# Far-infrared molecular lines from Low- to High-Mass Star Forming Regions observed with Herschel

2 FORMATION STELLAIRE 2014
L3AB - Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux, OASU - Observatoire aquitain des sciences de l'univers, LAB - Laboratoire d'Astrophysique de Bordeaux [Pessac], Université Sciences et Technologies - Bordeaux 1
Abstract : (Abridged) We study the response of the gas to energetic processes associated with high-mass star formation and compare it with studies on low- and intermediate-mass young stellar objects (YSOs) using the same methods. The far-IR line emission and absorption of CO, H$_2$O, OH, and [OI] reveals the excitation and the relative contribution of different species to the gas cooling budget. Herschel-PACS spectra covering 55-190 um are analyzed for ten high-mass star forming regions of various luminosities and evolutionary stages at spatial scales of ~10^4 AU. Radiative transfer models are used to determine the contribution of the envelope to the far-IR CO emission. The close environments of high-mass YSOs show strong far-IR emission from molecules, atoms, and ions. Water is detected in all 10 objects even up to high excitation lines. CO lines from J=14-13 up to typically 29-28 show a single temperature component, Trot~300 K. Typical H$_2$O temperatures are Trot~250 K, while OH has Trot~80 K. Far-IR line cooling is dominated by CO (~75 %) and to a smaller extent by OI (~20 %), which increases for the most evolved sources. H$_2$O is less important as a coolant for high-mass sources because many lines are in absorption. Emission from the envelope is responsible for ~45-85 % of the total CO luminosity in high-mass sources compared with only ~10 % for low-mass YSOs. The highest-J lines originate most likely from shocks, based on the strong correlation of CO and H$_2$O with physical parameters of the sources from low- to high-masses. Excitation of warm CO is very similar for all mass regimes, whereas H$_2$O temperatures are ~100 K higher for high-mass sources than the low-mass YSOs. Molecular cooling is ~4 times more important than cooling by [OI]. The total far-IR line luminosity is about 10$^{-3}$ and 10$^{-5}$ times lower than the dust luminosity for the low- and high-mass YSOs.
Type de document :
Article dans une revue
Astronomy and Astrophysics - A&A, EDP Sciences, 2014, 562, pp.id.A45. 〈10.1051/0004-6361/201321954〉
Domaine :

https://hal.archives-ouvertes.fr/hal-00944378
Contributeur : Marie-Paule Pomies <>
Soumis le : lundi 10 février 2014 - 15:23:08
Dernière modification le : jeudi 11 janvier 2018 - 06:26:59

### Citation

A. Karska, Fabrice Herpin, S. Bruderer, J. R. Goicoechea, G. J. Herczeg, et al.. Far-infrared molecular lines from Low- to High-Mass Star Forming Regions observed with Herschel. Astronomy and Astrophysics - A&A, EDP Sciences, 2014, 562, pp.id.A45. 〈10.1051/0004-6361/201321954〉. 〈hal-00944378〉

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