Observations of [OI]63-=μm line emission in main-sequence galaxies at z ∼ 1.5
Date Issued
2020
Author(s)
Wagg, J.
•
Aravena, M.
•
Brisbin, D.
•
Valtchanov, I.
•
Carilli, C.
•
Daddi, E.
•
Dannerbauer, H.
•
•
Díaz-Santos, T.
•
Riechers, D.
•
Sargent, M.
•
Walter, F.
Abstract
We present Herschel-PACS spectroscopy of four main-sequence star-forming galaxies at z ∼ 1.5. We detect [OI]63-=μm line emission in BzK-21000 at z = 1.5213, and measure a line luminosity, $L_{\rm [O\, {\small I}]63\, \mu m} = (3.9\pm 0.7)\times 10^9$ -=L⊙. Our PDR modelling of the interstellar medium in BzK-21000 suggests a UV radiation field strength, G ∼ 320G0, and gas density, n ∼ 1800-=cm-3, consistent with previous LVG modelling of the molecular CO line excitation. The other three targets in our sample are individually undetected in these data, and we perform a spectral stacking analysis which yields a detection of their average emission and an [O-=I]63-=μm line luminosity, $L_{\rm [O\, {\small I}]63\, \mu m} = (1.1\pm 0.2)\times 10^9$ -=L⊙. We find that the implied luminosity ratio, $L_{\rm [O\, {\small I}]63\, \mu m}/L_{\rm IR}$ , of the undetected BzK-selected star-forming galaxies broadly agrees with that of low-redshift star-forming galaxies, while BzK-21000 has a similar ratio to that of a dusty star-forming galaxy at z ∼ 6. The high [O-=I]63-=μm line luminosities observed in BzK-21000 and the z ∼ 1-3 dusty and sub-mm luminous star-forming galaxies may be associated with extended reservoirs of low density, cool neutral gas.
Volume
499
Issue
2
Start page
1788
Issn Identifier
0035-8711
Ads BibCode
2020MNRAS.499.1788W
Rights
open.access
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