ИЕ

И. Е. Вальтц

Astro Space Center

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V. I. Slysh

Astro Space Center

O. S. Bayandina

Arcetri Astrophysical Observatory

S. V. Kalenskiĭ

Astro Space Center

V. Migenes

Texas Southern University

НН

Н. Н. Шахворостова

Astro Space Center

G. M. Larionov

Russian Academy of Sciences

АВ

А. В. Алакоз

Astro Space Center

S. Kurtz

Universidad Nacional Autónoma de México

Ross A. Burns

Pioneer (Japan)

L. N. Volvach

Special Astrophysical Observatory

Cooperative Institutions

Center for Astrophysics Harvard & Smithsonian

Astro Space Center

Max Planck Institute for Radio Astronomy

Russian Academy of Sciences

Universidad de Guanajuato

Union astronomique internationale

P.N. Lebedev Physical Institute of the Russian Academy of Sciences

National Astronomical Observatory of Japan

Lomonosov Moscow State University

Max Planck Society

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Magnetic Fields in 7 Young Stellar Objects Observed with Nançay Radio Telescope

Proceedings of the International Astronomical Union (2013)

O. S. Bayandina А. В. Алакоз И. Е. Вальтц

Abstract Magnetic fields (MF) can play an essential role in the evolution of the interstellar medium - especially at the early evolutionary stages. Small scale research related to the interaction of MF and pre-stellar condensations are unresolved issues. In quantitative terms, submissions about forming a full picture of gas-dust fragments evolution are far from complete, considering delay of their collapse caused by MF and the reverse effect of self-gravitating objects on the transformation of force lines and changing the values of local strength. The role of these interrelated processes is very important in the estimation of time of evolution of protostellar structures. In contrast to OH, in methanol molecule (most investigating at the moment) there is no unpaired electron, and the Zeeman splitting of the energy levels in CH 3 OH regards only the levels caused by the nuclear spin. Therefore, Zeeman spectrum in methanol is certainly not going to be as effective as in OH. However, since many methanol masers - Class I (MMI - formed at the earliest stage of the evolution of gas and dust condensations) and Class II (MMII - the area around very young stars and protoplanetary disks) - are associated with OH masers, then from spectra of OH masers the parameters of MF can be estimated, at least, near different methanol masers classes, i.e. in condensations which are at different evolutionary stages. This report presents the results of polarization observations 7 OH maser sources at the NRT (France). The main goal is comparing similarities and differences in MF strength and orientation in these masers, which essentially different according to the type of methanol masers associated with them, i.e. the evolutionary type.

Protostar

10.1017/s1743921314001665

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FLUX DENSITIES OF DISCRETE RADIO SOURCES AT 3.5 cm.

Izvestiya Ordena Trudovogo Krasnogo Znameni Krymskoj Astrofizicheskoj Observatorii (1971)

A. E. Andrievskii E. E. Spangenberg И. Е. Вальтц

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Multi-epoch VLBI of a double maser super burst

evn (2018)

Ross A. Burns O. S. Bayandina Gábor Orosz M. Olech K. Immer

Epoch (astronomy)

Very-long-baseline interferometry

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Total linear polarization in the OH maser W75N: VLBA polarization structure.

American Astronomical Society Meeting Abstracts (2001)

V. Migenes V. I. Slysh И. Е. Вальтц S. Yu. Lyubchenko S. Horiuchi

Polarization in astronomy

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Map of the 6.7 GHz class II methanol maser emission of the protoplanetary disk G23.01-0.41

Astronomy Reports (2011)

S. V. Polushkin И. Е. Вальтц

Protostar

Parallax

Ellipse

Very-long-baseline interferometry

Line (geometry)

Line-of-sight

Vetting

10.1134/s1063772911040068

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Citations (1)

The discovery of methanol maser lines at 1.9 mm.

IAU Symposium (1997)

V. I. Slysh S. V. Kalenskiĭ И. Е. Вальтц

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Flux densities of discrete radio sources at 3.5 cm wavelength.

ATsir (1968)

A. E. Andrievskij E. E. Spangenberg И. Е. Вальтц Л. М. Гиндилис A. G. Gorshkov

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The detection of new methanol masers in the 5−1–40 E line

Astronomy Reports (2001)

S. V. Kalenskiĭ V. I. Slysh И. Е. Вальтц A. Winnberg L. E. B. Johansson

Outflow

Line (geometry)

Bipolar outflow

Opacity

10.1134/1.1336598

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Citations (21)

Overview of the Maser Monitoring Organisation

Proceedings of the International Astronomical Union (2022)

Ross A. Burns Agnieszka Kobak A. Caratti o Garatti А. М. Толмачев A. E. Volvach

Abstract The Maser Monitoring Organisation is a collection of researchers exploring the use of time-variable maser emission in the investigation of astrophysical phenomena. The forward directed aspects of research primarily involve using maser emission as a tool to investigate star formation. Simultaneously, these activities have deepened knowledge of maser emission itself in addition to uncovering previously unknown maser transitions. Thus a feedback loop is created where both the knowledge of astrophysical phenomena and the utilised tools of investigation themselves are iteratively sharpened. The project goals are open-ended and constantly evolving, however, the reliance on radio observatory maser monitoring campaigns persists as the fundamental enabler of research activities within the group.

10.1017/s1743921323003381

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Hyperfine structure of the methanol molecule as traced by Class I methanol masers

Monthly Notices of the Royal Astronomical Society (2024)

I. I. Agafonova O. S. Bayandina Y. Gong C. Henkel Kee‐Tae Kim

ABSTRACT We present results on simultaneous observations of Class I methanol masers at 25, 36, and 44 GHz towards 22 Galactic targets carried out with the Effelsberg 100-m telescope. The study investigates relations between the hyperfine (HF) structure of the torsion–rotation transitions in CH$_3$OH and maser activity. By analysing the radial velocity shifts between different maser lines together with the patterns of the HF structure based on laboratory measurements and quantum-chemical calculations, we find that in any source only one specific HF transition forms the maser emission and that this transition changes from source to source. The physical conditions leading to this selective behaviour are still unclear. Using accurate laboratory rest frequencies for the 25 GHz transitions, we have refined the centre frequencies for the HF multiplets at 36, 44, and 95 GHz: $f_{\scriptscriptstyle 36} = (36169.2488\pm 0.0002_{\scriptscriptstyle \rm stat} \pm 0.0004_{\scriptscriptstyle \rm sys})$ MHz. $f_{\scriptscriptstyle 44} = (44069.4176\pm 0.0002_{\scriptscriptstyle \rm stat} \pm 0.0004_{\scriptscriptstyle \rm sys})$ MHz, and $f_{\scriptscriptstyle 95} = (95169.4414\pm 0.0003_{\scriptscriptstyle \rm stat} \pm 0.0004_{\scriptscriptstyle \rm sys})$ MHz. Comparison with previous observations of 44 GHz masers performed 6–10 yr ago with a Korean 21-m Korean Very Long Baseline Interferometry Network telescope towards the same targets confirms the kinematic stability of Class I maser line profiles during this time interval and reveals a systematic radial velocity shift of $0.013\pm 0.005$ km s$^{-1}$ between the two telescopes.

10.1093/mnras/stae1815

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