Zeeman Effect Observations in Class I Methanol Masers. Issue Volume 14:Issue A30(2018) (August 2018)

• Record Type: Journal Article
• Authors: Momjian, Emmanuel; Sarma, Anuj P.
• Editors: Lago, Maria Teresa
• Is Part Of: Proceedings of the International Astronomical Union. Volume 14:Issue A30(2018)
• Page Start: 140
• Page End: 140
• Publication Date: 2018-08
• Subjects: Masers, -- magnetic fields, -- techniques: interferometric, -- radio lines: ISM; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921319003910
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: We report the detection of the Zeeman effect in the 44 GHz Class I methanol maser line toward the star forming region DR21W. The 44 GHz methanol masers in this source occur in a ∼3" linear structure that runs from northwest to southeast, with the two dominant components at each end, and several weaker maser components in between. Toward a 93 Jy maser in the dominant northwestern component, we find a significant Zeeman detection of −23.4 ± 3.2 Hz. If we use the recently published result of Lankhaar et al . (2018 ) that the F =5-4 hyperfine transition is responsible for the 44 GHz methanol maser line, then their value of z = −0.92 Hz mG −1 yields a line-of-sight magnetic field of B los =25.4 ± 3.5 mG. If Class I methanol masers are pumped in high density regions with n∼10 7–8 cm −3, then magnetic fields in these maser regions should be a few to several tens of mG. Therefore, our result in DR21W is certainly consistent with the expected values. Using the above noted splitting factor in past Zeeman effect detections in Class I methanol masers reported by Sarma & Momjian (2011 ) and Momjian & Sarma (2017 ) in the star forming regions OMC-2 and DR21(OH) result in B los values of 20.0 ± 1.2 mG and 58.2 ± 2.9 mG, respectively. These are also consistent with the expected values.