Maser Action in Methanol Transitions

Voronkov, Maxim; Соболев, А. М.; Ellingsen, Simon; Ostrovskii, A. B.; Alakoz, A. V.

doi:10.1007/1-4020-3831-3_25

Cited by 2 publications

(3 citation statements)

References 5 publications

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“…Perhaps more importantly, modelling predicts that in some conditions the 6.6‐GHz class II transition can be weakly inverted, simultaneously with strong inversion in the 25‐GHz class I transitions. This situation may have recently been detected towards the archetypal class I maser source Orion KL (Voronkov et al 2005). Kurtz, Hofner & Álvarez (2004) found coincidence within 0.5 arcsec of class I and II methanol masers in one source, although there is a significant velocity difference between the two transitions suggesting that it may be a chance alignment along our line of sight.…”

Section: Introductionmentioning

confidence: 79%

“…The majority of the well‐studied class I methanol maser sources are ‘traditional’ class I sources with no (or weak) class II emission, Orion KL (Plambeck & Wright 1988; Johnston et al 1992), DR21 (Batrla & Menten 1988; Plambeck & Menten 1990) and Sgr B2 (Mehringer & Menten 1997). There are no strong class II methanol masers towards Orion KL, although weak masers, and possibly quasi‐thermal emission has been detected (Voronkov et al 2005). There is class II methanol maser emission towards DR21(OH), this likely to be from the same region as the OH maser emission (which is offset from the class I masers), but this has not been confirmed.…”

Section: Introductionmentioning

confidence: 99%

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The relationship between class I and class II methanol masers

Ellingsen

2005

Monthly Notices of the Royal Astronomical Society

124

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The Australia Telescope National Facility Mopra millimetre telescope has been used to search for 95.1-GHz class I methanol masers towards 62 6.6-GHz class II methanol masers. A total of 26 95.1-GHz masers were detected, 18 of these being new discoveries. Combining the results of this search with observations reported in the literature, a near complete sample of 66 6.6-GHz class II methanol masers has been searched in the 95.1-GHz transition, with detections towards 38 per cent (25 detections; not all of the sources studied in this paper qualify for the complete sample, and some of the sources in the sample were not observed in the present observations).There is no evidence of an anticorrelation between either the velocity range, or peak flux density of the class I and II transitions, contrary to suggestions from previous studies. The majority of class I methanol maser sources have a velocity range that partly overlaps with the class II maser transitions. The presence of a class I methanol maser associated with a class II maser source is not correlated with the presence (or absence) of main-line OH or water masers. Investigations of the properties of the infrared emission associated with the maser sources shows no significant difference between those class II methanol masers with an associated class I maser and those without. This may be consistent with the hypothesis that the objects responsible for driving class I methanol masers are generally not those that produce main-line OH, water or class II methanol masers.

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Section: Introductionmentioning

confidence: 79%

Section: Introductionmentioning

confidence: 99%

The relationship between class I and class II methanol masers

Ellingsen

2005

Monthly Notices of the Royal Astronomical Society

124

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“…The maser was associated with a massive protostellar core that could host a nascent high-mass star. Recent observations by Voronkov et al (2004) have also revealed methanol emission at 6.7 GHz in the OMC-1 region near the 25-GHz maser site, i.e. a class I maser source.…”

Section: Follow-up Observationsmentioning

confidence: 93%

A general catalogue of 6.7-GHz methanol masers

Pestalozzi

Minier²,

Booth

2005

A&A

227

268

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Abstract. Methanol masers are often detected in regions of intense star formation. Several studies in the last decade indicate that they may even be the earliest signpost of a high-mass star-forming region. Their powerful emission make them very good candidates for observations using both single-dish telescopes and interferometers, the latter allows detailed structural and dynamical studies of these objects. We have prepared a catalogue of all known 6.7-GHz methanol masers, discovered both by surveys that targeted possible associated objects and unbiased surveys covering a large fraction of galactic longitudes across the Galactic plane (−0.5• ≤ b ≤ 0.5• for most of the regions). The catalogue contains 519 sources which are listed with their kinematic (galactocentric and heliocentric) distances as well as possibly associated IR objects. We find that 6.7-GHz methanol masers clearly trace the molecular ring of our Galaxy, where most of the OB associations are located. The present list of masers also reports detections of other masing transitions of methanol as further information for the study of the maser phenomenon. In a further publication we will address some statistical considerations.

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Maser Action in Methanol Transitions

Cited by 2 publications

References 5 publications

The relationship between class I and class II methanol masers

The relationship between class I and class II methanol masers

A general catalogue of 6.7-GHz methanol masers

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