Distribution and Motion of the Water Masers near IRAS 05413−0104

Claussen, M. J.; Marvel, Kevin B.; Wootten, Alwyn; Wilking, B. A.

doi:10.1086/311669

Cited by 110 publications

(122 citation statements)

References 13 publications

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“…Codella et al (2007) report no sign of jet rotation in the SiO emission near NK1, whereas in the region SK2−SK4 (∼10−14 from source), they find a gradient in a direction contrary to that reported for SK1 by Davis et al (2000). It is therefore also contrary to that of the disk which has a 5 km s −1 difference between the blue-shifted ammonia gas in the north-east and the red-shifted Claussen et al 1998;(8) Wiseman et al 2001. gas in the south-west (Wiseman et al 2001). However, Lee et al (2008) recently conducted a higher resolution rotation study of the HH 212 flow and report matching gradients in the southern and northern lobes of the SiO jet in a sense that also matches that of the disk.…”

Section: Hh 212 Nk1 and Sk1mentioning

confidence: 73%

Searching for jet rotation in Class 0/I sources observed with GEMINI/GNIRS

Coffey

Bacciotti

Chrysostomou

et al. 2010

A&A

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Context. In recent years, there has been a number of detections of gradients in the radial velocity profile across jets from young stars. The significance of these results is considerable. They may be interpreted as a signature of jet rotation about its symmetry axis, thereby representing the only existing observational indications supporting the theory that jets extract angular momentum from stardisk systems. However, the possibility that we are indeed observing jet rotation in pre-main sequence systems is undergoing active debate. Aims. To test the validity of a rotation argument, we must extend the survey to a larger sample, including younger sources. Methods. We present the latest results of a radial velocity analysis on jets from Class 0 and I sources, using high resolution data from the infrared spectrograph GNIRS on GEMINI South. We obtained infrared spectra of protostellar jets HH 34, HH 111-H, HH 212 NK1 and SK1. Results. The [Fe II] emission was unresolved in all cases and so Doppler shifts across the jet width could not be accessed. The H 2 emission was resolved in all cases except HH 34. Doppler profiles across the molecular emission were obtained, and gradients in radial velocity of typically 3 km s −1 identified. Conclusions. Agreement with previous studies implies they may be interpreted as jet rotation, leading to toroidal velocity and angular momentum flux estimates of 1.5 km s −1 and 1 × 10 −5 M yr −1 AU km s −1 respectively. However, caution is needed. For example, emission is asymmetric across the jets from HH 212 suggesting a more complex interpretation is warranted. Furthermore, observations for HH 212 and HH 111-H are conducted far from the source implying external influences are more likely to confuse the intrinsic flow kinematics. These observations demonstrate the difficulty of conducting this study from the ground, and highlight the necessity for high angular resolution via adaptive optics or space-based facilities.

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Section: Hh 212 Nk1 and Sk1mentioning

confidence: 73%

Searching for jet rotation in Class 0/I sources observed with GEMINI/GNIRS

Coffey

Bacciotti

Chrysostomou

et al. 2010

A&A

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“…Such conditions are easily met in the shocked gas compressed by winds as well as in circumstellar disks. This dual behavior is indeed observed, although most masers seem to be tracing outflowing rather than infalling gas (Claussen et al 1998b;Claussen 2002;Imai et al 2002;Furuya et al 2003). Interestingly, this dichotomy also seems to be present in galaxies with evidence of megamasers tracing both outflows and disks (Miyoshi et al 1995;Claussen et al 1998a).…”

Section: Introductionmentioning

confidence: 89%

Evidence for Evolution of the Outflow Collimation in Very Young Stellar Objects

Torrelles

Patel

Anglada

et al. 2003

ApJ

107

119

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We present Very Long Baseline Array proper-motion measurements of water masers toward two young stellar objects (YSOs) of the W75 N star-forming region. We find that these two objects are remarkable for having a similar spectral type, being separated by 0Љ .7 (corresponding to 1400 AU), and sharing the same environment, but with a strikingly different outflow ejection geometry. One source has a collimated, jetlike outflow at a 2000 AU scale, while the other has a shell outflow at a 160 AU scale expanding in multiple directions with respect to a central compact radio continuum source. This result reveals that outflow collimation is not only a consequence of ambient conditions but is something intrinsic to the individual evolution of stars and brings to light the possibility of noncollimated outflows in the earliest stages of YSOs.

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“…Water masers have been identified with the jet-disc interaction in a low mass YSO (Moscadelli et al 2006) and with a rotating disc around an intermediate mass YSO (Trinidad et al 2009). In more cases, the masers clearly trace a bow shock (Claussen et al 1998;Furuya et al 2000;Sanna et al 2012;Trinidad et al 2013;Burns et al 2015Burns et al , 2016 and it can be argued that quantifiable physical properties like outflow velocity and outflow momentum rate can be most reliably derived from maser bowshocks.…”

Section: Introductionmentioning

confidence: 99%

Bow shocks in a newly discovered maser source in IRAS 20231+3440

Ogbodo

Burns

Handa

et al. 2017

Monthly Notices of the Royal Astronomical Society

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From measuring the annual parallax of water masers over one and a half years with VERA, we present the trigonometric parallax and corresponding distance of another newly identified water maser source in the region of IRAS 20231+3440 as π = 0.611 ± 0.022 mas and D = 1.64 ± 0.06 kpc respectively. We measured the absolute proper motions of all the newly detected maser spots (30 spots) and presented two pictures describing the possible spatial distribution of the water maser as the morphology marks out an arc of masers whose average proper motion velocity in the jet direction was 14.26 km s −1 . As revealed by the ALLWISE composite image, and by applying the colour-colour method of YSO identification and classification on photometric archived data, we identified the driving source of the north maser group to be a class I, young stellar object. To further probe the nature of the progenitor, we used the momentum rate maximum value (1.2×10 −4 M yr −1 km s −1 ) of the outflow to satisfy that the progenitor under investigation is a low mass young stellar object concurrently forming alongside an intermediate-mass YSO ∼ 60, 000 au (∼ 37 arcsecs) away from it.

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Distribution and Motion of the Water Masers near IRAS 05413−0104

Cited by 110 publications

References 13 publications

Searching for jet rotation in Class 0/I sources observed with GEMINI/GNIRS

Searching for jet rotation in Class 0/I sources observed with GEMINI/GNIRS

Evidence for Evolution of the Outflow Collimation in Very Young Stellar Objects

Bow shocks in a newly discovered maser source in IRAS 20231+3440

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