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

Liu, Mengyao; Tan, Jonathan C.; Buizer, James M. De; Zhang, Yichen; Beltrán, M. T.; Staff, Jan E.; Tanaka, Kei E. I.; Whitney, B. A.; Rosero, Viviana

doi:10.3847/1538-4357/ab07b7

Cited by 22 publications

(26 citation statements)

References 82 publications

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“…Overall, our model for IRAS 17527, based on a better defined SED and an improved version of the SED fitting tool, agrees reasonably well with the one derived by Varricatt (2011), and is within the range of parameters obtained for other intermediate-mass and massive young stars of similar characteristics (see e.g. Fazal et al 2008;Grave & Kumar 2009;Liu et al 2019).…”

Section: The Iras 17527-2439 Sed Modelsupporting

confidence: 80%

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS

Ferrero

Günthardt

García

et al. 2022

A&A

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Aims. We investigated the possible cause–effect relation between the wiggling shape of two stellar jets, MHO 1502 and MHO 2147, and the potential binarity of the respective driving stars. Methods. We present high-angular-resolution H2 (2.122 μm) and K-band images obtained with the Gemini South Adaptive Optics Imager (GSAOI) and the Gemini Multi-conjugate Adaptive Optics System (GeMS). The profiles of the jets are depicted in detail by the H2 images. We used K-band data to search for potential close companions to the previously suggested exciting sources, and used archive data to investigate these sources and the environments in which the jets are located. We also applied a model to reproduce the wiggling profiles of the jets. Results. MHO 1502 is composed of a chain of knots delineating the wiggling jet, suggesting that the driving source emitted them in an intermittent manner. Our K-band image of the previously proposed exciting star, IRAC 18064, shows two sources separated by ~240 AU, hinting at its binarity. However, as IRAC 18064 is located off the jet axis at ~2064 AU, it is questionable as to whether this source is the true exciting star. Moreover, the orbital model centred on IRAC 18064 suggests a binary companion at a much greater distance (~2200 AU) than the nearby star (at ~240 AU). On the other hand, the orbital model centred on the axis provides the best fits. Nevertheless, the precession model centred on the axis cannot be discarded, despite having larger residuals and χ2. MHO 2147 displays an S-shaped gentle continuous emission in H2. We identify two other jets in the field of MHO 2147: a previously reported quasi-perpendicular jet, MHO 2148, and a third jet adjacent to MHO 2147. The model that best fits the morphology of the MHO 2147 jet and that of its adjacent jet is precession. The exciting source of MHO 2147 may be a triple system.

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Section: The Iras 17527-2439 Sed Modelsupporting

confidence: 80%

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS

Ferrero

Günthardt

García

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

Section: The Iras 17527−2439 Sed Modelsupporting

confidence: 80%

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS

Ferrero,

Günthardt,

García

et al. 2021

Preprint

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Aims. We investigated the possible cause-effect relation between the wiggling shape of two stellar jets, MHO 1502 and MHO 2147, and the potential binarity of the respective driving stars. Methods. We present high-angular-resolution H 2 (2.122 µm) and K-band images obtained with the Gemini South Adaptive Optics Imager (GSAOI) and the Gemini Multi-conjugate Adaptive Optics System (GeMS). The profiles of the jets are depicted in detail by the H 2 images. We used K-band data to search for potential close companions to the previously suggested exciting sources, and used archive data to investigate these sources and the environments in which the jets are located. We also applied a model to reproduce the wiggling profiles of the jets. Results. MHO 1502 is composed of a chain of knots delineating the wiggling jet, suggesting that the driving source emitted them in an intermittent manner. Our K-band image of the previously proposed exciting star, IRAC 18064, shows two sources separated by ∼ 240 AU, hinting at its binarity. However, as IRAC 18064 is located off the jet axis at ∼ 2064 AU, it is questionable as to whether this source is the true exciting star. Moreover, the orbital model centred on IRAC 18064 suggests a binary companion at a much greater distance (∼ 2200 AU) than the nearby star (at ∼240 AU). On the other hand, the orbital model centred on the axis provides the best fits. Nevertheless, the precession model centred on the axis cannot be discarded, despite having larger residuals and χ 2 . MHO 2147 displays an S-shaped gentle continuous emission in H 2 . We identify two other jets in the field of MHO 2147: a previously reported quasi-perpendicular jet, MHO 2148, and a third jet adjacent to MHO 2147. The model that best fits the morphology of the MHO 2147 jet and that of its adjacent jet is precession. The exciting source of MHO 2147 may be a triple system.

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“…The optimum aperture was defined by which beyond 30% of that radius, the background flux increases is within 10% (Telkamp et al 2022, in prep). The integrated flux at Herschel and Spitzer wavelengths are derived following the methods in the SOMA survey (Liu et al 2019). We fit only the Herschel, WISE, Spitzer and SOFIA data to a grid of models following the Zhang & Tan (2018) radiative transfer models.…”

Section: Protostellar Properties From Sed Modelingmentioning

confidence: 99%

Isolated Massive Star Formation in G28.20-0.05

Law¹,

Tan²,

Gorai³

et al. 2022

Preprint

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We report high-resolution 1.3mm continuum and molecular line observations of the massive protostar G28.20-0.05 with ALMA. The continuum image reveals a ring-like structure with 2,000 au radius, similar to morphology seen in archival 1.3cm VLA observations. Based on its spectral index and associated H30α emission, this structure mainly traces ionized gas. However, there is evidence for ∼ 30 M of dusty gas near the main mm continuum peak on one side of the ring, as well as in adjacent regions within 3,000 au. A virial analysis on scales of ∼2,000 au from hot core line emission yields a dynamical mass of ∼ 80M . A strong velocity gradient in the H30α emission is evidence for a rotating, ionized disk wind, which drives a larger-scale molecular outflow. An infrared SED analysis indicates a current protostellar mass of m * ∼ 24 M forming from a core with initial mass M c ∼ 400 M in a clump with mass surface density of Σ cl ∼ 3 g cm −2 . Thus the SED and other properties of the system can be understood in the context of core accretion models. Structure-finding analysis on the largerscale continuum image indicates G28.20-0.05 is forming in a relatively isolated environment, with no other concentrated sources, i.e., protostellar cores, above ∼ 1 M found from ∼0.1 to 0.4 pc around the source. This implies that a massive star is able to form in relative isolation and the dearth of other protostellar companions within the ∼ 1 pc environs is a strong constraint on massive star formation theories that predict the presence of a surrounding protocluster.

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

Cited by 22 publications

References 82 publications

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS

Isolated Massive Star Formation in G28.20-0.05

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