TY - JOUR
T1 - ALMA lensing cluster survey
T2 - Bright [CII] 158μm lines from a multiply imaged sub-L★ galaxy at z=6.0719
AU - Fujimoto, Seiji
AU - Oguri, Masamune
AU - Brammer, Gabriel
AU - Yoshimura, Yuki
AU - Laporte, Nicolas
AU - González-López, Jorge
AU - Caminha, Gabriel B.
AU - Kohno, Kotaro
AU - Zitrin, Adi
AU - Richard, Johan
AU - Ouchi, Masami
AU - Bauer, Franz E.
AU - Smail, Ian
AU - Hatsukade, Bunyo
AU - Ono, Yoshiaki
AU - Kokorev, Vasily
AU - Umehata, Hideki
AU - Schaerer, Daniel
AU - Knudsen, Kirsten
AU - Sun, Fengwu
AU - Magdis, Georgios
AU - Valentino, Francesco
AU - Ao, Yiping
AU - Toft, Sune
AU - Dessauges-Zavadsky, Miroslava
AU - Shimasaku, Kazuhiro
AU - Caputi, Karina
AU - Kusakabe, Haruka
AU - Morokuma-Matsui, Kana
AU - Shotaro, Kikuchihara
AU - Egami, Eiichi
AU - Lee, Minju M.
AU - Rawle, Timothy
AU - Espada, Daniel
N1 - Funding Information: This paper makes use of the ALMA data: ADS/JAO. ALMA #2018.1.00035.L. ALMA is a partnership of the 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 the ESO, AUI/NRAO, and NAOJ. This work is based on observations and archival data acquired using 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. This work was supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI grant No. JP18K03693. S.F. acknowledges support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179) and Independent Research Fund Denmark grant DFF–7014-00017. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. N.L. acknowledges the Kavli Foundation. G.B.C. and K.I.C. acknowledge funding from the European Research Council via the Consolidator grant ID 681627-BUILDUP. F.E.B acknowledges support from ANID grants CATA-Basal AFB-170002, FONDECYT Regular 1190818, and 1200495, and the Millennium Science Initiative ICN12_009. I.R.S. acknowledges support from STFC (ST/T000244/1). K.K. acknowledges support from the Swedish Research Council and the Knut and Alice Wallenberg Foundation. Publisher Copyright: © 2021. The American Astronomical Society. All rights reserved.
PY - 2021/4/20
Y1 - 2021/4/20
N2 - We present bright [C II] 158 μm line detections from a strongly magnified and multiply imaged (μ ∼ 20–160) sub–L* (MUV = -19.75-+0.440.55) Lyman-break galaxy (LBG) at z = 6.0719 ± 0.0004, drawn from the ALMA Lensing Cluster Survey (ALCS). Emission lines are identified at 268.7 GHz at 8σ exactly at the positions of two multiple images of the LBG, behind the massive galaxy cluster RXCJ0600−2007. Our lens models, updated with the latest spectroscopy from VLT/MUSE, indicate that a sub region of the LBG crosses the caustic, and is lensed into a long (∼6″) arc with a local magnification of μ ∼ 160, for which the [C II] line is also significantly detected. The source plane reconstruction resolves the interstellar medium (ISM) structure, showing that the [C II] line is co-spatial with the rest-frame UV continuum at a scale of ∼300 pc. The [C II] line properties suggest that the LBG is a rotation-dominated system, whose velocity gradient explains a slight difference in redshifts between the whole LBG and its sub-region. The star formation rate (SFR)–L[CII] relations, for whole and sub-regions of the LBG, are consistent with those of local galaxies. We evaluate the lower limit of the faint-end of the [C II] luminosity function at z = 6, finding it to be consistent with predictions from semi-analytical models and from the local SFR–L[CII] relation with a SFR function at z = 6. These results imply that the local SFR–L[CII] relation is universal for a wide range of scales, including the spatially resolved ISM, the whole region of the galaxy, and the cosmic scale, even in the epoch of reionization.
AB - We present bright [C II] 158 μm line detections from a strongly magnified and multiply imaged (μ ∼ 20–160) sub–L* (MUV = -19.75-+0.440.55) Lyman-break galaxy (LBG) at z = 6.0719 ± 0.0004, drawn from the ALMA Lensing Cluster Survey (ALCS). Emission lines are identified at 268.7 GHz at 8σ exactly at the positions of two multiple images of the LBG, behind the massive galaxy cluster RXCJ0600−2007. Our lens models, updated with the latest spectroscopy from VLT/MUSE, indicate that a sub region of the LBG crosses the caustic, and is lensed into a long (∼6″) arc with a local magnification of μ ∼ 160, for which the [C II] line is also significantly detected. The source plane reconstruction resolves the interstellar medium (ISM) structure, showing that the [C II] line is co-spatial with the rest-frame UV continuum at a scale of ∼300 pc. The [C II] line properties suggest that the LBG is a rotation-dominated system, whose velocity gradient explains a slight difference in redshifts between the whole LBG and its sub-region. The star formation rate (SFR)–L[CII] relations, for whole and sub-regions of the LBG, are consistent with those of local galaxies. We evaluate the lower limit of the faint-end of the [C II] luminosity function at z = 6, finding it to be consistent with predictions from semi-analytical models and from the local SFR–L[CII] relation with a SFR function at z = 6. These results imply that the local SFR–L[CII] relation is universal for a wide range of scales, including the spatially resolved ISM, the whole region of the galaxy, and the cosmic scale, even in the epoch of reionization.
UR - http://www.scopus.com/inward/record.url?scp=85105593216&partnerID=8YFLogxK
U2 - https://doi.org/10.3847/1538-4357/abd7ec
DO - https://doi.org/10.3847/1538-4357/abd7ec
M3 - Article
SN - 0004-637X
VL - 911
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 99
ER -