Miracle-dz/UniFAR-FTUs huggingface dataset:
Weak Gravitational Lensing by Galaxies

We report a detection of weak, tangential distortion of the images of cosmologically distant, faint galaxies due to gravitational lensing by foreground galaxies. A mean image polarization of ({ital p})=0.011{plus_minus}0.006 (95{percent} confidence bounds) is obtained for 3202 pairs of source (23{lt}{ital r}{sub {ital s}}{le}24) and lens (20{le}{ital r}{sub {ital d}}{le}23) galaxies with projected separations of 5{double_prime}{le}{theta}{le}34{double_prime}. Averaged over annuli of inner radius 5{double_prime} and outer radius {theta}{sub max}, the signal is string for lens-source separations of {theta}{sub max}{approx_lt}90{double_prime} consistent with quasi-isothermal galaxy halos extending to large radii ({approx_gt}100{ital h}{sup {minus}1} kpc). The observed polarization is also consistent with the signal expected on the basis of simulations incorporating measured properties of local galaxies and modest extrapolations of the observed redshift distribution of faint galaxies (to which the results are somewhat sensitive). From the simulations we obtain formal best-fit model parameters for the dark halos of the lens galaxies that consist of a characteristic circular velocity of {ital V}{asterisk}{approximately}220{plus_minus}80 kms{sup {minus}1} and characteristic radial extent of {ital s}{asterisk}{approx_gt}100{ital h}{sup {minus}1} kpc. The predicted polarization based on the model is relatively insensitive to the characteristic radial extent of the halos, {ital s}{asterisk}, and very small halos ({ital s}{asterisk}{approximately}10{ital h}{sup {minus}1} kpc) are excludedmore » only at the 2 {sigma} level. The formal best-fit halo parameters imply typical masses for the lens galaxies within a radius of 100{ital h}{sup -1} kpc on the order of 1.0{sup +1.2}{sub {minus}0.5}{times}10{sup 12} {ital h}{sup {minus}1}{ital M}{sub {circle_dot}} (90% confidence bounds), in agreement with recent dynamical estimates of the masses of local spiral galaxies. « less
The evolution of 3CR radio galaxies from z1

We present the results of a comprehensive re-analysis of the images of a virtually complete sample of 28 powerful 3CR radio galaxies with redshifts 0.6<z<1.8 from the Hubble Space Telescope (HST) archive. Using a two-dimensional modelling technique we have derived scalelengths and absolute magnitudes for a total of 16 3CR galaxies with a median redshift of z=0.8. Our results confirm the basic conclusions of Best, Longair & Rottgering in that we also find z=1 3CR galaxies to be massive, well-evolved ellipticals, the infrared emission of which is dominated by starlight. However, we in fact find that the scalelength distribution of 3CR galaxies at z≃1 is completely indistinguishable from that derived for their low-redshift counterparts from our own recently completed HST study of active galactic nuclei hosts at z≃0.2. There is thus no evidence that 3CR radio galaxies at z≃1 are dynamically different from 3CR galaxies at low redshift. Moreover, for a 10-object subsample we have determined the galaxy parameters with sufficient accuracy to demonstrate, for the first time, that the z≃1 3CR galaxies follow a Kormendy relation that is indistinguishable from that displayed by low-redshift ellipticals if one allows for purely passive evolution. The implied rather modest level of passive evolution since z≃1 is consistent with that predicted from spectrophotometric models provided one assumes a high formation redshift (z≥4) within a low-density universe. We conclude that there is no convincing evidence for significant dynamical evolution among 3CR galaxies in the redshift interval 0<z<1, and that simple passive evolution remains an acceptable interpretation of the K–z relation for powerful radio galaxies.
First principles study of rare-earth oxides

The self-interaction-corrected local-spin-density approximation is used to describe the electronic structure of dioxides, REO2, and sesquioxides, RE2O3, for the rare earths, RE=Ce, Pr, Nd, Pm, Sm, Eu, Gd, Tb, Dy and Ho. The valencies of the rare earth ions are determined from total energy minimization. We find Ce, Pr, Tb in their dioxides to have the tetravalent configuration, while for all the sesquioxides the trivalent groundstate configuration is found to be the most favourable. The calculated lattice constants for these valency configurations are in good agreement with experiment. Total energy considerations are exploited to show the link between oxidation and f-electron delocalization, and explain why, among the dioxides, only the CeO2, PrO2, and TbO2 exist in nature. Tetravalent NdO2 is predicted to exist as a metastable phase - unstable towards the formation of hexagonal Nd2O3.
Simultaneous long-term monitoring of LS I +61°303 by OVRO and Fermi-LAT

Previous long-term monitorings of the gamma-ray-loud X-ray binary LS I +61{\deg}303 have revealed the presence of a long-term modulation of ~4.5 years. After nine years of simultaneous monitoring of LS I +61{\deg}303 by the Owens Valley Radio Observatory and the Fermi-LAT, two cycles of the long-term period are now available. Here we perform timing-analysis on the radio and the gamma-ray light curves. We confirm the presence of previously detected periodicities at both radio and GeV gamma-ray wavelengths. Moreover, we discover an offset of the long-term modulation between radio and gamma-ray data which could imply different locations of the radio (15 GHz) and GeV emission along the precessing jet.
Chiral Lattice Gauge Theories Via Mirror-Fermion Decoupling: A Mission (im)Possible?

This is a review of the status and outstanding issues in attempts to construct chiral lattice gauge theories by decoupling the mirror fermions from a vectorlike theory. In the first half, we explain why studying nonperturbative chiral gauge dynamics may be of interest, enumerate the problems that a lattice formulation of chiral gauge theories must overcome, and briefly review our current knowledge. We then discuss the motivation and idea of mirror–fermion decoupling and illustrate the desired features of the decoupling dynamics by a simple solvable toy model. The role of exact chiral symmetries and matching of 't Hooft anomalies on the lattice is also explained. The second, more technical, half of the paper is devoted to a discussion of the known and unknown features of mirror-decoupling dynamics formulated with Ginsparg–Wilson fermions. We end by pointing out possible directions for future studies.
Galaxy stellar mass functions of different morphological types in clusters, and their evolution between z= 0.8 and 0

We present the galaxy stellar mass function and its evolution in clusters from z ∼ 0.8 to the current epoch, based on the WIde-field Nearby Galaxy-cluster Survey (WINGS) (0.04 ≤ z ≤ 0.07), and the ESO Distant Cluster Survey (EDisCS) (0.4 ≤ z ≤ 0.8). We investi- gate the total mass function and find that it evolves noticeably with redshift. The shape at M∗ > 10 11 Mdoes not evolve, but below M∗ ∼ 10 10.8 Mthe mass function at high red- shift is flat, while in the local Universe it flattens out at lower masses. The population of M∗ = 10 10.2 -10 10.8 Mgalaxies must have grown significantly between z = 0.8 and 0. We analyse the mass functions of different morphological types (ellipticals, S0s and late types), and also find that each of them evolves with redshift. All types have proportionally more massive galaxies at high than at low-z, and the strongest evolution occurs among S0 galaxies. Examining the morphology-mass relation (the way the proportion of galaxies of different morphological types changes with galaxy mass), we find it strongly depends on redshift. At both redshifts, ∼40 per cent of the stellar mass is in elliptical galaxies. Another ∼43 per cent of the mass is in S0 galaxies in local clusters, while it is in late types in distant clusters. To explain the observed trends, we discuss the importance of those mechanisms that could shape the mass function. We conclude that mass growth due to star formation plays a crucial role in driving the evolution. It has to be accompanied by infall of galaxies on to clusters, and the mass distribution of infalling galaxies might be different from that of cluster galaxies. However, comparing with high-z field samples, we do not find conclusive evidence for such an environmental mass segregation. Our results suggest that star formation and infall change directly the mass function of late-type galaxies in clusters and, indirectly, that of early-type galaxies through subsequent morphological transformations.
‘Management of a spoiled identity’: systematic review of interventions to address self-stigma among people living with and affected by HIV

Background Self-stigma, also known as internalised stigma, is a global public health threat because it keeps people from accessing HIV and other health services. By hampering HIV testing, treatment and prevention, self-stigma can compromise the sustainability of health interventions and have serious epidemiological consequences. This review synthesised existing evidence of interventions aiming to reduce self-stigma experienced by people living with HIV and key populations affected by HIV in low-income and middle-income countries. Methods Studies were identified through bibliographic databases, grey literature sites, study registries, back referencing and contacts with researchers, and synthesised following Cochrane guidelines. Results Of 5880 potentially relevant titles, 20 studies were included in the review. Represented in these studies were 9536 people (65% women) from Ethiopia, India, Kenya, Lesotho, Malawi, Nepal, South Africa, Swaziland, Tanzania, Thailand, Uganda and Vietnam. Seventeen of the studies recruited people living with HIV (of which five focused specifically on pregnant women). The remaining three studies focused on young men who have sex with men, female sex workers and men who inject drugs. Studies were clustered into four categories based on the socioecological level of risk or resilience that they targeted: (1) individual level only, (2) individual and relational levels, (3) individual and structural levels and (4) structural level only. Thirteen studies targeting structural risks (with or without individual components) consistently produced significant reductions in self-stigma. The remaining seven studies that did not include a component to address structural risks produced mixed effects. Conclusion Structural interventions such as scale-up of antiretroviral treatment, prevention of medication stockouts, social empowerment and economic strengthening may help substantially reduce self-stigma among individuals. More research is urgently needed to understand how to reduce self-stigma among young people and key populations, as well as how to tackle intersectional self-stigma.
THE STAR FORMATION RATE AND GAS SURFACE DENSITY RELATION IN THE MILKY WAY: IMPLICATIONS FOR EXTRAGALACTIC STUDIES

We investigate the relation between star formation rate (SFR) and gas surface densities in Galactic star-forming regions using a sample of young stellar objects (YSOs) and massive dense clumps. Our YSO sample consists of objects located in 20 large molecular clouds from the Spitzer cores to disks (c2d) and Gould's Belt (GB) surveys. These data allow us to probe the regime of low-mass star formation, essentially invisible to tracers of high-mass star formation used to establish extragalactic SFR–gas relations. We estimate the gas surface density (Σgas) from extinction (AV) maps and YSO SFR surface densities (ΣSFR) from the number of YSOs, assuming a mean mass and lifetime. We also divide the clouds into evenly spaced contour levels of AV, counting only Class I and Flat spectral energy distribution YSOs, which have not yet migrated from their birthplace. For a sample of massive star-forming clumps, we derive SFRs from the total infrared luminosity and use HCN gas maps to estimate gas surface densities. We find that c2d and GB clouds lie above the extragalactic SFR–gas relations (e.g., Kennicutt–Schmidt law) by factors of up to 17. Cloud regions with high Σgas lie above extragalactic relations up to a factor of 54 and overlap with high-mass star-forming regions. We use 12CO and 13CO gas maps of the Perseus and Ophiuchus clouds from the COMPLETE survey to estimate gas surface densities and compare to measurements from AV maps. We find that 13CO, with the standard conversions to total gas, underestimates the AV-based mass by factors of ∼4–5. 12CO may underestimate the total gas mass at Σgas ≳ 200 M☉ pc−2 by ≳30%; however, this small difference in mass estimates does not explain the large discrepancy between Galactic and extragalactic relations. We find evidence for a threshold of star formation (Σth) at 129 ± 14 M☉ pc−2. At Σgas>Σth, the Galactic SFR–gas relation is linear. A possible reason for the difference between Galactic and extragalactic relations is that much of Σgas is below Σth in extragalactic studies, which detect all the CO-emitting gas. If the Kennicutt–Schmidt relation (ΣSFR ∝ Σ1.4gas) and a linear relation between dense gas and star formation are assumed, the fraction of dense star-forming gas (fdense) increases as ∼Σ0. 4gas. When Σgas reaches ∼300 Σth, the fraction of dense gas is ∼1, creating a maximal starburst.
Rainbow-Like Black-Hole Metric from Loop 
Quantum Gravity

Hypersurface deformation algebra consists of a fruitful approach to derive deformedsolutions of general relativity based on symmetry considerations with quantum-gravity effects,of which the linearization has been recently demonstrated to be connected to the DSR programby k-Poincaré symmetry. Based on this approach, we analyzed the solution derived for theinterior of a black hole and we found similarities with the so-called rainbow metrics, like amomentum-dependence of the metric functions. Moreover, we derived an effective, time-dependentPlanck length and compared different regularization schemes.
Validation of content and structure of the Return-to-work assessment for post-stroke survivors

Background Validation of an instrument consist of three main types: content, criterion and construct. Content validity needs to be determined in order for an instrument to be acceptable for use, validity establishes the fact that an instrument measures exactly what it proposes to measure. The Return-to-work assessment scale (RAS) was developed to measure three aspects of return to work: (Personal factors and/or issues, work issues and contextual factors) in 2021. Objective To report on the processes followed in establishing the face and content validity of the RAS. Method Twenty participants took part in our study, they were selected purposively and conveniently from a pool of professionals and post stroke survivors. The Delphi survey technique was used to arrive at consensus and professional opinion on the items included in the RAS. Consensus was sought on the items, domains and subdomains included in the RAS that was used to assess return-to-work after a stroke. Our study was concluded after the third round. Result One item was remove out of the original 86, three (3) domains made up of eleven (11) subdomains were retained. The RAS had consensus of 100% after three rounds of scrutiny for all items. Conclusion The RAS was found to be valid, thereby establishing its face and content validity. Clinical implication The RAS is valid and was recommended for psychometric testing which was the next stage after face and content validity.
PS16dtm: A Tidal Disruption Event in a Narrow-line Seyfert 1 Galaxy

We present observations of PS16dtm (also known as SN 2016ezh), a luminous transient that occurred at the nucleus of a narrow-line Seyfert 1 galaxy hosting a 106 M⊙ black hole. The light curve shows that PS16dtm exhibited a plateau phase for ∼100 days, during which it showed no color evolution, maintained a blackbody temperature of K, and radiated at approximately the Eddington luminosity of the supermassive black hole (SMBH). The spectra exhibit multicomponent hydrogen emission lines and strong Fe ii emission, show little time evolution, and closely resemble the spectra of NLS1s while being distinct from those of Type IIn supernovae (SNe IIn). Moreover, PS16dtm is undetected in the X-rays to a limit an order of magnitude below an archival X-ray detection of its host galaxy. These observations strongly link PS16dtm to activity associated with the SMBH and are difficult to reconcile with an SN origin or known forms of active galactic nucleus (AGN) variability. Therefore, we argue that PS16dtm is a tidal disruption event (TDE) in which the accretion of the stellar debris powers the rise in the continuum and excitation of the preexisting broad-line region, while obscuring the X-ray-emitting region of the preexisting AGN disk. We predict that PS16dtm will remain bright for years and that the X-ray emission will reappear on a similar timescale as the accretion rate declines. Placing PS16dtm in the context of other TDEs, we find that TDEs in AGN galaxies are more efficient and reach Eddington luminosities, likely due to interaction of the stellar debris with the preexisting accretion disk.
Comparison of pulmonary computed tomography scan findings and clinical symptoms of COVID-19 in three outbreak peaks in Isfahan, Iran

Background: The aim of the present study was to investigate and compare the relationship between the anatomical distribution of pulmonary lesions in computed tomography scan of patients with COVID-19. Materials and Methods: This is a cross-sectional study that was performed in 2020–2021 in Isfahan on 300 patients infected with COVID-19 pneumonia. We collected data on the age, gender, and comorbidities of patients. In addition, we gathered data on the clinical manifestations of the patients from their medical records. Results: We noted a significant decline in symptoms such as fever and sputum production in the second and third peak in comparison to the first peak (P < 0.05). Moreover, cough and muscular pain were higher in the second and third peaks compared to the first peak (P < 0.05). Cough was the most common clinical manifestation related to the peripheral distribution of the involvements, bilateral lung disease, and right lower lobe (RLL) involvements in the first peak. In the second COVID-19 peak, fever and cough were the most common clinical findings, respectively, that were mostly associated with peripheral distribution and left lower lobe involvement. Conclusion: Cough was the most common clinical manifestation related to the peripheral distribution of the involvements, bilateral lung disease, and RLL involvements in the first peak. In the second COVID-19 peak, fever and cough were the most common clinical findings.
Estimation of the mass of the black hole candidate MAXI J1659-152 using TCAF and POS models

The Galactic transient black hole candidate (BHC) MAXI~J1659-152 exhibited temporal and spectral evolution during its very first X-ray outburst (2010) after its discovery on 25th Sept. 2010. Our recent studies of a few transient BHCs including MAXI~J1659-152 using Chakrabarti-Titarchuk two-component advective flow (TCAF) solution as an additive table local model in XSPEC revealed details of accretion flow dynamics around the black hole (BH). The TCAF model fitted normalization (N) comes out to be almost constant throughout the entire outburst consisting of several spectral states. We introduce two independent methods to determine the mass ($M_{BH}$) of the BHC, namely, {\it $i)$ keeping TCAF fitted normalization parameter in a narrow range}, and {\it $ii)$ studying evolution of the Quasi-Periodic Oscillation frequency ($\nu_{QPO}$) with time, fitted with the propagating oscillatory shock (POS) model}. The predicted mass ranges of the source with these two methods are $4.7-7.8~M_\odot$, and $5.1-7.4~M_\odot$ respectively. Combining results of these two methods, we obtain a most probable mass range of the source to be $4.7-7.8~M_\odot$ or $6^{+1.8}_{-1.3}~M_\odot$.
The age of elliptical galaxies and bulges in a merger model

A support structure for various types of receptacles or the like comprising a plurality of securing hooks having a substantially "S"-shaped configuration for removably attaching to a first hanging structure, the lower portion of the hooks being adapted to receive eye members of a pair of supporting cords. Each of the cords hangs downwardly therefrom and is threaded through apertures disposed within a base plate wherein the base plate is centrally positioned directly below the first hanging structure, whereby a receptacle is disposed between the supporting cords resting on the base plate to provide a means by which any fluid overflow deposited in the first hanging structure is caught and retained in the supported receptacle.
Systematic Survey of Extended Lyα Sources over z ~ 3-5

Spatially extended Lyα sources that are faint and compact in continuum are candidates for extremely young (≲107 yr) galaxies at high redshifts. We carried out a systematic survey for extended Lyα sources, using deep intermediate-band imaging data taken with the Suprime-Cam on the Subaru Telescope. Our survey covers a field of view of 33′ × 25′ and a redshift range of 3.24 ≲ z ≲ 4.95, down to a Lyα flux of ~1 × 10-17 ergs cm-2 s-1. We identified 41 extended Lyα sources. The redshift distribution of these sources shows that this kind of object is common in the early universe over the surveyed redshift range. The identified objects have typical sizes of ~10-15 kpc and luminosities of ~1042 ergs s-1. Follow-up spectroscopy made for 7 of the 41 objects showed that our sample suffers from little contamination. All 7 objects have large equivalent widths of Lyα emission line, all but one exceeding 240 Å in the rest frame. The large equivalent widths suggest that their extended Lyα emissions are unlikely to be due to normal starbursts, but possibly originate from very young galaxies. All 41 objects in our sample have much smaller Lyα luminosities than the two Lyα blobs (LABs) found at a z ≃ 3.1 protocluster, in spite of our much larger survey volume. This suggests that large and luminous extended Lyα objects like the two LABs are very rare and are clustered in overdense regions.
STAR CLUSTERS, GALAXIES, AND THE FUNDAMENTAL MANIFOLD

We explore whether global observed properties, specifically half-light radii, mean surface brightness, and integrated stellar kinematics, suffice to unambiguously differentiate galaxies from star clusters, which presumably formed differently and lack dark matter halos. We find that star clusters lie on the galaxy scaling relationship referred to as the fundamental manifold (FM), on the extension of a sequence of compact galaxies, and so conclude that there is no simple way to differentiate star clusters from ultracompact galaxies. By extending the validity of the FM over a larger range of parameter space and a wider set of objects, we demonstrate that the physics that constrains the resulting baryon and dark matter distributions in stellar systems is more general than previously appreciated. The generality of the FM implies (1) that the stellar spatial distribution and kinematics of one type of stellar system do not arise solely from a process particular to that set of systems, such as violent relaxation for elliptical galaxies, but are instead the result of an interplay of all processes responsible for the generic settling of baryons in gravitational potential wells, (2) that the physics of how baryons settle is independent of whether the system is embedded within a dark matter halo, and (3) that peculiar initial conditions at formation or stochastic events during evolution do not ultimately disturb the overall regularity of baryonic settling. We also utilize the relatively simple nature of star clusters to relate deviations from the FM to the age of the stellar population and find that stellar population models systematically and significantly overpredict the mass-to-light ratios of old, metal-rich clusters. We present an empirical calibration of stellar population mass-to-light ratios with age and color. Finally, we use the FM to estimate velocity dispersions for the low surface brightness, outer halo clusters that lack such measurements.