The Wayback Machine - https://web.archive.org/web/20190203062819/http://adsabs.harvard.edu/abs/1994MNRAS.269..753H
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)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (57) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (2)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Infrared Signatures of the Inner Spiral Arms and Bar
Authors:
Hammersley, P. L.; Garzon, F.; Mahoney, T.; Calbet, X.
Publication:
Monthly Notices of the Royal Astronomical Society, Vol. 269, NO. 3/AUG1, P. 753, 1994 (MNRAS Homepage)
Publication Date:
08/1994
Origin:
KNUDSEN
DOI:
10.1093/mnras/269.3.753
Bibliographic Code:
1994MNRAS.269..753H

Abstract

Star counts from the Two-Micron Galactic Survey are used to determine the nature of peaks for 350> 1> 150 in the Galactic plane in the 2- m surface-brightness maps. Low extinction by itself is demonstrated to be insufficient to explain the peaks. The peak at 1=330 is shown to have a different luminosity function from those at 1=210 and 270, the latter being almost certainly caused by very luminous, massive young stars. By far the most likely explanation is that they are associated with a star formation region at the near end of the bar. A simple model which includes the bar is proposed; this accurately predicts the form of the major features in the 2.2- m surface-brightness maps on the Galactic plane for 400> 1> 100 and - 100>1> 400. As a consequence, we find that the most probable position angle for the bar is 750+ 50 that the semimajor axis of the bar is 3.7-4 kpc, that there are few if any luminous stars in the 3-kpc ring, and that the width of the stellar population of the Scutum arm is 300 pc. Key words: stars: formation - Galaxy: stellar content - Galaxy: structure - infrared: stars.

Printing Options

Send high resolution image to Level 2 Postscript Printer
Send low resolution image to Level 2 Postscript Printer
Send low resolution image to Level 1 Postscript Printer
Get high resolution PDF image
Get low resolution PDF
Send 300 dpi image to PCL Printer
Send 150 dpi image to PCL Printer

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