Near- and mid-infrared colors of evolved stars in the Galactic plane. The<i>Q</i>1 and<i>Q</i>2 parameters

Messineo, M.; Menten, K. M.; Churchwell, E.; Habing, H. J.

doi:10.1051/0004-6361/201117772

Cited by 40 publications

(91 citation statements)

References 101 publications

(237 reference statements)

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“…This fact allowed us to use the absorption ratios (r X = A X /A V ) given by Johnson (1968) van der Hulst curve 15 and Cambrésy et al (2002). Then, following Borissova et al (2012) and Messineo et al (2012) we separated the selected stars among the early normal MS stars (−0.1 < Q NIR < 0.15; blue symbols) and, stars with emission features or revealing IR excess (Q NIR < −0.1; red symbols), including, for example, PMS stars and YSOs. We noticed that some spectroscopically confirmed OB stars in the DBS 77 and DBS 160 regions (see Figs.…”

Section: Photometric Diagramsmentioning

confidence: 99%

The embedded clusters DBS 77, 78, 102, and 160−161, and their link with the interstellar medium

Corti

Baume

Panei

et al. 2016

A&A

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Aims. We report on a study of the global properties of some embedded clusters that are found in the fourth quadrant of the Milky Way. We aim to clarify some issues that relate to their location in the Galaxy and their stellar formation processes. Methods. We performed BVI photometric observations in the region of DBS 77, 78, 102, 160, and 161 clusters, and infrared spectroscopy in the DBS 77 region. These were complemented with JHK data from the VVV survey combined with the 2MASS catalogue, and used mid-infrared information from the GLIMPSE catalogue. We also searched for HI data from the SGPS and PMN radio surveys, and previous spectroscopic stellar classifications. The spectroscopic and photometric information enabled us to estimate the spectral classification of the brightest stars for each of the studied regions. On the other hand, we used radio data to investigate the interstellar material parameters and the continuum sources that are probably associated with the respective stellar components. Results. We estimated the basic physical parameters of the clusters (reddening, distance, age, and initial mass function). We searched for HII regions located near to the studied clusters and we analyzed the possible links between them. In the particular case of the DBS 160−161 clusters, we identified the HI bubble B332.5-0.1-42 that is located around them. We found that the mechanical energy injected in to the interstellar medium by the more massive stars of this couple of clusters was enough to generate the bubble.

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Section: Photometric Diagramsmentioning

confidence: 99%

The embedded clusters DBS 77, 78, 102, and 160−161, and their link with the interstellar medium

Corti

Baume

Panei

et al. 2016

A&A

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“…Messineo et al (2012) provided new criteria to separate RSGs and LBVs from AGB stars, which are based on near-IR indices, Q1 and Q2. These indices measure the deviation from the reddening vector in the H − K s versus J − K s plane and the J − K s versus K s − [8.0] plane, respectively.…”

Section: Contamination From Other Luminous Sourcesmentioning

confidence: 99%

Identification of red supergiants in nearby galaxies with mid-IR photometry

Britavskiy

Bonanos

Mehner

et al. 2014

A&A

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Context. The role of episodic mass loss in massive-star evolution is one of the most important open questions of current stellar evolution theory. Episodic mass loss produces dust and therefore causes evolved massive stars to be very luminous in the mid-infrared and dim at optical wavelengths. Aims. We aim to increase the number of investigated luminous mid-IR sources to shed light on the late stages of these objects. To achieve this we employed mid-IR selection criteria to identity dusty evolved massive stars in two nearby galaxies. Methods. The method is based on mid-IR colors, using 3.6 μm and 4.5 μm photometry from archival Spitzer Space Telescope images of nearby galaxies and J-band photometry from 2MASS. We applied our criteria to two nearby star-forming dwarf irregular galaxies, Sextans A and IC 1613, selecting eight targets, which we followed-up with spectroscopy. Results. Our spectral classification and analysis yielded the discovery of two M-type supergiants in IC 1613, three K-type supergiants and one candidate F-type giant in Sextans A, and two foreground M giants. We show that the proposed criteria provide an independent way for identifying dusty evolved massive stars that can be extended to all nearby galaxies with available Spitzer/IRAC images at 3.6 μm and 4.5 μm.

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“…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.…”

Section: Red Supergiants In Stellar Clustersmentioning

confidence: 99%

“…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.…”

Section: Maser Occurrence Versus the Q1 And Q2 Parametersmentioning

confidence: 99%

“…We know only about 500 RSGs (e.g. Messineo et al 2012;Figer et al 2006;Davies et al 2007) relations (i) between the maximum luminosity of a given star and its main-sequence mass and (ii) between mass-loss rate,Ṁ, and stellar luminosity, L * and initial metallicity, Z. Possible stellar rotation complicates these relations (Meynet & Maeder 2000).…”

Section: Introductionmentioning

confidence: 99%

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SiO maser emission from red supergiants across the Galaxy

Verheyen¹,

Messineo²,

Menten³

2012

A&A

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Aims. Red supergiants (RSGs) are among the most luminous of all stars, easily detectable in external galaxies, and may ideally serve as kinematic tracers of Galactic structure. Some RSGs are surrounded by circumstellar envelopes detectable by their dust and molecular and, in particular, maser emission. This study consists of a search for maser emission from silicon monoxide (SiO) toward a significant number of RSGs that are members of massive stellar clusters, many of which have only recently been discovered. Further, we aim to relate the occurrence of maser action to properties of the host stars. Methods. Using the IRAM 30 m telescope, we searched for maser emission in the J = 2−1 rotational transition within the first vibrationally excited state of SiO toward a sample of 88 RSGs. Results. With an average rms noise level of 0.25 Jy, we detected maser emission in 15% of the sample, toward most of the sources for the first time in this transition. The peak of the emission provides accurate radial velocities for the RSGs. The dependence of the detection rate on infrared colors supports a radiative pumping mechanism for the SiO masers.

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Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

Cited by 40 publications

References 101 publications

The embedded clusters DBS 77, 78, 102, and 160−161, and their link with the interstellar medium

The embedded clusters DBS 77, 78, 102, and 160−161, and their link with the interstellar medium

Identification of red supergiants in nearby galaxies with mid-IR photometry

SiO maser emission from red supergiants across the Galaxy

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