A Rotating Disk around a High-Mass Young Star

Zhang, Qizhou; Hunter, T. R.; Sridharan, T. K.

doi:10.1086/311609

Cited by 125 publications

(136 citation statements)

References 13 publications

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“…If the disk is inclined 27¡ with respect to the line of sight (perpendicular to the outÑow) then we expect a disk height above the midplane of D70 AU. This is signiÐcantly smaller than the 10,000 AU diameter core or the 1700 AU core detected NH 3 CH 3 CN around the massive YSO IRAS 20126]4104 (Cesaroni et al 1997(Cesaroni et al , 1999Zhang, Hunter, & Sridharan 1998).…”

Section: Rotation and Mass Of The Diskmentioning

confidence: 74%

A 1000 AU Rotating Disk around the Massive Young Stellar Object G192.16−3.82

Shepherd

Kurtz

1999

ApJ

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We present evidence for a circumstellar disk around the luminous young stellar object G192.16[3.82. Observations of 2.6 mm, 7 mm, and 3.6 cm continuum emission and 13CO, C18O, and maser line H 2 O emission support the interpretation that a 1000 AU rotating disk exists around the central B2 star. The disk major axis is roughly perpendicular to the outÑow, and the maser velocities are consistent with Keplerian rotation. The mass of the disk plus circumstellar envelope traced by millimeter continuum emission is D15The source is embedded in a 500 molecular cloud from which a massive M _ . M _ outÑow emerges. Updated outÑow parameters yield a total Ñow mass of 95 and a mass Ñow rate of M _ 5.6 ] 10~4 yr~1. The outÑow opening angle, deÐned by a 13CO shell, is approximately 90¡. A weak, M _ one-sided, ionized jet emanates from the young stellar object system. The estimated momentum rate of the jet (D10~3 km s~1 yr~1) is about a factor of 4 too low to power the Ñow. These results are M

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Section: Rotation and Mass Of The Diskmentioning

confidence: 74%

A 1000 AU Rotating Disk around the Massive Young Stellar Object G192.16−3.82

Shepherd

Kurtz

1999

ApJ

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“…If massive OB stars are formed by accretion, we expect that disks and jets will be present in their earliest stages of evolution, as in the case of low-mass stars. Accretion disks and collimated outflows around Btype protostars have been tentatively reported toward Cepheus A HW2 (Rodríguez et al 1994;Torrelles et al 1996), IRAS 20126+4104 (Cesaroni et al 1997;Zhang, Hunter, & Sridharan 1998), G192.16-3.82 (Shepherd et al 1998Devine et al 1999;Shepherd, Claussen, & Kurtz 2001), AFGL 5142 (Zhang et al 2002), and AFGL 2591 (Trinidad et al 2003). A possible collimated outflow associated with a luminous O-type protostar is IRAS 16547À4247, a bright infrared source that is associated with a triple radio source consisting of a compact central object and two outer lobes (Garay et al 2003).…”

Section: Introductionmentioning

confidence: 93%

VLA and BIMA Observations toward the Exciting Source of the Massive HH 80–81 Outflow

Gómez¹,

Rodrı́guez²,

Girart

et al. 2003

ApJ

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We present high angular resolution Very Large Array (VLA) and Berkeley-Illinois-Maryland Association (BIMA) observations of NH 3 , HCO + , HCN, and SO molecular emission and 1.4, 3.5, and 7 mm continuum emission toward the exciting source of the HH 80-81 system. This object is one of the few massive protostars known to be driving a collimated outflow. We report the first detection of SO 5 5 -4 4 molecular emission toward the exciting source of HH 80-81, suggesting that this transition may be a good tracer of molecular gas near massive protostars. We also detected toward this source dust continuum emission at 1.4 and 3.5 mm. From the SO molecular emission and the dust emission we roughly estimated that the molecular mass associated with the circumstellar surroundings of the exciting source of the thermal jet is in the range 1-3 M . Weak and broad (2, 2) ammonia emission was also found in the direction of the jet, suggesting the presence of small amounts of molecular gas at high temperatures (>50 K). The VLA observations show the presence of three ammonia components toward the HH 80-81 region. The brightest component peaks at $8 00 northeast of the thermal jet and is associated with the H 2 O maser spots in the region. A second ammonia clump is located about 25 00 northeast of the jet and is associated with Class I methanol masers. The third ammonia component is located 1 0 south of the thermal jet and may be a molecular core, yet without stellar formation. The BIMA observations show that the strongest emission in the HCO + and HCN lines originates close to the H 2 O maser and covers the same spatial region and velocity range as the brightest ammonia component.

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“…-IRAS 20126+4104 is associated with a Keplerian disk rotating about a ∼7 M protostar (Cesaroni et al 1997Zhang et al 1998); -the disk is also seen in silhouette as a dark lane at nearand mid-IR wavelengths (Sridharan et al 2005;De Buizer et al 2007); -the YSO is powering a bipolar jet/outflow, imaged in a variety of tracers from ∼1 down to ∼100 mas from the star (Wilking et al 1990;Cesaroni et al 1997Cesaroni et al , 1999Cesaroni et al , 2005Shepherd et al 2000;Su et al 2007;Shinnaga et al 2008;Hofner et al 1999Hofner et al , 2007Moscadelli et al 2000Moscadelli et al , 2005Trinidad et al 2005); -the jet/outflow appears to be undergoing precession (Shepherd et al 2000;Cesaroni et al 2005;Lebrón et al 2006), perhaps caused by the presence of another YSO A&A 526, A66 (2011) detected at radio and IR wavelengths (Hofner et al 1999;Sridharan et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Methanol and water masers in IRAS 20126+4104: the distance, the disk, and the jet

Moscadelli

Cesaroni

Rioja

et al. 2010

A&A

104

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Context. Knowledge of the distance to high-mass star forming regions is crucial to obtain accurate luminosity and mass estimates of young OB-type (proto)stars and thus better constrain their nature and age. IRAS 20126+4104 is a special case, being the best candidate of a high-mass (proto)star surrounded by an accretion disk. Such a fact may be used to set constraints on theories of highmass star formation, but requires confirmation that the mass and luminosity of IRAS 20126+4104 are indeed typical of a B0.5 star, which in turn requires an accurate estimate of the distance. Aims. The goal of our study is twofold: to determine the distance to IRAS 20126+4104, using the parallax of H 2 O masers associated with the source, and unveil the 3D velocity field of the disk, through proper motion measurements of the 6.7 GHz CH 3 OH masers. At the same time, we can also obtain an estimate of the systemic velocity in the plane of the sky of the disk+star system. Methods. We used the Very Long Baseline Array and the European VLBI Network to observe the 22.2 GHz H 2 O and 6.7 GHz CH 3 OH masers in IRAS 20126+4104 at a number of epochs suitably distributed in time. The absolute positions of the maser features were established with respect to reference quasars, which allowed us to derive absolute proper motions. Results. From the parallax of the H 2 O masers we obtain a distance of 1.64 ± 0.05 kpc, which is very similar to the value adopted so far in the literature (1.7 kpc) and confirms that IRAS 20126+4104 is a high-mass (proto)star. From the CH 3 OH masers we derive the component in the plane of the sky of the systemic velocity of the disk+star system (−16 km s −1 in right-ascension and +7.6 km s −1 in declination). Accurate knowledge of the distance and systemic velocity allows us to improve on the model fit to the H 2 O maser jet presented in a previous study. Finally, we identify two groups of CH 3 OH maser features, one undergoing rotation in the disk and possibly distributed along a narrow ring centered on the star, the other characterised by relative proper motions indicating that the features are moving away from the disk, perpendicular to it. We speculate that the latter group might be tracing the disk material marginally entrained by the jet. Conclusions. VLBI multi-epoch observations with phase referencing are confirmed to be an excellent tool for distance determinations and for the investigation of the structure and 3D velocity field within a few 100 AU from newly born high-mass stars.

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A Rotating Disk around a High-Mass Young Star

Cited by 125 publications

References 13 publications

A 1000 AU Rotating Disk around the Massive Young Stellar Object G192.16−3.82

A 1000 AU Rotating Disk around the Massive Young Stellar Object G192.16−3.82

VLA and BIMA Observations toward the Exciting Source of the Massive HH 80–81 Outflow

Methanol and water masers in IRAS 20126+4104: the distance, the disk, and the jet

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