TY - JOUR
T1 - Cloud structure and physical conditions in star-forming regions from optical observations. I. Data and component structure
AU - Pan, K.
AU - Federman, S. R.
AU - Cunha, K.
AU - Smith, V. V.
AU - Welty, D. E.
PY - 2004/4
Y1 - 2004/4
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=2442454749&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=2442454749&partnerID=8YFLogxK
U2 - 10.1086/381805
DO - 10.1086/381805
M3 - Article
AN - SCOPUS:2442454749
SN - 0067-0049
VL - 151
SP - 313
EP - 343
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 2
ER -