J/ApJS/155/595 OH maser IRAS and MSX observations (Deacon+, 2004)
OH maser observations of likely planetary nebulae precursors.
Deacon R.M., Chapman J.M., Green A.J.
<Astrophys. J. Suppl. Ser., 155, 595-622 (2004)>
=2004ApJS..155..595D 2004ApJS..155..595D
ADC_Keywords: Masers ; Radio lines ; Infrared sources
Keywords: circumstellar matter - masers - radio lines: stars -
stars: AGB and post-AGB - stars: evolution - stars: mass loss
Abstract:
We present OH maser observations at 1612, 1665, 1667, and 1720MHz
for 86 likely post-asymptotic giant branch (post-AGB) stars selected
from a survey of 1612MHz maser sources in the Galactic plane. The
observations were taken with the Parkes Telescope and the Australia
Telescope Compact Array between 2002 September and 2003 August. We
redetected all 86 sources at 1612MHz, while 27 sources were detected
at 1665MHz and 45 at 1667MHz. One source was redetected at 1720MHz.
We present a classification scheme for the maser profiles and show
that 25% of sources in our sample are likely to have asymmetric or
bipolar outflows.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 110 88 Source data
table3.dat 73 259 Results from 1612, 1665 and 1667 MHz observations
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See also:
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
V/114 : MSX6C Infrared Point Source Catalog (Egan+ 2003)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- ID The ATCA/VLA survey source identifier (G1)
6- 15 A10 --- Name IRAS name
17- 18 I2 h RAh Hour of Right Ascension (J2000)
20- 21 I2 min RAm Minute of Right Ascension (J2000)
23- 28 F6.3 s RAs Second of Right Ascension (J2000)
30 A1 --- DE- Sign of the Declination (J2000)
31- 32 I2 deg DEd Degree of Declination (J2000)
34- 35 I2 arcmin DEm Arcminute of Declination (J2000)
37- 41 F5.2 arcsec DEs Arcsecond of Declination (J2000)
43- 48 F6.1 km/s VLSR Local Standard of Rest velocity
50- 55 F6.2 Jy S12umI ? IRAS 12 micron flux density
57- 62 F6.2 Jy S25umI ? IRAS 25 micron flux density
64- 70 F7.2 Jy S60umI ? IRAS 60 micron flux density
72- 77 F6.2 Jy S8umM ? MSX 8 micron flux density
79- 84 F6.2 Jy S12umM ? MSX 12 micron flux density
86- 91 F6.2 Jy S15umM ? MSX 15 micron flux density
93- 98 F6.2 Jy S21umM ? MSX 21 micron flux density
100-106 A7 --- ClassM The MSX classification (1)
108-109 A2 --- ClassI The IRAS classification (2)
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Note (1): MSX classification as follows:
Quad I = late post-AGB stars;
Quad IV = early post-AGB stars.
Note (2): IRAS classification as follows:
RI = Right-hand IRAS region traditionally associated with post-AGB
stars that have evolved to the right of the AGB evolutionary track.
LI = Left-hand IRAS region containing likely post-AGB stars that have
evolved left of the AGB evolutionary track.
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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- 4 A4 --- ID The ATCA/VLA survey source identifier (G1)
6- 9 I4 Hz Freq Observed frequency
11- 17 F7.2 km/s Vb ? Blue-shifted velocity (1)
19- 24 F6.2 Jy Sb ? Blue-shifted peak flux density (1)
26- 30 F5.1 Jy.km/s Ib ? Blue-shifted integrated flux density (1)
32- 38 F7.2 km/s Vr ? Red-shifted velocity
40- 45 F6.2 Jy Sr ? Red-shifted peak flux density
47- 51 F5.1 Jy.km/s Ir ? Red-shifted integrated flux density
53- 57 F5.2 --- Sb/Sr ? Peak-to-peak flux density ratio
59- 62 F4.1 --- Ib/Ir ? Integrated flux density ratio
64- 65 I2 km/s Vrange ? Total velocity range of detected emission (2)
67- 68 A2 --- SpType Spectral classification (3)
70- 72 A3 --- Flag Variability, marginal detection and date flag (4)
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Note (1): Or for the strongest emission feature from sources with single peaks,
irregular and many-peaked spectra.
Note (2): Measured at a cutoff level of 3σ (excluding absorption and
identified confusion).
Note (3): Spectral classification as follows:
D = Double. Double-peaked profiles with peak-peak flux density
ratios <8.0. This is the "classic" profile type associated with
OH/IR stars on the AGB.
De = Double extreme. Profiles with peak-peak flux density ratios >8.0.
There is a large population of sources with peak-to-peak ratios
of 3 or less, and a small population with much larger ratios.
A cutoff of 8.0 separates these two groups cleanly.
Dw = Double with wings. Double-peaked profiles with sloping outer
edges rather than the near-vertical outer edge of D sources.
DD = Double-double) One source in our sample, d47, shows four emission
peaks at 1612 MHz, symmetrical in outflow velocity and strength
around the central stellar velocity.
S = Single. Single-peaked profiles with one narrow emission peak with
a steep edge on one side of the feature.
I = Irregular. These profiles exhibit a range of features that
include one wide peak, several peaks, or plateaus of emission
with peaks superimposed.
Note (4): Flags as follows:
V = Sources which are more than 30% variable at 1612MHz;
2nd = d47 has two lines for 1612MHz data;
m = Marginal detection, Sept 2002 data;
# = August 2003 data;
m# = Marginal detection, August 2003 data.
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Global notes:
Note (G1): Nomenclature note:
dNNN = SCHD NNN, bNNN = SCHB NNN, vNNN = [SVM2001b] in Simbad
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 21-Mar-2006