J/ApJS/190/348    1mm spectral survey of IRC+10216 & VY CMa   (Tenenbaum+, 2010)

The arizona radio observatory 1 mm spectral survey of IRC +10216 and VY Canis Majoris (215-285 GHz). Tenenbaum E.D., Dodd J.L., Milam S.N., Woolf N.J., Ziurys L.M. <Astrophys. J. Suppl. Ser., 190, 348-417 (2010)> =2010ApJS..190..348T 2010ApJS..190..348T
ADC_Keywords: Radio lines ; Line Profiles ; Spectra, millimetric/submm ; Stars, supergiant Keywords: astrochemistry - circumstellar matter - stars: AGB and post-AGB - stars: individual (IRC +10216, VY CMa) - supergiants Abstract: A low noise (1σrms∼3mK) 1mm spectral survey (214.5-285.5GHz) of the oxygen-rich supergiant VY Canis Majoris and the carbon-rich asymptotic giant branch star IRC +10216 has been conducted using the Arizona Radio Observatory's 10m Submillimeter Telescope. Here the complete data set is presented. This study, carried out with a new ALMA-type receiver, marks the first continuous band scan of an O-rich circumstellar envelope, and the most sensitive survey to date of IRC+10216. In VY CMa, 130 distinct molecular lines were detected, 14 of which cannot be identified; in IRC +10216, 717 lines were observed, with 126 features remaining unidentified. In the 1mm bands of VY CMa and IRC +10216, emission is present from 18 and 32 different chemical compounds, respectively, with 10 species common to both sources. Many narrow emission lines were observed in both circumstellar shells, arising from vibrationally excited molecules and from refractory-containing species. Line profiles in VY CMa also exhibit a variety of different shapes, caused by the complex, asymmetric outflow of this object. Description: The measurements were conducted during the period 2007 February to 2009 December using the ARO's 10m SMT on Mt. Graham. Objects: -------------------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------------------- 07 22 58.3 -25 46 03 VY Canis Majoris = V* VY CMa 09 47 57.4 +13 16 44 IRC +10216 = V* CW Leo -------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 220 717 Parameters for emission lines in IRC +10216 table2.dat 140 192 Parameters for emission lines in VY CMa -------------------------------------------------------------------------------- See also: J/ApJS/177/275 : 1.3 and 2mm survey of IRC+10216 (He+, 2008) J/A+A/330/676 : IRC+10216 Silicon and sulfur chemistry (Willacy+ 1998) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 F8.1 MHz Freq.0 Rest frequency (νrest) 10- 66 A57 --- Molecule Molecule identification 68-159 A92 --- Trans Transition identification 161 A1 --- u_TA* [~] Approximate flag on T* 162-167 F6.3 K TA* Center antenna brightness temperature 169-174 F6.4 K e_TA* ? The 1σ uncertainty in TA* (1) 177-180 F4.1 km/s Vexp ? Half-Width at Zero-Power, also referred to as expansion velocity 182-185 F4.1 km/s e_Vexp ? Uncertainty in Vexp 187-193 F7.3 K.km/s intTA* ? Integrated brightness temperature 195-199 F5.3 K.km/s e_intTA* ? Uncertainty in IntTA* 201 A1 --- u_VLSR [~] Approximate flag on VLSR 204-208 F5.1 km/s VLSR ? Local Standard of Rest velocity 210-212 F3.1 km/s e_VLSR ? Uncertainty in VLSR 214-220 A7 --- Notes Note(s) (2) -------------------------------------------------------------------------------- Note (1): Measured from 2MHz resolution data. Note (2): Notes as follows: S = double peaked line profile; B = unresolvable blend of emission lines from different molecules; P = partial blend of resolvable emission features; R = νrest is average of rotational transition frequencies; F = νrest is average of fine-structure transition frequencies; H = νrest is average of hyperfine-structure transition frequencies; V = νrest is average of rotational transition frequencies of different vibrational states of the same molecule; L = νrest is unreliable (see text section 4.4); ? = uncertain line assignment. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 F8.1 MHz Freq.0 Rest frequency (νrest) 10- 25 A16 --- Molecule Molecule identification 27- 79 A53 --- Trans Transition identification 81- 87 A7 --- Out Outflow direction (Blue, Red or Central) 89- 94 F6.3 K TA* Center antenna brightness temperature 96-101 F6.4 K e_TA* The 1σ uncertainty in TA* (1) 103-106 F4.1 km/s delV ? Full-Width at Half-Maximum line width 108-111 F4.1 km/s e_delV ? Uncertainty in delV 113-118 F6.3 K.km/s intTA* ? Integrated brightness temperature 120-124 F5.3 K.km/s e_intTA* ? Uncertainty in IntTA* 126 A1 --- u_VLSR [~] Approximate flag on VLSR 128-131 F4.1 km/s VLSR Local Standard of Rest velocity 133-135 F3.1 km/s e_VLSR ? Uncertainty in VLSR 137-140 A4 --- Notes Note(s) (2) -------------------------------------------------------------------------------- Note (1): Measured from 2MHz resolution data. Note (2): Notes as follows: B = unresolvable blend of emission lines from different molecules; P = partial blend of resolvable emission features; R = νrest is average of rotational transition frequencies; F = νrest is average of fine-structure transition frequencies; H = νrest is average of hyperfine-structure transition frequencies; ? = uncertain line assignment. -------------------------------------------------------------------------------- History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 07-Oct-2010
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