Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Printable Article (PDF/Postscript)
· Scanned Article (GIF)
· SIMBAD Objects (3)
· NED Objects (3)
· Reads History
·
· Translate This Page
Title:
CO In A Dynamically Spectacular Ringlike Luminous IR Merger
Authors:
Gao, Yu; Solomon, P. M.; Radford, S. J. E.; Downes, D.
Affiliation:
AA(SUNY, Stony Brook), AB(SUNY, Stony Brook), AC(Institut de Radio Astronomie Millimétrique, France), AD(Institut de Radio Astronomie Millimétrique, France)
Publication:
American Astronomical Society, 183rd AAS Meeting, #77.05; Bulletin of the American Astronomical Society, Vol. 25, p.1413
Publication Date:
12/1993
Origin:
AAS
Bibliographic Code:
1993BAAS...25.1413G

Abstract

NGC 1144, the eastern component of an interacting galaxy system Arp 118 which has an elliptical companion --- NGC 1143, has a distorted disk and an extended ringlike structure of HII regions. Using the IRAM 30-m telescope, we have detected extremely strong and wide CO emission line (FWZI ~ 1100 \ km s(-1) ) from the nuclei of NGC 1144 which itself is an interacting, infrared-luminous, ring-like Seyfert II. The extended ring structure, ~ 10 \ kpc from the nuclei also shows very strong CO emission. The total molecular mass is MH_2 ~ 4 times 10(10) \ Msun, exceeds that of Arp 220 and is one of the highest in the local universe. About 1 times 10(10) ms molecular gas is contained in the ``ring'' ~ 10 \ kpc from the nuclear region. Although the galaxy has a huge molecular mass, the OB star formation efficiency, indicated by the ratio of LIR/MH_2 ~ 5 , is comparable to the Milky Way and is one of the lowest observed for any interacting IR-luminous galaxy. Arp 118 (in particular NGC 1144) is one of the most fascinating merging systems yet observed. It clearly has huge quantities of molecular gas and may be a merger at an early stage with a strong Extranuclear starburst, but a very low massive star formation efficiency. Our future interferometry of the CO(1-0) line will provide the best opportunity to study the distribution and kinematics of the molecular gas in this spectacular merging/interacting galaxy system.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints