An informal meeting of the radio groups at ASU and the Institute of Atmospheric Physics to discuss the use of radio observations in astronomy and space science, including solar radio research and Jovian science, the involvement in the international infrastructures LOFAR, ALMA, as well as local radio instrumentation in Ondřejov. The seminar will also explore the outreach potential of portable radio antennas, including an LWA antenna and a CubeSat cardboard Yagi antenna, and discuss possibilities for future collaboration.

Location: ASU Spořilov, 101

Deep imaging with the James Webb Space Telescope is revealing a growing number of faint and morphologically complex sources whose nature is not immediately clear. In this talk, we focus on a peculiar extended object identified in the field of WR-124, which at first glance exhibits an unusually elongated structure reminiscent of an accretion disk around a supermassive black hole. We analyze multi-wavelength imaging from the MIRI and NIRCam instruments and perform aperture photometry to estimate the source brightness and angular size (~1 × 1.5 arcsec). Using spectral energy distribution fitting, we constrain its physical properties and find a likely redshift of z ≈ 0.8. Based on the combined photometric and morphological analysis, we consider possible interpretations of the object, in particular a galaxy merger or a gravitational lensing configuration. We present the methodology used to derive these constraints and discuss the limitations of the current data in distinguishing between these scenarios.

Location: ASU Spořilov, 101

Magnetised bubbles pervade the interstellar medium across a vast range of scales, from individual supernova remnants (SNRs) to the superbubbles they collectively inflate. We present two complementary 3D magnetohydrodynamic studies tracing this hierarchy from its smallest building blocks to its most prominent local example. We simulate SNRs expanding into a non-homogeneous, magnetised two-phase medium, obtaining complex magnetic field configurations in their interiors. Strongly magnetised remnants develop magnetically confined hot cavities surrounded by a diffuse magnetised halo, and remain orders of magnitude more X-ray luminous than their weakly magnetised counterparts. We then extend our study to larger scales, simulating the Local Bubble: a superbubble encasing the Solar neighbourhood, whose expansion has been driven by numerous supernovae. We characterise its turbulent interior magnetic field and its amplification in the shell, while also modelling neighbouring superbubbles and SNRs within 1 kpc of the Sun. Together, these parsec- to kiloparsec-scale frameworks give us insights on the coupling between magnetic fields and stellar feedback, from individual remnants to the large-scale cavities structuring the local interstellar medium.

Location: Spořilov - Lecture Room 101