The observations of star formation regions by RT-22 PRAO ASC LPI - water maser sources survey. Lekht E.E. (1), Samodurov V.A. (2), Tolmachev A.M. (2) (1) Sternberg Astron.Inst. of MSU(2) PRAO ASC LPI

The regular monitoring of approximately one hundred maser sources in the line of H2O with the wavelength of 1.35 cm are carried out on RT-22 PRAO ASC LPI radiotelescope in Pushchino within 30 years! ( since 1979/80 ).
Наблюдения мазеров в линии водяного пара (22 GHz) раз в 1-2 месяца
проводились на радиотелескопе РТ-22 в рамках многолетнего мониторинга (c 1979 г.) нескольких десятков мазерных источников коллективом сотрудников ПРАО ФИАН и ГАИШ МГУ.

РТ-22 ПРАО АКЦ ФИАН:

Линия излучения H2O

The accurate measurements of the line profiles

Radiometer:
Filterband spectrometer:
128 channels x 7.5 kHz (0.1 km/s)
Autocorrelator:
Passband = 12.5 MHz – 2048 ch., res. = 6.1 kHz

Источник α(1950) δ(1950) VLSR
W 3 (2) 2 21 53.3 61 52 20 –41.0
W 3 OH 2 23 18 61 38 58 –48.8
IRC+60154 5 15 5 63 12 54 50
WB 652 5 27 31 33 45 12 – 2.2
Ori A KL 5 32 47 – 5 24 20 9
OMC-2 5 33 0 – 5 11 30 9.03
M 24 5 33 51.3 - 6 23 59 7.4
HH 1 ……………………………………………….
……………………………………………………………………….
LkHa 234 21 41 59 65 52 48 1.9
HD 209458
S 140
WB 176
IRAS 22480+6002
IRAS 22506+5944
Cep A
S 152
NGC 7538 23 11 37 61 11 49 –50.73
NGC 7538 N
G111.26–0.77
Программа наблюдений в линии H2O λ=1.35 см

The long time monitoring

The variations of flux densities from right, central and left part of the spectrum.

Variability for some days.

Orion A (KL) spectra

Orion A (KL)
The intensity variations of spectral details.

NGC 7538

Young star Lkh 234 is in the centre of NGC 7129

For example our observations show the existence of triplet structures in the spectra of H2O line in some sources, and it suggests that H2O line radiation are formed in rotating discs with clots like protoplanets.

A doughnut like protoplanet disk.

Молодая протозвезда в ИК-лучах (в туманности Ориона)
Слева – снимок, справа – модель протозвезды – звезда,
вращающийся (иногда и расширяющийся) тор, биполярные истекающие струи

In some cases our observations reveal expanding gaseous clouds near young stars or protostars and on the contrary – clouds, which fall on protostar clumps.

The correlation of water vapour masers locations with the locations of other masers (OH, SiO, methanol…),
HII regions, dence molecular clouds and IR sources.

Late spectral types stars.
Masers flares are late relatively IR flares.

We intend to publish the spectra catalog of water masers to present all these features of them.