The hot stellar component in elliptical galaxies and spiral bulges. I - The far-ultraviolet spectrum of the bulge of M31

1993 ◽  
Vol 408 ◽  
pp. 92 ◽  
Author(s):  
Henry C. Ferguson ◽  
Arthur F. Davidsen
Keyword(s):  
Elliptical Galaxies ◽  
Ultraviolet Spectrum ◽  
Stellar Component ◽  
Far Ultraviolet

scholarly journals The Far‐Ultraviolet Spectrum of the Io Plasma Torus

2004 ◽  
Vol 601 (1) ◽  
pp. 583-591 ◽  
Author(s):  
Paul D. Feldman ◽  
Darrell F. Strobel ◽  
H. Warren Moos ◽  
Harold A. Weaver
Keyword(s):  
Ultraviolet Spectrum ◽  
Plasma Torus ◽  
Far Ultraviolet ◽  
Io Plasma Torus

scholarly journals The Dark Halo – Spheroid Conspiracy

2012 ◽  
Vol 8 (S295) ◽  
pp. 208-208
Author(s):  
Rhea-Silvia Remus ◽  
Andreas Burkert ◽  
Klaus Dolag ◽  
Peter H. Johansson ◽  
Thorsten Naab ◽  
...  
Keyword(s):  
Elliptical Galaxies ◽  
Total Density ◽  
Dark Halo ◽  
Coma Cluster ◽  
Density Profiles ◽  
Stellar Component ◽  
Strong Lensing ◽  
The Galaxy ◽  
Good Agreement

AbstractObservational results from strong lensing and dynamical modeling indicate that the total density profiles of early-type galaxies are close to isothermal, i.e. ρtot ∝ rγ with γ ≈ −2. To understand the origin of this universal slope we study a set of simulated spheroids formed in cosmological hydrodynamical zoom-in simulations (see Oser et al. 2010 for more details). We find that the total stellar plus dark matter density profiles of all our simulations on average can be described by a power law with a slope of γ ≈ −2.1, with a tendency towards steeper slopes for more compact, lower mass ellipticals, while the total intrinsic velocity dispersion is flat for all simulations, independent of the values of γ. Our results are in good agreement with observations of Coma cluster ellipticals (Thomas et al. 2007) and results from strong lensing (Sonnenfeld et al. 2012). We find that for z ≳ 2 the majority of the stellar build-up occurs through in-situ star formation, i.e. the gas falls to the center of the galaxy and forms stars, causing the galaxy to be more compact and thus the stellar component to be more dominant. As a result, the total density slopes at z ≈ 2 are generally steeper (around γ ≈ −3). Between z = 2 and z = 0 galaxies grow mostly through dry merging, with each merging event shifting the slope more towards γ ≈ −2. We conclude from our simulations that the steepness of the slope of present day galaxies is a signature of the importance of mostly dry mergers in the formation of an elliptical, and suggest that all elliptical galaxies will with time end up in a configuration with a density slope of γ ≈ −2. For a more detailed analysis with a larger sample of simulations see Remus et al. (2013).

Hopkins ultraviolet telescope observations of the far-ultraviolet spectrum of NGC 4151

1992 ◽  
Vol 392 ◽  
pp. 485 ◽  
Author(s):  
G. A. Kriss ◽  
A. F. Davidsen ◽  
William P. Blair ◽  
C. W. Bowers ◽  
W. V. Dixon ◽  
...  
Keyword(s):  
Ultraviolet Spectrum ◽  
Ngc 4151 ◽  
Far Ultraviolet

Far‐Ultraviolet Spectrum of Ethylene and Ethylene‐d4

1967 ◽  
Vol 47 (4) ◽  
pp. 1517-1524 ◽  
Author(s):  
Ruth McDiarmid ◽  
Elliot Charney
Keyword(s):  
Ultraviolet Spectrum ◽  
Far Ultraviolet

scholarly journals The Far‐Ultraviolet Spectrum of Z Camelopardalis in Quiescence and Standstill

2005 ◽  
Vol 623 (1) ◽  
pp. 425-441 ◽  
Author(s):  
Louise E. Hartley ◽  
Knox S. Long ◽  
Cynthia S. Froning ◽  
Janet E. Drew
Keyword(s):  
Ultraviolet Spectrum ◽  
Far Ultraviolet

scholarly journals Far-Ultraviolet Spectrum of Fairall 9 with the Hopkins Ultraviolet Telescope

1995 ◽  
Vol 454 (1) ◽  
Author(s):  
Wei Zheng ◽  
Gerard A. Kriss ◽  
Arthur F. Davidsen ◽  
Jeffrey W. Kruk
Keyword(s):  
Ultraviolet Spectrum ◽  
Far Ultraviolet
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