2013ApJ...777...19H
A Low-metallicity Molecular Cloud in the Lower Galactic Halo
Hernandez, Audra K. ( Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706, USA ); Wakker, Bart P. ( Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706, USA ); Benjamin, Robert A. ( Department of Physics, University of Wisconsin-Whitewater, Whitewater, WI 53190, USA ); French, David ( Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706, USA ); Kerp, Juergen ( Argelander-Institut für Astronomie, Auf dem Hügel 71, D-53121 Bonn, Germany ); Lockman, Felix J. ( National Radio Astronomy Observatory, Green Bank, WV 24944, USA ); O'Toole, Simon ( Australian Astronomical Observatory, P.O. Box 296, Epping 1710, Australia ); Winkel, Benjamin ( Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, D-53121 Bonn, Germany ) show affiliations
The Astrophysical Journal, Volume 777, Issue 1, article id. 19, 14 pp. (2013).
Published in Nov 2013
We find evidence for the impact of infalling, low-metallicity gas on the Galactic disk. This is based on FUV absorption line spectra, 21 cm emission line spectra, and far-infrared (FIR) mapping to estimate the abundance and physical properties of IV21 (IVC135+54-45), a galactic intermediate-velocity molecular cloud that lies ~300 pc above the disk. The metallicity of IV21 was estimated using observations toward the subdwarf B star PG1144+615, located at a projected distance of 16 pc from the cloud's densest core, by measuring ion and H I column densities for comparison with known solar abundances. Despite the cloud's bright FIR emission and large column densities of molecular gas as traced by CO, we find that it has a sub-solar metallicity of log (Z/Z ) = -0.43 ± 0.12 dex. IV21 is thus the first known sub-solar metallicity cloud in the solar neighborhood. In contrast, most intermediate-velocity clouds (IVC) have near-solar metallicities and are believed to originate in the Galactic Fountain. The cloud's low metallicity is also atypical for Galactic molecular clouds, especially in light of the bright FIR emission which suggest a substantial dust content. The measured I 100 μm/N(H I) ratio is a factor of three below the average found in high latitude H I clouds within the solar neighborhood. We argue that IV21 represents the impact of an infalling, low-metallicity high-velocity cloud that is mixing with disk gas in the lower Galactic halo.Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from MAST at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program No. 12275. The Green Bank Telescope is part of the National Radio Astronomy Observatory which is a Facility of the National Science Foundation, operated by Associated Universities, Inc.
Keywords:
Free Keywords: Astrophysics - Galaxy Astrophysics; Galaxy: disk; Galaxy: halo; ISM: clouds; ISM: general; ultraviolet: ISM
Astronomy: Galaxy: disk; Galaxy: halo; ISM: clouds; ISM: general; ultraviolet: ISM
arXiv: Astrophysics - Galaxy Astrophysics
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