The ALPINE-ALMA [CII] Survey: Multi-Wavelength Ancillary Data and Basic Physical Measurements. (arXiv:1912.01621v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Faisst_A/0/1/0/all/0/1">A. L. Faisst</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:+Lemaux_B/0/1/0/all/0/1">B. C. Lemaux</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:+Fudamoto_Y/0/1/0/all/0/1">Y. Fudamoto</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:+Bethermin_M/0/1/0/all/0/1">M. Bethermin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capak_P/0/1/0/all/0/1">P. L. Capak</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:+Silverman_J/0/1/0/all/0/1">J. D. Silverman</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:+Ginolfi_M/0/1/0/all/0/1">M. Ginolfi</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:+Morselli_L/0/1/0/all/0/1">L. Morselli</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:+Brammer_G/0/1/0/all/0/1">G. Brammer</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:+Hemmati_S/0/1/0/all/0/1">S. Hemmati</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:+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:+Pozzi_F/0/1/0/all/0/1">F. Pozzi</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:+Tasca_L/0/1/0/all/0/1">L. A. M. Tasca</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:+Romano_M/0/1/0/all/0/1">M. Romano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scoville_N/0/1/0/all/0/1">N. Scoville</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 the ancillary data and basic physical measurements for the
galaxies in the ALMA Large Program to Investigate C+ at Early Times (ALPINE)
survey – the first large multi-wavelength survey which aims at characterizing
the gas and dust properties of 118 main-sequence galaxies at redshifts 4.4 < z < 5.9 via the measurement of [CII] emission at 158 micro-meter and the surrounding far-infrared (FIR) continuum in conjunction with a wealth of optical and near-infrared data. We outline in detail the spectroscopic data and selection of the galaxies as well as the ground- and space-based imaging products. In addition, we provide several basic measurements including stellar masses, star formation rates (SFR), rest-frame ultra-violet (UV) luminosities, UV continuum slopes ($beta$), and absorption line redshifts, as well as H-alpha emission derived from Spitzer colors. Overall, we find that the ALPINE sample is representative of the 4 < z < 6 galaxy population and only slightly biased towards bluer colors ($Deltabeta$ ~ 0.2). Using [CII] as tracer of the systemic redshift (confirmed for one galaxy at z=4.5 for which we obtained optical [OII]3727um emission), we confirm red shifted Ly-alpha emission and blue shifted absorption lines similar to findings at lower redshifts. By stacking the rest-frame UV spectra in the [CII] rest-frame we find that the absorption lines in galaxies with high specific SFR are more blue shifted, which could be indicative of stronger winds and outflows.

We present the ancillary data and basic physical measurements for the
galaxies in the ALMA Large Program to Investigate C+ at Early Times (ALPINE)
survey – the first large multi-wavelength survey which aims at characterizing
the gas and dust properties of 118 main-sequence galaxies at redshifts 4.4 < z
< 5.9 via the measurement of [CII] emission at 158 micro-meter and the
surrounding far-infrared (FIR) continuum in conjunction with a wealth of
optical and near-infrared data. We outline in detail the spectroscopic data and
selection of the galaxies as well as the ground- and space-based imaging
products. In addition, we provide several basic measurements including stellar
masses, star formation rates (SFR), rest-frame ultra-violet (UV) luminosities,
UV continuum slopes ($beta$), and absorption line redshifts, as well as
H-alpha emission derived from Spitzer colors. Overall, we find that the ALPINE
sample is representative of the 4 < z < 6 galaxy population and only slightly
biased towards bluer colors ($Deltabeta$ ~ 0.2). Using [CII] as tracer of the
systemic redshift (confirmed for one galaxy at z=4.5 for which we obtained
optical [OII]3727um emission), we confirm red shifted Ly-alpha emission and
blue shifted absorption lines similar to findings at lower redshifts. By
stacking the rest-frame UV spectra in the [CII] rest-frame we find that the
absorption lines in galaxies with high specific SFR are more blue shifted,
which could be indicative of stronger winds and outflows.

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