Free Access
Issue
A&A
Volume 541, May 2012
Article Number A36
Number of page(s) 12
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201118265
Published online 24 April 2012

© ESO, 2012

1. Introduction

Near the end of their lifetimes, stars of moderately high mass (10 M  < M <  30 M) go through the red supergiant evolutionary phase. Red supergiants (RSGs) are burning helium in their core, have luminosities more than 105 times that of the Sun and, since their effective temperature is low (~3000−4000 K), are intrinsically luminous in the near-infrared range (Levesque 2010). Studying RSGs and, in particular, their mass-loss history, is important for several reasons. Given their luminosities, RSGs may be recognized as individual objects in external galaxies and serve as tracers of young populations and as distance indicators. They contribute to the enrichment of the interstellar medium by losing mass at a high rate (up to several times 10-4   M yr-1), and by eventually exploding as core-collapse supernovae. RSG stars are often surrounded by circumstellar envelopes (CSEs). Maser emission may arise from these envelopes, revealing stellar line-of-sight velocities to within a few km s-1 (Jewell et al. 1991). Frequently detected maser lines are from OH at 1.612 GHz, H2O at 22.2 GHz, and silicon monoxide (SiO) at 43 GHz and 86 GHz. At higher frequencies, also a number of (sub)millimeter transitions have been detected (see, e.g. Humphreys 2007; Menten et al. 2008).

Some fundamental issues limit the use of RSGs as well-calibrated tracers of young stellar populations. We know only about 500 RSGs (e.g. Messineo et al. 2012; Figer et al. 2006; Davies et al. 2007), and their properties (stellar and circumstellar) are still poorly understood. Interstellar extinction and poor knowledge on stellar distances render the identification of RSGs difficult. Important open questions are those of the relations (i) between the maximum luminosity of a given star and its main-sequence mass and (ii) between mass-loss rate, , and stellar luminosity, L and initial metallicity, Z. Possible stellar rotation complicates these relations (Meynet & Maeder 2000). Periodic stellar light variations and circumstellar extinction make it difficult to distinguish between massive RSGs and intermediate age mass-losing late-type stars (Comerón et al. 2004; Messineo et al. 2005, 2012).

All these uncertainties limit our understanding of these stars’ CSEs. In particular, it is unclear why some stars exhibit maser emission in a certain species and others don’t. Maser occurrence is certainly not only a function of envelope temperature and mass-loss rate alone; other parameters, like elemental abundances and stellar luminosity may play an important role (Habing 1996).

Large-scale searches for maser emission toward evolved late-type stars (mostly Mira-type long period variables and OH/IR stars) have been carried out, successfully yielding radial velocity measurements, and new views on the structure of the Milky Way, in particular on its bar and bulge (Sevenster 1999; Deguchi et al. 2002; Habing et al. 2006). The power of velocity determinations via observations of SiO maser lines was demonstrated by Messineo et al. (2002, 2004, 2005) and Habing et al. (2006), who used the IRAM 30 m telescope to find 86 GHz SiO maser emission toward 271 color-selected AGB stars in the Inner Galaxy with a detection rate higher than 60%. With ages of up to a few tens of Myr, the much younger RSGs, on the other hand, are found in the general vicinity of their birth places.

Recently, trigonometric parallaxes of maser sources in star-forming regions and toward a few RSGs located in the spiral arms of the Milky Way have been measured with the NRAO Very Long Baseline Array (VLBA) and VLBI Exploration of Radio Astrometry (VERA) with a precision of 10%. These accurate distances are leading to a revised view of Galactic structure (Reid et al. 2009; Choi et al. 2008; Asaki et al. 2010). RSGs are found in the spiral arms and their associated masers are thus excellent potential targets for such studies. In fact, one purpose of the present work is to increase the number of RSG/SiO maser sources suitable for Very Long Baseline Interferometry (VLBI).

In order to use RSGs as kinematic probes, it is necessary to significantly increase the number of such objects with known associated maser emission. Strong masers (with hundreds to  > thousand Jy intensities) were first detected in nearby “classical” OH/IR RSGs (VY CMa, VX Sgr, NML Cyg, and also S Per) in the early 1970s (Buhl et al. 1974; Kaifu et al. 1975). Searches for RSG masers in the far reaches of the Galaxy require sensitive searches with few- to even sub-Jy sensitivity.

In this paper, we present a search for 86 GHz SiO maser emission toward 88 known RSG stars associated with open clusters.

In Sect. 2, we report recent discoveries of massive clusters that have RSGs amongst their members (the so named RSG clusters, RSGCs), and in Sect. 3 give a brief summary of SiO maser emission and the motivation for its study. The observations are described in Sect. 4. General results are presented in Sect. 5, discussed, cluster by cluster, in Sect. 6 and analyzed in Sect. 7. Some conclusions are presented in Sect. 8.

2. Red supergiants in stellar clusters

Ideally, one wishes to observe RSG stars in clusters, because membership in a stellar cluster guarantees similar distance, age and metallicity for all its constituents, including the RSGs. The RSGs’ distinct properties, compared to other cluster members, will thus only depend on its large initial masses. Due to the steepness of the initial mass function stellar clusters rich in RSGs must naturally be very massive, and have an age from about 5 to 30 Myr (Meynet & Maeder 2000).

Only 15 massive clusters (mass  > 104 M) are currently known in the Milky Way (the most recently found ones reported by Messineo et al. 2009; Negueruela et al. 2010, 2011; Messineo et al. 2012). They are all located at the near-side of the Galaxy, suggesting that their census is highly incomplete (Messineo et al. 2009). A few clusters e.g., the Westerlund I, Arches, and Quintuplet clusters (Westerlund 1961; Cotera et al. 1996; Figer et al. 1999, 2002, 2004; Clark et al. 2005) were known to be massive since the 1990s or even earlier and have been studied at various wavelengths. However, the Arches and the Quintuplet may not be representative of massive clusters elsewhere in the Milky Way because of the peculiar physical conditions in the Galactic center region. Thanks to the new generation of near- and mid-infrared surveys (e.g. DENIS, 2MASS, GLIMPSE, Epchtein et al. 1999; Cutri et al. 2003; Benjamin et al. 2003), recently several more massive Galactic stellar clusters containing RSGs have been discovered around l ~ 25°, at the base of the Scutum-Crux arm. In the red supergiant cluster 1 (RSGC1) a total of 14 RSGs have been spectroscopically confirmed (Figer et al. 2006; Davies et al. 2008). Only a few hundred parsecs from the RSGC1, another massive cluster was found. RSGC2, also called the Stephenson 2 cluster (Stephenson 1990), contains 26 RSGs (Davies et al. 2007). A nearby third massive cluster (RSGC3) with 16 RSGs was discovered by Clark et al. (2009) and Alexander et al. (2009). Recently, two other clusters rich of RSGs were identified in the same direction (Negueruela et al. 2010, 2011). The Alicante 8 or RSGC4 contains 13 candidate RSG members, while the RSGC5 cluster contains seven RSGs. Since the latter two clusters were not yet discovered at the time of the observations presented in this paper, they were not considered in our search. The total number of confirmed RSG stars in these five clusters amounts to 64, increasing the number of known RSGs by at least 15%. Before this, only the NGC 7419 cluster was known to contain five RSGs (Beauchamp et al. 1994; Caron et al. 2003). All five RSGCs are concentrated within a few degrees of longitude (25° < l < 29°), likely at similar distance (5−6 kpc). The location of this remarkable burst of star formation coincides with the near endpoint of the Galactic bar (Davies et al. 2009b), where also the W43 “mini starburst” region is found (Nguyen Luong et al. 2011). These clusters offer an extraordinarily important natural laboratory in which to study the evolution of RSGs and the properties of their envelopes. Altogether, we now have a sample of more than 119 Galactic RSGs in clusters at our disposal (Messineo et al. 2012). Here we present a search for 86 GHz SiO maser emission toward RSG stars.

The RSGCs are at distances of approximately 3.5 kpc from the Galactic center, all are at kinematically interesting locations, namely at the corotation radius of the Galactic bar (Habing et al. 2006), at the base of the Scutum-Crux arm, or near an endpoint of the Galactic bar. Studies of their properties and kinematics, e.g. via SiO maser emission, will place constraints on Galactic structure and evolution models and address, e.g., questions how the Galactic bar and the spiral arms are dynamically related, which is still unclear (Bissantz et al. 2003).

3. SiO masers in RSGs

Analysis of existing photometric data (from the 2MASS, MSX, Spitzer/GLIMPSE databases) has shown that many RSGs show infrared excesses, caused by their CSEs, and therefore high mass-loss rates (e.g. Figer et al. 2006; Davies et al. 2007). Typical mass-loss rates range from 10-8 to 10-4  per year (Verhoelst et al. 2009; Harwit et al. 2001). This makes them likely to exhibit maser emission, as, e.g., the SiO maser flux is known to correlate with the mid-infrared continuum flux density see Sect. 3.1. Most commonly, RSGs show maser emission from OH (at 1.612 GHz), H2O (22 GHz) and SiO (43 GHz and 86 GHz) (see e.g. Habing 1996). In this paper, we will focus on the 86 GHz SiO (v = 1,J = 2−1) maser line.

3.1. SiO maser pumping

The pumping mechanism for SiO masers is still under debate. Both radiative and collisional pumping models have been proposed. The basic mechanism for SiO maser pumping is described by Kwan & Scoville (1974). They find that SiO population inversions can occur when vibrational transitions become optically thick. Namely, in this case the vibrational de-excitation rates will be modified in such way that they decrease with increasing rotational level J. The logical result is an overpopulation of higher J rotational levels, thus an inversion, as long as the pumping happens by collisions or an indirect radiative route.

Models favoring either collisional or radiative pumping have been proposed by a number of authors. A mechanism for pumping through collisions with H2 molecules was first presented by Elitzur (1980). Further modeling by, e.g., Lockett & Elitzur (1992) and Humphreys et al. (2002) also supported collisional pumping as the primary pumping mechanism for SiO masers. On the other hand, contrasting studies find radiative pumping to be dominant (e.g. Bujarrabal et al. 1987; Bujarrabal 1994a,b). From the observational point of view, a radiative pumping model explains the observed correlation between SiO maser intensity and the infrared emission (e.g. Bujarrabal et al. 1987), while the dependence on stellar pulsations could be explained by collisional pumping (e.g. Heske 1989). The above models find that radiative pumping requires that the infrared (IR) flux at 8   μm (the equivalent wavelength of the first excited rotational level of SiO) is greater than the flux of the maser line.

3.2. Importance of SiO maser studies: obtaining accurate velocities

To summarize the above: Finding new SiO maser-hosting RSGs associated with stellar clusters, i.e., of stars in environments of similar age, metallicity, distance and interstellar extinction is useful for analyzing the occurrence of SiO maser emission in RSGs, as a function of their luminosities and mass-loss rates (Davies et al. 2008). Very importantly, maser lines provide accurate radial velocities; the midpoint of an SiO maser spectrum gives the stellar velocity with an accuracy of a few km s-1 (Jewell et al. 1991). In contrast, radial velocities from infrared CO absorption at 2.29 μm in Mira stars may vary with the stellar pulsation up to 15 km s-1 (Scholz & Wood 2000). We note, however, that for the RSGs for which we have both maser and CO absorption LSR velocity measurements, both values are quite similar; see Table 5.

With accurate radial velocities of cluster members a determination of dynamical cluster masses is possible. Furthermore, they allow a determination of kinematic distances. However, such distances are based on models of Galactic rotation, i.e., only meaningful outside of the corotation radius and may be wrong due to peculiar motions (see, e.g., Xu et al. 2006). Given all this, a main motivation for this work is to find new samples of RSGs with SiO maser emission whose distances can be studied with VLBI. The distances thus obtainable, typically with uncertainties of 10% at 10 kpc, will greatly improve our knowledge of massive cluster properties and place more stringent constraints on Galactic structure.

4. Observations

4.1. Pico Veleta observations

We observed the SiO v = 1, J = 2−1 maser transition at 86.24335 GHz in 88 sources with the IRAM 30-m telescope on Pico Veleta, Spain, during 3 epochs in 2006 September/October and 2008 May and August (Table 1). The A100 and B100 receivers were used, connected to the 256-channel low (1 MHz) resolution filterbank with 3.5 km s-1 spectral resolution, as well as the VESPA autocorrelator with 240 MHz bandwidth (1600 km s-1) and a resolution of 40 kHz, corresponding to an adequate 0.14 km s-1. We used a total power observing mode with integration times between 5 and 15 minutes per source, employing wobbler switching with a wobbler throw of 100′′ − 120′′. This gives an rms noise around 20–65 mK in a corrected antenna temperature, , scale, equivalent to 0.12−0.54 Jy, assuming a conversion factor from antenna temperature to flux density of 6 Jy/K. The system temperatures ranged from 90 to 300 K. We conducted telescope pointing checks every 1.5 − 3 h and, based on these, estimate that pointing errors are smaller than 3′′, much smaller than the 29′′ FWHM beam width.

4.2. Data reduction

We reduced the data with the CLASS program, which is part of the GILDAS software package1. Special attention was paid to the possible confusion with the interstellar H13CN J = 1−0 line, which has 3 hyperfine transitions in the 240 MHz VESPA band (Messineo et al. 2002). We detected the H13CN line in all of the Galactic center sources from the Blum et al. (2003) sample.

Table 1

IRAM 30 m observing dates.

4.3. Target stars

The targets of our 86 GHz observations are late-type stars that are located mostly in the directions of massive clusters containing confirmed or candidate RSGs. Our sample is presented, with the outcome of our observations in Tables 2 and 3. Table 2 gives the coordinates of the targets toward which an SiO maser was detected and the line parameters (peak flux density, rms noise, peak local standard of rest (LSR) velocity, velocity range of maser emission, and velocity-integrated flux). Table 3 reports the coordinates of the targets not detected as well as the rms noise (1σ) of the spectra. Several of our target RSGs have already been found to show SiO maser action in the v = 1 and/or 2, J = 1−0 lines at 43 GHz (e.g. Nakashima & Deguchi 2006), as well as the 86 GHz v = 1,J = 2−1 line (Haikala et al. 1994) or the 43 GHz lines and the 86 GHz line2 (Deguchi et al. 2010). Since SiO maser emission is often variable (e.g. Alcolea et al. 1990, 1999), a second epoch of observations may reveal new sources as maser emitters even if previous searches had shown negative results.

Table 2

SiO v = 1; J = 2−1 detections toward RSGs.

Table 3

Red supergiants without SiO v = 1; J = 2 − 1 detection.

thumbnail Fig. 1

Spectra of the SiO v = 1, J = 2−1 transition toward the stars where the line was detected. All stars but X 18, U Her, and IK Tau are RSGs. The latter two are Mira variables and we show their much narrower spectra for comparison.

Open with DEXTER

5. General results

We searched 88 (candidate) RSGs for 86 GHz SiO maser emission. We have detected SiO maser emission from RSGs in the RSGC1 and RSGC2, NGC 7419, GLIMPSE13, and Trumpler 27 clusters, and from two RSGs in the Perseus OB1 association, S Per, and W Per, which were already known to host SiO masers (Kaifu et al. 1975; Jiang et al. 1996). In total, 13 out of the 88 observed RSGs were found to exhibit SiO maser emission in the v = 1,J = 2−1 transition at 86 GHz.

All spectra are presented in Fig. 1 and the observed line parameter are listed in Table 2. The columns specify the RSG’s name (taken from SIMBAD3), its position by right ascension (αJ 2000) and declination (δJ 2000), the peak flux density (S, in Jy), the rms noise (rms, in Jy), the LSR velocity of the peak flux density (vLSR, in km s-1), the LSR velocity range covered by the maser emission (v-range, in km s-1), the velocity-integrated flux density (∫S dv, in Jy km s-1), and a reference number. Table 3 lists upper limits for sources toward which no maser emission was found. The columns specify the RSG’s name (taken from SIMBAD), its position by right ascension (αJ 2000) and declination (δJ 2000), and the rms noise (rms, in Jy).

Toward several of the 13 sources in which we detect SiO maser emission SiO, OH and/or H2O masers had been found previously. For these, Table 4 gives an overview of all the maser detections.

Table 4

Previous maser observations.

Table 5

Comparison between RSG LSR velocities determined from SiO maser emission and IR CO absorption.

6. Results on individual clusters

In the following we discuss our targets and our observations cluster by cluster.

6.1. RSGC1

Figer et al. (2006) reported on a cluster containing 14 RSGs, the RSGC1 located at . High-resolution near-infrared spectroscopy confirmed their memberships (Davies et al. 2008). The 14 RSG stars have spectral types between K2 and M6. The mean radial velocity of the stars is 123.0 ± 1.0 km s-1, while the velocity dispersion is 3.7 km s-1, which yields a dynamical mass of a few times 104 M. With the derived kinematic distance of 6.6  ±  0.9 kpc, Davies et al. (2008) estimated luminosities log (L/L) from 4.87 to 5.45, which are consistent with a cluster age of 12 ± 2 Myr and initial masses of 18 M. We observed 8 of the 14 RSGs, for which we use the identification numbers introduced by Davies et al. (2008). We also included the nearby source X 18. This bright mid-infrared source was suggested to be a cluster member and possibly associated with the X-ray emitter AX J1838.0-0655 by Figer et al. (2006). Toward this source, located 2′ south of the cluster, SiO emission was found by Nakashima & Deguchi (2006, see below). A radial velocity of 74 km s-1, significantly lower than that of the stellar cluster, however, suggests non-membership (Nakashima & Deguchi 2006). Nakashima & Deguchi (2006) already searched for the SiO v = 1 and v = 2, J = 1−0 transitions at 43 GHz in the RSGs of RSGC1. They detected maser emission from four of the 14 RSGs: FMR2006 1, FMR2006 2, FMR2006 4, and FMR2006 13. Only the latter was detected in both transitions, the other three objects only showed the v = 1 line. Additionally, in a follow-up observation the 86 GHz v = 1,J = 2−1 SiO maser line was detected in FMR2006 1 and FMR2006 2. On top of that, Nakashima & Deguchi (2006) also found emission from both the v = 1 and v = 2 transitions toward X 18.

We detected 5 SiO masers in the direction of the RSGC1. We detected the v = 1, J = 2−1 transitions toward those objects found masing in the J = 1−0 lines by Nakashima & Deguchi (2006), except for FMR2006 2, which we did not observe (see Table 2). In addition, we made an additional detection, toward FMR2006 3. Our LSR velocities compare well with the values determined by Nakashima & Deguchi (2006).

We detected SiO maser emission toward X 18 with a velocity of 71 km s-1 (see Table 2), which makes its cluster membership highly unlikely. This value is in agreement with that measured at 43 GHz, i.e., 30 km s-1 below the average cluster velocity. Were the maser star in a binary system, its velocity could deviate from the average cluster velocity. However, the agreement between the two radial velocities taken at two different epochs appears to discard this hypothesis. Nevertheless, it is tempting to speculate that X 18 is a higher energy version of the famous R Aqr symbiotic binary system. This system consists of an M-type AGB star and a compact object, most likely a white dwarf. It hosts a strong SiO maser (Zuckerman 1979) and shows radio and ultraviolet emission but, in contrast to X 18, is not very luminous in X rays (Viotti et al. 1987; Kafatos et al. 1989; Kellogg et al. 2007).

6.2. RSGC2

The RSGC2 was detected by Davies et al. (2007) as an overdensity of bright infrared stars in GLIMPSE and MSX images at . Remarkably, a total of 26 cluster members are spectroscopically confirmed RSG stars (Davies et al. 2007) and have spectral types from K2 to M5. In order to host such a large number of RSGs implies a mass of 4 × 104 M for this cluster. From the average radial velocity (109.3 ± 0.7 km s-1) a kinematic distance of kpc is inferred. By assuming this distance, and using theoretical models from Meynet & Maeder (2000), the authors derived a likely cluster age of 17 ± 3 Myr (or 12 ± 1 when considering non-rotating isochrones). Luminosities log (L/L) of the RSGs range from 4.4 to 5.4, suggesting initial stellar masses of about 15 M (Meynet & Maeder 2000). All 26 RSGs were included in our SiO maser search program. We used the identification numbers given by Davies et al. (2007). We also included star number one, which has been classified as a candidate RSG star in the foreground of the cluster because of its brightness (KS = 2.9 mag) and radial velocity ~95 km s-1 (Davies et al. 2007).

Recently, Deguchi et al. (2010) conducted an SiO v = 1 and v = 2, J = 1−0 maser search at 43 GHz in 18 objects of the RSGC2 cluster, resulting in five detections. Stephenson 2 DFK 1 and DFK 2 were detected only in the v = 1 transition, while DFK 22, DFK 49 and 2MASS J18385699-0606459 showed maser emission in both the v = 1 and v = 2 lines.

We detected three of the objects toward which Deguchi et al. (2010) found maser emission in the 43 GHz J = 1−0 lines: Stephenson 2 DFK 1, DFK 2 and DFK 49. The LSR velocities derived from the 43 GHz maser lines are within a few km s-1 of the values we determine for the J = 2 − 1 line, see Table 5. We note that star number 1, which has a significantly different velocity than the other two, is likely a field RSG, not associated with RSGC2 (Davies et al. 2007).

6.3. RSGC3

The RSGC3 was identified by Clark et al. (2009). It contains 8 RSGs with spectral types from K3 to M4, and 8 other candidate RSGs on the basis of photometric information. The number of RSGs suggests a cluster mass of about 2 × 104 M − 4 × 104 M. The values of log (L/L) range from 4.5 and 4.8 when assuming a distance of 6 kpc, and suggest initial masses similar to those of the RSGs in RSGC2.

The target selection and IRAM observations presented here were carried out before completion of the analysis of Clark et al. (2009). The 8 spectroscopically confirmed RSGs and one of the candidate RSG were unsuccessfully searched for SiO masers. For those stars, we use the identification numbers given by Clark et al. (2009). Our list includes also 2MASS J18452254-0322261, which is not listed among the stellar members by Clark et al. (2009).

6.4. NGC 7419

Before the discovery of the RSGCs, the NGC 7419 cluster was the cluster with the largest number of known RSGs (Caron et al. 2003). The cluster is located at at a photometric distance of 2.3 ± 0.3 kpc (Beauchamp et al. 1994; Caron et al. 2003), and has an age of 25 ± 5 Myr (Subramaniam et al. 2006). Its four RSG members have spectral types from M2.5 to M7.5. We list these RSGs with the names provided in the SIMBAD database. The RSG MY Cep has already been detected in several maser surveys. It shows SiO, OH, and water masers (Nakashima & Deguchi 2007; Sivagnanam et al. 1990; Takaba et al. 2001).

We only found maser emission at 86 GHz toward the brightest member of the NGC 7419 cluster, the M7.5 star MY Cep. SiO Maser emission at 43 GHz had been detected before by Nakashima & Deguchi (2007). They derived a radial velocity of  −53.7 km s-1 from the v = 1,J = 1−0 transition and  −51.9 km s-1 from the v = 2,J = 1−0 line. Our observations resulted in a very similar LSR velocity of  −52 km s-1 (see Table 5).

6.5. Perseus OB1

The Perseus OB1 association contains the famous double cluster h/χ Per. These young clusters (age ~14 My) have distances of kpc and kpc, respectively (Currie et al. 2010). The association contains at least 22 RSGs (Humphreys 1978; Garmany & Stencel 1992; Pierce et al. 2000). For one of them, S Per, recently a trigonometric parallax distance of 2.42 + 0.11-0.09 kpc was measured (Asaki et al. 2010); see Xu et al. (2006) for another VLBI distance and a relevant discussion.

No SiO maser survey of the complete sample of RSGs in Per OB1 had been conducted so far. Only a few sources had been searched for SiO masers and maser emission was detected before in W Per (Jiang et al. 1996) and the well studied S Per, which is known for its strong maser emission (e.g. Kaifu et al. 1975). The 28SiO v = 1 and v = 2, J = 1−0 and 29SiO v = 0, J = 1−0 masers were searched for toward FZ Per and T Per, but no emission was detected (Jiang et al. 1999). SU Per was targeted in a SiO v = 1, v = 2 and v = 3, J = 1−0 search, but no maser was found (Spencer et al. 1981).

W Per was found to show emission in the 43 GHz v = 1, J = 1−0 transition (Jiang et al. 1996). S Per was observed by various authors in a number of transitions. The first detection was the v = 1,J = 2−1 line at 86 GHz by Kaifu et al. (1975). Furthermore, maser emission was found in the SiO v = 1, v = 2 and v = 3, J = 1−0 transitions (e.g. Spencer et al. 1977; Cho et al. 1996), the v = 0 and v = 2, J = 2−1 transitions (e.g. Morris et al. 1979; Olofsson et al. 1981), and the v = 1, J = 3−2 transition (Herpin et al. 1998). Pardo et al. (1998) studied more than 15 different transitions of the SiO maser in S Per, detecting some high transitions such as v = 2 and v = 3, J = 4−3 and v = 1, J = 5−4.

The RSGs in the Perseus OB1 association discussed by Pierce et al. (2000) were part of our target list. We also observed the brightest member of the NGC 457 cluster, which is a M1.5 Iab star (Mermilliod et al. 2008).

We detected SiO maser emission toward two RSGs in the Per OB1 association, W Per and S Per. Both sources were known to host masers (see above). The detected stars are among the three RSG members with longer periods and have redder colors of 485 and 822 days, respectively. This led Pierce et al. (2000) to suggest that these objects are surrounded by a CSE.

We obtain an LSR velocity of  −41 km s-1 for S Per and  −40 km s-1 for W Per, respectively (see Table 2). Jiang et al. (1996) reported  −41.3 km s-1 for W Per based on their 43 GHz maser observations, in agreement with our findings. For S Per, several results can be found in the literature that agree within a km s-1 with our value (Alcolea et al. 1990; Kim et al. 2010).

6.6. GLIMPSE13

The GLIMPSE13 cluster contains a large number of spectroscopically confirmed G9 and M1 stars (Messineo et al. 2009; Mercer et al. 2005). including suspected supergiants with spectral types ranging from early K to late G. Since yellow supergiants are rarer than RSGs, and Galactic RSGs have a median spectral type of M2, it is more likely that the stars in GLIMPSE13 are massive giants with an age between 50 and 100 Myr (Messineo et al. 2009). The bright star GLIMPSE13 1, however, is too luminous to be a giant member of the same cluster (KS = 2.67 mag) and is of type M0I or M7III.

GLIMPSE13 was targeted in the searches for SiO and water masers in stellar clusters conducted by Deguchi et al. (2010). There is only an overlap of two sources with the stars for which Messineo et al. (2009) report IR data. Deguchi et al. (2010) detected three SiO masing stars (including GLIMPSE13 1, our one target star) with radial velocities around 70 km s-1 (72.3, 74.9 and 70.2 km s-1), and they found water maser emission with a velocity of 21.4 km s-1 toward GLIMPSE13 2 (a K5III star). A velocity of 71 km s-1 corresponds to a near-kinematic distance of kpc, while a velocity of 21 km s-1 implies a distance of 1.6 ± 0.4 kpc. The cluster is located in a particularly rich portion of the disk at a longitude of 33.8°. Several young stellar objects are located a few arcminutes north of the cluster, and a number of bright mid-infrared sources surround the cluster. It is most likely that we are seeing different groups of stars along neighboring lines-of-sight that are not physically associated.

We detected SiO maser emission in the v = 1, J = 2−1 line in the RSG candidate GLIMPSE13 1. Maser emission at 43 GHz had been observed before by Deguchi et al. (2010) in the v = 1, J = 1−0 transition. They found LSR velocities of peak emission of 69.4 km s-1 and 72.3 km s-1 on two separate observing days, completely in agreement with our value of 71 km s-1 (see Table 2). The SiO maser lines’ shape and breadth suggest that GLIMPSE13 1 is a RSG. The mean equivalent width of the maser emission is 27 km s-1.

6.7. GLIMPSE9

The stellar cluster number 9 in the list of Mercer et al. (2005) was analyzed with near-infrared spectroscopy and HST/NICMOS photometry by Messineo et al. (2009). These authors detected 3 RSG stars and one late M giant (or early type RSG). The cluster is located at a spectro-photometric distance of 4.2 kpc, has a likely age of 15−27 Myr, and a cluster mass of at least 1600 M.

We included in our target list all 4 late-type stars detected in the direction of the GLIMPSE9 cluster (3 RSGs and 1 giant). Maser lines were not detected.

6.8. SGR 1900+14

We also included among the targets the two RSG stars that are members of the stellar cluster associated with the magnetar (soft gamma ray repeater) SGR1900+14 (Davies et al. 2009a). The cluster is located at a kinematic distance of 12.5 ± 1.7 kpc, and has a likely age of 14 Myr. The two M5I stars have an angular separation of just ~2′′. Therefore only a single pointing was needed with the IRAM 30 m telescope. Maser lines were not detected.

6.9. MFD2008 (Cl 1813-178)

A young massive cluster was recently identified in the direction of the W33 complex at a kinematic distance of about 4 kpc. It contains several evolved early-type stars and 1 RSG (Messineo et al. 2008, 2011), from which a likely age of 4.5 Myr and a cluster mass of 104M are inferred. We included among our targets the RSG identified in the MFD2008 cluster by Messineo et al. (2008). We did not detect SiO maser emission toward this cluster member.

6.10. Trumpler 27

The Trumpler 27 cluster is located at at a spectro-photometric distance of 2.1 ± 0.2 kpc (Moffat et al. 1977). It contains a binary RSG of M0 type (Massey et al. 2001). The presence of two Wolf Rayet stars and several other evolved OB stars suggests a cluster age below 6 Myr. We included in our program the RSG. The 43 GHz v = 1, J = 1−0 transition was already observed by Hall et al. (1990). The 86 GHz v = 1, J = 2−1 line was also found before (Haikala et al. 1994).

We detected SiO maser emission at 86 GHz toward the binary RSG in Trumpler 27. We determine an LSR velocity of  −17 km s-1 (see Table 2), slightly higher than the  −11 km s-1 reported by Haikala et al. (1994).

6.11. The Galactic center and Inner Galaxy RSGs not associated with clusters

Blum et al. (2003) performed a spectro-photometric analysis of a sample of 79 luminous late-type stars in the central parsecs of the Galaxy. We observed 7 out of the 17 RSGs listed by Blum et al. (2003), but no maser lines were detected. One of the sources, BSD96 66, is the famous IRS 7, the brightest near IR source in the central parsec (Becklin & Neugebauer 1975). Toward this source, Menten et al. (1997) detected the 43.3 GHz v = 1, J = 1−0 SiO line with the NRAO Very Large Array (VLA) with a peak flux density of 0.38 Jy. Given that the 43 and 86 GHz v = 1 maser fluxes are comparable (see Sect. 7.3), it is not surprising that we did not obtain a detection given our noise level (0.22 Jy; see Table 3).

With a similar technique, Comerón et al. (2004) identified 18 RSGs located in the Inner Galaxy. We observed nine of these RSGs, but maser emission was not detected.

6.12. Clusters without SiO maser detections – summary

With our average rms noise of 0.23 Jy, we report the first unsuccessful searches toward targets in RSGC3, GLIMPSE9, MFD2008 and SGR 1900+14, as well as the isolated RSGs (Blum et al. 2003; Comerón et al. 2004) discussed in Sect. 6.11 (see Table 3). SiO masers vary with pulsation phase (e.g. Alcolea et al. 1990, 1999). New and deeper SiO maser observations could be useful to detect possible maser emission.

7. Analysis

7.1. Line equivalent widths

For comparison, we also observed SiO v = 1, J = 2−1 maser emission from the Mira variables IK Tau and U Her. From Table 2 and Fig. 1, it is obvious that the emission from the Miras, while very strong because close to Earth (~100 pc), covers much smaller velocity intervals than the RSGs’ emission. The SiO maser lines in RSGs are generally broader than those in Mira stars (e.g. Le Bertre & Nyman 1990; within error our new data confirms this previous result). Figure 2 shows a histogram of the velocity range covered by the SiO maser line. The Mira variables IK Tau and U Her are shown in a grey color. Clearly, their profiles are much narrower than those of the bulk of the RSG’s. Alcolea et al. (1990) found the mean equivalent width, given by (profile-area)/(peak-intensity), of the 86 GHz SiO maser lines to be 8.6 km s-1 (rms of 1.3 km s-1) for their sample of 10 RSGs, and only 4 km s-1 (rms of 1 km s-1) for the 17 Miras. In our case, using the values of Table 2, the 13 RSGs have a mean equivalent width of 7.4 km s-1 (rms of 2.7 km s-1), while the 2 Miras have a width of 2.4 km s-1 (rms of 0.4 km s-1).

thumbnail Fig. 2

Histogram of the LSR velocity range covered by the maser emission. The grey region shows the Mira variables IK Tau and U Her.

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Since for a CSE created by mass outflow, the terminal expansion velocity is proportional to the mass loss rate, the higher line widths we find for the RSGs (compared to Miras), simply reflects their greater degree of mass loss.

7.2. Maser occurrence versus the Q1 and Q2 parameters

With a combination of near- and mid-IR colors it is possible to identify mass-losing stars and to distinguish between highly reddened “naked” stars and dust-enshrouded stars. Messineo et al. (2012) proposed a new source selection method for identifying mass-losing late-type stars, which is based on photometric data from 2MASS and GLIMPSE (Cutri et al. 2003; Benjamin et al. 2003) and on the Q1 and Q2 parameters. These two parameters are independent of interstellar extinction. The Q1 parameter (Q1 = (J − H) − 1.8 × (H − KS)) is a measure of the deviation from the reddening vector in the 2MASS (J − H) versus (H − KS) plane (HJ, and KS are the stars’ magnitudes in the corresponding IR bands). Early-type stars have Q1 values around 1 and K-giants around 0.4 mag. Dusty CSEs change the energy distribution of late-type stars, and generate smaller Q1 values. On average, higher mass-loss rates produce smaller Q1 values (see trend in Fig. 4 by Messineo et al. 2012). Similarly, the Q2 parameter (Q2 = (J − KS) − 2.69 × (KS − [8.0] )) measures the deviation from the interstellar vector in the 2MASS/GLIMPSE plane (J − KS) versus (KS − [8.0] ). On average, higher mass-loss rates imply smaller Q2 values (see trends in Figs. 2 and 6 by Messineo et al. 2012).

thumbnail Fig. 3

The two extinction-free parameters Q1 and Q2 are plotted. Small dots indicate SiO maser detections by Messineo et al. (2002). Empty hexagons are our targeted RSGs without maser detections, and filled hexagons are those with maser emission.

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A plot of the Q1 versus Q2 parameters for the targeted RSGs is shown in Fig. 3. It shows that with our sensitivity we were able to detect masers only in stars with Q2 values smaller than  −1.9 mag. This implies that SiO maser emission was detected toward the reddest sources, and supports a radiative pumping mechanism for the SiO masers in RSGs (Alcolea et al. 1990). For comparison, points representing the SiO maser star sample of Messineo et al. (2002) are also plotted in Fig. 3. The corresponding data were taken with the same telescope as for our sample and have similar rms noise. However, the Messineo et al. sample is composed of Mira-like AGB stars, i.e. of stars of luminosity class III, (Messineo et al. 2004, 2005), while our new data points represent RSGs (luminosity class I).

There is an interesting shift between the Q2 values of masing sources from the one to the other sample. This suggests that higher mass-loss rates are required for RSGs to show SiO maser action than for AGB stars. Perhaps, the higher luminosities of RSGs push the dust condensation radius and the masing shell farther out. Mass-loss is indeed proportional to density and envelope size (see equation A3 in Sevenster 1999). A large statistics is needed to confirm this suggested color threshold.

Table 6

Maser/maser and maser/8 μm IR continuum flux ratios

7.3. SiO maser intensities

In Table 6, we list the ratio of the 43 GHz peak flux from the literature over the 86 GHz peak flux derived here. Apart from IK Tau, MY Cep and Cl* Stephenson 2 DFK 2, the 86 GHz transition is found to be stronger in all sources. The mean value of the 43/86 GHz ratio is 0.73 with a standard deviation of 0.41. This makes the 86 GHz transition a good line for determining radial velocities of RSG stars. Nyman et al. (1993) concluded that the 43 GHz over 86 GHz ratio increases with increasing mass-loss rates. Values above average are measured for MY Cep and DFK 2. We should note, however, that the SiO maser intensity is found to vary during the stellar variability cycle (e.g. Alcolea et al. 1990, 1999). The 43 GHz and 86 GHz observations are not simultaneously taken, and their peak intensities could vary with stellar phase. Therefore, the individual ratios may be not conclusive, and a simultaneous detection program should be carried out. A large fraction of stars have ratios below unity, confirming that with single dish telescopes surveys for 86 GHz SiO maser emission are more efficient than for 43 GHz emission. One should however, note that the VLA has been a very sensitive instrument for 43 GHz SiO maser searches (see Menten et al. 1997) and its expanded version, the Karl G. Jansky Very Large Array (JLVA) will be even more so. However, its sensitivity will be matched by the Atacama Large Millimeter Array (ALMA), which (after completion) will cover both lines with formidable sensitivity for sources with declinations up to ~40°.

We also calculated the ratio of the 86 GHz peak flux over the IR 8 μm peak flux (see Table 6). The 8 μm fluxes were taken from the MSX (Price et al. 2001) and GLIMPSE (Benjamin et al. 2003) catalogs when available. Previously, Alcolea et al. (1990) performed a SiO maser search in Miras and supergiants, and found a SiO(86 GHz peak flux)/IR(8 μm flux) ratio ~1/5 for Miras and the RSGs with the strongest maser emission, but significantly lower for the other supergiants (with 0.003 for SW Vir being the lowest ratio). We find a mean value of 0.32 for the 86 GHz peak flux over the 8 μm flux ratio (standard deviation of 0.34). Clearly, for all stars, the SiO maser flux is smaller than the 8   μm flux. Therefore they meet the criterion required by a radiative pump, which was established by the modeling of SiO maser pumping schemes; see Sect. 3.1. Again, we should note that both SiO maser and IR flux, which both are variable, generally were not measured contemporaneously.

8. Conclusions

We performed an extensive search for the SiO v = 1, J = 2 − 1 maser line at 86 GHz in 88 (candidate) RSGs in Galactic open clusters. Most of these stellar clusters were never before covered covered by a 86 GHz SiO maser survey. In total, we detected maser emission from 13 RSGs, 1 of which is the first detection on any SiO in the respective object. The measurements provide accurate LSR velocities, which can be used in studies of the Galactic structure. For the clusters containing masing stars, our non-detection of SiO emission in other RSG members may, in combination with a well determined distance to the cluster, yield information on the fraction of RSGs with high enough mass-loss to form maser containing CSEs or a dependence on maser occurrence with spectral type.

The FWHMs of the SiO maser lines are broader in RSGs than in Mira AGBs. The intensities of the 86 GHz SiO maser lines are somewhat stronger than those of 43 GHz v = 1, J = 1 − 0 SiO maser lines in most the sources (11 out of the 14 known to be masing in both lines). The JVLA and ALMA will provide all sky coverage for extremely sensitive surveys in both lines.

SiO maser emission was detected in targets with Q2 values larger than ~ − 2 mag. This increase of the detection rate with redder colors supports a radiative pumping mechanism for the SiO maser. The Q1 and Q2 parameters are proven to be useful tools for efficient targeted searches for SiO masers.


2

While, in oxygen-rich evolved stars, the SiO v = 1 and 2,J = 1−0 lines have comparable intensity, the v = 2,J = 2−1 is always much weaker than the v = 2,J = 1−0 line and has not yet been reported in a RSG (Bujarrabal et al. 1996).

Acknowledgments

We thank the IRAM 30 m staff for the support during the observations. L.V. was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. M.M. thanks Don Figer, Ben Davies, Simon Clark, and Ignatio Negueruela, for creative discussions on red supergiant clusters (RSGCs). The co-proposed SiO observations (non-detections) on RSGC3 are here included. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078).

References

All Tables

Table 1

IRAM 30 m observing dates.

Table 2

SiO v = 1; J = 2−1 detections toward RSGs.

Table 3

Red supergiants without SiO v = 1; J = 2 − 1 detection.

Table 4

Previous maser observations.

Table 5

Comparison between RSG LSR velocities determined from SiO maser emission and IR CO absorption.

Table 6

Maser/maser and maser/8 μm IR continuum flux ratios

All Figures

thumbnail Fig. 1

Spectra of the SiO v = 1, J = 2−1 transition toward the stars where the line was detected. All stars but X 18, U Her, and IK Tau are RSGs. The latter two are Mira variables and we show their much narrower spectra for comparison.

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In the text
thumbnail Fig. 2

Histogram of the LSR velocity range covered by the maser emission. The grey region shows the Mira variables IK Tau and U Her.

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In the text
thumbnail Fig. 3

The two extinction-free parameters Q1 and Q2 are plotted. Small dots indicate SiO maser detections by Messineo et al. (2002). Empty hexagons are our targeted RSGs without maser detections, and filled hexagons are those with maser emission.

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In the text

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