Einstein X-ray observations of QSO's with absorption-line systems

1982 ◽  
Vol 87 ◽  
pp. 845 ◽  
Author(s):  
V. T. Junkkarinen ◽  
A. P. Marscher ◽  
E. M. Burbidge
Keyword(s):  
Absorption Line ◽  
X Ray

Detection of Absorption‐Line Features in the X‐Ray Spectra of the Galactic Superluminal Source GRO J1655–40

1998 ◽  
Vol 500 (2) ◽  
pp. 1069-1069 ◽  
Author(s):  
Y. Ueda ◽  
H. Inoue ◽  
Y. Tanaka ◽  
K. Ebisawa ◽  
F. Nagase ◽  
...  
Keyword(s):  
Absorption Line ◽  
X Ray ◽  
Line Features

scholarly journals A phase-dependent absorption line in the spectrum of the X-ray pulsar RX J0720.4-3125

2004 ◽  
Vol 419 (3) ◽  
pp. 1077-1085 ◽  
Author(s):  
F. Haberl ◽  
V. E. Zavlin ◽  
J. Trümper ◽  
V. Burwitz
Keyword(s):  
Absorption Line ◽  
X Ray ◽  
Dependent Absorption

scholarly journals The Frequency of Intrinsic X-Ray Weakness among Broad Absorption Line Quasars

2018 ◽  
Vol 859 (2) ◽  
pp. 113 ◽  
Author(s):  
Hezhen Liu ◽  
B. Luo ◽  
W. N. Brandt ◽  
S. C. Gallagher ◽  
G. P. Garmire
Keyword(s):  
Absorption Line ◽  
Broad Absorption ◽  
X Ray ◽  
Broad Absorption Line

scholarly journals 9.18. Galactic winds in active galaxies

1998 ◽  
Vol 184 ◽  
pp. 417-418 ◽  
Author(s):  
S. Veilleux ◽  
J. Bland-Hawthorn ◽  
G. Cecil ◽  
P. Shopbell
Keyword(s):  
Absorption Line ◽  
Galaxy Formation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Active Galaxies ◽  
Large Scale Circulation ◽  
X Ray ◽  
Hubble Sequence ◽  
Galactic Winds ◽  
X Ray Background

The effects of large-scale galactic winds in active galaxies may be far-reaching. It has been suggested that the Hubble sequence can be understood in terms of a galaxy's greater ability to sustain winds with increasing bulge-to-disk ratio. The large-scale circulation of gas associated with these galactic winds might help explain the mass-metallicity relation between galaxies and the metallicity-radius relation within galaxies. Galactic winds probably contribute non-negligibly to the cosmic X-ray background and may be involved in the quasar absorption-line phenomenon. The cosmological implications of the wind phenomenon have been widely explored in the context of proto-galaxies and quasars. The extremely energetic galactic winds that were likely associated with galaxy formation almost certainly played a key role in heating and ionizing the intergalactic medium at high redshifts and may have created the seeds for the large-scale structure we see today.

scholarly journals X-ray Spectra of Clusters of Galaxies

1990 ◽  
Vol 115 ◽  
pp. 209-218 ◽  
Author(s):  
Craig L. Sarazin
Keyword(s):  
High Resolution ◽  
Absorption Line ◽  
Physical State ◽  
Thermal Emission ◽  
Clusters Of Galaxies ◽  
X Ray ◽  
Line Measurement ◽  
History Of ◽  
Intracluster Gas ◽  
X Ray Absorption

AbstractX-ray line observations of clusters of galaxies have shown that the X-ray emission in clusters is mainly thermal emission from hot diffuse gas, and that much of this gas has come out of stars, probably having been ejected from galaxies in the cluster. Future high resolution observations should allow us to determine the physical state of the gas. X-ray line measurements and abundance determinations can lead to strong constraints on the origin of the intracluster gas, and on the chemical evolution and history of galaxies. Some of the stronger resonant X-ray lines may be observable as absorption lines against a background quasar. Such X-ray absorption line measurement can be used to directly derive distances to clusters, using a technique similar to (and possibly complementary to) that the well-known method using the Zel’dovich-Syunyaev effect.

scholarly journals Discovery of a cyclotron absorption line in the transient X-ray pulsar XTE J1829−098

2018 ◽  
Vol 482 (1) ◽  
pp. L14-L18 ◽  
Author(s):  
A E Shtykovsky ◽  
A A Lutovinov ◽  
S S Tsygankov ◽  
S V Molkov
Keyword(s):  
Absorption Line ◽  
X Ray ◽  
Cyclotron Absorption

scholarly journals On the absorption of X-ray bright broad absorption line quasars

2008 ◽  
Vol 491 (2) ◽  
pp. 425-434 ◽  
Author(s):  
M. Giustini ◽  
M. Cappi ◽  
C. Vignali
Keyword(s):  
Absorption Line ◽  
Broad Absorption ◽  
X Ray ◽  
Broad Absorption Line

scholarly journals Observations of Highly-Ionized Interstellar Iron

1984 ◽  
Vol 81 ◽  
pp. 189-191
Author(s):  
L.M. Hobbs
Keyword(s):  
Radial Velocity ◽  
Absorption Line ◽  
Equivalent Width ◽  
Column Density ◽  
Light Path ◽  
Interstellar Gas ◽  
X Ray ◽  
X Ray Background ◽  
Multi Phase ◽  
No Absorption

AbstractThe spectra of 24 stars, including 5 at distances d < 200 pc, have been observed in the regions of the coronal [Fe X] λ6375 and [Fe XIV] λ5303 lines at detection limits near an equivalent width of 1 mÅ in the best cases. In general agreement with predictions based on a multi-phase model of the interstellar medium, no absorption which can be attributed to Fe X or Fe XIV ions in hot interstellar gas emitting the soft x-ray background is seen in any of these spectra, except for two. Toward λ Cephei an absorption line near λ6375 is measured with an equivalent width of 8.1 ± 2 mÅ, a width corresponding to 20 ± 5 km s-1 or a temperature T ≤ (0.5 ± 0.25) x 106 °K, and, if it is caused by Fe X ions, a radial velocity of -355 km s-1. On that hypothesis, the hot interstellar gas constitutes at least 63% of the column density of gas along this light path.

scholarly journals Episodic dust formation in the wind of HD 193793

1987 ◽  
Vol 122 ◽  
pp. 453-454
Author(s):  
P.M. Williams ◽  
K.A. Van der Hucht ◽  
D.R. Florkowski ◽  
A.M.T. Pollock ◽  
W.M. Wamsteker
Keyword(s):  
Binary System ◽  
Radio Source ◽  
Absorption Line ◽  
Radial Velocities ◽  
Published Data ◽  
Dust Formation ◽  
Infrared Photometry ◽  
Dust Shell ◽  
X Ray ◽  
Thermal Radio

In 1985 April, the WC7+abs star HD 193793 was observed, using UKIRT, to have brightened significantly in the infrared owing to the formation of a new dust shell. Examination of infrared photometry of this star since 1979 and previously published data indicates that the dust formation occurs at intervals of 7.9 years. Phasing the published radial velocities of the absorption line component with this period confirms that it is a member of an eccentric (e = 0.7−0.8) binary system having periastron passage shortly before dust formation. The X-ray spectrum also changed between 1984 and 1985 in becoming significantly “harder” while the non-thermal radio source disappeared, both changes indicating greater extinction. This suggests a model wherein the source of the non-thermal radio and X-ray emission moves deep into the Wolf-Rayet wind.

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