Star Formation and Chemical Enrichment in Protoclusters

We examine star formation and chemical enrichment in protoclusters (PCs) using cosmological zoom-in hydrodynamic simulations. We find that the total star formation rate (SFR) in all PC ($>10^{14.4}\,h^{-1}$M$_\odot$) reaches $>10^4\,\mathrm{M}_\odot \mathrm{yr}^{-1}$ at $z=3$, equivalent to the observed PCs. The SFR in the Core region accounts for about $30\%$ of the total star formation in the PC at $z\gtrsim1$, suggesting the importance of the outer regions to reveal the evolution of galaxy clusters. We find that the total SFR of PC is dominated by galaxies with $10^{10}\,\le\,(\mathrm{M}_\star/M_\odot)\,\le\,10^{11}$, while more massive galaxies dominate the SFR in the Core. For the chemical abundance evolution, we find that the higher-density region has a higher metallicity and faster evolution. We show that the [O/Fe] vs. [Fe/H] relation turns down in the Core at $z=3.4$ due to the enrichment of Fe by Type Ia supernovae. We find no environmental effects for the mass--metallicity relations (MZR) or $\log$(N/O) vs. $12+\log$(O/H) for galaxies. We find that the chemical enrichment in galaxy clusters proceeds faster in the high redshift Universe ($z>1$). Our work will benefit future tomographic observations, particularly using PCs as unique probes of accelerated structure formation and evolution in high-density regions of the universe.Comment: 19 pages, 18 figures, 2 tables, 2 appendices, Accepted for publication in MNRA

Detection Prospects for Majorana Fermion WIMPless Dark Matter

We consider both velocity-dependent and velocity-independent contributions to spin-dependent (SD) and spin-independent (SI) nuclear scattering (including one-loop corrections) of WIMPless dark matter, in the case where the dark matter candidate is a Majorana fermion. We find that spin-independent scattering arises only from the mixing of exotic squarks, or from velocity-dependent terms. Nevertheless (and contrary to the case of MSSM neutralino WIMPs), we find a class of models which cannot be detected through SI scattering, but can be detected at IceCube/DeepCore through SD scattering. We study the detection prospects for both SI and SD detection strategies for a large range of Majorana fermion WIMPless model parameters.Comment: 14 pages, 3 figures. v2: updated to match published versio

Probing Chemical Enrichment in Extremely Metal-Poor Galaxies and First Galaxies

The chemical composition of galaxies offers vital insights into their formation and evolution. A key aspect of this study is the correlation between helium abundance (He/H) and metallicity, which is instrumental in estimating the primordial helium generated by Big Bang nucleosynthesis. We study the chemical enrichment history of low-metallicity galaxies, specifically focusing on extremely metal-poor galaxies (EMPGs) and the first galaxies, using the one-zone model and cosmological hydrodynamic simulations. Our one-zone model, using the Limongi & Chieffi (2018) yield, aligns well with observed high He/H ratios at low metallicities and reproduces Fe/O ratios akin to EMPGs. Conversely, the Nomoto et al. (2013) yield does not fully match the high Fe/O ratios seen in EMPGs. Our cosmological hydrodynamic simulations of the first galaxy successfully replicate the stellar mass and star formation rate of galaxies like GN-z11 but fail to produce metallicity and high He/H at low O/H. This is consistent with the results of the one-zone model, which shows that the slope of the He/H-O/H relation is moderate in young, actively star-forming galaxies, suggesting the importance of using galaxies with similar star formation histories for the fit. These results highlight the need for high-resolution simulations and expanded observational datasets to refine our understanding of early galactic chemical evolution.Comment: 14 pages, 7 figures, 1 table, submitted to Ap

Denoising using deep-learning-based reconstruction for whole-heart coronary MRA with sub-millimeter isotropic resolution at 3 T: a volunteer study

PURPOSEThe aim of this study was to assess the usefulness of denoising deep-learning-based reconstruction (dDLR) to improve image quality and vessel delineation in noncontrast 3-T wholeheart coronary magnetic resonance angiography (WHCMRA) with sub-millimeter isotropic resolution (Sub-mm) compared with a standard resolution without dDLR (Standard).METHODSFor 10 healthy volunteers, we acquired the WHCMRA with Sub-mm with and without dDLR and Standard to quantify signal- (SNR) and contrast-to-noise ratio (CNR) and vessel edge signal response (VESR) in all the 3 image types. Two independent readers subjectively graded vessel sharpness and signal homogeneity of 8 coronary segments in each patient. We used Kruskal– Wallis test with Bonferroni correction to compare SNR, CNR, VESR, and the subjective evaluation scores among the 3 image types and weighted kappa test to evaluate inter-reader agreement on the scores.RESULTSSNR was significantly higher with Sub-mm with dDLR (P .05); the subjective signal homogeneity was significantly improved from Sub-mm without dDLR to Standard to Sub-mm with dDLR (P < .001). The inter-reader agreement was excellent (kappa=0.84).CONCLUSIONApplication of dDLR is useful for improving image quality and vessel delineation in the WHCMRA with Sub-mm compared with Standard