2009
DOI: 10.1111/j.1365-2966.2009.15501.x
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ISOobservation of molecular hydrogen and fine-structure lines in the photodissociation region IC���63

Abstract: We wish to constrain the main physical properties of the photodissociation region (PDR) IC 63. We present the results of a survey for the lowest pure-rotational lines of H 2 with the Short Wavelength Spectrometer and for the major fine-structure cooling lines of O I at 63 and 145 μm and C II at 157.7 μm with the Long Wavelength Spectrometer on board the Infrared Space Observatory (ISO) in the high-density PDR IC 63. The observations are compared with available photochemical models based on optical absorption a… Show more

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Cited by 27 publications
(40 citation statements)
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References 37 publications
(50 reference statements)
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“…Theoretical calculations, confirmed by experimental results studying H 2 formation on graphite (Latimer et al, 2008;Islam et al, 2007Islam et al, , 2010, show that ro-vibrational excitation of H 2 leaving the surface upon formation is concentrated around high values of the vibrational quantum number (3-4) and low values of the rotational quantum number. There have been a few attempts to detect a signature of such H 2 formation, via observations of transitions of H 2 in appropriate regions of the ISM, but with no success to date (Tiné et al, 2003;Thi et al, 2009). The ortho (odd rotational quantum number J) to para (even J) ratio of H 2 can yield information concerning the thermal history of the associated cloud, as well as concerning the conditions associated with H 2 formation on the grains of the cloud (Wilgenbus et al, 2000;Le Bourlot, 2000), although presence of other H 2 molecules co-adsorbed on the grain can hinder the release of excited molecules (Congiu et al, 2009).…”
Section: Experiments and Quantum Calculationsmentioning
confidence: 99%
“…Theoretical calculations, confirmed by experimental results studying H 2 formation on graphite (Latimer et al, 2008;Islam et al, 2007Islam et al, , 2010, show that ro-vibrational excitation of H 2 leaving the surface upon formation is concentrated around high values of the vibrational quantum number (3-4) and low values of the rotational quantum number. There have been a few attempts to detect a signature of such H 2 formation, via observations of transitions of H 2 in appropriate regions of the ISM, but with no success to date (Tiné et al, 2003;Thi et al, 2009). The ortho (odd rotational quantum number J) to para (even J) ratio of H 2 can yield information concerning the thermal history of the associated cloud, as well as concerning the conditions associated with H 2 formation on the grains of the cloud (Wilgenbus et al, 2000;Le Bourlot, 2000), although presence of other H 2 molecules co-adsorbed on the grain can hinder the release of excited molecules (Congiu et al, 2009).…”
Section: Experiments and Quantum Calculationsmentioning
confidence: 99%
“…This model has already been successfully used several times to model PDRs in the Galaxy (e.g. Thi et al 2009).…”
Section: The Minimum Gas Temperature In Crdrmentioning
confidence: 99%
“…Searches of rovibrational excitation of H 2 that could be ascribed to "UV formation pumping" in PDR and dense clouds yielded no positive detection (Tinéetal. 2003;Lemaire & Field 2001;Thi et al 2009). …”
Section: Introductionmentioning
confidence: 99%