Detection of the ^{2}Π_{3/2}, J = 5/2 State of OH at 5-CENTIMETER Wavelength

Yen, J. L.; Zuckerman, B.; Palmer, Patrick; Penfield, H.

doi:10.1086/180342

Cited by 28 publications

(16 citation statements)

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“…Often seen in association with 6668‐MHz methanol, the 6035‐MHz ( 2 Π 3/2 J = 5/2, F = 3−3) excited‐state OH maser was first detected in the late‐1960s/early‐1970s (e.g. Yen et al 1969; Rydbeck, Kollberg & Elldér 1970; Zuckerman et al 1972; Knowles et al 1973). After a number of small‐scale targeted observations (Knowles, Caswell & Goss 1976; Guilloteau et al 1984), an extensive search by Caswell & Vaile (1995) detected 72 sources (of which 52 were new to that survey).…”

Section: The Mmb Galactic Plane Surveymentioning

confidence: 99%

The 6-GHz multibeam maser survey - I. Techniques

Green

Caswell

Fuller

et al. 2009

Monthly Notices of the Royal Astronomical Society

159

163

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A new seven‐beam 6–7 GHz receiver has been built to survey the Galaxy and the Magellanic Clouds for newly forming high‐mass stars that are pinpointed by strong methanol maser emission at 6668 MHz. The receiver was jointly constructed by Jodrell Bank Observatory (JBO) and the Australia Telescope National Facility (ATNF) and allows simultaneous coverage at 6668 and 6035 MHz. It was successfully commissioned at Parkes in 2006 January and is now being used to conduct the Parkes–Jodrell multibeam maser survey of the Milky Way. This will be the first systematic survey of the entire Galactic plane for masers of not only 6668‐MHz methanol, but also 6035‐MHz excited‐state hydroxyl. The survey is two orders of magnitude faster than most previous systematic surveys and has an rms noise level of ∼0.17 Jy. This paper describes the observational strategy, techniques and reduction procedures of the Galactic and Magellanic Cloud surveys, together with deeper, pointed, follow‐up observations and complementary observations with other instruments. It also includes an estimate of the survey detection efficiency. The 111 d of observations with the Parkes telescope have so far yielded >800 methanol sources, of which ∼350 are new discoveries. The whole project will provide the first comprehensive Galaxy‐wide catalogue of 6668‐MHz and 6035‐MHz masers.

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Section: The Mmb Galactic Plane Surveymentioning

confidence: 99%

The 6-GHz multibeam maser survey - I. Techniques

Green

Caswell

Fuller

et al. 2009

Monthly Notices of the Royal Astronomical Society

159

163

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“…Since the original discovery of emission from the 2 Π 3/2 , J = 5/2 (Yen et al 1969), many surveys were made for detection of 5 cm maser emission toward a variety of sources (Knowles et al 1976;Guilloteau et al 1984;Smits 1994). Caswell and Vaile (1995) surveyed for 6035…”

Section: Comparison With Observationsmentioning

confidence: 99%

5 Centimeter OH Masers as Diagnostics of Physical Conditions in Star‐forming Regions

Pavlakis

Kylafis

2000

ApJ

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We demonstrate that the observed characteristics of the 5 cm OH masers in star-forming regions can be explained with the same model and the same parameters as the 18 cm and the 6 cm OH masers. In our already published study of the 18 cm and the 6 cm OH masers in star-forming regions we had examined the pumping of the 5 cm masers, but did not report the results we had found because of some missing collision rate coefficients, which in principle could be important. The recently published observations on the 5 cm masers of OH encourage us to report our old calculations along with some new ones that we have performed. These calculations, in agreement with the observations, reveal the main lines at 5 cm as strong masers, the 6049 MHz satellite line as a weak maser, and the 6017 MHz satellite line as never inverted for reasonable values of the parameters.

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“…Caswell 1999;Forster & Caswell 1999;Argon et al 2000;Edris et al 2007;Beuther et al 2019;Qiao et al 2020). They are sometimes accompanied by the excited-state OH ( 2 Π 3/2 , J = 5/2) transitions at 5 cm wavelength, where the main line 6035 MHz dominates in most cases (Yen et al 1969;Knowles et al 1976;Smits 1994;Caswell & Vaile 1995;Baudry et al 1997;Caswell 2001Caswell , 2003Avison et al 2016). As this excited state of OH lies immediately above the ground state, it provides a critial test for maser pumping schemes (Baudry et al 1997;Pavlakis & Kylafis 2000;Cragg et al 2002).…”

Section: Introductionmentioning

confidence: 99%

A search for the OH 6035 MHz line in high-mass star-forming regions

Szymczak

Wolak

Bartkiewicz

et al. 2020

A&A

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Context. The excited states of OH masers detected in the environment of high-mass young stellar objects (HMYSOs) are important for improving our understanding of the physical conditions of these objects and also provide information about their magnetic fields. Aims. We aim to search for excited-state OH 6035 MHz maser emission in HMYSOs which might have escaped detection in previous surveys or were never searched for. Methods. A sample of HMYSOs derived from untargeted surveys of the 6668 MHz methanol maser line was observed at 6035 MHz OH transition with the Torun 32 m radio telescope. The 6035 MHz detections were observed in the OH 6031 MHz line. Two-thirds of the detections were observed at least three times over a two-year period. Results. Out of 445 targets, 37 were detected at 6035 MHz, including seven new discoveries. The 6031 MHz line was detected towards ten 6035 MHz sources, one of which was not previously reported. All the newly detected sources are faint with the peak flux density lower than 4 Jy and show significant or high variability on timescales of 4 to 20 months. Zeeman pair candidates identified in three new sources imply a magnetic field intensity of 2–11 mG. Comparison of our spectra with those obtained ~10 yr ago indicates different degrees of variability but there is a general increase in the variability index on an ~25 yr timescale, usually accompanied by significant changes in the profile shape.

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Detection of the ^{2}Π_{3/2}, J = 5/2 State of OH at 5-CENTIMETER Wavelength

Cited by 28 publications

References 0 publications

The 6-GHz multibeam maser survey - I. Techniques

The 6-GHz multibeam maser survey - I. Techniques

5 Centimeter OH Masers as Diagnostics of Physical Conditions in Star‐forming Regions

A search for the OH 6035 MHz line in high-mass star-forming regions

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