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J/A+AS/93/121 CO emission from a sample of IRAS sources (Nyman+ 1992)
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A survey of circumstellar CO emission from a sample of IRAS sources
Nyman L.A., Booth R.S., Carlstroem U., Habing H.J., Heske A., Sahai R.,
Stark R., van der Veen W.E.C.J., Winnberg A.
<Astron. Astrophys. Suppl. Ser. 93, 121 (1992)>
=1992A&AS...93..121N
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ADC_Keywords: Infrared sources; CO; Stars, late-type; Mass loss
Keywords: stars: circumstellar matter - stars: mass loss - radio lines:
molecular (CO) - infrared radiation
Abstract:
The first results from a survey of circumstellar CO(1-0) emission are
presented. The sources were selected from the IRAS point source catalog
according to the IRAS color criteria described in van der Veen and Habing
(1988). The sources have good quality fluxes at 12, 25, and 60 microns,
flux densities larger than 20 Jy at 25 microns, and are situated more than
5 deg away from the Galactic plane. The survey is undertaken to study the
relationship between mass loss rates, dust properties, and the evolution
along the AGB. The sample consists of 787 sources and contains both oxygen
and carbon-rich stars, including Mira variables, OH/IR objects,
protoplanetary nebulae, planetary nebulae, and 60-micron excess sources.
So far, 519 objects, situated on both the northern and the southern sky,
have been observed; 163 sources were found to have circumstellar CO
emission, and in 58 of these CO emission has not previously been detected.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4 90 519 Detected and undetected sources
table6 69 103 Objects with cold envelopes
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Byte-by-byte Description of file: table4
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Bytes Format Units Label Explanations
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1 A1 --- T Table indicator a,b,c
2- 11 A10 --- IRAS IRAS Source Name
13- 16 A4 --- Region in the IRAS two color diagram as defined by
van der Veen & Habing, 1988 , A&A 194, 125.
18- 23 F6.0 Jy F12 IRAS 12 micrometer flux density
25- 30 F6.0 Jy F25 IRAS 25 micrometer flux density
32- 37 F6.0 Jy F60 IRAS 60 micrometer flux density
39- 43 F5.3 K rms ? Rms noise the CO spectrum, given in K (Tmb).
45- 49 F5.2 K Tmb ? Main beam brightness peak intensity of the
detected line
51- 56 F6.1 km/s V0 ? Center velocity of the CO line (in km/s).
57 A1 --- n_V0 Remark on V0 (1)
59- 62 F4.1 km/s Vexp ? Expansion velocity. This is half of the
full line width at zero intensity.
64- 68 F5.1 km/s Ico ? CO intensity integrated over the whole line
(in K km/s, Tmb scale).
70- 71 I2 --- Ref ? Reference to a previous CO detection of
the source. (2)
73- 90 A18 --- Ident Source name (if different from the IRAS name).
An asterisk after the name indicates that
there is an interstellar line included in
the CO spectrum.
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Note (1):
a. The centre velocity is uncertain up to +/-10 kms^-1 (see text).
b. Previous CO detections. For sources previously detected in CO (1--0)
emission and not detected by us, the CO (1--0) line was usually too weak
to be seen with our sensitivity limit, and in a few cases it may
only have been a tentative detection. Sources detected in the
CO (2--1) line are also listed as previous detections.
The CO (2--1) line can be brighter than the (1--0) line
because of optical depth and beam filling effects, and the
(1--0) line may be too weak to be detected.
Note (2):
References:
1. Knapp & Morris (1985),
2. Zuckerman et al. (1986),
3. Zuckerman & Dyck (1986a),
4. Zuckerman & Dyck (1986b),
5. Zuckerman & Dyck (1989),
6. Olofsson et al. (1987),
7. Olofsson et al. (1988),
8. Sopka et al. (1989),
9. Lindqvist et al. (1988),
10. Wannier & Sahai (1986),
11. Nguyen--Q--Rieu et al. (1987),
12. Knapp et al. (1982),
13. Likkel et al. (1987),
14. Knapp et al. (1989),
15. Deguchi et al. (1990),
16. Loup et al. (1990),
17. Heske et al. (1990),
18. Huggins & Healy (1989),
19. Woodsworth et al. (1990),
20. Margulis et al. (1990),
21. Knapp (1986),
22. Leahy et al. (1987),
23. Arquilla et al. (1986)
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Table 5: CO parameters as function of IRAS regions
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Region v_exp Dv_exp K_60 +/- A_60 +/- r_60 n
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II 11.4 5.4 0.64 0.19 -0.48 0.28 0.63 19
IIIa 14.5 4.0 0.87 0.06 -0.76 0.09 0.88 67
IIIb 17.2 3.7 0.68 0.20 -0.51 0.30 0.79 9
IV 18.9
V 12.7 2.0
VIa 16.1 8.9 1.03 0.18 -0.67 0.21 0.92 8
VIb 17.7
VII 16.6 6.6 0.91 0.07 -0.50 0.10 0.87 50
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r_60 is the correlation coefficient to the fit
log(I_CO)=K_60.log(F_60)+A_60
and n is the number of sources included in the fit.
Byte-by-byte Description of file: table6
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Bytes Format Units Label Explanations
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1- 10 A10 --- IRAS IRAS Source Name
12- 15 A4 --- Region in the IRAS two color diagram as defined by
van der Veen & Habing, 1988 , A&A 194, 125.
17- 18 A2 --- Det Detection, as:
D = Detected by us
? = Tentative detection
N = Non--detection
* = Interstellar line in the CO spectrum.
20- 21 I2 --- r_Det ? Reference to previous detection (1)
23- 58 A36 --- Ident Identification
61- 65 A5 --- Sp-type Spectral type
67- 70 A4 --- r_Id Reference to Identification (1)
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Note (1):
References:
1. Zijlstra et al. (1989)
2. Volk & Kwok (1989)
3. Kwok et al. (1989)
4. te Lintel Hekkert et al. (1988)
5. Hrivnak et al. (1988)
6. Cernicharo et al. (1989)
7. Cohen & Schwarz (1984)
8. Beichman et al. (1986)
9. Gaylard et al. (1989)
10. te Lintel Hekkert et al. (1989)
11. Menzies & Wolstencroft (1990)
12. Hu et al. (1989)
13. Hu et al. (1990)
14. Rao et al. (1990)
15. Lambert et al. (1986)
16. Heske et al. (1990)
17. Olofsson et al. (1987)
18. Woodsworth et al. (1990)
19. Sopka et al. (1989)
20. Knapp & Morris (1985)
21. Loup et al. (1990)
22. Zuckerman et al. (1986)
23. Olofsson et al. (1988)
24. Knapp et al. (1989)
25. Zuckerman & Dyck (1986b)
26. Huggins & Healy (1989)
27. Likkel et al. (1987)
28. Zuckerman & Dyck (1986a)
29. Arquilla et al. (1986)
30. Pesce et al. (1988).
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(End) [CDS] 19-Mar-1993