Rest-frame FUV-to-FIR view of Lyman break galaxies at $zsim3$: dust attenuation. (arXiv:1907.11463v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Alvarez_Marquez_J/0/1/0/all/0/1">J. Álvarez-Márquez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgarella_D/0/1/0/all/0/1">D. Burgarella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buat_V/0/1/0/all/0/1">V. Buat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilbert_O/0/1/0/all/0/1">O. Ilbert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prez_Gonzalez_P/0/1/0/all/0/1">P.G. Pŕez-González</a>
This work explores from a statistical point of view the rest-frame
far-ultraviolet (FUV) to far-infrared (FIR) emission of a population of Lyman
break galaxies (LBGs) at $zsim3$ that cannot be individually detected from
current FIR observations. We perform a stacking analysis over a sample of
$sim$17000 LBGs at redshift $2.5
This work explores from a statistical point of view the rest-frame
far-ultraviolet (FUV) to far-infrared (FIR) emission of a population of Lyman
break galaxies (LBGs) at $zsim3$ that cannot be individually detected from
current FIR observations. We perform a stacking analysis over a sample of
$sim$17000 LBGs at redshift $2.5<z<3.5$ in the COSMOS field. The sample is
binned as a function of UV luminosity ($L_{mathrm{FUV}}$), UV continuum slope
($beta_{mathrm{UV}}$), and stellar mass (M$_{*}$), and then, stacked at
optical ($BVriz$ bands), near-infrared ($YJHKs$ bands), IRAC (3.6, 4.5, 5.6 and
8.0 $mu$m), MIPS (24$mu$m), PACS (100 and 160~$mu$m), SPIRE (250, 350, and
500~$mu$m), and AzTEC (1.1mm) observations. We obtain thirty rest-frame
FUV-to-FIR spectral energy distribution (SEDs) of LBGs at $zsim3$, and analyse
them with CIGALE SED-fitting analysis code. We are able to derive fully
consistent physical parameters (M$_{*}$, $beta_{mathrm{UV}}$,
$L_{mathrm{FUV}}$, $L_{mathrm{IR}}$, A$_{FUV}$, SFR, and slope of the dust
attenuation law), and build a semi-empirical library of thirty rest-frame
FUV-to-FIR stacked LBG SEDs as a function of $L_{mathrm{FUV}}$,
$beta_{mathrm{UV}}$, and M$_{*}$. We used the so-called IR-excess ($IRX
equiv L_{mathrm{IR}} / L_{mathrm{FUV}}$) to investigate the dust attenuation
as a function of $beta_{mathrm{UV}}$ and M$_{*}$. Additionally, the
SED-fitting analysis results provide a diversity of dust attenuation curve
along the LBG sample, and their slope are well correlated with M$_{*}$. Stepper
dust attenuations curves than Calzetti’s are favoured in low stellar mass LBGs
($log(M_{*} [M_{odot}]) < 10.25$), while grayer ones are favoured in high
stellar mass LBGs ($log(M_{*} [M_{odot}]) > 10.25$).
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