Daniel Maschmann Emission lines with a double-peak (DP) shape, detected in the centre of <span class="search-hit mathjax">galaxies</span>, have been extensively used in the past to identify peculiar kinematics such as dual active galactic nuclei, outflows or <span class="search-hit mathjax">mergers</span>. From a large DP <span class="search-hit mathjax">galaxy</span> sample, a connection to minor <span class="search-hit mathjax">merger</span> <span class="search-hit mathjax">galaxies</span> with ongoing star formation was suggested. To gain a better understanding of different mechanisms creating a DP signature, we here explore synthetic SDSS spectroscopic observations computed from disc models and simulations.

First author: Daniel Maschmann Emission lines with a double-peak (DP) shape, detected in the centre of galaxies, have been extensively used in the past to identify peculiar kinematics such as dual active galactic nuclei, outflows or mergers. From a large DP galaxy sample, a connection to minor merger galaxies with ongoing star formation was suggested. To gain a better understanding of different mechanisms creating a DP signature, we here explore synthetic SDSS spectroscopic observations computed from disc models and simulations.

First author: Janice C. Lee The PHANGS collaboration has been building a reference dataset for the multi-scale, multi-phase study of star formation and the interstellar medium in nearby galaxies. With the successful launch and commissioning of JWST, we can now obtain high-resolution infrared imaging to probe the youngest stellar populations and dust emission on the scales of star clusters and molecular clouds ($\sim$5-50 pc). In Cycle 1, PHANGS is conducting an 8-band imaging survey from 2-21$\mu$m of 19 nearby spiral galaxies.

Georg Herzog We examine the gas content of field dwarf galaxies in a high-resolution cosmological simulation. In agreement with previous work, we find that galaxies inhabiting dark matter haloes with mass below a critical value, $M_{200} \lesssim M_{\rm crit} \approx 5\times 10^{9} \ M_{\odot}$, are quiescent at the present day. The gas content of these galaxies is thus insensitive to feedback from evolving stars. Almost half of these quiescent systems today have gas masses much smaller than that expected for their mass.

First author: Rachel J. Bruch Spectroscopic detection of transient narrow emission lines (flash-ionisation features) traces the presence of circumstellar material (CSM) around massive stars exploding as core-collapse supernovae. Transient emission lines disappearing shortly after the SN explosion suggest that the spatial extent of this material is compact; hence implying that the progenitor star experienced episodes of enhanced mass loss shortly prior to explosion. The early light curves of Type II supernovae (SNe II) are assumed to be initially powered by shock-cooling emission.

First author: Ulrich P. Steinwandel We present the first results from a high resolution simulation with a focus on galactic wind driving for an isolated galaxy with a halo mass of $\sim 10^{11}$ M${\odot}$ (similar to the Large Magellanic Cloud) and a total gas mass of $\sim 6 \times 10^{8}$ M${\odot}$, resulting in $\sim 10^{8}$ gas cells at $\sim 4$ M${\odot}$ mass resolution. We adopt a resolved stellar feedback model with non-equilibrium cooling and heating, including photoelectric heating and photo-ionizing radiation, as well as supernovae (SNe), coupled to the second order meshless finite mass (MFM) method for hydrodynamics.

First author: Tom Ben-Ami Type Ibn supernovae (SNe) are a rare class of stellar explosions whose progenitor systems are not yet well determined. We present and analyze observations of the Type Ibn SN 2019kbj, and model its light curve in order to constrain its progenitor and explosion parameters. SN 2019kbj shows roughly constant temperature during the first month after peak, indicating a power source (likely CSM interaction) that keeps the continuum emission hot at ~15000K.

First author: Josh Borrow Early galaxies were the radiation source for reionization, with the photoheating feedback from the reionization process expected to reduce the efficiency of star formation in low mass haloes. Hence, to fully understand reionization and galaxy formation, we must study their impact on each other. The THESAN project has so far aimed to study the impact of galaxy formation physics on reionization, but here we present the new THESAN simulations with a factor 50 higher resolution ($m_{\rm b} \approx 10^4$~M$\odot$) that aim to self-consistently study the back-reaction of reionization on galaxies.

First author: Jade Powell We perform three-dimensional simulations of magnetorotational supernovae using a $39,M_{\odot}$ progenitor star with two different initial magnetic field strengths of $10^{10}$ G and $10^{12}$ G in the core. Both models rapidly undergo shock revival and their explosion energies asymptote within a few hundred milliseconds to values of $\gtrsim 2\times10^{51}$ erg after conservatively correcting for the binding energy of the envelope. Magnetically collimated, non-relativistic jets form in both models, though the jets are subject to non-axisymmetric instabilities.

First author: Gao Xuyang Double radio lobes are generally believed to be produced by active nuclei of elliptical galaxies. However, several double-lobed radio sources have been solidly found to be associated with spiral galaxies. By cross-matching $\sim9\times10^5$ spiral galaxies selected from the SDSS DR8 data with the full 1.4-GHz radio source catalogs of NVSS and FIRST, we identify three new spiral galaxies: J0326$-$0623, J1110+0321 and J1134+3046 that produce double radio lobes, in addition to five double-lobed spirals previously known.