2010
DOI: 10.1088/0004-637x/713/1/423
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Abstract: We present high angular resolution (θ syn 0. ′′ 2) observations of the 23.1-GHz methanol (CH 3 OH) transition toward the massive star forming region NGC 7538 IRS 1. The two velocity components previously reported by Wilson et al. are resolved into distinct spatial features with brightness temperatures (T B ) greater than 10 4 K, proving their maser nature. Thus, NGC 7538 IRS 1 is the third region confirmed to show methanol maser emission at this frequency. The brighter 23.1-GHz spot coincides in position with … Show more

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Cited by 13 publications
(19 citation statements)
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References 37 publications
(51 reference statements)
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“…The OH masers are located southward and show no obvious disk structure or relation to the outflow direction (Hutawarakorn & Cohen 2003). H 2 CO and H 2 O masers are located near the center of the continuum emission, and the H 2 O masers are also almost aligned with the outflow (Galván-Madrid et al 2010). The 6.7 and 12.2-GHz CH 3 OH masers show a cone shape that opens to the north-west (Minier et al 2000).…”
Section: Introductionmentioning
confidence: 90%
See 1 more Smart Citation
“…The OH masers are located southward and show no obvious disk structure or relation to the outflow direction (Hutawarakorn & Cohen 2003). H 2 CO and H 2 O masers are located near the center of the continuum emission, and the H 2 O masers are also almost aligned with the outflow (Galván-Madrid et al 2010). The 6.7 and 12.2-GHz CH 3 OH masers show a cone shape that opens to the north-west (Minier et al 2000).…”
Section: Introductionmentioning
confidence: 90%
“…Besides the CH 3 OH masers, other maser species were detected around NGC 7538-IRS 1: OH, H 2 O, NH 3 , and H 2 CO (e.g., Hutawarakorn & Cohen 2003;Galván-Madrid et al 2010;Gaume et al 1991;Hoffman et al 2003). The OH masers are located southward and show no obvious disk structure or relation to the outflow direction (Hutawarakorn & Cohen 2003).…”
Section: Introductionmentioning
confidence: 99%
“…4.2.1). As in the case of the main 12.2 GHz methanol maser velocity component, the main component of the 22.2 GHz water masers has approximately the same peak velocity (−58.2 km s −1 ) as Component I of the 6 cm formaldehyde maser (−57.8 km s −1 ), both show a negative flux density rate of change, and the masers are not spatially coincident at sub-arcsecond resolution (e.g., see Surcis et al 2011 andGalván-Madrid et al 2010). However, in contrast to the formaldehyde masers, significant radial velocity drift of the water maser components is observed over the years, which makes it difficult to track the evolution of individual maser components, particularly when comparing results from different telescopes and different epochs.…”
Section: Water Masersmentioning
confidence: 99%
“…The blue ellipses show the approximate location of 6.7 GHz CH3OH maser groups. The identification of the CH3OH maser groups (A to E) and the radio continuum sources (Northern Core, Southern Core, and Southern Spherical) are as presented by Moscadelli & Goddi (2014 Galván-Madrid et al 2010). Doppler tracking was centered at a LSR velocity of −55.00 km s −1 .…”
Section: Introductionmentioning
confidence: 99%
“…All these groups are reported in Table B.1, where their position, peak flux density S ν , peak velocity, and velocity range are listed. We have compared our maser positions with the work of Galván-Madrid et al (2010), taking into account the proper motions from Moscadelli & Goddi (2014), µ RA = −2.45 mas/yr and µ Dec = −2.45 mas/yr. Both maps are consistent.…”
Section: Map Of the 22 Ghz Maser Emissionmentioning
confidence: 99%