TY - JOUR
T1 - ALMA Reveals Extended Cool Gas and Hot Ionized Outflows in a Typical Star-forming Galaxy at Z = 7.13
AU - Akins, Hollis B.
AU - Fujimoto, Seiji
AU - Finlator, Kristian
AU - Watson, Darach
AU - Knudsen, Kirsten K.
AU - Richard, Johan
AU - Tom, Tom J.L.
AU - Hashimoto, Takuya
AU - Inoue, Akio K.
AU - Matsuo, Hiroshi
AU - Michałowski, Michał J.
AU - Tamura, Yoichi
N1 - Funding Information:
The authors are grateful to Francesca Rizzo, Andrea Pallottini, Livia Vallini, Mahsa Kohandel, Andrea Ferrara, David Frayer, and Harley Katz for helpful discussions regarding the physical interpretations of the extended [C II] emission around A1689-zD1. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.01406.S, ADS/JAO.ALMA#2017.1.00775.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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was supported by the U.S. NSF under grant OISE-2005578 (DAWN-IRES). This project has recieved funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 847523 “INTERACTIONS.” H.B.A. acknowledges the support and collaboration of the mentors and fellow students involved in the 2021 DAWN-IRES program. S.F. and D.W. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179) and Independent Research Fund Denmark grant DFF7014-00017. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. K.K. acknowledges support from the Knut and Alice Wallenberg Foundation. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan (HJH02007) and KAKENHI (20K22358). A.K.I. is supported by NAOJ ALMA Scientific Research Grant Code 2020-16B. M.J.M. acknowledges the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208. Much of this work was conducted on the ancestral land of the Meskwaki, Sauk, and Ioway Peoples.
Funding Information:
The authors are grateful to Francesca Rizzo, Andrea Pallottini, Livia Vallini, Mahsa Kohandel, Andrea Ferrara, David Frayer, and Harley Katz for helpful discussions regarding the physical interpretations of the extended [C II ] emission around A1689-zD1. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.01406.S, ADS/JAO.ALMA#2017.1.00775.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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was supported by the U.S. NSF under grant OISE-2005578 (DAWN-IRES). This project has recieved funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 847523 “INTERACTIONS.” H.B.A. acknowledges the support and collaboration of the mentors and fellow students involved in the 2021 DAWN-IRES program. S.F. and D.W. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179) and Independent Research Fund Denmark grant DFF7014-00017. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. K.K. acknowledges support from the Knut and Alice Wallenberg Foundation. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan (HJH02007) and KAKENHI (20K22358). A.K.I. is supported by NAOJ ALMA Scientific Research Grant Code 2020-16B. M.J.M. acknowledges the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208. Much of this work was conducted on the ancestral land of the Meskwaki, Sauk, and Ioway Peoples.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/7/1
Y1 - 2022/7/1
N2 - We present spatially resolved morphological properties of [C II] 158 μm, [O III] 88 μm, dust, and rest-frame ultraviolet (UV) continuum emission for A1689-zD1, a strongly lensed, sub-L* galaxy at z = 7.13, by utilizing deep Atacama Large Millimeter/submillimeter Array (ALMA) and Hubble Space Telescope (HST) observations. While the [O III] line and UV continuum are compact, the [C II] line is extended up to a radius of r ∼ 12 kpc. Using multi-band rest-frame far-infrared continuum data ranging from 52 to 400 μm, we find an average dust temperature and emissivity index of T dust = 41 − 14 + 17 K and β = 1.7 − 0.7 + 1.1 , respectively, across the galaxy. We find slight differences in the dust continuum profiles at different wavelengths, which may indicate that the dust temperature decreases with distance. We map the star formation rate (SFR) via IR and UV luminosities and determine a total SFR of 37 ± 1M ⊙yr−1 with an obscured fraction of 87%. While the [O III] line is a good tracer of the SFR, the [C II] line shows deviation from the local L [C II]-SFR relations in the outskirts of the galaxy. Finally, we observe a clear difference in the line profile between [C II] and [O III], with significant residuals (∼5σ) in the [O III] line spectrum after subtracting a single Gaussian model. This suggests a possible origin of the extended [C II] structure from the cooling of hot ionized outflows. The extended [C II] and high-velocity [O III] emission may both contribute in part to the high L [O III]/L [C II] ratios recently reported in z > 6 galaxies.
AB - We present spatially resolved morphological properties of [C II] 158 μm, [O III] 88 μm, dust, and rest-frame ultraviolet (UV) continuum emission for A1689-zD1, a strongly lensed, sub-L* galaxy at z = 7.13, by utilizing deep Atacama Large Millimeter/submillimeter Array (ALMA) and Hubble Space Telescope (HST) observations. While the [O III] line and UV continuum are compact, the [C II] line is extended up to a radius of r ∼ 12 kpc. Using multi-band rest-frame far-infrared continuum data ranging from 52 to 400 μm, we find an average dust temperature and emissivity index of T dust = 41 − 14 + 17 K and β = 1.7 − 0.7 + 1.1 , respectively, across the galaxy. We find slight differences in the dust continuum profiles at different wavelengths, which may indicate that the dust temperature decreases with distance. We map the star formation rate (SFR) via IR and UV luminosities and determine a total SFR of 37 ± 1M ⊙yr−1 with an obscured fraction of 87%. While the [O III] line is a good tracer of the SFR, the [C II] line shows deviation from the local L [C II]-SFR relations in the outskirts of the galaxy. Finally, we observe a clear difference in the line profile between [C II] and [O III], with significant residuals (∼5σ) in the [O III] line spectrum after subtracting a single Gaussian model. This suggests a possible origin of the extended [C II] structure from the cooling of hot ionized outflows. The extended [C II] and high-velocity [O III] emission may both contribute in part to the high L [O III]/L [C II] ratios recently reported in z > 6 galaxies.
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U2 - 10.3847/1538-4357/ac795b
DO - 10.3847/1538-4357/ac795b
M3 - Article
AN - SCOPUS:85139464258
SN - 0004-637X
VL - 934
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 64
ER -