Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-25T22:02:07.193Z Has data issue: false hasContentIssue false
  • English
  • Français

The Deuterium Abundance In The Galactic Center 50 km/s Molecular Cloud: Evidence For A Cosmological Origin Of D

Published online by Cambridge University Press:  25 May 2016

D. A. Lubowich ,
Jay M. Pasachoff ,
Robert P. Galloway ,
Thomas J. Balonek ,
Christy Tremonti ,
Tom Millar  and
Helen Roberts
D. A. Lubowich
Affiliation:
Dept. of Physics, Hofstra U., Hempstead, NY &AIP, Melville, NY
Jay M. Pasachoff
Affiliation:
Dept. of Astronomy, Williams College, Williamstown, MA
Robert P. Galloway
Affiliation:
Dept. of Astronomy, Williams College, Williamstown, MA
Thomas J. Balonek
Affiliation:
Dept. of Physics, Colgate University, Hamilton, NY
Christy Tremonti
Affiliation:
Dept. of Physics, Colgate University, Hamilton, NY
Tom Millar
Affiliation:
Dept. of Physics, Univ. Manchester Institute of Technology, Manchester, UK
Helen Roberts
Affiliation:
Dept. of Physics, Univ. Manchester Institute of Technology, Manchester, UK

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We confirm that deuterium exists in the Galactic Center (GC) and estimate that D/H = 3 × 10−6 using a new 5192-chemical reaction model. This is the lowest D/H ratio observed in the Galaxy, five times lower than the local ISM D/H = 1.5 × 10−5 but 106 × larger than D/H predicted by GC models. We detected DCN in the GC Sgr A 50 km/s molecular cloud located 10 pc from the GC with the NRAO 12m telescope and obtained T*R = 0.061 ± 0.007 K and 0.04 ± 0.02 K for the J = 1-0 and 2-1 lines. The most likely source of the GC D is continuous injection from the infall of primordial matter with D/H = 5 × 10−5 with the D/H determined by astration and mixing. Thus there are no significant Galactic sources of D and no recent quasar or AGN activity in the GC. This primordial D/H implies that the baryon density is less than the density necessary to close the Universe; most of the baryons are in dark matter; and there are fewer than four ν families.

Type
3. Abundances of D, 3He and 4He
Information
Symposium - International Astronomical Union , Volume 198: The Light Elements and their Evolution , 2000 , pp. 167 - 175
Copyright
Copyright © Astronomical Society of the Pacific 2000 

References

Audouze, J., Lequeux, J., Reeves, H., & Vigroux, L. 1976, ApJ, 208, L51 Google Scholar
Boyd, R.N., Ferland, G.J., & Schramm, D.N. 1989, ApJ, 336, L1 Google Scholar
Chengalur, J. N., Braun, R., & Butler, , Burton, W. 1997, A&A, 318, L35.Google Scholar
Copi, C. J., Schramm, D.N., & Turner, M.S. 1995, Phys. Rev. Letters, 75, 3981 Google Scholar
Genzel, R., Hollenbach, D., & Townes, C.H. 1994, Reports Prog. Phys., 57, 417 Google Scholar
Glisten, R. & Ungerechts, H. 1985, A&A, 145, 241 Google Scholar
Harris, , Michael, J., Share, , Gerald, H., & Messina, , Daniel, C. 1995, ApJ, 448, 157 Google Scholar
Hatchell, J., Millar, T.J., & Rodgers, S. D. 1998, A&A, 332, 695.Google Scholar
Jacq, T., Baudry, A., Walmsley, C.M., & Caselli, P., 1999, A&A, 347, 957 Google Scholar
Linsky, J. L. 1998, Space Sci. Rev. 84, 285 Google Scholar
Lovas, F. J. 1992. J. Phys. & Chem. Reference Data 21, 181 Google Scholar
Lubowich, D. A., Anantharamaiah, K.R., & Pasachoff, J.M. 1989, ApJ, 345, 770 Google Scholar
Lubowich, D. A., Turner, B.E., & Hobbs, L.M. 1998 ApJ, 508, 729 Google Scholar
Mastichades, A. & Ozernoy, L. M. 1994, ApJ, 426, 599 Google Scholar
Mayer-Hasselwander, et al. 1998, A&A, 335, 161 Google Scholar
Minh, Y.C., Irvine, W.M., & Friberg, P. 1992, A&A, 258, 489 Google Scholar
Ozernoi, L., & Chernomordik, V.V. 1975, Sov. Astron. 19, 693 Google Scholar
Pasachoff, J. M., & Vidal Madjar, A. 1989, Comments in Astrophysics, 14, 61 Google Scholar
Penzias, A.A. 1979, ApJ, 228, 430 Google Scholar
Poglitsch, A., Stacey, G. J., Geis, N., Haggerty, M., Jackson, J., Rumitz, M., Genzel, R., Townes, C. H. 1991, ApJ, L33 Google Scholar
Prantzos, N. 1996, A&A, 310, 106 Google Scholar
Rodgers, S.D. & Millar, T.J. 1996, MNRAS, 280, 1046 Google Scholar
Schramm, D. N., & Turner, M. S. 1998, Rev. Mod. Physics, 70, 303 Google Scholar
Serabyn, E., Lacy, J.H., & Actermann, J.M. 1992, ApJ 395, 166 Google Scholar
Simpson, J.P., Colgan, S.W.J., Rubin, R.H., Erickson, E.F., & Haas, M.R. 1995, ApJ, 444, 721 Google Scholar
Vidal-Madjar, A. 2000, Nucl. Phys. B (Proc. Suppl.), 80 119 Google Scholar