We used the ultra-deep GLIMPSE JWST/NIRCam survey to constrain the faint end of the [O III]+H beta luminosity function (LF) down to 10(39)erg s(-1) at z similar to 7 - 9 behind the lensed Hubble Frontier Field galaxy cluster Abell S1063. We applied a spectral energy distribution fitting on a Lyman-break galaxy selected sample of 164 lensed galaxies and measured their combined H beta+[O III]lambda lambda 4960, 5008 flux to build the emission line LF. We found a [O III]+H beta LF with a faint-end slope (alpha = -1.78(-0.06)(+0.06) for z = 7 - 8 and alpha = -1.55(-0.11)(+0.11) for z = 8 - 9), which is flatter than the UV LF at similar redshifts (alpha <= -2) and suggests a lower number density of weak [O III]+H beta emitting galaxies at fixed M-UV. We analysed several possible explanations: (i) a decrease in the [O III]+H beta-to-UV ratio due to bursty star formation histories (SFHs), (ii) the effect of metallicity on the [O III]-to-H beta ratio, or (iii) signs of a faint-end turnover in the UV LF. Under the assumption of an evolving [O III]-to-H beta ratio, we separated the contribution of [O III]lambda 5008 and H beta and obtained a flatter [O III]lambda 5008 LF (alpha = -1.66(-0.05)(+0.05) for z = 7 - 8 and alpha = -1.45(-0.10)(+0.09) for z = 8 - 9) but steeper H beta LF (alpha=-1.95-0.08+0.08 for z = 7 - 8 and alpha = -1.68(-0.14)(+0.13) for z = 8 - 9). The combination of a decreasing metallicity and bursty SFH can reconcile the observed differences between the UV and [O III]+H beta LF. By converting this LF into the ionising photon-production rate N-ion, we show that galaxies with L-H alpha >= 10(39) erg s(-1), that is, with a star formation rate (SFR) (H alpha) >= 5 & times; 10(-3) M-circle dot yr(-1)) cause 31%-90% and 46%-156% of the ionising photon budget (at 7 < z < 8 and 8 < z < 9), when we assume a constant escape fraction of Lyman-continuum photon (f(esc) = 0.14). The shape of the LF further shows the negligible contribution of faint galaxies to the N-ion. Additionally, we derived the cosmic star formation rate density (SFRD), finding results consistent with previous estimates. However, the sensitivity of GLIMPSE to lower SFRs reinforces the conclusion that very faint galaxies contribute very little to N-ion and the SFRD. Our results suggests that GLIMPSE has detected the bulk of the total [O III]+H beta emission from star-forming galaxies, and that galaxies below our detection limits are likely minor contributors to cosmic re-ionisation.
Two marine sediment cores (MDBT 557 and MDBT 561) from the southern Brazilian shelf were analyzed to reconstruct Holocene variations in terrigenous organic matter (OM) input, vegetation dynamics, and the climatic-oceanographic processes influencing sediment deposition. Using sedimentological, molecular and isotopic proxies we identified site-specific differences in OM delivery but coherent long-term regional trends. During the early Holocene, both records indicate low terrigenous input, reflecting a weakened South American Monsoon System (SAMS) over the La Plata River (LPR) basin and reduced continental runoff, which, despite lower relative sea level (RSL), likely limited effective sediment export from the LPR and smaller coastal watersheds. Molecular proxies show that vegetation in southeastern South America was dominated by C4-rich grasslands, with minimal forest contribution, consistent with drier regional conditions. In the middle Holocene, weakened monsoon precipitation combined with a sustained RSL highstand restricted sediment dispersal across the shelf, maintaining low terrigenous OM input. Nonetheless, subtle lipid biomarker shifts suggest transitional vegetation states and gradual increases in humidity at the basin margins. A marked change occurs around 6,000 cal BP, when hydrodynamic reorganizations expanded the LPR plume over the shelf, altering the provenance of terrigenous OM. This shift marks the late-Holocene onset conditions, characterized by increased precipitation driven by strengthening summer insolation, intensification of the SAMS, and the establishment of a modern ENSO-like regime after similar to 4,000 cal BP. Consequently, terrigenous OM input and forest-derived signatures increased substantially, reflecting the expansion of Araucaria and Atlantic Forest taxa across southeastern South America.
The recent discovery of a large number of massive black holes within the first two billion years after the big bang, as well as their peculiar properties, have been largely unexpected based on the extrapolation of the properties of luminous quasars. These findings have prompted the development of several theoretical models for the early formation and growth of black holes, which are, however, difficult to differentiate. We report the metallicity measurement around a gravitationally lensed massive black hole at redshift 7.04 (classified as a Little Red Dot), hosted in a galaxy with very low dynamical mass. The weakness of the [O III]5007 emission line relative to the narrow H beta emission indicates extremely low metallicity, about 4 & times;10(-3) solar, and even more metal poor in the surrounding few 100 pc. We argue that such properties cannot be uncommon among accreting black holes around this early cosmic epoch. Explaining such a low chemical enrichment in a system that has developed a massive black hole is challenging for most theories. Models assuming heavy black hole seeds (such as Direct Collapse Black Holes) or super-Eddington accretion scenarios struggle to explain the observations, although they can potentially reproduce the observed properties in some cases. Models invoking 'primordial black holes' (i.e. putative black holes formed shortly after the big bang) may potentially explain the low chemical enrichment associated with this black hole, although this class of models also requires further developments for proper testing.
James Webb Space Telescope (JWST) has revealed a population of 'Little Red Dots' (LRDs): compact, red objects at redshifts z = 2-9 with 'v'-shaped spectral energy distributions, broad permitted lines, and, often, hydrogen Balmer absorption. We use NIRSpec/IFS data from the BlackTHUNDER survey to study the H alpha line in the LRD Abell2744-QSO1 at z = 7 . 04 , which is a confirmed active galactic nucleus (AGN) due to time-variable equivalent width (EW) in its broad emission lines. The H alpha spectral profile is non-Gaussian, requiring at least two Gaussian components. We also detect a narrow-line Gaussian component, and strong H alpha absorption (EW relative to the continuum similar to 22(+12)(-7) & Aring;), confirming a connection between the strong Balmer break and line absorption. The absorber is at rest with respect to broad H alpha , suggesting that the gas cannot be interpreted as an inflow or outflow, forming instead a long-lived structure. Its velocity dispersion is Q(abs) = 110(-10)(+20) km s(-1), consistent with the value inferred from the analysis of the Balmer break. Based on H alpha , we infer a black hole mass of log(M-center dot/M-circle dot) = 7 . 2 , smaller but close to the previous estimates based on H . The Eddington ratio is 0.09. Combining the high signal-to-noise ratio of the narrow H alpha line with the spectral resolution R = 3 , 700 of the G395H grating, we infer a narrow-line intrinsic dispersion Q(n) = 22(-6)(+5) km s(-1) , which places a stringent constraint on the black hole-to-dynamical mass ratio of this system to be M-center dot/M-dyn= 0 . 15-1 . 2 , confirming the overmassive nature of the black hole and potentially leaving little room for a host galaxy.
High-risk neuroblastoma remains a challenging pediatric cancer, with survival rates lagging despite advances in multimodal therapy. This review aims to critically synthesize recent advances in GD2-directed chimeric antigen receptor (CAR) T cell therapy for neuroblastoma and to highlight its potential to improve long-term outcomes. In early-phase trials of GD2-directed CAR-T cell therapy for relapsed or refractory neuroblastoma, no dose-limiting toxicities were observed. Objective responses ranged from 6
