scholarly journals The Structure of the Radio Nucleus of M81

1984 ◽  
Vol 110 ◽  
pp. 259-260
Author(s):  
P. C. Crane ◽  
R. M. Price
Keyword(s):  
Emission Line ◽  
Spiral Galaxy ◽  
Linear Dimension ◽  
Linear Dimensions ◽  
Vlbi Observations ◽  
Line Region ◽  
Seyfert Type ◽  
Narrow Emission

New observations of the radio nucleus of the nearby bright spiral galaxy M81 (NGC 3031) show that the structure of the nucleus is considerably more complex than previously thought. The radio nucleus has a slightly inverted, variable spectrum (de Bruyn et al. 1976; Crane, Guffrida, and Carlson 1976). The variability and VLBI observations (Kellermann et al. 1976; Jones, Sramek, and Terzian 1981) both indicate a linear dimension of ~1500 AU. The recent VLBI observations of Bartel et al. (1982) determined that nearly 100% of the emission originates in an elongated region with linear dimensions of 1000–4000 AU. Peimbert and Torres-Peimbert (1981) have classified the optical nucleus of M81 as Seyfert type 1.5 (the weakest known) with the narrow-emission-line region extending over ~5″ (Münch 1959).

The extended narrow emission-line region of NGC 7469 revisited

1986 ◽  
Vol 91 ◽  
pp. 1026 ◽  
Author(s):  
M. M. de Robertis ◽  
R. W. Pogge
Keyword(s):  
Emission Line ◽  
Line Region ◽  
Ngc 7469 ◽  
Narrow Emission

Infrared Spectroscopy of NGC 4151:Infrared Space ObservatoryObservations and Narrow Emission Line Region Line Profiles

1999 ◽  
Vol 512 (1) ◽  
pp. 197-203 ◽  
Author(s):  
E. Sturm ◽  
T. Alexander ◽  
D. Lutz ◽  
A. Sternberg ◽  
H. Netzer ◽  
...  
Keyword(s):  
Infrared Spectroscopy ◽  
Emission Line ◽  
Line Profiles ◽  
Ngc 4151 ◽  
Line Region ◽  
Narrow Emission ◽  
Region Line

scholarly journals Substructures in the Narrow-Line Region of AGN

1989 ◽  
Vol 134 ◽  
pp. 312-313
Author(s):  
Sylvain Veilleux
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Seyfert Galaxies ◽  
Narrow Line ◽  
Line Profiles ◽  
Preliminary Results ◽  
Line Region ◽  
Narrow Line Region ◽  
Narrow Emission ◽  
Resolution Study

The preliminary results of a high-resolution study of narrow emission-line profiles in bright Seyfert galaxies are reported. Profile substructures such as secondary peaks and shoulders are observed in nearly all the objects. The results of profile comparisons in Mrk 359, Mrk 533, and Mrk 1066 are briefly discussed.

scholarly journals The Interaction of Quasar Winds and the Circumquasar Environment

1983 ◽  
Vol 6 ◽  
pp. 593-601
Author(s):  
J. E. Dyson
Keyword(s):  
Emission Line ◽  
High Speed ◽  
Stellar Winds ◽  
Lower Velocity ◽  
Interstellar Clouds ◽  
Line Region ◽  
Cool Gas ◽  
Set Up ◽  
The Impact ◽  
Narrow Emission

High speed winds from quasars interact with the gas and stars in a surrounding galaxy and produce a variety of effects. The winds sweep up the general interstellar matter into fast moving shells of cool gas which can produce lower velocity (≲, 0.01c) sharp absorption line systems. The impact of the wind on dense interstellar clouds may contribute to the narrow emission line region. Finally, supernovae or stellar winds near the QSO set up shock waves in the outflow. Shocked QSO wind material is responsible for the broad emission line material.

scholarly journals Spectroscopy of CN Orionis

1987 ◽  
Vol 93 ◽  
pp. 501-505
Author(s):  
K.H. Mantel ◽  
H. Barwig ◽  
R. Haefner ◽  
R. Schoembs
Keyword(s):  
Emission Line ◽  
Velocity Curve ◽  
Minimum Phase ◽  
Radial Velocity Curve ◽  
System Parameters ◽  
The Core ◽  
Line Region ◽  
Approximate System ◽  
Balmer Decrement ◽  
Narrow Emission

AbstractTwo outbursts and a minimum phase of the dwarf nova CN Orionis have been observed spectroscopically. One outburst was covered almost completely. The outburst spectra show periodic variations of the absorption lines which are interpreted with the formation of an elliptic disc during outburst stage. During decline from outburst a narrow emission line appears in the core of the broad H« absorption line. The balmer decrement in the outburst phase is much steeper than in the minimum phase. This implies that during the outburst the emission line region is located more outward in the disk. The semi amplitude of the radial velocity curve was determined to Kl = 152 km/s ± 10 km/s. Using the photometric orbital period and an assumption about the inclination angle the approximate system parameters could be derived.

scholarly journals Exploring the link between C IV outflow kinematics and sublimation-temperature dust in quasars

2020 ◽  
Author(s):  
Matthew J Temple ◽  
Manda Banerji ◽  
Paul C Hewett ◽  
Amy L Rankine ◽  
Gordon T Richards
Keyword(s):  
Emission Line ◽  
High Frequency ◽  
Infrared Emission ◽  
Black Hole Mass ◽  
Sublimation Temperature ◽  
Continuum Source ◽  
Broad Emission ◽  
Line Region ◽  
Using Data

Abstract Using data from SDSS, UKIDSS and WISE, we investigate the properties of the high-frequency cutoff to the infrared emission in ≃5000 carefully selected luminous (Lbol ∼ 1047) type 1 quasars. The strength of ≃2 μm emission, corresponding to emission from the hottest ($T>1200\rm \, K$) dust in the sublimation zone surrounding the central continuum source, is observed to correlate with the blueshift of the C iv λ1550 emission line. We therefore find that objects with stronger signatures of nuclear outflows tend to have a larger covering fraction of sublimation-temperature dust. When controlling for the observed outflow strength, the hot dust covering fraction does not vary significantly across our sample as a function of luminosity, black hole mass or Eddington fraction. The correlation between the hot dust and the C iv line blueshifts, together with the lack of correlation between the hot dust and other parameters, therefore provides evidence of a link between the properties of the broad emission line region and the infrared-emitting dusty regions in quasars.

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