DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS

By C. Hao, Robert C. Kennicutt Jr., Benjamin D. Johnson, D. Calzetti, D. Dale, John Moustakas. 2011

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We present new calibrations of far-ultraviolet (FUV) attenuation as derived from the total infrared to FUV luminosity ratio (IRX) and the FUV–near-UV(NUV) color. We find that the IRX-corrected FUV luminosities are tightly and linearly correlated with the attenuation-corrected Hα luminosities (as measured from the Balmer decrement), with an rms scatter of ±0.09 dex. The ratios of these attenuation-corrected FUV to Hα luminosities are consistent with evolutionary synthesis model predictions, assuming a constant star formation rate over 100 Myr, solar metallicity, and either a Salpeter or a Kroupa initial mass function with lower and upper mass limits of 0.1 and 100 M☉. The IRX-corrected FUV to Balmer-corrected Hα luminosity ratios do not show any trend with other galactic properties over the ranges covered by our sample objects. In contrast, FUV attenuation derived from the FUV–NUV color (UV spectral slope) show much larger random and systematic uncertainties. When compared to either Balmer-corrected Hα luminosities or IRX-corrected FUV luminosities the color-corrected FUV luminosities show ∼2.5 times larger rms scatter, and systematic nonlinear deviations as functions of luminosity and other parameters. Linear combinations of 25 μm and 1.4 GHz radio continuum luminosities with the observed FUV luminosities are also well correlated with the Balmer-corrected Hα luminosities. These results provide useful prescriptions for deriving attenuation-corrected star formation rates of galaxies based on linear combinations of UV and IR or radio luminosities, which are presented in convenient tabular form. Comparisons of our calibrations with attenuation corrections in the literature and with dust attenuation laws are also made.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, methodology): “We use the SFR parameterization of Hao et al. (2011), which combines far-UV (1500 Å) and TIR (Eqn.”
The lifecycle of molecular clouds in nearby star-forming disc galaxies (2019, background): “Infrared (IR) emission (e.g. at 24 µm) is also a common tracer of young star formation and can be used in particular to correct for extinction, which often heavily affects embedded young stars (e.g Kennicutt et al. 2009; Hao et al. 2011).”
The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, methodology): “In this paper, we choose GALEX FUV and MIPS 24 µm as reference SFR tracers to probe the unobscured and obscured star formation component, respectively, and we rely on the SFR calibrations presented by Hao et al. (2011) and Murphy et al. (2011 see Table A.1).”
Star Formation in the Milky Way and Nearby Galaxies (2012, methodology): “Table 2 lists examples of dust attenuation corrections using combinations of FUV and Hα fluxes with various infrared and radio tracers, taken from Hao et al. (2011) and Kennicutt et al. (2009), respectively.”
CONFIRMATION OF A STAR FORMATION BIAS IN TYPE Ia SUPERNOVA DISTANCES AND ITS EFFECT ON THE MEASUREMENT OF THE HUBBLE CONSTANT (2014, background): “Modifications to the initial mass function, metallicity, etc., can alter these conversion factors by ±0.2 dex; see Table 2 of Hao et al. (2011) for examples.”
GALEX–SDSS–WISE LEGACY CATALOG (GSWLC): STAR FORMATION RATES, STELLAR MASSES, AND DUST ATTENUATIONS OF 700,000 LOW-REDSHIFT GALAXIES (2016, result): “Evidence for a steeper-than-Calzetti curve has been found in other studies as well (Charlot & Fall 2000; Buat et al. 2011; Wild et al. 2011; Hao et al. 2011; Salmon et al. 2015), though not as steep as the one found here and in Conroy et al. More detailed investigation of these results and their…”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “For additional discussion on the nature of SFR indicators and the assumptions used to derive them, see Hao et al. (2011), Murphy et al. (2011), Murphy et al. (2012), KE12.”
Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe (2016, methodology): “Hao et al. (2011) perform the above conversion, from observed UV slope and luminosities to the dust-free UV luminosity, finding an RMS scatter of 0.23 dex between the observed and predicted Hα.”
The ATLAS3D Project – XXVIII. Dynamically driven star formation suppression in early-type galaxies (2014, methodology): “We also use a combined relation from Hao et al. (2011) to estimate the SFR from WISEandGALEXdata together.”
A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies (2019, background): “Other studies have built on these works and considered larger populations of local galaxies, aiming for internal consistency among the available tracers (Calzetti et al. 2010; Hao et al. 2011).”
GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies (2012, methodology): “Although the situation is more complex for non-starbursting galaxies (e.g. Burgarella et al., 2005; Boissier et al., 2007; Hao et al., 2011; Boquien et al., 2012, and references therein), this relation seems to hold for high-redshift systems forming stars intensively, such as Lyman break or BzK…”