The ultraviolet to far-infrared spectral energy distribution of star-forming galaxies in the redshift desert

Oteo, I.; Bongiovanni, Á.; Magdis, G.; Pérez-García, A. M.; Cepa, J.; Sánchez, H. Domínguez; Ederoclite, A.; Sánchez‐Portal, M.; Pintos-Castro, Irene

doi:10.1093/mnras/stt2468

Cited by 23 publications

(44 citation statements)

References 144 publications

(319 reference statements)

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“…The red circles are for the spectroscopic β, while the blue circles are for the photometric β. The black small-dashed line is the dust-UV slope relation at 1 < ∼ z < ∼ 2 from Buat et al (2012), the black dot-dashed line is the dust-UV slope relation at z ∼ 2 from Oteo et al (2014), and the black long-dashed line is the dust-UV slope relation at 1 < z < 3 from Talia et al (2015). The background gray points are the values for all galaxies (crosses are β spec and open circles are β phot ).…”

Section: Uv Spectral Slope (β)mentioning

confidence: 99%

“…4 (right panel) is estimated from E s (B − V) using the Calzetti law (A 1600 ∼ 10 × E s (B − V); Calzetti et al 2000). We have added the best-fit relations from three different studies (Talia et al 2015;Oteo et al 2014;Buat et al 2012). The Oteo et al (2014) relation is for galaxies at z ∼ 2, while the Buat et al (2012) relation is for galaxies at 1 < ∼ z < ∼ 2.…”

Section: β Versus E S (B-v)mentioning

confidence: 99%

“…We have added the best-fit relations from three different studies (Talia et al 2015;Oteo et al 2014;Buat et al 2012). The Oteo et al (2014) relation is for galaxies at z ∼ 2, while the Buat et al (2012) relation is for galaxies at 1 < ∼ z < ∼ 2. The Talia et al (2015) relation covers a wider redshift range, 1 < z < 3.…”

Section: β Versus E S (B-v)mentioning

confidence: 99%

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The VIMOS Ultra Deep Survey: Lyαemission and stellar populations of star-forming galaxies at 2 < z < 2.5

Fèvre

Ilbert

Cassata

et al. 2016

A&A

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The aim of this paper is to investigate spectral and photometric properties of 854 faint (i AB < ∼ 25 mag) star-forming galaxies (SFGs) at 2 < z < 2.5 using the VIMOS Ultra-Deep Survey (VUDS) spectroscopic data and deep multi-wavelength photometric data in three extensively studied extragalactic fields (ECDFS, VVDS, COSMOS). These SFGs were targeted for spectroscopy as a result of their photometric redshifts. The VUDS spectra are used to measure the UV spectral slopes (β) as well as Lyα equivalent widths (EW). On average, the spectroscopically measured β (-1.36 ± 0.02), is comparable to the photometrically measured β (-1.32 ± 0.02), and has smaller measurement uncertainties. The positive correlation of β with the spectral energy distribution (SED)-based measurement of dust extinction E s (B − V) emphasizes the importance of β as an alternative dust indicator at high redshifts. To make a proper comparison, we divide these SFGs into three subgroups based on their rest-frame Lyα EW: SFGs with no Lyα emission (SFG N ; EW ≤ 0 Å), SFGs with Lyα emission (SFG L ; EW > 0 Å), and Lyα emitters (LAEs; EW ≥ 20 Å). The fraction of LAEs at these redshifts is ∼10%, which is consistent with previous observations. We compared best-fit SED-estimated stellar parameters of the SFG N , SFG L and LAE samples. For the luminosities probed here (∼L * ), we find that galaxies with and without Lyα in emission have small but significant differences in their SED-based properties. We find that LAEs have less dust, and lower star-formation rates (SFR) compared to non-LAEs. We also find that LAEs are less massive compared to non-LAEs, though the difference is smaller and less significant compared to the SFR and E s (B − V). When we divide the LAEs according to their Spitzer/IRAC 3.6 μm fluxes, we find that the fraction of IRAC-detected (m 3.6 < ∼ 25 mag) LAEs is much higher than the fraction of IRAC-detected narrow band (NB)-selected LAEs at z 2-3. This could imply that UV-selected LAEs host a more evolved stellar population, which represents a later stage of galaxy evolution, compared to NB-selected LAEs.

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Section: Uv Spectral Slope (β)mentioning

confidence: 99%

Section: β Versus E S (B-v)mentioning

confidence: 99%

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The VIMOS Ultra Deep Survey: Lyαemission and stellar populations of star-forming galaxies at 2 < z < 2.5

Fèvre

Ilbert

Cassata

et al. 2016

A&A

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“…In our case, since we lack observational data in this wavelength interval for the majority of the sample, we estimated β from a linear interpolation of our best-fit MAGPHYS spectral model discussed in Sect. 4.1, as done, for example, in Oteo et al (2014). To test the robustness of this slightly model-dependent estimate of the UV slope, we also computed β from the UV restframe photometry, when available (i.e.…”

Section: Measurements Of the Continuum Extinctionmentioning

confidence: 99%

Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

Puglisi

Rodighiero

Franceschini

et al. 2016

A&A

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We combined the spectroscopic information from the 3D-HST survey with Herschel data to characterize the Hα dust attenuation properties of a sample of 79 main sequence star-forming galaxies at z ∼ 1 in the GOODS-S field. The sample was selected in the far-IR at λ = 100 and/or 160 µm and only includes galaxies with a secure Hα detection (S/N > 3). From the low resolution 3D-HST spectra we measured the redshifts and the Hα fluxes for the whole sample. (A factor of 1/1.2 was applied to the observed fluxes to remove the [NII] contamination.) The stellar masses (M ), infrared (L IR ), and UV luminosities (L UV ) were derived from the spectral energy distributions by fitting multiband data from GALEX near-UV to SPIRE 500 µm. We estimated the continuum extinction E star (B − V) from both the IRX = L IR /L UV ratio and the UV-slope, β, and found excellent agreement between the two. The nebular extinction was estimated from comparison of the observed SFR Hα and SFR UV . We obtained f = E star (B − V)/E neb (B − V) = 0.93 ± 0.06, which is higher than the canonical value of f = 0.44 measured in the local Universe. Our derived dust correction produces good agreement between the Hα and IR+UV SFRs for galaxies with SFR > ∼ 20 M /yr and M > ∼ 5 × 10 10 M , while objects with lower SFR and M seem to require a smaller f -factor (i.e. higher Hα extinction correction). Our results then imply that the nebular extinction for our sample is comparable to extinction in the optical-UV continuum and suggest that the f -factor is a function of both M and SFR, in agreement with previous studies.

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“…In large samples, a rather small fraction is individually detected but biased towards LBGs that are more massive and have redder rest frame UV colors, for both GALEX-selected 0.7 < z < 2.0 LBGs (Burgarella et al 2011, Oteo et al 2013c) and for z ∼ 3 LBGs (Oteo et al 2013b). These Herschel -detected LBGs have large IR luminosities LIR > 10 11 .…”

Section: Lyman Break Galaxiesmentioning

confidence: 99%

Far-Infrared Surveys of Galaxy Evolution

Lutz

2014

Annu. Rev. Astron. Astrophys.

100

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Roughly half of the radiation from evolving galaxies in the early universe reaches us in the far-infrared and submillimeter wavelength range. Recent major advances in observing capabilities, in particular the launch of the Herschel Space Observatory in 2009, have dramatically enhanced our ability to use this information in the context of multiwavelength studies of galaxy evolution. Near its peak, three quarters of the cosmic infrared background is now resolved into individually detected sources. The use of far-infrared diagnostics of dust-obscured star formation and of interstellar medium conditions has expanded from rare extreme high-redshift galaxies to more typical main sequence galaxies and hosts of active galactic nuclei, out to z 2. These studies shed light on the evolving role of steady equilibrium processes and of brief starbursts, at and since the peak of cosmic star formation and black hole accretion. This review presents a selection of recent far-infrared studies of galaxy evolution, with an emphasis on Herschel results. The road to Herschel surveysThe very first steps to use far-infrared emission as a tool to study galaxy evolution date back to the pioneering IRAS mission, when 60 µm source counts in the ecliptic pole region were found to exceed no-evolution models (Hacking, Condon & Houck 1987). The Infrared Space Observatory (ISO) obtained the first deep surveys at both mid-and far-infrared wavelengths, detecting strong evolution of the luminosity function out to z ∼ 1 and supporting by plausible extrapolation that such dusty galaxies constitute the cosmic infrared background. ISO also pioneered the application of the rich mid-infrared spectra as a tool of studying energy sources and physical conditions in dusty galaxies (see Genzel & Cesarsky 2000, for a review). The Spitzer Space Telescope revolutionized mid-infrared surveys and opened the window to direct mid-infrared spectroscopy of faint high-z galaxies (review by Soifer, Helou & Werner 2008). The Akari mission (Murakami et al. 2007) provided uniquely detailed mid-infrared photometric coverage. Independently and at a similar time, ground-based (sub)millimeter surveys at wavelengths 850 µm -1.2 mm detected luminous 'SCUBA galaxies' (Blain et al.

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The ultraviolet to far-infrared spectral energy distribution of star-forming galaxies in the redshift desert

Cited by 23 publications

References 144 publications

The VIMOS Ultra Deep Survey: Lyαemission and stellar populations of star-forming galaxies at 2 < z < 2.5

The VIMOS Ultra Deep Survey: Lyαemission and stellar populations of star-forming galaxies at 2 < z < 2.5

Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

Far-Infrared Surveys of Galaxy Evolution

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