Observations of astronomical objects using radio (Irbene RT-32 telescope) and optical (Baldone Schmidt) methods

Abstract

Institute of Astronomy (University of Latvia) with Ventspils International Radio Astronomy Centre (Ventspils University of Applied Sciences) participation is implementing the scientific project "Complex investigations of the small bodies in the Solar system" which is related to the research of the small bodies in the Solar system (mainly focusing on asteroids and comets) using methods of radio and optical astronomy and signal processing.To detect the rotation period and other physical characteristics of NEO objects using optical methods, 566 positions and photo-metric observations of NEO objects 2006 VB14 = Y5705 = 345705 (hereafter 2006 VB14) and 1986 DA = 6178 (hereafter 1986 DA) were obtained with Baldone Schmidt telescope in 2018. A Fourier transform was applied to determine the rotation period for asteroid 1986 DA. Value 3.12 0.02 h was obtained. Observations confirm the previously obtained rotation period P = 3.25 h for 2006 VB14. To detect weak (~0.1 Jy) OH maser of astronomical objects using radio methods, a researcher group in VIRAC adapted Irbene RT-32 radio telescope working at 1665.402 and 1667.359 MHz frequencies. Novel data processing methods were used to acquire weak signals. Spectral analysis using Fourier transform and continuous wavelet transform were applied to radio astronomical data from multiple observations related to weak OH maser detection. Successful observations of multiple galactic masers were carried out in 2019 and adapted Irbene RT32 radio telescope is ready for the observations of comets in the near future.

Observations of Weak Galactic OH Masers in 1.6 GHz Frequency Band Using Irbene RT-32 Radio Telescope

“…The developed flux detection threshold estimation model, which is related to noise floor dS vs integration time, shows that the detection of the source with the flux density below 0.4 Jy is possible using radio telescope RT-32 complex if the spectral channel bandwidth is small and integration time is large [8]. Practically, existing RT-32 1.6 GHz receiver and data processing methods allow identifying the weak OH masers with emission being below 0.4 Jy.…”

“…Weakness of the radio signal of a comet OH maser is the main challenging factor. The calculated results of the noise floor dS vs. integration time showed that the detection of the source with the flux density below 0.4 Jy was possible by RT-32 antenna if integration time was larger than 8 hours and total power bandwidth (BW) -10 KHz [8].…”