The infrared emission of ultraviolet-selected galaxies from<i>z</i>= 0 to<i>z</i>= 1

Buat, V.; Takeuchi, Tsutomu T.; Burgarella, D.; Giovannoli, É.; Murata, K. L.

doi:10.1051/0004-6361/200912024

Cited by 47 publications

(80 citation statements)

References 55 publications

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“…7, A FUV is plotted versus L FUV and M star . There is a decrease of the upper envelope of the dust attenuation for large L FUV in agreement with other findings based on UV selected samples at similar redshifts (Burgarella et al 2007;Buat et al 2009;Burgarella et al 2011;Heinis et al 2012). For a given UV luminosity, dust attenuation increases with stellar mass.…”

Section: The Amount Of Dust Attenuationsupporting

confidence: 92%

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

Buat

Noll

Burgarella

et al. 2012

A&A

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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 (SEDs) 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 Å 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.

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Section: The Amount Of Dust Attenuationsupporting

confidence: 92%

“…Martin et al (2007) and Buat et al (2009) studied UV selected samples up to z ∼ 1. They reported variations of A FUV as a function of the stellar mass or K-band rest-frame luminosity.…”

Section: The Amount Of Dust Attenuationmentioning

confidence: 99%

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

Buat

Noll

Burgarella

et al. 2012

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“…The discrepancy could either be explained by a larger PAH emission in distant ULIRGs or instead by the hot dust heated by a buried AGN. We note however, that part of this discrepancy could be due to uncertain local SEDs templates (Takeuchi et al 2005;Buat et al 2009). In Fig.…”

Section: Resultsmentioning

confidence: 74%

“…ISO and Spitzer studies have suggested that luminous IR galaxies (LIRGs, 10 12 > L IR /L ≥ 10 11 ) dominate global SF at z ∼ 1 (Chary & Elbaz 2001 -hereafter CE01;Le Floc'h et al 2005;Magnelli et al 2009), while submm and Spitzer data demonstrate that ultra-luminous IR galaxies (ULIRGs, L IR ≥ 10 12 L ) are equally important at z ∼ 2 (Papovich et al 2007;Caputi et al 2007;Daddi et al 2007;A&A 518, L29 (2010) Magnelli et al 2009Magnelli et al , 2010. Until the launch of the Herschel Space Observatory (Pilbratt et al 2010), these analyses relied strongly on substantial extrapolation from the mid-IR or submm or on even more uncertain corrections of the UV luminosity (Buat et al 2009;Daddi et al 2007). Our aim is to determine how accurate these extrapolations are and search for evidence of a major change in the IR properties of galaxies with increasing redshift, using the combined power of the PACS (Poglitsch et al 2010) and SPIRE (Griffin et al 2010) instruments.…”

Section: Introductionmentioning

confidence: 99%

Herschelunveils a puzzling uniformity of distant dusty galaxies

Elbaz¹,

Hwang²,

Magnelli

et al. 2010

A&A

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The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved over the last 80% of the age of the Universe. We discuss possible consequences for the determination of starformation rates (SFR) and any evidence for a major change in their star-formation properties. We use Herschel deep extragalactic surveys from 100 to 500 μm to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and HerMES key programs). An extension to fainter luminosities is done by stacking images on 24 μm prior positions. We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used, e.g. at 24 μm, to identify "isolated" galaxies whose flux is not boosted by bright neighbors. Below z ∼ 1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15 dex), therefore similar to z ∼ 0 galaxies, over three decades in luminosity below the regime of ultra-luminous IR galaxies (ULIRGs, L IR ≥ 10 12 L ). This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160 μm, 250 μm or 350 μm bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ∼150 μm (rest-frame) before Herschel on those templates. We also note that the dust temperature of luminous IR galaxies (LIRGs, L IR ≥ 10 11 L ) around z ∼ 1 is mildly colder by 10-15% than their local analogs and up to 20% for ULIRGs at z ∼ 1.6 (using a single modified blackbody-fit to the peak far-IR emission with an emissivity index of β = 1.5). Above z = 1.5, distant galaxies are found to exhibit a substantially larger mid-over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor coeval star formation at very high SFR and in conditions similar to purely star-forming galaxies.

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“…Elbaz et al (2011) show that the IR SEDs of star-forming galaxies are not evolving with redshift and that, instead, there is a much stronger dependence on the location of galaxies with respect to the galaxy MS. In addition, Buat et al (2009), by using Spitzer MIPS data, also show that the dust attenuation expressed in terms of log (L IR /L UV ) as a function of the log (L IR + L UV ), which is proportional to the SFR, seems to be redshift independent ( fig. 2 of Buat et al 2009) in particular between redshift 0 and 1 as considered in this work.…”

Section: Stellar Masses and Sfr From Sed Fittingmentioning

confidence: 91%

The evolution of star formation activity in galaxy groups

Erfanianfar¹,

Popesso²,

Finoguenov³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We study the evolution of the total star formation (SF) activity, total stellar mass and halo occupation distribution in massive halos by using one of the largest X-ray selected sample of galaxy groups with secure spectroscopic identification in the major blank field surveys (ECDFS, CDFN, COSMOS, AEGIS). We provide an accurate measurement of SFR for the bulk of the star-forming galaxies using very deep midinfrared Spitzer MIPS and far-infrared Herschel PACS observations. For undetected IR sources, we provide a well-calibrated SFR from SED fitting. We observe a clear evolution in the level of SF activity in galaxy groups. The total SF activity in the high redshift groups (0.5

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The infrared emission of ultraviolet-selected galaxies fromz= 0 toz= 1

Cited by 47 publications

References 55 publications

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

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

Herschelunveils a puzzling uniformity of distant dusty galaxies

The evolution of star formation activity in galaxy groups

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