First detections of FS Canis Majoris stars in clusters

Fuente, D. de la; Najarro, F.; Trombley, Christine; Davies, Ben; Figer, Donald F.

doi:10.1051/0004-6361/201425371

Cited by 19 publications

(22 citation statements)

References 126 publications

(132 reference statements)

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“…2 in Davies et al 2012) were identified as late WN Wolf-Rayet stars (see Fig. 3 in de la Fuente et al 2013). We concur with these results.…”

Section: Mass Denissupporting

confidence: 90%

“…near-IR spectroscopy with ESO/ISAAC and the results of these observations are reported in Davies et al (2012) and de la Fuente et al (2013). The authors derived a 11 ± 2 kpc distance and showed that Mercer 81 was mainly populated with nitrogen-rich Wolf-Rayet and blue supergiant stars; in particular, sources 1278 and 1279 (labelled 8 and 2 in these papers, see Fig.…”

Section: Mass Denismentioning

confidence: 78%

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Near-infrared spectroscopy of 20 newChandrasources in the Norma arm

Rahoui

Tomsick

Fornasini

et al. 2014

A&A

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We report on CTIO/NEWFIRM and CTIO/OSIRIS photometric and spectroscopic observations of 20 new X-ray (0.5-10 keV) emitters discovered in the Norma arm Region Chandra Survey (NARCS). NEWFIRM photometry was obtained to pinpoint the nearinfrared counterparts of NARCS sources, while OSIRIS spectroscopy was used to help identify 20 sources with possible high mass X-ray binary properties. We find that (1) two sources are WN8 Wolf-Rayet stars, maybe in colliding wind binaries, part of the massive star cluster Mercer 81; (2) two are emission-line stars, possibly in X-ray binaries, that exhibit near-and mid-infrared excesses either due to free-free emission from the decretion discs of Be stars or warm dust in the stellar winds of peculiar massive stars such as B[e] supergiants or luminous blue variables; (3) one is a B8-A3 IV-V star that could be in a quiescent high mass X-ray binary system; (4) two are cataclysmic variables including one intermediate polar; (5) three may be neutron star symbiotic binaries; (6) five are most likely white dwarf symbiotic binaries; and (7) five exhibit properties more consistent with isolated giant/dwarf stars. The possible detection of one to three high mass X-ray binaries is in good agreement with our predictions. However, our study illustrates the difficulty of clearly differentiating quiescent or intermediate X-ray luminosity systems from isolated massive stars, which may lead to an underestimation of the number of known high mass X-ray binaries.

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“…2 in Davies et al 2012) were identified as late WN Wolf-Rayet stars (see Fig. 3 in de la Fuente et al 2013). We concur with these results.…”

Section: Mass Denissupporting

confidence: 90%

Section: Mass Denismentioning

confidence: 78%

Near-infrared spectroscopy of 20 newChandrasources in the Norma arm

Rahoui

Tomsick

Fornasini

et al. 2014

A&A

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“…The surface density of the W-R stars in the W-R region of NGC 5430 is more than 100 times higher than that of the Milky Way (Massey 2003;Mauerhan et al 2011;Davies et al 2012;de la Fuente et al 2013). Moreover, the HII region associated with the W-R region deviates from the global HII regions in terms of the luminosity function, which is similar to our Milky Way (Keel 1982).…”

Section: The Externally Triggered Starburst At the Bar Endsupporting

confidence: 67%

Constraints on the minor merging and star formation history of the Wolf–Rayet galaxy NGC 5430 through observations

Pan

Kuno

Saito

et al. 2015

Publications of the Astronomical Society of Japan

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We used multi-wavelength analysis of the newly observed molecular gas ( 12 CO and 13 CO (1-0)) with interferometer CARMA and archival star formation tracers to constrain the interaction, merging, and star formation history of an off-center minor merger, a three-spiral barred galaxy NGC 5430 and its satellite embedded in the bar. Morphology of the molecular gas in the bar of NGC 5430 shows minimal signs of recent interactions in our resolution. The apparent morphological remnant of the past galaxy interaction is an asymmetric spiral arm, containing more molecular gas and exhibiting higher star formation rate (SFR) surface density than the two primary arms. Rotation curve analysis suggests that NGC 5430 and its satellite collided several Gyr ago. History of star formation was constrained by using SFRs that trace different timescales (infrared, radio continuum, and Hα). The collision occurred 5 -10 Myr ago, triggering a transient off-center starburst of Wolf-Rayet stars at the eastern bar end. In the past, the global SFR during the Wolf-Rayet starburst peaked at 35 M ⊙ yr −1 . At present, the merger-driven starburst is rapidly decaying and the current global SFR has decreased to the Galactic value. The SFR will continue to decay as suggested by the present amount of dense gas (traced by HCN (1-0)). Nonetheless, the global SFR is still dominated by the Wolf-Rayet region rather than the circumnuclear region. Compared with other barred galaxies, the circumnuclear region exhibits particularly low dense gas fraction, low star formation activity and high concentration of gas. Physical properties of the molecular gas are inferred by using the large velocity gradient (LVG) calculations. The initial mass ratio of the NGC 5430 and its satellite are suggested to be in the intermediate ratio range of 7:1-20:1.

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“…( (23) Chené et al (2013), (24) Rahman, Moon, & Matzner (2011), (25) Anderson et al (2011), (26) Marston et al (2013), (27) Kanarek et al (2014), (28) Davies et al (2012), (29) de La Fuente, Najarro, Davies, & Figer (2013), (30) Borissova et al (2012), (31) Mikles et al (2006), (32) Hyodo et al (2008), (33) Faherty et al (2014) (34) Smith et al (2012), (35) Corradi et al (2010), (36) Gvaramadze et al (2009), (37) Burgemeister et al (2013) He ii This paper has been typeset from a T E X/ L A T E X file prepared by the author.…”

mentioning

confidence: 99%

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

Rosslowe

Crowther

2015

Monthly Notices of the Royal Astronomical Society

123

143

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We construct revised near-infrared absolute magnitude calibrations for 126 Galactic Wolf-Rayet (WR) stars at known distances, based in part upon recent large scale spectroscopic surveys. Application to 246 WR stars located in the field, permits us to map their Galactic distribution. As anticipated, WR stars generally lie in the thin disk (∼40 pc half width at half maximum) between Galactocentric radii 3.5-10 kpc, in accordance with other star formation tracers. We highlight 12 WR stars located at vertical distances of 300 pc from the midplane. Analysis of the radial variation in WR subtypes exposes a ubiquitously higher N W C /N W N ratio than predicted by stellar evolutionary models accounting for stellar rotation. Models for non-rotating stars or accounting for close binary evolution are more consistent with observations. We consolidate information acquired about the known WR content of the Milky Way to build a simple model of the complete population. We derive observable quantities over a range of wavelengths, allowing us to estimate a total number of 1200 +300 −100 Galactic WR stars, implying an average duration of ∼ 0.25 Myr for the WR phase at the current Milky Way star formation rate. Of relevance to future spectroscopic surveys, we use this model WR population to predict follow-up spectroscopy to K S ≃ 13 mag will be necessary to identify 95% of Galactic WR stars. We anticipate that ESA's Gaia mission will make few additional WR star discoveries via low-resolution spectroscopy, though will significantly refine existing distance determinations. Appendix A provides a complete inventory of 322 Galactic WR stars discovered since the VIIth catalogue (313 including Annex), including a revised nomenclature scheme.

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First detections of FS Canis Majoris stars in clusters

Cited by 19 publications

References 126 publications

Near-infrared spectroscopy of 20 newChandrasources in the Norma arm

Near-infrared spectroscopy of 20 newChandrasources in the Norma arm

Constraints on the minor merging and star formation history of the Wolf–Rayet galaxy NGC 5430 through observations

Spatial distribution of Galactic Wolf–Rayet stars and implications for the global population

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