dc.contributor.author | Doherty, M. J. | |
dc.contributor.author | Geach, J. E. | |
dc.contributor.author | Ivison, R. J. | |
dc.contributor.author | Menten, K. M. | |
dc.contributor.author | Jacob, A. M. | |
dc.contributor.author | Forbrich, J. | |
dc.contributor.author | Dye, S. | |
dc.date.accessioned | 2022-11-08T16:45:01Z | |
dc.date.available | 2022-11-08T16:45:01Z | |
dc.date.issued | 2022-09-23 | |
dc.identifier.citation | Doherty , M J , Geach , J E , Ivison , R J , Menten , K M , Jacob , A M , Forbrich , J & Dye , S 2022 , ' Ammonia in the interstellar medium of a starbursting disc at z=2.6 ' , Monthly Notices of the Royal Astronomical Society: Letters , vol. 517 , no. 1 , pp. L60-L64 . https://doi.org/10.1093/mnrasl/slac111 | |
dc.identifier.issn | 1745-3925 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/2209.09268v1 | |
dc.identifier.other | ORCID: /0000-0001-8694-4966/work/122647056 | |
dc.identifier.uri | http://hdl.handle.net/2299/25883 | |
dc.description | © 2022 The Authors. This is the accepted manuscript version of an article which has been published in final form at https://doi.org/10.1093/mnrasl/slac111 | |
dc.description.abstract | We report the detection of the ground state rotational emission of ammonia, ortho-NH$_3$ $(J_K=1_0\rightarrow0_0)$ in a gravitationally lensed, intrinsically hyperluminous, star-bursting galaxy at $z=2.6$. The integrated line profile is consistent with other molecular and atomic emission lines which have resolved kinematics well-modelled by a 5 kpc-diametre rotating disc. This implies that the gas responsible for NH$_3$ emission is broadly tracing the global molecular reservoir, but likely distributed in pockets of high density ($n\gtrsim5\times10^4$ cm$^{-3}$). With a luminosity of $2.8\times10^{6}$ $L_\odot$, the NH$_3$ emission represents $2.5\times10^{-7}$ of the total infrared luminosity of the galaxy, comparable to the ratio observed in the Kleinmann-Low nebula in Orion and consistent with sites of massive star formation in the Milky Way. If $L_{\rm NH_3}/L_{\rm IR}$ serves as a proxy for the 'mode' of star formation, this hints that the nature of star formation in extreme starbursts in the early Universe is similar to that of Galactic star-forming regions, with a large fraction of the cold interstellar medium in this state, plausibly driven by a storm of violent disc instabilities in the gas-dominated disc. This supports the 'full of Orions' picture of star formation in the most extreme galaxies seen close to the peak epoch of stellar mass assembly. | en |
dc.format.extent | 835822 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society: Letters | |
dc.subject | astro-ph.GA | |
dc.title | Ammonia in the interstellar medium of a starbursting disc at z=2.6 | en |
dc.contributor.institution | School of Physics, Engineering & Computer Science | |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.contributor.institution | Centre of Data Innovation Research | |
dc.contributor.institution | Centre for Climate Change Research (C3R) | |
dc.contributor.institution | Department of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
dc.identifier.url | https://academic.oup.com/mnrasl/article/517/1/L60/6712731 | |
rioxxterms.versionofrecord | 10.1093/mnrasl/slac111 | |
rioxxterms.type | Other | |
herts.preservation.rarelyaccessed | true | |