A5052038103- Astrophysics and Cosmic Phenomena
- Gamma-ray bursts and supernovae
- Dark Matter and Cosmic Phenomena
- Neutrino Physics Research
- Astrophysical Phenomena and Observations
- Astronomy and Astrophysical Research
- Particle Detector Development and Performance
- Radio Astronomy Observations and Technology
- Computational Physics and Python Applications
- Particle physics theoretical and experimental studies
- Pulsars and Gravitational Waves Research
- Solar and Space Plasma Dynamics
- Galaxies: Formation, Evolution, Phenomena
University of Tübingen
2023-2024
Durham University
2023
University of Turku
2023
Niels Brock
2023
University of Copenhagen
2023
Main Astronomical Observatory
2023
Taras Shevchenko National University of Kyiv
2023
National Academy of Sciences of Ukraine
2023
Georgia Institute of Technology
2023
AGH University of Krakow
2023
The eROSITA telescope array aboard the Spektrum Roentgen Gamma (SRG) satellite began surveying sky in December 2019, with aim of producing all-sky X-ray source lists and maps an unprecedented depth. Here we present catalogues both point-like extended sources using data acquired first six months survey operations (eRASS1; completed June 2020) over half whose proprietary rights lie German Consortium. We describe observation process, analysis pipelines, characteristics sources. With nearly 930...
A thorough inspection of known Galactic Supernova Remnants (SNRs) along the plane with SRG/eROSITA yielded detection X-ray counterpart SNR G279.0+01.1. The is located just 1.5 deg above plane. Its emission emerges as an incomplete, partial shell $\sim$3 angular extension. It strongly correlated to fragmented shell-type morphology its radio continuum emission. spatial seems be linked presence dust clouds in surroundings. majority soft (exhibiting strong O, Ne and Mg lines), occurs a narrow...
The Simeis~147 nebula (S147), particularly well known for a spectacular net of ${\rm H}_\alpha$-emitting filaments, is often considered one the largest and oldest supernova remnants in Milky Way. Here, companion paper, we present studies X-ray emission from S147 using data SRG/eROSITA All-Sky Survey observations. In this argue that many inferred properties emitting gas are broadly consistent with scenario explosion low-density cavity, e.g. wind-blown-bubble. This assumes $\sim 20\,{\rm...
Simeis 147 (S147, G180.0-01.7, ``Spaghetti nebula'') is a supernova remnant (SNR) extensively studied across the entire electromagnetic spectrum, from radio to GeV $\gamma$-rays, except in X-rays. In this study, we report first detection of significant X-ray emission SNR. Here, and companion paper, present studies S147 nebula using data extended ROentgen Survey Imaging Telescope Array (eROSITA) onboard Russian-German Spektrum Roentgen Gamma (SRG). The object located at Galactic anti-center,...
Simeis 147 (S147, G180.0-01.7, ``Spaghetti nebula'') is a supernova remnant (SNR) extensively studied across the entire electromagnetic spectrum, from radio to giga-electronvolt gamma -rays, except in X-rays. Here, we report first detection of significant X-ray emission SNR using data extended ROentgen Survey Imaging Telescope Array (eROSITA) onboard Russian-German Spektrum Roentgen Gamma (SRG). The object located at Galactic anticenter, and its $3 size classifies it among largest SNRs ever...
The Simeis 147 nebula (S147) is particularly well known for a spectacular net of H α -emitting filaments. It often considered one the largest and oldest (∼10 5 yr) cataloged supernova remnants in Milky Way, although kinematics pulsar PSR J0538+2817 suggests that this remnant might be factor three younger. former case companion paper, while here we pursue latter. Both studies are based on data SRG/eROSITA All-Sky Survey observations. Here, confront inferred properties X-ray emitting gas with...
A thorough inspection of known Galactic supernova remnants (SNRs) along the plane with SRG/eROSITA yielded detection X-ray counterpart SNR G279.0+01.1. The is located just 1.5° above plane. Its emission emerges as an incomplete, partial shell ~3° angular extension. It strongly correlated to fragmented shell-type morphology its radio continuum emission. spatial seems be linked presence dust clouds in surroundings. majority soft (exhibiting strong O, Ne, and Mg lines), it occurs a narrow range...
Supernova remnant (SNR) detection along the Galactic plane poses a number of challenges. A diffuse X-ray emission component emanating from unidentified sources on further complicates such in X-rays. Due to presence dense dust clouds plane, photons are also subject high absorption. Similarly, signals cause γ -ray contamination signal individual objects. The SNR G309.8+00.0 lies exactly with its center coinciding galactic latitude (b) = 0°. In this paper we report first X-rays and rays, using...
Supernova remnant (SNR) detection along the Galactic plane poses a number of challenges. The SNR G309.8+00.0 lies exactly on plane, with its center coinciding galactic latitude (b)=0 deg. In this paper we report first in X-rays and $\gamma$ rays, using stacked data from four consecutive extended ROentgen Survey Imaging Telescope Array (eROSITA) -- board Russian-German Spektrum Roentgen Gamma (SRG) all-sky surveys (eRASS:4) $\sim15.5$ yr Pass 8 recorded Fermi-LAT, respectively. appears to...
Abstract M31 and M33 are the closest spiral galaxies largest members (together with Milky Way) of Local group, which makes them interesting targets for indirect dark matter searches. In this paper we present studies expected sensitivity Cherenkov Telescope Array (CTA) to an annihilation signal from weakly interacting massive particles M33. We show that a 100 h long observation campaign will allow CTA probe cross-sections up 〈 συ 〉 ≈ 5·10 -25 cm 3 s -1 τ + - channel (for M31, at DM mass 0.3...
M31 and M33 are the closest spiral galaxies largest members (together with Milky Way) of Local group, which makes them interesting targets for indirect dark matter searches. In this paper, we present studies expected sensitivity Cherenkov Telescope Array (CTA) to an annihilation signal from weakly interacting massive particles M33. We show that a 100 h long observation campaign will allow CTA probe cross-sections up $\langle\sigma\upsilon\rangle\approx 5\cdot10^{-25}$ cm$^{3}$s$^{-1}$...