A Chandra X-ray and Infrared Study of the Stellar Population in the High-Mass Star Forming Region IRAS 16562-3959

Montes, Virginie; Höfner, P.; Oskinova, L. M.; Linz, H.

doi:10.48550/arxiv.1806.06293

Cited by 1 publication

(4 citation statements)

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“…The closer knot located ∼15 NE of the central source is associated with the 92.3 GHz peak 18 in Guzmán et al (2014), as well as a K-band source (see Figure 12). It may correspond to the X-ray source 178 in Montes et al (2018). There is OH maser emission (Caswell 1998(Caswell , 2004, but no radio continuum emission detected.…”

Section: Iras 16562-3959mentioning

confidence: 95%

“…Guzmán et al (2010) carried out ATCA observations to reveal five 6 cm radio sources: a compact bright central (C) component, two inner lobes that are separated by about 7 and symmetrically offset from the central source, and two outer lobes that are separated by about 45 (see Figure 4 in Guzman et al 2010). The central radio source has a 3 mm counterpart, source 10 in Guzmán et al (2014), and an X-ray counterpart, source 161 in Montes et al (2018), and is associated with OH maser emission (Caswell 1998(Caswell , 2004. It is interpreted as a HC HII region based on hydrogen recombination line (HRL) observations (Guzmán et al 2014).…”

Section: Iras 16562-3959mentioning

confidence: 99%

“…The farther knot, located ∼36 northeast of the central source, has counterparts in all of the J, H, K bands. We did not find any associated X-ray source for this knot in the Montes et al (2018) refer to these maser sites as G305A and G305B, respectively, and we will adopt that nomenclature here.…”

Section: Iras 16562-3959mentioning

confidence: 99%

“…López-Calderón et al (2016) reported 13 CO(3-2) APEX observations of this region and showed that the high-mass protostellar candidate is located at the column density maximum Montes et al (2018). decomposed the wider region into 11 subclusters with results from Chandra X-ray observations together with…”

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confidence: 96%

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The SOFIA Massive (SOMA) Star Formation Survey. II. High Luminosity Protostars

Liu

Tan

Buizer

et al. 2019

ApJ

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We present multi-wavelength images observed with SOFIA-FORCAST from ∼10 to 40 µm of seven high luminosity massive protostars, as part of the SOFIA Massive (SOMA) Star Formation Survey. Source morphologies at these wavelengths appear to be influenced by outflow cavities and extinction from dense gas surrounding the protostars. Using these images, we build spectral energy distributions (SEDs) of the protostars, also including archival data from Spitzer, Herschel and other facilities. Radiative transfer (RT) models of Zhang & Tan (2018), based on Turbulent Core Accretion theory, are then fit to the SEDs to estimate key properties of the protostars. Considering the best five models fit to each source, the protostars have masses m * ∼ 12 − 64 M accreting at rates ofṁ * ∼ 10 −4 − 10 −3 M yr −1 inside cores of initial masses M c ∼ 100 − 500 M embedded in clumps with mass arXiv:1901.01958v2 [astro-ph.GA] 18 Feb 2019 2 Liu et al.surface densities Σ cl ∼ 0.1 − 3 g cm −2 and span a luminosity range of 10 4 − 10 6 L . Compared with the first eight protostars in Paper I, the sources analyzed here are more luminous, and thus likely to be more massive protostars. They are often in a clustered environment or have a companion protostar relatively nearby. From the range of parameter space of the models, we do not see any evidence that Σ cl needs to be high to form these massive stars. For most sources the RT models provide reasonable fits to the SEDs, though the cold clump material often influences the long wavelength fitting. However, for sources in very clustered environments, the model SEDs may not be such a good description of the data, indicating potential limitations of the models for these regions.

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Section: Iras 16562-3959mentioning

confidence: 95%