Physics and chemistry of UV illuminated gas: the Horsehead case. (5th March 2015)

• Record Type: Journal Article
• Authors: Guzmán, V.; Pety, J.; Gratier, P.; Goicoechea, J. R.; Gerin, M.; Roueff, E.; Teyssier, D.
• Editors: Montmerle, Thierry
• Is Part Of: Proceedings of the International Astronomical Union. Volume 10:Number H16(2012)Highlights
• Page Start: 593
• Page End: 593
• Publication Date: 2015-03-05
• Subjects: astrochemistry, -- ISM: clouds, -- ISM: molecules; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921314012332
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: Molecular lines are used to trace the physical conditions of the gas in different environments, from high-z galaxies to proto-planetary disks. To fully benefit from the diagnostic power of the molecular lines, the formation and destruction paths of the molecules must be quantitatively understood. This is challenging because the physical conditions are extreme and the dynamic plays an important role. In this context the PDR of the Horsehead mane is a particularly interesting case because the geometry is simple (almost 1D, viewed edge-on; Abergel et al. 2003 ), the density profile is well constrained and we are making several efforts to constrain the thermal profile. The combination of small distance to Earth (at 400 pc, 1″ corresponds to 0.002 pc), low illumination (χ = 60) and high density ( n H ~ 10 5 cm −3 ) implies that all the interesting physical and chemical processes can be probed in a field-of-view of less than 50″ (with typical spatial scales ranging between 1″ and 10″). Hence, the Horsehead PDR is a good source to benchmark the physics and chemistry of UV illuminated neutral gas. In our recent work on the ISM physics and chemistry in the Horsehead we have shown the importance of the interplay between the solid and gas phase chemistry in the formation of (complex) organic molecules, like H2 CO, CH3 OH and CH3 CN, which reveal that photo-desorption of ices is an efficient mechanism to release molecules into the gas phase (Guzmán et al. 2011, Gratier et al. in prep, Guzman et al. in prep)}. We have also provided new diagnostics of the UV illuminated matter. For example, we detected CF + and resolved its hyperfine structure (Guzman et al. 2012b ). We propose that CF +, which is observable from the ground, can be used as a proxy of C + (Guzman et al. 2012 ). Finally, we reported the first detection of the small hydrocarbon C3 H +, which sheds light on the formation pathways of other observed small hydrocarbons, like C3 H and C3 H2 ((Pety et al. 2012). Part of these results were possible thanks to a complete an unbiased line survey at 1, 2 and 3 mm performed with the IRAM-30m telescope (Horsehead WHISPER), where approximately 30 species (plus their isotopologues) are detected.