Search

Lyman-alpha (Ly α) emission from galaxies is currently our most promising probe for constraining when and how reionization began, and thus when the first galaxies formed. At z > 7, the majority of galaxies detected with Ly α are in candidate overdensities. Here, we quantify the probability of these galaxies residing in large ionized bubbles. We create (1.6 Gpc)3 intergalactic medium (IGM) simulations: sufficient volume to robustly measure bubble size distributions around UV-bright galaxies and rare overdensities. We find |${M_{\small UV}}\lesssim -16$| galaxies and overdensities are ≳10–1000 × more likely to trace ionized bubbles compared to randomly selected positions. The brightest galaxies and strongest overdensities have bubble size distributions with highest characteristic size and least scatter. We compare two models: gradual reionization driven by numerous UV-faint galaxies versus rapid reionization by rarer brighter galaxies, producing larger bubbles at fixed neutral fraction. We demonstrate that recently observed z ∼ 7 overdensities are highly likely to trace large ionized bubbles, corroborated by their high Ly α detection rates. However, Ly α detections at z ≈ 8.7 in EGS and z  = 10.6 in GN-z11 are unlikely to trace large bubbles in our fiducial model – 11 and 7 per cent probability of >1 proper Mpc bubbles, respectively. Ly α detections at such high redshifts could be explained by: a less neutral IGM than previously expected; larger ionized regions at fixed neutral fraction; or if intrinsic Ly α flux is unusually strong in these galaxies. We discuss how to test these scenarios with JWST and prospects for upcoming wide-area surveys to distinguish between reionization models. [ABSTRACT FROM AUTHOR]

Revealing the cosmic hydrogen reionization history is one of the main goals of the modern cosmology. z > 5 quasars (QSOs) have been used as back-lights to investigate the evolution of the intervening intergalactic medium (IGM) during the cosmic reionization since their first discovery. However, due to the small population of luminous QSOs (∼130 QSOs known to date), a tight constraint on the reionization history has not yet been placed. In this work, we aim to tighten the constraint using the 93 QSOs (5.5 < z < 7.1) recently discovered in the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQS) project. This is the largest QSO sample used to constrain the epoch of reionization. We measure the mean IGM Ly α transmission and the QSO near-zone size using the UV spectra of these QSOs. The mean IGM Ly α transmission rises above zero at z ≲ 6, indicating the end of the reionization. The near-zone sizes of the SHELLQs QSOs are consistent with sizes spanned by QSOs of lifetime t q ∼ 1–100 Myr in simulations. Due to the scatter created by the low signal-to-noise spectra and large Ly α redshift uncertainty, we cannot conclude whether the redshift evolution of the near-zone size is affected by the reionization effect. [ABSTRACT FROM AUTHOR]

This study investigated the role of the miR-871-5p/proliferator-activated receptor α (PGC1α) pathway in ameliorating hepatic steatosis. We examined miR-871-5p expression in liver tissues of aging mice and AML12 senescent cells co-induced by low serum and palmitic acid (PA). Bioinformatics and multiple experiments were employed to validate the expression level of the target gene PGC1α for miR-871-5p. In this study, we aimed to investigate the potential role of miR-871-5p in regulating hepatic lipid deposition associated with aging. To do so, we performed in vitro transfection of both miR-871-5p mimic and inhibitor into senescent hepatocytes. Our results showed that miR-871-5p could inhibit PGC1α expression and cause lipid deposition in the liver due to aging. miR-871-5p controls this process by regulating PGC1α/fatty acid β-oxidation. H&E staining displayed the appearance of fat vacuoles in the livers of aging mice, and fatty acid β-oxidation-related genes (acyl-coenzyme A oxidase 1 carnitine palmitoyl transferase 1α and peroxisome proliferator-activated receptor α) expression was significantly reduced. Lipogenic genes (sterol regulatory element binding protein 1C and fatty acid synthase) expression level was increased in the livers of aging mice. In AML12 cells co-induced by low serum and PA, miR-871-5p mimics decreased PGC1α expression and increased lipid droplet accumulation in senescent hepatocytes. Conversely, miR-871-5p inhibitor promoted PGC1α expression and reduced lipid deposition in senescent hepatocytes. Our findings suggest that inhibiting miR-871-5p could be crucial in ameliorating aging-associated hepatic steatosis. These findings offer valuable insights into the molecular mechanisms driving hepatic steatosis in aging. [ABSTRACT FROM AUTHOR]

ABSTRACT Using the optical data from the Wide component of the Canada-France-Hawaii Telescope (CFHT) Legacy Survey, and new ultraviolet (UV) data from GALEX, we study the colours and specific star formation rates (SSFRs) of ∼ 100 galaxy clusters at 0.16 < z < 0.36, over areas extending out to radii of r∼ 7 Mpc. We use a multicolour, statistical background subtraction method to study the galaxy population at this radius; thus our results pertain to those galaxies which constitute an excess over the average field density. We find that the average SSFR and its distribution of the star-forming galaxies (with at z∼ 0.2 and at z∼ 0.3) have no measurable dependence on the clustercentric radius and are consistent with the field values. However, the fraction of galaxies with SFR above these thresholds, and the fraction of optically blue galaxies, are lower for the overdense galaxy population in the cluster outskirts compared with the average field value, at all stellar masses and at all radii out to at least 7 Mpc. Most interestingly, the fraction of blue galaxies that are forming stars at a rate below our UV detection limit is much higher in all radial bins around our cluster sample compared with the general field value. This is most noticeable for massive galaxies ; while almost all blue field galaxies of this mass have detectable star formation, this is true for less than 20 per cent of the blue cluster galaxies, even at 7 Mpc from the cluster centre. Our results support a scenario where galaxies are pre-processed in locally overdense regions in a way that reduces their SFR below our UV detection limit, but not to zero. [ABSTRACT FROM AUTHOR]

The genome of Streptomyces coelicolor encodes hundreds of putative regulatory proteins, most of which are of unknown function, including SCO5351. In this study, we determined that deletion of sco5351 largely abrogates production of actinorhodin (ACT) and reduces production of the calcium-dependent antibiotic (CDA). Comprehensive transcriptional analyses indicated that transcription of genes of the ACT pathway, including the pathway-specific regulator actII-orf4 and those involved in the building of the chemical compound, was markedly lower in Δ sco5351 in the late growth phase. However, transcription of genes in the CDA cluster was notably reduced in Δ sco5351 only in the early growth phase, suggesting that SCO5351 has a regulatory role throughout growth. Similar to the observations with Δ sco5351, ACT production was blocked by mutagenesis of three conserved amino acids potentially involved in dimerization of SCO5351, indicating that protein dimerization is critical to the function of SCO5351. In addition, disruption of sco5351 delayed the formation of aerial mycelium and spores under the conditions tested and, consistent with this, transcription of developmental genes associated with spore formation was reduced in Δ sco5351, implying that SCO5351 is involved in developmental control. Our findings reveal SCO5351 as a pleiotropic regulator with roles in both secondary metabolism and morphological development in S. coelicolor. [ABSTRACT FROM AUTHOR]

We describe new JWST /NIRSpec observations of galaxies at z ≳ 7 taken from the CEERS survey. Previous observations of this area have revealed associations of Lyα emitters at redshifts (z = 7.5, 7.7, and 8.7) where the intergalactic medium (IGM) is thought to be mostly neutral, leading to suggestions that these systems are situated in large ionized bubbles. We identify 21 z ≳ 7 galaxies with robust redshifts in the CEERS data set, including 10 in the Lyα associations. Their spectra are indicative of very highly ionized and metal poor gas, with line ratios (O32 = 17.84 and Ne3O2 = 0.89, linear scale) and metallicity (⁠|$12+\log {(\rm {O/H})}=7.84$|⁠) that are rarely seen at lower redshifts. We find that the most extreme spectral properties are found in the six z ≳ 7 Lyα emitters in the sample. Each has a hard ionizing spectrum indicating that their visibility is likely enhanced by efficient ionizing photon production. Lyα velocity offsets are found to be very large (≳300 km s−1), likely also contributing to their detectability. We find that Lyα in z ≳ 7 galaxies is 6–12 × weaker than in lower redshift samples with matched rest-optical spectral properties. If the bubbles around the Lyα emitters are relatively small (≲0.5–1 pMpc), we may expect such significant attenuation of Lyα in these ionized regions. We discuss several other effects that may contribute to weaker Lyα emission at z ≳ 7. Deep spectroscopy of fainter galaxies in the vicinity of the Lyα emitters will better characterize the physical scale of the ionized bubbles in this field. [ABSTRACT FROM AUTHOR]

Revealing the cosmic reionization history is at the frontier of extragalactic astronomy. The power spectrum of the cosmic microwave background (CMB) polarization can be used to constrain the reionization history. Here, we propose a CMB-independent method using fast radio bursts (FRBs) to directly measure the ionization fraction of the intergalactic medium (IGM) as a function of redshift. FRBs are new astronomical transients with millisecond time-scales. Their dispersion measure (DMIGM) is an indicator of the amount of ionized material in the IGM. Since the differential of DMIGM against redshift is proportional to the ionization fraction, our method allows us to directly measure the reionization history without any assumption on its functional shape. As a proof of concept, we constructed mock non-repeating FRB sources to be detected with the Square Kilometre Array, assuming three different reionization histories with the same optical depth of Thomson scattering. We considered three cases of redshift measurements: (A) spectroscopic redshift for all mock data, (B) spectroscopic redshift for 10 per cent of mock data, and (C) redshift estimated from an empirical relation of FRBs between their time-integrated luminosity and rest-frame intrinsic duration. In all cases, the reionization histories are consistently reconstructed from the mock FRB data using our method. Our results demonstrate the capability of future FRBs in constraining the reionization history. [ABSTRACT FROM AUTHOR]

Background Nasopharyngeal carcinoma (NPC) is closely associated with genetic factors and Epstein-Barr virus infection, showing strong familial aggregation. Individuals with a family history suffer elevated NPC risk, requiring effective genetic counseling for risk stratification and individualized prevention. Methods We performed whole-exome sequencing on 502 familial NPC patients and 404 unaffected relatives and controls. We systematically evaluated the established cancer predisposition genes and investigated novel NPC susceptibility genes, making comparisons with 21 other familial cancers in the UK biobank (N = 5218). Results Rare pathogenic mutations in the established cancer predisposition genes were observed in familial NPC patients, including ERCC2 (1.39%), TP63 (1.00%), MUTYH (0.80%), and BRCA1 (0.80%). Additionally, 6 novel susceptibility genes were identified. RAD54L , involved in the DNA repair pathway together with ERCC2 , MUTYH , and BRCA1 , showed the highest frequency (4.18%) in familial NPC. Enrichment analysis found mutations in TP63 were enriched in familial NPC, and RAD54L and EML2 were enriched in both NPC and other Epstein-Barr virus–associated cancers. Besides rare variants, common variants reported in the studies of sporadic NPC were also associated with familial NPC risk. Individuals in the top quantile of common variant-derived genetic risk score while carrying rare variants exhibited increased NPC risk (odds ratio = 13.47, 95% confidence interval = 6.33 to 28.68, P  =   1.48 × 10–11); men in this risk group showed a cumulative lifetime risk of 24.19%, much higher than those in the bottom common variant-derived genetic risk score quantile and without rare variants (2.04%). Conclusions This study expands the catalog of NPC susceptibility genes and provides the potential for risk stratification of individuals with an NPC family history. [ABSTRACT FROM AUTHOR]

The Hubble constant (H 0) is a measurement to describe the expansion rate of the Universe in the current era. However, there is a 4.4σ discrepancy between the measurements from the early Universe and the late Universe. In this research, we propose a model-free and distance-free method to constrain H 0. Combining Friedman–Lemaître–Robertson–Walker cosmology with geometrical relation of the proper motion of extragalactic jets, the lower limit (H 0,min) of H 0 can be determined using only three cosmology-free observables: the redshifts of the host galaxies, and the approaching and receding angular velocities of radio jets. Using these, we propose to use the Kolmogorov–Smirnov test (K–S test) between cumulative distribution functions of H 0,min to differentiate cosmology. We simulate 100, 200, and 500 extragalactic jets with three levels of accuracy of the proper motion (μa and μr), at 10, 5, and 1 per cent, corresponding to the accuracies of the current and future radio interferometers. We perform K–S tests between the simulated samples as theoretical distributions with different H 0 and power-law index of velocity distribution of jets and mock observational data. Our result suggests increasing sample sizes leads to tighter constraints on both power-law index and the Hubble constant at moderate accuracy (i.e. |$10$| and |$5{{\ \rm per\ cent}}$|⁠), while at |$1{{\ \rm per\ cent}}$| accuracy, increasing sample sizes leads to tighter constraints on power-law index more. Improving accuracy results in better constraints in the Hubble constant compared with the power-law index in all cases, but it alleviates the degeneracy. [ABSTRACT FROM AUTHOR]

Addressing how strong UV radiation affects galaxy formation is central to understanding their evolution. The quenching of star formation via strong UV radiation (from starbursts or active galactic nuclei) has been proposed in various scenes to solve certain astrophysical problems. Around luminous sources, some evidence of decreased star formation has been found but is limited to a handful of individual cases. No direct, conclusive evidence on the actual role of strong UV radiation in quenching star formation has been found. Here, we present statistical evidence of decreased number density of faint (AB magnitude ≥ 24.75 mag) Ly α emitters (LAEs) around bright (AB magnitude < 24.75 mag) LAEs even when the radius goes up to 10 pMpc for z ≃ 5.7 LAEs. A similar trend is found for z ≃ 6.6 LAEs but only for faint LAEs within 1 pMpc radius from the bright LAEs. We use a large sample of 1077 (962) LAEs at z ≃ 5.7 (z ≃ 6.6) selected in total areas of 14 (21) deg2 with Subaru/Hyper Suprime-Cam narrow-band data, and thus, the result is of statistical significance for the first time at these high redshift ranges. A simple analytical calculation indicates that the radiation from the central LAE is not enough to suppress LAEs with AB mag ≥ 24.75 mag around them, suggesting additional physical mechanisms we are unaware of are at work. Our results clearly show that the environment is at work for the galaxy formation at z ∼ 6 in the Universe. [ABSTRACT FROM AUTHOR]

The origins of fast radio bursts (FRBs), astronomical transients with millisecond time-scales, remain unknown. One of the difficulties stems from the possibility that observed FRBs could be heterogeneous in origin; as some of them have been observed to repeat, and others have not. Due to limited observing periods and telescope sensitivities, some bursts may be misclassified as non-repeaters. Therefore, it is important to clearly distinguish FRBs into repeaters and non-repeaters, to better understand their origins. In this work, we classify repeaters and non-repeaters using unsupervised machine learning, without relying on expensive monitoring observations. We present a repeating FRB recognition method based on the Uniform Manifold Approximation and Projection (UMAP). The main goals of this work are to: (i) show that the unsupervised UMAP can classify repeating FRB population without any prior knowledge about their repetition, (ii) evaluate the assumption that non-repeating FRBs are contaminated by repeating FRBs, and (iii) recognize the FRB repeater candidates without monitoring observations and release a corresponding catalogue. We apply our method to the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) data base. We found that the unsupervised UMAP classification provides a repeating FRB completeness of 95 per cent and identifies 188 FRB repeater source candidates from 474 non-repeater sources. This work paves the way to a new classification of repeaters and non-repeaters based on a single epoch observation of FRBs. [ABSTRACT FROM AUTHOR]

How does the environment affect active galactic nucleus (AGN) activity? We investigated this question in an extinction-free way by selecting 1120 infrared (IR) galaxies in the AKARI North Ecliptic Pole Wide field at redshift z ≤ 1.2. A unique feature of the AKARI satellite is its continuous nine-band IR filter coverage, providing us with an unprecedentedly large sample of IR spectral energy distributions (SEDs) of galaxies. By taking advantage of this, for the first time, we explored the AGN activity derived from SED modelling as a function of redshift, luminosity, and environment. We quantified AGN activity in two ways: AGN contribution fraction (ratio of AGN luminosity to the total IR luminosity), and AGN number fraction (ratio of number of AGNs to the total galaxy sample). We found that galaxy environment (normalized local density) does not greatly affect either definitions of AGN activity of our IRG/LIRG samples (log L TIR ≤ 12). However, we found a different behaviour for ULIRGs (log L TIR > 12). At our highest redshift bin (0.7 ≲ z ≲ 1.2), AGN activity increases with denser environments, but at the intermediate redshift bin (0.3 ≲ z ≲ 0.7), the opposite is observed. These results may hint at a different physical mechanism for ULIRGs. The trends are not statistically significant (p ≥ 0.060 at the intermediate redshift bin, and p ≥ 0.139 at the highest redshift bin). Possible different behaviour of ULIRGs is a key direction to explore further with future space missions (e.g. JWST, Euclid, SPHEREx). [ABSTRACT FROM AUTHOR]

Fast radio bursts (FRBs) are millisecond transients of unknown origin(s) occurring at cosmological distances. Here we, for the first time, show time-integrated-luminosity functions and volumetric occurrence rates of non-repeating and repeating FRBs against redshift. The time-integrated-luminosity functions of non-repeating FRBs do not show any significant redshift evolution. The volumetric occurrence rates are almost constant during the past ∼10 Gyr. The nearly-constant rate is consistent with a flat trend of cosmic stellar-mass density traced by old stellar populations. Our findings indicate that the occurrence rate of non-repeating FRBs follows the stellar-mass evolution of long-living objects with ∼Gyr time-scales, favouring e.g. white dwarfs, neutron stars, and black holes, as likely progenitors of non-repeating FRBs. In contrast, the occurrence rates of repeating FRBs may increase towards higher redshifts in a similar way to the cosmic star formation rate density or black hole accretion rate density if the slope of their luminosity function does not evolve with redshift. Short-living objects with ≲Myr time-scales associated with young stellar populations (or their remnants, e.g. supernova remnants, young pulsars, and magnetars) or active galactic nuclei might be favoured as progenitor candidates of repeating FRBs. [ABSTRACT FROM AUTHOR]

Fast radio bursts (FRBs) are mysterious extragalactic radio signals. Revealing their origin is one of the central foci in modern astronomy. Previous studies suggest that occurrence rates of non-repeating and repeating FRBs could be controlled by the cosmic stellar-mass density (CSMD) and cosmic star formation-rate density (CSFRD), respectively. The Square Kilometre Array (SKA) is one of the best future instruments to address this subject due to its high sensitivity and high-angular resolution. Here, we predict the number of FRBs to be detected with the SKA. In contrast to previous predictions, we estimate the detections of non-repeating and repeating FRBs separately, based on latest observational constraints on their physical properties including the spectral indices, FRB luminosity functions, and their redshift evolutions. We consider two cases of redshift evolution of FRB luminosity functions following either the CSMD or CSFRD. At |$z$| ≳ 2, |$z$| ≳ 6, and |$z$| ≳ 10, non-repeating FRBs will be detected with the SKA at a rate of ∼104, ∼102, and ∼10 (sky−1 d−1), respectively, if their luminosity function follows the CSMD evolution. At |$z$| ≳ 1, |$z$| ≳ 2, and |$z$| ≳ 4, sources of repeating FRBs will be detected at a rate of ∼103, ∼102, and ≲10 (sky−1 d−1), respectively, assuming that the redshift evolution of their luminosity function is scaled with the CSFRD. These numbers could change by about one order of magnitude depending on the assumptions on the CSMD and CSFRD. In all cases, abundant FRBs will be detected by the SKA, which will further constrain the luminosity functions and number density evolutions. [ABSTRACT FROM AUTHOR]

Observationally, it has been reported that the densest stellar system in the Universe does not exceed a maximum stellar surface density, |$\Sigma ^{\max }_{*}$| = |$3\times 10^5\, {\rm M}_{\odot }\,{\rm pc}^{-2}$|⁠ , throughout a wide physical scale ranging from star cluster to galaxy. This suggests that there exists a fundamental physics that regulates the star formation and stellar density. However, factors that determine this maximum limit are not clear. In this study, we show that |$\Sigma ^{\max }_{*}$| of galaxies is not a constant as previous work reported, but actually it depends on the stellar mass. We select galaxy sample from the Sloan Digital Sky Survey Data Release 12 at z  = 0.01–0.5. In contrast to a constant maximum predicted by theoretical models, |$\Sigma ^{\max }_{*}$| strongly depends on stellar mass, especially for less massive galaxies with |$\text{$\sim$}10^{10}\, {\rm M}_{\odot }$|⁠. We also found that a majority of high-Σ* galaxies show red colours and low star formation rates. These galaxies probably reach the |$\Sigma ^{\max }_{*}$| as a consequence of the galaxy evolution from blue star forming to red quiescent by quenching star formation. One possible explanation of the stellar-mass dependence of |$\Sigma ^{\max }_{*}$| is a mass-dependent efficiency of stellar feedback. The stellar feedback could be relatively more efficient in a shallower gravitational potential, which terminates star formation quickly before the stellar system reaches a high stellar density. [ABSTRACT FROM AUTHOR]

We present the analysis of a new near-infrared (NIR) spectrum of a recently discovered |$z$|  = 6.621 quasar PSO J006 + 39 in an attempt to explore the early growth of supermassive black holes (SMBHs). This NIR (rest-frame ultraviolet, UV) spectrum shows blue continuum slope and rich metal emission lines in addition to Lyα line. We utilize the |$\rm{Mg\,\rm {\small II}}$| line width and the rest-frame luminosity |$L_{3000\,\mathring{\rm A}}$| to find the mass of SMBH (M BH) to be |${\sim } 10^8 \, \mathrm{M}_\odot$|⁠, making this one of the lowest mass quasars at high redshift. The power-law slope index (αλ) of the continuum emission is −2.94 ± 0.03, significantly bluer than the slope of αλ = −7/3 predicted from standard thin disc models. We fit the spectral energy distribution (SED) using a model which can fit local SMBHs, which includes warm and hot Comptonization powered by the accretion flow as well as an outer standard disc. The result shows that the very blue slope is probably produced by a small radial (∼230 gravitational radius, R g) extent of the standard accretion disc. All plausible SED models require that the source is super-Eddington (L bol/ L Edd ≳ 9), so the apparently small disc may simply be the inner funnel of a puffed up flow, and clearly the SMBH in this quasar is in a rapid growth phase. We also utilize the rest-frame UV emission lines to probe the chemical abundance in the broad-line region (BLR) of this quasar. We find that this quasar has super solar metallicity through photoionization model calculations. [ABSTRACT FROM AUTHOR]

We present NuSTAR spectral and timing studies of the supergiant fast X-ray transient (SFXT) IGR J17544−2619. The spectrum is well described by an ∼1 keV blackbody and a hard continuum component, as expected from an accreting X-ray pulsar. We detect a cyclotron line at 17 keV, confirming that the compact object in IGR J17544−2619 is indeed a neutron star. This is the first measurement of the magnetic field in an SFXT. The inferred magnetic field strength, B = (1.45 ± 0.03) × 1012G (1 + z) is typical of neutron stars in X-ray binaries, and rules out a magnetar nature for the compact object. We do not find any significant pulsations in the source on time-scales of 1–2000 s. [ABSTRACT FROM AUTHOR]

STUDY QUESTION Do any mutations in growth differentiation factor 9 (GDF9) have a role in diminished ovarian reserve (DOR) in young women? SUMMARY ANSWER The GDF9 p.R146C mutation may be a source of DOR in some young women. WHAT IS KNOWN ALREADY DOR affects 10% of women under 37 years of age and is associated with accelerated expenditure of follicles. GDF9 is an oocyte-secreted factor that plays a critical role in follicular development and female fertility. Several GDF9 variants have been linked to ovarian dysfunction. STUDY DESIGN, SIZE, DURATION This case–control study included 139 women with DOR and 152 controls aged under 37 years. PARTICIPANTS/MATERIALS, SETTING, METHODS All women were recruited in a Chinese tertiary center and underwent DNA sequencing of GDF9 gene. We then determined the molecular and biological properties of mutant GDF9 proteins using protein expression, structural prediction and functional analyses. MAIN RESULTS AND THE ROLE OF CHANCE We identified two mutations in the proregion of GDF9 gene: c.169T > G (p.D57Y) and c.436T > C (p.R146C). The p.R146C mutation was found in three women with DOR but was absent in the control population. This mutation was also associated with significant reductions in GDF9 mature protein secretion in cultured cells. Functional studies with human granulosa cells (GCs) showed that the p.R146C mutation reduced the abilities of GDF9 to stimulate GC proliferation and to activate the Smad2 pathway. Protein structure modeling predicted that p.R146C disrupted an α-helix in GDF9 protein. In contrast with p.R146C, the p.D57Y mutation, found in both the DOR and control groups (6 versus 2), had no obvious deleterious effects. LIMITATIONS, REASONS FOR CAUTION Larger studies in varying populations may validate the role of GDF9 mutation in young women with DOR. WIDER IMPLICATIONS OF THE FINDINGS These results may provide new insights into the pathophysiological mechanisms of early-onset DOR. STUDY FUNDING/COMPETING INTEREST(S) This work was supported by the National Natural Science Foundation of China (30900517 and 81100468), the National Basic Research Program of China (2012CB944901 and 2011CB944502), the Fundamental Research Funds for the Central Universities, Ministry of Education, China (2011KYJD008), Program for Changjiang Scholars and Innovative Research Team in University (IRT1184) and Program for Key Subjects Group of Reproductive Medicine at Zhejiang Province (XKQ-009-002). The authors have no competing interests to declare. [ABSTRACT FROM PUBLISHER]

We analyse the stellar and hot gas content of 18 nearby, low-mass galaxy clusters, detected in redshift space and selected to have a dynamical mass ), as measured from the 2dF Galaxy Redshift Survey. We combine X-ray measurements from both Chandra and XMM with ground-based near-infrared observations from CTIO, Anglo-Australian Telescope and Canada-France-Hawaii Telescope to compare the mass in hot gas and stars to the dynamical mass and state of the clusters. Only 13 of the clusters are detected in X-ray emission, and for these systems we find that a range of 7-20 per cent of their baryonic mass, and per cent of their dynamical mass, is detected in starlight, similar to what is observed in more massive clusters. In contrast, the five undetected clusters are underluminous in X-ray emission, by up to a factor of 10, given their stellar mass. Although the velocity distribution of cluster members in these systems is indistinguishable from a Gaussian, all show subtle signs of being unrelaxed: either they lack a central, dominant galaxy, or the bright galaxy distribution is less concentrated and/or more elongated than the rest of the sample. Thus we conclude that low-mass clusters and groups selected from the velocity distribution of their galaxies exhibit a dichotomy in their hot gas properties. Either they are detected in X-ray, in which case they generally lie on the usual scaling relations, or they are completely undetected in X-ray emission. The non-detections may be partly related to the apparently young dynamical state of the clusters, but it remains a distinct possibility that some of these systems are exceptionally devoid of hot emitting gas as the result of its expulsion or rarefaction. [ABSTRACT FROM AUTHOR]