GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies

By V. Buat, S. Noll, D. Burgarella, E. Giovannoli, Vassilis Charmandaris, M. Pannella, H. Hwang, D. Elbaz, Mark Dickinson, G. Magdis and 2 more. 2012

147 citations recorded by the source corpus.

Context. Dust attenuation in galaxies is poorly known, especially at high redshift. And yet the amount of dust attenuation is a key parameter to deduce accurate star formation rates from ultraviolet (UV) rest-frame measurements. The wavelength dependence of the dust attenuation is also of fundamental importance to interpret the observed spectral energy distributions (SED) and to derive photometric redshifts or physical properties of galaxies. Aims. We want to study dust attenuation at UV wavelengths at high redshift, where the UV is redshifted to the observed visible light wavelength range. In particular, we search for a UV bump and related implications for dust attenuation determinations. Methods. We use photometric data in the Chandra Deep Field South (CDFS), obtained in intermediate and broad band filters by the MUSYC project, to sample the UV rest-frame of 751 galaxies with 0:95 < z < 2:2. When available, infrared (IR) Herschel/PACS ? data from the GOODS-Herschel project, coupled with Spitzer/MIPS measurements, are used to estimate the dust emission and to constrain dust attenuation. The SED of each source is fit using the CIGALE code. The amount of dust attenuation and the characteristics of the dust attenuation curve are obtained as outputs of the SED fitting process, together with other physical parameters linked to the star formation history. Results. The global amount of dust attenuation at UV wavelengths is found to increase with stellar mass and to decrease as UV luminosity increases. A UV bump at 2175 A is securely detected in 20% of the galaxies, and the mean amplitude of the bump for the sample is similar to that observed in the extinction curve of the LMC supershell region. This amplitude is found to be lower in galaxies with very high specific star formation rates, and 90% of the galaxies exhibiting a secure bump are at z < 1:5. The attenuation curve is confirmed to be steeper than that of local starburst galaxies for 20% of the galaxies. The large dispersion found for these two parameters describing the attenuation law is likely to reflect a wide diversity of attenuation laws among galaxies. The relations between dust attenuation, IR-to-UV flux ratio, and the slope of the UV continuum are derived for the mean attenuation curve found for our sample. Deviations from the average trends are found to correlate with the age of the young stellar population and the shape of the attenuation curve. Conclusions.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b3ac61fe94094b34848029d08cdce7224518072c

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In Astronomy and Astrophysics

1. P. V. van Dokkum
2. C. Conroy
3. P. Hopkins
4. R. Dav'e
5. L. Hernquist
6. E. Daddi
7. M. Franx
8. D. M. Alexander

In Instrumentation

1. P. V. van Dokkum
2. C. Conroy
3. M. Franx
4. I. Labbé
5. Mark Dickinson
6. E. Daddi
7. P. Hopkins
8. R. Dav'e

Citations in the corpus

• CIGALE: a python Code Investigating GALaxy Emission (2018, background): “…have been applied to study a wide variety of issues: why quiescent galaxies do not follow the starburst IRX–β relation (Boquien et al. 2012), the attenuation properties of galaxies (Buat et al. 2011, 2012, 2018; Boquien et al. 2013; Lo Faro et al. 2017; Salim et al. 2018, Decleir et al., in prep.)”
• The evolution of the dust and gas content in galaxies (2013, background): “…to its improved sensitivity and angular resolution with respect to previous instruments, it has become possible to investigate dust properties in large samples of galaxies (e.g., Dunne et al. 2011; Buat et al. 2012; Magdis et al. 2012; Magnelli et al. 2014; Symeonidis et al. 2013, and many others).”
• GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, background): “This is consisent with a number of previous studies (e.g., Pannella et al. 2009a; Buat et al. 2012; Heinis et al. 2013).”
• 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, background): “…with serious differences between the Milky Way (Cardelli et al. 1989), Small Magellanic Cloud (SMC; Prevot et al. 1984; Bouchet et al. 1985), and Large Magellanic Cloud (LMC; Fitzpatrick 1986), as well as in high redshift galaxies (Buat et al. 2012; Reddy et al. 2015; Salmon et al. 2016).”
• Constraining the properties of AGN host galaxies with spectral energy distribution modelling (2015, methodology): “For the lowest value of the parameter, the PDF will be truncated, and thus taking its mean value will slightly shift the output value of the parameter toward a larger value, yielding to its overestimation, as explained in Noll et al. (2009) and Buat et al. (2012).”
• Dusty Star Forming Galaxies at High Redshift (2014, background): “Note that recent work on Herschel samples of modest star formers at 0.2 < z < 2 have found tight correlations between dust masses and stellar mass (e.g. Dunne et al., 2011; Buat et al., 2012; Magdis et al., 2012b) or specific star-formation rate, sSFR (Santini et al., 2014).”
• Dust Attenuation Curves in the Local Universe: Demographics and New Laws for Star-forming Galaxies and High-redshift Analogs (2018, methodology): “Evidence for a moderate bump (0.5 < B < 2.5) and a range of steep curves (−0.7 < δ < 0.1) has also been found in the SED analysis of a 1 < z < 2.2 sample by Buat et al. (2012), as shown in their Fig.”
• THE DUST ATTENUATION LAW IN DISTANT GALAXIES: EVIDENCE FOR VARIATION WITH SPECTRAL TYPE (2013, background): “See Conroy (2013) for more discussion on the proposed explanations Our values for Eb and δ are in the same range to those found by Buat et al. (2012), who fit the photometry of individual galaxies in the GOODS-S field.”
• The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, background): “…al. 2014; c.f., Heinis et al. 2013; Álvarez-Márquez et al. 2016), though with some deviations that depend on galaxy age (Reddy et al. 2006b; Siana et al. 2008; Reddy et al. 2010; Buat et al. 2012), bolometric luminosity (e.g., Chapman et al. 2005; Reddy et al. 2006b; Casey et al. ar X iv :1 70 5.”
• Panchromatic spectral energy distributions of Herschel sources (2013, background): “It is worth to note that, since we are fitting the median photometry of several galaxies, possible variations of the eff ctive attenuation law (e.g. Buat et al. 2012; Reddy et al. 2012, 2006; Wild et al. 2011) are diluted.”
• THE MOSDEF SURVEY: MEASUREMENTS OF BALMER DECREMENTS AND THE DUST ATTENUATION CURVE AT REDSHIFTS z ∼ 1.4–2.6 (2015, methodology): “…Fitzpatrick & Massa 1986), is absent from the attenuation curve found for local UV starburst galaxies (Calzetti et al. 2000), but its presence to varying degrees has been noted in higher-redshift galaxies (e.g., Noll et al. 2009; Buat et al. 2011, 2012; Kriek & Conroy 2013; Scoville et al. 2015).”