The physical properties of star-forming galaxies in the low-redshift universe

By J. Brinchmann, S. Charlot, Simon D. M. White, Christy A. Tremonti, G. Kauffmann, T. Heckman, J. Brinkmann. 2003

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We present a comprehensive study of the physical properties of ∼ 10 5 galaxies with measurable star formation in the Sloan Digital Sky Survey (SDSS). By comparing physical information extracted from the emission lines with continuum properties, we build up a picture of the nature of star-forming galaxies at z < 0.2. We develop a method for aperture correction using resolved imaging and show that our method takes out essentially all aperture bias in the star formation rate (SFR) estimates, allowing an accurate estimate of the total SFRs in galaxies. We determine the SFR density to be 1.915 +0.02 −0.01 (random) +0.14

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ad6e9e16252b74aa4c65def5ef98d41ed2b5e82e

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. C. Conroy
5. R. Somerville
6. Volker Springel
7. Simon D. M. White
8. A. Dekel

Citations in the corpus

• On the impact of empirical and theoretical star formation laws on galaxy formation (2010, methodology): “M plane based on the Sloan Digital Sky C© 2011 The Authors, MNRAS 416, 1566–1584 Monthly Notices of the Royal Astronomical Society C© 2011 RAS Survey Data Release 7 (SDSS DR7),4 which corresponds to an update of the Brinchmann et al. (2004) analysis.”
• Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, background): “…galaxies appear to be consuming their gas rapidly enough that fuel must be constantly replenished (Tacconi et al. 2010; Papovich et al. 2010), but merger-induced starbursts do not appears to be driving global star formation (Brinchmann et al. 2004; Noeske et al. 2007; Jogee et al. 2009).”
• GALAXY PAIRS IN THE SLOAN DIGITAL SKY SURVEY. I. STAR FORMATION, ACTIVE GALACTIC NUCLEUS FRACTION, AND THE LUMINOSITY/MASS–METALLICITY RELATION (2008, methodology): “…compiled by the Munich group.4 Pipeline processing which fits galaxy templates and spectral synthesis models to the spectra yields physical properties such as stellar masses and SFRs as well as measurements of line fluxes (e.g., Kauffmann et al. 2003b; Brinchmann et al. 2004; Tremonti et al. 2004).”
• The star formation histories of galaxies in the sloan digital sky survey (2006, methodology): “…attempts have been made previously to study in detail the physical properties of the SDSS galaxies either by using selected features in the spectra (Brinchmann et al. 2004; Kauffmann E-mail: raulj@physics.upenn.edu †Scottish Universities Physics Alliance. et al.2004; Tremonti et al. 2004) or using…”
• New insights into the stellar content and physical conditions of star-forming galaxies at z = 2-3 from spectral modelling (2008, methodology): “In our case, the equivalent width of the Hα emission line is closely related to the specific star formation rate (SFR/M , where M is the assembled stellar mass), and both quantities then obviously depend on M (Brinchmann et al. 2004).”
• Semi-empirical analysis of Sloan Digital Sky Survey galaxies – II. The bimodality of the galaxy population revisited (2005, methodology): “Journal compilation C© 2006 RAS, MNRAS 370, 721–737 to that of Brinchmann et al. (2004).”
• The Properties of Ultraviolet-luminous Galaxies at the Current Epoch (2004, background): “Salim et al. (2005) and Brinchmann et al. (2004) have shown that the specific star formation rates in galaxies correlate strongly with the FUV-optical colors and the 4000 breakÅ amplitude (D4000), respectively.”
• RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES (2009, background): “The empirical relation for starbursts closely follows the model predictions for b = 5, which falls in the range where starbursts are commonly found (b > 2-3; see Brinchmann et al. 2004 and references therein).”
• Chemical Abundances of DEEP2 Star-forming Galaxies at z~1.0-1.5 (2005, background): “Finally, we consider the contribution of an AGN.”
• CONSTRAINING THE LOW-MASS SLOPE OF THE STAR FORMATION SEQUENCE AT 0.5 < z < 2.5 (2014, background): “…a picture where the majority of star-forming galaxies follow a relatively tight relation between star formation rate (SFR ≡ Ψ) and stellar mass (M ) (Brinchmann et al. 2004; Noeske et al. 2007; Elbaz et al. 2007; Daddi et al. 2007; Magdis et al. 2010; González et al. 2010; Whitaker et al.…”
• Formation of z~6 Quasars from Hierarchical Galaxy Mergers (2006, background): “The specific star formation rate (SSFR), or ‘‘b parameter’’ (e.g., Brinchmann et al. 2004), is defined as SSFR ¼ SFR/Mstar.”
• Eliminating error in the chemical abundance scale for extragalactic H ii regions (2012, background): “…are suggesting that there actually is a deep physical connection between metallicities, masses and starformation rate (e.g. Tremonti et al. 2004; Brinchmann et al. 2004; Kewley & Ellison 2008; Lara-López et al. 2010a,b), although these results are mainly based on trends of the chemical…”
• An Hα Imaging Survey of Galaxies in the Local 11 Mpc Volume (2004, background): “…spectroscopic survey that uniformly targets galaxies within a given magnitude and redshift range, such as the Sloan Digital Sky Survey (SDSS), and SDSS data have produced the most comprehensive characterization of the low-redshift star-forming galaxy population to date (Brinchmann et al. 2004).”
• THE NINTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY (2012, methodology): “The Galspec product (Kauffmann et al. 2003; Brinchmann et al. 2004; Tremonti et al. 2004) provided by the Max Planck Institute for Astrophysics and the Johns Hopkins University (MPA-JHU) introduced in DR8 is maintained for SDSS-I/II galaxies, but is not available for SDSS-III BOSS spectra.”
• Physical properties and environments of nearby galaxies (2009, methodology): “In Figure 2, we show a small sampling of the major trends in galaxy spectroscopic properties in the optical, using the same sample as in Figure 1, with parameters determined by Brinchmann et al. (2004) and Tremonti et al. (2004) for our SDSS sample.”