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DAV08 - The Cool Supergiant Population of the Massive Young Star Cluster RSGC1

Short title: Davies et al. (2008)
Authors: Davies, Ben Figer, Don F. Law, Casey J. Kudritzki, Rolf-Peter Najarro, Francisco Herrero, Artemio MacKenty, John W.
Journal: The Astrophysical Journal, Volume 676, Issue 2, article id. 1016-1028, pp. (2008).
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Detection table: Show detection table (1 detection) Non-detection table: Show non-detection table (16 non-detection)

Abstract
We present new high-resolution near-IR spectroscopy and OH maser observations to investigate the population of cool luminous stars of the young massive Galactic cluster RSGC1. Using the 2.293 mum CO band-head feature, we make high-precision radial velocity measurements of 16 of the 17 candidate red supergiants (RSGs) identified by Figer et al. We show that F16 and F17 are foreground stars, while we confirm that the rest are indeed physically associated RSGs. We determine that star F15, also associated with the cluster, is a yellow hypergiant based on its luminosity and spectroscopic similarity to rho Cas. Using the cluster's radial velocity, we have derived the kinematic distance to the cluster and revisited the stars' temperatures and luminosities. We find a larger spread of luminosities than in the discovery paper, consistent with a cluster age 30% older than previously thought (12 +/- 2 Myr), and a total initial mass of (3 +/- 1) � 10⁴ M_&sun. The spatial coincidence of the OH maser with F13, combined with similar radial velocities, is compelling evidence that the two are related. Combining our results with recent SiO and H₂O maser observations, we find that those stars with maser emission are the most luminous in the cluster. From this we suggest that the maser active phase is associated with the end of the RSG stage, when the luminosity-mass ratios are at their highest. eprintid: arXiv:0711.4757

Abstract

We present new high-resolution near-IR spectroscopy and OH maser observations to investigate the population of cool luminous stars of the young massive Galactic cluster RSGC1. Using the 2.293 mum CO band-head feature, we make high-precision radial velocity measurements of 16 of the 17 candidate red supergiants (RSGs) identified by Figer et al. We show that F16 and F17 are foreground stars, while we confirm that the rest are indeed physically associated RSGs. We determine that star F15, also associated with the cluster, is a yellow hypergiant based on its luminosity and spectroscopic similarity to rho Cas. Using the cluster's radial velocity, we have derived the kinematic distance to the cluster and revisited the stars' temperatures and luminosities. We find a larger spread of luminosities than in the discovery paper, consistent with a cluster age 30% older than previously thought (12 +/- 2 Myr), and a total initial mass of (3 +/- 1) � 10⁴ M_&sun. The spatial coincidence of the OH maser with F13, combined with similar radial velocities, is compelling evidence that the two are related. Combining our results with recent SiO and H₂O maser observations, we find that those stars with maser emission are the most luminous in the cluster. From this we suggest that the maser active phase is associated with the end of the RSG stage, when the luminosity-mass ratios are at their highest. eprintid:

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Detection table from Davies et al. (2008)

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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	18 37 58.9	-06 52 32.1	25.2826	-0.1569	G25.279-0.153	F13	1612	34.3	103.8	0.090	ENG15	-H₂O +OH +SiO	EVOLVED		DAV08

Non-detection table from Davies et al. (2008)

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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	18 38 1.3	-06 52 52	25.2823	-0.1683	G25.279-0.153	F16	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
2	18 37 48.8	-06 53 7.7	25.2546	-0.1242	G25.254-0.124	F17	1.612 GHz;	0.012	ENG15	-OH +SiO	EVOLVED	DAV08
3	18 37 47.6	-06 53 2.3	25.2538	-0.1193	G25.254-0.124	F14	1.612 GHz;	0.012	ENG15	-OH +SiO	EVOLVED	DAV08
4	18 37 57.8	-06 52 32	25.2805	-0.1528	G25.279-0.153	F15	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
5	18 37 59.5	-06 53 31.9	25.2691	-0.1668	G25.279-0.153	F10	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
6	18 37 51.7	-06 51 49.9	25.2794	-0.1251	G25.279-0.153	F11	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
7	18 38 3.3	-06 52 45.1	25.2878	-0.1747	G25.279-0.153	F12	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
8	18 37 57.8	-06 52 22.2	25.2829	-0.1515	G25.279-0.153	F09	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
9	18 37 57.5	-06 53 25.3	25.2667	-0.1584	G25.279-0.153	F06	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
10	18 37 54.3	-06 52 34.7	25.2733	-0.1404	G25.279-0.153	F07	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
11	18 37 56.3	-06 52 32.2	25.2776	-0.1473	G25.279-0.153	F01	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
12	18 37 55.3	-06 52 48.4	25.2717	-0.1457	G25.279-0.153	F02	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
13	18 37 59.7	-06 53 49.4	25.2651	-0.1698	G25.279-0.153	F03	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
14	18 37 50.9	-06 53 38.2	25.2511	-0.1359	G25.254-0.124	F04	1.612 GHz;	0.012	ENG15	-OH +SiO	EVOLVED	DAV08
15	18 37 55.5	-06 52 12.2	25.2811	-0.1419	G25.279-0.153	F05	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08
16	18 37 55.2	-06 52 10.7	25.2809	-0.1405	G25.279-0.153	F08	1.612 GHz;	0.012	ENG15	-H₂O +OH +SiO	EVOLVED	DAV08

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 DAV08

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