Access to Astronomical Catalogues

← Click to display the menu
J/A+A/504/853      Molecular lines in 5 massive dense cores     (Herpin, 2009)

S-bearing molecules in massive dense cores Herpin F., Marseille M., Wakelam V., Bontemps S., Lis D.C. <Astron. Astrophys. 504, 853 (2009)> =2009A&A...504..853H
ADC_Keywords: Interstellar medium ; Infrared sources ; Line Profiles Keywords: ISM: individual objects: W43MM1, IRAS18264-1152, IRAS05358+3543, IRAS18162-2048 - ISM: abundances - stars: formation - line: profiles Abstract: Two mid-infrared quiet and two brighter massive cores were observed in various transitions (Eup up to 289K) of CS, OCS, H2S, SO, and SO2 and of their 34S isotopologues at mm wavelengths with the IRAM 30m and CSO telescopes. The 1D modeling of the dust continuum is used to derive the density and temperature laws, which were then applied in the RATRAN code to modeling the observed line emission and to deriving the relative abundances of the molecules. All lines are detected, except the highest energy SO2 transition. Infall (up to 2.9km/s) may be detected towards the core W43MM1. We propose an evolutionary sequence of our sources (W43MM1 - IRAS18264-1152 - IRAS05358+3543 - IRAS18162-2048), based on the SED analysis. The analysis of the variations in abundance ratios from source to source reveals that the SO and SO2 relative abundances increase with time, while CS and OCS decrease. Molecular ratios, such as [OCS/H2S], [CS/H2S], [SO/OCS], [SO2/OCS], [CS/SO], and [SO2/SO] may be good indicators of evolution, depending on layers probed by the observed molecular transitions. Observations of molecular emission from warmer layers, so that involving higher upper energy levels must be included. Description: The figure 14-17 show some line profiles (not shown in the paper) from observations with the IRAM-30m and CSO telescopes (all observational parameters can be found in the Table 2 of the paper). The reduced data for all the observed lines are given in the individual fit files, labelled as follows:, where "o" represents the observed source and is "i1" for IRAS05358+3543, "i2" for IRAS18162-2048, "i3" for IRAS18264-1152, and "w" for W43MM1, respectively; "s" is the species (e.g. CS); "l" is the first number (level) of the line transition (e.g. "3" for "3-2"). The Tables 6-9 give all the parameters for the observed line emissions. Table 10 shows the opacities derived from modeling the molecular emission of the sources. Objects: ------------------------------------------------------------------------ RA (2000) DE Designation(s) (Table) ------------------------------------------------------------------------ 18 47 47.0 -01 54 28 W43MM1 = [MSL2003] W43-MM1 (table6.dat) 18 29 14.3 -11 50 26 IRAS18264-1152 = IRAS 18264-1152 (table7.dat) 05 39 10.4 +35 45 19 IRAS05358+3543 = IRAS 05358+3543 (table8.dat) 18 19 11.8 -20 47 35 IRAS18162-2048 = IRAS 18162-2048 (table9.dat) ------------------------------------------------------------------------ File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table6.dat 115 25 Observed line emissions parameters for W43MM1 table7.dat 115 25 Observed line emissions parameters for IRAS18264-1152 table8.dat 115 25 Observed line emissions parameters for IRAS05358+3543 table9.dat 115 25 Observed line emissions parameters for IRAS18162-2048 table10.dat 55 24 Opacities derived from modeling the molecular emission of the sources fits/* 0 78 Individual line profiles
Byte-by-byte Description of file: table6.dat table7.dat table8.dat table9.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Species Species 11- 27 A17 --- Trans Observed line transition 30- 33 F4.2 km/s dV ? Linewidth 35- 38 F4.2 km/s e_dV ? rms uncertainty on dV 40 A1 --- u_dV [?] Uncertainty flag on dV 42- 45 F4.2 K Tmb ? Main beam temperature 46 A1 --- u_Tmb [?] Uncertainty flag on Tmb 48- 50 I3 mK e_Tmb ? rms uncertainty on Tmb 53 A1 --- l_Flux Limit flag on Flux 54- 59 F6.3 Flux ? Integrated flux 61- 64 F4.2 e_Flux ? rms uncertainty on Flux 66 A1 --- ueFlux [?] Uncertainty flag on Flux 69- 73 F5.2 km/s dV3s ? linewidth at 3 sigma 74 A1 --- u_dV3s [?] Uncertainty flag on dV3s 77- 80 F4.2 km/s dV1/2 ? half-power linewidth 81 A1 --- u_dV1/2 [?] Uncertainty flag on dV1/2 82 A1 --- Flag [abcdfg] Flag on profile (1) 88-101 A14 --- Com Comments 103-115 A13 --- FileName Name of the fits file in subdirectory fits
Note (1): Flags as follows: a = self-absorption at dV_source b = line blend with H2CO line from image band c = unidentified line at 34.87km/s (216.716GHz) d = + other line at 29.1km/s (135.78223GHz), Tmb=0.14K, δ=1.1km/s, Tmbδ=0.17 f = detected at 2σ with two peaks at -15.57 and -16.21km/s g = unidentified lines at 216.701026 and 216.71.6GHz (25 and 4km/s)
Byte-by-byte Description of file: table10.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Species Species 11- 27 A17 --- Trans Observed line transition 29- 34 F6.2 --- Opac1 ? Line opacity for source W43MM1 35- 36 A2 --- n_Opac1 [ND] ND for no data 38- 41 F4.2 --- Opac2 Line opacity for source IRAS18264-1152 43- 46 F4.2 --- Opac3 ? Line opacity for source IRAS05358+3543 47- 48 A2 --- n_Opac3 [ND] ND for no data 50- 53 F4.2 --- Opac4 ? Line opacity for source IRAS18162-2048 54- 55 A2 --- n_Opac4 [ND] ND for no data
Acknowledgements: Fabrice Herpin, herpin(at)
(End) Fabrice Herpin [LAB/OASU, France], Patricia Vannier [CDS] 17-Jul-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service