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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
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:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
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)
Note (1): The "D" sign in the parentheses indicates the H2O detection noted in the cited paper, but no data available.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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
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.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Ref Reference code 10- 28 A19 --- BibCode BibCode 30- 54 A25 --- Aut Author's name 56- 93 A38 --- Com Comments
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.
History: From electronic version of the journal
(End) James Marcout, Patricia Bauer [CDS] 10-Jan-2002
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

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