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GOL17 - The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity

Short title: Goldman et al. (2017)
Authors: Goldman, Steven R.van Loon, Jacco Th.Zijlstra, Albert A.Green, James A.Wood, Peter R.Nanni, AmbraImai, HiroshiWhitelock, Patricia A.Matsuura, MikakoGroenewegen, Martin A. T.Gomez, Jose F.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 465, Issue 1, p.403-433
Bibcode:

Target type: star,Extragalactic
Transitions: OH_1612

Abstract
We present the results of our survey of 1612-MHz circumstellar OH maser emission from asymptotic giant branch (AGB) stars and red supergiants (RSGs) in the Large Magellanic Cloud (LMC). We have discovered four new circumstellar maser sources in the LMC, and increased the number of reliable wind speeds from infrared (IR) stars in the LMC from 5 to 13. Using our new wind speeds, as well as those from Galactic sources, we have derived an updated relation for dust-driven winds: vexp ~ ZL^0.4. We compare the subsolar metallicity LMC OH/IR stars with carefully selected samples of more metal-rich OH/IR stars, also at known distances, in the Galactic Centre and Galactic bulge. We derive pulsation periods for eight of the bulge stars for the first time by using near-IR photometry from the Vista Variables in the Via Lactea survey. We have modelled our LMC OH/IR stars and developed an empirical method of deriving gas-to-dust ratios and mass-loss rates by scaling the models to the results from maser profiles. We have done this also for samples in the Galactic Centre and bulge and derived a new mass-loss prescription which includes luminosity, pulsation period, and gas-to-dust ratio dot{M} = 1.06^{+3.5}_{-0.8} × }10^{-5 (L/10^4 L_{⊙})^{0.9± 0.1}(P/500 {d})^{0.75± 0.3} (r_gd/200)^{-0.03± 0.07}. The tightest correlation is found between mass-loss rate and luminosity. We find that the gas-to-dust ratio has little effect on the mass-loss of oxygen-rich AGB stars and RSGs within the Galaxy and the LMC. This suggests that the mass-loss of oxygen-rich AGB stars and RSGs is (nearly) independent of metallicity between a half and twice solar.

Abstract

We present the results of our survey of 1612-MHz circumstellar OH maser emission from asymptotic giant branch (AGB) stars and red supergiants (RSGs) in the Large Magellanic Cloud (LMC). We have discovered four new circumstellar maser sources in the LMC, and increased the number of reliable wind speeds from infrared (IR) stars in the LMC from 5 to 13. Using our new wind speeds, as well as those from Galactic sources, we have derived an updated relation for dust-driven winds: vexp ~ ZL^0.4. We compare the subsolar metallicity LMC OH/IR stars with carefully selected samples of more metal-rich OH/IR stars, also at known distances, in the Galactic Centre and Galactic bulge. We derive pulsation periods for eight of the bulge stars for the first time by using near-IR photometry from the Vista Variables in the Via Lactea survey. We have modelled our LMC OH/IR stars and developed an empirical method of deriving gas-to-dust ratios and mass-loss rates by scaling the models to the results from maser profiles. We have done this also for samples in the Galactic Centre and bulge and derived a new mass-loss prescription which includes luminosity, pulsation period, and gas-to-dust ratio dot{M} = 1.06^{+3.5}_{-0.8} × }10^{-5 (L/10^4 L_{⊙})^{0.9± 0.1}(P/500 {d})^{0.75± 0.3} (r_gd/200)^{-0.03± 0.07}. The tightest correlation is found between mass-loss rate and luminosity. We find that the gas-to-dust ratio has little effect on the mass-loss of oxygen-rich AGB stars and RSGs within the Galaxy and the LMC. This suggests that the mass-loss of oxygen-rich AGB stars and RSGs is (nearly) independent of metallicity between a half and twice solar.

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Detection table from Goldman et al. (2017)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	V_peak	F_peak	∫F dv	Telescope	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			(km/s)	(Jy)	(Jy*km/s)		(mJy)	(arcsec)	Yes/No		(kpc)
1	04 40 28.5	-69 55 14	281.9047	-36.4074	G281.905-36.407	IRAS 04407-7000	239.5 237		35.5	Parkes	5.900	720	+OH	EVOLVED		14-22 Aug 2003
	04 40 28.5	-69 55 14	281.9047	-36.4074	G281.905-36.407	IRAS 04407-7000	222.8	35.5		Parkes		720	+OH	EVOLVED		14-22 Aug 2003
	04 40 28.5	-69 55 14	281.9047	-36.4074	G281.905-36.407	IRAS 04407-7000	240 237		89.8	Parkes	8.800	720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	04 40 28.5	-69 55 14	281.9047	-36.4074	G281.905-36.407	IRAS 04407-7000	240 237		105.8	Combined	4.800		+OH	EVOLVED
	04 40 28.5	-69 55 14	281.9047	-36.4074	G281.905-36.407	IRAS 04407-7000	223	105.8		Combined			+OH	EVOLVED
6	04 49 41.5	-68 37 52	280.0574	-36.0800	G280.057-36.080	IRAS 04498-6842	272.3		44.5	ATCA	10.600	7	+OH	EVOLVED		6-8 Mar 2015
	04 49 41.5	-68 37 52	280.0574	-36.0800	G280.057-36.080	IRAS 04498-6842	246.3	44.5		ATCA		7	+OH	EVOLVED		6-8 Mar 2015
	04 49 41.5	-68 37 52	280.0574	-36.0800	G280.057-36.080	IRAS 04498-6842	272.3		6.4	Combined	6.300		+OH	EVOLVED
	04 49 41.5	-68 37 52	280.0574	-36.0800	G280.057-36.080	IRAS 04498-6842	246.3	6.4		Combined			+OH	EVOLVED
10	04 50 40.5	-69 17 32	280.7977	-35.7876	G280.798-35.788	IRAS 04509-6922	274.7		3.4	Parkes	10.100	720	+OH	EVOLVED		14-22 Aug 2003
	04 50 40.5	-69 17 32	280.7977	-35.7876	G280.798-35.788	IRAS 04509-6922	254.2	3.4		Parkes		720	+OH	EVOLVED		14-22 Aug 2003
	04 50 40.5	-69 17 32	280.7977	-35.7876	G280.798-35.788	IRAS 04509-6922	278.6		44.2	Parkes	3.900	720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	04 50 40.5	-69 17 32	280.7977	-35.7876	G280.798-35.788	IRAS 04509-6922	255.9	44.2		Parkes		720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	04 50 40.5	-69 17 32	280.7977	-35.7876	G280.798-35.788	IRAS 04509-6922	278.6		52.1	Combined	3.700		+OH	EVOLVED
	04 50 40.5	-69 17 32	280.7977	-35.7876	G280.798-35.788	IRAS 04509-6922	255	52.1		Combined			+OH	EVOLVED
16	04 51 29	-68 57 50	280.3855	-35.8223	G280.385-35.822	IRAS 04516-6902	287.3		16	Parkes	7.000	720	+OH	EVOLVED		14-22 Aug 2003
	04 51 29	-68 57 50	280.3855	-35.8223	G280.385-35.822	IRAS 04516-6902	287.3		30.6	ATCA	3.800	7	+OH	EVOLVED		6-8 Mar 2015
	04 51 29	-68 57 50	280.3855	-35.8223	G280.385-35.822	IRAS 04516-6902	287.1		30.4	Combined	3.400		+OH	EVOLVED
	04 51 29	-68 57 50	280.3855	-35.8223	G280.385-35.822	IRAS 04516-6902	267.1	30.4		Combined			+OH	EVOLVED
20	04 54 10.1	-69 55 58	281.4280	-35.2979	G281.428-35.298	IRAS 04545-7000	274			Parkes	6.100	720	+OH	EVOLVED		1992
	04 54 10.1	-69 55 58	281.4280	-35.2979	G281.428-35.298	IRAS 04545-7000	274		37.6	Parkes	6.100	720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	04 54 10.1	-69 55 58	281.4280	-35.2979	G281.428-35.298	IRAS 04545-7000	258.7	37.6		Parkes		720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	04 54 10.1	-69 55 58	281.4280	-35.2979	G281.428-35.298	IRAS 04545-7000	274		37.6	Combined	6.100		+OH	EVOLVED
	04 54 10.1	-69 55 58	281.4280	-35.2979	G281.428-35.298	IRAS 04545-7000	258.7	37.6		Combined			+OH	EVOLVED
25	04 55 10.5	-68 20 30	279.5301	-35.6877	G279.530-35.688	IRAS 04553-6825	281 300.90		11.7 8.2	Parkes	12.700	720	+OH	EVOLVED		14-22 Aug 2003
	04 55 10.5	-68 20 30	279.5301	-35.6877	G279.530-35.688	IRAS 04553-6825	253.4 263	11.7 8.2		Parkes		720	+OH	EVOLVED		14-22 Aug 2003
	04 55 10.5	-68 20 30	279.5301	-35.6877	G279.530-35.688	IRAS 04553-6825	281 300.90		74.1 52.6	Parkes	14.000	720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	04 55 10.5	-68 20 30	279.5301	-35.6877	G279.530-35.688	IRAS 04553-6825	253.4 263	74.1 52.6		Parkes		720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	04 55 10.5	-68 20 30	279.5301	-35.6877	G279.530-35.688	IRAS 04553-6825	281 300.90		32.3 21.9	Combined	9.800		+OH	EVOLVED
	04 55 10.5	-68 20 30	279.5301	-35.6877	G279.530-35.688	IRAS 04553-6825	253.4 263	32.3 21.9		Combined			+OH	EVOLVED
31	05 00 19	-67 07 58	277.9366	-35.5449	G277.937-35.545	IRAS 05003-6712	269.5			Parkes	6.700	720	+OH	EVOLVED		14-22 Aug 2003
	05 00 19	-67 07 58	277.9366	-35.5449	G277.937-35.545	IRAS 05003-6712	269.5			Parkes	5.800	720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	05 00 19	-67 07 58	277.9366	-35.5449	G277.937-35.545	IRAS 05003-6712	269.5			Combined	4.200		+OH	EVOLVED
34	05 27 40.1	-69 08 05	279.6638	-32.6416	G279.664-32.642	IRAS 05280-6910	289		398	Parkes	17.000	720	+H₂O +OH	EVOLVED		1992
	05 27 40.1	-69 08 05	279.6638	-32.6416	G279.664-32.642	IRAS 05280-6910	255	398		Parkes		720	+H₂O +OH	EVOLVED		1992
	05 27 40.1	-69 08 05	279.6638	-32.6416	G279.664-32.642	IRAS 05280-6910	292.6		147.3	ATCA	11.500	7	+H₂O +OH	EVOLVED		21-26 Feb 2016
	05 27 40.1	-69 08 05	279.6638	-32.6416	G279.664-32.642	IRAS 05280-6910	258.1	147.3		ATCA		7	+H₂O +OH	EVOLVED		21-26 Feb 2016
38	05 28 48.2	-71 02 29	281.8715	-32.2259	G281.872-32.226	IRAS 05294-7104	290.3		34.2	ATCA	5.500	7	+OH	SFR_MIXED		21-26 Feb 2016
	05 28 48.2	-71 02 29	281.8715	-32.2259	G281.872-32.226	IRAS 05294-7104	269.7	34.2		ATCA		7	+OH	SFR_MIXED		21-26 Feb 2016
40	05 29 24.6	-69 55 14	280.5544	-32.3649	G280.554-32.365	IRAS 05298-6957	292		448	Parkes	17.000	720	+OH	EVOLVED		1992
	05 29 24.6	-69 55 14	280.5544	-32.3649	G280.554-32.365	IRAS 05298-6957	271	448		Parkes		720	+OH	EVOLVED		1992
42	05 39 44.8	-69 55 18	280.4097	-31.4864	G280.410-31.486	IRAS 05402-6956	284		181	Parkes	17.000	720	+OH	EVOLVED		1992
	05 39 44.8	-69 55 18	280.4097	-31.4864	G280.410-31.486	IRAS 05402-6956	263	181		Parkes		720	+OH	EVOLVED		1992
44	05 55 21	-70 00 03	280.3675	-30.1481	G280.368-30.148	IRAS 05558-7000	281.5		11.7	Parkes	5.700	720	+OH	EVOLVED		14-22 Aug 2003
	05 55 21	-70 00 03	280.3675	-30.1481	G280.368-30.148	IRAS 05558-7000	265	11.7		Parkes		720	+OH	EVOLVED		14-22 Aug 2003
	05 55 21	-70 00 03	280.3675	-30.1481	G280.368-30.148	IRAS 05558-7000	281.5		52.5	Parkes	5.900	720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	05 55 21	-70 00 03	280.3675	-30.1481	G280.368-30.148	IRAS 05558-7000	265	52.5		Parkes		720	+OH	EVOLVED		8 Jul - 22 Aug 2005
	05 55 21	-70 00 03	280.3675	-30.1481	G280.368-30.148	IRAS 05558-7000	281.5		51	Combined	4.100		+OH	EVOLVED
	05 55 21	-70 00 03	280.3675	-30.1481	G280.368-30.148	IRAS 05558-7000	265	51		Combined			+OH	EVOLVED
50	05 32 37.2	-67 06 56	277.2156	-32.4651	G277.216-32.465	MSX LMC 807	322.7		12.1	ATCA	4.600	7	+OH	EVOLVED		6-8 Mar 2015
	05 32 37.2	-67 06 56	277.2156	-32.4651	G277.216-32.465	MSX LMC 807	306.4	12.1		ATCA		7	+OH	EVOLVED		6-8 Mar 2015
52	05 32 51.3	-67 06 52	277.2111	-32.4425	G277.211-32.443	MSX LMC 811	318.9		188	ATCA	4.300	7	+OH	EVOLVED		6-8 Mar 2015
	05 32 51.3	-67 06 52	277.2111	-32.4425	G277.211-32.443	MSX LMC 811	302.4	188		ATCA		7	+OH	EVOLVED		6-8 Mar 2015

Non-detection table from Goldman et al. (2017)