2013A&A...558A.132D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST14:02:31

2013A&A...558A.132D - Astronomy and Astrophysics, volume 558A, 132-132 (2013/10-1)

PO and PN in the wind of the oxygen-rich AGB star IK Tauri.

DE BECK E., KAMINSKI T., PATEL N.A., YOUNG K.H., GOTTLIEB C.A., MENTEN K.M. and DECIN L.

Abstract (from CDS):

Phosphorus-bearing compounds have only been studied in the circumstellar environments of the asymptotic giant branch star IRC +10216 and the protoplanetary nebula CRL 2688, both carbon-rich objects, and the oxygen-rich red supergiant VY CMa. The current chemical models cannot reproduce the high abundances of PO and PN derived from observations of VY CMa. No observations have been reported of phosphorus in the circumstellar envelopes of oxygen-rich asymptotic giant branch stars. We aim to set observational constraints on the phosphorous chemistry in the circumstellar envelopes of oxygen-rich asymptotic giant branch stars, by focussing on the Mira-type variable star IK Tau. Using the IRAM 30m telescope and the Submillimeter Array, we observed four rotational transitions of PN (J=2-1,3-2,6-5,7-6) and four of PO (J=5/2-3/2,7/2-5/2,13/2-11/2,15/2-13/2). The IRAM 30m observations were dedicated line observations, while the Submillimeter Array data come from an unbiased spectral survey in the frequency range 279-355GHz. We present the first detections of PN and PO in an oxygen-rich asymptotic giant branch star and estimate abundances X(PN/H2)≃3x10–7 and X(PO/H2) in the range 0.5-6.0x10–7. This is several orders of magnitude higher than what is found for the carbon-rich asymptotic giant branch star IRC +10216. The diameter (≲0.7") of the PN and PO emission distributions measured in the interferometric data corresponds to a maximum radial extent of about 40 stellar radii. The abundances and the spatial occurrence of the molecules are in very good agreement with the results reported for VY CMa. We did not detect PS or PH3 in the survey. We suggest that PN and PO are the main carriers of phosphorus in the gas phase, with abundances possibly up to several 10–7. The current chemical models cannot account for this, underlining the strong need for updated chemical models that include phosphorous compounds.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - stars: individual: IK Tau - stars: mass-loss - astrochemistry

Simbad objects: 6

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Number of rows : 6

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 V* IK Tau Mi* 03 53 28.8884898148 +11 24 21.865959095 16.99 17.03 13.39 7.29 3.20 M7-11 570 0
2 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1053 3
3 V* VY CMa s*r 07 22 58.32877 -25 46 03.2355 12.01 10.19 7.95     M5Iae 995 0
4 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2133 0
5 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5316 1
6 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 830 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-14:02:31

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