On the ages of bright galaxies ∼500\sim 500 Myr after the Big Bang: insights into star formation activity at z≳15z \gtrsim 15 with JWST

With JWST, new opportunities to study the formation and evolution of galaxies in the early Universe are now emerging. Spitzer constraints on rest-optical properties of $z \gtrsim 7$ galaxies demonstrated the power of using stellar masses and star formation histories (SFHs) of galaxies to indirectly infer the star formation history of the Universe. However, only the brightest individual objects at $z \gtrsim 8$ could be detected with Spitzer, making it difficult to robustly constrain past activity at $z \gtrsim 10$. Here, we leverage the greatly improved rest-optical sensitivity of JWST at $z \gtrsim 8$ to constrain the ages and SFHs of eleven UV-bright ($M_\text{UV} \lesssim -19.5$) galaxies selected to lie at $z \sim 8.5 - 11$, then investigate implications for star formation activity at $z \gtrsim 15$. We infer the properties of individual objects in our sample with two spectral energy distribution modelling codes, then infer a distribution of ages for bright $z \sim 8.5 - 11$ galaxies. We find a median age of $\sim 30$ Myr, younger than that inferred at $z \sim 7$ with a similar analysis, which is consistent with an evolution towards larger specific star formation rates at early times. The age distribution suggests that only $\sim 9$ percent of bright $z \sim 8.5 - 11$ galaxies would be similarly luminous at $z \gtrsim 15$, implying that the number density of bright galaxies declines by approximately an order of magnitude between $z \sim 8.5 - 11$ and $z \sim 15$. This evolution is challenging to reconcile with some early JWST results suggesting that the abundance of bright galaxies does not significantly decrease towards very early times, but we suggest this tension may be eased if young stellar populations form on top of older stellar components, or if bright galaxies at $z \sim 15$ are observed during a burst of star formation.Comment: 13 pages, 9 figure

Searching for Extremely Blue UV Continuum Slopes at z=7−11z=7-11 in JWST/NIRCam Imaging: Implications for Stellar Metallicity and Ionizing Photon Escape in Early Galaxies

The ultraviolet (UV) continuum slope ($\beta$ where f$_\lambda\propto \lambda^\beta$) of galaxies is sensitive to a variety of properties, from the metallicity and age of the stellar population to the attenuation from dust through the galaxy. Considerable attention has focused on identifying reionization-era galaxies with very blue UV slopes ($\beta<-3$). Not only do such systems provide a signpost of low metallicity stars, but they also identify galaxies that likely have ionizing photons leaking from their HII regions as such blue UV slopes can only be seen if the reddening effect of nebular continuum has been diminished. In this paper we present a search for reionization-era galaxies with very blue UV colors in recent JWST/NIRCam imaging of the EGS field. We characterize UV slopes for a large sample of $z\simeq 7-11$ galaxies, finding a median value of $\beta =-2.1$. Three of the lower luminosity (M$_{\rm{UV}}\simeq -19.5$) and lower stellar mass (5-6$\times10^7$M$_\odot$) systems exhibit both extremely blue UV slopes ($\beta=-3.1$ to $-3.2$) and rest-optical photometry indicating weak nebular line emission. Each system is very compact (r$_e<$260 pc) with very high star formation rate surface densities. We model the SEDs with a suite of BEAGLE models with varying levels of ionizing photon escape. The SEDs cannot be reproduced with our fiducial (f$_{\rm{esc,HII}}$=0) or alpha enhanced (Z$_*<Z_{\rm{ISM}}$) models. The combined blue UV slopes and weak nebular emission are best-fit by models with significant ionizing photon escape from HII regions (f$_{\rm{esc,HII}}$=0.6-0.8) and extremely low metallicity massive stars (Z$_*$=0.01-0.06 Z$_\odot$). The discovery of these galaxies highlights the potential for JWST to identify large numbers of candidate Lyman Continuum leaking galaxies in the reionization era and suggests low metallicity stellar populations may be veryComment: 11 pages, 8 figures, 2 tables; Submitted to Ap

A JWST/NIRCam Study of Key Contributors to Reionization: The Star-forming and Ionizing Properties of UV-faint z∼7−8z\sim7-8 Galaxies

Spitzer/IRAC imaging has revealed that the brightest $z\sim7-8$ galaxies often exhibit young ages and strong nebular line emission, hinting at high ionizing efficiency among early galaxies. However, IRAC's limited sensitivity has long hindered efforts to study the fainter, more numerous population often thought largely responsible for reionization. Here we use CEERS JWST/NIRCam data to characterize 116 UV-faint (median M$_{UV}=-19.5$) $z\sim6.5-8$ galaxies. The SEDs are typically dominated by young ($\sim$10-50 Myr), low-mass ($M_\ast\sim10^8\ M_\odot$) stellar populations, and we find no need for extremely high stellar masses ($\sim10^{11} M_\odot$). Considering previous studies of UV-bright (M$_{UV}\sim-22$) $z\sim7-8$ galaxies, we find evidence for a strong (5-10$\times$) increase in specific star formation rate toward lower luminosities (median sSFR=103 Gyr$^{-1}$ in CEERS). The larger sSFRs imply a more dominant contribution from OB stars in the relatively numerous UV-faint population, perhaps suggesting that these galaxies are very efficient ionizing agents (median $\xi_{ion}=10^{25.7}$ erg$^{-1}$ Hz). In spite of their much larger sSFRs, we find no significant increase in [OIII]$+$H$\beta$ EWs towards fainter M$_{UV}$ (median $\approx$780 $\mathring{A}$). If confirmed, this may indicate that a substantial fraction of our CEERS galaxies possess extremely low metallicities ($\lesssim$3% $Z_\odot$) where [OIII] emission is suppressed. Alternatively, high ionizing photon escape fractions or bursty star formation histories can also weaken the nebular lines in a subset of our CEERS galaxies. While the majority of our objects are very blue (median $\beta=-2.0$), we identify a significant tail of very dusty galaxies ($\beta\sim-1$) at $\approx$0.5$L_{UV}^\ast$ which may contribute significantly to the $z\sim7-8$ star formation rate density.Comment: Accepted in MNRAS. Updated to use the most recent NIRCam zeropoints. There are no significant changes to the conclusions relative to v

Gene Selection for Multiclass Prediction by Weighted Fisher Criterion

Gene expression profiling has been widely used to study molecular signatures of many diseases and to develop molecular diagnostics for disease prediction. Gene selection, as an important step for improved diagnostics, screens tens of thousands of genes and identifies a small subset that discriminates between disease types. A two-step gene selection method is proposed to identify informative gene subsets for accurate classification of multiclass phenotypes. In the first step, individually discriminatory genes (IDGs) are identified by using one-dimensional weighted Fisher criterion (wFC). In the second step, jointly discriminatory genes (JDGs) are selected by sequential search methods, based on their joint class separability measured by multidimensional weighted Fisher criterion (wFC). The performance of the selected gene subsets for multiclass prediction is evaluated by artificial neural networks (ANNs) and/or support vector machines (SVMs). By applying the proposed IDG/JDG approach to two microarray studies, that is, small round blue cell tumors (SRBCTs) and muscular dystrophies (MDs), we successfully identified a much smaller yet efficient set of JDGs for diagnosing SRBCTs and MDs with high prediction accuracies (96.9% for SRBCTs and 92.3% for MDs, resp.). These experimental results demonstrated that the two-step gene selection method is able to identify a subset of highly discriminative genes for improved multiclass prediction

Impact of alirocumab/evolocumab on lipoprotein (a) concentrations in patients with familial hypercholesterolaemia: a systematic review and meta-analysis of randomized controlled trials

Introduction: Familial hypercholesterolaemia (FH) is a common hereditary genetic disorder, characterized by elevated circulating low-density lipoprotein cholesterol (LDL-C) and lipoprotein (a) [Lp(a)] concentrations, leading to atherosclerotic cardiovascular disease (ASCVD). Two types of proprotein convertase subtilisin/kexin type 9 (PCSK9) inhibitors — alirocumab and evolocumab — are efficient drugs in the treatment of FH, which can effectively reduce Lp(a) levels. Material and methods: Embase, MEDLINE, and PubMed up to November 2022 were searched for randomized clinical trials (RCTs) evaluating the effect of alirocumab/evolocumab and placebo treatment on plasma Lp(a) levels in FH. Statistics were analysed by Review Manager (RevMan 5.3) and Stata 15.1. Results: Eleven RCTs involved a total of 2408 participants. Alirocumab/evolocumab showed a significant efficacy in reducing Lp(a) [weighted mean difference (WMD): –20.10%, 95% confidence interval (CI): –25.59% to –14.61%] compared with placebo. In the drug type subgroup analyses, although the efficacy of evolocumab was slightly low (WMD: –19.98%, 95% CI: –25.23% to –14.73%), there was no difference with alirocumab (WMD: –20.54%, 95% CI: –30.07% to –11.02%). In the treatment duration subgroup analyses, the efficacy of the 12-week duration group (WMD: –17.61%, 95% CI: –23.84% to –11.38%) was lower than in the group of ≥ 24 weeks’ duration (WMD: –22.81%, 95% CI: –31.56% to –14.07%). In the participants’ characteristics subgroup analyses, the results showed that no differential effect of alirocumab/evolocumab therapy on plasma Lp(a) concentrations was observed (heterozygous FH [HeFH] WMD: –20.07%, 95% CI: –26.07% to –14.08%; homozygous FH [HoFH] WMD: –20.04%, 95% CI: –36.31% to –3.77%). Evaluation of all-cause adverse events (AEs) between alirocumab/evolocumab groups and placebo groups [relative risk (RR): 1.05, 95% CI: 0.98–1.12] implied no obvious difference between the 2 groups. Conclusions: Anti-PCSK9 drugs (alirocumab and evolocumab) may be effective as therapy for reducing serum Lp(a) levels in FH, and no differences were observed in treatment durations, participant characteristics, and other aspects of the 2 types of PCSk9 inhibitors. However, further experimental studies and RCTs are warranted to clarify the mechanism of PSCK9 inhibitors to lowering Lp(a) concentrations in FH

Metal-Enriched Neutral Gas Reservoir around a Strongly-lensed, Low-mass Galaxy at z=4z=4 Identified by JWST/NIRISS and VLT/MUSE

Direct observations of low-mass, low-metallicity galaxies at $z\gtrsim4$ provide an indispensable opportunity for detailed inspection of the ionization radiation, gas flow, and metal enrichment in sources similar to those that reionized the Universe. Combining the James Webb Space Telescope (JWST), VLT/MUSE, and ALMA, we present detailed observations of a strongly lensed, low-mass ($\approx 10^{7.6}$ ${\rm M}_\odot$) galaxy at $z=3.98$ (also see Vanzella et al. 2022). We identify strong narrow nebular emission, including CIV $\lambda\lambda1548,1550$, HeII $\lambda1640$, OIII] $\lambda\lambda1661,1666$, [NeIII] $\lambda3868$, [OII] $\lambda3727$, and Balmer series of Hydrogen from this galaxy, indicating a metal-poor HII region ($\lesssim 0.12\ {\rm Z}_\odot$) powered by massive stars. Further, we detect a metal-enriched damped Ly$\alpha$ system (DLA) associated with the galaxy with the HI column density of $N_{\rm{HI}}\approx 10^{21.8}$ cm$^{-2}$. The metallicity of the associated DLA may reach the super solar metallicity (${\gtrsim Z}_\odot$). Moreover, thanks to JWST and gravitational lensing, we present the resolved UV slope ($\beta$) map at the spatial resolution of $\approx 100$ pc at $z=4$, with steep UV slopes reaching $\beta \approx -2.5$ around three star-forming clumps. Combining with low-redshift analogs, our observations suggest that low-mass, low-metallicity galaxies, which dominate reionization, could be surrounded by a high covering fraction of the metal-enriched, neutral-gaseous clouds. This implies that the metal enrichment of low-mass galaxies is highly efficient, and further support that in low-mass galaxies, only a small fraction of ionizing radiation can escape through the interstellar or circumgalactic channels with low column-density neutral gas.Comment: 4 pages, 1 table; submitted to the ApJL; welcome comment