BIB-VERSION:: AST-PP-v1.0 ID:: epreps.stsci//prep1206 ENTRY:: March 9, 1998 TITLE:: Cold Massive Molecular Clouds in the Inner Disk of M31 SUBTITLE:: AUTHOR:: Loinard, Laurent (1)(2) AUTHOR:: Allen, Ronald J. (1) AFFIL:: (1) Space Telescope Science Institute 3700 San Martin Drive Baltimore, MD 21218 USA AFFIL:: (2) Observatoire de Grenoble, Laboratoire d'Astrophysique, Université Joseph Fourier, B.P. 53X, F-38041 Grenoble Cedex France DATE:: December 1997 JOURNAL:: To appear in: The Astrophysical Journal SUBMITTED:: 10 October 1997 ACCEPTED:: 9 December 1997 OTHER_ACCESS:: COPYRIGHT:: Copyright 1997 The Association of Universities for Research in Astronomy, Inc. All Rights Reserved. LANGUAGE:: English ABSTRACT:: We present new interferometric ¹²CO(1-0) and single-dish ¹²CO(3-2) observations of the central parts of D478, a large (> 200 pc) dark dust cloud located in a quiescent region in the inner disk of M31 where single-dish ¹²CO(1-0) and ¹²CO(2-1) observations were previously obtained. Only a small fraction (< 15%) of the ¹²CO(1-0) flux previously detected in this region with the single-dish telescope is recorded by the interferometer. Most of the ¹²CO(1-0) emission must therefore have the appearance of a smooth surface with very little structure on scales smaller than ~ 25" (85 pc). Together with the earlier ¹²CO(1-0) and ¹²CO(2-1) single-dish results the new ¹²CO(3-2) data are in good agreement with LTE predictions for optically thick lines at T_ex = T_kin = 3.5K. These results rule out the conventional model for these clouds consisting of warm clumps with a low filling factor (as would be the case if they resembled Galactic GMCs) and confirm that large, massive, cold molecular clouds exist in the inner disk of M31 with kinetic temperatures close to that of the cosmic microwave background. Such extremely low temperatures are likely to be a consequence of the low heating rate in these particular regions of M31, where very little massive star formation is occurring at present. From the ¹²CO line profile widths we estimate the Virial mass surface density of D478 to be 80 - 177 M

pc^-2. This is a factor 7 - 16 times larger than the value obtained by multiplying the ¹²CO profile integrals with the conventional "X-factor". END:: epreps.stsci//prep1206