2008/11/10 by Maryvonne Gérin, Maryvonne Gerin, J. R. Goicoechea +5 · 3 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics and Star Formation Studies #Atmospheric Ozone and Climate #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:200810933
submitted to Astronomy and Astrophysics, 11 pages, abridged abstract
arxiv created 2008/11/10 · openalex publication_date 2008/12/22 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
<i>Context. <i/>Far-UV photons (FUV) strongly affect the physical and chemical state of molecular gas in the vicinity of young massive stars.<i>Aims. <i/>Finding molecular tracers of the presence of FUV radiation fields in the millimeter wavelength domain is desirable because IR diagnostics (for instance PAHs) are not easily accessible along high extinction line-of-sights. Furthermore, gas phase diagnostics provide information on the velocity fields.<i>Methods. <i/>We have obtained maps of the HCO and H<sup>13<sup/>CO<sup>+<sup/> ground state lines towards the Horsehead edge at angular resolution with a combination of Plateau de Bure Interferometer (PdBI) and the IRAM-30 m telescope observations. These maps have been complemented with IRAM-30 m observations of several excited transitions at two different positions.<i>Results. <i/>Bright formyl radical emission delineates the illuminated edge of the nebula, with a faint emission remaining towards the shielded molecular core. Viewed from the illuminated star, the HCO emission almost coincides with the PAH and CCH emission. HCO reaches a similar abundance to HCO<sup>+<sup/> in the photon dissociation region (PDR), 1– with respect to H<sub>2<sub/>. To our knowledge, this is the highest HCO abundance ever measured. Pure gas-phase chemistry models fail to reproduce the observed HCO abundance by ~2 orders of magnitude, except if reactions of atomic oxygen with carbon radicals abundant in the PDR (i.e., CH<sub>2<sub/>) play a significant role in the HCO formation. Alternatively, HCO could be produced in the PDR by non-thermal processes such as photo-processing of ice mantles and subsequent photo-desorption of either HCO or H<sub>2<sub/>CO, and further gas phase photodissociation. <i>Conclusions. <i/>The measured HCO/H<sup>13<sup/>CO<sup>+<sup/> abundance ratio is large towards the PDR (50), and much lower toward the gas shielded from FUV radiation (<i>≲<i/>1). We propose that high HCO abundances (<i>≳<i/>10<sup>-10<sup/>) together with large HCO/H<sup>13<sup/>CO<sup>+<sup/> abundance ratios (<i>≳<i/>1) are sensitive diagnostics of the presence of active photochemistry induced by FUV radiation.