Study of H2O and OH Masers in the Region Formation of a Young High Mass Stellar Object (S255 NIRS 3)

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The results of a study of a star formation region are presented. S255 IR, where a young high-mass star is forming (20M•). Observations in H2O were carried out on RT-22 in Pushchino, and in the OH lines at the Large Radio Telescope in Nance (France). Data observations in the H2O line at 1.35 cm were used for the period 2017–2023. Our observations in H2O showed the existence strong flares, especially in 2023. Drift was also observed emission by radial velocity for most spectral details and predominantly in the direction of decreasing radial velocity.

In OH lines 18 cm in 2008 no emission was detected. We observed OH emission in the main lines 1665 and 1667 MHz in 2015, 2023 and 2024. Structures of spectra, degrees of circular and linear polarizations varied greatly during these epoch. However, at the same time the longitudinal magnetic field vectors had predominantly two directions:  relative to the vertical, i. e. almost perpendicular to the jet or along it. Zeeman splitting was detected only in the 1667 MHz line for one pair of features: 2.26 and 2.37 km/s. The amount of splitting 0.11 km/s corresponds to a longitudinal magnetic field value of 0.31 mGs; the field is directed towards the observer.

It is assumed that the appearance of OH maser emission in 2015 associated with an accretion flares. Significant structure changes OH spectra, their degrees of polarization and very strong flares H2O maser in 2023 may be associated with a new possibility accretion flares in S255 IR.

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作者简介

N. Ashimbaeva

Lomonosov Moscow State University

Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow

E. Lekht

Lomonosov Moscow State University

编辑信件的主要联系方式.
Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow

V. Krasnov

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

Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow

V. Shutenkov

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

Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow

参考

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2. Fig. 1. H2O maser emission spectra of H2O in the S255 IR direction obtained in 2017. Observation epochs are indicated

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3. Fig. 2. Continuation. Same as Fig. 1 for 2018

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4. Fig. 3. Continuation. Same as Fig. 1 for 2019

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5. Fig. 4. Continuation. Same as in Fig. 1 for 2020

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6. Fig. 5. Continuation. Same as in Fig. 1 for 2021

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7. Fig. 6. Continuation. Same as in Fig. 1 for 2022

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8. Fig. 7. Conclusion. Same as Fig. 1 for 2023

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9. Fig. 8. Variability of the integral flux of H2O maser emission in the S255 IR direction. The radial velocities of the most intense parts are indicated for each maximum

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10. Fig. 9. Variability of the radial velocity of individual emission details in the H2O spectra. Large light circles mark the details at those epochs when their flux density exceeded 200 Jans. The velocity variations of the most intense details are approximated by straight line segments and these details are numbered from 1 to 12. On the left, asterisks show the positions of the H2O details for the epoch of 14 May 2017, taken from [14, Table 4]. The darkened asterisks show masers observed at 22 GHz, and the bright asterisks show masers observed at 321 GHz

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11. Fig. 10. Spectra of OH maser emission in the 1665 MHz main line towards S255 IR at the epoch of 22 November 2015. The top panel (a) shows the spectra in right (bold line) and left (thin line) circular polarisations. In panel (b), the Stokes parameter V is given. The remaining panels show the spectra in linear polarisation at antenna polarisation plane (PA) positions of 0°, 45°, 90° and 135°

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12. Fig. 11. Same as Fig. 10, but in the period of 18 October 2023

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13. Fig. 12. Same as Fig. 10, but in the period of 17 January 2024

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14. Fig. 13. Same as Fig. 10, but for the 1667 MHz line in the period of 20 November 2015

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15. Fig. 14. Same as in Fig. 10, but for the 1667 MHz line in the period of 18 October 2023

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16. Fig. 15. Same as Fig. 10, but for the 1667 MHz line in the period of 17 January 2024

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17. Fig. 16. Variability of flux density and radial velocity of the main H2O maser part

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18. Fig. 17. Plots of the degree of circular (a) and linear (b) polarisations, position angle (c) of linear polarisation of individual parts in the OH 1665 and 1667 MHz lines, as well as the direction of transverse magnetic field vectors for individual maser parts at different epochs of observations (d)

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19. Fig. 18. Dependence of the radial velocity of two patterns in the OH 1665 MHz line on the antenna position angle

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