The UV-Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star-forming Sequence

By David Schiminovich, T. Wyder, D. Martin, B. D. Johnson, S. Salim, M. Seibert, M. Treyer, Tamás Budavári, C. Hoopes, M. Zamojski and 16 more. 2007

266 citations recorded by the source corpus.

We use the UV-optical color magnitude diagram in combination with spectroscopic and photometric measurements derived from the SDSS spectroscopic sample to measure the distribution of galaxies in the local universe (z < 0.25) and their physical properties as a function of specific star formation rate (SFR/M⋆) and stellar mass (M⋆). Throughout this study our emphasis is on the properties of galaxies on and off of a local “star-forming sequence.” We discuss how the physical characteristics of galaxies along this sequence are related to scaling relations typically derived for galaxies of different morphological types. We find, among other trends, that our measure of the star formation rate surface density, ΣSFR, is nearly constant along this sequence. We discuss this result and implications for galaxies at higher redshift. For the first time, we report on measurements of the local UV luminosity function versus galaxy structural parameters, as well as inclination. We also split our sample into disk-dominated and bulge-dominated subsamples using the i-band Sersic index and find that disk-dominated galaxies occupy a very tight locus in SFR/M⋆ vs. M⋆ space, while bulge-dominated galaxies display a much larger spread of SFR/M⋆ at fixed stellar mass. A significant fraction of galaxies with SFR/M⋆ and ΣSFR above those on the “star-forming sequence” are bulge-dominated. We can use our derived distribution functions to ask whether a significant fraction of these galaxies may be experiencing a final episode of star formation (possibly induced by a merger or other burst), soon to be quenched, by determining whether this population can explain the growth rate of the non-star-forming galaxies on the “red sequence.” We find that this is a plausible scenario for bulge-dominated galaxies near the characteristic transition mass under reasonable assumptions regarding quenching timescales. Similarly, we use this technique to estimate the rate of mergers/starbursts that take galaxies off of the star-forming sequence and show that the implied merger rates are consistent with local measurements.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/c288ca0fff62c3672df736a2c454e4c9931e4f35

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Citations in the corpus

Fluctuations in the high-redshift Lyman–Werner background: close halo pairs as the origin of supermassive black holes (2008, background): “7 of Schiminovich et al. 2007).”
THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, unknown): “Also in the local universe GALEX/UV-based values around β = −0.35, consistent with our study, have been reported for galaxies taken from the Sloan Digital Sky Survey (SDSS) (Salim et al. 2007; Schiminovich et al. 2007).”
The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early-and late-type galaxies (2014, background): “…represent the transition population between the blue cloud of star-forming galaxies and the red sequence of quenched, passively evolving galaxies (e.g. Bell et al. 2004; Faber et al. 2007; Martin et al. 2007; Schiminovich et al. 2007; Wyder et al. 2007; Mendez et al. 2011; Gonçalves et al. 2012).”
The UV-Optical Galaxy Color-Magnitude Diagram. I. Basic Properties (2007, background): “In another paper, Schiminovich et al. (2007) have investigated the correlation of morphology and other characteristics with position in the CMD.”
THE ARECIBO LEGACY FAST ALFA SURVEY: THE GALAXY POPULATION DETECTED BY ALFALFA (2012, background): “The bimodal distribution evident in the color-magnitude diagram (Baldry et al. 2004; Schiminovich et al. 2007) suggests a likely evolution scenario whereby galaxies in the blue cloud form stars vigorously and grow through mergers and later, after depleting their gas reservoirs, then migrate to the…”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, background): “These quiescent-classified systems, even while they occupy mostly the lower range on the M-SFR diagram, have a significant long tail up to higher SFRs that overlaps with the SF-systems (Schiminovich et al. 2007).”
Galaxies in a simulated ΛCDM universe – II. Observable properties and constraints on feedback (2009, background): “In addition, observed red sequence galaxies are preferentially early-type (morphologically) relative to galaxies on the star-forming sequence (e.g. Schiminovich et al. 2007) and suppressing accretion will not in itself change a galaxy’s morphology, though it can help preserve early types by…”
PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, background): “…almost linear relation between stellar mass (M*) and star formation rate (SFR), the ‘star-formation main sequence (MS)’ (e.g. Brinchmann et al. 2004, Schiminovich et al. 2007, Noeske et al. 2007, Daddi et al. 2007, Franx et al. 2008, Elbaz et al. 2007, 2011, Rodighiero et al. 2010, 2011, Peng et…”
COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, background): “…et al. 2011, Sargent et al. 2012), which is a fairly tight (±0.3 dex scatter), near-linear relationship between stellar mass and star formation rate (Schiminovich et al. 2007, Noeske et al. 2007, Elbaz et al. 2007, 2011, Daddi et al. 2007, Panella et al. 2009, Peng et al. 2010, Rodighiero et al.…”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, background): “By contrast, we identify quiescent and star-forming galaxies according to whether they lie on or below the star-forming sequence, which allows us to select a purer sample of quiescent galaxies (Salim et al. 2007; Schiminovich et al. 2007).”
A LINK BETWEEN STAR FORMATION QUENCHING AND INNER STELLAR MASS DENSITY IN SLOAN DIGITAL SKY SURVEY CENTRAL GALAXIES (2013, background): “Indeed, a similar threshold has been found when examining the Sersic index (Sersic 1968), which quantifies the mass (more precisely, the light) distribution (Driver et al. 2006; Schiminovich et al. 2007; Bell 2008).”
Dependence of galaxy quenching on halo mass and distance from its centre (2012, background): “This SFR derivation is described in more detail in (Schiminovich et al. 2007).”
The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2 (2013, background): “…between the star formation rate (SFR) and the stellar mass (M∗) of star-forming galaxies, SFR ∝ Mα∗ , with 0.5 < α < 1.0 (Brinchmann et al. 2004; Schiminovich et al. 2007; Noeske et al. 2007; Elbaz et al. 2007; Daddi et al. 2007; Pannella et al.(2009)Pannella Carilli; Dunne et al. 2009;…”
BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, background): “…galaxy surveys demonstrated that quiescence is strongly linked with structural and morphological parameters such as the Sérsic index, stellar mass density and the central velocity dispersion (Kauffmann et al. 2003, 2006; Schiminovich et al. 2007; Bell 2008; Fang et al. 2013; Cheung et al. 2012).”
LSD: Lyman-break galaxies Stellar populations and Dynamics – I. Mass, metallicity and gas at z∼ 3.1 (2009, background): “…differ significantly with what is invoked to explain the yields in the local universe: given the correlation between SFR and M∗ (Erb et al. 2006b; Schiminovich et al. 2007), at z ∼ 2 these outflows are expected to increase, rather than decrease, with stellar mass. Erb et al. (2006a) and Erb…”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “…of “quiescent” galaxies with predominantly old stellar populations, while the “blue cloud” represents “star forming” galaxies with younger stellar populations and significant ongoing star formation (Brinchmann et al. 2004, Kauffmann et al. 2003, Salim et al. 2007, Schiminovich et al. 2007).”
The dust scaling relations of the Herschel Reference Survey (2012, background): “The dust-to-stellar mass ratio strongly anti-correlates with M∗, NUV − r (a proxy for specific star formation rate, SSFR; e.g., Schiminovich et al. 2007) andµ∗, while a very weak non-linear trend is observed with the concentration index.”
The effect of the environment on the Hi scaling relations (2011, background): “Our findings nicely complement the scaling relations between SSFR and galaxy properties revealed by large optical and ultraviolet surveys (Blanton et al. 2005; Schiminovich et al. 2007).”