Stacking of DESI quasar spectra reveals strong, localized Hα emission aligned with radio jet axes around radio galaxies, indicating anisotropic jet-CGM interaction.
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Hybrid hydro/direct N-body simulations of dense high-redshift gas clouds form very massive stars via runaway collisions that collapse to IMBHs capable of growing from ~6700 to ~62000 solar masses in 100 Myr under optimistic assumptions.
Simulations of dwarf galaxies show V/σ rising with stellar mass, with HI gas and young stars more rotation-supported than old stars.
TNG50 shows galactic outflow mass loading is non-monotonic with stellar mass, rising rapidly above 10^10.5 Msun due to black hole feedback, and produces fast multi-phase outflows with emergent collimation.
Empirical halo-to-[O III] emitter modeling with realistic JWST survey mocks produces cross-correlations consistent with z~6 data within large scatter, but with a ~10 cMpc offset in the 1D peak.
Simulations demonstrate that high-specific-energy supernova outflows sustain hot CGM at virial temperature, raise t_cool/t_ff above 10, and transition dwarf galaxy feedback from ejective to preventive mode around 5 Gyr.
The paper identifies underproduction of oxygen in low-mass simulated dwarf galaxies as the likely cause of missing OVI in the CGM, based on comparisons across two simulation suites.
UV background suppresses NEI in galaxy haloes, restoring equilibrium shock thresholds and producing extended absorption columns for OVI, CIV, and HI beyond the virial radius.
Simulations constrain the mass scale for efficient ISM stripping of dwarf satellites to M_star ≲ 10^7 M_sun in MW-like halos, 0.5-1 dex below observed values, indicating additional quenching mechanisms are needed.
Shape-preserving LADE models with fixed local LF shape provide the statistically preferred description of UV QLF evolution to z~7.5 over flexible alternatives based on AIC/BIC.
Comparisons of three cosmological simulations show HI-rich failed halos occupy different mass regimes and predict that more can be discovered locally in HI-poor environments rather than at high redshift.
Simba simulations find that IGM gas fractions in cosmic web structures vary by only a few percent across feedback variants, while jet feedback noticeably enhances diffuse gas on the outskirts of filaments and knots.
The PINK updates enhance the CELEBI FRB pipeline with better astrometry, time-frequency gating, polarization calibration, DM optimization tools, and a software container for improved efficiency and localization of events like FRB 20251019A.