A [C II] 158 mu m emitter associated with an O I absorber at the end of the reionization epoch
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A [C II] 158 mu m emitter associated with an O I absorber at the end of the reionization epoch. / Wu, Yunjing; Cai, Zheng; Neeleman, Marcel; Finlator, Kristian; Zhang, Shiwu; Prochaska, J. Xavier; Wang, Ran; Emonts, Bjorn H. C.; Fan, Xiaohui; Keating, Laura C.; Wang, Feige; Yang, Jinyi; Hennawi, Joseph F.; Wang, Junxian.
In: Nature Astronomy, Vol. 5, 27.09.2021, p. 1110-1117.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - A [C II] 158 mu m emitter associated with an O I absorber at the end of the reionization epoch
AU - Wu, Yunjing
AU - Cai, Zheng
AU - Neeleman, Marcel
AU - Finlator, Kristian
AU - Zhang, Shiwu
AU - Prochaska, J. Xavier
AU - Wang, Ran
AU - Emonts, Bjorn H. C.
AU - Fan, Xiaohui
AU - Keating, Laura C.
AU - Wang, Feige
AU - Yang, Jinyi
AU - Hennawi, Joseph F.
AU - Wang, Junxian
PY - 2021/9/27
Y1 - 2021/9/27
N2 - The physical and chemical properties of the circumgalactic medium at z greater than or similar to 6 have been studied successfully through the absorption in the spectra of background quasi-stellar objects(1-3). One of the most crucial questions is to Investigate the nature and location of the source galaxies that give rise to these early metal absorbers(4-6). Theoretical models suggest that momentum-driven outflows from typical star-forming galaxies can eject metals into the circumgalactic medium and the intergalactic medium at z = 5-6 (refs. (7-9)). Deep, dedicated surveys have searched for Ly alpha emission associated with strong C IV absorbers at z approximate to 6, but only a few Ly alpha-emitter candidates have been detected. Interpreting these detections is moreover ambiguous because Ly alpha is a resonant line(10-12), raising the need for complementary techniques for detecting absorbers' host galaxies. Here we report a [C II] 158 mu m emitter detected using the Atacama Large Millimeter Array that is associated with a strong low-ionization absorber, O I, at z = 5.978. The projected impact parameter between O I and [C II] emitter is 20.0 kpc. The measured [CII] luminosity is 7.0 x 10(7) solar luminosities. Further analysis indicates that strong O I absorbers may reside in the circumgalactic medium of massive halos one to two orders of magnitude more massive than expected values(8,14).
AB - The physical and chemical properties of the circumgalactic medium at z greater than or similar to 6 have been studied successfully through the absorption in the spectra of background quasi-stellar objects(1-3). One of the most crucial questions is to Investigate the nature and location of the source galaxies that give rise to these early metal absorbers(4-6). Theoretical models suggest that momentum-driven outflows from typical star-forming galaxies can eject metals into the circumgalactic medium and the intergalactic medium at z = 5-6 (refs. (7-9)). Deep, dedicated surveys have searched for Ly alpha emission associated with strong C IV absorbers at z approximate to 6, but only a few Ly alpha-emitter candidates have been detected. Interpreting these detections is moreover ambiguous because Ly alpha is a resonant line(10-12), raising the need for complementary techniques for detecting absorbers' host galaxies. Here we report a [C II] 158 mu m emitter detected using the Atacama Large Millimeter Array that is associated with a strong low-ionization absorber, O I, at z = 5.978. The projected impact parameter between O I and [C II] emitter is 20.0 kpc. The measured [CII] luminosity is 7.0 x 10(7) solar luminosities. Further analysis indicates that strong O I absorbers may reside in the circumgalactic medium of massive halos one to two orders of magnitude more massive than expected values(8,14).
KW - SIMILAR-TO 6
KW - STAR-FORMATION
KW - HOST GALAXIES
KW - CIRCUMGALACTIC MEDIUM
KW - INTERGALACTIC MEDIUM
KW - SPECTROSCOPIC SURVEY
KW - ULTRAVIOLET-SPECTRA
KW - LUMINOSITY FUNCTION
KW - DUST CONTENT
KW - EMISSION
U2 - 10.1038/s41550-021-01471-4
DO - 10.1038/s41550-021-01471-4
M3 - Journal article
VL - 5
SP - 1110
EP - 1117
JO - Nature Astronomy
JF - Nature Astronomy
SN - 2397-3366
ER -
ID: 281221831