抄録
We present the average [C II] 158 μm emission line sizes of UV-bright star-forming galaxies at z ~ 7. Our results are derived from a stacking analysis of [C II] 158 μm emission lines and dust continua observed by the Atacama Large Millimeter/submillimeter Array (ALMA), taking advantage of the large program Reionization Era Bright Emission Line Survey. We find that the average [C II] emission at z ~ 7 has an effective radius re of 2.2 ± 0.2 kpc. It is ≥2× larger than the dust continuum and the rest-frame UV emission, in agreement with recently reported measurements for z ≤ 6 galaxies. Additionally, we compared the average [C II] size with 4 < z < 6 galaxies observed by the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). By analyzing [C II] sizes of 4 < z < 6 galaxies in two redshift bins, we find an average [C II] size of re = 2.2 ± 0.2 kpc and re = 2.5 ± 0.2 kpc for z ~ 5.5 and z ~ 4.5 galaxies, respectively. These measurements show that star-forming galaxies, on average, show no evolution in the size of the [C II] 158 μm emitting regions at redshift between z ~ 7 and z ~ 4. This finding suggests that the star-forming galaxies could be morphologically dominated by gas over a wide redshift range.
| 本文言語 | English |
|---|---|
| 論文番号 | 144 |
| ジャーナル | Astrophysical Journal |
| 巻 | 934 |
| 号 | 2 |
| DOI | |
| 出版ステータス | Published - 2022 8月 1 |
ASJC Scopus subject areas
- 天文学と天体物理学
- 宇宙惑星科学
フィンガープリント
「The ALMA REBELS Survey: Average [CII] 158μm Sizes of Star-forming Galaxies from z~7 to z~4」の研究トピックを掘り下げます。これらがまとまってユニークなフィンガープリントを構成します。引用スタイル
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The ALMA REBELS Survey : Average [CII] 158μm Sizes of Star-forming Galaxies from z~7 to z~4. / Fudamoto, Y.; Smit, R.; Bowler, R. A.A. その他.
In: Astrophysical Journal, Vol. 934, No. 2, 144, 01.08.2022.研究成果: Article › 査読
}
TY - JOUR
T1 - The ALMA REBELS Survey
T2 - Average [CII] 158μm Sizes of Star-forming Galaxies from z~7 to z~4
AU - Fudamoto, Y.
AU - Smit, R.
AU - Bowler, R. A.A.
AU - Oesch, P. A.
AU - Bouwens, R.
AU - Stefanon, M.
AU - Inami, H.
AU - Endsley, R.
AU - Gonzalez, V.
AU - Schouws, S.
AU - Stark, D.
AU - Algera, H. S.B.
AU - Aravena, M.
AU - Barrufet, L.
AU - Da Cunha, E.
AU - Dayal, P.
AU - Ferrara, A.
AU - Graziani, L.
AU - Hodge, J. A.
AU - Hygate, A. P.S.
AU - Inoue, A. K.
AU - Nanayakkara, T.
AU - Pallottini, A.
AU - Pizzati, E.
AU - Schneider, R.
AU - Sommovigo, L.
AU - Sugahara, Y.
AU - Topping, M.
AU - Van Der Werf, P.
AU - Bethermin, M.
AU - Cassata, P.
AU - Dessauges-Zavadsky, M.
AU - Ibar, E.
AU - Faisst, A. L.
AU - Fujimoto, S.
AU - Ginolfi, M.
AU - Hathi, N.
AU - Jones, G. C.
AU - Pozzi, F.
AU - Schaerer, D.
N1 - Funding Information: This paper makes use of the following ALMA data: ADS/JAO. ALMA#2019.1.01634.L, ADS/JAO.ALMA#2018.1.00085.;S, ADS/JAO.ALMA#2017.1.00428.L, and ADS/JAO.ALMA# 2015.1.01111.S. 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. Y.F., Y.S., and A.K.I. acknowledge support from NAOJ ALMA Scientific Research grant No. 2020-16B. P.A.O. and L.B. acknowledge support from the Swiss National Science Foundation through the SNSF Professorship grant 190079 "Galaxy Buildup at Cosmic Dawn". S.S. acknowledges support from the Nederlandse Onderzoekschool voor Astronomie (NOVA). R.S. acknowledges support from STFC Ernest Rutherford Fellowships and grant No. ST/S004831/1. R.B. acknowledges support from an STFC Ernest Rutherford Fellowship grant No. ST/T003596/1. R.E. acknowledges funding from JWST/NIRCam contract to the University of Arizona, NAS5-02015. H.I. and H.S.B.A. acknowledge support from the NAOJ ALMA Scientific Research grant No. 2021-19A. H.I. acknowledges support from the JSPS KAKENHI grant No. JP19K23462. J.H. gratefully acknowledges support of the VIDI research program with project number 639.042.611, which is (partly) financed by the Netherlands Organisation for Scientific Research (NWO). M.A. acknowledges support from FONDECYT grant 1211951, "CONICYT + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG190030" and "CONICYT+ PCI+REDES 190194" and ANID BASAL project FB210003. P.D. acknowledges support from the European Research Council's starting grant ERC StG-717001 ("DELPHI"), from the NWO grant 016.VIDI.189.162 ("ODIN") and the European Commission's and University of Groningen's COFUND Rosalind Franklin program. L.G. and R.S. acknowledge support from the Amaldi Research Center funded by the MIUR program "Dipartimento di Eccellenza" (CUP:B81I18001170001). A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. Partial support from the Carl Friedrich von Siemens-Forschungspreis der Alexander von Humboldt-Stiftung Research Award is kindly acknowledged (A. F.). I.D.L. acknowledges support from ERC starting grant 851622 DustOrigin. J.W. acknowledges support from the ERC Advanced Grant 695671, "QUENCH", and from the Fondation MERAC. G. C.J. acknowledges funding from the "FirstGalaxies" Advanced grant from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (Grant agreement No. 789056). The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. E.I. acknowledge funding by ANID FONDECYT Regular 1221846. Funding Information: This paper makes use of the following ALMA data: ADS/JAO. ALMA#2019.1.01634.L, ADS/JAO.ALMA#2018.1.00085.;S, ADS/JAO.ALMA#2017.1.00428.L, and ADS/JAO.ALMA# 2015.1.01111.S. 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. Y.F., Y.S., and A.K.I. acknowledge support from NAOJ ALMA Scientific Research grant No. 2020-16B. P.A.O. and L.B. acknowledge support from the Swiss National Science Foundation through the SNSF Professorship grant 190079 “Galaxy Buildup at Cosmic Dawn”. S.S. acknowledges support from the Nederlandse Onderzoekschool voor Astronomie (NOVA). R.S. acknowledges support from STFC Ernest Rutherford Fellowships and grant No. ST/S004831/1. R.B. acknowledges support from an STFC Ernest Rutherford Fellowship grant No. ST/T003596/1. R.E. acknowledges funding from JWST/NIRCam contract to the University of Arizona, NAS5-02015. H.I. and H.S.B.A. acknowledge support from the NAOJ ALMA Scientific Research grant No. 2021-19A. H.I. acknowledges support from the JSPS KAKENHI grant No. JP19K23462. J.H. gratefully acknowledges support of the VIDI research program with project number 639.042.611, which is (partly) financed by the Netherlands Organisation for Scientific Research (NWO). M.A. acknowledges support from FONDECYT grant 1211951, “CONICYT + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG190030” and “CON-ICYT+PCI+REDES 190194” and ANID BASAL project FB210003. P.D. acknowledges support from the European Research Council’s starting grant ERC StG-717001 (“DELPHI”), from the NWO grant 016.VIDI.189.162 (“ODIN”) and the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. L.G. and R.S. acknowledge support from the Amaldi Research Center funded by the MIUR program “Dipartimento di Eccellenza” (CUP:B81I18001170001). A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. Partial support from the Carl Friedrich von Siemens-Forschungspreis der Alexander von Humboldt-Stiftung Research Award is kindly acknowledged (A. F.). I.D.L. acknowledges support from ERC starting grant 851622 DustOrigin. J.W. acknowledges support from the ERC Advanced Grant 695671, “QUENCH”, and from the Fondation MERAC. G. C.J. acknowledges funding from the “FirstGalaxies” Advanced grant from the European Research Council (ERC) under the European Unionʼs Horizon 2020 research and innovation program (Grant agreement No. 789056). The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. E.I. acknowledge funding by ANID FONDECYT Regular 1221846. Publisher Copyright: © 2022. The Author(s).
PY - 2022/8/1
Y1 - 2022/8/1
N2 - We present the average [C II] 158 μm emission line sizes of UV-bright star-forming galaxies at z ~ 7. Our results are derived from a stacking analysis of [C II] 158 μm emission lines and dust continua observed by the Atacama Large Millimeter/submillimeter Array (ALMA), taking advantage of the large program Reionization Era Bright Emission Line Survey. We find that the average [C II] emission at z ~ 7 has an effective radius re of 2.2 ± 0.2 kpc. It is ≥2× larger than the dust continuum and the rest-frame UV emission, in agreement with recently reported measurements for z ≤ 6 galaxies. Additionally, we compared the average [C II] size with 4 < z < 6 galaxies observed by the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). By analyzing [C II] sizes of 4 < z < 6 galaxies in two redshift bins, we find an average [C II] size of re = 2.2 ± 0.2 kpc and re = 2.5 ± 0.2 kpc for z ~ 5.5 and z ~ 4.5 galaxies, respectively. These measurements show that star-forming galaxies, on average, show no evolution in the size of the [C II] 158 μm emitting regions at redshift between z ~ 7 and z ~ 4. This finding suggests that the star-forming galaxies could be morphologically dominated by gas over a wide redshift range.
AB - We present the average [C II] 158 μm emission line sizes of UV-bright star-forming galaxies at z ~ 7. Our results are derived from a stacking analysis of [C II] 158 μm emission lines and dust continua observed by the Atacama Large Millimeter/submillimeter Array (ALMA), taking advantage of the large program Reionization Era Bright Emission Line Survey. We find that the average [C II] emission at z ~ 7 has an effective radius re of 2.2 ± 0.2 kpc. It is ≥2× larger than the dust continuum and the rest-frame UV emission, in agreement with recently reported measurements for z ≤ 6 galaxies. Additionally, we compared the average [C II] size with 4 < z < 6 galaxies observed by the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). By analyzing [C II] sizes of 4 < z < 6 galaxies in two redshift bins, we find an average [C II] size of re = 2.2 ± 0.2 kpc and re = 2.5 ± 0.2 kpc for z ~ 5.5 and z ~ 4.5 galaxies, respectively. These measurements show that star-forming galaxies, on average, show no evolution in the size of the [C II] 158 μm emitting regions at redshift between z ~ 7 and z ~ 4. This finding suggests that the star-forming galaxies could be morphologically dominated by gas over a wide redshift range.
UR - http://www.scopus.com/inward/record.url?scp=85136091025&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85136091025&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ac7a47
DO - 10.3847/1538-4357/ac7a47
M3 - Article
AN - SCOPUS:85136091025
SN - 0004-637X
VL - 934
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 144
ER -