Hot Gas Flows on Global and Nuclear Galactic Scales

Pellegrini, Silvia

doi:10.1007/978-1-4614-0580-1_2

Silvia Pellegrini³

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 378))

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Abstract

Since its discovery as an X-ray source with the EinsteinObservatory, the hot X-ray emitting interstellar medium of early-type galaxies has been studied intensively, taking advantage of observations of improving quality performed by the subsequent X-ray satellites ROSAT, ASCA, Chandraand XMM − Newton, and comparing the observational results with extensive modeling by means of numerical simulations. The hot medium originates from the ejecta produced by the normal stellar evolution, and during the galaxy lifetime it can be accumulated or expelled from the galaxy potential well. The main features of the hot gas evolution are outlined here, focussing on the mass and energy input rates, the relationship between the hot gas flow and the main properties characterizing its host galaxy, the flow behavior on the nuclear and global galactic scales, and the sensitivity of the flow to major galaxy properties as the shape of the mass distribution and the mean rotation velocity of the stars.

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Notes

1.
The stellar mass M _∗changes very little at late epochs, for example by < 1% for a variation of ± 2 Gyr at an age of 12 Gyr.
2.
An expression equal to that in (2.8) can be written for L _grav ⁺, just replacing Γ ⁻with a function \({\Gamma }^{+}(\mathcal{R},\beta )\); the latter has the same trend as Γ ⁻to increase for increasing \(\mathcal{R}\)and decreasing β; for reasonable galaxy mass models, \({\Gamma }^{+} \sim2{\Gamma }^{-}\)(see Pellegrini 2011).
3.
In order to account for all the heating sources, one should add to the denominator of (2.9) also L _σ, that has been neglected for simplicity, since typically \({L}_{\sigma } << {L}_{SN}\), as written below (2.5).
4.
In the notation used here and in Sect. 2.2.3, Πis twice the energy due to random motions.
5.
For a totally velocity dispersion supported galaxy, \({L}_{\sigma }\)accounts for the whole energy input to the gas from the stellar motions, that is significantly lower than L _SN(Sect. 2.2.3, below (2.5)).
6.
The inner light profiles of central cluster galaxies are for the vast majority of core type, with cusp profiles only in 10% of the cases (Laine et al. 2003).

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Acknowledgements

I acknowledge support from the Italian Ministery of Education, University and Research (MIUR) through the Funding Program PRIN 2008.

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Department of Astronomy, University of Bologna, via Ranzani 1, 40127, Bologna, Italy
Silvia Pellegrini

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Harvard Smithsonian Center for Astrophys, Garden Street 60, Cambridge, 02138, Massachusetts, USA
Dong-Woo Kim
, Università di Bologna, Dipartimento di Astronomia, Via Ranzani 1, Bologna, 40127, Italy
Silvia Pellegrini

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Pellegrini, S. (2012). Hot Gas Flows on Global and Nuclear Galactic Scales. In: Kim, DW., Pellegrini, S. (eds) Hot Interstellar Matter in Elliptical Galaxies. Astrophysics and Space Science Library, vol 378. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-0580-1_2

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DOI: https://doi.org/10.1007/978-1-4614-0580-1_2
Published: 09 August 2011
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