Mingyu Li, Zheng Cai
We present the mass-metallicity relation (MZR) at $z=2-3$ in the stellar mass range of $M_\star\approx 10^{6.5}-10^{9.5}M_\odot$ using 55 dwarf galaxies in the Abell 2744 and SMACS J0723-3732 galaxy cluster fields. These dwarf galaxies are identified and confirmed by deep JWST/NIRISS imaging and slitless grism spectroscopic observations. Taking advantage of the gravitational lensing effect, we extend the previous MZR relation at $z=2-3$ to a much lower mass regime by more than 2.
First author: Tzu-Yin Hsu
Fast radio bursts (FRBs) are millisecond-duration transients with large dispersion measures. The origin of FRBs is still mysterious. One of the methods to comprehend FRB origin is to probe the physical environments of FRB host galaxies. Mapping molecular-gas kinematics in FRB host galaxies is critical because it results in star formation that is likely connected to the birth of FRB progenitors. However, most previous works of FRB host galaxies have focused on its stellar component.
First author: C. D. Leonard
The rapidly increasing statistical power of cosmological imaging surveys requires us to reassess the regime of validity for various approximations that accelerate the calculation of relevant theoretical predictions. In this paper, we present the results of the ‘N5K non-Limber integration challenge’, the goal of which was to quantify the performance of different approaches to calculating the angular power spectrum of galaxy number counts and cosmic shear data without invoking the so-called ‘Limber approximation’, in the context of the Rubin Observatory Legacy Survey of Space and Time (LSST).
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.
