J/PASJ/59/1185 Water maser in galactic IRAS sources (Sunada+, 2007)
Water maser and ammonia survey toward IRAS sources in the Galaxy. I. H2O maser data. Sunada K., Nakazato T., Ikeda N., Hongo S., Kitamura Y., Yang J. <Publ. Astron. Soc. Jap., 59, 1185-1219 (2007)> =2007PASJ...59.1185S
ADC_Keywords: Surveys ; Infrared sources ; Masers Keywords: masers - radio lines: ISM - stars: pre-main sequence - surveys Abstract: We present H2O maser data from a survey toward IRAS sources in the Galaxy with the Nobeyama 45m telescope. This survey had a 1σ noise level as small as 0.24Jy, resulting in one of the most sensitive water-maser surveys. The maximum distance of the masers to be detected by our survey is estimated to be 3kpc for sources with Fnu,1kpc<10Jy and 10kpc for those with 10Jy≤Fnu,1kpc<100Jy, where Fnu,1kpc is the maser flux density converted at a distance of 1kpc. For strong masers with Fnu,1kpc≥100Jy, our survey could detect all sources in the Galaxy. We carried out a total of 2229 observations toward 1563 sources and detected water-maser emission toward 222 sources. Our survey newly found masers from 75 of the 222 sources. Description: We started observations in the middle of 2004 September, and completed them at the beginning of 2005 June. We observed all of the sources with the Nobeyama 45m telescope. We simultaneously observed the maser lines of H2O (616-523 at 22.235GHz), and the 3 inversion transition lines of NH3 (23.6-23.9GHz) File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 93 2229 Source parameters table2.dat 92 114 Line Parameters of the new H2O masers table3.dat 92 228 Line Parameters of the previous known H2O masers
See also: J/MNRAS/276/57 : IRAS Galactic star-forming regions. II. (Codella+ 1995) J/A+AS/115/283 : A catalogue of high velocity molecular outflows (Wu+, 1996) J/PASJ/53/517 : Water maser survey of late-type stars (Takaba+, 2001) J/A+A/426/503 : Catalogue of high velocity molecular outflows (Wu+ 2004) J/ApJ/651/L125 : Water masers associated with IR dark cloud cores (Wang+, 2006) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Seq Sequential number 5 A1 --- m_Seq [abc] Multiplicity index on Seq 6 A1 --- f_Seq [*] For BIP 14, misprint on position (1) 7- 22 A16 --- Name Source name 24- 25 I2 h RAh Right ascension (J2000.0) 27- 28 I2 min RAm Right ascension (J2000.0) 30- 33 F4.1 s RAs [0/60] Right ascension (J2000.0) 35 A1 --- DE- Declination sign (J2000.0) 36- 37 I2 deg DEd Declination (J2000.0) 39- 40 I2 arcmin DEm Declination (J2000.0) 42- 43 I2 arcsec DEs [0/60] Declination (J2000.0) 45- 51 A7 --- Ref Position reference (2) 53- 62 A10 "DD/MM/YYYY" Date Observation date 64- 67 F4.2 Jy 1sig Survey sensitivity (1σ rms flux density) 69- 93 A25 --- Note Notes (3)
Note (1): For BIP 14, the correct position is 06 59 16.7 -03 59 35. Position in the table comes from a misprint in Lada & Lada, 2003ARA&A..41...57L Note (2): References of positions as follows: 1 = Yang et al., 2002, Cat. J/ApJS/141/157 2 = Furuya et al., 2003ApJS..144...71F 3 = Wu, Huang and He, 1996, Cat. J/A+AS/115/283 4 = Lada and Lada, 2003ARA&A..41...57L Note (3): H2O means this source is a a known H2O maser source. An angular distance from the position of the known H2O maser source is indicated in parenthesis. If the difference is less than 10", we neglect this difference. If we give an ID number, it means this is the same H2O maser source as the ID source, but the position is farther than the ID source. An angular distance from the position of the ID source is indicated in parenthesis. The symbols mean: ++ = Observation positions of these sources were taken from the catalogue of Furuya et al. (2003ApJS..144...71F) as the positions of the H2O maser sources. The positions, however, are different from the ones of the catalogue of Valdettaro et al., 2001, Cat. J/A+A/368/845. We give the angular distances from the positions of the catalogue of Valdettaro et al., 2001, in parenthesis. $ = This position was taken from the catalogue of Furuya et al. (2003ApJS..144...71F). In the neighborhood, there are two H2O maser sources in the catalogue of Valdettaro et al., 2001, Cat. J/A+A/368/845. We give the angular distances from two H2O maser sources in parenthesis.
Byte-by-byte Description of file: table.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Seq Sequential number 5 A1 --- m_Seq [abc] Multiplicity index on Seq 7- 16 A10 "DD/MM/YYYY" Date Observation date 18- 23 F6.1 km/s Vmin ? LSR velocity range of H2O maser emission, lower value 25- 29 F5.1 km/s Vmax ? LSR velocity range of H2O maser emission, upper value 31- 36 F6.2 km/s Vmean ? Flux-density-weighted mean velocity 38- 43 F6.2 km/s Vpeak ? Peak velocity of the strongest maser component 44- 51 F8.2 Jy.km/s Ipeak ? Integrated flux density of the strongest maser component 52 A1 --- --- [/] 53- 61 F9.2 Jy.km/s Itot ? Total-integrated flux density over the range of the minimum to maximum velocities 63 A1 --- l_Fpeak Limit flag on Fpeak 64- 71 F8.2 Jy Fpeak ? Peak flux density of the strongest component 73- 76 F4.2 km/s FWHM ? Line width of the strongest component 78- 92 A15 --- Note Notes (1)
Note (1): Signal-to-noise ratio for peak flux density between 4σ and 5σ noise levels. + = We found that the H2O maser emission toward these sources could not be explained by a single source. Identification of these sources are discussed in the main text.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Dec-2008
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