Star formation and dust attenuation properties in galaxies from a statistical ultraviolet‐to‐far‐infrared analysis

By D. Burgarella, V. Buat, J. Marseille, France Instituto de Astrofisica de Andalucia, Spain. 2005

333 citations recorded by the source corpus.

We study two galaxies samples selected in near-ultraviolet (NUV) and in far-infrared (FIR) for which the spectral energy distributions (SEDs) from the far-UV (FUV) to the FIR are available. We compared the observed SEDs to modelled SEDs with several star formation histories (SFHs; decaying star formation rate plus burst) and dust attenuation laws (power law + 2175 A bump). The Bayesian method allows one to estimate statistically the best parameters by comparing each observed SED to the full set of 82 800 models. We reach the conclusion that the UV dust attenuation cannot be estimated correctly from SED analysis if the FIR information is not used. The dispersion is larger than with the FIR data. The distribution is also not symmetrically distributed about zero: there is an overestimation for UV-selected galaxies and an underestimation for FIR-selected galaxies. The output from the analysis process suggests that UV-selected galaxies have attenuation laws in average similar to the Large Magellanic Cloud extinction law while FIR-selected galaxies attenuation laws resemble more the Milky Way extinction law. The dispersion about the average relation in the log (F dust /F FUV ) versus FUV-NUV diagram (once the main relation with FUV - NUV accounted for) is explained by two other parameters: the slope of the attenuation law and the instantaneous birthrate parameters b 0 for UV-selected galaxies and the same ones plus the strength of the bump for the FIR-selected galaxies. We propose a recipe to estimate the UV dust attenuation for UV galaxies only (that should only be used whenever the FIR information is not available because the resulting A FUV is poorly defined with an uncertainty of about 0.32): A FUV = 1.4168 (FUV - NUV) 2 + 0.3298 (NUV - I) 2 + 2.1207 (FUV - NUV) + 2.7465 (NUV - I) + 5.8408.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a92e4e76777224efdbf70dfeb2da676987d6a033

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

In Instrumentation

Citations in the corpus

Stellar Population Inference with Prospector (2020, background): “Early Bayesian codes such as Kauffmann et al. 2003; Salim et al. 2007, CIGALE (Burgarella et al. 2005), and MAGPHYS (da Cunha et al. 2008), were successful in this effort.”
Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density (2013, methodology): “The FUV dust attenuation is estimated from the IRX and converted to AFUV using Burgarella et al.(2005)2.”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, background): “MNRAS 462, 1415–1443 (2016) by guest on O ctober 5, 2016 http://m nras.oxfordjournals.org/ D ow nloaded from zBPZ − zspec 0.005 0.028 2.4 per cent zEAZY − zspec −0.013 0.030 5.9 per cent zBEAGLE − zspec 0.007 0.047 7.1 per cent zBEAGLE − zBPZ 0.005 0.042 8.3 per cent zBEAGLE − zEAZY 0.039 0.058 7.3 ”
THE DUST ATTENUATION LAW IN DISTANT GALAXIES: EVIDENCE FOR VARIATION WITH SPECTRAL TYPE (2013, background): “…at Santa Cruz, Santa Cruz, CA 95064 galaxies as well, out to z ∼ 1 or even higher, though not as strong as for the Milky Way (e.g., Motta et al. 2002; Burgarella et al. 2005; Noll et al. 2009; Eĺıasdott́ır et al. 2009; Conroy et al. 2010b; Conroy 2010; Wild et al. 2011; Buat et al. 2011).”
Radial Variation of Attenuation and Star Formation in the Largest Late-Type Disks Observed with GALEX (2006, background): “Actually, Burgarella et al. (2005) showed that the slope of the extinction and the presence or not of a bump has a larger impact on the position in the IRX-β plane than the star formation history (and the b parameter).”
GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies (2012, background): “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…”
Dusty Star Forming Galaxies at High Redshift (2014, methodology): “The Code Investigating GALaxy Emission (Cigale) was developed from an algorithm described in Burgarella et al. (2005) and formally presented in Noll et al. (2009).”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, background): “7 match to the wavelength range used for studies of the dust extinction in galaxies at z ∼ 0 (e.g., Meurer et al. 1995; Meurer et al. 1999; Burgarella et al. 2005).”
CIGALE: a python Code Investigating GALaxy Emission (2018, methodology): “Numerous works have found and tried to explain the extensive variations observed in the IRX-β relation over the years (e.g. Kong et al. 2004; Burgarella et al. 2005; Boquien et al. 2009, 2012; Overzier et al. 2011; Grasha et al. 2013; Ye et al. 2016; Popping et al. 2017; Reddy et al. 2018, and many…”
CEERS Key Paper. I. An Early Look into the First 500 Myr of Galaxy Formation with JWST (2022, methodology): “As a check on our fiducial EAZY photometric redshifts, we also measured photometric redshifts with Cigale (Burgarella et al. 2005).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS (2011, methodology): “In nearby star-forming galaxies, the dust attenuation in the UV can vary from zero to several magnitudes (e.g., Buat et al. 2005; Burgarella et al. 2005).”
Dust Attenuation Curves in the Local Universe: Demographics and New Laws for Star-forming Galaxies and High-redshift Analogs (2018, methodology): “Burgarella et al. (2005), using UV to far-IR SED fitting, also find on average a steep (n = 1.1) and moderately bumpy slope for a sample of ∼ 100 local galaxies.”
A Long Time Ago in a Galaxy Far, Far Away: A Candidate z ∼ 12 Galaxy in Early JWST CEERS Imaging (2022, methodology): “Software: Astropy (Astropy Collaboration et al. 2013), BAGPIPES (Carnall et al. 2018), CIGALE (Burgarella et al. 2005; Noll et al. 2009; Boquien et al. 2019), DENSE BASIS (Iyer & Gawiser 2017; Iyer et al. 2019), Drizzle (Fruchter & Hook 2002), EAZY (Brammer et al. 2008), GALFITM (Peng et al. 2010;…”
Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample (2009, background): “21 early-type spirals also exhibit the largest deviations from the relation between LIR/LFUV andAFUV for nearby star-forming galaxies derived by Burgarella et al. (2005) (cf. Buat et al. 2005; Cortese et al.2008).”
x-cigale: fitting AGN/galaxy SEDs from X-ray to infrared (2020, methodology): “CIGALE is an efficient SED-fitting code which has been developed for more than a decade (Burgarella et al. 2005; Noll et al. 2009; Serra et al. 2011; Boquien et al. 2019).”
An Older, More Quiescent Universe from Panchromatic SED Fitting of the 3D-HST Survey (2018, methodology): “Bayesian forward-modeling techniques pioneered by Kauffmann et al. (2003), Burgarella et al. (2005), and Salim et al. (2007) help to constrain the complex, correlated parameter uncertainties typically present in galaxy models.”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Subsequent analyses extending to normal star-forming galaxies (e.g., Hirashita et al. 2003; Kong et al. 2004; Burgarella et al. 2005; Buat et al. 2005; Treyer et al. 2010; Hao et al. 2011) typically produce values of η which are somewhat lower (e.g., 0.46 for Hao et al. 2011), which almost…”