The UV-optical color magnitude diagram. II. Physical properties and morphological evolution on and off of a star-forming sequence

David Schiminovich, Ted K. Wyder, D. Christopher Martin, Benjamin D. Johnson, Samir Salim, Mark Seibert, Marie A. Treyer, Tamás Budavári, Charles Hoopes, Michel Zamojski, Tom A. Barlow, Karl G. Forster, Peter G. Friedman, Patrick Morrissey, Susan G. Neff, Todd A. Small, Luciana Bianchi, José Donas, Timothy M. Heckman, Young Wook LeeBarry F. Madore, Bruno Milliard, R. Michael Rich, Alex S. Szalay, Barry Y. Welsh, Sukyoung Yi

Research output: Contribution to journalArticle

214 Citations (Scopus)

Abstract

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.

Original languageEnglish
Pages (from-to)315-341
Number of pages27
JournalAstrophysical Journal, Supplement Series
Volume173
Issue number2
DOIs
Publication statusPublished - 2007 Dec 1

Fingerprint

color-magnitude diagram
physical property
physical properties
diagram
galaxies
stars
merger
star formation rate
stellar mass
rate
timescale
disk galaxies
loci
inclination
star formation
bursts
universe
distribution functions
quenching
luminosity

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Schiminovich, David ; Wyder, Ted K. ; Martin, D. Christopher ; Johnson, Benjamin D. ; Salim, Samir ; Seibert, Mark ; Treyer, Marie A. ; Budavári, Tamás ; Hoopes, Charles ; Zamojski, Michel ; Barlow, Tom A. ; Forster, Karl G. ; Friedman, Peter G. ; Morrissey, Patrick ; Neff, Susan G. ; Small, Todd A. ; Bianchi, Luciana ; Donas, José ; Heckman, Timothy M. ; Lee, Young Wook ; Madore, Barry F. ; Milliard, Bruno ; Rich, R. Michael ; Szalay, Alex S. ; Welsh, Barry Y. ; Yi, Sukyoung. / The UV-optical color magnitude diagram. II. Physical properties and morphological evolution on and off of a star-forming sequence. In: Astrophysical Journal, Supplement Series. 2007 ; Vol. 173, No. 2. pp. 315-341.
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abstract = "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.",
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Schiminovich, D, Wyder, TK, Martin, DC, Johnson, BD, Salim, S, Seibert, M, Treyer, MA, Budavári, T, Hoopes, C, Zamojski, M, Barlow, TA, Forster, KG, Friedman, PG, Morrissey, P, Neff, SG, Small, TA, Bianchi, L, Donas, J, Heckman, TM, Lee, YW, Madore, BF, Milliard, B, Rich, RM, Szalay, AS, Welsh, BY & Yi, S 2007, 'The UV-optical color magnitude diagram. II. Physical properties and morphological evolution on and off of a star-forming sequence', Astrophysical Journal, Supplement Series, vol. 173, no. 2, pp. 315-341. https://doi.org/10.1086/524659

The UV-optical color magnitude diagram. II. Physical properties and morphological evolution on and off of a star-forming sequence. / Schiminovich, David; Wyder, Ted K.; Martin, D. Christopher; Johnson, Benjamin D.; Salim, Samir; Seibert, Mark; Treyer, Marie A.; Budavári, Tamás; Hoopes, Charles; Zamojski, Michel; Barlow, Tom A.; Forster, Karl G.; Friedman, Peter G.; Morrissey, Patrick; Neff, Susan G.; Small, Todd A.; Bianchi, Luciana; Donas, José; Heckman, Timothy M.; Lee, Young Wook; Madore, Barry F.; Milliard, Bruno; Rich, R. Michael; Szalay, Alex S.; Welsh, Barry Y.; Yi, Sukyoung.

In: Astrophysical Journal, Supplement Series, Vol. 173, No. 2, 01.12.2007, p. 315-341.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The UV-optical color magnitude diagram. II. Physical properties and morphological evolution on and off of a star-forming sequence

AU - Schiminovich, David

AU - Wyder, Ted K.

AU - Martin, D. Christopher

AU - Johnson, Benjamin D.

AU - Salim, Samir

AU - Seibert, Mark

AU - Treyer, Marie A.

AU - Budavári, Tamás

AU - Hoopes, Charles

AU - Zamojski, Michel

AU - Barlow, Tom A.

AU - Forster, Karl G.

AU - Friedman, Peter G.

AU - Morrissey, Patrick

AU - Neff, Susan G.

AU - Small, Todd A.

AU - Bianchi, Luciana

AU - Donas, José

AU - Heckman, Timothy M.

AU - Lee, Young Wook

AU - Madore, Barry F.

AU - Milliard, Bruno

AU - Rich, R. Michael

AU - Szalay, Alex S.

AU - Welsh, Barry Y.

AU - Yi, Sukyoung

PY - 2007/12/1

Y1 - 2007/12/1

N2 - 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.

AB - 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.

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