Miracle-dz/UniFAR-FTUs huggingface dataset:
THE PROPERTIES OF LOW REDSHIFT INTERGALACTIC O vi ABSORBERS DETERMINED FROM HIGH S/N OBSERVATIONS OF 14 QSOs WITH THE COSMIC ORIGINS SPECTROGRAPH

We report on the observed properties of the plasma revealed through high signal-to-noise observations of 54 intervening O vi absorption systems containing 85 O vi and 133 H i components in a blind survey of 14 QSOs observed at ∼18 km s−1 resolution with the Cosmic Origins Spectrograph over a redshift path of 3.52 at z < 0.5. Simple systems with one or two H i components and one O vi component comprise 50% of the systems. For a sample of 45 well-aligned absorption components where the temperature can be estimated, we find evidence for cool photoionized gas in 31 (69%) and warm gas (6 > log T > 5) in 14 (31%) of the components. The total hydrogen content of the 14 warm components can be estimated from the temperature and the measured value of log N(H i). The very large implied values of log N(H) range from 18.38 to 20.38 with a median of 19.35. The metallicity, [O/H], in the 6 warm components with log T > 5.45 ranges from −1.93 to 0.03 with a median value of −1.0 dex. Ground-based galaxy redshift studies reveal that most of the absorbers we detect sample gas in the intergalactic medium extending 200 to 600 kpc beyond the closest associated galaxy. For the warm aligned O vi absorbers, we estimate Ωb(O vi)Warm = 0.0019 ± 0.0005 which corresponds to (4.1 ± 1.1)% of the baryons at low z. The warm plasma traced by the aligned O vi and H i absorption contains nearly as many baryons as are found in galaxies.
Journal Pre-proof Unexpected cardiotoxicity in HER2 -mutant non-small cell lung cancer patients treated with trastuzumab deruxtecan

32 Antibody-drug conjugates (ADC) targeting receptor tyrosine-protein kinase erbB-2 ( ERBB2, HER2 ) have 33 emerged as promising targeted options for HER2 -mutant non-small cell lung cancer (NSCLC). Among ADCs 34 targeting HER2, trastuzumab deruxtecan has shown the most impressive efficacy and is a potential new 35 standard of care. Drug-related interstitial lung disease remains a serious unpredictable identified risk for 36 patients treated with trastuzumab deruxtecan, requiring careful monitoring and multidisciplinary 37 management. We report the first two cases of drug-related cardiotoxicity with acute myocarditis that 38 developed after the first trastuzumab deruxtecan cycle. Routine cardiovascular risk screening is advisable, 39 with close collaboration between cardiology specialists and oncologists. 40 conclusion, to our knowledge, we report here the first two cases of trastuzumab deruxtecan-induced cardiotoxicity in the form of acute myocarditis, appearing early after the first treatment injection. These two cases reinforce the importance routine troponin monitoring from initiation of trastuzumab deruxtecan and the role of cardiac MRI to depict myocarditis in these patients, and suggest that repeat cardiac MRI may be useful in the event of an initial “negative” outcome. Further investigation into screening, understanding, and management is required to limit cardiotoxicity related to trastuzumab deruxtecan.
Advanced Human Capital Structure, Industrial Intelligence and Service Industry Structure Upgrade ——Experience from China’s Developments

ABSTRACT This study investigates the relationship between advanced human capital structure, industrial intelligence, and service industry structure based on China’s development from provincial data from 2008 to 2019. It finds that the advanced human capital structure can significantly promote the structural development of the service industry. Meanwhile, there is some heterogeneity in the impact of advanced human capital structure on the service industry. In the eastern region and high level of elemental market development in China, advanced human capital structure has a more significant contribution to the service industry structure upgrade. More importantly, industrial intelligence will play a positive moderating effect on the process of upgrading the human capital structure to the service sector structure. Further, the effect of advanced human capital structure on the service industry’s development depends on the threshold of industrial intelligence. When industrial intelligence exceeds the threshold, it can strengthen the “promotion effect” of advanced human capital structure.
Tidal deformation of a slowly rotating black hole

In the first part of this article I determine the geometry of a slowly rotating black hole deformed by generic tidal forces created by a remote distribution of matter. The metric of the deformed black hole is obtained by integrating the Einstein field equations in a vacuum region of spacetime bounded by r r min, where rmin is a minimum distance that must be much larger than the black hole’s radius. The black-hole and post-Newtonian metrics provide alternative descriptions of the same gravitational field in an overlap rmin <r<r max, and matching the metrics determine the tidal moments, which are expressed as post-Newtonian expansions carried out through one-and-a-half post-Newtonian order. Explicit expressions are obtained in the specific case in which the black hole is a member of a post-Newtonian two-body system. DOI: 10.1103/PhysRevD.91. 044004
SOLAR-CYCLE VARIATION OF SOUND SPEED NEAR THE SOLAR SURFACE

We present evidence that the sound-speed variation with solar activity has a two-layer configuration, similar to the one observed below an active region, which consists of a negative layer near the solar surface and a positive one in the layer immediately below the first one. Frequency differences between the activity minimum and maximum of solar cycle 23, obtained applying global helioseismology to the Michelson Doppler Imager on board the Solar and Heliospheric Observatory, is used to determine the sound-speed variation from below the base of the convection zone to a few Mm below the solar surface. We find that the sound speed at solar maximum is smaller than at solar minimum at the limit of our determination (5.5 Mm). The min-to-max difference decreases in absolute values until ∼7 Mm. At larger depths, the sound speed at solar maximum is larger than at solar minimum and the difference increases with depth until ∼10 Mm. At this depth, the relative difference (δc2/c2) is less than half of the value observed at the lowest depth determination. At deeper layers, it slowly decreases with depth until there is no difference between maximum and minimum activity.
AGN feedback on molecular gas reservoirs in quasars at z ~ 2.4

We present new ALMA observations aimed at mapping molecular gas reservoirs through the CO(3−2) transition in three quasars at z ≃ 2.4, LBQS 0109+0213, 2QZ J002830.4-281706, and [HB89] 0329-385. Previous [Oiii] λ 5007 observations of these quasars showed evidence for ionised outflows quenching star formation in their host galaxies. Systemic CO(3−2) emission has been detected only in one quasar, LBQS 0109+0213, where the CO(3−2) emission is spatially anti-correlated with the ionised outflow, suggesting that most of the molecular gas may have been dispersed or heated in the region swept by the outflow. In all three sources, including the one detected in CO, our constraints on the molecular gas mass indicate a significantly reduced reservoir compared to main-sequence galaxies at the same redshift, supporting a negative feedback scenario. In the quasar 2QZ J002830.4-281706, we tentatively detect an emission line blob blue-shifted by v ~ − 2000 km s -1 with respect to the galaxy systemic velocity and spatially offset by 0.2′′ (1.7 kpc) with respect to the ALMA continuum peak. Interestingly, such emission feature is coincident in both velocity and space with the ionised outflow as seen in [Oiii] λ 5007. This tentative detection must be confirmed with deeper observations but, if real, it could represent the molecular counterpart of the ionised gas outflow driven by the Active Galactic Nucleus (AGN). Finally, in all ALMA maps we detect the presence of serendipitous line emitters within a projected distance ~160 kpc from the quasars. By identifying these features with the CO(3−2) transition, we find that the serendipitous line emitters would be located within | Δ v | -1 from the quasars, hence suggesting an overdensity of galaxies in two out of three quasars.
Enhancing student learning of two-level quantum systems with interactive simulations

The QuVis Quantum Mechanics Visualization project aims to address challenges of quantum mechanics instruction through the development of interactive simulations for the learning and teaching of quantum mechanics. In this article, we describe the evaluation of simulations focusing on two-level systems developed as part of the Institute of Physics Quantum Physics resources. Simulations are research-based and have been iteratively refined using student feedback in individual observation sessions and in-class trials. We give evidence that these simulations are helping students learn quantum mechanics concepts at both the introductory and advanced undergraduate level, and that students perceive simulations to be beneficial to their learning.
On the role of corotation radius in the low T/W dynamical instability of differentially rotating stars

We investigate the nature of so-called low $T/W$ dynamical instability in a differentially rotating star by focusing on the role played by the corotation radius of the unstable oscillation modes. An one dimensional model of linear perturbation, which neglects dependence of variables on the coordinate along the rotational axis of the star, is solved to obtain stable and unstable eigenmodes. A linear eigenmode having a corotation radius, at which azimuthal pattern speed of the mode coincides with the stellar angular velocity, is categorized to either a complex (growing or damping) mode or a purely real mode belonging to a continuous spectrum of frequency. We compute canonical angular momentum and its flux to study eigenmodes with corotation radius. In a dynamically unstable mode, sound wave transports its angular momentum in such a way that the absolute value of the angular momentum is increased on both sides of the corotation radius. We further evaluate growth of amplitude of reflected sound wave incident to a corotation point and find that the over-reflection of the wave and the trapping of it between the corotation radius and the surface of the star may qualitatively explain dependences of eigenfrequencies on the stellar differential rotation. The results suggest that the low $T/W$ instability may be caused by over-reflection of sound waves trapped mainly between the surface of the star and a corotation radius.
On the reliability of protostellar disc mass measurements and the existence of fragmenting discs

We couple non-magnetic, hydrodynamical simulations of collapsing protostellar cores with radiative transfer evolutionary models to generate synthetic observations. We then use these synthetic observations to investigate the extent to which a simple method for measuring protostellar disc masses used in the literature recovers the intrinsic masses of the discs formed in the simulations. We evaluate the effects of contamination from the surrounding core, partially resolving out the disc, optical depth, fixed assumed dust temperatures, inclination, and the dust opacity law. We show that the combination of these effects can lead to disc mass underestimates by up to factors of 2–3 at millimeter wavelengths and up to an order of magnitude or larger at submillimeter wavelengths. The optically thin portions of protostellar discs are generally cooler in the Class I stage than the Class 0 stage since Class I discs are typically larger and more optically thick, and thus more shielded. The observed disc mass distribution closely resembles the intrinsic distribution if this effect is taken into account, especially at millimeter wavelengths where optical depth effects are minimized. Approximately 50%–70% of protostellar discs observed to date with this method are consistent with the masses of the gravitationally unstable discs formed in the simulations, suggesting that at least some protostellar discs are likely sufficiently massive to f ragment. We emphasize key future work needed to confirm these results, including assembling larger, less biased samples, and using molecular line observations to distinguish between rotationally supported, Keplerian discs and magnetically supported pseudodiscs.
Multi-Connectivity for URLLC and Coexistence With eMBB in Time-Varying and Frequency-Selective Fading Channels

Multi-connectivity enables a 5G cellular system to meet the challenging reliability requirements of downlink ultra-reliable low-latency communication (URLLC) data traffic. In it, multiple base stations (BSs) transmit to the URLLC user by pre-empting time-frequency resources assigned to enhanced mobile broadband (eMBB) users. We derive insightful expressions for achievability, which is the probability that the URLLC user’s block error rate (BLER) requirement is met by multi-connectivity. We do so for both joint transmission (JT) and orthogonal transmission (OT) modes of URLLC for the general case in which the transmissions occur over frequency-selective channels. We then propose a low-complexity algorithm to jointly select the set of cooperating BSs and their modulation and coding schemes (MCSs) to minimize the eMBB throughput loss. For time-varying channels with feedback delays, we present an alternate stochastic reliability requirement for URLLC traffic. The MCS selected on the basis of this requirement has a markedly higher probability of meeting the BLER target over the grid of URLLC user locations. Our results highlight the different trade-offs between URLLC achievability, eMBB throughput loss, and channel state information feedback overhead of OT and JT. They bring out the significant impact of feedback delays even at moderate Doppler spreads.
Dynamical analysis of nearby clusters - Automated astrometry from the ground: precision proper motions over a wide field

The kinematic properties of the different classes of objects in a given association hold important clues about its member's history, and offer a unique opportunity to test the predictions of the various models of stellar formation and evolution. DANCe (standing for Dynamical Analysis of Nearby ClustErs) is a survey program aimed at deriving a comprehensive and homogeneous census of the stellar and substellar content of a number of nearby (<1kpc) young (<500Myr) associations. Whenever possible, members will be identified based on their kinematics properties, ensuring little contamination from background and foreground sources. Otherwise, the dynamics of previously confirmed members will be studied using the proper motion measurements. We present here the method used to derive precise proper motion measurements, using the Pleiades cluster as a test bench. Combining deep wide field multi-epoch panchromatic images obtained at various obervatories over up to 14 years, we derive accurate proper motions for the sources present in the field of the survey. The datasets cover ~80 square degrees, centered around the Seven Sisters. Using new tools, we have computed a catalog of 6116907 unique sources, including proper motion measurements for 3577478 of them. The catalogue covers the magnitude range between i=12~24mag, achieving a proper motion accuracy <1mas/yr for sources as faint as i=22.5mag. We estimate that our final accuracy reaches 0.3mas/yr in the best cases, depending on magnitude, observing history, and the presence of reference extragalactic sources for the anchoring onto the ICRS.
General intrinsic theory of general large $N_{c}$ QCD, SU(3) QCD, SU(2) hadron-dynamics and U(1) QED gauge field theories in general field theory and progress towards solving the nucleon spin crisis

This paper gives general intrinsic theory of general large $N_{c}$ QCD, SU(3) QCD, SU(2) hadron-dynamics and U(1) QED gauge field theories in general field theory and progress towards solving the nucleon spin crisis, i.e., presents general large $N_{c}$ QCD's inner structures, gauge invariant angular momenta and new corresponding Coulomb theorem in quark-gluon field interaction systems based on general field theory, and naturally deduces the gauge invariant spin and orbital angular momentum operators of quark and gauge fields with $SU(N_{c})$ gauge symmetry by Noether theorem in general field theory. In the general large $N_{c}$ QCD, we discover not only the general covariant transverse and parallel conditions ( namely, non-Abelian divergence and curl ), but also that this general system has good intrinsic symmetry characteristics. Specially, this paper's generally decomposing gauge potential theory presents a new technique, it should play a votal role in future physics research. Therefore, this paper breakthroughs the some huge difficulties in the nucleon spin crisis and opens a door of researching on lots of strong interacting systems with different symmetric properties, which is popularly interesting, and keeps both the gauge invariance and their angular momentum commutation relations so that their theories are consistent. Especially, the achieved results here can be utilized to calculate the general QCD strong interactions and to give the precise predictions that can be exactly measured by current particle physics experiments due to their gauge invariant properties etc.
The Properties of Parsec-scale Blazar Jets

I show that, by assuming a standard Blandford–Königl jet, it is possible to determine the bulk Lorentz factor and angle to the line of sight of self-similar parsec-scale blazar jets by using five measured quantities: redshift, core radio flux, extended radio flux, the magnitude of the core shift between two frequencies, and apparent jet opening angle. From the bulk Lorentz factor and angle computed with this method, one can compute other jet properties such as the Doppler factor, magnetic field strength, and intrinsic jet opening angle. I use data taken from the literature and marginalize over nuisance parameters associated with the electron distribution and equipartition to compute these quantities, although the errors are large. Results are generally consistent with constraints from other methods. Primary sources of uncertainty are the errors on the core shift measurements and the uncertainty in the electron spectral index.
Extreme TeV blazars and the intergalactic magnetic field

We study the four BL Lac objects (RGBJ0152+017, IES 0229+200, 1ES 0347―121 and PKS 0548-322) detected in the TeV band but not present in the first Fermi-LAT (1FGL) catalogue of the Fermi/Large Area Telescope (LAT). We analyse the 24 months of LAT data deriving γ-ray fluxes or upper limits that we use to assemble their spectral energy distributions (SED). We model the SEDs with a standard one-zone leptonic model, also including the contribution of the reprocessed radiation in the multi-GeV band, emitted by the pairs produced through the conversion of the primary TeV emission by interaction with the cosmic optical-infrared background. For simplicity, in the calculation of this component we adopt an analytical approach including some simplifying assumptions, in particular (i) the blazar high-energy emission is considered on average stable over times of the order of 10 7 yr and (ii) the observer is exactly on-axis. We compare the physical parameters derived by the emission model with those of other high-energy emitting BL Lacs, confirming that TeV BL Lacs with a rather small GeV flux are characterized by extremely low values of the magnetic field and large values of the electron energies. The comparison between the flux in the GeV band and that expected from the reprocessed TeV emission allows us to confirm and strengthen the lower limit of B ≳ 10 ―15 G for the intergalactic magnetic field using a theoretically motivated spectrum for the primary high-energy photons.
Integrated Markov Chain Monte Carlo (MCMC) analysis of primordial non-Gaussianity (fNL) in the recent CMB data

We have made a Markov Chain Monte Carlo (MCMC) analysis of primordial non-Gaussianity (fNL) using the WMAP bispectrum and power spectrum. In our analysis, we have simultaneously constrained fNL and cosmological parameters so that the uncertainties of cosmological parameters can properly propagate into the fNL estimation. Investigating the parameter likelihoods deduced from MCMC samples, we find slight deviation from Gaussian shape, which makes a Fisher matrix estimation less accurate. Therefore, we have estimated the confidence interval of fNL by exploring the parameter likelihood without using the Fisher matrix. We find that the best-fit values of our analysis make a good agreement with other results, but the confidence interval is slightly different.
A combined photometric and kinematic recipe for evaluating the nature of bulges using the CALIFA sample

Understanding the nature of bulges in disc galaxies can provide important insights into the formation and evolution of galaxies. For instance, the presence of a classical bulge suggests a relatively violent history, in contrast, the presence of simply an inner disc (also referred to as a "pseudobulge") indicates the occurrence of secular evolution processes in the main disc. However, we still lack criteria to effectively categorise bulges, limiting our ability to study their impact on the evolution of the host galaxies. Here we present a recipe to separate inner discs from classical bulges by combining four different parameters from photometric and kinematic analyses: The bulge S\'ersic index $n_\mathrm{b}$, the concentration index $C_{20,50}$, the Kormendy (1977) relation and the inner slope of the radial velocity dispersion profile $\nabla\sigma$. With that recipe we provide a detailed bulge classification for a sample of 45 galaxies from the integral-field spectroscopic survey CALIFA. To aid in categorising bulges within these galaxies, we perform 2D image decomposition to determine bulge S\'ersic index, bulge-to-total light ratio, surface brightness and effective radius of the bulge and use growth curve analysis to derive a new concentration index, $C_{20,50}$. We further extract the stellar kinematics from CALIFA data cubes and analyse the radial velocity dispersion profile. The results of the different approaches are in good agreement and allow a safe classification for approximately $95\%$ of the galaxies. In particular, we show that our new "inner" concentration index performs considerably better than the traditionally used $C_{50,90}$ when yielding the nature of bulges. We also found that a combined use of this index and the Kormendy (1977) relation gives a very robust indication of the physical nature of the bulge.