Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-10T15:45:09.544Z Has data issue: false hasContentIssue false
  • English
  • Français

Connecting Lost Baryons and Dark Galaxies via QSO Absorption Lines

Published online by Cambridge University Press:  01 June 2007

Todd M. Tripp
Todd M. Tripp*
Affiliation:
Department of Astronomy, University of Massachusetts-Amherst, Amherst, MA 01003, USA email: tripp@astro.umass.edu
Rights & Permissions [Opens in a new window]

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.

QSO absorption lines are sensitive to very low density gas, and consequently, QSO spectroscopy provides a powerful tool for measuring the distribution, physical conditions, and metal enrichment of baryons in the intergalactic medium and in “dark galaxies”. However, ultraviolet spectroscopy is required to study QSO absorbers in the nearby universe where the connections between the absorbing gas and galaxies/environment can be probed. This talk reviewed several recent studies of low-z QSO absorbers in order to demonstrate the value of combining high-resolution ultraviolet spectroscopy with complementary information on the absorber environment, e.g., mapping of 21 cm emission in the vicinity of the absorbers; some notes on these examples are presented in this paper. The absorbers probed range from high-N(H I) damped Lyman α absorbers down to very low-column Lyα forest clouds with log N(H I) < 13.5. The high-N(H I) systems are candidate “dark galaxies” – these systems are more metal enriched than the high-z IGM, possibly due to in-situ star formation, and some of the absorbers are highly metal enriched. However, we have obtained follow-up 21cm emission mapping with the VLA and deep optical imaging, and while we do find H I clouds associated with the absorbers in 21cm emission, we often do not find any evidence of in-situ stars. At this juncture, it seems more likely that these low-z absorbers were enriched with metals within galaxies and were subsequently transported out into the IGM, e.g., by tidal stripping or galactic winds. This contribution also summarizes some recent results on the search for lost baryons in the “warm-hot” (shock-heated) low-redshift IGM.

Keywords

Intergalactic mediumquasars: absorption lines
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S244: Dark Galaxies and Lost Baryons , June 2007 , pp. 63 - 72
Copyright
Copyright © International Astronomical Union 2008

References

Aracil, B., Tripp, T. M., Bowen, D. V., Prochaska, J. X., Chen, H.-W., & Frye, B. L. 2005, ApJ, 367, 139Google Scholar
Briggs, F. H., & Barnes, D. G. 2006, ApJ, 640, L127CrossRefGoogle Scholar
Cen, R. & Ostriker, J. P. 1999, ApJ, 514, 1CrossRefGoogle Scholar
Chen, H.-W., & Prochaska, J. X. 2000, ApJ, 543, L9CrossRefGoogle Scholar
Danforth, C. W., & Shull, J. M. 2005, ApJ, 624, 555CrossRefGoogle Scholar
Davé, R., Hernquist, L., Katz, N., & Weinberg, D. 1999, ApJ, 511, 521CrossRefGoogle Scholar
de Vaucouleurs, G. 1961, ApJS, 6, 213CrossRefGoogle Scholar
Fukugita, M., Hogan, C. J., & Peebles, P. J. E. 1998, ApJ, 503, 518CrossRefGoogle Scholar
Giovanelli, R., & Haynes, M. P. 1989 ApJ, 346, L5CrossRefGoogle Scholar
Gnat, O., & Sternberg, A. 2007, ApJS, 168, 213CrossRefGoogle Scholar
Jenkins, E. B. 1996, ApJ, 471, 292CrossRefGoogle Scholar
Jenkins, E. B., Bowen, D. V., Tripp, T. M., & Sembach, K. R. 2005, ApJ, 623, 767CrossRefGoogle Scholar
Jenkins, E. B., Bowen, D. V., Tripp, T. M., Sembach, K. R., Leighly, K. M., Halpern, J. P., & Lauroesch, J. T. 2003, AJ, 125, 2824CrossRefGoogle Scholar
Klypin, A., Kravtsov, A. V., Valenzuela, O., & Prada, F. 1999, ApJ, 522, 82CrossRefGoogle Scholar
Lehner, N., Savage, B. D., Richter, P., Sembach, K. R., Tripp, T. M., & Wakker, B. P. 2007, ApJ, 658, 680CrossRefGoogle Scholar
Lehner, N., Savage, B. D., Wakker, B. P., Sembach, K. R., & Tripp, T. M. 2006, ApJS, 164, 1CrossRefGoogle Scholar
Minchin, R., et al. 2005, ApJ, 622, L21CrossRefGoogle Scholar
Minchin, R., et al. 2007, ApJ, in press (astro-ph/0706.1586)Google Scholar
Moore, B., et al. 1999, ApJ, 524, L19CrossRefGoogle Scholar
O'Meara, J. M., Burles, S., Prochaska, J. X., Prochter, G. E., Berstein, R. A., & Burgess, K. M. 2006, ApJ, 649, L61CrossRefGoogle Scholar
Penton, S. V., Stocke, J. T., & Shull, J. M. 2004, ApJS, 152, 29CrossRefGoogle Scholar
Persic, M., & Salucci, P. 1992, MNRAS, 258, 14PCrossRefGoogle Scholar
Prochaska, J. X., Chen, H.-W., Howk, J. C., Weiner, B. J., & Mulchaey, J. 2004, ApJ, 617, 718CrossRefGoogle Scholar
Prochaska, J. X., Weiner, B. J., Chen, H.-W., & Mulchaey, J. S. 2006, ApJ, 643, 680CrossRefGoogle Scholar
Richter, P., Savage, B. D., Sembach, K. R., & Tripp, T. M., A&A, 445, 827CrossRefGoogle Scholar
Richter, P., Savage, B. D., Tripp, T. M., & Sembach, K. R. 2004, ApJS, 153, 165CrossRefGoogle Scholar
Savage, B. D., Lehner, N., Wakker, B. P., Sembach, K. R., & Tripp, T. M. 2005, ApJ, 626, 776CrossRefGoogle Scholar
Savage, B. D., & Sembach, K. R. 1991, ApJ, 379, 245CrossRefGoogle Scholar
Savage, B. D., & Sembach, K. R. 1996, ARA&A, 34, 279Google Scholar
Savage, B. D., Sembach, K. R., Tripp, T. M., & Richter, P. 2002, ApJ, 564, 631CrossRefGoogle Scholar
Schaye, J., et al. 2003, ApJ, 596, 768CrossRefGoogle Scholar
Schneider, S. E. 1989, ApJ, 343, 94CrossRefGoogle Scholar
Sembach, K. R. 1999, in Stromlo Workshop on High Velocity Clouds, ASP Conf. Series 166, eds. Gibson, B. K. & Putman, M. E., (San Francisco: ASP), 243Google Scholar
Sembach, K. R., Tripp, T. M., Savage, B. D., & Richter, P. 2004, ApJS, 155, 351CrossRefGoogle Scholar
Shull, J. M., Tumlinson, J., & Giroux, M. L. 2003, ApJ, 594, L107CrossRefGoogle Scholar
Solanes, J. M., Sanchis, T., Salvador-Solé, E., Giovanelli, R., & Haynes, M. P. 2002, AJ, 124, 2440CrossRefGoogle Scholar
Spergel, D. N., et al. 2007, ApJS, 170, 377CrossRefGoogle Scholar
Tonry, J. L., et al. , 2001, ApJ, 546, 681CrossRefGoogle Scholar
Tripp, T. M., Aracil, B., Bowen, D. V., & Jenkins, E. B. 2006, ApJ, 643, L77CrossRefGoogle Scholar
Tripp, T. M., et al. 2003, AJ 125, 3122CrossRefGoogle Scholar
Tripp, T. M., Jenkins, E. B., Bowen, D. V., Prochaska, J. X., Aracil, B., & Ganguly, R. 2005, ApJ, 619, 714CrossRefGoogle Scholar
Tripp, T. M., & Savage, B. D. 2000, ApJ, 542, 42CrossRefGoogle Scholar
Tripp, T. M., Savage, B. D., & Jenkins, E. B. 2000, ApJ 534, L1CrossRefGoogle Scholar
Tripp, T. M., Sembach, K. R., Bowen, D. V., Savage, B. D., Jenkins, E. B., Lehner, N., & Richter, P. 2007, ApJS, submitted (astro-ph/0706.1214)Google Scholar
Tumlinson, J., Shull, J. M., Giroux, M. L., & Stocke, J. T. 2005, ApJ, 620, 95CrossRefGoogle Scholar
Wakker, B. P., & van Woerden, H. 1997, ARA&A, 35, 217Google Scholar