Aims. Our scientific goal is to provide revised membership lists of the α Per, Pleiades, and Praesepe clusters exploiting the second data release of Gaia and produce five-dimensional maps (α, δ, π, ...μα cos δ, μδ) of these clusters. Methods. We implemented the kinematic method combined with the statistical treatment of parallaxes and proper motions to identify astrometric member candidates of three of the most nearby and best studied open clusters in the sky. Results. We cross-correlated the Gaia catalogue with large-scale public surveys to complement the astrometry of Gaia with multi-band photometry from the optical to the mid-infrared. We identified 517, 1248, and 721 bona fide astrometric member candidates inside the tidal radius of α Per, the Pleiades, and Praesepe, respectively. We cross-matched our final samples with catalogues from previous surveys to address the level of completeness. We update the main physical properties of the clusters, including mean distance and velocity, as well as core, half-mass, and tidal radii. We infer updated ages from the white dwarf members of the Pleiades and Praesepe. We derive the luminosity and mass functions of the three clusters and compare them to the field mass function. We compute the positions in space of all member candidates in the three regions to investigate their distribution in space. Conclusions. We provide updated distances and kinematics for the three clusters. We identify a list of members in the α Per, Pleiades, and Praesepe clusters from the most massive stars all the way down to the hydrogen-burning limit with a higher confidence and better astrometry than previous studies. We produce complete 5D maps of stellar and substellar bona fide members in these three regions. The photometric sequences derived in several colour–magnitude diagrams represent benchmark cluster sequences at ages from 90 to 600 Myr. We note the presence of a stream around the Pleiades cluster extending up to 40 pc from the cluster centre.
Aims. Our scientific goal is to provide a 3D map of the nearest open cluster to the Sun, the Hyades, combining the recent release of Gaia astrometric data, ground-based parallaxes of sub-stellar ...member candidates and photometric data from surveys which cover large areas of the cluster. Methods. We combined the second Gaia release with ground-based H-band parallaxes obtained with the infrared camera on the 2 m robotic Liverpool telescope to astrometrically identify stellar and sub-stellar members of the Hyades, the nearest open cluster to the Sun. Results. We find 1764 objects within 70° radius from the cluster centre from the Gaia second data release, whose kinematic properties are consistent with the Hyades. We limit our study to 30 pc from the cluster centre (47.03 ± 0.20 pc) where we identify 710 candidate members, including 85 and 385 in the core and tidal radius, respectively. We determine proper motions and parallaxes of eight candidate brown dwarf members and confirm their membership. Using the 3D positions and a model-based mass-luminosity relation we derive a luminosity and mass function in the 0.04–2.5 M⊙ range. We confirm evidence for mass segregation in the Hyades and find a dearth of brown dwarfs in the core of the cluster. From the white dwarf members we estimate an age of 640 −49+67 − 49 + 67 $ ^{+67}_{-49} $ Myr. Conclusions. We identify a list of members in the Hyades cluster from the most massive stars down to the brown dwarfs. We produce for the first time a 3D map of the Hyades cluster in the stellar and sub-stellar regimes and make available the list of candidate members.
Context. Sigma Orionis is an open cluster in the nearest giant star formation site – Orion. Its youth (3−5 Myr), low reddening, and relative vicinity make it an important benchmark cluster to study ...stellar and substellar formation and evolution. Aims. Young star-forming sites are complex and hierarchical. Precision astrometry from Gaia DR3 enables the exploration of their fine structure. Methods. We used the modified convergent point technique to kinematically re-evaluate the members in the Sigma Orionis cluster and its vicinity. Results. We present clear evidence for three kinematically distinct groups in the Sigma Orionis region. The second group, the RV Orionis association, is adjacent to the Sigma Orionis cluster and is composed only of low-mass stars. The third group, the Flame association, whose age is comparable to that of Sigma Orionis, overlaps with the younger NGC 2024 in the Flame Nebula. In total, we have discovered 105 members of this complex not previously found in the literature (82 in Sigma Orionis, 19 in the Flame association, and 4 in the RV Orionis association).
Aims. Our aim is to identify brown dwarf members of the nearby Hyades open star cluster to determine the photometric and spectroscopic properties of brown dwarfs at moderately old ages and extend the ...knowledge of the substellar mass function of the cluster. Methods. We cross-matched the 2MASS and AllWISE public catalogues and measured proper motions to identify low-mass stars and brown dwarf candidates in an area of radius eight degrees around the central region of the Hyades cluster. We identified objects with photometry and proper motions consistent with cluster membership. For the faintest (J = 17.2 mag) most promising astrometric and photometric low-mass candidate 2MASS J04183483+2131275, with a membership probability of 94.5%, we obtained low-resolution (R = 300−1000) and intermediate-resolution (R = 2500) spectroscopy with the 10.4m Gran Telescopio Canarias. Results. From the low-resolution spectra we determined a L5.0 ± 0.5 spectral type, consistent with the available photometry. In the intermediate dispersion spectrum we detected Hα in emission (marginally resolved with a full width half maximum of ~2.8 Å) and determined a log (LHα/Lbol) = −6.0 dex. From Hα we obtained a radial velocity of 38.0 ± 2.9 km s-1, which combined with the proper motion leads to space velocities which are fully consistent with membership in the Hyades cluster. We also report a detection in the H2 band by the UKIDSS Galactic Plane Survey. Using evolutionary models we determine from the available photometry of the object a mass in the range 0.039−0.055 M⊙. Brown dwarfs with masses below 0.055 M⊙ should fully preserve its initial lithium content, and indeed the spectrum at 6708 Å may show a feature consistent with lithium preservation; however, a higher S/N is needed to confirm this point. Conclusions. We have identified a new high-probability L5 brown dwarf member of the Hyades cluster. This is the first relatively old L5 brown dwarf with a well-determined age (500−700 Myr) and measured chromospheric emission.
Aims. From the luminosity, effective temperature and age of the Hyades brown dwarf 2MASS J04183483+2131275 (2M0418), substellar evolutionary models predict a mass in the range 39−55 Jupiter masses ...(MJup) which is insufficient to produce any substantial lithium burning except for the very upper range >53 MJup. Our goal is to measure the abundance of lithium in this object, test the consistency between models and observations and refine constraints on the mass and age of the object. Methods. We used the 10.4-m Gran Telescopio Canarias (GTC) with its low-dispersion optical spectrograph to obtain ten spectra of 2277 s each covering the range 6300–10 300 Å with a resolving power of R ~ 500. Results. In the individual spectra, which span several months, we detect persistent unresolved Hα in emission with pseudo equivalent widths (pEW) in the range 45–150 Å and absorption lines of various alkalis with the typical strengths found in objects of L5 spectral type. The lithium resonance line at 6707.8 Å is detected with pEW of 18 ± 4 Å in 2M0418 (L5). Conclusions. We determine a lithium abundance of log N(Li) = 3.0 ± 0.4 dex consistent with a minimum preservation of 90% of this element which confirms 2M0418 as a brown dwarf with a maximum mass of 52 MJup. We infer a maximum age for the Hyades of 775 Myr from a comparison with the BHAC15 models. Combining recent results from the literature with our study, we constrain the mass of 2M0418 to 45–52 MJup and the age of the cluster to 580–775 Myr (1σ) based on the lithium depletion boundary method.
Glucagon and thyroid hormone (T3) exhibit therapeutic potential for metabolic disease but also exhibit undesired effects. We achieved synergistic effects of these two hormones and mitigation of their ...adverse effects by engineering chemical conjugates enabling delivery of both activities within one precisely targeted molecule. Coordinated glucagon and T3 actions synergize to correct hyperlipidemia, steatohepatitis, atherosclerosis, glucose intolerance, and obesity in metabolically compromised mice. We demonstrate that each hormonal constituent mutually enriches cellular processes in hepatocytes and adipocytes via enhanced hepatic cholesterol metabolism and white fat browning. Synchronized signaling driven by glucagon and T3 reciprocally minimizes the inherent harmful effects of each hormone. Liver-directed T3 action offsets the diabetogenic liability of glucagon, and glucagon-mediated delivery spares the cardiovascular system from adverse T3 action. Our findings support the therapeutic utility of integrating these hormones into a single molecular entity that offers unique potential for treatment of obesity, type 2 diabetes, and cardiovascular disease.
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•Glucagon/T3 corrects dyslipidemia, obesity, and hyperglycemia in DIO mice•Glucagon/T3 improves NASH and atherosclerosis in preclinical disease models•Precise delivery of T3 to the liver mediates benefits and spares cardiac toxicity•Hepatic T3 action counteracts the diabetogenic liability of glucagon
The therapeutic benefits of two hormones are maximized in a synthetic hybrid molecule that treats metabolic syndrome in mice by synergizing favorable effects and off-setting liabilities.
Visuospatial working memory (VSWM) deficits have been demonstrated to occur during the development of type‐1‐diabetes (T1D). Despite confirming the early appearance of distinct task‐related brain ...activation patterns in T1D patients compared to healthy controls, the effect of VSWM load on functional brain connectivity during task performance is still unknown. Using electroencephalographic methods, the present study evaluated this topic in clinically well‐controlled T1D young patients and healthy individuals, while they performed a VSWM task with different memory load levels during two main VSWM processing phases: encoding and maintenance. The results showed a significantly lower number of correct responses and longer reaction times in T1D while performing the task. Besides, higher and progressively increasing functional connectivity indices were found for T1D patients in response to cumulative degrees of VSWM load, from the beginning of the VSWM encoding phase, without notably affecting the VSWM maintenance phase. In contrast, healthy controls managed to solve the task, showing lower functional brain connectivity during the initial VSWM processing steps with more gradual task‐related adjustments. Present results suggest that T1D patients anticipate high VSWM load demands by early recruiting supplementary processing resources as the probable expression of a more inefficient, though paradoxically better adjusted to task demands cognitive strategy.
Previously, we have documented that type‐1‐diabetes (TD1) affects visuospatial working memory (VSWM) operation. The present study evaluates the functional brain connectivity underlying the performance of a VSWM task with two memory load levels in young T1D patients and healthy controls. We found differences between the groups, primarily affecting the encoding phase of working memory processing. The results suggest that T1D patients anticipate task demands by engaging more early neural processing resources and functional connections.
Aims. Our aim is to identify substellar members of the nearby Hyades open star cluster to determine the photometric and spectroscopic properties of brown dwarfs at moderately old ages and extend our ...knowledge of the substellar mass function of the cluster. Methods. We cross-matched the 2MASS and WISE public catalogues and measured proper motions to identify low-mass stars and brown dwarf member candidates in an area of a radius of ten degrees around the central region of the Hyades cluster. We employed astrometric and photometric criteria, Gaia data, and a maximum likelihood method developed by our group to estimate distances. We selected 36 objects that are candidate Hyades members, 21 of which have not been reported previously. Results. We have identified 21 new Hyades member candidates that are placed at the lower end of the main sequence. The photometry of 9 candidates places them in the substellar regime, and 2 are at the L/T transition. We also recovered a number of L dwarfs from earlier surveys. Finally, we calculated the mass function for the low-mass population of the cluster and found that the Hyades cluster might have lost 60%–80% of its substellar members.
We present the discovery of a companion near the deuterium-burning mass limit located at a very wide distance, at an angular separation of lambda 6 double prime + 0.1 double prime (projected distance ...of similar to 670 AU) from UScoCTIO 108, a brown dwarf of the very young Upper Scorpius association. Optical and near-infrared photometry and spectroscopy confirm the cool nature of both objects, with spectral types of M7 and M9.5, respectively, and that they are bona fide members of the association, showing low gravity and features of youth. Their masses, estimated from the comparison of their bolometric luminosities and theoretical models for the age range of the association, are 60 plus or minus 20 and 14 super(+) sub(-) super(2) sub(8) super(M) sub(Jup), respectively. The existence of this object around a brown dwarf at this wide orbit suggests that the companion is unlikely to have formed in a disk based on current planet formation models. Because this system is rather weakly bound, they probably did not form through dynamical ejection of stellar embryos.
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