Taurus Observations of the Emission-Line Velocity Field of Centaurus A (NGC 5128)

1983 ◽  
pp. 331-334 ◽  
Author(s):  
Keith Taylor ◽  
Paul D. Atherton
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Centaurus A

scholarly journals Taurus Observations of the Emission-Line Velocity Field of Centaurus A (NGC 5128)

1983 ◽  
Vol 100 ◽  
pp. 331-334
Author(s):  
Keith Taylor ◽  
Paul D. Atherton
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Spatial Resolution ◽  
Line Material ◽  
Fabry Perot ◽  
Dark Lane ◽  
Centaurus A

Using TAURUS – an Imaging Fabry Perot system in conjunction with the IPCS on the AAT, we have studied the velocity field of the Ha emission line at a spatial resolution of 1.7″ over the dark lane structure of Centaurus A. The derived velocity field is quite symmetrical and strongly suggests that the emission line material is orbiting the elliptical component, as a warped disc.

scholarly journals Emission Lines: Sign of a New Energy Source?

1982 ◽  
Vol 97 ◽  
pp. 69-70
Author(s):  
David S. De Young
Keyword(s):  
Energy Source ◽  
Interstellar Medium ◽  
Emission Line ◽  
Emission Lines ◽  
Class I ◽  
Radio Sources ◽  
Extended Radio ◽  
New Energy ◽  
Centaurus A

In addition to the occurrence of emission line regions coexistent with extended radio sources which have been discussed at this Symposium, this phenomenon has been observed earlier in 3C277.3 (Miley et al. 1981) and in Centaurus A (Graham and Price 1981). This gas has been detected only in the Fanaroff and Riley “Class I” radio sources. Data concerning this class of object suggest that outflow from the nucleus is proceeding at transonic or subsonic speeds and this correlation has led to the suggestion (De Young 1981) that the origin of the emission line gas arises from entrainment of the interstellar medium into the ejected material.

scholarly journals Observational Constraints on the Internal Velocity Field of Quasar Emission‐Line Clouds

2000 ◽  
Vol 542 (2) ◽  
pp. 644-654 ◽  
Author(s):  
Mark Bottorff ◽  
Gary Ferland ◽  
Jack Baldwin ◽  
Kirk Korista
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Observational Constraints ◽  
Internal Velocity

What are the emission line filaments along the radio axis of Centaurus A?

2005 ◽  
pp. 87-91
Author(s):  
R. Morganti ◽  
C. N. Tadhunter ◽  
R. A. E. Fosbury ◽  
D. Malin
Keyword(s):  
Emission Line ◽  
Centaurus A

scholarly journals γ2 Velorum, photon loss and the velocity field

1999 ◽  
Vol 193 ◽  
pp. 229-230
Author(s):  
Orsola De Marco ◽  
Werner Schmutz ◽  
Alex de Koter
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Loss Model ◽  
Ionization Structure ◽  
Classical Models ◽  
Photon Loss

The interception of 0.01% of photons (termed photon loss) from the He II Lyα line by Fe VI and Ca V line-opacity can alter substantially the ionization structure of the wind. This is shown to increase the stellar luminosity and hence the wind driving efficiency. Our classical models for WR11 (the WR component in the γ2 Vel binary) underestimate the stellar luminosity as compared to the luminosity derived from the mass-luminosity relation. Here we present a model for WR11 where photon-loss is included. This model succeeds in that it has a higher luminosity for the same spectral appearance and V brightness. Line-blanketing has not yet been added, so that the force-factors and the velocity-law cannot yet be calculated. However, a hydro-dynamical velocity-law derived from a photon-loss model of a WN5 star improves considerably the fit to the narrow He II λ4686 emission line over the use of a β-law.

Emission line velocity field in the central region of M82

1986 ◽  
Vol 119 (1) ◽  
pp. 181-184
Author(s):  
Minoru Sasaki ◽  
Mamoru Saito
Keyword(s):  
Velocity Field ◽  
Emission Line ◽  
Central Region

scholarly journals High-Velocity Outflow in the Extended Emission-Line Region of the Seyfert Galaxy NGC 7319

1997 ◽  
Vol 159 ◽  
pp. 357-358
Author(s):  
Kentaro Aoki
Keyword(s):  
Velocity Field ◽  
Compact Group ◽  
Emission Line ◽  
High Velocity ◽  
Seyfert Galaxy ◽  
Line Region ◽  
Systemic Velocity ◽  
Extended Emission

NGC 7319 is a member of the compact group of galaxies known as Stephan’s Quintet. The systemic velocity 6740 km s−1 gives a distance of 90Mpc (H0= 75 kms−1 Mpc−1) for NGC 7319. This galaxy has a tail and/or ring which suggests interaction with a neighboring pair of galaxies, NGC 7318A and B (e.g., Arp 1973). Durret & Warrin (1990) and Durret (1994) performed optical long-slit spectroscopy and found an extended emission-line region (EELR) in NGC 7319. They detected highly excited gas over along PA = 61° and 10″ along PA – 151°. Apart from these works, there have not been any studies on the velocity field and excitation of the gas in the EELR of NGC 7319. More details were published by Aoki et al. (1996).

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