2007A&A...473..863D


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.16CEST20:14:27

2007A&A...473..863D - Astronomy and Astrophysics, volume 473, 863-870 (2007/10-3)

Molecular gas in high-velocity clouds: revisited scenario.

DESSAUGES-ZAVADSKY M., COMBES F. and PFENNIGER D.

Abstract (from CDS):

We report a new search for 12CO(1-0) emission in high-velocity clouds (HVCs) performed with the IRAM 30m millimeter-wave telescope. This search was motivated by the recent detection of cold dust emission (T∼10.7K) in the HVCs of Complex C, implying a total gas column density 5 times larger than the column density measured in HI and suggesting undetected gas, presumably in molecular form. Despite a spatial resolution which is three times better and sensitivity twice as good compared to previous studies, no CO emission is detected in the HVCs of Complex C down to a best 5σ limit of 0.16K.km/s at a 22'' resolution. The non-detection of both the 12CO(1-0) emission and of the diffuse H2 absorption with the Far Ultraviolet Spectroscopic Explorer does not provide any evidence in favor of large amounts of molecular gas in these HVCs and hence in favor of the infrared findings. We discuss different configurations which, however, allow us to reconcile the negative CO result with the presence of molecular gas and cold dust emission. H2 column densities higher than our detection limit, N(H2)=3x1019cm–2, are expected to be confined in very small and dense clumps with 20 times smaller sizes than the 0.5pc clumps resolved in our observations according to the results obtained in cirrus clouds, and might thus still be highly diluted. As a consequence, the inter-clump gas at the 1pc scale, as resolved in our data, has a volume density lower than 20/cm3 and already appears as too diffuse to excite the CO molecules. The observed physical conditions in the HVCs of Complex C also play an important role against CO emission detection. The sub-solar metallicity of 0.1-0.3 dex affects the H2 formation rate onto dust grains, and it has been shown that the CO-to-H2 conversion factor in low metallicity media is 60 times higher than at the solar metallicity, leading for a given H2 column density to a 60 times weaker integrated CO intensity. And the very low dust temperature estimated in these HVCs implies the possible presence of gas cold enough (<20K) to cause CO condensation onto dust grains under interstellar medium pressure conditions and thus CO depletion in gas-phase observations.

Abstract Copyright:

Journal keyword(s): Galaxy: halo - ISM: clouds - ISM: molecules - radio lines: ISM

Simbad objects: 8

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Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME Magellanic Stream HVC 00 32 -30.0           ~ 773 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9088 1
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5373 1
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14323 1
5 HRK 135.3+54.5 Cld 11 51 39 +61 13.3           ~ 21 0
6 NAME HVC Complex C HVC 16 34.8 +63 07           ~ 225 1
7 NAME Draco Cloud MoC 16 48 17 +60 11.8           ~ 63 1
8 NAME Local Group GrG ~ ~           ~ 6658 0

    Equat.    Gal    SGal    Ecl

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2019.10.16-20:14:27

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