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1. The CluMPR galaxy cluster-finding algorithm and DESI legacy survey galaxy cluster catalogue.

Author

Yantovski-Barth, M J, Newman, Jeffrey A, Dey, Biprateep, Andrews, Brett H, Eracleous, Michael, Golden-Marx, Jesse, and Zhou, Rongpu

Subjects
GALAXY clusters, GALACTIC evolution, STELLAR mass, DARK matter, GALAXIES, CATALOGS
Abstract

Galaxy clusters enable unique opportunities to study cosmology, dark matter, galaxy evolution, and strongly lensed transients. We here present a new cluster-finding algorithm, CluMPR (Clusters from Masses and Photometric Redshifts), that exploits photometric redshifts (photo- z 's) as well as photometric stellar mass measurements. CluMPR uses a 2D binary search tree to search for overdensities of massive galaxies with similar redshifts on the sky and then probabilistically assigns cluster membership by accounting for photo- z uncertainties. We leverage the deep DESI Legacy Survey grzW1W2 imaging over one-third of the sky to create a catalogue of |$\sim 300\, 000$| galaxy cluster candidates out to z = 1, including tabulations of member galaxies and estimates of each cluster's total stellar mass. Compared to other methods, CluMPR is particularly effective at identifying clusters at the high end of the redshift range considered (z = 0.75–1), with minimal contamination from low-mass groups. These characteristics make it ideal for identifying strongly lensed high-redshift supernovae and quasars that are powerful probes of cosmology, dark matter, and stellar astrophysics. As an example application of this cluster catalogue, we present a catalogue of candidate wide-angle strongly lensed quasars in Appendix C. The nine best candidates identified from this sample include two known lensed quasar systems and a possible changing-look lensed QSO with SDSS spectroscopy. All code and catalogues produced in this work are publicly available (see Data Availability). [ABSTRACT FROM AUTHOR]

Published
2024
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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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3. SDSS-IV MaNGA: How the Stellar Populations of Passive Central Galaxies Depend on Stellar and Halo Mass.

Author

Oyarzún, Grecco A., Bundy, Kevin, Westfall, Kyle B., Tinker, Jeremy L., Belfiore, Francesco, Argudo-Fernández, Maria, Zheng, Zheng, Conroy, Charlie, Masters, Karen L., Wake, David, Law, David R., McDermid, Richard M., Aragón-Salamanca, Alfonso, Parikh, Taniya, Yan, Renbin, Bershady, Matthew, Sánchez, Sebastián F., Andrews, Brett H., Fernández-Trincado, José G., and Lane, Richard R.

Subjects
STELLAR populations, GALAXIES, GAS as fuel, SIGNAL-to-noise ratio, ELLIPTICAL galaxies, GALAXY formation, STELLAR mass
Abstract

We analyze spatially resolved and co-added SDSS-IV MaNGA spectra with signal-to-noise ratio ∼100 from 2200 passive central galaxies (z ∼ 0.05) to understand how central galaxy assembly depends on stellar mass (M *) and halo mass (M h ). We control for systematic errors in M h by employing a new group catalog from Tinker and the widely used Yang et al. catalog. At fixed M *, the strengths of several stellar absorption features vary systematically with M h . Completely model-free, this is one of the first indications that the stellar populations of centrals with identical M * are affected by the properties of their host halos. To interpret these variations, we applied full spectral fitting with the code alf. At fixed M *, centrals in more massive halos are older, show lower [Fe/H], and have higher [Mg/Fe] with 3.5 σ confidence. We conclude that halos not only dictate how much M * galaxies assemble but also modulate their chemical enrichment histories. Turning to our analysis at fixed M h , high- M * centrals are older, show lower [Fe/H], and have higher [Mg/Fe] for M h > 1012 h âˆ'1 M ⊙ with confidence >4 σ. While massive passive galaxies are thought to form early and rapidly, our results are among the first to distinguish these trends at fixed M h . They suggest that high- M * centrals experienced unique early formation histories, either through enhanced collapse and gas fueling or because their halos were early forming and highly concentrated, a possible signal of galaxy assembly bias. [ABSTRACT FROM AUTHOR]

Published
2022
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4. SDSS-IV MaNGA: radial gradients in stellar population properties of early-type and late-type galaxies.

Author

Parikh, Taniya, Thomas, Daniel, Maraston, Claudia, Westfall, Kyle B, Andrews, Brett H, Boardman, Nicholas Fraser, Drory, Niv, and Oyarzun, Grecco

Subjects
STELLAR populations, GALAXIES, GALAXY spectra, STELLAR mass, STELLAR spectra
Abstract

We derive ages, metallicities, and individual element abundances of early- and late-type galaxies (ETGs and LTGs) out to 1.5  R e. We study a large sample of 1900 galaxies spanning 8.6–11.3 log M/M⊙ in stellar mass, through key absorption features in stacked spectra from the SDSS-IV/MaNGA survey. We use mock galaxy spectra with extended star formation histories to validate our method for LTGs and use corrections to convert the derived ages into luminosity- and mass-weighted quantities. We find flat age and negative metallicity gradients for ETGs and negative age and negative metallicity gradients for LTGs. Age gradients in LTGs steepen with increasing galaxy mass, from −0.05 ± 0.11 log Gyr/ R e for the lowest mass galaxies to −0.82 ± 0.08 log Gyr/ R e for the highest mass ones. This strong gradient–mass relation has a slope of −0.70 ± 0.18. Comparing local age and metallicity gradients with the velocity dispersion σ within galaxies against the global relation with σ shows that internal processes regulate metallicity in ETGs but not age, and vice versa for LTGs. We further find that metallicity gradients with respect to local σ show a much stronger dependence on galaxy mass than radial metallicity gradients. Both galaxy types display flat [C/Fe] and [Mg/Fe], and negative [Na/Fe] gradients, whereas only LTGs display gradients in [Ca/Fe] and [Ti/Fe]. ETGs have increasingly steep [Na/Fe] gradients with local σ reaching 6.50 ± 0.78 dex/log km s−1 for the highest masses. [Na/Fe] ratios are correlated with metallicity for both galaxy types across the entire mass range in our sample, providing support for metallicity-dependent supernova yields. [ABSTRACT FROM AUTHOR]

Published
2021
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5. The Fourteenth Data Release of the Sloan Digital Sky Survey:First Spectroscopic Data from the Extended Baryon Oscillation Spectroscopic Survey and from the Second Phase of the Apache Point Observatory Galactic Evolution Experiment

Author

Abolfathi , Bela, Aguado , D. S., Aguilar , Gabriela, Prieto , Carlos Allende, Almeida , Andres, Ananna , Tonima Tasnim, Anders , Friedrich, Anderson , Scott F., Andrews , Brett H., Anguiano , Borja, Aragon-Salamanca , Alfonso, Argudo-Fernandez , Maria, Armengaud , Eric, Ata , Metin, Aubourg , Eric, Avila-Reese , Vladimir, Badenes , Carles, Bailey , Stephen, Balland , Christophe, Barger , Kathleen A., Barrera-Ballesteros , Jorge, Bartosz , Curtis, Bastien , Fabienne, Bates , Dominic, Baumgarten , Falk, Bautista , Julian, Beaton , Rachael, Beers , Timothy C., Belfiore , Francesco, Bender , Chad F., Bernardi , Mariangela, Bershady , Matthew A., Beutler , Florian, Bird , Jonathan C., Bizyaev , Dmitry, Blanc , Guillermo A., Blanton , Michael R., Blomqvist , Michael, Bolton , Adam S., Boquien , Médéric, Borissova , Jura, Bovy , Jo, Diaz , Christian Andres Bradna, Brandt , William Nielsen, Brinkmann , Jonathan, Brownstein , Joel R., Bundy , Kevin, Burgasser , Adam J., Burtin , Etienne, Busca , Nicolás G., Canas , Caleb I., Cano-Diaz , Mariana, Cappellari , Michele, Carrera , Ricardo, Casey , Andrew R., Sodi , Bernardo Cervantes, Chen , Yanping, Cherinka , Brian, Chiappini , Cristina, Choi , Peter Doohyun, Chojnowski , Drew, Chuang , Chia-Hsun, Chung , Haeun, Clerc , Nicolas, Cohen , Roger E., Comerford , Julia M., Comparat , Johan, Nascimento , Janaina Correa do, da Costa , Luiz, Cousinou , Marie-Claude, Covey , Kevin, Crane , Jeffrey d., Cruz-Gonzalez , Irene, Cunha , Katia, Ilha , Gabriele da Silva, Damke , Guillermo J., Darling , Jeremy, Davidson Jr. , James W., Dawson , Kyle, Lizaola , Miguel Angel C. de Icaza, de la Macorra , Axel, De La Torre , Sylvain, De Lee , Nathan, Agathe , Victoria de Sainte, Machado , Alice Deconto, Dell'Agli , Flavia, Delubac , Timothée, Diamond-Stanic , Aleksandar M., Donor , John, Downes , Juan Jose, Drory , Niv, Bourboux , Hélion du Mas des, Duckworth , Christopher J., Dwelly , Tom, Dyer , Jamie, Ebelke , Garrett, Eigenbrot , Arthur Davis, Eisenstein , Daniel J., Elsworth , Yvonne P., Emsellem , Eric, Eracleous , Mike, Erfanianfar , Ghazaleh, Escoffier , Stéphanie, Fan , Xiaohui, Alvar , Emma Fernandez, Fernandez-Trincado , J. G., Cirolini , Rafael Fernando, Feuillet , Diane, Finoguenov , Alexis, Fleming , Scott W., Font-Ribera , Andreu, Freischlad , Gordon, Frinchaboy , Peter, Fu , Hai, Chew , Yilen Gomez Maqueo, Galbany , Lluis, Perez , Ana E. Garcia, Garcia-Dias , R., García-Hernández , D. A., Oehmichen , Luis Alberto Garma, Gaulme , Patrick, Gelfand , Joseph, Gil-Marin , Hector, Gillespie , Bruce A., Goddard , Daniel, Hernandez , Jonay I. Gonzalez, Gonzalez-Perez , Violeta, Grabowski , Kathleen, Green , Paul J., Grier , Catherine J., Gueguen , Alain, Guo , Hong, Guy , Julien, Hagen , Alex, Hall , Patrick, Harding , Paul, Hasselquist , Sten, Hawley , Suzanne, Hayes , Christian R., Hearty , Fred, Hekker , Saskia, Hernández , Jesús, Toledo , Hector Hernandez, Hogg , David W., Holley-Bockelmann , Kelly, Holtzman , Jon, Hou , Jiamin, Hsieh , Bau-Ching, Hunt , Jason A. S., Hutchinson , Timothy A., Hwang , Ho Seong, Angel , Camilo Eduardo Jimenez, Johnson , Jennifer A., Jones , Amy, Jönsson , Henrik, Jullo , Eric, Khan , Fahim Sakil, Kinemuchi , Karen, Kirkby , David, Kirkpatrick IV , Charles C., Kitaura , Francisco-Shu, Knapp , Gillian R., Kneib , Jean-Paul, Kollmeier , Juna A., Lacerna , Ivan, Lane , Richard R., Lang , Dustin, Law , David R., Goff , Jean-Marc Le, Lee , Young-Bae, Li , Hongyu, Li , Cheng, Lian , Jianhui, Liang , Yu, Lima , Marcos, Lin , Lihwai, Long , Dan, Lucatello , Sara, Lundgren , Britt, Mackereth , J. Ted, MacLeod , Chelsea L., Mahadevan , Suvrath, Maia , Marcio Antonio Geimba, Majewski , Steven, Manchado , Arturo, Maraston , Claudia, Mariappan , Vivek, Marques-Chaves , Rui, Masseron , Thomas, Masters , Karen L., Mcdermid , Richard M., McGreer , Ian D., Melendez , Matthew, Meneses-Goytia , Sofia, Merloni , Andrea, Merrifield , Michael R., Meszaros , Szabolcs, Meza , Andres, Minchev , Ivan, Minniti , Dante, Prieto , Carlos, Ananna , Tonima, Anderson , Scott, Andrews , Brett, Aragón-Salamanca , Alfonso, Argudo-Fernández , Maria, Barger , Kathleen, Beers , Timothy, Bender , Chad, Bershady , Matthew, Bird , Jonathan, Blanc , Guillermo, Blanton , Michael, Bolton , Adam, Andres , Christian, Diaz , Bradna, Brandt , William, Brownstein , Joel, Burgasser , Adam, Busca , Nicolás, Cañas , Caleb, Cano-Díaz , Mariana, Casey , Andrew, Sodi , Bernardo, Choi , Peter, 10 , Davidson, Angel , Miguel, De Icaza Lizaola , C, De Sainte , Victoria, 72 , Agathe, Machado , Alice, Dell 'agli , Flavia, Diamond-Stanic , Aleksandar, Downes , Juan, du Mas des Bourboux , Hélion, Duckworth , Christopher, Davis Eigenbrot , Arthur, Eisenstein , Daniel, Elsworth , Yvonne, Fernández Alvar , Emma, Fernández-Trincado , J., Cirolini , Rafael, Fleming , Scott, Gómez , Yilen, Chew , Maqueo, Galbany , Lluís, García Pérez , Ana, Alberto , Luis, Oehmichen , Garma, Gil-Marín , Héctor, Gillespie , Bruce, González Hernández , Jonay, Green , Paul, Grier , Catherine, Hayes , Christian, Toledo , Hector, Hogg , David, Hunt , Jason, Hutchinson , Timothy, Hwang , Ho, Jimenez Angel , Camilo, Johnson , Jennifer, Fahim , Sakil, Kirkpatrick , Charles, 94 , Iv, Knapp , Gillian, Kollmeier , Juna, Lane , Richard, Law , DAvid, Le Goff , Jean-Marc, Macleod , Chelsea, Antonio , Marcio, Maia , Geimba, Masters , Karen, Mueller , Eva-Maria, Muller-Sanchez , Francisco, Muna , Demitri, Muñoz , Ricardo, Myers , Adam, Nair , Preethi, Nandra , Kirpal, Ness , Melissa, Newman , Jeffrey, Nichol , Robert, Nidever , David, Nitschelm , Christian, Noterdaeme , Pasquier, O 'connell , Julia, Oelkers , Ryan, Oravetz , Audrey, Oravetz , Daniel, Aquino Ortíz , Erik, Osorio , Yeisson, Pace , Zach, Padilla , Nelson, Palanque-Delabrouille , Nathalie, Palicio , Pedro, Pan , Hsi-An, Pan , Kaike, Parikh , Taniya, Pâris , Isabelle, Park , Changbom, Peirani , Sebastien, Pellejero-Ibanez , Marcos, Penny , Samantha, Percival , Will, Perez-Fournon , Ismael, Petitjean , Patrick, Pieri , Matthew, Pinsonneault , Marc, Pisani , Alice, Prada , Francisco, Prakash , Abhishek, Bárbara De Andrade Queiroz , Anna, Raddick , M, Raichoor , Anand, Rembold , Sandro, Richstein , Hannah, Riffel , Rogemar, Riffel , Rogério, Rix , Hans-Walter, Robin , Annie, Torres , Sergio, Román-Zúñiga , Carlos, Ross , Ashley, Rossi , Graziano, Ruan , John, Ruggeri , Rossana, Ruiz , Jose, Salvato , Mara, Sánchez , Ariel, Sanchez , Sebastian, Sanchez Almeida , Jorge, Sánchez-Gallego , José, Antonio , Felipe, Rojas , Santana, Santiago , Basílio, Schiavon , Ricardo, Schimoia , Jaderson, Schlafly , Edward, Schlegel , David, Schneider , Donald, Schuster , William, Schwope , Axel, Seo , Hee-Jong, Serenelli , Aldo, Shen , Shiyin, Shen , Yue, Shetrone , Matthew, Shull , Michael, Aguirre , Silva, Simon , Joshua, Skrutskie , Mike, Slosar , Anže, Smethurst , Rebecca, Smith , Verne, Sobeck , Jennifer, Somers , Garrett, Souter , Barbara, Souto , Diogo, Spindler , Ashley, Stark , David, Stassun , Keivan, Steinmetz , Matthias, Stello , Dennis, Storchi-Bergmann , Thaisa, Streblyanska , Alina, Stringfellow , Guy, Suárez , Genaro, Sun , Jing, Szigeti , Laszlo, Taghizadeh-Popp , Manuchehr, talbot , michael, Tang , Baitian, Tao , Charling, Tayar , Jamie, Tembe , Mita, Teske , Johanna, Aniruddha R. , Thakar, Daniel , Thomas, Tissera , Patricia, Tojeiro , Rita, Tremonti , Christy, Troup , Nicholas W., Urry , Meg, Valenzuela , O., van den Bosch , Remco, Vargas-González , Jaime, Magaña , Mariana Vargas, Vazquez , Jose Alberto, Villanova , Sandro, Vogt , Nicole, Wake , David, Wang , Yuting, Weaver , Benjamin Alan, Weijmans , Anne-Marie, Weinberg , David H., Westfall , Kyle B., Whelan , David G., Wilcots , Eric, Wild , Vivienne, Williams , Rob A., Wilson , John, Wood-Vasey , W.M., Wylezalek , Dominika, Xiao , Ting, Yan , Renbin, Yang , Meng, Ybarra , Jason E., Yèche , Christophe, Zakamska , Nadia, Zamora , Olga, Zarrouk , Pauline, Zasowski , Gail, Zhang , Kai, Zhao , Chang, Zhao , Gong-Bo, Zheng , Zheng, Zhou , Zhi-Min, Zhu , Guangtun, Zinn , Joel C., Zou , Hu, 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), Department of Astrophysical Sciences [Princeton], Princeton University, 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), Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Université Paris Diderot - Paris 7 (UPD7), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, 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), Département de Physique des Particules (ex SPP) (DPhP), 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, European Southern Observatory (ESO), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Matemáticas [Madrid], Universidad Autónoma de Madrid (UAM), Department of Physics and Astronomy [Nashville], Vanderbilt University [Nashville], Korea Institute for Advanced Study (KIAS), Sainsbury Laboratory Cambridge University (SLCU), University of Cambridge [UK] (CAM), Wuhan University [China], Equipe de Recherche sur l’Utilisation des Données Individuelles en lien avec la Théorie Economique (ERUDITE), Université Paris-Est Marne-la-Vallée (UPEM)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Institute of Astronomy [Cambridge], Max-Planck-Institut für Astrophysik (MPA), Department of Physics and Astronomy [Rochester], University of Rochester [USA], Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Inflammation, Tissus épithéliaux et Cytokines (LITEC), Université de Poitiers, Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS (UMR_7596)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Universidad Politécnica de Madrid (UPM), Universidad de Jaén (UJA), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), University of Edinburgh, Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Alfred P. Sloan Foundation, Department of Energy (US), University of Utah, AVL, AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Astronomy and Astrophysics ( PENNSYLVANIA STATE UNIVERSITY ), PennState University [Pennsylvania] ( PSU ), Université Paris Diderot - Paris 7 ( UPD7 ), University of Pennsylvania [Philadelphia], 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'Etudes Spatiales ( CNES ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), California Institute of Technology ( CALTECH ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, University of Oxford [Oxford]-University of Oxford [Oxford], Imaging Diagnostic Center, Nanfang Hospital Guangzhou, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid ( UAM ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Carnegie Institution of Washington, AUTRES, Département de Physique des Particules (ex SPP) ( DPP ), 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, School of Physics and Astronomy, University of Birmingham [Birmingham], European Southern Observatory ( ESO ), Département de Physique Nucléaire (ex SPhN) ( DPHN ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Max-Planck-Institut für Astronomie ( MPIA ), STScI, University of California [Irvine] ( UCI ), ISO Data Centre ( ESA - Espagne ), European Space Agency ( ESA ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, Research Institute of Forest Resource Information Techniques, Chinese Academy of Forestry, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Korea Institute for Advanced Study ( KIAS ), Department of Astronomy ( Ohio State University ), Ohio State University [Columbus] ( OSU ), Institute of Infection, Immunity & Inflammation, University of Glasgow, Sainsbury Laboratory Cambridge, University of Cambridge [UK] ( CAM ), Equipe de Recherche sur l’Utilisation des Données Individuelles en lien avec la Théorie Economique ( ERUDITE ), Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Université Paris-Est Marne-la-Vallée ( UPEM ), Institute of Physics, Universidade de Brasilia [Brasília] ( UnB ), Department of Chemical and Biomolecular Engineering, University of California [Berkeley], Max-Planck-Institut für Astrophysik ( MPA ), Bioinformatics and Functional Genomics Research Group, Cancer Research Center (IBMCC-CIC, CSIC-USAL), University of Wisconsin-Madison [Madison], Texas Tech University Health Sciences Center, Texas Tech University [Lubbock] ( TTU ), Institute for Astronomy ( IfA ), University of Hawaii, Research Institute of Organic Agriculture ( FiBL ), Dept. of Physics, Princess Margaret Hospital, University of Toronto-Princess Margaret Hospital, J. A. Baker Institute, Cornell University, The Observatories of the Carnegie Institution for Science, Economics, Bangor, Physics Department, Carnegie Mellon University [Pittsburgh] ( CMU ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Inflammation, Tissus épithéliaux et Cytokines ( LITEC ), School of Physics, Korea Institute for Advanced Study, Korea Institute for Advanced Study-Korea Institute for Advanced Study, Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques ( REHSEIS ), Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Universidad Politécnica de Madrid ( UPM ), Universidad de Jaén ( UJA ), Institute of Space Sciences [Barcelona] ( ICE-CSIC ), Spanish National Research Council [Madrid] ( CSIC ), Department of Physics and Astronomy - Stellar Astrophysics Centre, Department of Physics, The Leverhulme Trust, University of St Andrews. School of Physics and Astronomy, University of St Andrews. Centre for Contemporary Art, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Département de Physique des Particules (ex SPP) (DPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universidad Autonoma de Madrid (UAM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of California [Irvine] (UCI), University of California-University of California, ISO Data Centre (ESA - Espagne), European Space Agency (ESA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Universidade de Brasilia [Brasília] (UnB), University of Wisconsin-Madison, Texas Tech University [Lubbock] (TTU), Institute for Astronomy [Honolulu] (IfA), University of Hawai'i [Honolulu] (UH), Research Institute of Organic Agriculture (FiBL), University of Toronto, Bangor University, Carnegie Mellon University [Pittsburgh] (CMU), Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), 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 Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Université Paris-Est Marne-la-Vallée (UPEM), Research Institute of Organic Agriculture - Forschungsinstitut für biologischen Landbau (FiBL), Cornell University [New York], Carnegie Observatories, Carnegie Institution for Science [Washington], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), 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), 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
Astrophysics, E-SCIENCE, 01 natural sciences, HISTORIES, TARGET SELECTION, Observatory, QB Astronomy, 010303 astronomy & astrophysics, R2C, QC, media_common, QB, Physics, CATALOGS, Point (typography), ~DC~, Astrophysics::Instrumentation and Methods for Astrophysics, 520 Astronomie und zugeordnete Wissenschaften, atlases, GALAXIES, X-RAY SURVEYS, BDC, Astrophysics - Instrumentation and Methods for Astrophysics, METALLICITY, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], TELESCOPE, media_common.quotation_subject, astro-ph.GA, Phase (waves), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Data-driven, Data cube, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, 0103 physical sciences, ddc:530, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, 115 Astronomy, Space science, Catalogues, 530 Physik, Astrophysics - Astrophysics of Galaxies, Galaxy, Baryon, QC Physics, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), ddc:520, catalogs, astro-ph.IM, SDSS-IV MANGA
Abstract

Open Access. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI., The fourth generation of the Sloan Digital Sky Survey (SDSS-IV) has been in operation since 2014 July. This paper describes the second data release from this phase, and the 14th from SDSS overall (making this Data Release Fourteen or DR14). This release makes the data taken by SDSS-IV in its first two years of operation (2014-2016 July) public. Like all previous SDSS releases, DR14 is cumulative, including the most recent reductions and calibrations of all data taken by SDSS since the first phase began operations in 2000. New in DR14 is the first public release of data from the extended Baryon Oscillation Spectroscopic Survey; the first data from the second phase of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE-2), including stellar parameter estimates from an innovative data-driven machine-learning algorithm known as ¿The Cannon¿ and almost twice as many data cubes from the Mapping Nearby Galaxies at APO (MaNGA) survey as were in the previous release (N = 2812 in total). This paper describes the location and format of the publicly available data from the SDSS-IV surveys. We provide references to the important technical papers describing how these data have been taken (both targeting and observation details) and processed for scientific use. The SDSS web site (www.sdss.org) has been updated for this release and provides links to data downloads, as well as tutorials and examples of data use. SDSS-IV is planning to continue to collect astronomical data until 2020 and will be followed by SDSS-V. © 2018. The American Astronomical Society.., Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org.

Published
2018

6. Evidence for the Accretion of Gas in Star-forming Galaxies: High N/O Abundances in Regions of Anomalously Low Metallicity.

Author

Luo, Yuanze, Heckman, Timothy, Hwang, Hsiang-Chih, Rowlands, Kate, Sánchez-Menguiano, Laura, Riffel, Rogério, Bizyaev, Dmitry, Andrews, Brett H., Fernández-Trincado, José G., Drory, Niv, Almeida, Jorge Sánchez, Maiolino, Roberto, Lane, Richard R., and Argudo-Fernández, Maria

Subjects
INTERSTELLAR medium, GALAXIES, STAR formation, GALACTIC evolution, GASES
Abstract

While all models for the evolution of galaxies require the accretion of gas to sustain their growth via on-going star formation, it has proven difficult to directly detect this inflowing material. In this paper we use data of nearby star-forming galaxies in the SDSS IV Mapping Nearby Galaxies at Apache Point Observatory survey to search for evidence of accretion imprinted in the chemical composition of the interstellar medium. We measure both the O/H and N/O abundance ratios in regions previously identified as having anomalously low values of O/H. We show that the unusual locations of these regions in the N/O versus O/H plane indicate that they have been created through the mixing of disk gas having higher metallicity with accreted gas having lower metallicity. Taken together with previous analysis on these anomalously low-metallicity regions, these results imply that accretion of metal-poor gas can probably sustain star formation in present-day late-type galaxies. [ABSTRACT FROM AUTHOR]

Published
2021
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7. SDSS-IV MaNGA: identification of active galactic nuclei in optical integral field unit surveys.

Author

Wylezalek, Dominika, Zakamska, Nadia L., Greene, Jenny E., Riffel, Rogemar A., Drory, Niv, Andrews, Brett H., Merloni, Andrea, and Thomas, Daniel

Subjects
ACTIVE galactic nuclei, GALACTIC nuclei, GALAXIES, IONIZED gases, PHOTOIONIZATION, EARLY stars, STAR formation
Abstract

In this paper, we investigate 2727 galaxies observed by MaNGA as of 2016 June to develop spatially resolved techniques for identifying signatures of active galactic nuclei (AGNs). We identify 303AGNcandidates. The additional spatial dimension imposes challenges in identifying AGNs due to contamination from diffuse ionized gas, extraplanar gas and photoionization by hot stars. We show that the combination of spatially resolved line diagnostic diagrams and additional cuts on Hα surface brightness and Hα equivalent width can distinguish between AGN-like signatures and high-metallicity galaxies with low-ionization nuclear emission-line regions-like spectra. Low-mass galaxies with high specific star formation rates are particularly difficult to diagnose and routinely show diagnostic line ratios outside of the standard star formation locus.We develop a new diagnostic -- the distance from the standard diagnostic line in the line-ratio space -- to evaluate the significance of the deviation from the star formation locus. We find 173 galaxies that would not have been selected as AGN candidates based on single-fibre spectral measurements but exhibit photoionization signatures suggestive of AGN activity in the Mapping Nearby Galaxies at APO resolved observations, underscoring the power of large integral field unit surveys. A complete census of these new AGN candidates is necessary to understand their nature and probe the complex co-evolution of supermassive black holes and their hosts. [ABSTRACT FROM AUTHOR]

Published
2018
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8. THE MASS-METALLICITY RELATION WITH THE DIRECT METHOD ON STACKED SPECTRA OF SDSS GALAXIES.

Author

ANDREWS, BRETT H. and MARTINI, PAUL

Subjects
*STELLAR mass, *GALACTIC evolution, *STAR formation, *SIGNAL-to-noise ratio
Abstract

The relation between galaxy stellar mass and gas-phase metallicity is a sensitive diagnostic of the main processes that drive galaxy evolution, namely cosmological gas inflow, metal production in stars, and gas outflow via galactic winds. We employed the direct method to measure the metallicities of ~200,000 star-forming galaxies from the Sloan Digital Sky Survey that were stacked in bins of (1) stellar mass and (2) both stellar mass and star formation rate (SFR) to significantly enhance the signal-to-noise ratio of the weak [O iii] λ4363 and [O ii] λλ7320, 7330 auroral lines required to apply the direct method. These metallicity measurements span three decades in stellar mass from log(M" /M☉) = 7.4-10.5, which allows the direct method mass-metallicity relation to simultaneously capture the high-mass turnover and extend a full decade lower in mass than previous studies that employed more uncertain strong linemethods. The direct method mass-metallicity relation rises steeply at low mass (O/H∝M" 1/2) until it turns over at log(M" /M☉) = 8.9 and asymptotes to 12 + log(O/H) = 8.8 at high mass. The direct method mass-metallicity relation has a steeper slope, a lower turnover mass, and a factor of two to three greater dependence on SFR than strong line mass-metallicity relations. Furthermore, the SFR-dependence appears monotonic with stellar mass, unlike strong line mass-metallicity relations.We also measure the N/O abundance ratio, an important tracer of star formation history, and find the clear signature of primary and secondary nitrogen enrichment. N/O correlates tightly with oxygen abundance, and even more so with stellar mass. [ABSTRACT FROM AUTHOR]

Published
2013
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