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YOO14 - SiO and H2O Maser Survey toward Post-asymptotic Giant Branch and Asymptotic Giant Branch Stars

Short title: Yoon et al. (2014)
Authors: Yoon, Dong-Hwan Cho, Se-Hyung Kim, Jaeheon Yun, Young joo Park, Yong-Sun
Journal: The Astrophysical Journal Supplement, Volume 211, Issue 1, article id. 15, 27 pp. (2014).
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Target type: pAGB_PN
Observations category: star.general

Abstract
We performed simultaneous observations of SiO v = 1, 2, ²⁹SiO v = 0, J = 1-0 and H₂O 6₁₆-5₂₃ maser lines toward 143 AGB and 164 post-asymptotic giant branch (AGB) stars in order to investigate how evolutionary characteristics from AGB to post-AGB stars appear in both SiO and H₂O maser emissions. The observations were carried out from 2011 February to 2012 March using the Korean VLBI Network single-dish telescopes. We have detected SiO and/or H₂O maser emission from 21 sources out of 164 post-AGB stars including 12 new detections. Of 143 AGB stars, we detected SiO and/or H₂O maser emission from 44 stars including 24 new detections. SiO v = 2, J = 1-0 maser emission without a SiO v = 1 maser was detected from 7 sources among 14 SiO-detected post-AGB stars, and the intensity of the SiO v = 2, J = 1-0 maser tends to be much stronger than that of SiO v = 1, which is different from those of AGB stars. This may be related to the development of hot dust shells according to the evolutionary processes of post-AGB stars. We also found that both SiO and H₂O masers were detected in the blue group (LI, or Left of IRAS), while only the H₂O maser was detected in the red group (RI, or Right of IRAS) for post-AGB stars. These different detection rates between SiO and H₂O masers may originate from the different abundances of masing molecules in the circumstellar envelope according to the different mass and expansion velocity between LI and RI regions together with their evolutionary stages.

Abstract

We performed simultaneous observations of SiO v = 1, 2, ²⁹SiO v = 0, J = 1-0 and H₂O 6₁₆-5₂₃ maser lines toward 143 AGB and 164 post-asymptotic giant branch (AGB) stars in order to investigate how evolutionary characteristics from AGB to post-AGB stars appear in both SiO and H₂O maser emissions. The observations were carried out from 2011 February to 2012 March using the Korean VLBI Network single-dish telescopes. We have detected SiO and/or H₂O maser emission from 21 sources out of 164 post-AGB stars including 12 new detections. Of 143 AGB stars, we detected SiO and/or H₂O maser emission from 44 stars including 24 new detections. SiO v = 2, J = 1-0 maser emission without a SiO v = 1 maser was detected from 7 sources among 14 SiO-detected post-AGB stars, and the intensity of the SiO v = 2, J = 1-0 maser tends to be much stronger than that of SiO v = 1, which is different from those of AGB stars. This may be related to the development of hot dust shells according to the evolutionary processes of post-AGB stars. We also found that both SiO and H₂O masers were detected in the blue group (LI, or Left of IRAS), while only the H₂O maser was detected in the red group (RI, or Right of IRAS) for post-AGB stars. These different detection rates between SiO and H₂O masers may originate from the different abundances of masing molecules in the circumstellar envelope according to the different mass and expansion velocity between LI and RI regions together with their evolutionary stages.

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Detection table from Yoon et al. (2014)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Other name	Line	V_peak	T_a	∫T_a dv	Detection	Class	Dist. (parallax)
	(J2000)	(J2000)	(deg.)	(deg.)				Seq	H₂O	(km/s)	(K)	(K*km/s)	Yes/No		(kpc)
1	18 08 16.4	-20 16 11.3	10.0760	-0.0950	G10.076-0.095	G10.0759-0.0950	OH10.1-0.1	73	22 GHz;	26.3	0.2		+H₂O +OH	EVOLVED
2	18 21 6.4	-15 03 29.8	16.1142	-0.2898	G16.117-0.291	G16.1170-0.2906	OH16.12-0.29	83	22 GHz;	6.4	0.59		+H₂O -CH₃OH I +CH₃OH II +OH +SiO	EVOLVED
3	19 01 20.1	+04 32 31.6	38.1014	-0.1253	G38.101-0.125	G38.1012-0.1253	OH38.10-0.13	113	22 GHz;	31.9	0.92		+H₂O +OH +SiO	SFR_MIXED
4	07 06 58.9	+08 52 37	206.7481	7.4671	G206.748+7.467	G206.7477+7.4668	V CMi	52	22 GHz;	16.6	0.06		+H₂O -SiO	EVOLVED
5	07 07 21.9	+28 17 55.9	188.7705	15.6988	G188.771+15.699	G188.7705+15.6988	AM Gem	53	22 GHz;	-53.6	0.17		+H₂O +SiO	EVOLVED
6	07 18 23.3	+38 03 11.1	180.0032	21.3020	G180.003+21.302	G180.0032+21.3020	IRC+40172	54	22 GHz;	-30.3	0.11		+H₂O	EVOLVED
7	07 20 19.5	-13 20 13.7	228.0662	0.2108	G228.066+0.211	G228.0659+0.2108	IRAS 07180-1314	55	22 GHz;	48.8	0.82		+H₂O +OH +SiO	EVOLVED
8	08 52 5.6	-33 05 43.9	256.0364	7.2189	G256.036+7.219	G256.0364+7.2189	IRAS 08500-3254	67	22 GHz;	56.4	0.21		+H₂O +SiO	EVOLVED
9	09 42 22.7	+77 51 7.4	133.8016	34.9504	G133.802+34.950	G133.8016+34.9504	Y Dra	71	22 GHz;	22.1	0.13		+H₂O -OH +SiO	EVOLVED
10	18 27 24.2	-01 00 45.6	29.2805	4.8813	G29.281+4.881	G29.2805+4.8813	IRAS 18248-0102	103	22 GHz;	-6.9	0.13		+H₂O -OH +SiO	EVOLVED
11	18 54 18.4	-06 48 56.4	27.1832	-3.7369	G27.183-3.737	G27.1832-3.7369	IRAS 18516-0652	104	22 GHz;	-19.7	0.07		+H₂O +SiO	EVOLVED
12	20 36 57	+37 52 33.9	77.8983	-1.8432	G77.898-1.843	G77.8983-1.8432	V1828 Cyg	113	22 GHz;	-4.9	0.54		+H₂O +SiO	EVOLVED
13	20 39 39.6	+50 12 15	88.0143	5.2351	G88.014+5.235	G88.0144+5.2354	IRAS 20381+5001	118	22 GHz;	-43.0	0.51		+H₂O +SiO	EVOLVED
14	21 27 31.4	+71 48 59.7	108.3974	14.9723	G108.398+14.972	G108.3979+14.9722	V363 Cep	120	22 GHz;	-22.6	0.11		+H₂O +SiO	EVOLVED
15	22 49 59.2	+60 17 55	108.4259	0.8932	G108.426+0.893	G108.4257+0.8933	IRC+60370	134	22 GHz;	-40.5	1.81		+H₂O -OH	UNK
16	07 35 41.1	+00 14 57.9	217.8017	9.9475	G217.801+9.947	G217.8013+9.9475	AI CMi	21	22 GHz;	29.8	0.39	0.31	+H₂O +OH	EVOLVED
17	16 58 27.8	-30 55 6.2	352.5667	7.2977	G352.567+7.298	G352.5667+7.2976	IRAS 16552-3050	28	22 GHz;	-64.3	0.67	6.69	+H₂O -OH	EVOLVED
18	17 32 11.2	-21 50 2.2	4.4168	6.3403	G4.415+6.344	G4.4168+6.3403	IRAS 17291-2147	40	22 GHz;	-16.4	0.11	0.17	+H₂O -CH₃OH I -OH	EVOLVED
19	18 06 53.3	-19 03 09	10.9810	0.7819	G10.981+0.782	G10.9810+0.7819	IRAS 18039-1903	69	22 GHz;	153.1	0.92	1.35	+H₂O -CH₃OH I +OH	EVOLVED
20	18 14 26.7	-25 02 54.8	6.5666	-3.6396	G6.566-3.638	G6.5655-3.6383	IRAS 18113-2503	81	22 GHz;	-137.7	0.98	19.29	+H₂O -CH₃OH I -OH	EVOLVED
21	19 09 30.1	+09 02 25	43.0280	0.1400	G43.027+0.141	G43.0270+0.1410	IRAS 19071+0857	118	22 GHz;	-6.7	0.16	1.11	+H₂O -CH₃OH I	SFR_MIXED
22	19 21 25.1	+11 08 41	46.2559	-1.4764	G46.256-1.477	G46.2560-1.4773	IRAS 19190+1102	128	22 GHz;	0.2	1.54	10.71	+H₂O -CH₃OH I +OH	EVOLVED
23	01 46 35.3	+19 05 4.5	140.5437	-41.8933	G140.544-41.893	G140.5438-41.8933	SV Psc	10	22 GHz;	7.4	0.66	0.59	+H₂O -OH	EVOLVED
24	05 26 54.6	+36 54 11.2	171.1759	0.9871	G171.176+0.987	G171.1757+0.9869	W Aur	32	22 GHz;	-144.6	0.16	0.08	+H₂O -OH -SiO	EVOLVED
25	07 57 54.1	-20 25 43.3	238.6664	4.5502	G238.666+4.550	G238.6664+4.5502	V407 Pup	58	22 GHz;	-44.7	0.07	0.44	+H₂O	UNK
26	17 13 1.9	-10 34 42	11.5475	16.2901	G11.547+16.290	G11.5475+16.2901	IRC-10359	97	22 GHz;	-38.1	0.19	0.39	+H₂O -OH	EVOLVED

Non-detection table from Yoon et al. (2014)