Miracle-dz/UniFAR-FTUs huggingface dataset:
Mass profiles and galaxy orbits in nearby galaxy clusters from the analysis of the projected phase space

We analyse kinematic data of 41 nearby (z < 0.1) relaxed galaxy clusters in terms of the projected phase-space density using a phenomenological, fully anisotropic model of the distribution function. We apply the Markov Chain Monte Carlo approach to place constraints on total mass distribution approximated by the universal Navarro, Frenk and White (NFW) profile and the profile of the anisotropy of galaxy orbits. We find the normalization of the mean mass– concentration relation is c = 6.9 +0.6 −0.7 at the virial mass Mv = 5 × 10 14 M� . By comparison with the calibration from cosmological N-body simulations it is demonstrated that this result is fully consistent with σ 8 from 1-yr Wilkinson Microwave Anisotropy Probe (WMAP1) data release and agrees at ∼1σ level with that from WMAP5. Assuming a one-to-one correspondence between σ 8 and the normalization of the mass–concentration relation in the framework of the concordance model we estimate the normalization of the linear power spectrum to be σ8 = 0.91 +0.07 −0.08. Our constraints on the parameters of the mass profile are compared with estimates from X-ray observations and other methods based on galaxy kinematics. We also study correlations between the virial mass and different mass proxies including the velocity dispersion, the X-ray temperature and the X-ray luminosity. We demonstrate that the mass scaling relations with the velocity dispersion and the X-ray temperature are fully consistent with the predictions of the virial theorem. We show that galaxy orbits are isotropic at the cluster centres (with the mean ratio of the radial-to-tangential velocity dispersions σr /σθ = 0.97 ± 0.04) and radially anisotropic at the virial sphere (with the mean ratio σr /σθ = 1.75 +0.23 −0.19 ). Although the value of the central anisotropy appears to be universal, the anisotropy at the virial radius differs between clusters within the range 1 (σr /σθ ) 2. Utilizing the Bautz–Morgan morphological classification and information on the prominence of a cool core we select two subsamples of galaxy clusters corresponding to less and more advanced evolutionary states. It is demonstrated that less evolved clusters have shallower mass profiles and their galaxy orbits are more radially biased at the virial sphere. This property is consistent with the expected evolution of the mass profiles as well as with the observed orbital segregation of late- and early-type galaxies.
Approaches for management of Meloidogyne incognita in pulses

Meloidogyne incognita can be effectively managed through biological control agents. The present study on the bio-intensive management of M. incognita on blackgram with bio-agents, viz. Bacillus marisflavi, Bacillus altitudinis, Bacillus subtilis, Trichoderma viride, Verticillium lecanii and Pseudomonas fluorescens as soil application was carried out under net house conditions at the Department of Nematology, Assam Agricultural University, Jorhat, Assam under controlled conditions during the winter (rabi) season of 2020–21. Treatment with soil application of Pseudomonas fluorescens @1 × 108 cfu/ml enriched in vermicompost @20 g/m2 was found to be the most effective in enhancing plant growth parameters, number of nodules per root system and reducing the number of galls per root system, egg masses per root system and final root-knot nematode population in the soil. Given the importance of pulses in maintaining national food and nutritional security, as well as the importance of root-knot nematode as a limiting factor in pulse production, biological agents for nematode control are a viable alternative to pesticides. Biocontrol agents studied help in attaining favourable plant growth and health, therefore considered a more promising management practice against root-knot nematode.
A GLOBAL MODEL OF THE LIGHT CURVES AND EXPANSION VELOCITIES OF TYPE II-PLATEAU SUPERNOVAE

We present a new self-consistent and versatile method that derives photospheric radius and temperature variations of Type II-Plateau supernovae based on their expansion velocities and photometric measurements. We apply the method to a sample of 26 well-observed, nearby supernovae with published light curves and velocities. We simultaneously fit ∼230 velocity and ∼6800 mag measurements distributed over 21 photometric passbands spanning wavelengths from 0.19 to 2.2 μm. The light-curve differences among the Type II-Plateau supernovae are well modeled by assuming different rates of photospheric radius expansion, which we explain as different density profiles of the ejecta, and we argue that steeper density profiles result in flatter plateaus, if everything else remains unchanged. The steep luminosity decline of Type II-Linear supernovae is due to fast evolution of the photospheric temperature, which we verify with a successful fit of SN 1980K. Eliminating the need for theoretical supernova atmosphere models, we obtain self-consistent relative distances, reddenings, and nickel masses fully accounting for all internal model uncertainties and covariances. We use our global fit to estimate the time evolution of any missing band tailored specifically for each supernova, and we construct spectral energy distributions and bolometric light curves. We produce bolometric corrections for all filter combinations in our sample. We compare our model to the theoretical dilution factors and find good agreement for the B and V filters. Our results differ from the theory when the I, J, H, or K bands are included. We investigate the reddening law toward our supernovae and find reasonable agreement with standard reddening law in UBVRI bands. Results for other bands are inconclusive. We make our fitting code publicly available.
New calibrations for abundance determinations in H ii regions

Simple relations for deriving the oxygen abundance in HII regions with intensities of the three strong emission lines R_2, R_3, and N_2 (R calibration) or S_2, R_3, and N_2 (S calibration) in their spectra are suggested. A sample of 313 reference HII regions of the counterpart method is used as calibrating data points. Relations for the determination of nitrogen abundances, the R calibration, are also constructed. We find that the oxygen and nitrogen abundances in high-metallicity HII regions can be estimated using the intensities of the two strong lines R_2 and N_2 (or S_2 and N_2 for oxygen) only. The corresponding two-dimensional relations are provided. There are considerable advantages of the suggested calibration relations as compared to the existing ones. First, the oxygen and nitrogen abundances estimated through the suggested calibrations agree with the Te-based abundances within ~0.1 dex over the whole metallicity range, i.e., the relative accuracy of the calibration-based abundances is 0.1 dex. Although we constructed distinct relations for high- and low-metallicity objects, the separation between these two can be simply obtained from the intensity of the N_2 line. Moreover, the applicability ranges of the high- and low-metallicity relations overlap for adjacent metallicities, i.e., the transition zone disappears. Second, the oxygen abundances produced by the two suggested calibrations are in remarkable agreement with each other. In fact, the R-based and S-based oxygen abundances agree within ~0.05 dex in the majority of cases for more than three thousand HII region spectra.
POLARIZED RADIO SOURCES: A STUDY OF LUMINOSITY, REDSHIFT, AND INFRARED COLORS

The Dominion Radio Astrophysical Observatory Deep Field polarization study has been matched with the Spitzer Wide-Area Infrared Extragalactic Survey of the European Large Area Infrared Space Observatory Survey North 1 field. We have used Very Large Array observations with a total intensity rms of 87 μJy beam−1 to match SWIRE counterparts to the radio sources. Infrared color analysis of our radio sample shows that the majority of polarized sources are elliptical galaxies with an embedded active galactic nucleus. Using available redshift catalogs, we found 429 radio sources of which 69 are polarized with redshifts in the range of 0.04 < z < 3.2. We find no correlation between redshift and percentage polarization for our sample. However, for polarized radio sources, we find a weak correlation between increasing percentage polarization and decreasing luminosity.
Scattering by regular black holes: Planar massless scalar waves impinging upon a Bardeen black hole

Singularities are common features of general relativity black holes. However, within general relativity, one can construct black holes that present no singularities. These regular black hole solutions can be achieved by, for instance, relaxing one of the energy conditions on the stress energy tensor sourcing the black hole. Some regular black hole solutions were found in the context of non-linear electrodynamics, the Bardeen black hole being the first one proposed. In this paper, we consider a planar massless scalar wave scattered by a Bardeen black hole. We compare the scattering cross section computed using a partial-wave description with the classical geodesic scattering of a stream of null geodesics, as well as with the semi-classical glory approximation. We obtain that, for some values of the corresponding black hole charge, the scattering cross section of a Bardeen black hole has a similar interference pattern of a Reissner-Nordstr\"om black hole.
Willingness and Its Associated Factors for Blood Donation in Gondar Town, Northwest Ethiopia: A Community-Based Cross-Sectional Study

Background: Although the World Health Organization recommends 100% willingness for blood donation, the percentage of blood collected from willing blood donors and the average annual blood collection rate is extremely low in Ethiopia. Adults can serve as an essential pool formeeting the demand of safe blood. Thus, this study is aimed at examining willingness and its associated factors for blood donation among the adult population in Gondar town, Northwest Ethiopia. Methods: A community-based cross-sectional study was conducted on548 respondents from 1–30 October2021. Multistage sampling techniques were used to select the study participants. The data were collected using an interviewer-administered structured questionnaire. Epi-data version 4.6 and SPSS version 23 software was used for data entry and analysis, respectively. A binary logistic regression (bivariable and multivariable) was performed to identify the statistically significant variables. Results: Less than half, 45.3% (95% CI: 41.4, 49.9), of the study participants hadthe willingness to donate blood. Participants who were renters of their own houses [AOR: 3.19; (95% CI: 2.09, 4.62)], had a history of blood donation practice [AOR: 1.90(95% CI: 1.16, 3.19)], had witnessed blood being donated [AOR: 2.56 (95% CI:1.65, 6.95)], had a history of relatives who have died through blood loss [AOR: 2.28 (95% CI:1.19, 4.36)], and had good knowledge [AOR: 2.23; (95% CI: 1.49, 3.34)] were more willing to donate blood, with these factors being the significant predictors. Conclusions: Generally, willingness towards blood donation is low in the study area. In order to increase community willingness to donate blood, healthcare providers, national blood banks, and transfusion agencies should design strategies to promote and motivate their communities. In addition to this, participants should receive information on the health benefits of donating blood, the volume of blood donated, and the number of patients benefiting from a single unit of blood donated.
Multiply imaged time-varying sources behind galaxy clusters

With upcoming (continuum) surveys of high-resolution radio telescopes, detection rates of fast radio bursts (FRBs) might approach 105 per sky per day by future extremely large observatories, such as the possible extension of the Square Kilometer Array (SKA) to a phase-2 array. Depending on the redshift distribution of FRBs and using the repeating FRB121102 as a model, we calculate a detection rate of multiply imaged FRBs with their multiply imaged hosts caused by the distribution of galaxy-cluster-scale gravitational lenses of the order of 10−4 per square degree per year for a minimum total flux of the host of 10 μJy at 1.4 GHz for SKA phase 2. Our comparison of estimated detection rates for quasars (QSOs), supernovae (SNe), gamma ray bursts (GRBs), and FRBs shows that multiple images of FRBs could be more numerous than those of GRBs and SNe and as numerous as multiple images of QSOs. Time delays between the multiple images of an FRB break degeneracies in model-based and model-independent lens reconstructions as other time-varying sources do, yet without a microlensing bias, as FRBs are more point-like and have shorter duration times. We estimate the relative imprecision of FRB time-delay measurements to be 10−10 for time delays on the order of 100 days for galaxy-cluster-scale lenses, yielding more precise (local) lens properties than time delays from the other time-varying sources. Using the lens modelling software Grale, we show the increase in accuracy and precision of the reconstructed scaled surface mass density map of a simulated cluster-scale lens when adding time delays for one set of multiple images to the set of observational constraints.
THE RISE OF MASSIVE RED GALAXIES: THE COLOR–MAGNITUDE AND COLOR–STELLAR MASS DIAGRAMS FOR zphot ≲ 2 FROM THE MULTIWAVELENGTH SURVEY BY YALE–CHILE

We present the color–magnitude and color–stellar mass diagrams for galaxies with zphot ≲ 2, based on a K(AB) < 22 catalog of the Extended Chandra Deep Field South from the MUltiwavelength Survey by Yale–Chile. Our main sample of 7840 galaxies contains 1297 M*>1011M☉ galaxies in the range 0.2 < zphot < 1.8. We show empirically that this catalog is approximately complete for M*>1011 M☉ galaxies for zphot < 1.8. For this mass-limited sample, we show that the locus of the red sequence color–stellar mass relation evolves as Δ(u − r) ∝ (−0.44 ± 0.02)zphot for zphot ≲ 1.2. For zphot ≳ 1.3, however, we are no longer able to reliably distinguish red and blue subpopulations from the observed color distribution; we show that this would require much deeper near-infrared data. At 1.5 < zphot < 1.8, the comoving number density of M*>1011 M☉ galaxies is ≈50% of the local value, with a red fraction of ≈33%. Making a parametric fit to the observed evolution, we find ntot(z) ∝ (1 + zphot)−0.52±0.12(±0.20). We find stronger evolution in the red fraction: fred(z) ∝ (1 + zphot)−1.17±0.18(±0.21). Through a series of sensitivity analyses, we show that the most important sources of systematic error are (1) systematic differences in the analysis of the z ≈ 0 and z ≫ 0 samples; (2) systematic effects associated with details of the photometric redshift calculation; and (3) uncertainties in the photometric calibration. With this in mind, we show that our results based on photometric redshifts are consistent with a completely independent analysis which does not require redshift information for individual galaxies. Our results suggest that, at most, 1/5 of local red sequence galaxies with M*>1011M☉ were already in place at z ∼ 2.
THE EVOLVING RELATIONS BETWEEN SIZE, MASS, SURFACE DENSITY, AND STAR FORMATION IN 3 × 104 GALAXIES SINCE z = 2

The presence of massive, compact, quiescent galaxies at z>2 presents a major challenge for theoretical models of galaxy formation and evolution. Using one of the deepest large public near-IR surveys to date, we investigate in detail the correlations between star formation and galaxy structural parameters (size, stellar mass, and surface density) from z = 2 to the present. At all redshifts, massive quiescent galaxies (i.e., those with little or no star formation) occupy the extreme high end of the surface density distribution and follow a tight mass–size correlation, while star-forming galaxies show a broad range of both densities and sizes. Conversely, galaxies with the highest surface densities comprise a nearly homogeneous population with little or no ongoing star formation, while less dense galaxies exhibit high star formation rates and varying levels of dust obscuration. Both the sizes and surface densities of quiescent galaxies evolve strongly from z = 2–0; we parameterize this evolution for both populations with simple power-law functions and present best-fit parameters for comparison to future theoretical models. Higher-mass quiescent galaxies undergo faster structural evolution, consistent with previous results. Interestingly, star-forming galaxies’ sizes and densities evolve at rates similar to those of quiescent galaxies. It is therefore possible that the same physical processes drive the structural evolution of both populations, suggesting that “dry mergers” may not be the sole culprit in this size evolution.
Texture zeros and weak basis transformations in the quark sector of the standard model

Stimulated by the recent attention given to the texture zeros found in the quark mass matrices sector of the Standard Model, an analytical method for identifying (or to exclude) texture zeros models will be implemented here, starting from arbitrary quark mass matrices and making a suitable weak basis (WB) transformation, we are be able to find equivalent quark mass matrix. It is shown that the number of non-equivalent quark mass matrix representations is finite. We give exact numerical results for parallel and non-parallel four-texture zeros models. We find that some five-texture zeros Ansatze are in agreement with all present experimental data. And we confirm definitely that six-texture zeros of Hermitian quark mass matrices are not viable models anymore.
Toward the Limits of Matter: Ultra-relativistic nuclear collisions at CERN

Strongly interacting matter as described by the thermodynamics of QCD undergoes a phase transition, from a low temperature hadronic medium to a high temperature quark-gluon plasma state. In the early universe this transition occurred during the early microsecond era. It can be investigated in the laboratory, in collisions of nuclei at relativistic energy, which create "fireballs" of sufficient energy density to cross the QCD Phase boundary. We describe 3 decades of work at CERN, devoted to the study of the QCD plasma and the phase transition. From modest beginnings at the SPS, ultra-relativistic heavy ion physics has evolved today into a central pillar of contemporary nuclear physics and forms a significant part of the LHC program.
MICROLENSING-BASED ESTIMATE OF THE MASS FRACTION IN COMPACT OBJECTS IN LENS GALAXIES

We estimate the fraction of mass that is composed of compact objects in gravitational lens galaxies. This study is based on microlensing measurements (obtained from the literature) of a sample of 29 quasar image pairs seen through 20 lens galaxies. We determine the baseline for no microlensing magnification between two images from the ratios of emission line fluxes. Relative to this baseline, the ratio between the continua of the two images gives the difference in microlensing magnification. The histogram of observed microlensing events peaks close to no magnification and is concentrated below 0.6 mag, although two events of high magnification, Δm ∼ 1.5, are also present. We study the likelihood of the microlensing measurements using frequency distributions obtained from simulated microlensing magnification maps for different values of the fraction of mass in compact objects, α. The concentration of microlensing measurements close to Δm ∼ 0 can be explained only by simulations corresponding to very low values of α (10% or less). A maximum likelihood test yields α = 0.05+0.09−0.03 (90% confidence interval) for a quasar continuum source of intrinsic size . This estimate is valid in the 0.1–10 M☉ range of microlens masses. We study the dependence of the estimate of α with , and find that α ≲ 0.1 for . High values of α are possible only for source sizes much larger than commonly expected . Regarding the current controversy about Milky Way/LMC and M31 microlensing studies, our work supports the hypothesis of a very low content in MACHOS (Massive Compact Halo Objects). In fact, according to our study, quasar microlensing probably arises from the normal star populations of lens galaxies and there is no statistical evidence for MACHOS in the dark halos.
Ram pressure profiles in galaxy groups and clusters

Using a hybrid method that combines non-radiative hydrodynamical simulations with a semi-analytic model of galaxy formation, we determine the ram pressure experienced by galaxies in haloes with virial masses 12.5 ≤ log (M200/ h-1 M⊙) < 15.35 as a function of the halocentric distance, for redshifts 0 ≤ z ≤ 3. The ram pressure is calculated with a self-consistent method that uses the simulation gas particles to obtain the properties of the intergalactic medium. The ram pressure profiles obtained can be well described by beta profile models, with parameters that depend on redshift and halo virial mass in a simple fashion. The fitting formulae provided here will prove useful to include ram pressure effects into semi-analytic models based on methods that lack gas physics, such as dark-matter-only simulations or the Press-Schechter formalism.
Various Local Heating Events in the Earliest Phase of Flux Emergence

Emerging flux regions (EFRs) are known to exhibit various sporadic local heating events in the lower atmosphere. To investigate the characteristics of these events, especially to link the photospheric magnetic fields and atmospheric dynamics, we analyze Hinode, Interface Region Imaging Spectrograph (IRIS), and Solar Dynamics Observatory data of a new EFR in NOAA AR 12401. Out of 151 bright points (BPs) identified in Hinode/SOT Ca images, 29 are overlapped by an SOT/SP scan. Seven BPs in the EFR center possess mixed-polarity magnetic backgrounds in the photosphere. Their IRIS UV spectra (e.g., Si iv 1402.8 Å) are strongly enhanced and red- or blueshifted, with tails reaching , which is highly suggestive of bi-directional jets; each brightening lasts for 10–15 minutes, leaving flare-like light curves. Most of this group show bald patches, the U-shaped photospheric magnetic loops. Another 10 BPs are found in unipolar regions at the EFR edges. They are generally weaker in UV intensities and exhibit systematic redshifts with Doppler speeds up to , which could exceed the local sound speed in the transition region. Both types of BPs show signs of strong temperature increase in the low chromosphere. These observational results support the physical picture that heating events in the EFR center are due to magnetic reconnection within cancelling undular fields like Ellerman bombs, while the peripheral heating events are due to shocks or strong compressions caused by fast downflows along the overlying arch filament system.
Identifying Structural VARs from Sparse Narrative Instruments Dynamic Effects of U.S. Macroprudential Policies

We study the identiﬁcation of policy shocks in Bayesian proxy VARs for the case that the instrument consists of sparse qualitative observations indicating the signs of certain shocks. We propose two identiﬁcation schemes, i.e. linear discriminant analysis and a non-parametric sign concordance criterion. Monte Carlo simulations suggest that these provide more accurate conﬁdence bounds than standard proxy VARs. Our application to U.S. macroprudential policies ﬁnds persistent eﬀects of capital requirements and mortgage underwriting standards on credit volumes and house prices together with moderate eﬀects on GDP and inﬂation.