The Ultraviolet Spectra of Old Stellar Populations

1996 ◽  
pp. 367-367
Author(s):  
Ben Dorman ◽  
Robert W. O’Connell
Keyword(s):  
Stellar Populations ◽  
Ultraviolet Spectra

Infrared and ultraviolet spectra of 3-fluorobenzoylchloride

1976 ◽  
Vol 73 ◽  
pp. 902-904
Author(s):  
G. N. R. Tripathi ◽  
V. M. Pandey
Keyword(s):  
Ultraviolet Spectra

Stellar Populations in the Host Galaxies of Markarian 1014, IRAS 07598+6508, and Markarian 231

2000 ◽  
Vol 120 (4) ◽  
pp. 1750-1763 ◽  
Author(s):  
Gabriela Canalizo ◽  
Alan Stockton
Keyword(s):  
Stellar Populations ◽  
Host Galaxies

The Stellar Populations of NGC 3109: Another Dwarf Irregular Galaxy with a Population II Stellar Halo

1999 ◽  
Vol 117 (2) ◽  
pp. 881-893 ◽  
Author(s):  
Dante Minniti ◽  
Albert A. Zijlstra, ◽  
M. Victoria Alonso
Keyword(s):  
Stellar Populations ◽  
Irregular Galaxy ◽  
Stellar Halo

scholarly journals Infrared Dust Bubbles: Probing the Detailed Structure and Young Massive Stellar Populations of Galactic HiiRegions

2008 ◽  
Vol 681 (2) ◽  
pp. 1341-1355 ◽  
Author(s):  
C. Watson ◽  
M. S. Povich ◽  
E. B. Churchwell ◽  
B. L. Babler ◽  
G. Chunev ◽  
...  
Keyword(s):  
Stellar Populations ◽  
Detailed Structure

scholarly journals A method for recovering the star formation history of resolved stellar populations

2006 ◽  
Vol 2 (S241) ◽  
Author(s):  
M. Cignoni ◽  
S. Degl'Innocenti ◽  
P. G. Prada Moroni ◽  
S. N. Shore
Keyword(s):  
Star Formation ◽  
Stellar Populations ◽  
Star Formation History ◽  
Formation History ◽  
History Of

scholarly journals The Metallicity Distribution of Late Type Dwarfs

1998 ◽  
Vol 11 (1) ◽  
pp. 571-571
Author(s):  
M. Haywood ◽  
J. Palasi ◽  
A. Gómez ◽  
L. Meillon Dasgal
Keyword(s):  
Star Formation Rate ◽  
Formation Rate ◽  
Angular Separation ◽  
Stellar Populations ◽  
Late Type ◽  
Limited Sample ◽  
Hipparcos Catalogue ◽  
Galactic Stellar Populations ◽  
Metallicity Distribution ◽  
Hr Diagram

The Hipparcos catalogue provides an accurate and extensive sampling of the solar neighbourhood HR diagram. The morphology of this diagram depends on selection criteria of the catalogue such as the limiting magnitude, angular separation and on the characteristics of the stellar populations near the sun (space density, metallicity, star formation rate, etc). Since the Hipparcos data are so accurate, one needs to model precisely the different selection bias and, at the same time, parametrize models of the galactic stellar populations with sufficient flexibility that as much information as possible can be grasped from the catalogue. Comparisons between our model and the Hipparcos catalogue will be presented elsewhere. Since the quantity of information contained in the Hipparcoscatalogue is so important, models ought to be complex, and external contraints, obtained prior to any general comparison with the model, are welcome. A major factor that influences the distribution of the stars in the HR diagram is the metallicity. For the late type stars, the metallicity distribution can be best studied by re-analysing a volume-limited sample of stars from the catalogue.

scholarly journals The weak imprint of environment on the stellar populations of galaxies

2020 ◽  
Vol 500 (4) ◽  
pp. 4469-4490 ◽  
Author(s):  
James Trussler ◽  
Roberto Maiolino ◽  
Claudia Maraston ◽  
Yingjie Peng ◽  
Daniel Thomas ◽  
...  
Keyword(s):  
Environmental Effects ◽  
Unique Feature ◽  
Stellar Populations ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Star Forming ◽  
Sky Survey ◽  
Satellite Galaxies ◽  
Projected Distance ◽  
Environmental Dependence

ABSTRACT We investigate the environmental dependence of the stellar populations of galaxies in Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Echoing earlier works, we find that satellites are both more metal-rich (<0.1 dex) and older (<2 Gyr) than centrals of the same stellar mass. However, after separating star-forming, green valley, and passive galaxies, we find that the true environmental dependence of both stellar metallicity (<0.03 dex) and age (<0.5 Gyr) is in fact much weaker. We show that the strong environmental effects found when galaxies are not differentiated result from a combination of selection effects brought about by the environmental dependence of the quenched fraction of galaxies, and thus we strongly advocate for the separation of star-forming, green valley, and passive galaxies when the environmental dependence of galaxy properties are investigated. We also study further environmental trends separately for both central and satellite galaxies. We find that star-forming galaxies show no environmental effects, neither for centrals nor for satellites. In contrast, the stellar metallicities of passive and green valley satellites increase weakly (<0.05 and <0.08 dex, respectively) with increasing halo mass, increasing local overdensity and decreasing projected distance from their central; this effect is interpreted in terms of moderate environmental starvation (‘strangulation’) contributing to the quenching of satellite galaxies. Finally, we find a unique feature in the stellar mass–stellar metallicity relation for passive centrals, where galaxies in more massive haloes have larger stellar mass (∼0.1 dex) at constant stellar metallicity; this effect is interpreted in terms of dry merging of passive central galaxies and/or progenitor bias.

scholarly journals Variable, Optically Thick, Hot Plasma Observed in Interacting Binaries

1984 ◽  
Vol 80 ◽  
pp. 281-286
Author(s):  
Y. Kondo ◽  
G. E. McCluskey ◽  
S. B. Parsons
Keyword(s):  
Binary Systems ◽  
Ultraviolet Spectra ◽  
Hot Plasma ◽  
International Ultraviolet Explorer

AbstractWe report recent International Ultraviolet Explorer (IUE) observations of two interacting binaries, R Arae and HD 207739. The ultraviolet spectra indicate the presence of optically-thick, variable hot plasma in those binary systems. These two binaries may belong to a class of binaries that are currently undergoing a rarely observed and probably short-lived phase in their evolution. Their properties are compared with those of two other interacting binaries, U Cephei and ß Lyrae.

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