The ALPINE-ALMA [CII] Survey: Dust Attenuation Properties and Obscured Star-Formation at z~4.4-5.8. (arXiv:2004.10760v1 [astro-ph.GA])

The ALPINE-ALMA [CII] Survey: Dust Attenuation Properties and Obscured Star-Formation at z~4.4-5.8. (arXiv:2004.10760v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Fudamoto_Y/0/1/0/all/0/1">Yoshinobu Fudamoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oesch_P/0/1/0/all/0/1">P. A. Oesch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faisst_A/0/1/0/all/0/1">A. Faisst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bethermin_M/0/1/0/all/0/1">M. Bethermin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ginolfi_M/0/1/0/all/0/1">M. Ginolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khusanova_Y/0/1/0/all/0/1">Y. Khusanova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loiacono_F/0/1/0/all/0/1">F. Loiacono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fevre_O/0/1/0/all/0/1">O. Le Fevre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capak_P/0/1/0/all/0/1">P. Capak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaerer_D/0/1/0/all/0/1">D. Schaerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silverman_J/0/1/0/all/0/1">J. Silverman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassata_P/0/1/0/all/0/1">P. Cassata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_L/0/1/0/all/0/1">L. Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amorin_R/0/1/0/all/0/1">R. Amorin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bardelli_S/0/1/0/all/0/1">S. Bardelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boquien_M/0/1/0/all/0/1">M. Boquien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cimatti_A/0/1/0/all/0/1">A. Cimatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dessauges_Zavadsky_M/0/1/0/all/0/1">M. Dessauges-Zavadsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujimoto_S/0/1/0/all/0/1">S. Fujimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruppioni_C/0/1/0/all/0/1">C. Gruppioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hathi_N/0/1/0/all/0/1">N. P. Hathi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ibar_E/0/1/0/all/0/1">E. Ibar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_G/0/1/0/all/0/1">G.C. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koekemoer_A/0/1/0/all/0/1">A. M. Koekemoer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagache_G/0/1/0/all/0/1">G. Lagache</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemaux_B/0/1/0/all/0/1">B.C. Lemaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maiolino_R/0/1/0/all/0/1">R. Maiolino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayanan_D/0/1/0/all/0/1">D. Narayanan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pozzi_F/0/1/0/all/0/1">F. Pozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">D. A. Riechers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodighiero_G/0/1/0/all/0/1">G. Rodighiero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Talia_M/0/1/0/all/0/1">M. Talia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toft_S/0/1/0/all/0/1">S. Toft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vallini_L/0/1/0/all/0/1">L. Vallini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vergani_D/0/1/0/all/0/1">D. Vergani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamorani_G/0/1/0/all/0/1">G. Zamorani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zucca_E/0/1/0/all/0/1">E. Zucca</a>

We present dust attenuation properties of spectroscopically confirmed star
forming galaxies on the main sequence at redshift ~4.4-5.8. Our analyses are
based on the far infrared continuum observations of 118 galaxies at rest-frame
$158,rm{mu m}$ obtained with the ALMA large program ALPINE. We study the
connection between the UV spectral slope ($beta$), stellar mass ($M_{star}$),
and infrared excess (IRX$=L_{rm{IR}}/L_{rm{UV}}$). Twenty-three galaxies are
individually detected in the continuum at $>3.5,sigma$ significance. We
perform a stacking analysis using both detections and non-detections to study
the average dust attenuation properties at z~4.4-5.8. The individual detections
and stacks show that the IRX-$beta$ relation at z~5 is consistent with a
steeper dust attenuation curve than typically found at lower redshifts (z<4).
The attenuation curve is similar to or even steeper than that of the extinction
curve of the Small Magellanic Cloud (SMC). This systematic change of the
IRX-$beta$ relation as a function of redshift suggests an evolution of dust
attenuation properties at $z>4$. Similarly, we find that our galaxies have
lower IRX values up to 1 dex on average at fixed mass compared to previously
studied IRX-$M_{star}$ relations at $zlesssim4$, albeit with significant
scatter. This implies a lower obscured fraction of star-formation than at lower
redshifts. Our results suggest that dust properties of UV-selected star forming
galaxies at $zgtrsim4$ are characterised by (i) a steeper attenuation curve
than at $zlesssim4$, and (ii) a rapidly decreasing dust obscured fraction of
star formation as a function of redshift. Nevertheless, even among this
UV-selected sample, massive galaxies ($log M_{star}/M_odot > 10$) at z~5-6
already exhibit an obscured fraction of star formation of $sim45%$,
indicating a rapid build-up of dust during the epoch of reionization.

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