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Date and Time of the Query: 2019-06-20 T09:30:39 PDT
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For refcode 1996A&A...307..237L:
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1996A&A...307..237L The Plateau de Bure survey of galactic {lambda}3mm HCO^+^ absorption toward compact extragalactic continuum sources R. Lucas and N. Liszt Institut de Radioastronomie Millimetrique, 300 Rue de la Piscine, F-38406 Saint Martin d'Heres, France National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA Received 20 March 1995/Accepted 28 June 1995 Abstract. We have observed galactic {lambda}3mm HCO^+^ absorption along 30 lines of sight toward compact extragalactic mm-wave continuum sources, using the Plateau de Bure Interferometer. Such absorption is surprisingly common, occurring approximately 30% as often as {lambda}21cm absorption in H I. In fact, the mean free path for detection of absorption with optical depth of unity is the same in both species. The slope of the HCO^+^ optical depth and column density distribution functions is very similar to that of H I but the mean HCO^+^ linewidth is much smaller, 0.95 km s^-1^. A search for accompanying HCO^+^ emission finds only an occasional weak (0.05 K) line, even when {tau}(HCO^+^) >~ 1, so that quite accurate column densities may be derived from observations of only the lowest line. In comparing CO (emission) and HCO^+^ absorption, little consistency is at first apparent. However, we can now show that the strength of CO emission increases abruptly when N(HCO^+^) ~ 1 - 2 x 10^12^cm^-2^. This is the same phenomenon observed in uv-absorption studies at N(H_2_)~4 x 10^20^ cm^-2^ and is understandable in terms of the onset of dust- and self-shielding at extinctions below 1 magnitude in diffuse clouds or the outer regions of dark clouds. A similar turn on occurs in N(H_2_CO) at the same values of N(HCO^+^). Comparison of CO and HCO^+^ emission and absorption can also be used to derive the physical conditions in the clouds; in general we find n(H_2_)T_K_ = 0.5 - 1.0 x 10^4^ cm^-3^ K if T_K_ >= 10K. This is within but at the high end of the range for diffuse clouds studied optically and well below values appropriate to dark cloud cores. In a few cases, the presence of a relatively large electron fraction (X(e) <~ 1 - 3 x 10^-4^) seems indicated, along with temperatures of 20 - 30K. Thus the excitation analysis is consistent with the existence of a CO turn on. Although it is somewhat surprising that relatively strong CO and (especially) ^13^CO emission is present when carbon is only partially recombined to and bound up in carbon monoxide, this is not atypical in the outer regions of dark clouds. We have also surveyed {lambda}18cm OH absorption in six directions using the VLA. Unlike most other species, but in keeping with traditional notions of diffuse cloud chemistry, there is a remarkably uniform relationship between the OH and HCO^+^ column densities, even at low values. We find X(HCO^+^) = 0.03 - 0.05X(OH) for 1 x 10^12^ cm^-2^ <~ N(OH) <~ 20 x 10^12^ cm^-2^; this is within 40% of values quoted for TMC-1, but at 100 times lower column density. Using relevant values of X(OH) observed in uv absorption spectra of diffuse clouds, X(OH) ~ 1 - 2 x 10^-7^ at N(OH) = 5 x 10^13^ cm^-2^ and E(B-V) = 0.3 mag, it follows that X(HCO^+^) ~ 3 - 6 x 10^-9^ across a very broad range of extinction. Apparently, many diatomics and polyatomics form readily in diffuse clouds as long as there is any appreciable amount of H_2_ formation, and well before the carbon conversion from C^+^ to CO is complete or CO emission is strong. Although the strong coupling between OH and HCO^+^ is characteristic of conventional diffuse cloud chemistry, such chemistry in general falls far short of reproducing the observed amounts of HCO^+^ and perhaps CO, even when OH can be explained. Although not understood at present, it is clearly the case that many molecules, including those formed on grains (i.e. H_2_CO), appear with abundances characteristic of dark, cold, cloud cores even when A_V_ <~ 1 mag. Key words: interstellar medium: molecules; abundances; clouds; structure - radio lines: ISM
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