The P Cygni supergiant [OMN2000] LS1 – implications for the star formation history of W51

Clark, J. S.; Davies, Ben; Najarro, F.; MacKenty, John; Crowther, P. A.; Messineo, M.

doi:10.1051/0004-6361/200911980

Cited by 45 publications

(90 citation statements)

References 51 publications

(83 reference statements)

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“…8 and 10). The three stars (#40,#41, and #42) have A K s of 1.95, 1.27, and 1.03 mag, which imply distances larger than 4 kpc (Clark et al 2009;Drimmel et al 2003). By assuming that they are at the distance of 4.6 kpc, we derived M bol = −7.49, −5.51, and −5.65 mag, respectively, and their likely association with the SNR.…”

Section: Reg7 Reg5 and Rsgcx1mentioning

confidence: 95%

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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: 95%

“…By assuming that they are at the distance of 4.6 kpc, we derived M bol = −7.49, −5.51, and −5.65 mag, respectively, and their likely association with the SNR. The presence of 3 cRSGs implies also the presence of a candidate massive cluster of stars (>10 000 M , Clark et al 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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“…(Groh et al 2012;Hillier et al 2001), WR 102ka (Barniske et al 2008), AG Car Groh et al (2009b;Groh et al, in prep. ), AFGL 2298 (Clark et al 2009a), FMM 362 and Pistol star ), Wray 17-96 (Egan et al 2002), G24.73+0.69 (Clark et al 2009a), [OMN2000] LS1 (Clark et al 2009b), HD 316285 (Hillier et al 1998), HD 160529, HD 168625 andHD 168607 (van Genderen 2001), P Cygni (Najarro 2001;2011, priv. comm.…”

Section: When Lbvs Are Sn Progenitors and Their Sn Typesmentioning

confidence: 99%

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

Groh

Meynet

Georgy

et al. 2013

A&A

193

223

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We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of M ini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with M ini = 9−20 M , we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the following types of SN progenitors:, and RSGs (9 ≤ M ini ≤ 18 M ). For non-rotating models, we found spectral types WO1-, and RSGs (9 ≤ M ini ≤ 20 M ). Our rotating models indicate that SN IIP progenitors are all RSG, SN IIL/b progenitors are 56% LBVs and 44% YHGs, SN Ib progenitors are 96% WN10-11 and 4% WOs, and SN Ic progenitors are all WO stars. We find that the most massive and luminous SN progenitors are not necessarily the brightest ones in a given filter, since this depends on their luminosity, temperature, wind density, and the way the spectral energy distribution compares to a filter bandpass. We find that SN IIP progenitors (RSGs) are bright in the RIJHK S filters and faint in the UB filters. SN IIL/b progenitors (LBVs and YHGs), and SN Ib progenitors (WNs) are relatively bright in optical/infrared filters, while SN Ic progenitors (WOs) are faint in all optical filters. We argue that SN Ib and Ic progenitors from single stars should be undetectable in the available pre-explosion images with the current magnitude limits, in agreement with observational results.

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“…Known magnetic OB stars are expected to demonstrate hard, overluminous X-ray emission (e.g. Clark et al 2009a, and refences therein); while several overluminous OB stars are present within Wd 1 ), they all demonstrate rather soft X-ray spectra; the sole exception being W30a, a known (colliding wind) binary. 8 Although simulations by Yoon et al (2010) suggests that such a mechanism is ineffective for stars below 25 M .…”

Section: Implications For Magnetar Formationmentioning

confidence: 99%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Clark

Ritchie

Najarro

et al. 2014

A&A

Self Cite

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Context. The first soft gamma-ray repeater was discovered over three decades ago, and was subsequently identified as a magnetar, a class of highly magnetised neutron star. It has been hypothesised that these stars power some of the brightest supernovae known, and that they may form the central engines of some long duration gamma-ray bursts. However there is currently no consenus on the formation channel(s) of these objects. Aims. The presence of a magnetar in the starburst cluster Westerlund 1 implies a progenitor with a mass ≥40 M , which favours its formation in a binary that was disrupted at supernova. To test this hypothesis we conducted a search for the putative pre-SN companion.Methods. This was accomplished via a radial velocity survey to identify high-velocity runaways, with subsequent non-LTE model atmosphere analysis of the resultant candidate, Wd1-5. Results. Wd1-5 closely resembles the primaries in the short-period binaries, Wd1-13 and 44, suggesting a similar evolutionary history, although it currently appears single. It is overluminous for its spectroscopic mass and we find evidence of He-and N-enrichement, O-depletion, and critically C-enrichment, a combination of properties that is difficult to explain under single star evolutionary paradigms. We infer a pre-SN history for Wd1-5 which supposes an initial close binary comprising two stars of comparable (∼41 M + 35 M ) masses. Efficient mass transfer from the initially more massive component leads to the mass-gainer evolving more rapidly, initiating luminous blue variable/common envelope evolution. Reverse, wind-driven mass transfer during its subsequent WC Wolf-Rayet phase leads to the carbon pollution of Wd1-5, before a type Ibc supernova disrupts the binary system. Under the assumption of a physical association between Wd1-5 and J1647-45, the secondary is identified as the magnetar progenitor; its common envelope evolutionary phase prevents spin-down of its core prior to SN and the seed magnetic field for the magnetar forms either in this phase or during the earlier episode of mass transfer in which it was spun-up. Conclusions. Our results suggest that binarity is a key ingredient in the formation of at least a subset of magnetars by preventing spin-down via core-coupling and potentially generating a seed magnetic field. The apparent formation of a magnetar in a Type Ibc supernova is consistent with recent suggestions that superluminous Type Ibc supernovae are powered by the rapid spin-down of these objects.

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The P Cygni supergiant [OMN2000] LS1 – implications for the star formation history of W51

Cited by 45 publications

References 51 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

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

A VLT/FLAMES survey for massive binaries in Westerlund 1

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