scholarly journals The Hot Interstellar Medium of Normal Elliptical Galaxies. I. AChandraGas Gallery and Comparison of X‐Ray and Optical Morphology

2007 ◽  
Vol 668 (1) ◽  
pp. 150-167 ◽  
Author(s):  
Steven Diehl ◽  
Thomas S. Statler
Keyword(s):  
Interstellar Medium ◽  
Elliptical Galaxies ◽  
X Ray

scholarly journals Abundance ratios in stars vs. hot gas in elliptical galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 281-281
Author(s):  
Antonio Pipino
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Elliptical Galaxies ◽  
Evolution Model ◽  
X Ray ◽  
Galactic Wind ◽  
Hot Gas ◽  
Self Consistent ◽  
Chemical Evolution Model ◽  
Gas Properties

AbstractI present predictions from a chemical evolution model for a self-consistent study of optical (i.e., stellar) and X-ray (i.e., gas) properties of present-day elliptical galaxies. Detailed cooling and heating processes in the interstellar medium are taken into account and allow a reliable modelling of the SN-driven galactic wind. The model simultaneously reproduces the mass-metallicity, colour-magnitude, LX - LB and LX - T relations, and the observed trend of [Mg/Fe] with σ. The "iron discrepancy" can be solved by taking into account the dust presence.

Evolution of the interstellar medium in elliptical galaxies. II - X-ray properties

1991 ◽  
Vol 369 ◽  
pp. 121 ◽  
Author(s):  
L. P. David ◽  
W. Forman ◽  
C. Jones
Keyword(s):  
Interstellar Medium ◽  
Elliptical Galaxies ◽  
X Ray

scholarly journals X-Rays from Elliptical Galaxies

1987 ◽  
Vol 127 ◽  
pp. 155-165
Author(s):  
A.C. Fabian ◽  
P.A. Thomas
Keyword(s):  
Star Formation ◽  
Interstellar Medium ◽  
Mass Loss ◽  
Elliptical Galaxies ◽  
Stellar Mass ◽  
X Rays ◽  
Early Type ◽  
X Ray ◽  
Isolated Galaxies

X-ray observations have shown that early-type galaxies contain a hot interstellar medium. This implies that the galaxies have a) a low supernova rate; b) high total gravitational binding masses and c) continuous star formation. Much of the gas in isolated galaxies is probably due to stellar mass-loss. The details of its behaviour are complex.

scholarly journals Hot gas morpoloy, thermal structure, and the AGN connection in elliptical galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 275-276
Author(s):  
Thomas S. Statler ◽  
Steven Diehl
Keyword(s):  
Interstellar Medium ◽  
Thermal Structure ◽  
Elliptical Galaxies ◽  
Temperature Gradients ◽  
Fundamental Plane ◽  
Nuclear Activity ◽  
X Ray ◽  
Hot Gas ◽  
Gas Properties

AbstractRecent studies of the hot interstellar medium in normal elliptical galaxies have shown that (1) the gas is only approximately hydrostatic; (2) morphological disturbances are corrleated with radio and X-ray signatures of AGN; and (3) temperature gradients in the main bodies of the galaxies are correlated with nuclear activity but not with environment. An X-ray Gas Fundamental Plane (XGFP), unrelated to the stellar fundamental plane, links the global gas properties in a relation whose origin is not yet understood.

scholarly journals The diverse X-ray properties of four truly isolated elliptical galaxies: NGC 2954, NGC 6172, NGC 7052, and NGC 7785

2009 ◽  
Vol 497 (2) ◽  
pp. 359-370 ◽  
Author(s):  
E. Memola ◽  
G. Trinchieri ◽  
A. Wolter ◽  
P. Focardi ◽  
B. Kelm
Keyword(s):  
Elliptical Galaxies ◽  
X Ray

scholarly journals 1/4 Ke V Diffuse Background and the Local Interstellar Medium

1989 ◽  
Vol 120 ◽  
pp. 536-536
Author(s):  
S.L. Snowden
Keyword(s):  
Interstellar Medium ◽  
Filling Factor ◽  
Thermal Emission ◽  
Mean Free Path ◽  
Physical Parameters ◽  
X Rays ◽  
Local Interstellar Medium ◽  
X Ray ◽  
Diffuse Background ◽  
X Ray Background

The 1/4 keV diffuse X-ray background (SXRB) is discussed in relation to the local interstellar medium (LISM). The most likely source for these soft X-rays is thermal emission from a hot diffuse plasma. The existence of a non-zero flux from all directions and the short ISM mean free path of these X-rays (1020HI cm-2), coupled with ISM pressure constraints, imply that the plasma has a local component and that it must, at least locally (nearest hundred parsecs), have a large filling factor. Our understanding of the geometry and physical parameters of the LISM is therefore directly tied to our understanding of the SXRB.

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