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)
· arXiv e-print (arXiv:astro-ph/0312095)
· On-line Data
· References in the article
· Citations to the Article (30) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (32)
· Associated Articles
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Cloud Structure and Physical Conditions in Star-forming Regions from Optical Observations. I. Data and Component Structure
Authors:
Pan, K.; Federman, S. R.; Cunha, K.; Smith, V. V.; Welty, D. E.
Affiliation:
AA(Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606; Guest Observer, McDonald Observatory, University of Texas at Austin.; Visiting Observer, Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by AURA, Inc., under cooperative agreement with the National Science Foundation.; Current address: Department of Physics and Astronomy, Bowling Green State University, Bowling Green, OH 43403.), AB(Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606), AC(Observatorio Nacional-MCT, Rua Gal Jose Cristino 77, Rio de Janeiro, 20921-400 RJ Brazil), AD(Department of Physics, University of Texas at El Paso, El Paso, TX 79968; and McDonald Observatory, University of Texas at Austin, Austin, TX 78712), AE(University of Chicago, Astronomy and Astrophysics Center, 5640 South Ellis Avenue, Chicago, IL 60637)
Publication:
The Astrophysical Journal Supplement Series, Volume 151, Issue 2, pp. 313-343. (ApJS Homepage)
Publication Date:
04/2004
Origin:
UCP
ApJ Keywords:
ISM: Clouds, ISM: Molecules, ISM: Structure, Stars: Formation
DOI:
10.1086/381805
Bibliographic Code:
2004ApJS..151..313P

Abstract

We present high-resolution optical spectra (at ~0.6-1.8 km s-1) of interstellar CN, CH, CH+, Ca I, K I, and Ca II absorption toward 29 lines of sight in three star-forming regions, ρ Oph, Cep OB2, and Cep OB3. The observations and data reduction are described. The agreement between earlier measurements of the total equivalent widths and our results is quite good. However, our higher resolution spectra reveal complex structure and closely blended components in most lines of sight. The velocity component structure of each species is obtained by analyzing the spectra of the six species for a given sight line together. The tabulated column densities and Doppler parameters of individual components are determined by using the method of profile fitting. Total column densities along lines of sight are computed by summing results from profile fitting for individual components and are compared with column densities from the apparent optical depth method. A more detailed analysis of these data and their implications will be presented in a companion paper.

Associated Articles

Part 1     Catalog Description     Part  2    

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