 APC White Paper: The MegaMapper: a z > 2 Spectroscopic Instrument for the Study of Inflation and Dark Energy

Author

Schlegel, David J., Kollmeier, Juna A., Aldering, Greg, Bailey, Stephen, Baltay, Charles, Bebek, Christopher, Benzvi, Segev, Besuner, Robert, Blanc, Guillermo, Bolton, Adam S., Bouri, Mohamed, Brooks, David, Buckley-Geer, Elizabeth, Cai, Zheng, Crane, Jeffrey, Dey, Arjun, Doel, Peter, Fan, Xiaohui, Ferraro, Simone, Font-Ribera, Andreu, Gutierrez, Gaston, Guy, Julien, Heetderks, Henry, Huterer, Dragan, Infante, Leopoldo, Jelinsky, Patrick, Johns, Matthew, Karagiannis, Dionysios, Kent, Stephen M., Kim, Alex G., Kneib, Jean-Paul, Kronig, Luzius, Konidaris, Nick, Lahav, Ofer, Lampton, Michael L., Lang, Dustin, Leauthaud, Alexie, Liguori, Michele, Linder, Eric V., Magneville, Christophe, Martini, Paul, Mateo, Mario, McDonald, Patrick, Miller, Christopher J., Moustakas, John, Myers, Adam D., Mulchaey, John, Newman, Jeffrey A., Nugent, Peter E., Palanque-Delabrouille, Nathalie, Padmanabhan, Nikhil, Piro, Anthony L., Poppett, Claire, Prochaska, Jason X., Pullen, Anthony R., Rabinowitz, David, Ramirez, Solange, Rix, Hans-Walter, Ross, Ashley J., Samushia, Lado, Schaan, Emmanuel, Schubnell, Michael, Seljak, Uros, Seo, Hee-Jong, Shectman, Stephen A., Silber, Joseph, Simon, Joshua D., Slepian, Zachary, Soares-Santos, Marcelle, Tarlé, Greg, Thompson, Ian, Valluri, Monica, Wechsler, Risa H., White, Martin, Wilson, Michael J., Yèche, Christophe, Zaritsky, Dennis, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and HEP, INSPIRE

Subjects
Astrophysics and Astronomy, [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], hep-ex, galaxy: redshift, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Astrophysics::Cosmology and Extragalactic Astrophysics, High Energy Physics - Experiment, observatory, DESI, [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, Astrophysics - Instrumentation and Methods for Astrophysics, dark energy, Particle Physics - Experiment, Astrophysics::Galaxy Astrophysics, astro-ph.IM
Abstract

International audience; MegaMapper is a proposed ground-based experiment to measure Inflation parameters and Dark Energy from galaxy redshifts at 2

Published
2019

35. LSST Cadence Optimization White Paper in Support of Observations of Unresolved Tidal Stellar Streams in Galaxies beyond the Local Group

Author

Laine, Seppo, Martinez-Delgado, David, Trujillo, Ignacio, Duc, Pierre-Alain, Grillmair, Carl J., Frenk, Carlos S., Hendel, David, Johnston, Kathryn V., Mihos, J. Chris, Moustakas, John, Beaton, Rachael L., Romanowsky, Aaron J., Greco, Johnny, and Erkal, Denis

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

Deep observations of faint surface brightness stellar tidal streams in external galaxies with LSST are addressed in this White Paper contribution. We propose using the Wide--Fast--Deep survey that contains several nearby galaxies (at distances where the stars themselves are not resolved, i.e., beyond 20 Mpc). In the context of hierarchical galaxy formation, it is necessary to understand the prevalence and properties of tidal substructure around external galaxies based on integrated (i.e., unresolved) diffuse light. This requires collecting observations on much larger samples of galaxies than the Milky Way and M31. We will compare the observed structures to the predictions of cosmological models of galactic halo formation that inform us about the number and properties of streams around Milky Way-like galaxies. The insight gained from these comparisons will allow us to infer the properties of stream progenitors (masses, dynamics, metallicities, stellar populations). The changes in the host galaxies caused by the interactions with the dissolving companion galaxies will be another focus of our studies. We conclude by discussing synergies with WFIRST and Euclid, and also provide concrete suggestions for how the effects of scattered light could be minimized in LSST images to optimize the search for low surface brightness features, such as faint unresolved stellar tidal streams., 13 pages, 2 figures, submitted to Call for White Papers on LSST Cadence Optimization

Published
2018

36. Tidal interactions and mergers in intermediate redshift EDisCS clusters

Author

Deger, Sinan, Rudnick, Gregory, Kelkar, Kshitija, Desai, Vandana, Lotz, Jennifer M., Jablonka, Pascale, Moustakas, John, and Zaritsky, Dennis

Subjects
Physical Sciences - Astrophysics & Universe Sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We study the fraction of tidal interactions and mergers with well identified observability timescales (fTIM) in group, cluster, and accompanying field galaxies and its dependence on redshift (z), cluster velocity dispersion (sigma) and environment analyzing HST-ACS images and catalogs from the ESO Distant Cluster Survey (EDisCS). Our sample consists of 11 clusters, 7 groups, and accompanying field galaxies at 0:4 equal or less z equal or less 0:8. We derive fTIM using both a visual classification of galaxy morphologies and an automated method, the G-M20 method. We calibrate this method using the visual classifications that were performed on a subset of our sample. We find marginal evidence for a trend between fTIM and z, in that higher z values correspond to higher fTIM. However, we also cannot rule out the null hypothesis of no correlation at higher than 68% confidence. No trend is present between fTIM and z. We find that fTIM shows suggestive peaks in groups, and tentatively in clusters at R > 0:5 x R200, implying that fTIM gets boosted in these intermediate density environments. However, our analysis of the local densities of our cluster sample does not reveal a trend between fTIM and density, except for a potential enhancement at the very highest densities. We also perform an analysis of projected radius-velocity phase space for our cluster members. Our results reveal that tidal interactions and mergers (TIM), and undisturbed galaxies only have a 6% probability of having been drawn from the same parent population in their velocity distribution and 37% in radii, in agreement with the modest differences obtained in fTIM at the clusters.

Published
2018

37. CHAOS. VI. Direct Abundances in NGC 2403.

Author

Rogers, Noah S. J., Skillman, Evan D., Pogge, Richard W., Berg, Danielle A., Moustakas, John, Croxall, Kevin V., and Sun, Jiayi

Subjects
ELECTRON temperature, SCATTER diagrams, SPECTROGRAPHS, INTEGRAL field spectroscopy
Abstract

We report the direct abundances for the galaxy NGC 2403 as observed by the CHemical Abundances Of Spirals (CHAOS) project. Using the Multi-Object Double Spectrograph on the Large Binocular Telescope, we observe two fields with H ii regions that cover an Rg/Re range of 0.18–2.31. Thirty-two H ii regions contain at least one auroral line detection, and we detect a total of 122 temperature-sensitive auroral lines. Here, for the first time, we use the intrinsic scatter in the Te–Te diagrams, added in quadrature to the uncertainty on the measured temperature, to determine the uncertainty on an electron temperature inferred for one ionization zone from a measurement in a different ionization zone. We then use all available temperature data within a H ii region to obtain a weighted-average temperature within each ionization zone. We rederive the oxygen abundances of all CHAOS galaxies using this new temperature prioritization method, and we find that the gradients are consistent with the results of a recent study of Berg et al. For NGC 2403, we measure a direct oxygen abundance gradient of −0.09(±0.03) dex/Re, with an intrinsic dispersion of 0.037(±0.017) dex and a N/O abundance gradient of −0.17(±0.03) dex/Re with an intrinsic dispersion of 0.060(±0.018) dex. For direct comparison, we use the line intensities from an earlier study of NGC 2403 by Berg et al. and find their recomputed values for the O/H and N/O gradients are consistent with ours. [ABSTRACT FROM AUTHOR]

Published
2021
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38. Baryon acoustic oscillations in the projected cross-correlation function between the eBOSS DR16 quasars and photometric galaxies from the DESI Legacy Imaging Surveys.

Author

Zarrouk, Pauline, Rezaie, Mehdi, Raichoor, Anand, Ross, Ashley J, Alam, Shadab, Blum, Robert, Brookes, David, Chuang, Chia-Hsun, Cole, Shaun, Dawson, Kyle S, Eisenstein, Daniel J, Kehoe, Robert, Landriau, Martin, Moustakas, John, Myers, Adam D, Norberg, Peder, Percival, Will J, Prada, Francisco, Schubnell, Michael, and Seo, Hee-Jong

Subjects
QUASARS, GALAXIES, OSCILLATIONS, GALACTIC redshift, ANGULAR distance, DETECTION limit
Abstract

We search for the baryon acoustic oscillations in the projected cross-correlation function binned into transverse comoving radius between the SDSS-IV DR16 eBOSS quasars and a dense photometric sample of galaxies selected from the DESI Legacy Imaging Surveys. We estimate the density of the photometric sample of galaxies in this redshift range to be about 2900 deg−2, which is deeper than the official DESI emission line galaxy selection, and the density of the spectroscopic sample is about 20 deg−2. In order to mitigate the systematics related to the use of different imaging surveys close to the detection limit, we use a neural network approach that accounts for complex dependences between the imaging attributes and the observed galaxy density. We find that we are limited by the depth of the imaging surveys that affects the density and purity of the photometric sample and its overlap in redshift with the quasar sample, which thus affects the performance of the method. When cross-correlating the photometric galaxies with quasars in the range 0.6 ≤ z ≤ 1.2, the cross-correlation function can provide better constraints on the comoving angular distance D M (6 per cent precision) compared to the constraint on the spherically averaged distance D V (9 per cent precision) obtained from the autocorrelation. Although not yet competitive, this technique will benefit from the arrival of deeper photometric data from upcoming surveys that will enable it to go beyond the current limitations we have identified in this work. [ABSTRACT FROM AUTHOR]

Published
2021
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39. Compact Starburst Galaxies with Fast Outflows: Central Escape Velocities and Stellar Mass Surface Densities from Multiband Hubble Space Telescope Imaging.

Author

Diamond-Stanic, Aleksandar M., Moustakas, John, Sell, Paul H., Tremonti, Christy A., Coil, Alison L., Davis, Julie D., Geach, James E., Gottlieb, Sophia C. W., Hickox, Ryan C., Kepley, Amanda, Lipscomb, Charles, Rines, Joshua, Rudnick, Gregory H., Thompson, Cristopher, Valdez, Kingdell, Bradna, Christian, Camarillo, Jordan, Cinquino, Eve, Ohene, Senyo, and Perrotta, Serena

Subjects
*STELLAR density (Stellar population), *SPACE telescopes, *EDDINGTON mass limit, *STELLAR mass, *STARBURSTS, *VELOCITY
Abstract

We present multiband Hubble Space Telescope imaging that spans rest-frame near-ultraviolet through near-infrared wavelengths (–1.1 μm) for 12 compact starburst galaxies at z = 0.4–0.8. These massive galaxies () are driving very fast outflows (–3000 km s−1), and their light profiles are dominated by an extremely compact starburst component (half-light radius ∼ 100 pc). Our goal is to constrain the physical mechanisms responsible for launching these fast outflows by measuring the physical conditions within the central kiloparsec. Based on our stellar population analysis, the central component typically contributes ≈25% of the total stellar mass, and the central escape velocities km s−1 are a factor of two smaller than the observed outflow velocities. This Requires physical mechanisms that can accelerate gas to speeds significantly beyond the central escape velocities, and it makes clear that these fast outflows are capable of traveling into the circumgalactic medium, and potentially beyond. We find central stellar densities kpc−2 comparable to theoretical estimates of the Eddington limit, and we estimate surface densities within the central kiloparsec comparable to those of compact massive galaxies at. Relative to "red nuggets" and "blue nuggets" at , we find significantly smaller re values at a given stellar mass, which we attribute to the dominance of a young stellar component in our sample and the better physical resolution for rest-frame optical observations at versus. We compare to theoretical scenarios involving major mergers and violent disk instability, and we speculate that our galaxies are progenitors of power-law ellipticals in the local universe with prominent stellar cusps. [ABSTRACT FROM AUTHOR]

Published
2021
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40. Determining the halo mass scale where galaxies lose their gas

Author

Rudnick, Gregory, Jablonka, Pascale, Moustakas, John, Zaritsky, Dennis, Jaffe, Yara L., De Lucia, Gabriella, Desai, Vandana, Halliday, Claire, Just, Dennis, Milvang-Jensen, Bo, and Poggianti, Bianca

Subjects
High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

A major question in galaxy formation is how the gas supply that fuels activity in galaxies is modulated by their environment. We use spectroscopy of a set of well characterized clusters and groups at $0.45$\AA\ is $f_{[OII]}=0.08^{+0.03}_{-0.02}$ and $f_{[OII]}=0.06^{+0.07}_{-0.04}$ respectively. For field galaxies we find $f_{[OII]}=0.27^{+0.07}_{-0.06}$, representing a 2.8$\sigma$ difference between the [OII] fractions for old galaxies between the different environments. We conclude that a population of old galaxies in all environments has ionized gas that likely stems from stellar mass loss. In the field galaxies also experience gas accretion from the cosmic web and in groups and clusters these galaxies have had their gas accretion shut off by their environment. Additionally, galaxies with emission preferentially avoid the virialized region of the cluster in position-velocity space. We discuss the implications of our results, among which is that gas accretion shutoff is likely effective at group halo masses (log~${\cal M}/$\msol$>12.8$) and that there are likely multiple gas removal processes happening in dense environments.

Published
2017

41. The clustering of DESI-like luminous red galaxies using photometric redshifts.

Author

Zhou, Rongpu, Newman, Jeffrey A, Mao, Yao-Yuan, Meisner, Aaron, Moustakas, John, Myers, Adam D, Prakash, Abhishek, Zentner, Andrew R, Brooks, David, Duan, Yutong, Landriau, Martin, Levi, Michael E, Prada, Francisco, and Tarle, Gregory

Subjects
GALAXIES, MARKOV chain Monte Carlo, LARGE scale structure (Astronomy), REDSHIFT
Abstract

We present measurements of the redshift-dependent clustering of a DESI-like luminous red galaxy (LRG) sample selected from the Legacy Survey imaging data set, and use the halo occupation distribution (HOD) framework to fit the clustering signal. The photometric LRG sample in this study contains 2.7 million objects over the redshift range of 0.4 < z < 0.9 over 5655 deg2. We have developed new photometric redshift (photo- z) estimates using the Legacy Survey DECam and WISE photometry, with σNMAD = 0.02 precision for LRGs. We compute the projected correlation function using new methods that maximize signal-to-noise ratio while incorporating redshift uncertainties. We present a novel algorithm for dividing irregular survey geometries into equal-area patches for jackknife resampling. For a five-parameter HOD model fit using the MultiDark halo catalogue, we find that there is little evolution in HOD parameters except at the highest redshifts. The inferred large-scale structure bias is largely consistent with constant clustering amplitude over time. In an appendix, we explore limitations of Markov chain Monte Carlo fitting using stochastic likelihood estimates resulting from applying HOD methods to N -body catalogues, and present a new technique for finding best-fitting parameters in this situation. Accompanying this paper, we have released the Photometric Redshifts for the Legacy Surveys catalogue of photo- z 's obtained by applying the methods used in this work to the full Legacy Survey Data Release 8 data set. This catalogue provides accurate photometric redshifts for objects with z < 21 over more than 16 000 deg2 of sky. [ABSTRACT FROM AUTHOR]

Published
2021
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42. Removing imaging systematics from galaxy clustering measurements with Obiwan: application to the SDSS-IV extended Baryon Oscillation Spectroscopic Survey emission-line galaxy sample.

Author

Kong, Hui, Burleigh, Kaylan J, Ross, Ashley, Moustakas, John, Chuang, Chia-Hsun, Comparat, Johan, de Mattia, Arnaud, du Mas des Bourboux, Hélion, Honscheid, Klaus, Lin, Sichen, Raichoor, Anand, Rossi, Graziano, and Zhao, Cheng

Subjects
EMISSION-line galaxies, GALAXY clusters, GALACTIC redshift, LARGE scale structure (Astronomy), DARK energy, REDSHIFT
Abstract

This work presents the application of a new tool, Obiwan , which uses image simulations to determine the selection function of a galaxy redshift survey and calculate three-dimensional (3D) clustering statistics. Obiwan relies on a forward model of the process by which images of the night sky are transformed into a 3D large-scale structure catalogue, and offers several advantages over more traditional map-based techniques – such as operating on individual exposures and adopting a maximum likelihood approach. The photometric pipeline automatically detects and models galaxies and then generates a catalogue of such galaxies with detailed information for each one of them, including their location, redshift, and so on. Systematic biases in the imaging data are therefore imparted into the catalogues and must be accounted for in any scientific analysis of their information content. Obiwan simulates this process for samples selected from the Legacy Surveys imaging data. This imaging data will be used to select target samples for the next-generation Dark Energy Spectroscopic Instrument (DESI) experiment. Here, we apply Obiwan to a portion of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey emission-line galaxies (ELGs). Systematic biases in the data are clearly identified and removed. We compare the 3D clustering results to those obtained by the map-based approach applied to the complete eBOSS Data Release 16 (DR16) sample. We find the results are consistent, thereby validating the eBOSS DR16 ELG catalogues, which is used to obtain cosmological results. [ABSTRACT FROM AUTHOR]

Published
2020
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43. Deviations from the Infrared-radio Correlation in Massive, Ultracompact Starburst Galaxies.

Author

Petter, Grayson C., Kepley, Amanda A., Hickox, Ryan C., Rudnick, Gregory H., Tremonti, Christy A., Diamond-Stanic, Aleksandar M., Geach, James E., Coil, Alison L., Sell, Paul H., Moustakas, John, Rupke, David S. N., Perrotta, Serena, Whalen, Kelly E., and Davis, Julie D.

Subjects
EDDINGTON mass limit, RADIATION pressure, GALAXY mergers, SYNCHROTRON radiation, STAR formation, STARBURSTS
Abstract

Feedback through energetic outflows has emerged as a key physical process responsible for transforming star-forming galaxies into the quiescent systems observed in the local universe. To explore this process, this paper focuses on a sample of massive and compact merger remnant galaxies hosting high-velocity gaseous outflows (km s−1), found at intermediate redshift (z ∼ 0.6). From their mid-infrared emission and compact morphologies, these galaxies are estimated to have exceptionally large star formation rate (SFR) surface densities (ΣSFR ∼ 103M⊙ yr−1 kpc−2), approaching the Eddington limit for radiation pressure on dust grains. This suggests that star formation feedback may be driving the observed outflows. However, these SFR estimates suffer from significant uncertainties. We therefore sought an independent tracer of star formation to probe the compact starburst activity in these systems. In this paper, we present SFR estimates calculated using 1.5 GHz continuum Jansky Very Large Array observations for 19 of these galaxies. We also present updated infrared (IR) SFRs calculated from WISE survey data. We estimate SFRs from the IR to be larger than those from the radio for 16 out of 19 galaxies by a median factor of 2.5. We find that this deviation is maximized for the most compact galaxies hosting the youngest stellar populations, suggesting that compact starbursts deviate from the IR-radio correlation. We suggest that this deviation stems either from free–free absorption of synchrotron emission, a difference in the timescale over which each indicator traces star formation, or exceptionally hot IR-emitting dust in these ultra-dense galaxies. [ABSTRACT FROM AUTHOR]

Published
2020
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44. The DESI Experiment Part I: Science,Targeting, and Survey Design

Author

Aghamousa, Amir, Aguilar, Jessica, Ahlen, Steve, Alam, Shadab, Allen, Lori E., Prieto, Carlos Allende, Annis, James, Bailey, Stephen, Balland, Christophe, Ballester, Otger, Baltay, Charles, Beaufore, Lucas, Bebek, Chris, Beers, Timothy C., Bell, Eric F., Bernal, José Luis, Besuner, Robert, Beutler, Florian, Blake, Chris, Bleuler, Hannes, Blomqvist, Michael, Blum, Robert, Bolton, Adam S., Briceno, Cesar, Brooks, David, Brownstein, Joel R., Buckley-Geer, Elizabeth, Burden, Angela, Burtin, Etienne, Busca, Nicolás G., Cahn, Robert N., Cai, Yan-Chuan, Cardiel-Sas, Laia, Carlberg, Raymond G., Carton, Pierre-Henri, Casas, Ricard, Castander, Francisco J., Cervantes-Cota, Jorge L., Claybaugh, Todd M., Close, Madeline, Coker, Carl T., Cole, Shaun, Comparat, Johan, Cooper, Andrew P., Cousinou, M. -C., Crocce, Martin, Cuby, Jean-Gabriel, Cunningham, Daniel P., Davis, Tamara M., Dawson, Kyle S., de La Macorra, Axel, de Vicente, Juan, Delubac, Timothée, Derwent, Mark, Dey, Arjun, Dhungana, Govinda, Ding, Zhejie, Doel, Peter, Duan, Yutong T., Ealet, Anne, Edelstein, Jerry, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Elliott, Ann, Escoffier, Stephanie, Evatt, Matthew, Fagrelius, Parker, Fan, Xiaohui, Fanning, Kevin, Farahi, Arya, Farihi, Jay, Favole, Ginevra, Feng, Yu, Fernandez, Enrique, Findlay, Joseph R., Finkbeiner, Douglas P., Fitzpatrick, Michael J., Flaugher, Brenna, Flender, Samuel, Font-Ribera, Andreu, Forero-Romero, Jaime E., Fosalba, Pablo, Frenk, Carlos S., Fumagalli, Michele, Gaensicke, Boris T., Gallo, Giuseppe, Garcia-Bellido, Juan, Gaztanaga, Enrique, Fusillo, Nicola Pietro Gentile, Gerard, Terry, Gershkovich, Irena, Giannantonio, Tommaso, Gillet, Denis, Gonzalez-De-Rivera, Guillermo, Gonzalez-Perez, Violeta, Gott, Shelby, Graur, Or, Gutierrez, Gaston, Guy, Julien, Habib, Salman, Heetderks, Henry, Heetderks, Ian, Heitmann, Katrin, Hellwing, Wojciech A., Herrera, David A., Ho, Shirley, Holland, Stephen, Honscheid, Klaus, Huff, Eric, Hutchinson, Timothy A., Huterer, Dragan, Hwang, Ho Seong, Laguna, Joseph Maria Illa, Ishikawa, Yuzo, Jacobs, Dianna, Jeffrey, Niall, Jelinsky, Patrick, Jennings, Elise, Jiang, Linhua, Jimenez, Jorge, Johnson, Jennifer, Joyce, Richard, Jullo, Eric, Juneau, Stéphanie, Kama, Sami, Karcher, Armin, Karkar, Sonia, Kehoe, Robert, Kennamer, Noble, Kent, Stephen, Kilbinger, Martin, Kim, Alex G., Kirkby, David, Kisner, Theodore, Kitanidis, Ellie, Kneib, Jean-Paul, Koposov, Sergey, Kovacs, Eve, Koyama, Kazuya, Kremin, Anthony, Kron, Richard, Kronig, Luzius, Kueter-Young, Andrea, Lacey, Cedric G., Lafever, Robin, Lahav, Ofer, Lambert, Andrew, Lampton, Michael, Landriau, Martin, Lang, Dustin, Lauer, Tod R., Goff, Jean-Marc Le, Guillou, Laurent Le, van Suu, Auguste Le, Lee, Jae Hyeon, Lee, Su-Jeong, Leitner, Daniela, Lesser, Michael, Levi, Michael E., L'Huillier, Benjamin, Li, Baojiu, Liang, Ming, Lin, Huan, Linder, Eric, Loebman, Sarah R., Lukić, Zarija, Ma, Jun, Maccrann, Niall, Magneville, Christophe, Makarem, Laleh, Manera, Marc, Manser, Christopher J., Marshall, Robert, Martini, Paul, Massey, Richard, Matheson, Thomas, Mccauley, Jeremy, Mcdonald, Patrick, Mcgreer, Ian D., Meisner, Aaron, Metcalfe, Nigel, Miller, Timothy N., Miquel, Ramon, Moustakas, John, Myers, Adam, Naik, Milind, Newman, Jeffrey A., Nichol, Robert C., Nicola, Andrina, da Costa, Luiz Nicolati, Nie, Jundan, Niz, Gustavo, Norberg, Peder, Nord, Brian, Norman, Dara, Nugent, Peter, O'Brien, Thomas, Oh, Minji, Olsen, Knut A. G., Padilla, Cristobal, Padmanabhan, Hamsa, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Palmese, Antonella, Pappalardo, Daniel, Paris, Isabelle, Park, Changbom, Patej, Anna, Peacock, John A., Peiris, Hiranya V., Peng, Xiyan, Percival, Will J., Perruchot, Sandrine, Pieri, Matthew M., Pogge, Richard, Pollack, Jennifer E., Poppett, Claire, Prada, Francisco, Prakash, Abhishek, Probst, Ronald G., Rabinowitz, David, Raichoor, Anand, Ree, Chang Hee, Refregier, Alexandre, Régal, Xavier, Reid, Beth, Reil, Kevin, Rezaie, Mehdi, Rockosi, Constance M., Roe, Natalie, Ronayette, Samuel, Roodman, Aaron, Ross, Ashley J., Ross, Nicholas P., Rossi, Graziano, Rozo, Eduardo, Ruhlmann-Kleider, Vanina, Rykoff, Eli S., Sabiu, Cristiano, Samushia, Lado, Sanchez, Eusebio, Sanchez, Javier, Schlegel, David J., Schneider, Michael, Schubnell, Michael, Secroun, Aurélia, Seljak, Uros, Seo, Hee-Jong, Serrano, Santiago, Shafieloo, Arman, Shan, Huanyuan, Sharples, Ray, Sholl, Michael J., Shourt, William V., Silber, Joseph H., Silva, David R., Sirk, Martin M., Slosar, Anze, Smith, Alex, Smoot, George F., Som, Debopam, Song, Yong-Seon, Sprayberry, David, Staten, Ryan, Stefanik, Andy, Tarlè, Gregory, Tie, Suk Sien, Tinker, Jeremy L., Tojeiro, Rita, Valdes, Francisco, Valenzuela, Octavio, Valluri, Monica, Vargas-Magaña, Mariana, Verde, Licia, Walker, Alistair R., Wang, Jiali, Wang, Yuting, Weaver, Benjamin A., Weaverdyck, Curtis, Wechsler, Risa H., Weinberg, David H., White, Martin, Yang, Qian, Yeche, Christophe, Zhang, Tianmeng, Zhao, Gong-Bo, Zheng, Yi, Zhou, Xu, Zhou, Zhimin, Zhu, Yaling, Zou, Hu, Zu, Ying, Korea Astronomy and Space Science Institute (KASI), Okayama University, University of California [Berkeley], University of California, National Optical Astronomy Observatory (NOAO), Instituto de Astrofisica de Canarias (IAC), Fermi National Accelerator Laboratory (Fermilab), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Yale University [New Haven], Ohio State University [Columbus] (OSU), The University of Notre Dame [Sydney], Department of Astronomy, University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Space Sciences Laboratory [Berkeley] (SSL), University of California-University of California, University of Portsmouth, University of British Columbia (UBC), Ecole Polytechnique Fédérale de Lausanne (EPFL), Laboratoire d'Astrophysique de Marseille (LAM), 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), Cerro Tololo Inter-American Observatory, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Department of Astronomy & Astrophysics [University of Toronto], University of Toronto, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Carreterra Mexico-Toluca, Department of Physics [Durham University], Durham University, Department of Astronomy, The Ohio State University, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Institute for Computational Cosmology (ICC), 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), Universidad Nacional Autónoma de México (UNAM), Department of Applied Physics, Departamento de Fisica Aplicada [Granada], Universidad de Granada (UGR)-Universidad de Granada (UGR), University College of London [London] (UCL), University of Wyoming (UW), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Arizona State University [Tempe] (ASU), Department of Information Engineering, Zhejiang University of Technology, Zhejiang University of Technology, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Departamento de Fisica Teorica, Institute of Cosmology & Gravitation [Portsmouth], Carnegie Mellon University [Pittsburgh] (CMU), NASA Goddard Space Flight Center (GSFC), Korea Institute for Advanced Study (KIAS), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UCI), Department of Physics, University of California, University of California [Los Angeles] (UCLA), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Center for Cosmology & AstroParticle Physics, California Institute of Technology (CALTECH), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), Department of Physics [Durham], University of New Hampshire (UNH), University of Waterloo [Waterloo], Universität Zürich [Zürich] = University of Zurich (UZH), Department of Astronomy and Space Science [Sejong University], Sejong University, Department of Physics [Oxford], University of Oxford [Oxford], Institute of Plasma Physics, Chinese Academy of Sciences (ASIPP), Department of Physics [Ann Arbor], University of St Andrews [Scotland], University of Science and Technology of China [Hefei] (USTC), Department of Computer Science and Engineering [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Karlsruhe Institute of Technology (KIT), National University of Defense Technology [China], DESI Collaboration, University of California [Berkeley] (UC Berkeley), University of California (UC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universidad Autónoma de Madrid (UAM), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Universidad de Granada = University of Granada (UGR)-Universidad de Granada = University of Granada (UGR), Harvard University-Smithsonian Institution, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), University of California [Irvine] (UC Irvine), University of Oxford, and Escoffier, Stephanie

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::Galaxy Astrophysics
Abstract

DESI (Dark Energy Spectroscopic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations (BAO) and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. To trace the underlying dark matter distribution, spectroscopic targets will be selected in four classes from imaging data. We will measure luminous red galaxies up to $z=1.0$. To probe the Universe out to even higher redshift, DESI will target bright [O II] emission line galaxies up to $z=1.7$. Quasars will be targeted both as direct tracers of the underlying dark matter distribution and, at higher redshifts ($ 2.1 < z < 3.5$), for the Ly-$\alpha$ forest absorption features in their spectra, which will be used to trace the distribution of neutral hydrogen. When moonlight prevents efficient observations of the faint targets of the baseline survey, DESI will conduct a magnitude-limited Bright Galaxy Survey comprising approximately 10 million galaxies with a median $z\approx 0.2$. In total, more than 30 million galaxy and quasar redshifts will be obtained to measure the BAO feature and determine the matter power spectrum, including redshift space distortions.

Published
2016

45. Imaging systematics and clustering of DESI main targets.

Author

Kitanidis, Ellie, White, Martin, Feng, Yu, Schlegel, David, Guy, Julien, Dey, Arjun, Landriau, Martin, Brooks, David, Levi, Michael, Moustakas, John, Prada, Francisco, Tarle, Gregory, and Weaver, Benjamin Alan

Subjects
EMISSION-line galaxies, SKY brightness, CLUSTER analysis (Statistics), ORDER statistics, ANGULAR measurements, SURFACE brightness (Astronomy), STELLAR luminosity function
Abstract

We evaluate the impact of imaging systematics on the clustering of luminous red galaxies (LRG), emission-line galaxies (ELG), and quasars (QSO) targeted for the upcoming Dark Energy Spectroscopic Instrument (DESI) survey. Using Data Release 7 of the DECam Legacy Survey, we study the effects of astrophysical foregrounds, stellar contamination, differences between north galactic cap and south galactic cap measurements, and variations in imaging depth, stellar density, galactic extinction, seeing, airmass, sky brightness, and exposure time before presenting survey masks and weights to mitigate these effects. With our sanitized samples in hand, we conduct a preliminary analysis of the clustering amplitude and evolution of the DESI main targets. From measurements of the angular correlation functions, we determine power law fits |$r_0 = 7.78 \pm 0.26\, h^{-1}$| Mpc, γ  = 1.98 ± 0.02 for LRGs and |$r_0 = 5.45 \pm 0.1\, h^{-1}$| Mpc, γ  = 1.54 ± 0.01 for ELGs. Additionally, from the angular power spectra, we measure the linear biases and model the scale-dependent biases in the weakly non-linear regime. Both sets of clustering measurements show good agreement with survey requirements for LRGs and ELGs, attesting that these samples will enable DESI to achieve precise cosmological constraints. We also present clustering as a function of magnitude, use cross-correlations with external spectroscopy to infer dN/dz and measure clustering as a function of luminosity, and probe higher order clustering statistics through counts-in-cells moments. [ABSTRACT FROM AUTHOR]

Published
2020
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46. Dynamic Observing and Tiling Strategies for the DESI Legacy Surveys.

Author

Burleigh, Kaylan J., Landriau, Martin, Dey, Arjun, Lang, Dustin, Schlegel, David J., Nugent, Peter E., Blum, Robert, Findlay, Joseph R., Finkbeiner, Douglas P., Herrera, David, Honscheid, Klaus, Juneau, Stéphanie, McGreer, Ian, Meisner, Aaron M., Moustakas, John, Myers, Adam D., Patej, Anna, Schlafly, Edward F., Valdes, Francisco, and Walker, Alistair R.

Published
2020
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47. CHAOS V: Recombination Line Carbon Abundances in M 101.

Author

Skillman, Evan D., Berg, Danielle A., Pogge, Richard W., Moustakas, John, Rogers, Noah S. J., and Croxall, Kevin V.

Subjects
PHOTOIONIZATION, SPIRAL galaxies, CORRECTION factors, CARBON, POLLUTION, TELESCOPES
Abstract

The CHemical Abundances Of Spirals (CHAOS) project is building a large database of Large Binocular Telescope (LBT) H ii region spectra in nearby spiral galaxies to use direct abundances to better determine the dispersion in metallicity as a function of galactic radius. Here, we present CHAOS LBT observations of C ii λ4267 emission detected in 10 H ii regions in M 101, and using a new photoionization model-based ionization correction factor, we convert these measurements into total carbon abundances. A comparison with M 101 C ii recombination line observations from the literature shows excellent agreement, and we measure a relatively steep gradient in log(C/H) of −0.37 ± 0.06 dex. The C/N observations are consistent with a constant value of log(C/N) = 0.84 with a dispersion of only 0.09 dex, which, given the different nucleosynthetic sources of C and N, is challenging to understand. We also note that when plotting N/O versus O/H, all of the H ii regions with detections of C ii λ4267 present N/O abundances at the minimum of the scatter in N/O at a given value of O/H. If the high surface brightness necessary for the detection of the faint recombination lines is interpreted as an indicator of H ii region youth, then this may point to a lack of nitrogen pollution in the youngest H ii regions. In the future, we anticipate that the CHAOS project will significantly increase the total number of C ii λ4267 measurements in extragalactic H ii regions. [ABSTRACT FROM AUTHOR]

Published
2020
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48. CHAOS IV: Gas-phase Abundance Trends from the First Four CHAOS Galaxies.

Author

Berg, Danielle A., Pogge, Richard W., Skillman, Evan D., Croxall, Kevin V., Moustakas, John, Rogers, Noah S. J., and Sun, Jiayi

Subjects
COSMIC abundances, ELECTRON temperature, GALAXIES, GALACTIC evolution, IONIZATION energy, TEMPERATURE measurements, SPIRAL galaxies
Abstract

The chemical abundances of spiral galaxies, as probed by H ii regions across their disks, are key to understanding the evolution of galaxies over a wide range of environments. We present Large Binocular Telescope/Multi-Object Double Spectrographs spectra of 52 H ii regions in NGC 3184 as part of the CHemical Abundances Of Spirals (CHAOS) project. We explore the direct-method gas-phase abundance trends for the first four CHAOS galaxies, using temperature measurements from one or more auroral-line detections in 190 individual H ii regions. We find that the dispersion in relationships is dependent on ionization, as characterized by , and so we recommend ionization-based temperature priorities for abundance calculations. We confirm our previous results that [N ii ] and [S iii ] provide the most robust measures of electron temperature in low-ionization zones, while [O iii ] provides reliable electron temperatures in high-ionization nebula. We measure relative and absolute abundances for O, N, S, Ar, and Ne. The four CHAOS galaxies marginally conform with a universal O/H gradient, as found by empirical integral field unit studies when plotted relative to effective radius. However, after adjusting for vertical offsets, we find a tight universal N/O gradient of dex/Re with σtot. = 0.08 for Rg/Re < 2.0, where N is dominated by secondary production. Despite this tight universal N/O gradient, the scatter in the N/O–O/H relationship is significant. Interestingly, the scatter is similar when N/O is plotted relative to O/H or S/H. The observable ionic states of S probe lower ionization and excitation energies than O, which might be more appropriate for characterizing abundances in metal-rich H ii regions. [ABSTRACT FROM AUTHOR]

Published
2020
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49. PRIMUS+DEEP2: CLUSTERING OF X-RAY, RADIO, AND IR-AGNs AT z similar to 0.7

Author

Mendez, Alexander J, Coil, Alison L, Aird, James, Skibba, Ramin A, Diamond-Stanic, Aleksandar M, Moustakas, John, Blanton, Michael R, Cool, Richard J, Eisenstein, Daniel J, Wong, Kenneth C, and Zhu, Guangtun

Subjects
Particle and Plasma Physics, active [galaxies], Molecular, Nuclear, Astronomy & Astrophysics, Atomic, Physical Chemistry, galaxies [infrared], Astronomical and Space Sciences, evolution [galaxies], galaxies [radio continuum], Physical Chemistry (incl. Structural), galaxies [X-rays]
Published
2016

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