Hostname: page-component-5c6d5d7d68-7tdvq Total loading time: 0 Render date: 2024-08-30T19:24:03.007Z Has data issue: false hasContentIssue false
  • English
  • Français

X-ray Astronomy and the IR Background

Published online by Cambridge University Press:  13 May 2016

Richard Mushotzky
Richard Mushotzky*
Affiliation:
Laboratory for High Energy Astrophysics, Goddard Space Flight Center, Greenbelt, MD, 20771, USA

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.

I review the recent Chandra results on the sources of the X-ray background and the X-ray properties of the SCUBA sources. We conclude that 10–20% of the IR background is produced by active galaxies and a similar fraction of the SCUBA sources harbor luminous AGN. Many of the Chandra sources are apparently luminous infrared galaxies themselves, but factors of 2–10 below the SCUBA limits. We summarize the X-ray evidence for metal production in groups and clusters and point out that these data require considerably more star formation than inferred from optical stellar data. The abundance ratios of Fe and Si indicate that much of the metals in groups and clusters was produced by massive stars, and the lack of evolution in Fe out to z ~ 0.5 argues for quite an early origin for the metals. This same process also seems to have injected considerable energy into the gas in groups and clusters, which may have dominated the mechanism of star formation and produced a metal-enriched intergalactic medium

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 204: The Extragalactic Infrared Background and its Cosmological Implication , 2001 , pp. 335 - 345
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Almaini, O., Lawrence, A., & Boyle, B. J. 1999, MNRAS, 305, L59 Google Scholar
Barger, A. J., Cowie, L. L., Mushotzky, R. F., & Richards, E. A. 2000, AJ, submitted; astro-ph/0007175 Google Scholar
Bautz, M. W., Malm, M. R., Baganoff, F. K., Ricker, G. R., et al. 2000, astroph/0008050 Google Scholar
Comastri, A., Setti, G., Zamorani, G., & Hasinger, G. 1995, A&A, 296, 1 Google Scholar
David, L. P., Forman, W., & Jones, C. 1991, ApJ, 380, 39 Google Scholar
Davé, R., Cen, R., Ostriker, J. P., Bryan, G., et al. 2000, astro-ph/0007217 Google Scholar
Davis, D. S., Mulchaey, J. S., & Mushotzky, R. F. 1999, ApJ, 511, 34 Google Scholar
Donahue, M., Voit, G. M., Scharf, C. A., Gioia, I. M., et al. 1999, ApJ, 527, 525 Google Scholar
Eke, V. R., Navarro, J. F., & Frenk, C. S. 1998, ApJ, 503, 569 CrossRefGoogle Scholar
Fabian, A. C., et al. 2000, MNRAS, 315, L8 Google Scholar
Fukazawa, Y., Makishima, K., Tamura, T., Ezawa, H., et al. 1998, PASJ, 50, 187 Google Scholar
Fukazawa, Y., Makishima, K., Tamura, T., Nakazawa, K., et al. 2000, MNRAS, 313, 21 Google Scholar
Fukugita, M., Hogan, C. J., & Peebles, P. J. E. 1998, ApJ, 503, 518 Google Scholar
Gebhardt, K., Bender, R., Bower, R., Dressier, A., et al. 2000, ApJ, 539, L13 Google Scholar
Gibson, B. K., Loewenstein, M., & Mushotzky, R. F. 1997, MNRAS, 290, 623 Google Scholar
Gunn, K. F., & Shanks, T. 1998, AN, 319, 66 Google Scholar
Haiman, Z., & Loeb, A. 1999, ApJ, 521, L9 Google Scholar
Heckman, T. M. 2000, in Proceedings, Gas & Galaxy Evolution, astro-ph/0009075 Google Scholar
Hornschemeier, A. E., Brandt, W. N., Garmire, G. P., Schneider, D. P., et al. 2000, ApJ, 541, 49 Google Scholar
Iwasawa, K., & Comastri, A. 1998, MNRAS, 297, 1219 Google Scholar
Krabbe, A., Boeker, T., & Maiolino, R. 2000, astro-ph/0010119 Google Scholar
Lloyd-Davies, E. J., Ponman, T. J., & Cannon, D. B. 2000, MNRAS, 315, 689 Google Scholar
Loewenstein, M. 2000, ApJ, 532, 17 Google Scholar
Loewenstein, M., & Mushotzky, R. F. 1996, ApJ, 466, 695 Google Scholar
Lutz, D., Genzel, R., Sternberg, A., Netzer, H., et al. 1996, A&A, 315, L137 Google Scholar
Madau, P., Ferguson, H., Dickinson, M., Giavalisco, M., et al. 1996, MNRAS, 283, 1388 Google Scholar
Madejski, G., Zycki, P., Done, C., Valinia, A., et al. 2000, ApJ, 535, L87 Google Scholar
Merritt, D., & Ferrarese, L. 2000, astro-ph/0009076 Google Scholar
Mushotzky, R., Loewenstein, M., Arnaud, K. A., Tamura, T., et al. 1996, ApJ, 466, 686 Google Scholar
Mushotzky, R. F., & Loewenstein, M. 1997, ApJ, 481, L63 Google Scholar
Mushotzky, R. F., Cowie, L. L., Barger, A. J., & Arnaud, K. A. 2000, Nature, 404, 459 Google Scholar
Pen, Ue-Li 1999, ApJ, 510, L1 Google Scholar
Ponman, T. J., Cannon, D. B., & Navarro, J. F. 1999, Nature, 397, 135 Google Scholar
Renzini, A., Ciotti, L., D'Ercole, A., & Pellegrini, S. 1993, ApJ, 419, 52 Google Scholar
Serlemitsos, P. J., Smith, B. W., Boldt, E. A., Holt, S. S., & Swank, J. H. 1977, ApJ, 211 L63 Google Scholar
Severgnini, P., Maiolino, R., Salvati, M., Axon, D., et al. 2000, astro-ph/0006233 Google Scholar
Somerville, R. S., & Primack, J. R. 1999, MNRAS, 310, 1087 Google Scholar
Valageas, P., & Silk, J. 1999, A&A, 350, 72 Google Scholar
White, R. E. III 1991, ApJ, 367, 69 Google Scholar
White, S. D. M., Navarro, J. F., Evrard, A. E., & Frenk, C. S. 1993, Nature, 366, 429 Google Scholar