The Progenitor Mass of the Magnetar Sgr1900+14

Davies, Ben; Figer, D. F.; Kudritzki, Rolf‐Peter; Trombley, Christine; Kouveliotou, C.; Wachter, Stefanie

doi:10.1088/0004-637x/707/1/844

Cited by 100 publications

(102 citation statements)

References 45 publications

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“…Swift J1834.9−0846 is one of the few Galactic magnetars associated with massive stars (e.g. Figer et al 2005;Bibby et al 2008;Muno et al 2006;Davies et al 2009a;Mori et al 2013). SNR G22.7−0.2 has a size similar to that of W41 (40 pc at 4.6 kpc, Green 2009).…”

Section: Reg7 Reg5 and Rsgcx1mentioning

confidence: 99%

Massive stars in the giant molecular cloud G23.3−0.3 and W41

Messineo

Menten

Figer

et al. 2014

A&A

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Context. Young massive stars and stellar clusters continuously form in the Galactic disk, generating new Hii regions within their natal giant molecular clouds and subsequently enriching the interstellar medium via their winds and supernovae. Aims. Massive stars are among the brightest infrared stars in such regions; their identification permits the characterisation of the star formation history of the associated cloud as well as constraining the location of stellar aggregates and hence their occurrence as a function of global environment. Methods. We present a stellar spectroscopic survey in the direction of the giant molecular cloud G23.3−0.3. This complex is located at a distance of ∼4-5 kpc, and consists of several Hii regions and supernova remnants. Results. We discovered 11 Of + K stars, one candidate luminous blue variable, several OB stars, and candidate red supergiants. Stars with K-band extinction from ∼1.3-1.9 mag appear to be associated with the GMC G23.3−0.3; O and B-types satisfying this criterion have spectrophotometric distances consistent with that of the giant molecular cloud. Combining near-IR spectroscopic and photometric data allowed us to characterize the multiple sites of star formation within it. The O-type stars have masses from ∼25-45 M , and ages of 5-8 Myr. Two new red supergiants were detected with interstellar extinction typical of the cloud; along with the two RSGs within the cluster GLIMPSE9, they trace an older burst with an age of 20-30 Myr. Massive stars were also detected in the core of three supernova remnants -W41, G22.7−0.2, and G22.7583−0.4917. Conclusions. A large population of massive stars appears associated with the GMC G23.3−0.3, with the properties inferred for them indicative of an extended history of stars formation.

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Section: Reg7 Reg5 and Rsgcx1mentioning

confidence: 99%

Massive stars in the giant molecular cloud G23.3−0.3 and W41

Messineo

Menten

Figer

et al. 2014

A&A

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“…The possible association of some AXPs/SGRs with clusters of massive stars seems to indicate that they descend from stars of mass above ∼40 M ⊙ . However, evidence for a lower mass progenitor has been derived for SGR 1900+14 [25].…”

Section: The Magnetar Modelmentioning

confidence: 99%

Pulsars and Magnetars

Mereghetti

2013

Braz J Phys

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The high-energy sources known as anomalous X-ray pulsars (AXPs) and soft γ-ray repeaters (SGRs) are well explained as magnetars: isolated neutron stars powered by their own magnetic energy. After explaining why it is generally believed that the traditional energy sources at work in other neutron stars (accretion, rotation, residual heat) cannot power the emission of AXPs/SGRs, I review the observational properties of the twenty AXPs/SGRs currently known and describe the main features of the magnetar model. In the last part of this review I discuss the recent discovery of magnetars with low external dipole field and some of the relations between AXPs/SGRs and other classes of isolated neutron stars.

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“…Five young massive stellar clusters (RSGC1, RSGC2, RSGC3, RSGC4, and RSGC5), extraordinarily rich in RSGs (14, 26, >8, >9, 7), have been located between 25 • and 30 • of longitude, at a distance of about 6 kpc probably at the near end-side of the Galactic Bar (Davies et al 2007;Figer et al 2006;Clark et al 2009;Negueruela et al 2010Negueruela et al , 2011. We restricted our analysis to a sample of 119 spectroscopically confirmed RSGs in clusters, because their association with a cluster confirms the luminosity class (Skiff 2010;Eggenberger et al 2002;Mermilliod et al 2008;Pierce et al 2000;Mengel & Tacconi-Garman 2007;Figer et al 1999;Messineo et al 2011Messineo et al , 2010Davies et al 2009a;Bernabei & Polcaro 2001;Caron et al 2003;Figer et al 2006;Davies et al 2008;Clark et al 2009;Negueruela et al 2010Negueruela et al , 2011. When comparing the distribution in colors of the 119 RSG stars in clusters with all RSGs listed by Skiff et al, however, no significant differences are seen.…”

Section: Red Supergiant Starsmentioning

confidence: 99%

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

Messineo

Menten

Churchwell

et al. 2011

A&A

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Context. Mass-loss from evolved stars chemically enriches the interstellar medium (ISM). Stellar winds from massive stars and their explosions as supernovae shape the ISM and trigger star formation. Studying evolved stars is fundamental for understanding galaxy formation and evolution at any redshift. Aims. We aim to establish a photometric classification scheme for Galactic mass-losing evolved stars (e.g., WR, RSG, and AGB stars) with the goal of identifying new ones, and subsequently to use these samples as tracers of Galactic structure. Methods. We searched for counterparts of known Galactic WR, LBV, RSG, and O-rich AGB stars in the 2MASS, GLIMPSE, and MSX catalogs, and we analyzed their properties with near-and mid-infrared color-color diagrams. Results. We used the Q1 parameter, which is a measure of the deviation from the interstellar reddening vector in the J − H versus H−K s diagram, and we defined a new parameter, Q2, which is a measure of the deviation from the interstellar reddening vector in the Conclusions. The GLIMPSE catalog is a powerful tool for photometric classification of Galactic mass-losing evolved stars. Our new criteria will yield many new RSGs and WRs.

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The Progenitor Mass of the Magnetar Sgr1900+14

Cited by 100 publications

References 45 publications

Massive stars in the giant molecular cloud G23.3−0.3 and W41

Massive stars in the giant molecular cloud G23.3−0.3 and W41

Pulsars and Magnetars

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

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