J/PASJ/53/517 Water maser survey of late-type stars (Takaba+, 2001)
Kashima 34-m water maser survey of late-type stars
Takaba H., Iwata T., Miyaji T., Deguchi S.
<Publ. Astron. Soc. Jap., 53, 517 (2001)>
=2001PASJ...53..517T 2001PASJ...53..517T
ADC_Keywords: Masers ; Stars, late-type ; Radio lines ; Radial velocities
Keywords: masers - radio lines: stars - stars: cricumstellar shells -
stars: late-type - stars: mass-loss
Abstract:
This paper presents new results of a water maser survey of late-type
stellar objects at 22.235GHz with the Kashima 34-m radio telescope. We
have detected 179 out of 643 observed sources, including 32 new
detections. The sources were selected in terms of the IRAS flux
density and colors of late-type stars, involving optically observable
Mira/semi-regular variables, IRC objects, OH/IR sources and
proto-planetary nebulae. We found the highest H2O detection rate for
the type of stars with a thin dust envelope (Mira/semi-regular
variables) among other types of sources. This is attributed to the
smaller distances to such stars in the sample. The velocity spread of
the H2O maser profile has an increasing tendency with the IRAS
color, though it becomes more difficult to access this color
dependence beyond an edge of the transition of the (oxygen-rich)
Asymptotic Giant Branch stars to protoplanetary nebulae in the
two-color diagram.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 92 32 List of new detections
table2.dat 78 147 List of known detections
table3.dat 52 464 List of non-detections
refs.dat 93 34 References
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- IRAS IRAS name
12- 23 A12 --- Name Star name
25 I1 --- Type [1/3] IRAS type (G1)
27 A1 --- Peak [SMD] Single, Multiple or Double peak
29- 32 F4.1 Jy S22GHz Flux density at 22.235GHz (G2)
34- 38 F5.1 km/s Vlsr LSR velocity (G2)
40- 43 F4.1 km/s DVlsr Separation in velocity between the
peaks (G2)
45- 54 A10 "YYYY/MM/DD" ObsDate1 First observation date
56- 65 A10 "YYYY/MM/DD" ObsDate2 Second observation date
67 A1 --- SiO [YN] SIO detection (Yes/No)
69 A1 --- OH [YN] OH detection (Yes/No)
71- 92 A22 --- r_Name References, separated by comma,
in refs.dat file (1)
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Note (1): The "D" sign in the parentheses indicates the H2O detection
noted in the cited paper, but no data available.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- IRAS IRAS designation
11 A1 --- n_IRAS [*] source not in IRAS-PSC (1)
13- 25 A13 --- Name Star name
27 I1 --- Type [0/3] IRAS type (G1)
29 A1 --- Peak [SMD] Single, Multiple or Double peak
31- 36 F6.1 Jy S22GHz Peak flux density at 22.235GHz (G2)
38- 42 F5.1 km/s Vlsr LSR velocity (G2)
44- 47 F4.1 km/s DVlsr Separation in velocity between the
peaks (G2)
49- 58 A10 "YYYY/MM/DD" ObsDate1 First observation date
60- 69 A10 "YYYY/MM/DD" ObsDate2 Second observation date
71- 78 A8 --- r_Name H2O reference in refs.dat file
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Note (1): this source was not found in the IRAS Point Source Catalog
so that we excluded this source from the statistical analysis
in the present paper.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- IRAS IRAS designation
12- 23 A12 --- Name Star name
24 A1 --- u_Name [?] Uncertainty flag on Name
26 I1 --- Type [1/3] IRAS type (G1)
28- 30 F3.1 Jy Flux Flux density at 22.235GHz upper limit
32- 41 A10 "YYYY/MM/DD" ObsDate1 First observation date
43- 52 A10 "YYYY/MM/DD" ObsDate2 Second observation date
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Ref Reference code
10- 28 A19 --- BibCode BibCode
30- 54 A25 --- Aut Author's name
56- 93 A38 --- Com Comments
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Global notes:
Note (G1): IRAS type as follows:
1 = -0.48<C12←0.2 and -1<C23←0.6
2 = -0.2<C12←0.2 and -1<C23←0.6
3 = 0<C12<1
where C12=log(F25/F12) and C23=log(F60/F25).
Note (G2):
-- For the single-peak sources, the line was fitted by a Gaussian
function; the resulting peak flux density (S22GHz), the peak
radial velocity (Vlsr), and the e-1 (DVlsr) width are listed.
-- For double-peak sources, each peak was fitted by a Gaussian function;
the peak flux density of the stronger peak (S22GHz) and the middle
velocity of the two peaks (Vlsr), as well as the separation in
velocity of the two peaks (DVlsr) are given.
-- For multiple-peak sources, the strongest peak intensity (S22GHz), the
average velocity of several peaks (Vlsr), and the largest separation
in velocity between the peaks (DVlsr) are listed.
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History:
From electronic version of the journal
(End) James Marcout, Patricia Bauer [CDS] 10-Jan-2002