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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 93 2229 Source parameters
table2.dat 85 114 Line Parameters of the new H2O masers
table3.dat 92 228 Line Parameters of the previous known H2O masers
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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
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Bytes Format Units Label Explanations
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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)
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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 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 2003ApJS..144...71F
3 = Wu, Huang and He, 1996, Cat. J/A+AS/115/283
4 = Lada and Lada, 2003ARA&A..41...57L 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 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 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.
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Byte-by-byte Description of file: table[23].dat
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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)
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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.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Dec-2008