A near-infrared survey of the inner Galactic plane for Wolf–Rayet stars – III. New methods: faintest WR stars

Kanarek, G.; Shara, Michael M.; Faherty, Jacqueline K.; Zurek, David; Moffat, A. F. J.

doi:10.1093/mnras/stv1342

Cited by 19 publications

(28 citation statements)

References 34 publications

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“…This was identified as a WR star by Kanarek et al (2015), who classified it WC8. It brightened in W1 and W2 between the All-Sky and Post-Cryo survey observations (Table 14, Fig.…”

Section: Wr 122-14 = Ksf14 1553-15dfmentioning

confidence: 99%

Variable dust emission by WC type Wolf–Rayet stars observed in the NEOWISE-R survey

Williams

2019

Monthly Notices of the Royal Astronomical Society

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ABSTRACT Photometry at 3.4 and 4.6 ${\mu m}$ of 128 Population I WC type Wolf–Rayet stars in the Galaxy and 12 in the Large Magellanic Cloud (LMC) observed in the WISE NEOWISE-R survey was searched for evidence of circumstellar dust emission and its variation. Infrared spectral energy distributions (SEDs) were assembled, making use of archival r, i, Z, and Y photometry to determine reddening and stellar wind levels for the WC stars found in recent IR surveys and lacking optical photometry. From their SEDs, 10 apparently non-variable stars were newly identified as dust makers, including three, WR 102-22, WR 110-10, and WR 124-10, having subtype earlier than WC8–9, the first such stars to show this phenomenon. The 11 stars found to show variable dust emission include six new episodic dust makers, WR 47c, WR 75-11, WR 91-1, WR 122-14, and WR 125-1 in the Galaxy and HD 38030 in the LMC. Of previously known dust makers, NEOWISE-R photometry of WR 19 captured its rise to maximum in 2018 confirming the 10.1-yr period, that of WR 125 the beginning of a new episode of dust formation suggesting a period near 28.3 yr. while that of HD 36402 covered almost a whole period and forced revision of it to 5.1 yr.

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“…This was identified as a WR star by Kanarek et al (2015), who classified it WC8. It brightened in W1 and W2 between the All-Sky and Post-Cryo survey observations (Table 14, Fig.…”

Section: Wr 122-14 = Ksf14 1553-15dfmentioning

confidence: 99%

Variable dust emission by WC type Wolf–Rayet stars observed in the NEOWISE-R survey

Williams

2019

Monthly Notices of the Royal Astronomical Society

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“…A three-color composite image of the G34.260+0.169 region (hereafter G34) is shown in Figure 3. This region hosts a WC8-type W-R star, 1553-15DF (Kanarek et al 2015). Wang et al (2016) reported the presence of a gaseous filament, F36, at a distance of 1.6 kpc projected toward this region.…”

Section: G34260+0169mentioning

confidence: 97%

“…The G51.840+0.410 region (hereafter G51) harbors a W-R star, 1697-38F, which is classified as WC9 (Kanarek et al 2015) and hosts two MIR bubbles, N108 and N109 (see Figure 5). Bania et al (2012) noted star formation toward the edge of N109, and identified this as one of the largest H ii regions in the Milky Way.…”

Section: G51840+0410mentioning

confidence: 99%

“…Recent systematic surveys aimed at identifying Galactic W-R stars (e.g. Shara et al 2012;Kanarek et al 2015) have increased their number by a factor of two with respect to the previous decade. This study aims to explore a few potential star-forming regions that could be associated with W-R stars and, subsequently, to examine whether the presence of W-R stars has any impact on the surrounding molecular gas.…”

Section: Introductionmentioning

confidence: 99%

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Influence of Wolf–Rayet Stars on Surrounding Star-forming Molecular Clouds

Baug¹,

Grijs

Dewangan

et al. 2019

ApJ

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We investigate the influence of Wolf-Rayet (W-R) stars on their surrounding star-forming molecular clouds. We study five regions containing W-R stars in the inner Galactic plane (l ∼[14 • -52 • ]), using multi-wavelength data from near-infrared to radio wavelengths. Analysis of 13 CO line data reveals that these W-R stars have developed gas-deficient cavities in addition to molecular shells with expansion velocities of a few km s −1 . The pressure owing to stellar winds primarily drives these expanding shells and sweeps up the surrounding matter to distances of a few pc. The column densities of shells are enhanced by a minimum of 14% for one region to a maximum of 88% for another region with respect to the column densities within their central cavities. No active star formationincluding molecular condensations, protostars, or ionized gas -is found inside the cavities, whereas such features are observed around the molecular shells. Although the expansion of ionized gas is considered an effective mechanism to trigger star formation, the dynamical ages of the H ii regions in our sample are generally not sufficiently long to do so efficiently. Overall, our results hint at the possible importance of negative W-R wind-driven feedback on the gas-deficient cavities, where star formation is quenched as a consequence. In addition, the presence of active star formation around the molecular shells indicates that W-R stars may also assist in accumulating molecular gas, and that they could initiate star formation around those shells.

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“…It is a radio and millimetre source and has been listed as a PN (Urquhart et al 2009). In a survey of the inner GP for Wolf-Rayet stars, Kanarek et al (2015) also class this object as a possible PN (object 1527-318B); their near-infrared spectrum shows strong emission from Hei (2.058 µm) and Br γ which can be characteristic of young PNe (e.g. Gledhill & Forde 2015).…”

Section: Colourmentioning

confidence: 99%

Planetary nebulae in the UWISH2 survey

Gledhill

Froebrich

Campbell-White

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Near-infrared imaging in the 1 − 0 S(1) emission line of molecular hydrogen is able to detect planetary nebulae (PNe) that are hidden from optical emission line surveys. We present images of 307 objects from the UWISH2 survey of the northern Galactic Plane, and with the aid of mid-infrared colour diagnostics draw up a list of 291 PN candidates. The majority, 183, are new detections and 85 per cent of these are not present in H α surveys of the region. We find that more than half (54 per cent) of objects have a bipolar morphology and that some objects previously considered as elliptical or point-source in H α imaging, appear bipolar in UWISH2 images. By considering a small subset of objects for which physical radii are available from the H α surface brightness-radius relation, we find evidence that the H 2 surface brightness remains roughly constant over a factor 20 range of radii from 0.03 to 0.6 pc, encompassing most of the visible lifetime of a PN. This leads to the H α surface brightness becoming comparable to that of H 2 at large radius (> 0.5 pc). By combining the number of UWISH2 PNe without H α detection with an estimate of the PN detection efficiency in H 2 emission, we estimate that PN numbers from H α surveys may underestimate the true PN number by a factor between 1.5 and 2.5 within the UWISH2 survey area.

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A near-infrared survey of the inner Galactic plane for Wolf–Rayet stars – III. New methods: faintest WR stars

Cited by 19 publications

References 34 publications

Variable dust emission by WC type Wolf–Rayet stars observed in the NEOWISE-R survey

Variable dust emission by WC type Wolf–Rayet stars observed in the NEOWISE-R survey

Influence of Wolf–Rayet Stars on Surrounding Star-forming Molecular Clouds

Planetary nebulae in the UWISH2 survey

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