Star Formation in the Nearby Universe: The Ultraviolet and Infrared Points of View

By J. Iglesias-Páramo, V. Buat, T. Takeuchi, K. Xu, S. Boissier, A. Boselli, D. Burgarella, B. Madore, A. G. D. Paz, L. Bianchi and 21 more. 2006

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This work presents the main ultraviolet (UV) and far-infrared (FIR) properties of two samples of nearby galaxies selected from the GALEX (λ = 2315 Å, hereafter NUV) and IRAS (λ = 60 μm) surveys, respectively. They are built in order to obtain detection at both wavelengths for most of the galaxies. Star formation rate (SFR) estimators based on the UV and FIR emissions are compared. Systematic differences are found between the SFR estimators for individual galaxies based on the NUV fluxes corrected for dust attenuation and on the total IR luminosity. A combined estimator based on NUV and IR luminosities seems to be the best proxy over the whole range of values of SFR. Although both samples present similar average values of the birthrate parameter b, their star-formation-related properties are substantially different: NUV-selected galaxies tend to show larger values of b for lower masses, SFRs, and dust attenuation, supporting previous scenarios of star formation history (SFH). Conversely, about 20% of the FIR-selected galaxies show high values of b, SFR, and NUV attenuation. These galaxies, most of them being LIRGs and ULIRGs, break down the downsizing picture of SFH; however, their relative contribution per unit volume is small in the local universe. Finally, the cosmic SFR density of the local universe is estimated in a consistent way from the NUV and IR luminosities.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering

View Paper: https://www.semanticscholar.org/paper/e34c20a425d323c12be3281819516198212e6068

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Citations in the corpus

An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies (2006, background): “However, combining both the ultraviolet and infrared luminosities in Equation 6 is akin to an extinction-corrected ultraviolet luminosity and thus more effectively recovers the true star formation rate (see also Bell 2003 and Iglesias-Páramo et al. 2006).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS (2011, methodology): “Even today, NUV is sometimes used to probe the star formation activity (e.g., Iglesias-Páramo et al. 2006); Recipes for using the IR/NUV ratio to estimate the attenuation in the NUV have been presented recently (e.g., Buat et al. 2005; Burgarella et al. 2005; Cortese et al. 2008).”
The role of cold gas and environment on the stellar mass-metallicity relation of nearby galaxies (2012, methodology): “Using the corrected NUV measurements, star formation rates (SFR) are estimated from the conversion relations of Iglesias-Páramo et al. (2006), who find that the relation log SFRNUV,cor (M yr−1) = log LNUV,cor (L ) − 9.33 (3) provides the rate to an accuracy <20% under the assumption of a Salpeter…”
Star Formation in NGC 5194 (M51a). II. The Spatially Resolved Star Formation Law (2007, methodology): “…of this approach was introduced by Gordon et al. (2000) as the “flux ratio method,” in which they used the combination of ultraviolet and infrared fluxes of galaxies to derive extinction-corrected UV luminosities and SFRs (also see Bell 2003, Hirashita et al. 2003, and Iglesias-Paramo et al. 2006).”
Star formation and mass assembly in high-redshift galaxies (2009, methodology): “A widely used SFR indicator is therefore based on a combination of IR and UV luminosity, which supplies complementary knowledge of the star formation process (Iglesias-Páramo et al. 2006; Calzettiet al. 2007).”
On the Normalization of the Cosmic Star Formation History (2006, methodology): “This technique, suggested as the preferred method by Iglesias-Paramo et al. (2006), has the strong advantage that it avoids assumptions about the extent or form of the obscuration, and variations due to possible luminosity bias in the UV selected sample (e.g., Hopkinset al. 2001; Sullivan et al.…”
The Relationship between Molecular Gas Tracers and Kennicutt-Schmidt Laws (2007, background): “…as LFIR, simply provides a calorimetric measurement of the total energy output by young stars, and is therefore an excellent tracer of recent star formation (Sanders & Mirabel 1996; Rowan-Robinson et al. 1997; Kennicutt 1998a,b; Hirashita et al. 2003; Bell 2003; Iglesias-Páramo et al. 2006).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, methodology): “…widely using the combination of UV and IR observations to estimate dust-corrected SFRs (e.g., Gordon et al. 2000; Bell 2003; Hirashita et al. 2003; Iglesias-Páramo et al. 2006; Cortese et al. 2008), and has been explored for Hαand IR-based SFR measurements by Inoue (2001), Inoue et al. (2001),…”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, methodology): “The accuracy of this extinction correction has been discussed using individual galaxies (Iglesias-Páramo et al. 2006) and by comparisons with independent Hα-derived SFR (Bell 2003); see also Hopkins (2004) and Hopkins & Beacom (2006).”
X-ray emission from star-forming galaxies – I. High-mass X-ray binaries (2011, methodology): “(10) and (11) by Iglesias-Páramo et al. (2006) are consistent with those of Kennicutt (1998) within 3% and 10% respectively.”
Slow Star Formation in Dense Gas: Evidence and Implications (2006, background): “Based on comparisons of multiple tracers of the star formation rate in a range of galaxy types, Iglesias-Páramo et al. (2006) find that equation (2) probably underestimates the star formation rate in normal spirals.”
A Search for Extended Ultraviolet Disk (XUV-Disk) Galaxies in the Local Universe (2007, methodology): “FUV and NUV calibrations are slightly different because we allow for the spectral shape predicted by Starburst99 for a young population continuously forming stars (e.g. Iglesias-Paramo et al. 2006).”
CALIBRATING EXTINCTION-FREE STAR FORMATION RATE DIAGNOSTICS WITH 33 GHz FREE–FREE EMISSION IN NGC 6946 (2011, background): “(9) This diagnostic is often used to characterize SFRs from galaxies in both low- (e.g., Iglesias-Páramo et al. 2006; Buat et al. 2007, 2011) and high-z (e.g., Iglesias-Páramo et al. 2004; Elbaz et al. 2007; Daddi et al. 2007; Reddy et al. 2010) studies.”
DETERMINING STAR FORMATION RATES FOR INFRARED GALAXIES (2008, background): “Galaxies selected in the ultraviolet will tend to favor those with lower absorption of the stellar output, although this appears to be only a moderate effect (Figure 3 of Iglesias-Páramo et al. 2006 or Figure 7 of Buat et al. 2007).”