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AGN feedback and star formation in ETGs: negative and positive feedback

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Luca Ciotti ,
Jeremiah P. Ostriker ,
Andrea Negri ,
Silvia Pellegrini ,
Silvia Posacki  and
Greg Novak
Luca Ciotti
Affiliation:
Dept. of Physics and Astronomy, University of Bologna, via Ranzani 1, I-40127 Bologna, Italy, email: luca.ciotti@unibo.it
Jeremiah P. Ostriker
Affiliation:
Dept. of Astrophysical Sciences, Princeton University, NJ, USA Dept. of Astronomy and Astrophysics, Columbia University, NY, USA
Andrea Negri
Affiliation:
Dept. of Physics and Astronomy, University of Bologna, via Ranzani 1, I-40127 Bologna, Italy, email: luca.ciotti@unibo.it Institut d'Astrophysique de Paris, CNRS, UMR 7095 98bis bvd Arago, F-75014 Paris, France
Silvia Pellegrini
Affiliation:
Dept. of Physics and Astronomy, University of Bologna, via Ranzani 1, I-40127 Bologna, Italy, email: luca.ciotti@unibo.it
Silvia Posacki
Affiliation:
Dept. of Physics and Astronomy, University of Bologna, via Ranzani 1, I-40127 Bologna, Italy, email: luca.ciotti@unibo.it
Greg Novak
Affiliation:
Observatoire de Paris, LERMA, CNRS, 61 Av de l'Observatoire, F-75014 Paris, France
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Abstract

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AGN feedback from supermassive black holes (SMBHs) at the center of early type galaxies is commonly invoked as the explanation for the quenching of star formation in these systems. The situation is complicated by the significant amount of mass injected in the galaxy by the evolving stellar population over cosmological times. In absence of feedback, this mass would lead to unobserved galactic cooling flows, and to SMBHs two orders of magnitude more massive than observed. By using high-resolution 2D hydrodynamical simulations with radiative transport and star formation in state-of-the-art galaxy models, we show how the intermittent AGN feedback is highly structured on spatial and temporal scales, and how its effects are not only negative (shutting down the recurrent cooling episodes of the ISM), but also positive, inducing star formation in the inner regions of the host galaxy.

Keywords

ISM: kinematics and dynamicsgalaxies: activegalaxies: cooling flowsgalaxies: elliptical and lenticularcDgalaxies: starburstgalaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , pp. 224 - 227
Copyright
Copyright © International Astronomical Union 2016 

References

Ciotti, L., D'Ercole, A., Pellegrini, S., & Renzini, A. 1991, ApJ, 376, 380 Google Scholar
Ciotti, L. & Ostriker, J. P. 1997, ApJ, 487, L105 Google Scholar
Ciotti, L. & Ostriker, J. P. 2007, ApJ 665 1038 (CO07) Google Scholar
Ciotti, L. & Ostriker, J. P. 2012, in Kim, D.W. and Pellegrini, S. (eds.), Hot interstellar matter in elliptical galaxies, (Springer, Heidelberg), ASSL, vol. 378, p. 83 Google Scholar
Ciotti, L. & Pellegrini, S. 1996, MNRAS, 279, 240 CrossRefGoogle Scholar
Hensley, B., Ostriker, J. P., & Ciotti, L. 2014, ApJ, 789, 78 Google Scholar
Negri, A., Posacki, S., Pellegrini, S., & Ciotti, L. 2014, MNRAS, 445, 1351 Google Scholar
Negri, A., Pellegrini, S., & Ciotti, L. 2015, MNRAS 451 1212 (N15) Google Scholar
Novak, G., Ostriker, J. P., & Ciotti, L. 2011, ApJ, 737, 26 Google Scholar
Novak, G., Ostriker, J. P., & Ciotti, L. 2012, MNRAS 427 2734 (N12)Google Scholar
Pellegrini, S. 2012, in Kim, D.W. and Pellegrini, S. (eds.), Hot interstellar matter in elliptical galaxies, (Springer, Heidelberg), ASSL, vol. 378, p. 21 CrossRefGoogle Scholar
Posacki, S., Pellegrini, S., & Ciotti, L. 2013, MNRAS, 433, 2259 CrossRefGoogle Scholar