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SZY95B - A search for observational evidence of OH molecule photoproduction

Short title: Szymczak & Le Squeren (1995B)
Authors: Szymczak, M. Le Squeren, A. M.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 276, Issue 2, pp. 635-639.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (7 detection) Non-detection table: Show non-detection table (18 non-detection)

Abstract
Observational evidence for OH molecule photoproduction by the interstellar UV radiation in the circumstellar envelopes of Mira variables has been searched for. A sample of Me-type Miras was observed in the main OH maser lines with the Nancay radio telescope. Two new lines were detected. The intensity of the 156.5-nm wavelength interstellar radiation is estimated by integration of the observed UV light of OB stars in common star catalogues. A statistically significant trend is found that OH Miras are illuminated by stronger UV fields than non-OH objects.	Comments: Velocity resolution: 0.28 km/s Upper limit for non-detections: 0.15 Jy (3σ)

Abstract

Observational evidence for OH molecule photoproduction by the interstellar UV radiation in the circumstellar envelopes of Mira variables has been searched for. A sample of Me-type Miras was observed in the main OH maser lines with the Nancay radio telescope. Two new lines were detected. The intensity of the 156.5-nm wavelength interstellar radiation is estimated by integration of the observed UV light of OB stars in common star catalogues. A statistically significant trend is found that OH Miras are illuminated by stronger UV fields than non-OH objects.

Comments:
Velocity resolution: 0.28 km/s
Upper limit for non-detections: 0.15 Jy (3σ)

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Detection table from Szymczak & Le Squeren (1995B)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Frequency	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(MHz)	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	04 38 14.6	+08 20 9.2	188.4411	-24.6667	G188.441-24.667	RX Tau	1665	48.4	-48.4	0.310	ENG15	+H₂O -CH₃OH II +OH +SiO	EVOLVED		SZY95B
	04 38 14.6	+08 20 9.2	188.4411	-24.6667	G188.441-24.667	RX Tau	1667	48.3	-48.3	0.350	ENG15	+H₂O -CH₃OH II +OH +SiO	EVOLVED		SZY95B
3	05 46 56.3	-31 41 28.4	236.6888	-26.7352	G236.689-26.735	S Col	1665	62.7	62.7	0.180	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95B
	05 46 56.3	-31 41 28.4	236.6888	-26.7352	G236.689-26.735	S Col	1667	65.0	65.0	0.310	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95B
5	09 35 30.3	-14 41 28.6	248.1490	26.7014	G248.149+26.701	X Hya	1667	4.6	24.1	0.080	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95B
6	15 29 34.6	+78 38 0.3	114.0547	35.6138	G114.055+35.614	S UMi	1665	0.3	-42.4	0.220	ENG15	-H₂O -CH₃OH II +OH +SiO	EVOLVED		SZY95B
7	21 09 31.8	+68 29 27.2	104.8051	13.8449	G104.805+13.845	T Cep	1665	4.0	-4.0	0.260	ENG15	+H₂O +OH +SiO	EVOLVED		SZY95B

Non-detection table from Szymczak & Le Squeren (1995B)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	F_peak	List	Detection	Class	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			OH	(Jy)		Yes/No
1	04 38 14.6	+08 20 9.2	188.4411	-24.6667	G188.441-24.667	RX Tau	1.612 GHz;	0.070	ENG15	+H₂O -CH₃OH II +OH +SiO	EVOLVED	SZY95B
2	08 16 33.8	+11 43 34.5	211.7494	24.1390	G211.749+24.139	R Cnc	1.665 GHz;	0.060	ENG15	+H₂O +OH +SiO	EVOLVED	SZY95B
3	08 16 33.8	+11 43 34.5	211.7494	24.1390	G211.749+24.139	R Cnc	1.667 GHz;	0.060	ENG15	+H₂O +OH +SiO	EVOLVED	SZY95B
4	09 35 30.3	-14 41 28.6	248.1490	26.7014	G248.149+26.701	X Hya	1.665 GHz;	0.360	ENG15	+H₂O +OH +SiO	EVOLVED	SZY95B
5	15 29 34.6	+78 38 0.3	114.0547	35.6138	G114.055+35.614	S UMi	1.667 GHz;	0.150	ENG15	-H₂O -CH₃OH II +OH +SiO	EVOLVED	SZY95B
6	19 55 56.4	-29 11 24.1	11.8391	-25.9881	G11.839-25.988	RR Sgr	1.665 GHz;	0.060	ENG15	+H₂O -CH₃OH II -OH	EVOLVED	SZY95B
7	19 55 56.4	-29 11 24.1	11.8391	-25.9881	G11.839-25.988	RR Sgr	1.667 GHz;	0.090	ENG15	+H₂O -CH₃OH II -OH	EVOLVED	SZY95B
8	21 09 31.8	+68 29 27.2	104.8051	13.8449	G104.805+13.845	T Cep	1.667 GHz;	0.100	ENG15	+H₂O +OH +SiO	EVOLVED	SZY95B
9	00 15 22.3	-32 02 43	358.6702	-80.7505	G358.670-80.750	S Scl	1.665 GHz;	0.090	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
10	00 15 22.3	-32 02 43	358.6702	-80.7505	G358.670-80.750	S Scl	1.667 GHz;	0.090	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
11	00 23 14.3	+55 47 33.2	118.9467	-6.8608	G118.947-6.861	T Cas	1.665 GHz;	0.110	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
12	00 23 14.3	+55 47 33.2	118.9467	-6.8608	G118.947-6.861	T Cas	1.667 GHz;	0.100	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
13	05 17 17.7	+53 35 10	156.3659	8.9741	G156.366+8.974	R Aur	1.665 GHz;	0.080	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
14	05 17 17.7	+53 35 10	156.3659	8.9741	G156.366+8.974	R Aur	1.667 GHz;	0.080	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
15	07 32 43.1	+08 19 5.2	210.1134	12.9280	G210.113+12.928	S CMi	1.665 GHz;	0.060	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
16	07 32 43.1	+08 19 5.2	210.1134	12.9280	G210.113+12.928	S CMi	1.667 GHz;	0.060	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
17	13 48 57	+39 32 33.2	82.6559	72.7697	G82.656+72.770	R CVn	1.665 GHz;	0.060	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B
18	13 48 57	+39 32 33.2	82.6559	72.7697	G82.656+72.770	R CVn	1.667 GHz;	0.060	ENG15	-H₂O -OH +SiO	EVOLVED	SZY95B

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from SZY95B

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