UV star formation rates in the local universe

Samir Salim, R. Michael Rich, Stéphane Charlot, Jarle Brinchmann, Benjamin D. Johnson, David Schiminovich, Mark Seibert, Ryan Mallery, Timothy M. Heckman, Karl Forster, Peter G. Friedman, D. Christopher Martin, Patrick Morrissey, Susan G. Neff, Todd Small, Ted K. Wyder, Luciana Bianchi, José Donas, Young Wook Lee, Barry F. MadoreBruno Milliard, Alex S. Szalay, Barry Y. Welsh, Sukyoung K. Yi

Research output: Contribution to journalArticle

968 Citations (Scopus)

Abstract

We measure star formation rates (SFRs) of ≈50,000 optically selected galaxies in the local universe (z ≈0.1) - from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the GALEX (ultraviolet) and SDSS photometry to a library of dust-attenuated population synthesis models. For star-forming galaxies, our UV-based SFRs compare remarkably well with those from SDSS-measured emission lines (Hα). Deviations from perfect agreement are shown to be due to differences in the dust attenuation estimates. In contrast to Hα measurements, UV provides reliable SFRs for galaxies with weak Ha, and where Ha is contaminated with AGN emission (1/2 of the sample). Using full-SED SFRs, we calibrate a simple prescription that uses GALEX far- and near-UV magnitudes to produce dust-corrected SFRs for normal star-forming galaxies. The specific SFR is considered as a function of stellar mass for (1) star-forming galaxies with no AGNs, (2) those hosting an AGN, and (3) galaxies without Ha emission. We find that the three have distinct star formation histories, with AGNs lying intermediate between the star-forming and the quiescent galaxies. Star-forming galaxies without an AGN lie on a relatively narrow linear sequence. Remarkably, galaxies hosting a strong AGN appear to represent the massive continuation of this sequence. On the other hand, weak AGNs, while also massive, have lower SFRs, sometimes extending to the realm of quiescent galaxies. We propose an evolutionary sequence for massive galaxies that smoothly connects normal star-forming galaxies to quiescent galaxies via strong and weak AGNs. We confirm that some galaxies with no Ha show signs of star formation in the UV We derive a cosmic star formation density at z = 0.1 with significantly smaller total error than previous measurements.

Original languageEnglish
Pages (from-to)267-292
Number of pages26
JournalAstrophysical Journal, Supplement Series
Volume173
Issue number2
DOIs
Publication statusPublished - 2007 Dec 1

Fingerprint

star formation rate
universe
galaxies
dust
stars
star formation
rate
stellar mass
history
photometry
gas
attenuation

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Salim, S., Rich, R. M., Charlot, S., Brinchmann, J., Johnson, B. D., Schiminovich, D., ... Yi, S. K. (2007). UV star formation rates in the local universe. Astrophysical Journal, Supplement Series, 173(2), 267-292. https://doi.org/10.1086/519218
Salim, Samir ; Rich, R. Michael ; Charlot, Stéphane ; Brinchmann, Jarle ; Johnson, Benjamin D. ; Schiminovich, David ; Seibert, Mark ; Mallery, Ryan ; Heckman, Timothy M. ; Forster, Karl ; Friedman, Peter G. ; Martin, D. Christopher ; Morrissey, Patrick ; Neff, Susan G. ; Small, Todd ; Wyder, Ted K. ; Bianchi, Luciana ; Donas, José ; Lee, Young Wook ; Madore, Barry F. ; Milliard, Bruno ; Szalay, Alex S. ; Welsh, Barry Y. ; Yi, Sukyoung K. / UV star formation rates in the local universe. In: Astrophysical Journal, Supplement Series. 2007 ; Vol. 173, No. 2. pp. 267-292.
@article{fafa0f547bb94228b1288d75e51ba2da,
title = "UV star formation rates in the local universe",
abstract = "We measure star formation rates (SFRs) of ≈50,000 optically selected galaxies in the local universe (z ≈0.1) - from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the GALEX (ultraviolet) and SDSS photometry to a library of dust-attenuated population synthesis models. For star-forming galaxies, our UV-based SFRs compare remarkably well with those from SDSS-measured emission lines (Hα). Deviations from perfect agreement are shown to be due to differences in the dust attenuation estimates. In contrast to Hα measurements, UV provides reliable SFRs for galaxies with weak Ha, and where Ha is contaminated with AGN emission (1/2 of the sample). Using full-SED SFRs, we calibrate a simple prescription that uses GALEX far- and near-UV magnitudes to produce dust-corrected SFRs for normal star-forming galaxies. The specific SFR is considered as a function of stellar mass for (1) star-forming galaxies with no AGNs, (2) those hosting an AGN, and (3) galaxies without Ha emission. We find that the three have distinct star formation histories, with AGNs lying intermediate between the star-forming and the quiescent galaxies. Star-forming galaxies without an AGN lie on a relatively narrow linear sequence. Remarkably, galaxies hosting a strong AGN appear to represent the massive continuation of this sequence. On the other hand, weak AGNs, while also massive, have lower SFRs, sometimes extending to the realm of quiescent galaxies. We propose an evolutionary sequence for massive galaxies that smoothly connects normal star-forming galaxies to quiescent galaxies via strong and weak AGNs. We confirm that some galaxies with no Ha show signs of star formation in the UV We derive a cosmic star formation density at z = 0.1 with significantly smaller total error than previous measurements.",
author = "Samir Salim and Rich, {R. Michael} and St{\'e}phane Charlot and Jarle Brinchmann and Johnson, {Benjamin D.} and David Schiminovich and Mark Seibert and Ryan Mallery and Heckman, {Timothy M.} and Karl Forster and Friedman, {Peter G.} and Martin, {D. Christopher} and Patrick Morrissey and Neff, {Susan G.} and Todd Small and Wyder, {Ted K.} and Luciana Bianchi and Jos{\'e} Donas and Lee, {Young Wook} and Madore, {Barry F.} and Bruno Milliard and Szalay, {Alex S.} and Welsh, {Barry Y.} and Yi, {Sukyoung K.}",
year = "2007",
month = "12",
day = "1",
doi = "10.1086/519218",
language = "English",
volume = "173",
pages = "267--292",
journal = "Astrophysical Journal, Supplement Series",
issn = "0067-0049",
publisher = "IOP Publishing Ltd.",
number = "2",

}

Salim, S, Rich, RM, Charlot, S, Brinchmann, J, Johnson, BD, Schiminovich, D, Seibert, M, Mallery, R, Heckman, TM, Forster, K, Friedman, PG, Martin, DC, Morrissey, P, Neff, SG, Small, T, Wyder, TK, Bianchi, L, Donas, J, Lee, YW, Madore, BF, Milliard, B, Szalay, AS, Welsh, BY & Yi, SK 2007, 'UV star formation rates in the local universe', Astrophysical Journal, Supplement Series, vol. 173, no. 2, pp. 267-292. https://doi.org/10.1086/519218

UV star formation rates in the local universe. / Salim, Samir; Rich, R. Michael; Charlot, Stéphane; Brinchmann, Jarle; Johnson, Benjamin D.; Schiminovich, David; Seibert, Mark; Mallery, Ryan; Heckman, Timothy M.; Forster, Karl; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Neff, Susan G.; Small, Todd; Wyder, Ted K.; Bianchi, Luciana; Donas, José; Lee, Young Wook; Madore, Barry F.; Milliard, Bruno; Szalay, Alex S.; Welsh, Barry Y.; Yi, Sukyoung K.

In: Astrophysical Journal, Supplement Series, Vol. 173, No. 2, 01.12.2007, p. 267-292.

Research output: Contribution to journalArticle

TY - JOUR

T1 - UV star formation rates in the local universe

AU - Salim, Samir

AU - Rich, R. Michael

AU - Charlot, Stéphane

AU - Brinchmann, Jarle

AU - Johnson, Benjamin D.

AU - Schiminovich, David

AU - Seibert, Mark

AU - Mallery, Ryan

AU - Heckman, Timothy M.

AU - Forster, Karl

AU - Friedman, Peter G.

AU - Martin, D. Christopher

AU - Morrissey, Patrick

AU - Neff, Susan G.

AU - Small, Todd

AU - Wyder, Ted K.

AU - Bianchi, Luciana

AU - Donas, José

AU - Lee, Young Wook

AU - Madore, Barry F.

AU - Milliard, Bruno

AU - Szalay, Alex S.

AU - Welsh, Barry Y.

AU - Yi, Sukyoung K.

PY - 2007/12/1

Y1 - 2007/12/1

N2 - We measure star formation rates (SFRs) of ≈50,000 optically selected galaxies in the local universe (z ≈0.1) - from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the GALEX (ultraviolet) and SDSS photometry to a library of dust-attenuated population synthesis models. For star-forming galaxies, our UV-based SFRs compare remarkably well with those from SDSS-measured emission lines (Hα). Deviations from perfect agreement are shown to be due to differences in the dust attenuation estimates. In contrast to Hα measurements, UV provides reliable SFRs for galaxies with weak Ha, and where Ha is contaminated with AGN emission (1/2 of the sample). Using full-SED SFRs, we calibrate a simple prescription that uses GALEX far- and near-UV magnitudes to produce dust-corrected SFRs for normal star-forming galaxies. The specific SFR is considered as a function of stellar mass for (1) star-forming galaxies with no AGNs, (2) those hosting an AGN, and (3) galaxies without Ha emission. We find that the three have distinct star formation histories, with AGNs lying intermediate between the star-forming and the quiescent galaxies. Star-forming galaxies without an AGN lie on a relatively narrow linear sequence. Remarkably, galaxies hosting a strong AGN appear to represent the massive continuation of this sequence. On the other hand, weak AGNs, while also massive, have lower SFRs, sometimes extending to the realm of quiescent galaxies. We propose an evolutionary sequence for massive galaxies that smoothly connects normal star-forming galaxies to quiescent galaxies via strong and weak AGNs. We confirm that some galaxies with no Ha show signs of star formation in the UV We derive a cosmic star formation density at z = 0.1 with significantly smaller total error than previous measurements.

AB - We measure star formation rates (SFRs) of ≈50,000 optically selected galaxies in the local universe (z ≈0.1) - from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the GALEX (ultraviolet) and SDSS photometry to a library of dust-attenuated population synthesis models. For star-forming galaxies, our UV-based SFRs compare remarkably well with those from SDSS-measured emission lines (Hα). Deviations from perfect agreement are shown to be due to differences in the dust attenuation estimates. In contrast to Hα measurements, UV provides reliable SFRs for galaxies with weak Ha, and where Ha is contaminated with AGN emission (1/2 of the sample). Using full-SED SFRs, we calibrate a simple prescription that uses GALEX far- and near-UV magnitudes to produce dust-corrected SFRs for normal star-forming galaxies. The specific SFR is considered as a function of stellar mass for (1) star-forming galaxies with no AGNs, (2) those hosting an AGN, and (3) galaxies without Ha emission. We find that the three have distinct star formation histories, with AGNs lying intermediate between the star-forming and the quiescent galaxies. Star-forming galaxies without an AGN lie on a relatively narrow linear sequence. Remarkably, galaxies hosting a strong AGN appear to represent the massive continuation of this sequence. On the other hand, weak AGNs, while also massive, have lower SFRs, sometimes extending to the realm of quiescent galaxies. We propose an evolutionary sequence for massive galaxies that smoothly connects normal star-forming galaxies to quiescent galaxies via strong and weak AGNs. We confirm that some galaxies with no Ha show signs of star formation in the UV We derive a cosmic star formation density at z = 0.1 with significantly smaller total error than previous measurements.

UR - http://www.scopus.com/inward/record.url?scp=39449092850&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=39449092850&partnerID=8YFLogxK

U2 - 10.1086/519218

DO - 10.1086/519218

M3 - Article

AN - SCOPUS:39449092850

VL - 173

SP - 267

EP - 292

JO - Astrophysical Journal, Supplement Series

JF - Astrophysical Journal, Supplement Series

SN - 0067-0049

IS - 2

ER -

Salim S, Rich RM, Charlot S, Brinchmann J, Johnson BD, Schiminovich D et al. UV star formation rates in the local universe. Astrophysical Journal, Supplement Series. 2007 Dec 1;173(2):267-292. https://doi.org/10.1086/519218