The Galactic Center (GC) is a key target for the radio component of Breakthrough Listen (BL) program. Offering the largest amount of stars in any given direction in the sky, the GC is widely cited as a location believed to harbour advanced civilizations, and it is also the most energetic region in the Milky Way. We aim to conduct BL-GC Survey with Parkes radio telescope for around 350 hours. We will cover the frequency range from 700 MHz to 4 GHz, utilizing the newly installed ultra-wideband receiver. Our team has already leveraged both standard and bespoke tools to construct a flexible software stack to search data for signals of interest. We will look for signals from extraterrestrial intelligence (ETI) by searching for both simple narrow-band signals and complex modulated signals. Along with that, as an ancillary science, we will also search for accelerated pulsars — likely orbiting a supermassive black hole at the centre of the Milky Way Galaxy. Data products produced during this program will also be publically available to engage larger pulsar community

The Galactic Center (GC) is a key target for the radio component of Breakthrough Listen (BL) program. Offering the largest amount of stars in any given direction in the sky, the GC is widely cited as a location believed to harbour advanced civilizations, and it is also the most energetic region in the Milky Way. We aim to conduct BL-GC Survey with Parkes radio telescope for around 350 hours. We will cover the frequency range from 700 MHz to 4 GHz, utilizing the newly installed ultra-wideband receiver. Our team has already leveraged both standard and bespoke tools to construct a flexible software stack to search data for signals of interest. We will look for signals from extraterrestrial intelligence (ETI) by searching for both simple narrow-band signals and complex modulated signals. Along with that, as an ancillary science, we will also search for accelerated pulsars — likely orbiting a supermassive black hole at the centre of the Milky Way Galaxy. Data products produced during this program will also be publically available to engage larger pulsar community

We request 8 GHz LBA observations of a nearby radio galaxy hosted by an active and likely unstable lenticular galaxy that may have underwent a minor merger in the past. Based on sub-arcsec resolution VLA observations, we propose to investigate the central 2 kpc region of the galaxy where we detected multi-component radio emission reminiscent of a relativistic jet but severely misaligned with the older large scale radio morphology (~80 deg reorientation). With this proposal we intend to verify if the detected central multi-component radio emission is indeed a relativistic jet as opposed to emission from star formation (or star bursts). This is a detection experiment and a pilot study. If the observations confirm that the radio emission is associated with a freshly launched realigned relativistic jet, a multi-epoch monitoring program will be designed and proposed in future semesters to characterise the emission and establish phenomenon at play causing the realignment.

Blazars are radio-loud active galactic nuclei whose jets point very close to the line of sight. High-resolution VLBI observations can provide the ultimate evidence for the blazar nature of a source, by revealing the compact, bright, high brightness temperature core with flat radio spectrum. Zywucka et al. (2018) selected the blazar candidates from the Magellanic Quasar Survey. The selection method based mainly on the optical variability and the radio-loudness of the sources. Using the infrared color-color selection for blazars derived from the data of the WISE satellite by Massaro et al. (2012) we found that 10 of the 27 WISE-detected sources are outside of the blazar gamma-ray strip. We propose to observe 7 sources from these list and additional 7 sources as a control sample which fall within the blazar strip. We want to compare the mas-scale properties of the two samples to asses whether (i) additional criteria is needed select blazar sources (ii) and if yes the WISE color-color criteria is able to improve the selection method. Optical emission and variability is thought to be dominated by the beamed jet in blazars while in non-beamed (and not radio-loud) sources it originates in the accretion disks thus governed by accretion processes. Therefore, if the physical mechanism causing the optical variability is intended to be studies the nature of the variable source is important to be ascertained.

The GMRT observations of the 2 sq. deg. COSMOS field were conducted using 30 antennas, their longest baseline being 25 km. The channel width of observations was 125 kHz, with a total bandwidth of 32 MHz.

Recent broad-band 34- and 44-GHz radio continuum observations of the Galactic center have revealed 41 massive stars identified with near-IR (NIR) counterparts, as well as 44 proplyd candidates within 30 arcseconds of Sgr A*. Radio observations obtained in 2011 and 2014 have been used to derive proper motions of eight young stars near Sgr A*. The accuracy of proper motion estimates based on NIR observations by Lu et al. (2009, ApJ, 690, 1463) and Paumard et al. (2006, ApJ, 643, 1011) have been investigated by using their proper motions to predict the 2014 epoch positions of NIR stars and comparing the predicted positions with those of radio counterparts in the 2014 radio observations. Predicted positions from Lu et al. show an rms scatter of 6 milliarcseconds (mas) relative to the radio positions, while those from Paumard et al. show rms residuals of 20 mas. In the reference paper, the authors also determine the mass-loss rates of 11 radio stars, finding rates that are on average ~2 times smaller than those determined from model atmosphere calculations and NIR data. Clumpiness of ionized winds would reduce the mass loss rate of WR and O stars by additional factors of 3 and 10, respectively. One important implication of this is a reduction in the expected mass accretion rate onto Sgr A* from stellar winds by nearly an order of magnitude to a value of a few x 10^-7 solar masses per year. The authors carried out A-array observations of the Galactic center region (VLA program 14A-232) in the Ka (9 mm, 34.5 GHz) band on 2014 March 9 in which they detected 318 compact radio sources within 30" of Sgr A*. The authors searched for NIR counterparts to these compact radio sources using high-angular resolution AOs-assisted imaging observations acquired with the VLT/NACO. A K_s-band (central wavelength 2.18 micron) image was obtained in a rectangular dither pattern on 2012 September 12. L'-band (3.8 micron) observations were obtained during various observing runs between 2012 June and September. The authors found that 45 of the compact radio sources had stellar counterparts in the K_s and L' bands. This table contains the details of the 318 compact radio sources detected at 34.5 GHz and their NIR counterparts. This table was created by the HEASARC in November 2016 based on CDS table J/ApJ/809/10, file table6.dat. This is a service provided by NASA HEASARC .