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J/ApJS/177/275           1.3 and 2mm survey of IRC+10216            (He+, 2008)

A spectral line survey in the 2 and 1.3 mm windows toward the carbon-rich envelope of IRC +10216. He J.H., Dinh-V-Trung J.H., Kwok S., Muller H.S.P., Zhang Y., Hasegawa T., Peng T.C., Huang Y.C. <Astrophys. J. Suppl. Ser., 177, 275-325 (2008)> =2008ApJS..177..275H
ADC_Keywords: Radio lines ; Spectra, millimetric/submm Keywords: line: identification - radio lines: ISM - stars: AGB and post-AGB stars: individual (IRC+10216) - submillimeter - surveys Abstract: We present the results of our spectral line surveys in the 1.3 and 2mm windows toward the carbon-rich envelope of IRC+10216. There were 377 lines detected in total, of which 360 lines are assigned to 57 known molecules (including 29 rare isotopomers and two cyclic isomers). Only 17 weak lines remain unidentified. Rotational lines of isotopomers 13CCH and HN13C are detected for the first time in IRC+10216 . The detection of the formaldehyde lines in this star is also confirmed. Possible abundance differences among the three 13C-substituted isotopic isomers of HC3N is reported. Isotopic ratios of C and O are confirmed to be nonsolar while those of S and Si to be nearly solar. Column densities have been estimated for 15 molecular species. Modified spectroscopic parameters have been calculated for NaCN, Na13CN, KCN, and SiC2. Transition frequencies from the present observations were used to improve the spectroscopic parameters of Si13CC, 29SiC2, and 30SiC2. Description: The surveys were carried out using the 2mm receiver of the Arizona Radio Observatory (ARO) 12m Telescope (KP12M) at Kitt Peak (2005 April 26 to 2006 April 29) and the 1.3mm JT receiver of the Heinrich Hertz Submillimeter Telescope (SMT) at Mt. Graham (2005 October 31 to 2007 January 24). Observed frequency ranges are 131.2-160.3GHz for the 2mm survey, 219.5-245.5 and 251.5-267.5GHz for the 1.3mm survey. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 09 47 57.4 +13 16 44 IRC+10216 = NAME PEANUT NEBULA ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 113 409 Line parameters of all detected lines in our survey
See also: J/A+AS/142/181 : 2mm molecular line survey of IRC+10 216 (Cernicharo+, 2000) Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 10 A10 ---- Species Species name 12- 45 A34 ---- Trans Transition 47- 55 F9.2 MHz Freq ? Observed line frequency 57- 60 F4.2 MHz e_Freq ? Uncertainty in Freq 62- 70 F9.2 MHz Freq0 ? Line frequency from CDMS/JPL catalogs (1) 72 A1 ---- n_Freq0 [abd] Note on Freq0 (2) 74- 79 F6.2 K.km/s Iint ? Integrated line intensity 81 A1 ---- n_Iint [*] Note on Iint (3) 83- 86 F4.2 K.km/s e_Iint ? Uncertainty in Iint 88- 92 I5 mK Tlc ? Fitted main beam temperature at line center 94- 96 I3 mK e_Tlc ? Uncertainty in Tlc 98-102 F5.2 km/s Vexp ? Fitted outflow velocity 104-108 F5.2 km/s e_Vexp ? Uncertainty in Vexp 110-113 A4 ---- Blend Notes on line blending (4)
Note (1): Line identification was performed by using the Cologne Database for Molecular Spectroscopy (CDMS; see Muller et al., 2001A&A...370L..49M, 2005JMoSt.742..215M) and the Molecular Spectroscopy database of Jet Propulsion Laboratory (JPL; see Pickett et al., 1998JQSRT..60..883P). Note (2): Notes on line frequency as follows: a = average frequency of hyperfine components; b = same as a, but the hyperfine of components of neighbouring fine structure lines blended together, so that the fine structure lines are also partially blended. (for MgNC); d = unresolved lambda doublet (for SiC). Note (3): Note on Iint: * = Integrated line intensity derived from SHELL fitting. Note (4): Notes on line blending as follows: s = single lines; a = lines fitted using fixed line frequency and line width of 14.5km/s; b = lines too narrow; c = differentiable blended lines of the same species; d = undifferentiable blended lines of different species; e = differentiable blended lines of the same species; (hyperfine or lambda doublet or weak asymmetric transitions); f = undifferentiable blended lines of different species.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 17-Sep-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

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