========================================================================== J/ApJ/669/446 SiO masers infrared colors and intensity ratios (Nakashima+, 2007) The following files can be converted to FITS (extension .fit or fit.gz) table1.dat table3.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/ApJ/669/446 ==========================================================================
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Beginning of ReadMe : J/ApJ/669/446 Observations of SiO masers (Nakashima+, 2007) ================================================================================ Correlation between infrared colors and intensity ratios of SiO maser lines. Nakashima J.-I., Deguchi S. <Astrophys. J., 669, 446-458 (2007)> =2007ApJ...669..446N ================================================================================ ADC_Keywords: Infrared sources ; Masers ; Stars, late-type ; Photometry, infrared Keywords: masers - stars: AGB and post-AGB - stars: late-type - stars: mass loss - stars: statistics Abstract: We present the results of SiO millimeter line observations of a sample of known SiO maser sources covering a wide dust temperature range. A cold part of the sample was selected from the SiO maser sources found in our recent SiO maser survey of cold dusty objects. The aim of the present research is to investigate the causes of the correlation between infrared colors and SiO maser intensity ratios among different transition lines. In particular, the correlation between infrared colors and SiO maser intensity ratio among the J=1-0 v=1, 2, and 3 lines are our main concern in this paper. We observed in total 75 SiO maser sources with the Nobeyama 45m telescope quasi-simultaneously in the SiO J=1-0 v=0, 1, 2, 3, 4 and J=2-1 v=1, 2 lines. We also observed the sample in the ^29^SiO J=1-0 v=0 and J=2-1 v=0 lines, ^30^SiO J=1-0 v=0 line, and the H_2_O 61,6-52,3 line. Description: SiO line observations with the Nobeyama 45m telescope were made in two separated periods: 2004 May 11-19 and 2006 February 15-19. In the first period we observed, in total, 38 objects with the cooled SIS-mixer receivers, S40 and S100. The frequency coverage of S40 and S100 was roughly 500MHz. In the second period we observed, in total, 53 objects with the HEMT receiver H40 with a frequency coverage of roughly 2.0GHz.