2013A&A...560A..82R


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST04:48:05

2013A&A...560A..82R - Astronomy and Astrophysics, volume 560A, 82-82 (2013/12-1)

Sensitive CO and 13CO survey of water fountain stars. Detections towards IRAS 18460-0151 and IRAS 18596+0315.

RIZZO J.R., GOMEZ J.F., MIRANDA L.F., OSORIO M., SUAREZ O. and DURAN-ROJAS M.C.

Abstract (from CDS):

Water fountain stars represent a stage between the asymptotic giant branch (AGB) and planetary nebulae phases, when the mass loss changes from spherical to bipolar. These types of evolved objects are characterized by high-velocity jets in the 22GHz water maser emission. The objective of this work is to detect and study in detail the circumstellar gas in which the bipolar outflows are emerging. The detection and study of thermal lines may help in understanding the nature and physics of the envelopes in which the jets are developing. We surveyed the CO and 13CO line emission towards a sample of ten water fountain stars through observing the J=1->0 and 2->1 lines of CO and 13CO, using the 30m IRAM radio-telescope at Pico Veleta. All the water fountains visible from the observatory were surveyed. Most of the line emission arises from foreground or background Galactic clouds, and we had to thoroughly analyse the spectra to unveil the velocity components related to the stars. In two sources, IRAS18460-0151 and IRAS18596+0315, we identified wide velocity components with a width of 35-40 km/s that are centred at the stellar velocities. These wide components can be associated with the former AGB envelope of the progenitor star. A third case, IRAS18286-0959, is reported as tentative; in this case a pair of narrow velocity components, symmetrically located with respect to the stellar velocity, have been discovered. We also modelled the line emission using an LVG code and derived some global physical parameters, which allowed us to discuss the possible origin of this gas in relation to the known bipolar outflows. For IRAS18460-0151 and IRAS18596+0315, we derived molecular masses close to 0.2M, mean densities of 104cm–3, and mass-loss rates of 10–4M/yr. The kinetic temperatures are rather low, between 10 and 50K in both cases, which suggests that the CO emission is arising from the outer and cooler regions of the envelopes. No fitting was possible for IRAS18286-0959, because line contamination can not be discarded in this case. The molecular masses, mean densities, and mass-loss rates estimated for the circumstellar material associated with IRAS18460-0151 and IRAS18596+0315 confirm that these sources are at the end of the AGB or the beginning of the post-AGB evolutionary stages. The computed mass-loss rates are among the highest ones possible according to current evolutionary models, which leads us to propose that the progenitors of these water fountains had masses in the range from 4 to 8M. We speculate that CO emission is detected in water fountains as a result of a CO abundance enhancement caused by current episodes of low-collimation mass-loss.

Abstract Copyright:

Journal keyword(s): masers - stars: AGB and post-AGB - stars: evolution - stars: winds, outflows - ISM: molecules

Simbad objects: 14

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Number of rows : 14

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 16342-3814 pA* 16 37 39.8700524769 -38 20 17.440442399           ~ 128 0
2 IRAS 16552-3050 pA? 16 58 27.31 -30 55 07.9           ~ 25 1
3 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11533 0
4 OH 9.097 -0.392 OH* 18 07 20.861 -21 16 10.86           ~ 33 0
5 IRAS 18113-2503 pA? 18 14 27.2682296591 -25 03 00.472537854           ~ 23 0
6 OH 12.8 -0.9 IR 18 16 49.214 -18 15 01.66           ~ 45 2
7 IRAS 18139-1816 mul 18 16 51.1 -18 15 02           ~ 16 1
8 IRAS 18286-0959 pA* 18 31 22.94232 -09 57 21.3948           ~ 29 0
9 OH 31.0 +0.0 OH* 18 47 41.13768 -01 45 11.4048           ~ 124 1
10 MSX6C G031.0126-00.2195 Mas 18 48 42.8 -01 48 40           ~ 42 0
11 OH 37.1 -0.8 OH* 19 02 06.286 +03 20 15.99           ~ 64 0
12 IRAS 18596+0315 mul 19 02 06.4 +03 20 15           ~ 59 1
13 IRAS 19134+2131 pA* 19 15 35.2088301392 +21 36 33.815011564           ~ 60 0
14 [MHL2007] G046.2561-01.4763 1 Y*? 19 21 25.09 +11 08 41.0           ~ 22 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-04:48:05

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