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ALMA deep field in SSA22: Blindly detected CO emitters and [C ii] emitter candidates

Hayatsu, N.H.; Matsuda, Y.; Umehata, H.; Yoshida, N.; Smail, I.; Swinbank, A.M.; Ivison, R.; Kohno, K.; Tamura, Y.; Kubo, M.; Iono, D.; Hatsukade, B.; Nakanishi, K.; Kawabe, R.; Nagao, T.; Inoue, A.K.; Takeuchi, T.T.; Lee, M.; Ao, Y.; Fujimoto, S.; Izumi, T.; Yamaguchi, Y.; Ikarashi, S.; Yamada, T.

ALMA deep field in SSA22: Blindly detected CO emitters and [C ii] emitter candidates Thumbnail


Authors

N.H. Hayatsu

Y. Matsuda

H. Umehata

N. Yoshida

Profile image of Ian Smail

Ian Smail ian.smail@durham.ac.uk
Emeritus Professor

A.M. Swinbank

R. Ivison

K. Kohno

Y. Tamura

M. Kubo

D. Iono

B. Hatsukade

K. Nakanishi

R. Kawabe

T. Nagao

A.K. Inoue

T.T. Takeuchi

M. Lee

Y. Ao

S. Fujimoto

T. Izumi

Y. Yamaguchi

S. Ikarashi

T. Yamada



Abstract

We report the identification of four millimeter line-emitting galaxies with the Atacama Large Milli/submillimeter Array (ALMA) in SSA22 Field (ADF22). We analyze the ALMA 1.1-mm survey data, with an effective survey area of 5 arcmin2, frequency ranges of 253.1–256.8 and 269.1–272.8 GHz, angular resolution of 0 ′′. .′′ 7 and rms noise of 0.8 mJy beam−1 at 36 km s−1 velocity resolution. We detect four line-emitter candidates with significance levels above 6σ. We identify one of the four sources as a CO(9–8) emitter at z = 3.1 in a member of the proto-cluster known in this field. Another line emitter with an optical counterpart is likely a CO(4–3) emitter at z = 0.7. The other two sources without any millimeter continuum or optical/near-infrared counterpart are likely to be [C II] emitter candidates at z = 6.0 and 6.5. The equivalent widths of the [C II] candidates are consistent with those of confirmed high-redshift [C II] emitters and candidates, and are a factor of 10 times larger than that of the CO(9–8) emitter detected in this search. The [C II] luminosity of the candidates are 4–7 × 108 L⊙. The star formation rates (SFRs) of these sources are estimated to be 10–20 M⊙ yr−1 if we adopt an empirical [C II] luminosity–SFR relation. One of them has a relatively low S/N ratio, but shows features characteristic of emission lines. Assuming that at least one of the two candidates is a [C II] emitter, we derive a lower limit of [C II]-based star formation rate density (SFRD) at z ∼ 6. The resulting value of >10−2 M⊙ yr−1 Mpc−3 is consistent with the dust-uncorrected UV-based SFRD. Future millimeter/submillimeter surveys can be used to detect a number of high-redshift line emitters, with which to study the star formation history in the early universe.

Citation

Hayatsu, N., Matsuda, Y., Umehata, H., Yoshida, N., Smail, I., Swinbank, A., …Yamada, T. (2017). ALMA deep field in SSA22: Blindly detected CO emitters and [C ii] emitter candidates. Publications of Astronomical Society of Japan, 69(3), https://doi.org/10.1093/pasj/psx018

Journal Article Type Article
Acceptance Date Feb 24, 2017
Online Publication Date May 4, 2017
Publication Date May 4, 2017
Deposit Date Aug 21, 2017
Publicly Available Date May 4, 2018
Journal Publications of Astronomical Society of Japan
Print ISSN 0004-6264
Electronic ISSN 2053-051X
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 69
Issue 3
DOI https://doi.org/10.1093/pasj/psx018
Public URL https://durham-repository.worktribe.com/output/1349238
Related Public URLs http://ukads.nottingham.ac.uk/abs/2017PASJ...69...45H

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Copyright Statement
This is a pre-copyedited, author-produced version of an article accepted for publication in Publications of the Astronomical Society of Japan following peer review. The version of record Hayatsu, N.H., Matsuda, Y., Umehata, H., Yoshida, N., Smail, I., Swinbank, A.M., Ivison, R., Kohno, K., Tamura, Y., Kubo, M., Iono, D., Hatsukade, B., Nakanishi, K., Kawabe, R., Nagao, T., Inoue, A.K., Takeuchi, T.T., Lee, M., Ao, Y., Fujimoto, S., Izumi, T., Yamaguchi, Y., Ikarashi, S. & Yamada, T. (2017). ALMA deep field in SSA22: Blindly detected CO emitters and [C ii] emitter candidates. Publications of the Astronomical Society of Japan 69(3): 45 is available online at: https://doi.org/https://doi.org/10.1093/pasj/psx018






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