UCHII Regions and Newly Born O-type Stars

Conti, Peter S.; Rho, Jeonghee; Furness, J. P.; Crowther, P. A.

doi:10.1017/s1743921308020607

Cited by 2 publications

(2 citation statements)

References 7 publications

(5 reference statements)

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“…Grammer & Humphreys (2013) put forth the explanation that objects in the bottom right of the color-color diagram may contain blended objects or compact H  regions. Indeed, at the limit of the HST resolution, ultra compact H  regions, which are typically connected to small clusters of stars (Conti et al 2008), may be contaminants. In a study of the clusters in the central fields of the HST data for M 83, Chandar et al (2010) show that reddening may cause the V − I values of candidate LBVs to move out of where they are expected in the same way as seen in our plot.…”

Section: B-vmentioning

confidence: 99%

The infrared massive stellar content of M 83

Bonanos

Whitmore

Prieto

et al. 2015

A&A

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Aims. We present an analysis of archival Spitzer images and new ground-based and Hubble Space Telescope (HST) near-infrared (IR) and optical images of the field of M 83 with the goal of identifying rare, dusty, evolved massive stars. Methods. We present point source catalogs consisting of 3778 objects from Spitzer Infrared Array Camera (IRAC) Band 1 (3.6 µm) and Band 2 (4.5 µm), and 975 objects identified in Magellan 6.5 m FourStar near-IR J and K s images. A combined catalog of coordinate matched near-and mid-IR point sources yields 221 objects in the field of M 83. Results. We find 49 strong candidates for massive stars which are very promising objects for spectroscopic follow-up. Based on their location in a B − V versus V − I diagram, we expect at least 24, or roughly 50%, to be confirmed as red supergiants.

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Section: B-vmentioning

confidence: 99%

The infrared massive stellar content of M 83

Bonanos

Whitmore

Prieto

et al. 2015

A&A

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“…UCHs are small (< 0.4 pc), hot (> 100 K), and massive (> 10 3 M ⊙ ), and emit 10 4 − 10 6 L ⊙ (Churchwell 2002). These regions of ionized gas are surrounded by molecular and dust clouds, out to as far as ten times the radius of the UCHs themselves (Conti et al 2007). This causes attenuation of much of the emitted luminosity, as it is absorbed and reradiated in the infrared.…”

Section: Introductionmentioning

confidence: 99%

SOFIA/FORCAST ANDSPITZER/IRAC IMAGING OF THE ULTRACOMPACT H II REGION W3(OH) AND ASSOCIATED PROTOSTARS IN W3

Hirsch

Adams

Herter

et al. 2012

ApJ

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We present infrared observations of the ultra-compact H II region W3(OH) made by the FORCAST instrument aboard SOFIA and by Spitzer/IRAC. We contribute new wavelength data to the spectral energy distribution, which constrains the optical depth, grain size distribution, and temperature gradient of the dusty shell surrounding the H II region. We model the dust component as a spherical shell containing an inner cavity with radius ∼ 600 AU, irradiated by a central star of type O9 and temperature ∼ 31, 000 K. The total luminosity of this system is 7.1 × 10 4 L ⊙ . An observed excess of 2.2 − 4.5 µm emission in the SED can be explained by our viewing a cavity opening or clumpiness in the shell structure whereby radiation from the warm interior of the shell can escape. We claim to detect the nearby water maser source W3 (H 2 O) at 31.4 and 37.1 µm using beam deconvolution of the FORCAST images. We constrain the flux densities of this object at 19.7 − 37.1 µm. Additionally, we present in situ observations of four young stellar and protostellar objects in the SOFIA field, presumably associated with the W3 molecular cloud. Results from the model SED fitting tool of Robitaille et al. (2006; suggest that two objects (2MASS J02270352+6152357 and 2MASS J02270824+6152281) are intermediate-luminosity (∼ 236 − 432 L ⊙ ) protostars; one object (2MASS J02270887+6152344) is either a high-mass protostar with luminosity 3×10 3 L ⊙ or a less massive young star with a substantial circumstellar disk but depleted envelope; and one object (2MASS J02270743+6152281) is an intermediate-luminosity (∼ 768 L ⊙ ) protostar nearing the end of its envelope accretion phase or a young star surrounded by a circumstellar disk with no appreciable circumstellar envelope.

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UCHII Regions and Newly Born O-type Stars

Cited by 2 publications

References 7 publications

The infrared massive stellar content of M 83

The infrared massive stellar content of M 83

SOFIA/FORCAST ANDSPITZER/IRAC IMAGING OF THE ULTRACOMPACT H II REGION W3(OH) AND ASSOCIATED PROTOSTARS IN W3

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