A Parsec-scale Bipolar H<sub>2</sub> Outflow in the Massive Star-forming Infrared Dark Cloud Core MSXDC G053.11+00.05 MM1*

<sup>†</sup>

Kim, Hyun-Jeong; Koo, Bon‐Chul; Pyo, Tae‐Soo; Davis, C. J.

doi:10.3847/1538-4357/aace9f

Cited by 5 publications

(3 citation statements)

References 96 publications

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“…3). This prefers a near kinematic distance of the source (e.g., dnear =1.7 kpc adopted by Kim et al 2018).…”

Section: G05314+0007 (Iras 19270+1750)mentioning

confidence: 99%

VERA astrometry toward the Perseus arm gap

Sakai,

Nakanishi,

Kurahara

et al. 2021

Preprint

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The Perseus arm has a gap in Galactic longitudes (l) between 50 • and 80 • (hereafter the Perseus arm gap) where the arm has little star formation activity. To better understand the gap, we conducted astrometric observations with VERA and analyzed archival H I data. We report on parallax and proper motion results from four star-forming regions, of which G050.28-00.39 and G070.33+01.59 are likely associated with the gap. The measured parallaxes are 0.140±0.018 (mas), 0.726±0.038 (mas), 0.074±0.037 (mas), and 0.118±0.035 (mas) for G050.28-00.39, G053.14+00.07, G070.33+01.59, and G079.08+01.33, respectively. Since the fractional parallax error of G070.33+01.59 is large (0.5), we estimated a 3D kinematic distance of the source to be 7.7±1.0 kpc using both the LSR velocity (V LSR ) and the measured proper motion. Perseus-arm sources G049.41+00.32 and G050.28-00.39 lag relative to a Galactic rotation by 77±17 km s −1 and 31±10 km s −1 , respectively. The noncircular motion of G049.41+00.32 cannot be explained by the gravitational potential of the Perseus arm. We discovered rectangular holes with integrated brightness temperatures of < 30 K arcdeg in l vs. V LSR of the H I data. One of the holes is centered near (l, V LSR ) = (47 • , −15 km s −1 ), and G049.41+00.32 is associated with the rim of the hole. However, G050.28-00.39 is not associated with the hole. We found extended H I emission on one side of the Galactic plane when integrating the H I data over the velocity range covering the hole (i.e., V LSR = [−25, −5] km s −1 ). G049.41+00.32 and G050.28-00.39 are moving toward the emission. The Galactic H I disk at the same velocity range showed an arc structure, indicating that the disk was pushed from the lower side of the disk. All the observational results might be explained by a cloud collision with the Galactic disk.

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“…3). This prefers a near kinematic distance of the source (e.g., dnear =1.7 kpc adopted by Kim et al 2018).…”

Section: G05314+0007 (Iras 19270+1750)mentioning

confidence: 99%

VERA astrometry toward the Perseus arm gap

Sakai,

Nakanishi,

Kurahara

et al. 2021

Preprint

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“…Observations in NIR narrowband H 2 emission trace shockheated gas in molecular outflows and are useful to investigate the ejection processes in young stars (Navarete et al 2015;Kim et al 2018). In Figure 4 we present a three-color composite image of the outflow region using NIR continuum-subtracted H 2 emission at 2.12 μm (green), NIR H band at 1.6 μm (red), and Spitzer 4.5 μm (blue).…”

Section: Narrowband H 2 Imagementioning

confidence: 99%

Near-infrared Polarimetry and H₂ Emission toward Massive Young Stars: Discovery of a Bipolar Outflow Associated to S235 e2s3

Devaraj

Garatti

Dewangan

et al. 2023

ApJ

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We present a near-infrared H-band polarimetric study toward the S235 e2s3 protostar, obtained using the POLICAN instrument on the 2.1 m OAGH telescope. The images reveal a bipolar outflow with a total length of about 0.5 pc. The outflow nebulosity presents a high degree of linear polarization (∼80%) and reveals a centrosymmetric pattern with the polarization position angles. The polarization characteristics suggest their origin to be single scattering associated with dust in the outflow. Using multiwavelength archival data, we performed spectral energy distribution (SED) fitting based on radiative transfer models of turbulent core accretion theory. The best-fit SED model indicated that the protostar has a mass of 6.8 ± 1.2 M ⊙, with a disk accretion rate of 3.6 ± 1.2 × 10−4 M ⊙ yr−1 and a total bolometric luminosity of 9.63 ± 2.1 × 103 L ⊙. Narrowband H2 (2.12 μm) observations show shocked emission along the bipolar lobes tracing the jet’s interaction with the surrounding medium. The estimated H2 luminosity of the outflow is 2.3 − 1.3 + 3.5 L ⊙ , which matched the known power-law correlation with the source bolometric luminosity, similar to other high-mass outflows. The orientation of the bipolar outflow was found to be parallel to the local magnetic field direction. The overall results assert the fact that the S235 e2s3 source is a massive young star driving a highly collimated bipolar outflow through disk accretion.

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“…Observations in NIR narrowband H 2 emission trace shock-heated gas in molecular outflows and are useful to investigate the ejection processes in young stars (Navarete et al 2015;Kim et al 2018). In Figure 4 we present a three-color composite image of the outflow region using NIR continuum-subtracted H 2 emission at 2.12 µm (green), NIR H band at 1.6 µm (red), and Spitzer 4.5 µm (blue).…”

Section: Narrowband H 2 Imagementioning

confidence: 99%

Near-Infrared Polarimetry and H$_2$ emission toward Massive Young Stars: Discovery of a Bipolar Outflow associated to S235 e2s3

Devaraj¹,

Garatti²,

Dewangan³

et al. 2023

Preprint

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We present a near-infrared H band polarimetric study toward the S235 e2s3 protostar, obtained using the POLICAN instrument on the 2.1m OAGH telescope. The images reveal a bipolar outflow with a total length of about 0.5 pc. The outflow nebulosity presents a high degree of linear polarization (∼80%) and reveals a centrosymmetric pattern with the polarization position angles. The polarization characteristics suggest their origin to be single scattering associated with dust in the outflow. Using multiwavelength archival data, we performed spectral energy distribution (SED) fitting based on radiative transfer models of turbulent core accretion theory. The best-fit SED model indicated that the protostar has a mass of 6.8 ± 1.2 M ⊙ , with a disk accretion rate of 3.6 ± 1.2 × 10 −4 M ⊙ yr −1 and a total bolometric luminosity of 9.63 ± 2.1 × 10 3 L ⊙ . Narrowband H 2 (2.12 µm) observations show shocked emission along the bipolar lobes tracing the jet's interaction with the surrounding medium. The estimated H 2 luminosity of the outflow is 2.3 +3.5 −1.3 L ⊙ , which matched the known power-law correlation with the source bolometric luminosity, similar to other high-mass outflows. The orientation of the bipolar outflow was found to be parallel to the local magnetic field direction. The overall results assert the fact that the S235 e2s3 source is a massive young star driving a highly collimated bipolar outflow through disk accretion.

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A Parsec-scale Bipolar H₂ Outflow in the Massive Star-forming Infrared Dark Cloud Core MSXDC G053.11+00.05 MM1* ^†

Cited by 5 publications

References 96 publications

VERA astrometry toward the Perseus arm gap

VERA astrometry toward the Perseus arm gap

Near-infrared Polarimetry and H₂ Emission toward Massive Young Stars: Discovery of a Bipolar Outflow Associated to S235 e2s3

Near-Infrared Polarimetry and H$_2$ emission toward Massive Young Stars: Discovery of a Bipolar Outflow associated to S235 e2s3

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A Parsec-scale Bipolar H2 Outflow in the Massive Star-forming Infrared Dark Cloud Core MSXDC G053.11+00.05 MM1* †

Cited by 5 publications

References 96 publications

VERA astrometry toward the Perseus arm gap

VERA astrometry toward the Perseus arm gap

Near-infrared Polarimetry and H2 Emission toward Massive Young Stars: Discovery of a Bipolar Outflow Associated to S235 e2s3

Near-Infrared Polarimetry and H$_2$ emission toward Massive Young Stars: Discovery of a Bipolar Outflow associated to S235 e2s3

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Product

Resources

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A Parsec-scale Bipolar H₂ Outflow in the Massive Star-forming Infrared Dark Cloud Core MSXDC G053.11+00.05 MM1* ^†

Near-infrared Polarimetry and H₂ Emission toward Massive Young Stars: Discovery of a Bipolar Outflow Associated to S235 e2s3