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J/A+A/582/A64       W51/e2 and G34.3+0.2 IRAM spectra           (Lykke+, 2015)

Tentative detection of ethylene glycol toward W51/e2 and G34.3+0.2. Lykke J.M., Favre C., Bergin E.A., Jorgensen J.K. <Astron. Astrophys. 582, A64 (2015)> =2015A&A...582A..64L (SIMBAD/NED BibCode)
ADC_Keywords: Associations, stellar ; Spectroscopy Keywords: ISM: molecules - ISM: abundances - ISM: individual objects: W51/e2 - methods: observational - astrochemistry - ISM: individual objects: G34.3+0.2 Abstract: With only a few low- and high-mass star-formation regions studied in detail so far, it is unclear what role the environment plays in complex molecule formation. In this light, a comparison of relative abundances of related species between sources might be useful for explaining any observed differences. We seek to measure the relative abundance between three important complex organic molecules, ethylene glycol ((CH2OH)2), glycolaldehyde (CH2OHCHO) and methyl formate (HCOOCH3), toward high-mass protostars and thereby provide additional constraints on their formation pathways. We use IRAM30 m single-dish observations of the three species toward two high-mass star-forming regions - W51/e2 and G34.3+0.2 - and report a tentative detection of (CH2OH)2 toward both sources. Description: Reduced spectra for two high-mass star forming regions: W51/e2 and G34.3+0.2. The observations were performed with the IRAM 30-m telescope at Pico Veleta, Spain on December 13 and 14, 2012. The EMIR receiver was used in dual band polarisation (E090/E230) in connection with i) the 200kHz Fourier transform spectrometer (FTS) back-end in the frequency ranges 99.70-106.3GHz and 238.2-246.0GHz for the E090 and E230 bands, respectively; ii) the WILMA back-end in the frequency ranges 99.88-103.6GHz and 238.4-242.1GHz for the E090 and E230 bands, respectively. The observations were reduced using The Continuum and Line Analysis Single-dish Software (CLASS). The resulting FTS spectra were smoothed to a spectral resolution of 1.15km/s for the E090 band and 1.22km/s for the E230 band while the WILMA spectra were smoothed to 5.88km/s and 2.49km/s for the E090 and E230 bands, respectively. Additional information about the observations and their reduction can be found in the article. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 18 53 18.54 +01 14 57.9 G34.3+0.2 = GPSR 034.257+0.155 19 23 43.90 +14 30 34.8 W51/e2 = W51 E2 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 143 12 List of spectra sp/* 0 12 Individual fits spectra
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 24 I5 --- Nx Number of pixels along X-axis 26- 48 A23 --- Obs.Date Observation date (YYYY-MM-DDThh:mm:ss.sss) 50- 61 E12.6 Hz bFreq Lower value of frequency interval 63- 74 E12.6 Hz BFreq Upper value of frequency interval 75- 81 I7 Hz dFreq Frequency resolution 83- 84 I2 Kibyte size Size of FITS file 86-114 A29 --- FileName Name of FITS file, in subdirectory sp 116-143 A28 --- Title Title of the FITS file
Acknowledgements: Julie Maria Lykke, juliemarialykke(at)gmail.com
(End) Patricia Vannier [CDS] 27-Aug-2015
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

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