On the Relationship between the Optical Emission‐Line and X‐Ray Luminosities in Seyfert 1 Galaxies

2004 ◽  
Vol 607 (2) ◽  
pp. 794-799 ◽  
Author(s):  
S. B. Kraemer ◽  
I. M. George ◽  
D. M. Crenshaw ◽  
J. R. Gabel
Keyword(s):  
Emission Line ◽  
Optical Emission ◽  
X Ray ◽  
The Relationship

X-ray and optical emission-line filaments in the cooling flow cluster 2A 0335 + 096

1992 ◽  
Vol 397 ◽  
pp. L31 ◽  
Author(s):  
Craig L. Sarazin ◽  
Robert W. O'Connell ◽  
Brian R. McNamara
Keyword(s):  
Emission Line ◽  
Optical Emission ◽  
X Ray ◽  
Cooling Flow

scholarly journals The Relationship Between the Emission-Line Spectra and X-Ray/UV Continuum

1997 ◽  
Vol 159 ◽  
pp. 252-253
Author(s):  
Youjun Lu ◽  
Tinggui Wang
Keyword(s):  
Emission Line ◽  
Inverse Correlation ◽  
Baldwin Effect ◽  
Spectral Parameters ◽  
X Ray ◽  
Physical Conditions ◽  
Broad Emission ◽  
The Baldwin Effect ◽  
The Relationship ◽  
The Continuum

According to photoionization calculations, the broad emission-line (BEL) spectrum depends not only on the physical conditions of line-emitting gas, but also on the spectral shape of incident ionizing continuum, especially from the UV to X-ray. Analysis of emission-line spectra and their correlations with the continuum, therefore, provide a way of probing the anisotropy of ionizing continuum on the BLR scale, which is predicted by current models. Previous works have concentrated on explaining the Baldwin effect, an inverse correlation between equivalent width and continuum luminosity. In this contribution, we present the results of an analysis of 75 AGNs which have well-determined soft X-ray spectral parameters from ROSAT and UV line and continuum measurements.

scholarly journals Stellar X-Ray Sources

1974 ◽  
Vol 60 ◽  
pp. 383-399
Author(s):  
Harvey D. Tananbaum
Keyword(s):  
Black Hole ◽  
Radio Emission ◽  
Optical Emission ◽  
Close Correlation ◽  
X Ray ◽  
Radio Outburst ◽  
The Relationship ◽  
Optical Behavior

Data are presented for Cygnus X-1, Cygnus X-3, and Scorpius X-1 from radio to X-ray wavelengths. The evidence for Cygnus X-1's being a black hole is now quite convincing. New data for Cygnus X-3 show the presence of X-ray activity at the time of the giant radio outburst. The data for Scorpius X-1 show a close correlation between the X-ray and optical behavior, but coverage was not sufficiently complete to fully assess the relationship (if any) between the X-ray and optical emission and the radio emission.

scholarly journals Emission Line Properties of Seyfert 1 Type AGN from RASS

2003 ◽  
Vol 214 ◽  
pp. 273-274
Author(s):  
D. W. Xu ◽  
S. Komossa ◽  
J. Y. Wei ◽  
X. Z. Zheng ◽  
Y. Qian
Keyword(s):  
Correlation Analysis ◽  
Emission Line ◽  
Optical Emission ◽  
Strong Correlations ◽  
X Ray ◽  
Narrow Component ◽  
Broad Component

We present the optical emission line properties of a sample of 155 bright X-ray selected ROSAT Seyfert 1 type AGN. The measured properties are gathered for correlation analysis. The strong correlations between Hβ redshift, flux ratios of Fe II to Hβ broad component and [O III] to Hβ narrow component are found.

scholarly journals X-ray Observations of SNR E0102.2-72.2 in the SMC

1988 ◽  
Vol 101 ◽  
pp. 125-128
Author(s):  
John P. Hughes
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Spectral Data ◽  
Proportional Counter ◽  
High Velocity ◽  
Supernova Remnant ◽  
Optical Emission ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Best Fit

AbstractThe supernova remnant (SNR) E0102.2-72.2 is the brightest in the Small Magellanic Cloud (SMC) at X-ray wavelengths. This object, which is remarkable because of its high velocity (∼4000 km s−1) oxygen-rich optical emission, appears to be similarly remarkable at X-ray wavelengths. The high resolution imager (HRI) data can be quite well described by a thick ring with a radius of ∼19" (6 pc at a distance of 63 kpc). The imaging proportional counter (IPC) X-ray spectral data can be best fit by a single emission line of energy ∼0.9 keV. It seems likely that this is the emission from a plasma of almost pure neon.

scholarly journals Tri-dimensional Spectroscopy of the Seyfert Galaxy NGC 1275: Kinematics and Excitation of the Cooling-Flow Gas

1997 ◽  
Vol 159 ◽  
pp. 353-354
Author(s):  
M. Yoshida ◽  
G. Kosugi ◽  
K. Aoki
Keyword(s):  
Emission Line ◽  
Seyfert Galaxy ◽  
Optical Emission ◽  
Two Dimensional ◽  
X Ray ◽  
Cooling Flow ◽  
Gas Kinematics ◽  
Line Region ◽  
Ngc 1275 ◽  
Perseus Cluster

NGC 1275, the Perseus cluster cD galaxy, is a well-known Seyfert 1 galaxy and also one of the strongest extragalactic radio sources (3C84). Although many studies have been done on the extended optical emission-line region of NGC 1275, which is thought to be associated with the X-ray cooling-flow phenomenon (e.g., Heckman et al. 1989, Ferruit and Pecontal 1994), the excitation mechanism of the emission-line gas and two-dimensional gas kinematics are still unclear. We made tri-dimensional spectroscopy of NGC 1275 in order to reveal two-dimensional kinematics and- the relation between the gas motion and the excitation of the emission lines.

scholarly journals Are LINERs Starbursts or Mini-quasars? A Comparative Study of their Ultraviolet Spectra

1999 ◽  
Vol 194 ◽  
pp. 71-74
Author(s):  
Anuradha Koratkar
Keyword(s):  
Emission Line ◽  
Hubble Space Telescope ◽  
Optical Emission ◽  
Uv Spectra ◽  
High Mass ◽  
X Ray ◽  
Compact Source ◽  
Continuum Source ◽  
Liner Galaxies ◽  
Super Star Clusters

Low Ionization Nuclear Emission Line Regions (LINERs) are found in ˜30% of all bright galaxies. The nuclear luminosities in these objects are such that they can be produced by a number of mechanisms and there have been heated debates on the nature of ionizing sources in LINERs. The variety of ionizing mechanisms suggested are low luminosity AGNs, starbursts, shocks, or any combination of these. We have studied Hubble Space Telescope (HST) ultraviolet (UV) spectra of seven LINERs having compact nuclear UV sources.The picture emerging from this comparison is that the compact source observed in these LINER galaxies, at least in some cases, is a nuclear star cluster rather than a low-luminosity active galactic nucleus (AGN). In these cases, the UV luminosity is driven by tens of thousands of O-type stars, depending on the assumed extinction for these objects. The O-stars could be the high-mass end of a bound stellar population, similar to those seen in super star clusters. Our data do not exclude the possibility that a similar stellar continuum source could dominate in all the LINERs. Alternatively, there may be two types of UV-bright LINERs: those where the UV continuum is produced by a starburst, and those where it is nonstellar.The “clearly-stellar”, weak [O I] emitters, LINERs have relatively weak X-ray emission, and their stellar populations probably provide enough ionizing photons to explain the observed optical emission-line flux. The other LINERs, strong [O I] emitters, have severe ionizing photon deficits, for reasonable extrapolations of their UV spectra beyond the Lyman limit, but have an X-ray/UV power ratio that is higher by two orders of magnitudes than that of the “clearly-stellar” LINERs. A component which emits primarily in the extreme-UV may be the main photoionizing agent in these objects.Recent results show that nuclear-starburst and quasar-like activity are often intermingled. Our results extend this result to the lower luminosities of the LINERs.

scholarly journals On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies

2006 ◽  
Vol 455 (1) ◽  
pp. 173-185 ◽  
Author(s):  
F. Panessa ◽  
L. Bassani ◽  
M. Cappi ◽  
M. Dadina ◽  
X. Barcons ◽  
...  
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Optical Emission ◽  
Seyfert Galaxies ◽  
Black Hole Mass ◽  
X Ray ◽  
Mass Properties

THE RELATIONSHIP AMONG XBLs, RBLs AND FSRQs

2010 ◽  
Vol 19 (06) ◽  
pp. 909-915
Author(s):  
HONG-GUANG WANG ◽  
JUN-HUI FAN ◽  
YONG HUANG ◽  
JING PAN ◽  
JIANG-HE YANG
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Central Black Hole ◽  
Bl Lacertae Objects ◽  
X Ray ◽  
Bolometric Luminosity ◽  
Bl Lacertae ◽  
Spectrum Radio ◽  
The Relationship ◽  
Black Hole Masses

In this work, we revisited the relationship between the subclasses of blazars (X–ray selected BL Lacertae objects (XBLs), radio selected BL Lacertae objects (RBLs), and flat spectrum radio quasars (FSRQs)) based on a sample of blazars. We found that the FSRQs–RBLs–XBLs relationship is clear in their bolometric luminosity, emission line luminosity and the accretion ratio with V FSRQs > V RBLs > V XBLs , where V stands for the three parameters. However, there is no clear difference amongst their central black hole masses. The bolometric luminosity is closely correlated with the emission line luminosity and the accretion ratio.

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