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The “entropy floor” is porous – remarks on the coexistence of star formation and kinetic AGN feedback

Published online by Cambridge University Press:  25 July 2014

Grant R. Tremblay
Grant R. Tremblay*
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany email: grant.tremblay@eso.org
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Abstract

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We discuss the morphology of star forming clouds and filaments in the central (≲ 50 kpc) regions of 16 low redshift (z<0.3) cool core brightest cluster galaxies (BCGs). The sample spans decades-wide ranges of X-ray mass deposition and star formation rates as well as active galactic nucleus (AGN) mechanical power, encompassing both high and low extremes of the supposed intracluster medium (ICM) cooling and AGN heating feedback cycle. Amid evidence that the gas fueling both star formation and AGN activity has condensed from the hot atmosphere, we present new and archival Hubble Space Telescope (HST) images of far ultraviolet (FUV) continuum emission directly associated with young stars, acting as a calorimeter for the degree to which the suppression of star formation by AGN mechanical feedback may be spatially or temporally inefficient. We discuss evidence for temporal and possibly cyclical variation in star formation rate, wherein elevated cooling episodes are permitted when AGN feedback is in a low-power state, and vice-versa. Several sources exhibit strong morphological evidence that low levels of star formation can survive and may indeed be triggered by the passage of a propagating radio source. We conclude by discussing the apparent coexistence of feedback and star formation. If AGN mechanical power does establish an “entropy floor”, this floor must be porous, or raise and lower as the AGN varies in power.

Keywords

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Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S304: Multiwavelength AGN Surveys and Studies , October 2013 , pp. 331 - 334
Copyright
Copyright © International Astronomical Union 2014 

References

Bîrzan, L., Rafferty, D. A., McNamara, B. R., Wise, M. W., & Nulsen, P. E. J., 2004, ApJ, 607, 800CrossRefGoogle Scholar
Donahue, M., Mack, J., Voit, G. M., Sparks, W., Elston, R., & Maloney, P. R., 2000, ApJ, 545, 670Google Scholar
Donahue, M., de Messières, G. E., O'Connell, R. W., et al. 2011, ApJ, 732, 40Google Scholar
Edge, A. C., 2001, MNRAS, 328, 762Google Scholar
Edge, A. C., Oonk, J. B. R., Mittal, R., et al. 2010, A&A, 518, L47Google Scholar
Fabian, A. C., 1994, ARA&A, 32, 277Google Scholar
Fabian, A. C., 2012, ARA&A, 50, 455Google Scholar
Heckman, T. M., Baum, S. A., van Breugel, W. J. M. & McCarthy, P., 1989, ApJ, 338, 48Google Scholar
Hlavacek-Larrondo, J., Fabian, A. C., Edge, A. C., Ebeling, H., Sanders, J. S., Hogan, M. T., & Taylor, G. B., 2012, MNRAS, 421, 1360Google Scholar
McNamara, B. R. & Nulsen, P. E. J., 2007, ARA&A, 45, 117Google Scholar
McNamara, B. R. & Nulsen, P. E. J., 2012, ArXiv e-printsGoogle Scholar
O'Dea, K. P., et al. 2010, ApJ, 719, 1619CrossRefGoogle Scholar
Salomé, P. & Combes, F., 2003, A&A, 412, 657Google Scholar
Tremblay, G. 2011, PhD, thesis, RITGoogle Scholar
Tremblay, G. R., O'Dea, C. P., Baum, S. A., et al. 2012, MNRAS, 424, 1042Google Scholar
Tremblay, G. R., O'Dea, C. P., Baum, S. A., et al. 2012, MNRAS, 424, 1026Google Scholar