First author: Stephen M. Wilkins
JWST has now made it possible to probe the rest-frame optical line emission of high-redshift galaxies extending to z~9, and potentially beyond. To aid in the interpretation of these emerging constraints, in this work we explore predictions for $[OIII]$ emission in high-redshift galaxies using the First Light and Reionisation Epoch Simulations (FLARES). We produce predictions for the $[OIII]$ luminosity function, its correlation with the UV luminosity, and the distribution of equivalent widths (EWs).
First author: Jeremy S. Sanders
High-spectral resolution observations of clusters of galaxies are a powerful tool to understand the physical processes taking place in these massive objects. Their hot multi-million-degree X-ray emitting cluster atmospheres, containing most of the baryons in these systems, are enriched to around 1/3 of the solar metallicity. Therefore, cluster spectra host a variety of spectral lines, in particular, the Fe-L complex around 1 keV typically emitted from cooler systems and Fe-K at 6.
P. Zhang
We report our analysis results for the globular cluster (GC) NGC~6341 (M92), as a millisecond pulsar (MSP) J1717$+$4308A has recently been reported found in this GC. The data used are from the Large Area Telescope onboard the {\it Fermi Gamma-ray Space Telescope (Fermi)}. We detect $γ$-ray pulsations of the MSP at a $4.4σ$ confidence level (the corresponding weighted H-test value is $\sim$28.4). This MSP, the fourth $γ$-ray pulsar found in a GC, does not have significant off-pulse emission and has $γ$-ray luminosity and efficiency $1.
Hao He
We employ the Feedback In Realistic Environments (FIRE-2) physics model to study how the properties of giant molecular clouds (GMCs) evolve during galaxy mergers. We conduct a pixel-by-pixel analysis of molecular gas properties in both the simulated control galaxies and galaxy major mergers. The simulated GMC-pixels in the control galaxies follow a similar trend in a diagram of velocity dispersion ($σ_v$) versus gas surface density ($Σ_{\mathrm{mol}}$) to the one observed in local spiral galaxies in the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) survey.
First author: Hao He
We employ the Feedback In Realistic Environments (FIRE-2) physics model to study how the properties of giant molecular clouds (GMCs) evolve during galaxy mergers. We conduct a pixel-by-pixel analysis of molecular gas properties in both the simulated control galaxies and galaxy major mergers. The simulated GMC-pixels in the control galaxies follow a similar trend in a diagram of velocity dispersion ($\sigma_v$) versus gas surface density ($\Sigma_{\mathrm{mol}}$) to the one observed in local spiral galaxies in the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) survey.
First author: Mohammad Malekjani
Given a \textit{model building} assumption on the (effective) equation of state (EoS) of the Universe, the Hubble constant $H_0$ arises as an integration constant when one solves the Friedmann equations. Therefore, while $H_0$ is \textit{mathematically} a constant, it need not be a constant \textit{observationally}, unless the EoS or model accurately describes the Universe. Building on earlier results, we show that redshift evolution of flat $\Lambda$CDM cosmological parameters $(H_0, \Omega_{m})$ persists in the most up-to-date Pantheon+ sample.
First author: F. Stanley
We present the results of a survey of CO(1-0) emission in 14 infrared luminous dusty star forming galaxies (DSFGs) at 2 < z < 4 with the NSF’s Karl G. Jansky Very Large Array. All sources are detected in CO(1-0), with an ~1arcsec angular resolution. Seven sources show extended and complex structure. We measure CO luminosities of $({\mu})L’{CO(1-0)}=0.4-2.9x10^{11}$ K km s$^{-1}$ pc$^2$, and molecular gas masses of (${\mu}$)M${H2}$ = 1.
Federico Sestito
Five stars in the extreme outskirts (from $\sim5$ to $\sim12$ elliptical half-light radii, r$_h$) of the Ursa Minor (UMi) dwarf galaxy have been identified as potential new members using a Bayesian algorithm applied to \textit{Gaia} EDR3 data. These targets were observed with the GRACES spectrograph, resulting in precise radial velocities and metallicities that confirm their association with UMi. For the brightest and outermost star (Target~1, at $\sim12$ r$_h$), the chemical abundances of $α$- (Mg, Ca, Ti), odd-Z (Na, K, Sc), Fe-peak (Fe, Ni, Cr), and neutron-capture process (Ba) elements have also been determined.
First author: Federico Sestito
Five stars in the extreme outskirts (from $\sim5$ to $\sim12$ elliptical half-light radii, r$_h$) of the Ursa Minor (UMi) dwarf galaxy have been identified as potential new members using a Bayesian algorithm applied to \textit{Gaia} EDR3 data. These targets were observed with the GRACES spectrograph, resulting in precise radial velocities and metallicities that confirm their association with UMi. For the brightest and outermost star (Target~1, at $\sim12$ r$_h$), the chemical abundances of $\alpha$- (Mg, Ca, Ti), odd-Z (Na, K, Sc), Fe-peak (Fe, Ni, Cr), and neutron-capture process (Ba) elements have also been determined.
Joseph Whittingham
The role of magnetic fields in galaxy evolution is still an unsolved question in astrophysics. We have previously shown that magnetic fields play a crucial role in major mergers between disc galaxies; in hydrodynamic simulations of such mergers, the Auriga model produces compact remnants with a distinctive bar and ring morphology. In contrast, in magnetohydrodynamic (MHD) simulations, remnants form radially-extended discs with prominent spiral arm structure. In this paper, we analyse a series of cosmological "zoom-in" simulations of major mergers and identify exactly $\textit{how}$ magnetic fields are able to alter the outcome of the merger.
