Miracle-dz/UniFAR-FTUs huggingface dataset:
EVALUATING GYROCHRONOLOGY ON THE ZERO-AGE-MAIN-SEQUENCE: ROTATION PERIODS IN THE SOUTHERN OPEN CLUSTER BLANCO 1 FROM THE KELT-SOUTH SURVEY

We report periods for 33 members of Blanco 1 as measured from Kilodegree Extremely Little Telescope-South light curves, the first reported rotation periods for this benchmark zero-age-main-sequence open cluster. The distribution of these stars spans from late-A or early-F dwarfs to mid-K with periods ranging from less than a day to ∼8 days. The rotation period distribution has a morphology similar to the coeval Pleiades cluster, suggesting the universal nature of stellar rotation distributions. Employing two different gyrochronology methods, we find an age of 146 Myr for the cluster. Using the same techniques, we infer an age of 134 Myr for the Pleiades measured from existing literature rotation periods. These rotation-derived ages agree with independently determined cluster ages based on the lithium depletion boundary technique. Additionally, we evaluate different gyrochronology models and quantify levels of agreement between the models and the Blanco 1/Pleiades rotation period distributions, including incorporating the rotation distributions of clusters at ages up to 1.1 Gyr. We find the Skumanich-like spin-down rate sufficiently describes the rotation evolution of stars hotter than the Sun; however, we find cooler stars rotating faster than predicted by a Skumanich law, suggesting a mass dependence in the efficiency of stellar angular momentum loss rate. Finally, we compare the Blanco 1 and Pleiades rotation period distributions to available nonlinear angular momentum evolution models. We find they require a significant mass dependence on the initial rotation rate of solar-type stars to reproduce the observed range of rotation periods at a given stellar mass and are furthermore unable to predict the observed over-density of stars along the upper envelope of the clusters' rotation distributions.
CALTECH CORE-COLLAPSE PROJECT (CCCP) OBSERVATIONS OF TYPE IIn SUPERNOVAE: TYPICAL PROPERTIES AND IMPLICATIONS FOR THEIR PROGENITOR STARS

Type IIn supernovae (SNe IIn) are rare events, constituting only a few percent of all core-collapse SNe, and the current sample of well-observed SNe IIn is small. Here, we study the four SNe IIn observed by the Caltech Core-Collapse Project (CCCP). The CCCP SN sample is unbiased to the extent that object selection was not influenced by target SN properties. Therefore, these events are representative of the observed population of SNe IIn. We find that a narrow P-Cygni profile in the hydrogen Balmer lines appears to be a ubiquitous feature of SNe IIn. Our light curves show a relatively long rise time (>20 days) followed by a slow decline stage (0.01–0.15 mag day−1), and a typical V-band peak magnitude of MV = −18.4 ± 1.0 mag. We measure the progenitor star wind velocities (600–1400 km s−1) for the SNe in our sample and derive pre-explosion mass-loss rates (0.026–0.12 M☉ yr−1). We compile similar data for SNe IIn from the literature and discuss our results in the context of this larger sample. Our results indicate that typical SNe IIn arise from progenitor stars that undergo luminous-blue-variable-like mass loss shortly before they explode.
Pathophysiology and Therapeutic Approaches for Spinal Cord Injury

Spinal cord injury (SCI) is a disabling condition that disrupts motor, sensory, and autonomic functions. Despite extensive research in the last decades, SCI continues to be a global health priority affecting thousands of individuals every year. The lack of effective therapeutic strategies for patients with SCI reflects its complex pathophysiology that leads to the point of no return in its function repair and regeneration capacity. Recently, however, several studies started to uncover the intricate network of mechanisms involved in SCI leading to the development of new therapeutic approaches. In this work, we present a detailed description of the physiology and anatomy of the spinal cord and the pathophysiology of SCI. Additionally, we provide an overview of different molecular strategies that demonstrate promising potential in the modulation of the secondary injury events that promote neuroprotection or neuroregeneration. We also briefly discuss other emerging therapies, including cell-based therapies, biomaterials, and epidural electric stimulation. A successful therapy might target different pathologic events to control the progression of secondary damage of SCI and promote regeneration leading to functional recovery.
STELLAR POPULATIONS OF HIGHLY MAGNIFIED LENSED GALAXIES: YOUNG STARBURSTS AT z ∼ 2

We present a comprehensive analysis of the rest-frame UV to near-IR spectral energy distributions (SEDs) and rest-frame optical spectra of four of the brightest gravitationally lensed galaxies in the literature: RCSGA 032727-132609 at z = 1.70, MS1512-cB58 at z = 2.73, SGAS J152745.1+065219 at z = 2.76, and SGAS J122651.3+215220 at z = 2.92. This includes new Spitzer imaging for RCSGA0327 as well as new spectra, near-IR imaging and Spitzer imaging for SGAS1527 and SGAS1226. Lensing magnifications of 3–4 mag allow a detailed study of the stellar populations and physical conditions. We compare star formation rates (SFRs) as measured from the SED fit, the Hα and [O ii] λ3727 emission lines, and the UV+IR bolometric luminosity where 24 μm photometry is available. The SFR estimate from the SED fit is consistently higher than the other indicators, which suggests that the Calzetti dust extinction law used in the SED fitting is too flat for young star-forming galaxies at z ∼ 2. Our analysis finds similar stellar population parameters for all four lensed galaxies: stellar masses (3–7) × 109 M☉, young ages ∼100 Myr, little dust content E(B − V) = 0.10–0.25, and SFRs around 20–100 M☉ yr−1. Compared to typical values for the galaxy population at z ∼ 2, this suggests we are looking at newly formed, starbursting systems that have only recently started the buildup of stellar mass. These results constitute the first detailed, uniform analysis of a sample of the growing number of strongly lensed galaxies known at z ∼ 2.
An Improved Bound for Upper Domination of Cartesian Products of Graphs

In this paper, we prove a problem proposed by Bresar: for any graphs $G$ and $H$, $\Gamma(G\square H)\ge\Gamma(G)\Gamma(H)+ \min\{|V(G)|-\Gamma(G),|V(H)|-\Gamma(H)\}$, where $\Gamma(G)$ denotes the upper domination number of $G$.
One dimensional description of the gravitational perturbation in a Kerr background

The perturbation equation in a Kerr background is written as a coupled system of one dimensional equations for the different modes in the time domain. Numerical simulations show that the dominant mode in the gravitational response is the one corresponding to the mode of the initial perturbation, allowing us to conjecture that the coupling among the modes has a weak influence in our system of equations. We conclude that by neglecting the coupling terms it can be obtained as a one dimensional harmonic equation which indeed describes with good accuracy the gravitational response from the Kerr black hole with low spin, while only a few couplings are necessary to describe a high-spin one. This result may help us to understand the structure of test fields in a Kerr background and even to generate accurate waveforms for various cases in an efficient manner.
Diffraction and Smith-Purcell radiation on the hemispherical bulges in a metal plate

The radiation resulting from the uniform motion of a charged particle near a hemispheric bulge on a metal plane is considered. The description of the radiation process based on the method of images is developed for the case of non-relativistic particle and a perfectly conducting target. The spectral-angular and spectral densities of the diffraction radiation on the single bulge (as well as the Smith-Purcell radiation on the periodic string of bulges) are computed. The possibility of application of the developed approach to the case of relativistic incident particle is discussed.
Example of applying a Health, Safety and Environment management system in cetacean research: Case study from a satellite tagging field accident

Satellite telemetry is a powerful method to study the movements and habitat use of cetaceans. The deployment of transmitters is usually conducted using remote techniques and involves close approaches to the target animals. The present study reports on an accidental collision between a female humpback whale and an inflatable boat, which occurred on 7 October 2010 off the coast of Brazil. At the time of the accident, the boat was occupied by four crew members: the tagger, the photographer, the driver and an observer. This collision resulted in head trauma and severe brain injury to the photographer. It also resulted in changes of the tagging deployment procedures and the implementation of a Health, Safety and Environment (HSE) management system. The objective of this work is to report on this accident and describe procedures adopted to assess and minimise risks. Changes and updates in deployment protocols are viewed as improvements to minimise accidents during marine mammal tagging operations. Some of these improvements were also discussed and implemented by other organisations. Accidents such as the one reported here can and should be prevented. However, when they occur, they provide an opportunity to assess and correct unanticipated deficiencies in field work procedures.
Nonsingular Global Fast Terminal Sliding Mode Control with Extended State Observer for Contact Force Regulation in Aerial Manipulator

The aerial manipulator is a novel flying robot consisting of an unmanned aerial vehicle (UAV) and a multi-degree-of-freedom (DoF) robotic arm. It can actively interact with the environment to conduct dangerous or inaccessible tasks for humans. In this paper, we propose a composite control scheme considering force and position for the aerial manipulator to operate in steady contact with the environment when influenced by external disturbances. First, a contact force control method without employing the force sensor is obtained on the mechanical relationship of the system’s contact with the environment. Second, we regard the system’s internal coupling and external disturbance as lumped disturbances and design an extended state observer (ESO) to estimate them. Combined with the disturbance estimation and the nonsingular global fast sliding mode algorithm, a controller derived from the Lyapunov theory is proposed. Finally, we compare the proposed controller with the other four controllers through simulations and actual flight experiments. The results show that the proposed controller can effectively restrain disturbances, reduce convergence time, and guarantee steady contact under external disturbances.
Rethinking the Role of Indigenous Knowledge in Sustainable Mountain Development and Protected Area Management in Canada and Aotearoa/New Zealand

For many Indigenous communities who live in mountain regions around the globe, the histories of mountain park development have often facilitated dispossession from ancestral territories. Diverse Indigenous communities share similar experiences, where park interests have conflicted with Indigenous lands. However, colonial practices of park management are consistently being rethought. Canada and Aotearoa/New Zealand are examples where new designations of parks are now emerging to support management practices that assert Indigenous knowledge and land rights. Guided by Indigenous methodologies and supported by secondary literature, the analysis of policy documents, and community-based research with Indigenous communities in Canada and Aotearoa/New Zealand, this article highlights grassroots Indigenous-led park management practices that move beyond colonial frameworks. This research indicates the potential of protected areas to strengthen the livelihoods of Indigenous Peoples and mountain ecosystems by demonstrating how colonial histories can be reconciled and conservation policies integrated to support the sustainable development of mountain regions.
Exploring the variable stars in the globular cluster NGC 5024 (M53): new RR Lyrae and SX Phoenicis stars

We report CCD V and I time series photometry of the globular cluster NGC 5024 (M53). The technique of difference image analysis has been used which enables photometric precisions better than 10 mmag for stars brighter than V ∼ 18.5 mag even in the crowded central regions of the cluster. The high photometric precision has resulted in the discovery of two new RR1 stars and 13 SX Phe stars. A detailed identification chart is given for all the variable stars in the field of our images of the cluster. Periodicities were calculated for all RR Lyrae and SX Phe stars and a critical comparison is made with previous determinations. Out of the four probable SX Phe variables reported by Dekany & Kovacs, the SX Phe nature is confirmed only for V80; V81 is an unlikely case while V82 and V83 remain as dubious cases. Previous misidentifications of three variables are corrected. Astrometric positions with an uncertainty of ∼0.3 arcsec are provided for all variables. The light-curve Fourier decomposition of RR0 and RR1 is discussed, we find a mean metallicity of [Fe/H] = ―1.92 ± 0.06 in the scale of Zinn & West from 19 RR0 stars. The true distance moduli 16.36 ± 0.05 and 16.28 ± 0.07 and the corresponding distances 18.7 ± 0.4 and 18.0 ± 0.5 kpc are found from the RR0 and RR1 stars, respectively. These values are in agreement with the theoretical period-luminosity relations for RR Lyrae stars in the I band and with recent luminosity determinations for the RR Lyrae stars in the Large Magellanic Cloud (LMC). The age of 13.25 ± 0.50 Gyr, for NGC 5024, E(B ― V) = 0.02 and the above physical parameters of the cluster, as indicated from the RR0 stars, produce a good isochrone fitting to the observed colour-magnitude diagram (CMD). The period-luminosity (PL) relation for SX Phe stars in NGC 5024 in the V and I bands is discussed in the light of the 13 newly found SX Phe stars, and their pulsation mode is identified in most cases.
Two-Weight Inequalities for Commutators with Fractional Integral Operators

In this paper we investigate weighted norm inequalities for the commutator of a fractional integral operator and multiplication by a function. In particular, we show that, for $\mu,\lambda\in A_{p,q}$ and $\alpha/n+1/q=1/p$, the norm $\| [b,I_\alpha]:L^p(\mu^p)\to L^q(\lambda^q) \|$ is equivalent to the norm of $b$ in the weighted BMO space $BMO(\nu)$, where $\nu=\mu\lambda^{-1}$. This work extends some of the results on this topic existing in the literature, and continues a line of investigation which was initiated by Bloom in 1985 and was recently developed further by the first author, Lacey, and Wick.
Bottom-quark associated Higgs-boson production: reconciling the four- and five-flavour scheme approach

The main arguments in the discussion of the proper treatment of the total inclusive cross section for bottom-quark associated Higgs-boson production are briefly reviewed. A simple and pragmatic formula for the combination of the so-called four- and five-flavour schemes is suggested, including the treatment of the respective theory error estimates. The numerical effects of this matching formula are discussed.
Genomics-Driven Application of Plant Genetic Resources for Sustainable Agriculture

Genebanks preserve the valuable genetic diversity in the form of huge collections of plant genetic resources (PGR). Dr Raj S. Paroda has spearheaded the modernization of one of the world’s largest genebanks, the ICAR-National Bureau of Plant Genetic Resources (NBPGR), New Delhi, India, which currently houses nearly 462,466 accessions. Dr Paroda’s notable contributions in the ﬁ eld of PGR management have earned him the popular name of “Genebank Guru”. As Dr Paroda turns 80 on August 28, 2022, we commemorate the occasion by synthesizing an article in line with Dr Paroda’ forward-thinking vision for PGR management and utilization. The present article highlights how modern genetic technologies have expanded our capacity to characterize and exploit the unexplored genetic diversity from genebanks. Extensive molecular and phenotypic characterisation support eﬃ cient strategies to minimize large PGR collections to workable sizes, thus allowing targeted search of plant diversity for sustainable agriculture. As the technological innovations transform genebanks into “bio-digital resource centres”, availability of detailed genotype-phenotype maps and genomic predictions for large PGR collections will guide selection and breeding decisions in crop improvement programmes. Eﬀ ective preservation and use of PGR collections is imperative to impart climate change adaptation to crop production systems and safeguarding our future food supply.
Simulating galactic outflows with thermal supernova feedback

Cosmological simulations make use of sub-grid recipes for the implementation of galactic winds driven by massive stars because direct injection of supernova energy in thermal form leads to strong radiative losses, rendering the feedback inefficient. We argue that the main cause of the catastrophic cooling is a mismatch between the mass of the gas in which the energy is injected and the mass of the parent stellar population. Because too much mass is heated, the temperatures are too low and the cooling times too short. We use analytic arguments to estimate, as a function of the gas density and the numerical resolution, the minimum heating temperature that is required for the injected thermal energy to be efficiently converted into kinetic energy. We then propose and test a stochastic implementation of thermal feedback that uses this minimum temperature increase as an input parameter and that can be employed in both particle-based and grid-based codes. We use smoothed particle hydrodynamic simulations to test the method on models of isolated disc galaxies in dark matter haloes with total mass 1010 and 1012 h−1 M⊙. The thermal feedback strongly suppresses the star formation rate and can drive massive, large-scale outflows without the need to turn off radiative cooling temporarily. In accordance with expectations derived from analytic arguments, for sufficiently high resolution the results become insensitive to the imposed temperature jump and also agree with high-resolution simulations employing kinetic feedback.
The Influence of Atomic Diffusion on Stellar Ages and Chemical Tagging

In the era of large stellar spectroscopic surveys, there is an emphasis on deriving not only stellar abundances but also the ages for millions of stars. In the context of Galactic archeology, stellar ages provide a direct probe of the formation history of the Galaxy. We use the stellar evolution code MESA to compute models with atomic diffusion—with and without radiative acceleration—and extra mixing in the surface layers. The extra mixing consists of both density-dependent turbulent mixing and envelope overshoot mixing. Based on these models we argue that it is important to distinguish between initial, bulk abundances (parameters) and current, surface abundances (variables) in the analysis of individual stellar ages. In stars that maintain radiative regions on evolutionary timescales, atomic diffusion modifies the surface abundances. We show that when initial, bulk metallicity is equated with current, surface metallicity in isochrone age analysis, the resulting stellar ages can be systematically overestimated by up to 20%. The change of surface abundances with evolutionary phase also complicates chemical tagging, which is the concept that dispersed star clusters can be identified through unique, high-dimensional chemical signatures. Stars from the same cluster, but in different evolutionary phases, will show different surface abundances. We speculate that calibration of stellar models may allow us to estimate not only stellar ages but also initial abundances for individual stars. In the meantime, analyzing the chemical properties of stars in similar evolutionary phases is essential to minimize the effects of atomic diffusion in the context of chemical tagging.
Perturbations of near-horizon geometries and instabilities of Myers-Perry black holes

It is shown that the equations governing linearized gravitational (or electromagnetic) perturbations of the near-horizon geometry of any known extreme vacuum black hole (allowing for a cosmological constant) can be Kaluza-Klein reduced to give the equation of motion of a charged scalar field in AdS{sub 2} with an electric field. One can define an effective Breitenloehner-Freedman bound for such a field. We conjecture that if a perturbation preserves certain symmetries then a violation of this bound should imply an instability of the full black hole solution. Evidence in favor of this conjecture is provided by the extreme Kerr solution and extreme cohomogeneity-1 Myers-Perry solution. In the latter case, we predict an instability in seven or more dimensions and, in five dimensions, we present results for operator conformal weights assuming the existence of a conformal field theory dual. We sketch a proof of our conjecture for scalar field perturbations.
On extreme transient events from rotating black holes and their gravitational wave emission

The super-luminous object ASASSN-15lh (SN2015L) is an extreme event with a total energy $E_{rad}\simeq 1.1\times 10^{52}$ erg in black body radiation on par with its kinetic energy $E_k$ in ejecta and a late time plateau in the UV, that defies a nuclear origin. It likely presents a new explosion mechanism for hydrogen-deprived supernovae. With no radio emission and no H-rich environment we propose to identify $E_{rad}$ with dissipation of a baryon-poor outflow in the optically thick remnant stellar envelope produced by a central engine. By negligible time scales of light crossing and radiative cooling of the envelope, SN2015L's light curve closely tracks the evolution of this engine. We here model its light curve by the evolution of black hole spin, during angular momentum loss in Alv\'en waves to matter at the Inner Most Stable Circular Orbit (ISCO). The duration is determined by $\sigma=M_T/M$ of the torus mass $M_T$ around the black hole of mass $M$: $\sigma\sim 10^{-7}$ and $\sigma\sim 10^{-2}$ for SN2015L and, respectively, a long GRB. The observed electromagnetic radiation herein represents a minor output of the rotational energy $E_{rot}$ of the black hole, while most is radiated unseen in gravitational radiation. This model explains the high-mass slow-spin binary progenitor of GWB150914, as the remnant of two CC-SNe in an intra-day binary of two massive stars. This model rigorously predicts a change in magnitude $\Delta m\simeq 1.15$ in the light curve post-peak, in agreement with the light curve of SN2015L with no fine-tuning.