Molecular gas content and high excitation of a massive main-sequence galaxy at z = 3
| Autor: | Lei, Han, Valentino, Francesco, Magdis, Georgios E., Kokorev, Vasily, Liu, Daizhong, Rigopoulou, Dimitra, Jin, Shuowen, Daddi, Emanuele |
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| Jazyk: | angličtina |
| Rok vydání: | 2023 |
| Předmět: | |
| Zdroj: | Lei, H, Valentino, F, Magdis, G E, Kokorev, V, Liu, D, Rigopoulou, D, Jin, S & Daddi, E 2023, ' Molecular gas content and high excitation of a massive main-sequence galaxy at z = 3 ', Astronomy & Astrophysics, vol. 673, L13 . https://doi.org/10.1051/0004-6361/202345925 Lei, H, Valentino, F, Magdis, G E, Kokorev, V, Liu, D, Rigopoulou, D, Jin, S & Daddi, E 2023, ' Molecular gas content and high excitation of a massive main-sequence galaxy at z = 3 ', Astronomy and Astrophysics, vol. 673, L13 . https://doi.org/10.1051/0004-6361/202345925 |
| DOI: | 10.1051/0004-6361/202345925 |
| Popis: | We present new CO ($J=5-4$ and $7-6$) and [CI] ($^3P_2\,-\, ^3P_1$ and $^3P_1\,-\, ^3P_0$) emission line observations of the star-forming galaxy D49 at the massive end of the Main Sequence at $z=3$. We incorporate previous CO ($J=3-2$) and optical-to-millimetre continuum observations to fit its spectral energy distribution (SED). Our results hint at high-$J$ CO luminosities exceeding the expected location on the empirical correlations with the infrared luminosity. [CI] emission fully consistent with the literature trends is found. We do not retrieve any signatures of a bright active galactic nucleus that could boost the $J=5-4,\,7-6$ lines in either the infrared or X-ray bands, but warm photon-dominated regions, shocks or turbulence could in principle do so. We suggest that mechanical heating could be a favourable mechanism able to enhance the gas emission at fixed infrared luminosity in D49 and other main-sequence star-forming galaxies at high redshift, but further investigation is necessary to confirm this explanation. We derive molecular gas masses from dust, CO, and [CI] that all agree within the uncertainties. Given its large star formation rate (SFR) $\sim 500~M_\odot~{\rm yr}^{-1}$ and stellar mass $>10^{11.5}~M_\odot$, the short depletion time scale of $ 7 pages, 4 figures, accepted for publication in A&A Letter |
| Databáze: | OpenAIRE |
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