Volume 600, April 2017
|Number of page(s)||6|
|Section||Interstellar and circumstellar matter|
|Published online||28 March 2017|
ALMA hints at the existence of an unseen reservoir of diffuse molecular gas in the Galactic bulge
1 LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, École Normale Supérieure, 75005 Paris, France
2 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
Received: 5 January 2017
Accepted: 6 February 2017
Aims. We aim to understand the unexpected presence of mm-wave molecular absorption at −200 km s-1<v<−140 km s-1 in a direction that is well away from regions of the Galactic bulge where CO emission at such velocities is prominent.
Methods. We compared 89 GHz Cycle 2 ALMA absorption spectra of HCO+, HCN, and HNC toward the extragalactic continuum source B1741-312 at l = −2.14°, b = −1.00° with existing CO, H I, and dust emission and absorption measurements. We placed the atomic and molecular gas in the bulge and disk using circular and non-circular galactic kinematics, deriving N(H I) from a combination of 21 cm emission and absorption and we derive N(H2) from scaling of the HCO+ absorption. We then inverted the variation of near-IR reddening E(J−K) with distance modulus and scale E(J−K) to a total gas column density N(H) that may be compared to N(H I) and N(H2).
Results. At galactocentric radii Rgal> 1.5 kpc, conventional measures such as the standard CO-H2 conversion factor and locally observed N(HCO+)/N(H2) ratio separately imply that H I and H2 contribute about equally to N(H), and the gas-derived N(H) values are in broad agreement with those derived from E(J−K). Within the Galactic bulge at Rgal< 1.5 kpc, H I contributes less than 10% of the material inferred from E(J−K), so that the molecular absorption detected here is needed to understand the extinction.
Key words: Galaxy: bulge / ISM: atoms / ISM: molecules
© ESO, 2017
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