Expansion of methanol maser rings

Bartkiewicz, A.; Sanna, A.; Szymczak, M.; Moscadelli, L.; Langevelde, H. J. van

doi:10.1017/s1743921317010055

Cited by 2 publications

(1 citation statement)

References 16 publications

(21 reference statements)

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“…A follow-up study in the near-IR and mid-IR again found no evidence to support the idea that these rings trace protostellar disks (De Buizer et al 2012). Proper motion studies show that the ring of masers in G23.657-0.127 is expanding (Szymczak et al 2017) and while the interpretation is still unclear, it may be the result of a disk wind (Bartkiewicz et al 2017).…”

Section: Spatial and Kinematic Structuresmentioning

confidence: 97%

The Extraordinary Outburst in the Massive Protostellar System NGC 6334I-MM1: Emergence of Strong 6.7 GHz Methanol Masers

Hunter

Brogan

MacLeod

et al. 2018

ApJ

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We report the first sub-arcsecond VLA imaging of 6 GHz continuum, methanol maser, and excitedstate hydroxyl maser emission toward the massive protostellar cluster NGC6334I following the recent 2015 outburst in (sub)millimeter continuum toward MM1, the strongest (sub)millimeter source in the protocluster. In addition to detections toward the previously known 6.7 GHz Class II methanol maser sites in the hot core MM2 and the UCHII region MM3 (NGC6334F), we find new maser features toward several components of MM1, along with weaker features ∼ 1 ′′ north, west, and southwest of MM1, and toward the non-thermal radio continuum source CM2. None of these areas have heretofore exhibited Class II methanol maser emission in three decades of observations. The strongest MM1 masers trace a dust cavity, while no masers are seen toward the strongest dust sources MM1A, 1B and 1D. The locations of the masers are consistent with a combination of increased radiative pumping due to elevated dust grain temperature following the outburst, the presence of infrared photon propagation cavities, and the presence of high methanol column densities as indicated by ALMA images of thermal transitions. The non-thermal radio emission source CM2 (2 ′′ north of MM1) also exhibits new maser emission from the excited 6.035 and 6.030 GHz OH lines. Using the Zeeman effect, we measure a line-of-sight magnetic field of +0.5 to +3.7 mG toward CM2. In agreement with previous studies, we also detect numerous methanol and excited OH maser spots toward the UCHII region MM3, with predominantly negative line-of-sight magnetic field strengths of −2 to −5 mG and an intriguing south-north field reversal.

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Section: Spatial and Kinematic Structuresmentioning

confidence: 97%