Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· References in the article
· Citations to the Article (15) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (11)
· NED Objects (2)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Evolution of gas and stars in the merger galaxy NGC 1316 (Fornax A)
Authors:
Mackie, G.; Fabbiano, G.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics), AB(Harvard-Smithsonian Center for Astrophysics)
Publication:
Astronomical Journal, vol. 115, p. 514 (AJ Homepage)
Publication Date:
02/1998
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
STELLAR EVOLUTION, RADIO GALAXIES, ELLIPTICAL GALAXIES, X RAY ASTRONOMY, HUBBLE SPACE TELESCOPE, X RAY IMAGERY
DOI:
10.1086/300203
Bibliographic Code:
1998AJ....115..514M

Abstract

We present optical and archival X-ray data on the disturbed-morphology radio elliptical galaxy NGC 1316 (Fornax A), which displays numerous low surface brightness shells, loops, and tails. An extended emission-line region (EELR) at a projected distance of 35 kpc from the nucleus has been discovered in an approximately 90 kpc x 35 kpc, 3.0 x 10 exp 9 L(B)(solar) tidal tail. The position and extreme size of the EELR suggest that it is related to the merger process. We suggest that the ionization mechanism of the EELR is shock excitation and that the gas is a remnant from the merger progenitor. X-ray emission is detected near two tidal tails. Hot, 5 x 10 exp 6 K, gas is probably the predominant gas component in the tidal-tail interstellar medium. However, based on the current tidal-tail gas mass, a large fraction of the progenitor gas may already reside in the nucleus of NGC 1316. The numerous and varied tidal-tail system suggests that a disk-disk or disk-E merger could have taken place 1 Gyr ago, while a low-mass, gas-rich galaxy would have started to merge 0.5 Gyr ago.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints