The ALPINE–ALMA [C II] Survey: Multiwavelength Ancillary Data and Basic Physical Measurements

Creators: Faisst, A. L.; Schaerer, D.; Lemaux, B. C.; Oesch, P. A.; Fudamoto, Y.; Cassata, P.; Béthermin, M.; Capak, P. L.; Le Fèvre, O.; Silverman, J. D.; Yan, L.; Ginolfi, M.; Koekemoer, A. M.; Morselli, L.; Amorín, R.; Bardelli, S.; Boquien, M.; Brammer, G.; Cimatti, A.; Dessauges-Zavadsky, M.; Fujimoto, S.; Gruppioni, C.; Hathi, N. P.; Hemmati, S.; Ibar, E.; Jones, G. C.; Khusanova, Y.; Loiacono, F.; Pozzi, F.; Talia, M.; Tasca, L. A. M.; Riechers, D. A.; Rodighiero, G.; Romano, M.; Scoville, N.; Toft, S.; Vallini, L.; Vergani, D.; Zamorani, G.; Zucca, E.

Abstract

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 multiwavelength survey that aims at characterizing the gas and dust properties of 118 main-sequence galaxies at redshifts 4.4 < z < 5.9 via the measurement of [C II] emission at 158µm (64% at >3.5σ) and the surrounding far-infrared 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 (β), and absorption line redshifts, as well as Hα emission derived from Spitzer colors. We find that the ALPINE sample is representative of the 4 < z < 6 galaxy population selected by photometric methods and only slightly biased toward bluer colors (Δβ ~ 0.2). Using [C II] as tracer of the systemic redshift (confirmed for one galaxy at z = 4.5 out of 118 for which we obtained optical [O III]λ3727Å emission), we confirm redshifted Lyα emission and blueshifted absorption lines similar to findings at lower redshifts. By stacking the rest-frame UV spectra in the [C II] rest frame, we find that the absorption lines in galaxies with high specific SFR are more blueshifted, which could be indicative of stronger winds and outflows.

Additional Information

© 2020. The American Astronomical Society. Received 2019 December 1; revised 2020 February 14; accepted 2020 March 3; published 2020 April 3. We would like to thank numerous people for the exchange of data without which the ALPINE ancillary data paper would not exist. In particular, we would like to thank E. Vanzella for helping us gathering the spectra in the ECDFS field and O. Ilbert for useful discussions that improved the SED-fitting results. We also thank the anonymous referee for the suggestions that improved this paper. This paper is based on data obtained with the ALMA Observatory, under Large Program 2017.1.00428.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This program receives funding from the CNRS national program Cosmology and Galaxies. This work is based on observations and archival data made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA along with archival data from the NASA/ESA Hubble Space Telescope. This research made also use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. In parts based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data center, Laboratoire d'Astrophysique de Marseille, France. This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Furthermore, this work is based on data from the W. M. Keck Observatory and the Canada–France–Hawaii Telescope, as well as collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by the Subaru Telescope and Astronomy Data Center at the National Astronomical Observatory of Japan. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Finally, we would also like to recognize the contributions from all of the members of the COSMOS Team who helped in obtaining and reducing the large amount of multiwavelength data that are now publicly available through IRSA at http://irsa.ipac.caltech.edu/Missions/cosmos.html. A.C., F.P., M.T., C.G., and F.L. acknowledge the support from grant PRIN MIUR 2017. G.C.J. acknowledges ERC Advanced Grant 695671 "QUENCH" and support by the Science and Technology Facilities Council (STFC). E.I. acknowledges partial support from FONDECYT through grant No. 1171710. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. S.T. acknowledges support from the ERC Consolidator Grant funding scheme (project Context, grant No. 648179). L.V. acknowledges funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 746119. D.R. acknowledges support from the National Science Foundation under grant Nos. AST-1614213 and AST-1910107 and from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers.

Attached Files

Published - Faisst_2020_ApJS_247_61.pdf

Accepted Version - 1912.01621.pdf

Files

Faisst_2020_ApJS_247_61.pdf

Files (25.8 MB)

Name	Size	Download all
Faisst_2020_ApJS_247_61.pdf md5:33f4e979546afffe32ab927d144fc705	14.5 MB	Preview Download
1912.01621.pdf md5:5fc53e18f48ceadc3b154c66a3b44007	11.3 MB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes