2019ApJ...878...90S


Query : 2019ApJ...878...90S

2019ApJ...878...90S - Astrophys. J., 878, 90-90 (2019/June-3)

Detection of 4765 MHz OH emission in a preplanetary nebula: CRL 618.

STRACK A., ARAYA E.D., LEBRON M.E., MINCHIN R.F., ARCE H.G., GHOSH T., HOFNER P., KURTZ S., OLMI L., PIHLSTROM Y. and SALTER C.J.

Abstract (from CDS):

Jets and outflows are ubiquitous phenomena in astrophysics, found in our Galaxy in diverse environments, from the formation of stars to late-type stellar objects. We present observations conducted with the 305 m Arecibo Telescope of the preplanetary nebula CRL 618 (Westbrook Nebula)-a well-studied late-type star that has developed bipolar jets. The observations resulted in the first detection of 4765 MHz OH in a late-type stellar object. The line was narrow (FWHM ∼ 0.6 km s–1) and ∼40 km s–1 blueshifted with respect to the systemic velocity, which suggests association with the expanding jets/bullets in CRL 618. We also report nondetection at Arecibo of any other OH transition between 1 and 9 GHz. The nondetections were obtained during the observations in 2008, when the 4765 MHz OH line was first discovered, and also in 2015 when the 4765 MHz OH line was not detected. Our data indicate that the 4765 MHz OH line was a variable maser. Modeling of the 4765 MHz OH detection and nondetection of the other transitions is consistent with the physical conditions expected in CRL 618. The 4765 MHz OH maser could originate from dissociation of H2O by shocks after sublimation of icy objects in this dying carbon-rich stellar system, although other alternatives such as OH in an oxygen-rich circumstellar region associated with a binary companion are also possible.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): circumstellar matter - masers - stars: AGB and post-AGB - stars: individual: CRL 618

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 970 0
2 V* U Ori Mi* 05 55 49.1689920441 +20 10 30.690374867 6.82 6.39 5.40     M6-9.5e 476 0
3 PN Vo 1 PN 06 59 26.4078328215 -79 38 47.129323563   16.7 15.8     [WC10] 94 0
4 V* AU Gem Mi* 07 45 27.4426742863 +30 46 41.342625121           M10 29 0
5 IRAS 08005-2356 pA* 08 02 40.7024600066 -24 04 42.576601013   12.85       F5Iae 85 0
6 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2205 0
7 V* Y CVn C* 12 45 07.8257032577 +45 26 24.898861195 14.03 7.41 4.87 3.12 1.74 C-N5 466 0
8 V* U Her Mi* 16 25 47.4723609675 +18 53 32.862370166 8.85 8.23 6.70     M6.5-8+e 523 1
9 IRAS 16342-3814 pA* 16 37 39.8700524769 -38 20 17.440442399           ~ 131 0
10 C* 3302 C* 19 15 01.5589012368 +54 17 29.206949628   16.3 11.8     C 31 0
11 PN Vy 2-2 PN 19 24 22.2390166933 +09 53 56.259102426   14.02 12.65 13.38   ~ 252 0
12 PN K 3-35 PN 19 27 43.9751068155 +21 30 02.898607561           ~ 136 0
13 MSB 38 C* 20 36 07.3863551706 +60 05 26.037276961   13.98 9.86 10.3   C-J4+ 119 0
14 NML Cyg s*r 20 46 25.5382179476 +40 06 59.396202678   18.64 16.60     M7/8 488 0
15 V* EU And C* 23 19 58.8815022082 +47 14 34.576375397   12.84 10.38     C-J5- 88 0

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2021.09.26-05:51:02

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