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The Stripe 82 Massive Galaxy Project. III. A lack of growth among Massive Galaxies

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The Stripe 82 Massive Galaxy Project. III. A lack of growth among Massive Galaxies. / Bundy, Kevin; Leauthaud, Alexie; Saito, Shun; Maraston, Claudia; Wake, David A.; Thomas, Daniel.

In: The Astrophysical Journal, Vol. 851, No. 1, 34, 08.12.2017.

Research output: Contribution to journalArticle

Harvard

Bundy, K, Leauthaud, A, Saito, S, Maraston, C, Wake, DA & Thomas, D 2017, 'The Stripe 82 Massive Galaxy Project. III. A lack of growth among Massive Galaxies', The Astrophysical Journal, vol. 851, no. 1, 34. https://doi.org/10.3847/1538-4357/aa9896

APA

Bundy, K., Leauthaud, A., Saito, S., Maraston, C., Wake, D. A., & Thomas, D. (2017). The Stripe 82 Massive Galaxy Project. III. A lack of growth among Massive Galaxies. The Astrophysical Journal, 851(1), [34]. https://doi.org/10.3847/1538-4357/aa9896

Vancouver

Author

Bundy, Kevin ; Leauthaud, Alexie ; Saito, Shun ; Maraston, Claudia ; Wake, David A. ; Thomas, Daniel. / The Stripe 82 Massive Galaxy Project. III. A lack of growth among Massive Galaxies. In: The Astrophysical Journal. 2017 ; Vol. 851, No. 1.

Bibtex

@article{8e538e1a2a1f408e95d3b153fb8e88c3,
title = "The Stripe 82 Massive Galaxy Project. III. A lack of growth among Massive Galaxies",
abstract = "The average stellar mass (M*) of high-mass galaxies (logM*/M⊙ > 11.5) is expected to grow by ~30% since z~1, largely through ongoing mergers that are also invoked to explain the observed increase in galaxy sizes. Direct evidence for the corresponding growth in stellar mass has been elusive, however, in part because the volumes sampled by previous redshift surveys have been too small to yield reliable statistics. In this work, we make use of the Stripe 82 Massive Galaxy Catalog to build a mass-limited sample of 41,770 galaxies (logM*/M⊙ >11.2) with optical-to-near-IR photometry and a large fraction (>55%) of spectroscopic redshifts. Our sample spans 139 deg2, significantly larger than most previous efforts. After accounting for a number of potential systematic errors, including the effects of M* scatter, we measure galaxy stellar mass functions over 0.3 < z < 0.65 and detect no growth in the typical M * of massive galaxies with an uncertainty of 9%. This confidence level is dominated by uncertainties in the star formation history assumed for M*estimates, although our inability to characterize low surface-brightness outskirts may be the most important limitation of our study. Even among these high-mass galaxies, we find evidence for differential evolution when splitting the sample by recent star formation (SF) activity. While low-SF systems appear to become completely passive, we find a mostly sub-dominant population of galaxies with residual, but low rates of star formation (~1 M⊙ yr-1) number density does not evolve. Interestingly, these galaxies become more prominent at higher M*, representing ~10% of all galaxies at 1012M* M⊙ and perhaps dominating at even larger masses.",
keywords = "astro-ph.GA, galaxies: abundances",
author = "Kevin Bundy and Alexie Leauthaud and Shun Saito and Claudia Maraston and Wake, {David A.} and Daniel Thomas",
note = "Accepted in ApJ",
year = "2017",
month = dec,
day = "8",
doi = "10.3847/1538-4357/aa9896",
language = "English",
volume = "851",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing",
number = "1",

}

RIS

TY - JOUR

T1 - The Stripe 82 Massive Galaxy Project. III. A lack of growth among Massive Galaxies

AU - Bundy, Kevin

AU - Leauthaud, Alexie

AU - Saito, Shun

AU - Maraston, Claudia

AU - Wake, David A.

AU - Thomas, Daniel

N1 - Accepted in ApJ

PY - 2017/12/8

Y1 - 2017/12/8

N2 - The average stellar mass (M*) of high-mass galaxies (logM*/M⊙ > 11.5) is expected to grow by ~30% since z~1, largely through ongoing mergers that are also invoked to explain the observed increase in galaxy sizes. Direct evidence for the corresponding growth in stellar mass has been elusive, however, in part because the volumes sampled by previous redshift surveys have been too small to yield reliable statistics. In this work, we make use of the Stripe 82 Massive Galaxy Catalog to build a mass-limited sample of 41,770 galaxies (logM*/M⊙ >11.2) with optical-to-near-IR photometry and a large fraction (>55%) of spectroscopic redshifts. Our sample spans 139 deg2, significantly larger than most previous efforts. After accounting for a number of potential systematic errors, including the effects of M* scatter, we measure galaxy stellar mass functions over 0.3 < z < 0.65 and detect no growth in the typical M * of massive galaxies with an uncertainty of 9%. This confidence level is dominated by uncertainties in the star formation history assumed for M*estimates, although our inability to characterize low surface-brightness outskirts may be the most important limitation of our study. Even among these high-mass galaxies, we find evidence for differential evolution when splitting the sample by recent star formation (SF) activity. While low-SF systems appear to become completely passive, we find a mostly sub-dominant population of galaxies with residual, but low rates of star formation (~1 M⊙ yr-1) number density does not evolve. Interestingly, these galaxies become more prominent at higher M*, representing ~10% of all galaxies at 1012M* M⊙ and perhaps dominating at even larger masses.

AB - The average stellar mass (M*) of high-mass galaxies (logM*/M⊙ > 11.5) is expected to grow by ~30% since z~1, largely through ongoing mergers that are also invoked to explain the observed increase in galaxy sizes. Direct evidence for the corresponding growth in stellar mass has been elusive, however, in part because the volumes sampled by previous redshift surveys have been too small to yield reliable statistics. In this work, we make use of the Stripe 82 Massive Galaxy Catalog to build a mass-limited sample of 41,770 galaxies (logM*/M⊙ >11.2) with optical-to-near-IR photometry and a large fraction (>55%) of spectroscopic redshifts. Our sample spans 139 deg2, significantly larger than most previous efforts. After accounting for a number of potential systematic errors, including the effects of M* scatter, we measure galaxy stellar mass functions over 0.3 < z < 0.65 and detect no growth in the typical M * of massive galaxies with an uncertainty of 9%. This confidence level is dominated by uncertainties in the star formation history assumed for M*estimates, although our inability to characterize low surface-brightness outskirts may be the most important limitation of our study. Even among these high-mass galaxies, we find evidence for differential evolution when splitting the sample by recent star formation (SF) activity. While low-SF systems appear to become completely passive, we find a mostly sub-dominant population of galaxies with residual, but low rates of star formation (~1 M⊙ yr-1) number density does not evolve. Interestingly, these galaxies become more prominent at higher M*, representing ~10% of all galaxies at 1012M* M⊙ and perhaps dominating at even larger masses.

KW - astro-ph.GA

KW - galaxies: abundances

U2 - 10.3847/1538-4357/aa9896

DO - 10.3847/1538-4357/aa9896

M3 - Article

VL - 851

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 34

ER -

ID: 8557594