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Structure of the H2O Maser in NGC 2071 IRS 1 from Observations on the Ground-Space Radio Interferometer RadioAstron

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Abstract

The observational data of an H2О maser at a frequency of 22.2280 GHz in the dark reflection nebula NGC 2071 in the direction of the infrared object IRS 1 at the target coordinates RA(2000) = \({{05}^{{\text{h}}}}{{47}^{{\text{m}}}}04_{.}^{{\text{s}}}758\), DEC(2000) = \(00{}^\circ 21' 42_{.}^{'' }700\) have been processed as part of the scientific program of the ground-space interferometer RadioAstron. The duration of the session on January 11, 2014 was 70 min. The space radio telescope (SRT-10) and three radio telescopes of the ground-based network took part in the observations: RT-32 (Medicina, Italy), RT-32 (Toruń, Poland), and RT-64 (Kalyazin, Russia). The following parameters were implemented: angular resolution 70 μs at the ground-space baseline with maximum baseline projections 3.1 ED (\( \sim {\kern 1pt} 40{\kern 1pt} {\kern 1pt} 000\) km); synthesized beam of the ground-based part of the interferometer \(0.006'' \times 0.0006'' \) (PA = –23°); spectral resolution 7.81 kHz (i.e., 0.11 km/s). A map of the distribution of maser spots with 13 spatial components was obtained. The map has a size \( \sim {\kern 1pt} 100 \times 100\) mas (milliarcseconds), which corresponds to \( \sim 40 \times 40\) AU at a distance of 390 pc to the nebula. The range of the line-of-sight velocities of the components is 4.7–20.5 km/s with a width of spectral features 0.2–0.6 km/s; the density of the correlated flux at the line maximum varies from \( \sim {\kern 1pt} 4\) to \( \sim {\kern 1pt} 29\) Jy. There was recorded one spatial component (with a radial velocity of 14.3 km/s) for which there was a correlation at the ground-space baselines SRT–Tr and SRT–Mc at an ultrahigh angular resolution with a reliability level above 6σ. Based on the analysis of the dependence of the visibility function on the baseline projections, a two-component model is proposed for the spatial structure of this component with the angular dimensions of the extended and compact constituents 4 mas and 0.06 mas, i.e., 1.56 AU (with an uncertainty of 10%) and 0.023 AU (with an uncertainty of 50%), respectively.

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  1. http://www.asc.rssi.ru/radioastron/index.html

  2. http://www.asc.rssi.ru/radioastron/news/newsl/ru/newsl_36_ru.pdf

  3. https://link.springer.com/content/pdf/10.1134/S0038094612070143.pdf

  4. https://www.evn.com.vn/

  5. http://asc-lebedev.ru/index.php?dep=6&page=5

  6. http://www.aips.nrao.edu

  7. http://www.asc.rssi.ru/shaddow/IMAGE1_NGC2071_180-260_512.jpg

  8. https://www.iram.fr/IRAMFR/GILDAS/

  9. http://astrogeo.org/pima/

  10. https://www.originlab.com/

  11. http://www.asc.rssi.ru/shaddow/IMAGE2_Seth-map_with_2014.jpg

  12. http://www.asc.rssi.ru/shaddow/IMAGE3_Tsutsumi_with_2014.jpg

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ACKNOWLEDGMENTS

The RadioAstron project is carried out by the Astro Space Center of the Lebedev Physical Institute of the Russian Academy of Sciences and the Lavochkin Research and Production Association under a contract with the State Corporation ROSCOSMOS together with many scientific and technical organizations in Russia and other countries.

This study used the observations at the radio telescope in Medicina, at the Radio Astronomy Observatory of the National Institute for Astrophysics INAF (Italy).

This study is partly based on the observations made with the 32-m radio telescope (Tr) in Toruń (Toruń Astronomy Center of the Nicolaus Copernicus University, Poland) with the support of a grant from the Polish Ministry of Science and Higher Education.

The authors are grateful to the staff of the Kalyazin radio telescope (Special Design Bureau of the Moscow Power Engineering Institute, Moscow, Russia) for the high quality of the observations.

We are grateful to A.V. Alakoz (ASC LPI) and O.S. Bayandina (JIVE) for helpful discussions and advice on the processing of the scientific data obtained in the RadioAstron project.

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  1. Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Moscow, Russia

    M. A. Shchurov, I. E. Val’tts & N. N. Shakhvorostova

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  1. M. A. Shchurov
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Shchurov, M.A., Val’tts, I.E. & Shakhvorostova, N.N. Structure of the H2O Maser in NGC 2071 IRS 1 from Observations on the Ground-Space Radio Interferometer RadioAstron. Astron. Rep. 65, 552–568 (2021). https://doi.org/10.1134/S1063772921070052

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