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A CRITICAL ASSESSMENT OF STELLAR MASS MEASUREMENT METHODS

Bahram MobasherDepartment of Physics and Astronomy, University of Cali-fornia, Riverside, CA 92521Tomas DahlenSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218Henry C. FergusonSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218Viviana AcquavivaPhysics Department, CUNY NYC College of Technology, 300 Jay Street, Brooklyn, NY 11201Guillermo BarroUCO/Lick Observatory, Department of Astronomy and As-trophysics, University of California, Santa Cruz, CA 95064Steven L. FinkelsteinDepartment of Astronomy, The University of Texas at Austin, Austin, TX 78712A. FontanaINAF, Osservatorio Astronomico di Roma, Via Frascati 33, I00040, Monteporzio, ItalyRuth GruetzbauchCenter for Astronomy and Astrophysics, Observatorio Astro-nomico de Lisboa, Tapada da Ajuda, 1349-018, Lisboa, PortugalSeth JohnsonDepartment of Astronomy, University of Massachusetts, 710 North Plesant Street, Amherst, MA 01003Yu LuKavli Institute for Particle Physics and Cosmology, Stanford University, Stanford, CA 94305Casey PapovichDepartment of Physics and astronomy, Texas A&M Re-search Foundation, College Station, TX 77843Janine PforrNational Optical Astronomy Observatories, 950 N Cherry Avenue, Tucson, AZ 85719M. SalvatoMax-Planck-Institut fr extraterrestrische Physik, Giessen-bachstrasse 1, D-85748 Garching bei Mnchen, GermanyRachel S. SomervilleDepartment of Physics and Astronomy, Rutgers, The State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854Tommy WiklindJoint ALMA Observatory, Alonso de Cordova 3107, Vi-tacura, Santiago, ChileStijn WuytsMax-Planck-Institut fr extraterrestrische Physik, Giessen-bachstrasse 1, D-85748 Garching bei Mnchen, GermanyM. L. N. AshbyDepartment of Astronomy, University of Michigan, 500 Chruch St., Ann Arbor, MI 48109Eric F. BellDepartment of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USAChristopher J. ConseliceSchool of Physics and Astronomy, University of Notting-ham, Nottingham, UKMark E. DickinsonNational Optical Astronomy Observatories, 950 N Cherry Avenue, Tucson, AZ 85719Sandra M. FaberUCO/Lick Observatory, Department of Astronomy and As-trophysics, University of California, Santa Cruz, CA 95064Giovanni FazioDepartment of Astronomy, University of Michigan, 500 Chruch St., Ann Arbor, MI 48109Kristian FinlatorDark Cosmology Center, Niels Bohr Institute, University of Copenhagen, DenmarkAudrey GalametzINAF, Osservatorio Astronomico di Roma, Via Frascati 33, I00040, Monteporzio, ItalyEric GawiserDepartment of Physics and Astronomy, Rutgers, The State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854Mauro GiavaliscoDepartment of Astronomy, University of Massachusetts, 710 North Plesant Street, Amherst, MA 01003A. GrazianINAF, Osservatorio Astronomico di Roma, Via Frascati 33, I00040, Monteporzio, ItalyNorman A. GroginSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218Yicheng GuoUCO/Lick Observatory, Department of Astronomy and As-trophysics, University of California, Santa Cruz, CA 95064Nimish P. HathiLAM -Laboratoire d'Astrophysique de Marseille, 38, Rue R. Jollot-Curie, 13388 Marseille, Cedex 13, FranceDale KocevskiDepartment of Physics and Astronomy, University of Ken-tucky, Lexington, KY 40506A. M. KoekemoerSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218David C. KooUCO/Lick Observatory, Department of Astronomy and As-trophysics, University of California, Santa Cruz, CA 95064Jeffrey A. NewmanDepartment of Physics and Astronomy, University of Pitts-burgh, Pittsburgh, PA 15260Naveen ReddyDepartment of Physics and Astronomy, University of Cali-fornia, Riverside, CA 92521P. SantiniINAF, Osservatorio Astronomico di Roma, Via Frascati 33, I00040, Monteporzio, ItalyRisa H. WechslerKavli Institute for Particle Physics and Cosmology, Stanford University, Stanford, CA 94305

2015en

ABI

Annotatsiya

This is the second paper in a series aimed at investigating the main sources of uncertainty in measuring the observable parameters in galaxies from their Spectral Energy Distributions (SEDs). In the first paper (Dahlen et al. 2013) we presented a detailed account of the photometric redshift measurements and an error analysis of this process. In this paper we perform a comprehensive study of the main sources of random and systematic error in stellar mass estimates for galaxies, and their relative contributions to the associated error budget. Since there is no prior knowledge of the stellar mass of galaxies (unlike their photometric redshifts), we use mock galaxy catalogs with simulated multiwaveband photometry and known redshift, stellar mass, age and extinction for individual galaxies. The multi-waveband photometry for the simulated galaxies were generated in 13 filters spanning from U-band to mid-infrared wavelengths. Given different parameters affecting stellar mass measurement (photometric S/N ratios, SED fitting errors and systematic effects), the inherent degeneracies and correlated errors, we formulated different simulated galaxy catalogs to quantify these effects individually. For comparison, we also generated catalogs based on observed photometric data of real galaxies in the GOODS-South field, spanning the same passbands. The simulated and observed catalogs were provided to a number of teams within the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) collaboration to estimate the stellar masses for individual galaxies. A total of eleven teams participated, with different combinations of stellar mass measurement codes/methods, population synthesis models, star formation histories, extinction and age. For each simulated galaxy, the differences between the input stellar masses, M input , and those estimated by each team, M est , is defined as log(M ) log(M estimated ) -log(M input ), and used to identify the most fundamental parameters affecting stellar mass estimate in galaxies, with the following results: (1). no significant bias in log(M ) was found among different codes, with all having comparable scatter ((log(M )) = 0.136 dex). The estimated stellar mass values are seriously affected by low photometric S/N ratios, with the rms scatter increasing for galaxies with H AB > 26 mag.; (2). A source of error contributing to the scatter in log(M ) is found to be due to photometric uncertainties (0.136 dex) and low resolution in age and extinction grids when generating the SED templates;(3). The median of stellar masses among different methods provides a stable measure of the mass associated with any given galaxy ((log(M )) = 0.142 dex); (4). The log(M ) values are strongly correlate with deviations in age (defined as the difference between the estimated and expected values), with a weaker correlation with extinction; (5). the rms scatter in the estimated stellar masses due to free parameters (after fixing redshifts and IMF) are quantified and found to be (log(M )) = 0.110 dex; (6). Using the observed data, we studied the sensitivity of stellar masses to both the population synthesis codes and inclusion of nebular emission lines and found them to affect the stellar mass by 0.2 dex and 0.3 dex respectively.

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DOI: 10.1088/0004-637x/808/1/101

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