2004A&A...423..209S


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.06CEST00:29:40

2004A&A...423..209S - Astronomy and Astrophysics, volume 423, 209-219 (2004/8-3)

Polarimetric observations of OH masers in proto-planetary nebulae.

SZYMCZAK M. and GERARD E.

Abstract (from CDS):

The 1612 and 1667MHz OH maser lines have been measured in all four Stokes parameters in 47 proto-planetary nebula (PPN) candidates. Out of 42 objects detected, 40 and 34 are 1612 and 1667MHz emitters, respectively. The spectral extent of the 1667MHz line overshoots that of the 1612MHz line in about 80% of the targets. 52% and 26% of the 1612 and 1667MHz sources, respectively, show linear polarization in at least some features. Circular polarization is more frequent, occurring in 78% and 32% of sources of the respective OH lines. The percentage polarization is usually small (<15%) reaching up to 50-80% in a few sources. Features of linearly polarized emission are usually weak (0.5-4Jy) and narrow (0.3-0.5km/s). The strength of the magnetic field inferred from likely Zeeman pairs in two sources of a few mG is consistent with values reported elsewhere for those classes of objects. An upper limit of the electron density in the envelope of OH17.7-2.0 derived from the difference in the position angle of polarization vectors for the two OH lines is about 1cm–3. Distinct profiles of polarization position angle at 1612 and 1667MHz are seen in about one third of the sources and strongly suggest that the envelopes are permeated by structured magnetic fields. The geometry of the magnetic field is implicated as an important cause of the depolarization found in some PPN candidates. For the subset of targets which show axisymmetric shells in the optical or radio images we found a dominance of magnetic field components which are orthogonal to the long axis of the nebulae. This finding supports the hypothesis that such bipolar lobes are shaped by the magnetic field.

Abstract Copyright:

Journal keyword(s): polarization - masers - stars: AGB and post-AGB - ISM: planetary nebulae: general - stars: circumstellar matter

Simbad objects: 48

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Number of rows : 48

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 IRAS 06530-0213 pA* 06 55 31.8196049619 -02 17 28.245201716   16.38 13.99 13.26   F5Ia 68 0
2 V* AI CMi pA* 07 35 41.1518203544 +00 14 57.987903123   9.83 8.31     G5Iab 51 0
3 OH 231.8 +4.2 OH* 07 42 16.947 -14 42 50.20           M10III+A 503 1
4 IRAS 08005-2356 pA* 08 02 40.7024600066 -24 04 42.576601013   12.85       F5Iae 84 0
5 IRAS 16342-3814 pA* 16 37 39.8700524769 -38 20 17.440442399           ~ 128 0
6 IRAS 16559-2957 pA* 16 59 08.2422710117 -30 01 40.205999181     13.2     F5I(e) 31 0
7 IRAS 17079-3844 pA* 17 11 23.2 -38 48 18           ~ 5 0
8 NGC 6302 PN 17 13 44.339 -37 06 10.95   7.1 10.10     ~ 757 1
9 RAFGL 6815S pA* 17 18 19.8316623567 -32 27 21.376880888           G2I 147 0
10 OH 349.36 -0.20 pA* 17 18 29.0 -37 58 02           ~ 21 0
11 OH 0.1 +5.1 OH* 17 26 28.995 -26 04 56.85         17.23 ~ 26 1
12 IRAS 17253-2831 pA* 17 28 33.3 -28 33 28           ~ 9 0
13 IRAS 17347-3139 PN 17 38 00.61 -31 40 55.2           ~ 55 1
14 IRAS 17371-2747 mul 17 40 20.7 -27 49 11           ~ 15 0
15 IRAS 17375-2759 PN 17 40 38.8631490417 -28 01 03.083801797           ~ 15 0
16 IRAS 17375-3000 PN 17 40 43.3808087335 -30 02 04.564576881           ~ 14 0
17 IRAS 17385-3332 pA* 17 41 52.2828274827 -33 33 40.575162432           ~ 26 0
18 OH 0.9 +1.3 pA* 17 42 33.0790162842 -27 28 25.844214046           ~ 52 0
19 IRC -30316 OH* 17 42 35.0213310681 -30 05 41.840711558     15     M4 32 0
20 OH 1.2 +1.3 OH* 17 43 38.0349806522 -27 14 44.167430575           ~ 28 0
21 HD 161796 pA* 17 44 55.4696 +50 02 39.484 8.00 7.68 7.21 6.77 6.51 F3Ib 310 0
22 Hen 3-1475 PN 17 45 14.1763468506 -17 56 46.890631888   13.84 12.87     B7e 189 0
23 IRAS 17433-1750 pA* 17 46 15.8274714137 -17 51 45.968535966           ~ 20 0
24 IRAS 17443-2949 PN 17 47 35.28 -29 50 56.2           ~ 30 0
25 IRAS 17516-2525 pA* 17 54 43.3467071361 -25 26 28.136063518           O-B? 36 1
26 IRAS 17579-3121 pA* 18 01 13.3684155706 -31 21 56.595824497   12.69 11.40 11.02   F4I 16 0
27 OH 3.175 -3.024 OH* 18 04 45.8 -27 43 11           ~ 12 1
28 IRAS 18025-3906 pA* 18 06 03.3022397498 -39 05 56.814513951       11.24 9.91 G2I 17 0
29 OH 10.0 -0.1 OH* 18 08 16.384 -20 16 11.56           ~ 30 0
30 OH 12.8 +0.9 pA* 18 10 06.08 -17 26 34.5           ~ 40 0
31 HD 335675 pA* 18 11 30.6604895815 +27 05 15.662372766   11.52 10.55     F3Ib 106 0
32 IRAS 18091-1815 pA* 18 12 03.4 -18 14 25           ~ 8 0
33 IRAS 18105-1935 OH* 18 13 29.922 -19 35 02.92           ~ 15 1
34 OH 15.7 +0.8 OH* 18 16 25.376 -14 55 15.66           ~ 72 0
35 OH 19.2 -1.0 OH* 18 29 28.7281021583 -12 37 53.122540549           ~ 48 0
36 OH 17.7 -2.0 pA* 18 30 30.703 -14 28 57.04           ~ 133 1
37 OH 31.0 +0.0 OH* 18 47 41.13768 -01 45 11.4048           ~ 125 1
38 IRAS 18491-0207 pA* 18 51 46.9 -02 04 09           ~ 19 1
39 OH 37.1 -0.8 OH* 19 02 06.286 +03 20 15.99           ~ 65 0
40 IRAS 18596+0315 mul 19 02 06.4 +03 20 15           ~ 59 1
41 OH 42.3 -0.1 OH* 19 09 07.4662208672 +08 16 22.702583816       16.16   ~ 79 0
42 HD 179821 pA* 19 13 58.6083165753 +00 07 31.934676028 10.81 9.694 8.19     G4_0-Ia 221 0
43 PN WhMe 1 PN 19 14 59.7260221295 +17 22 46.027423381     12.0     B9V 43 0
44 PN Vy 2-2 PN 19 24 22.2390166933 +09 53 56.259102426   14.02 12.65 13.38   ~ 248 0
45 PN K 3-35 PN 19 27 43.9751068155 +21 30 02.898607561           ~ 134 0
46 Min 1-92 pA* 19 36 18.9292148675 +29 32 49.838032394 12.13 12.35 11.75 11.54   B0.5IV[e] 236 1
47 IRAS 22036+5306 pA* 22 05 30.29 +53 21 32.8   19.2       F4III 74 0
48 IRAS 23321+6545 pA* 23 34 22.48 +66 01 51.7           C-rich 45 0

    Equat.    Gal    SGal    Ecl

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2020.08.06-00:29:40

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