ALMA twenty-six arcmin2 survey of GOODS-S at one millimeter (ASAGAO): Millimeter properties of stellar mass selected galaxies-Reference-Cited by-同舟云学术

ALMA twenty-six arcmin2 survey of GOODS-S at one millimeter (ASAGAO): Millimeter properties of stellar mass selected galaxies

Published:2020-06-30 Issue:4 Volume:72 Page:
ISSN:0004-6264
Container-title:Publications of the Astronomical Society of Japan
language:en
Short-container-title:

Author:

Yamaguchi Yuki¹,Kohno Kotaro¹²^ORCID,Hatsukade Bunyo¹^ORCID,Wang Tao¹³,Yoshimura Yuki¹,Ao Yiping⁴⁵,Dunlop James S⁶,Egami Eiichi⁷,Espada Daniel³⁸⁹,Fujimoto Seiji³¹⁰¹¹¹²¹³,Hayatsu Natsuki H³¹⁴¹⁵,Ivison Rob J¹⁵^ORCID,Kodama Tadayuki¹⁶,Kusakabe Haruka¹⁷¹⁸^ORCID,Nagao Tohru¹⁹,Ouchi Masami³¹⁰²⁰,Rujopakarn Wiphu¹⁰²¹²²,Tadaki Ken-ichi³^ORCID,Tamura Yoichi²³^ORCID,Ueda Yoshihiro²⁴,Umehata Hideki²⁵¹,Wang Wei-Hao²⁶

Affiliation:

1. Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan

2. Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan

3. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

4. Purple Mountain Observatory and Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, 8 Yuanhua Road, Nanjing 210034, China

5. School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui, China

6. Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK

7. Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA

8. Department of Astronomical Science, SOKENDAI (The Graduate University of Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

9. SKA Organization, Lower Withington, Macclesfield, Cheshire SK11 9DL, UK

10. Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan

11. Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan

12. Cosmic DAWN Center, Vibenshuset, Lyngbyvej 2, DK-2100 Copenhagen, Denmark

13. Niels Bohr Institute, University of Copenhagen, Lyngbyvej 2, DK-2100, Copenhagen, Denmark

14. Department of Physics, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan

15. European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany

16. Astronomical Institute, Tohoku University, 6-3 Aramaki, Aoba, Sendai, Miyagi 980-8578, Japan

17. Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan

18. Observatoire de Genéve, Université de Genéve, 51 chemin de Pégase, 1290 Versoix, Switzerland

19. Research Center for Space and Cosmic Evolution, Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan

20. Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), WPI, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan

21. Department of Physics, Faculty of Science, Chulalongkorn University, 254 Phayathai Road, Pathumwan, Bangkok 10330, Thailand

22. National Astronomical Research Institute of Thailand (Public Organization), Don Kaeo, Mae Rim, Chiang Mai 50180, Thailand

23. Division of Particle and Astrophysical Science, Nagoya University, Furocho, Chikusa, Nagoya, Aichi 464-8602, Japan

24. Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan

25. RIKEN Cluster for Pioneering Research, 2-1 Hirosawa, Wako-shi, Saitama 351-0198, Japan

26. Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), No. 1, Sec. 4, Roosevelt Rd., Taipei 10617, Taiwan

Abstract

Abstract We make use of the ALMA twenty-Six Arcmin2 survey of GOODS-S At One-millimeter (ASAGAO), deep 1.2 mm continuum observations of a 26-arcmin2 region in the Great Observatories Origins Deep Survey-South (GOODS-S) obtained with Atacama Large Millimeter/sub-millimeter Array (ALMA), to probe dust-enshrouded star formation in K-band selected (i.e., stellar mass selected) galaxies, which are drawn from the FourStar Galaxy Evolution Survey (ZFOURGE) catalog. Based on the ASAGAO combined map, which was created by combining ASAGAO and ALMA archival data in the GOODS-South field, we find that 24 ZFOURGE sources have 1.2 mm counterparts with a signal-to-noise ratio >4.5 (1σ ≃ 30–70 μJy beam−1 at 1.2 mm). Their median redshift is estimated to be $z$median = 2.38 ± 0.14. They generally follow the tight relationship of the stellar mass versus star formation rate (i.e., the main sequence of star-forming galaxies). ALMA-detected ZFOURGE sources exhibit systematically larger infrared (IR) excess (IRX ≡ LIR/LUV) compared to ZFOURGE galaxies without ALMA detections even though they have similar redshifts, stellar masses, and star formation rates. This implies the consensus stellar-mass versus IRX relation, which is known to be tight among rest-frame-ultraviolet-selected galaxies, cannot fully predict the ALMA detectability of stellar-mass-selected galaxies. We find that ALMA-detected ZFOURGE sources are the main contributors to the cosmic IR star formation rate density at $z$ = 2–3.

Funder

Alberta Livestock and Meat Agency

National Sleep Foundation

National Institutes of Natural Sciences

ASIAA

National Astronomical Observatory of Japan

Astronomy Data Center

Japanese Society for the Promotion of Science

National Natural Science Foundation of China

Publisher

Oxford University Press (OUP)

Subject