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Molecular cloud photoevaporation and far-infrared line emission
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden.;Dipartimento Fis & Astron, Viale Berti Pichat 6, I-40127 Bologna, Italy.;Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy..
Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.;Univ Tokyo, Todai Inst Adv Study, Kavli IPMU WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan..
Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.;Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.;Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England..
Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy..
2017 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 467, no 2, p. 1300-1312Article in journal (Refereed) Published
Abstract [en]

With the aim of improving predictions on far-infrared (FIR) line emission from Giant Molecular Clouds (GMCs), we study the effects of photoevaporation (PE) produced by external farultraviolet (FUV) and ionizing (extreme-ultraviolet) radiation on GMC structure. We consider three different GMCs with mass in the range M-GMC = 10(3)-10(6)M(O). Our model includes (i) an observationally based inhomogeneous GMC density field, and (ii) its time evolution during the PE process. In the fiducial case (M-GMC approximate to 10(5)M(O)), the PE time (t(pe)) increases from 1 to 30 Myr for gasmetallicityZ = 0.05-1 Z(O)), respectively. Next, we compute the time-dependent luminosity of key FIR lines tracing the neutral and ionized gas layers of the GMCs, ([C II] at 158 mu m, [O III] at 88 mu m) as a function of G(0), and Z until complete PE at t(pe). We find that the specific [C II] luminosity is almost independent of the GMC model within the survival time of the cloud. Stronger FUV fluxes produce higher [C II] and [O III] luminosities, however, lasting for progressively shorter times. At Z = Z(O), the [CII] emission is maximized (LCII approximate to 10(4) L-O for the fiducial model) for t < 1Myr and logG(0) >= 3. Noticeably, and consistently with the recent detection by Inoue et al. of a galaxy at redshift z approximate to 7.2, for Z = 0.2Z(O), the [OIII] line might outshine [C II] emission by up to approximate to 1000 times. We conclude that the [OIII] line is a key diagnostic of low-metallicity interstellar medium, especially in galaxies with very young stellar populations.

Place, publisher, year, edition, pages
Oxford University Press, 2017. Vol. 467, no 2, p. 1300-1312
Keywords [en]
line: formation, ISM: clouds, galaxies: high-redshift, galaxies: ISM, infrared: ISM
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-242300DOI: 10.1093/mnras/stx180ISI: 000398416700005Scopus ID: 2-s2.0-85018349619OAI: oai:DiVA.org:kth-242300DiVA, id: diva2:1287491
Note

QC 20190211

Available from: 2019-02-11 Created: 2019-02-11 Last updated: 2019-02-11Bibliographically approved

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