A Massive Protostar Embedded in the Scuba Core JCMT 18354-0649s

Zhu, Meiping; Davis, C. J.; Wu, Y. F.; Whitney, B. A.; Robitaille, Thomas; Peng, R.

doi:10.1088/0004-637x/739/1/53

Cited by 5 publications

(10 citation statements)

References 60 publications

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“…4.1.2. G25.40-0.14 Located at 5.7 kpc (Zhu et al 2011;Ai et al 2013), G25.40-0.14 is a UC H II region with a core halo structure (Garay et al 1993), also referred to as G25.4NW in Dewangan et al (2015). Even though G25.40-0.14 lies in the direction of W42, it is not thought to be associated with the W42 complex due to its very different 13 CO velocity components (58-69 km s −1 for W42 and 88-109 km s −1 for G25.40-0.14) as discussed by Ai et al (2013) and Dewangan et al (2015).…”

Section: Afgl 2591mentioning

confidence: 99%

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

Fedriani

Tan

Telkamp

et al. 2022

ApJ

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We present ∼10–40 μm SOFIA-FORCAST images of 11 isolated protostars as part of the SOFIA Massive (SOMA) Star Formation Survey, with this morphological classification based on 37 μm imaging. We develop an automated method to define source aperture size using the gradient of its background-subtracted enclosed flux and apply this to build spectral energy distributions (SEDs). We fit the SEDs with radiative transfer models, developed within the framework of turbulent core accretion (TCA) theory, to estimate key protostellar properties. Here, we release the sedcreator python package that carries out these methods. The SEDs are generally well fitted by the TCA models, from which we infer initial core masses M c ranging from 20–430 M ⊙, clump mass surface densities Σcl ∼ 0.3–1.7 g cm−2, and current protostellar masses m * ∼ 3–50 M ⊙. From a uniform analysis of the 40 sources in the full SOMA survey to date, we find that massive protostars form across a wide range of clump mass surface density environments, placing constraints on theories that predict a minimum threshold Σcl for massive star formation. However, the upper end of the m *−Σcl distribution follows trends predicted by models of internal protostellar feedback that find greater star formation efficiency in higher Σcl conditions. We also investigate protostellar far-IR variability by comparison with IRAS data, finding no significant variation over an ∼40 yr baseline.

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Section: Afgl 2591mentioning

confidence: 99%

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

Fedriani

Tan

Telkamp

et al. 2022

ApJ

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“…4.1.2. G25.40-0.14 Located at 5.7 kpc (Zhu et al 2011), G25.4-0.14 is an UC HII region with a core halo structure (Garay et al 1993). It is associated with the W42 complex (Woodward et al 1985;Dewangan et al 2015a).…”

Section: Afgl 2591mentioning

confidence: 99%

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

Fedriani¹,

Tan²,

Telkamp³

et al. 2022

Preprint

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We present ∼ 10 − 40 µm SOFIA-FORCAST images of 11 "isolated" protostars as part of the SOFIA Massive (SOMA) Star Formation Survey, with this morphological classification based on 37 µm imaging. We develop an automated method to define source aperture size based on the gradient of its background-subtracted enclosed flux and apply this to build spectral energy distributions (SEDs). We fit the SEDs with radiative transfer models, based on the Turbulent Core Accretion (TCA) theory, to estimate key protostellar properties. Here we release the sedcreator python package that carries out these methods. The SEDs are generally well-fit by the TCA models, from which we infer initial core masses M c ranging from 50 − 430 M , clump mass surface densities Σ cl ∼ 0.1 − 3 g cm −2 and current protostellar masses m * ∼ 2 − 40 M . From an uniform analysis of the 40 sources in the full SOMA survey to date, we find that massive protostars form across a wide range of clump mass surface density environments, placing constraints on theories that predict a minimum threshold Σ cl for massive star formation. However, the upper end of the m * − Σ cl distribution follows trends predicted by models of internal protostellar feedback that find greater star formation efficiency in higher Σ cl conditions. We also investigate protostellar FIR variability by comparison with IRAS data, finding no significant variation over a ∼40-year baseline.

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“…1 The VGPS 1420 MHz continuum contours of G25.4NW overlaid on (left) the 13 CO integrated intensity image (over the range 90-101 km s −1 ) and the HI single-channel map (right) at 95 km s −1 for the GMC G25.4-0.14 region. Contours are overlaid which show the 1420 MHz continuum emission at the level of 3σ (σ = 1 K) above the background emission of 29 K, and start from 67 K in steps of 57 K. The plus sign marks the position of the massive protostar JCMT18354-0649IRS1a found by Zhu et al (2011).…”

Section: Datamentioning

confidence: 99%

“…It is also on the list of the top two sources of IR-luminosity among the 18 radio-selected UCHII regions studied by Giveon et al (2007). Recently, a massive protostar (6-12 M ⊙ ) was found in the massive SCUBA core JCMT18354-0649S (Zhu et al 2011), which is about 1 ′ south of G25.4NW. It is believed to lie in the same molecular cloud as G25.4NW based on the smooth change of 13 CO and 18 CO spectral profiles.…”

Section: Introductionmentioning

confidence: 99%

“…In the case of JCMT18354-0649S, Zhu et al (2011) also found that if the far-side distance of 9.6 kpc was used, the mass of the central protostar derived from modeling the spectral energy distribution (SED) would be as high as 10-20 M ⊙ , and the temperature would be 4000-10 000 K, equivalent to a B2 star or earlier. Such a star should have detectable radio continuum and strong 24 µm MIR emission, which contradicts observational evidence.…”

Section: Introductionmentioning

confidence: 99%

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Properties of the UCHII region G25.4NW and its associated molecular cloud

Ai¹,

Zhu²,

Xiao³

et al. 2013

Res. Astron. Astrophys.

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UCHII G25.4NW is a bright IR source in the inner Galaxy region. New HI images from the VLA Galactic Plane Survey (VGPS) show clear absorption features associated with the UCHII region up to 95 km s −1 , and there is not any other absorptions up to the tangential velocity. It reveals that G25.4NW is at a near-side distance of 5.7 kpc, and it is located in the inner Galactic molecular ring region. Using the new distance, the bolometric luminosity of G25.4NW is estimated as 10 5.6 L ⊙ , which corresponds to an O6 star. It contains 460 M ⊙ of ionized gas. High-resolution 13 CO image from the Galactic Ring Survey (GRS) reveals that G25.4NW is part of a more extended star-formation complex with about 10 4 M ⊙ molecular gas.

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A Massive Protostar Embedded in the Scuba Core JCMT 18354-0649s

Cited by 5 publications

References 60 publications

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars

Properties of the UCHII region G25.4NW and its associated molecular cloud

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