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Volume 65 Supplement 10

Cosmic Dust V

Dust attenuation in galaxies up to redshift 2


We want to study dust attenuation at ultraviolet (UV) wavelengths at high redshift, where the UV is redshifted to the observed visible light wavelength range. In particular, we search for a bump at 2175 Å. 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 spectral energy distribution of each source is fit using the CIGALE code. The average attenuation curve found for our sample galaxies exhibits a UV bump whose amplitude is similar to that observed in the extinction curve of the LMC super-shell region. The slope of the average attenuation curve at UV wavelength is found steeper than that for local starburst galaxies. The amount of dust attenuation at UV wavelengths is found to increase with stellar mass and to decrease as UV luminosity increases.

1. Introduction

Although dust is a minor component in galaxies, it captures a large fraction of the stellar emission, especially at short wavelengths. This process makes the direct observation of stellar populations from the UV to the near-IR insufficient to recover all the emitted photons. Thus reliable dust corrections are mandatory for measuring the star formation rate (SFR) in the universe and its evolution with redshift from UV-optical surveys. The search for relations between dust attenuation and observed or commonly measured quantities are very useful in this context. It is also particularly important to study the dependence of dust attenuation on wavelength in order to recover the intrinsic spectral distribution of the stellar light, which gives information on the star formation history at work in galaxies.

Models solving radiation transfer rely on numerous free parameters and physical assumptions that are difficult to constrain from the integrated emission from entire galaxies and for very large numbers of objects. Simpler models have been specifically developed to analyze large samples of galaxies, introducing simple recipes and templates. The number of free parameters is considerably reduced. These codes are often developed to measure photometric redshifts and physical parameters such as the SFR and the stellar mass. With the availability of mid and far-IR data for large samples of galaxies, new codes are emerging that combine stellar and dust emission on the basis of the balance between the stellar luminosity absorbed by dust and the corresponding luminosity re-emitted in the IR. Attenuation laws are introduced in these codes. The most popular attenuation curve is that of Calzetti et al. (2000), built for local starburst galaxies. This law, based on spectroscopic data, does not exhibit a bump at 2175 Å such as that observed in the extinction curves of the Milky Way (MW) or the Large Magellanic Cloud supershell (LMC2). Since the Calzetti and collaborators work, numerous studies have tried to search for the presence of a bump in the attenuation curve of nearby, non starbursting, galaxies. Most studies based on very different approaches conclude to a presence of bump in large samples of nearby star forming galaxies (Burgarella et al., 2005; Conroy et al., 2010; Wild et al., 2011). At higher redshifts, the situation is more favorable because of the redshifting of the UV emission into visible. Direct evidence of bumps came from the analysis of the galaxy spectra at 1 < z < 2.5 (Noll et al., 2009). Recently Buat et al. (2011b), (2012) analyzed spectral energy distributions (SEDs) of UV selected galaxies in a redshift range between 0.95 and 2.2, observed through intermediate band filters and with IR detections from Herschel/PACS, and found evidence for a UV bump in the dust attenuation curve of all these galaxies. The present work extends the analysis performed in these two papers. After a brief description of the data (Section 2) and of the fitting tool used for the analysis (Section 3), the average attenuation curve obtained with the dataset is compared to extinction curves of LMC2 and MW and to the models of Inoue et al. (2006) in Section 4. Relations linking dust attenuation to UV luminosity and stellar mass are presented in Section 5.

2. High Redshift Galaxies Selected in the Ultraviolet

The sample selection is described in Buat et al. (2012). We briefly summarize the selection process and the main characteristics of the resulting sample. The field considered is located in the Great Observatories Origins Deep Survey Southern field (GOODS-S). It was observed at 100 and 160 µm over 264 hours by the PACS instrument onboard of the Herschel Space Observatory (Pilbratt et al., 2010) as part of the GOODS-Herschel open time key project (Elbaz et al., 2011). The MUSYC project (Cardamone et al., 2010) compiled a uniform catalogue of optical and IR photometry for sources in this field, incorporating the GOODS Spitzer IRAC and MIPS data as well as intermediate and broad-band optical data. It provides a valuable means of tracing the detailed shape of the UV rest-frame spectrum. We started with the MUSYC catalogue, selecting sources with a spectroscopic redshift between 0.95 and 2.2 and no X ray detection. In this redshift range we have more than ten photometric bands available in the UV rest-frame and a good sampling around 2175 Å. We consider all the optical broad bands (7 bands from U to z) and intermediate-band filters (11 bands) whose 5σ depth was fainter than 25 ABmag. Our sample contains 751 sources, all detected by IRAC at 3.6µm. 290 sources have a 3σ detection at 24 µm, 76 of these sources are also detected by PACS at 100 µm.

3. CIGALE: A SED Fitting Tool Aimed at Studying Dust Attenuation in Galaxies

The CIGALE code (Code Investigating GALaxy Emission, was developed by Noll et al. (2009). This is a physically-motivated code that derives properties of galaxies by fitting their UV-to-IR SEDs. CIGALE combines a UV-optical stellar SED with a dust component emitting in the IR and fully conserves the energy balance between the dust absorbed stellar emission and its re-emission in the IR. We refer to Noll et al. paper for details on the code. For the purpose of the present work we focus on the dust attenuation treatment performed by CIGALE, the various input parameters introduced for this analysis are discussed in Buat et al. (2012). The dust attenuation is described as


Throughout the paper the wavelength λ will be expressed in Å, λV = 5500 Å, k′(λ) 1 Footnote 1 comes from Calzetti et al. (2000) (Eq. (4)) and Dλ0,γEb(λ), the Lorentzian-like Drude profile commonly used to describe the UV bump, is defined as


The factor produces different slopes without modifying the visual attenuation AV. It implies changes in the value of the effective total obscuration RV, originally equal to 4.05 for the Calzetti et al. law.

The reliability of parameter determinations is extensively discussed in Buat et al. (2012) with the analysis of a catalog of artificial galaxies and that of the 76 galaxies detected by PACS. Parameters are better estimated when at least one IR measurement is available, which is the case for 290 of our objects. Without IR data dust attenuation at UV wavelength is found slightly over-estimated for low values of this parameter (of the order of 0.3 mag for an attenuation of 1 mag), the amplitude of the bump Eb is robustly estimated whereas the slope δ is over-estimated for low values (by 0.1 unit for δ = −0.5). We refer to Buat et al. (2012) for more details about the SED fitting analysis.

E b and δ are estimated for each object as the mean value of their probability distribution function (PDF) given by CIGALE. The resulting distributions obtained for these estimated parameters are shown in Fig. 1. The typical uncertainty for each estimation (dispersion of the PDF) is found to be 0.8 for E b and 0.15 for δ. The average values and standard deviations of the distributions of Fig. 1 are Eb = 1.6 ± 0.4 and δ = −0.27 ± 0.17. The large uncertainty in the determination of the parameters implies that only 20% of individual sources (40% of the sources detected in IR) exhibit a secure bump and and an attenuation curve steeper than the Calzetti et al. one. In the next section, we will focus on the analysis of the average attenuation curve and not on the dispersion found for individual source. A detailed discussion of the individual measurements can be found in Buat et al. (2012).

Fig. 1.
figure 1

Distribution of the amplitude of the bump Eb and slope of the attenuation curve δ as defined in Eq. (1) and (2). Both parameters are determined with the CIGALE code which does not only give the best model fitted (based on a χ2 minimization over all the models) but also calculates the probability of each input model and returns the probability distribution function (PDF) of each parameter. The histograms with spikes correspond to the values found for the best models and the continuous lines represent the distributions of the mean values of the PDF of Eb and δ obtained for each object. The values corresponding to the attenuation curve of Calzetti et al. (2000), (C00), of the extinction curves of the Milky Way (MW), LMC2 supershell (LMC2) and of the SMC (SMC) are plotted as dotted lines. The parameters for the MW are taken from Fitzpatrick and Massa (1990), those for the Magellanic Clouds come from Gordon et al. (2003).

4. Average Dust Attenuation Curve

We can tentatively derive an average attenuation curve for our sample.




Models predict a variation of the shape of the attenuation curve and of the amplitude of the bump with the amount of dust attenuation (e.g. Inoue et al., 2006). The mean dust attenuation at 1530 A for the sample is found to be AFUV= 2.2 mag and the average dust attenuation curve given above is expected to be representative of galaxies with this average attenuation.

The resulting curve is plotted in Fig. 2 with other curves already considered in Fig. 1. As underlined in Buat et al. (2012) the average attenuation curve is close to the extinction curve found for the LMC2 super-shell. Inoue et al. (2006) predicted various attenuation curves for the UV range. In Fig. 3 we compare the result of their models obtained with dust characteristics from Draine (2003) and corresponding to AFUV = 2 mag. The extinction curve for the LMC2 super-shell is also over-plotted. Whereas the amplitude of the bump is well reproduced in the Inoue et al. model with LMC dust, the corresponding attenuation curve is steeper than the one derived from the data. The general shape is better reproduced with a MW type dust but this time the predicted amplitude of the bump is too large. The best agreement is found with the LMC2 extinction curve.

Fig. 2.
figure 2

Mean dust attenuation curve (black heavy line), the thin black lines represent the 1 σ variation on E b and δ. The attenuation curve of Calzetti (2000) is plotted as a dotted line (C00), the LMC2 extinction curve with a dashed line and the SMC extinction curve with a dot-dashed line.

Fig. 3.
figure 3

Average dust attenuation curve derived in this work (black solid line) compared to models from Inoue et al. for a LMC2 type dust (filled circles and red line), and a MW type dust (empty circles and green line). The empty squares and blue line are for the LMC2 extinction curve from Gordon et al. (2003).

5. Dust Attenuation Variation

In the absence of IR emission to constrain dust attenuation, empirical relations linking the amount of dust attenuation to some galaxy characteristics are particularly useful. Any systematic trend with the observed UV luminosity is important to account for when intrinsic, attenuation corrected luminosity functions are studied. Another crucial physical parameter is the stellar mass. It is mainly constrained by the optical-NIR part of the SED which is not very sensitive to dust attenuation and can be securely estimated even when dust attenuation is badly known. As a consequence any relation between dust attenuation and stellar mass will be particularly useful at least to apply global corrections to large samples of galaxies. Hereafter we will discuss dust attenuation at FUV, with a FUV wavelength taken at 1530 Å (corresponding to the FUV GALEX filter). The FUV luminosity LFUV is defined as λ × Lλ and expressed in solar units (L).

5.1 Dust attenuation and observed luminosities

Buat et al. (2012) (see also Heinis et al., MNRAS, submitted) reported a decrease of the mean dust attenuation when the observed FUV luminosity increases with a dispersion increasing at low luminosities. The data points and the average values per bin of FUV luminosity calculated by Buat et al. (2012) are reported in Fig. 4. We perform a linear regression between the average values of AFUV expressed in magnitudes and LFUV in solar units:


the uncertainties on the coefficients (slope and constant) correspond to standard deviations, the global R.M.S. error is found equal to 0.04, and the correlation coefficient R is equal to 0.99.

Fig. 4.
figure 4

Dust attenuation versus FUV luminosity. Redshift is color coded. The connected black points and the vertical bars represent the mean and dispersion of AFUV per bin of LFUV. The solid line is the result of the linear regression.

The detected galaxies become more luminous when the redshift increases because of selection effects as clearly seen in Fig. 4. So any study of the variation of dust attenuation with z must account for this decrease of the attenuation when LFUV increases.

5.2 Dust attenuation and stellar masses

Stellar masses (Mstar) are obtained as an output of the fitting code CIGALE as described in Buat et al. (2012). The adopted IMF is that of Kroupa (2001). Mean dust attenuation factors can be calculated per bin of Mstar, the results are reported in Fig. 5. We perform a linear regression on these average values, the correlation coefficient is found very high (R = 0.97) and the linear regression gives:


the uncertainties on the coefficients (slope and constant) correspond to standard deviations, the global R.M.S. error is found equal to 0.16. This relation can be compared to other ones also obtained for UV selected galaxies from z = 0 to z = 2. Up to z = 1 the FUV rest-frame range is well sampled with GALEX data. Buat et al. (2007) performed a statistical analysis of the GALEX and IRAS surveys and deduced volume corrected relations about far-IR and FUV properties of galaxies in the nearby universe. Here, we use their UV selected sample to calculate the average far-IR to FUV flux ratio per bin of stellar mass following the method explained in Buat et al. (2007). The amount of dust attenuation is then calculated by applying the relation of Buat et al. (2011a). The average values and the result of the linear regression fitted on them is reported in Fig. 5. Garn and Best (2010) obtained a relation between dust attenuation and stellar mass for SDSS galaxies based on the measure of the Balmer decrement, their relation is extrapolated at FUV wavelength using the Meurer et al. (2009) relation AFUV = 1.68AHα and is also reported on Fig. 5. Note that this extrapolation is very crude given the large dispersion in the scatter plot between AFUV and AHα and the uncertainty on the average value of AFUV/AHα (Bell and Kennicutt, 2001; Buat et al., 2002; Boselli et al., 2013). Buat et al. (2009) investigated UV selected galaxies from z = 0 to z = 1 and found a trend with MFUV and no clear evolution with redshift of the AFUVMstar scatter plot. We report their average relation corresponding to log(LFUV) = 10.2[L], representative of our current sample (see Buat et al. (2012) for more details). At z = 2 Sawicki (2012) built a FUV selected sample from the Ultra-deep Hubble field and found a relation between dust attenuation and stellar mass (estimated from the observed FUV luminosity), his relation is also reported in Fig. 5. The relation obtained in the present work for galaxies with redshift between 0.95 and 2.2 predicts slightly higher dust attenuation factors than the three other ones but remain consistent within the error bars with most of the relations considered in Fig. 5. The relation found at z = 0 by Buat et al. (2007) leads to lower dust attenuation for massive galaxies by ~1 mag for log(Mstar) > 10.5[M] but their statistics for high mass galaxies was low. The Garn and Best relation based on larger statistics is found closer the other ones at higher z. We can conservatively conclude to a well defined relation between average dust attenuation and Mstar for UV selected galaxies which does not show a significant evolution from z = 0 to z = 2.

Fig. 5.
figure 5

Dust attenuation versus stellar mass. Upper panel: Individual values of Mstar and AFUV from Buat et al. (2012) are reported with the observed FUV luminosity color coded. The mean values and the related dispersion per bin of Mstar from Buat et al. (2012) are plotted with filled squares and vertical bars. The solid line is the result of the linear regression. Lower panel: the linear regression found in the upper panel (filled squares and black lines) is compared with other relations from previous works: at z < 0 from Buat et al. (2007) (lozenges and green dot-dashed regression line) and from Garn and Best (2010) (solid thin green line), for z < 1 from Buat et al. (2009) (red dots and dashed line, average relation for (log(LFUV) = 10.2[L])) and at z = 2 from Sawicki (2012) (blue dotted line and triangles).

The trend found with the FUV luminosity (i.e. a lower mean dust attenuation when LFUV increases) is clearly visible in Fig. 5, upper panel. It might imply a modification of the mean relation as a function of the luminosity, the FUV luminosity also acting as a parameter in the variation of dust attenuation. A complete analysis of this relation per bin of FUV luminosity and stellar mass at different redshifts has still to be performed. The current samples are too small for such a study. Heinis et al. (in preparation) will analyze a much larger sample of galaxies in the COSMOS field based on stacked Herschel/SPIRE images to better constrain average dust attenuation factors.


  1. k′(λ) = 2.659(−2.156+1.509104/λ− 0.198108/λ2 + 0.0111012/λ3) + 4.05 for 1200 < λ < 6300 Åand k′(λ) = 2.659(−1.857 + 1.040104/λ) + 4.05 for 6300 < λ < 22000 Å


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This work is partially supported by the French National Agency for research (ANR-09-BLAN-0224). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).

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Buat, V. Dust attenuation in galaxies up to redshift 2. Earth Planet Sp 65, 1095–1100 (2013).

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