Miracle-dz/UniFAR-FTUs huggingface dataset:
NTT and NOT spectroscopy of SDSS-II supernovae

Context. The Sloan Digital Sky Survey II (SDSS-II) Supernova Survey, conducted between 2005 and 2007, was designed to detect a large number of type Ia supernovae around z ∼ 0.2, the redshift “gap” between low-z and high-z supernova searches. The survey has provided multi-band (ugriz) photometric lightcurves for variable targets, and supernova candidates were scheduled for spectroscopic observations, primarily to provide supernova classification and accurate redshifts. We present supernova spectra obtained in 2006 and 2007 using the New Technology Telescope (NTT) and the Nordic Optical Telescope (NOT). Aims. We provide an atlas of supernova spectra in the range z = 0.03−0.32 that complements the well-sampled lightcurves from SDSS-II in the forthcoming three-year SDSS supernova cosmology analysis. The sample can, for example, be used for spectral studies of type Ia supernovae, which are critical for understanding potential systematic effects when supernovae are used to determine cosmological distances. Methods. The spectra were reduced in a uniform manner, and special care was taken in estimating the uncertainties for the different processing steps. Host-galaxy light was subtracted when possible and the supernova type fitted using the SuperNova IDentification code (SNID). We also present comparisons between spectral and photometric dating using SALT lightcurve fits to the photometry from SDSS-II, as well as the global distribution of our sample in terms of the lightcurve parameters: stretch and colour. Results. We report new spectroscopic data from 141 type Ia supernovae, mainly between − 9a nd+15 days from lightcurve maximum, including a few cases of multi-epoch observations. This homogeneous, host-galaxy subtracted, type Ia supernova spectroscopic sample is among the largest such data sets and unique in its redshift interval. The sample includes two potential SN 1991T-like supernovae (SN 2006on and SN 2007ni) and one potential SN 2002cx-like supernova (SN 2007ie). In addition, the new compilation includes spectra from 23 confirmed type II and 8 type Ib/c supernovae.
Patterns of Gendered Performance Difference in Introductory STEM Courses

Grades provide students with their primary performance feedback: signals which affect academic choices. Variations in grading practice among courses impose grade penalties (and bonuses) on students who take them. These grade penalties are sometimes gendered. Using extensive data from the University of Michigan, we report on patterns of grade penalty and gendered performance difference across 116 large courses. We find that significant gendered performance differences are ubiquitous in large introductory STEM lecture courses. They are largely absent in both STEM labs and in lecture courses in other disciplines. Exploring the features of these courses, we hypothesize that evaluation methods used in STEM lecture courses interact with stereotype threat to create these gendered performance differences.
SYNCHROTRON SELF-INVERSE COMPTON RADIATION FROM REVERSE SHOCK ON GRB 120326A

We present multi-wavelength observations of a typical long duration GRB 120326A at z = 1.798, including rapid observations using a Submillimeter Array (SMA) and a comprehensive monitoring in the X-ray and optical. The SMA observation provided the fastest detection to date among seven submillimeter afterglows at 230 GHz. The prompt spectral analysis, using Swift and Suzaku, yielded a spectral peak energy of keV and an equivalent isotropic energy of Eiso as erg. The temporal evolution and spectral properties in the optical were consistent with the standard forward shock synchrotron with jet collimation (6.°69 ± 0.°16). The forward shock modeling, using a two-dimensional relativistic hydrodynamic jet simulation, was also determined by the reasonable burst explosion and the synchrotron radiation parameters for the optical afterglow. The X-ray light curve showed no apparent jet break and the temporal decay index relation between the X-ray and optical (αo − αX = −1.45 ± 0.10) indicated different radiation processes in each of them. Introducing synchrotron self-inverse Compton radiation from reverse shock is a possible solution, and the detection and slow decay of the afterglow in submillimeter supports that this is a plausible idea. The observed temporal evolution and spectral properties, as well as forward shock modeling parameters, enabled us to determine reasonable functions to describe the afterglow properties. Because half of the events share similar properties in the X-ray and optical as the current event, GRB 120326A will be a benchmark with further rapid follow-ups, using submillimeter instruments such as an SMA and the Atacama Large Millimeter/submillimeter Array.
A long-term photometric study of the FU Orionis star V 733 Cephei

Context. The FU Orionis candidate V733 Cep was discovered by Roger Persson in 2004. The star is located in the dark cloud L1216 close to the Cepheus OB3 association. Because only a small number of FU Orionis stars have been detected to date, photometric and spectral studies of V733 Cep are of great interest. Aims. The studies of the photometrical variability of PMS stars are very important to the understanding of stellar evolution. The main purpose of our study is to construct a long-time light curve of V733 Cep. On the basis of BVRI monitoring we also study the photometric behavior of the star. Methods. We gather data from CCD photometry and archival photographic plates. The photometric BVRI data (Johnson-Cousins system) that we present were collected from June 2008 to October 2009. To facilitate transformation from instrumental measurements to the standard system, fifteen comparison stars in the field of V733 Cep were calibrated in BVRI bands. To construct a historical light curve of V733 Cep, a search for archival photographic observations in the Wide-Field Plate Database was performed. As a result, 192 photographic plates containing the field of V733 Cep were found. Some plates were analyzed at our request to estimate the magnitude of V733 Cep. Results. Our photometric study confirms the affiliation of V733 Cep to the group of FU Orionis objects. An outburst in the optical and a slow rise in brightness during the period 1971‐1993 are well documented. During the period 1993‐2004, V733 Cep exhibited its maximum brightness and the amplitude of the observed outburst exceeded 4. m 5( R). TheBVRI photometric data imply that from February 2007 to October 2009, a slow decrease in brightness of V733 Cep was observed. The observed color evolution of V − I index also suggest that V733 Cep is currently fading. The long-time light curve of V733 Cep is similar to the light curves of other FU Orionis objects.
RawNet: Fast End-to-End Neural Vocoder

Neural networks based vocoders have recently demonstrated the powerful ability to synthesize high quality speech. These models usually generate samples by conditioning on some spectrum features, such as Mel-spectrum. However, these features are extracted by using speech analysis module including some processing based on the human knowledge. In this work, we proposed RawNet, a truly end-to-end neural vocoder, which use a coder network to learn the higher representation of signal, and an autoregressive voder network to generate speech sample by sample. The coder and voder together act like an auto-encoder network, and could be jointly trained directly on raw waveform without any human-designed features. The experiments on the Copy-Synthesis tasks show that RawNet can achieve the comparative synthesized speech quality with LPCNet, with a smaller model architecture and faster speech generation at the inference step.
FRAGMENTATION IN THE FIRST GALAXIES

Motivated by recent simulations of galaxy formation in which protogalaxies acquire their baryonic content through cold accretion, we study the gravitational fragmentation of cold streams flowing into a typical first galaxy. We use a one-zone hydrodynamical model to examine the thermal evolution of the gas flowing into a 108 M☉ dark matter halo at redshift z = 10. The goal is to gain an understanding of the expected fragmentation mass scale and thus the characteristic mass of the first population of stars to form by shock fragmentation. Our model accurately describes the chemical and thermal evolution of the gas as we are specifically concerned with how the chemical abundances and initial conditions of the low-density, metal-enriched, cold accretion streams that pass an accretion shock alter the cooling properties and tendency to fragment in the post-shock gas. Cold accretion flows are not shock heated at the virial radius but instead flow along high-baryonic-density filaments of the cosmic web and penetrate deep into the host halo of the protogalaxy. In this physical regime, if molecular cooling is absent because of a strong Lyman–Werner background, we find there to be a sharp drop in the fragmentation mass at a metallicity of Z ∼ 10−4 Z☉. If, however, H2 and HD molecules are present, they dominate the cooling at T < 104 K, and metallicity then has no effect on the fragmentation properties of the cold stream. For a solar abundance pattern of metallicity, O is the most effective metal coolant throughout the evolution, while for a pair instability supernova (PISN) metallicity yield, Si+ is the most effective coolant. PISN abundance patterns also exhibit a slightly smaller critical metallicity. Dust grains are not included in our chemical model, but we argue that their inclusion would not significantly alter the results. We also find that this physical scenario allows for the formation of stellar clusters and large, 104 M☉ bound fragments, possibly the precursors to globular clusters and supermassive black holes. Finally, we conclude that the usual assumption of isobaricity for galactic shocks breaks down in gas of a sufficiently high metallicity, suggesting that metal cooling leads to thermal instabilities.
NEAR-CONTEMPORANEOUS OPTICAL SPECTROSCOPIC AND INFRARED PHOTOMETRIC OBSERVATIONS OF CANDIDATE HERBIG Ae/Be STARS IN THE MAGELLANIC CLOUDS

We present near-IR (J, H, Ks) photometry for 27 of the 28 candidate Herbig Ae/Be stars in the Small and Large Magellanic Clouds (SMC and LMC) identified via the EROS1 and EROS2 surveys as well as near-contemporaneous optical (Hα) spectroscopy for 21 of these 28 candidates. Our observations extend previous efforts to determine the evolutionary status of these objects. We compare the IR brightness and colors of a subset of our sample with archival ground-based IR data and find evidence of statistically significant photometric differences for EROS LMC HAeBe candidates (ELHC) 5, 7, 12, 18, and 21 in one or more filters. In all cases, these near-IR photometric variations exhibit a gray color as compared to earlier epoch data. The ∼1 mag IR brightening and minimal change in the Hα emission strength we observe in ELHC 7 is consistent with previous claims that it is a UX Ori type HAe/Be star, which is occasionally obscured by dust clouds. We also detect a ∼1 mag IR brightening of ELHC 12, but find little evidence of a similar large-scale change in its Hα line strength, suggesting that its behavior could also be caused by a UX Ori-like event. The ∼0.5 mag IR variability we observe for ELHC 21, which also exhibited little evidence of a change in its Hα emission strength, could conceivably be caused by a major recent enhancement in the density of the inner disk region of a classical Be star. We also report the first near-IR photometry for two EROS SMC HAeBe Candidates (ESHC) stars and the first Hα spectroscopy for one ELHC and five ESHC stars. Although Hα emission is detected in all of these new observations, they do not exhibit a strong near-IR excess. It is therefore possible that many of these objects may be classical Be stars rather than Herbig Ae/Be stars.
High-energy emitting BL Lacs and high-energy neutrinos - Prospects for the direct association with IceCube and KM3NeT

Context. The origin of the high-energy flux of neutrinos detected by IceCube remains unknown. Recent works report evidence for a possible positional correlation between the reconstructed neutrino arrival directions and the positions in the sky of low-power, high-energy-emitting BL Lac objects (HBL). Aims. Assuming that γ -ray-emitting HBL form the bulk of the sources of high-energy neutrinos above 100 TeV, we intend to calculate the number of events expected to be detected for each source by IceCube and KM3NeT. Methods. Based on a simple theoretically-motivated framework inspired by the structured jet scenario for these sources, we postulate a direct proportionality between high-energy γ -ray and neutrino fluxes. We calculate the expected neutrino event rate for the HBL sources of the Second Fermi -LAT Catalog of High-Energy Sources (2FHL) for IceCube and the presently under-construction KM3NeT using declination-dependent and exposure-weighted effective areas. Results. We provide a list of 2FHL HBL with the calculated number of events. For IceCube, the derived count rate for several sources is relatively high, of the order of ≲1 yr -1 , consistent with the recent findings of a possible positional correlation. For KM3NeT, the calculated rates are higher, with several sources with expected rates exceeding 1 yr -1 . This, coupled with the improved angular resolution, implies that the HBL origin can be effectively tested with few years of observation of KM3NeT (and IceCube Gen2, for which similar performances are foreseen) through the direct association of neutrinos and single HBL. Conclusions. Our results show that if, as suggested by recent works, HBL represent a possible population of high-energy neutrino emitters, several single sources should be identified in a few years of exposure of KM3NeT, highlighting the importance of the improved angular resolution anticipated for KM3NeT and IceCube Gen2.
Analyzing the Consequences of Financial Inclusion on the Effectiveness of the Financial System and its Capacity to be Maintained Through Evidence from Asia

Using yearly data for 40 countries between 2000 and 2021, this article seeks to examine the connection between the financial inclusion index and development factors in the world's poorest regions: Asia. As a means of investigating this connection, we use pooled panel regression and panel data analysis. This empirical evidence suggests that expanding economies is the key to expanding access to financial services. Women are more likely than males to be economically excluded due to a variety of reasons, including unemployment and literacy rates. People in rural regions of less developed nations have less access to financial resources because of the economy's reliance on agriculture. Wage disparity has a chilling effect on people's ability to participate in the financial system and hampers progress. Because of this low degree of financial inclusion, these nations are not as developed as they may be. This research has the potential to improve the lives of marginalized people in the nations under consideration. Policymakers should think about enacting measures to boost literacy, eradicate gender discrimination, and increase wage equity in order to better the environment for development.
Mammal tracks record anthropogenic environmental influence in late-Holocene inland dunes of the European Sand Belt, Poland

Structures previously suggested to be footprints or tracks, but which have been little described, were observed within Quaternary inland dunes of the European Sand Belt. Excavation of these in several localities of the eastern part of the belt in Poland reveal that they are hoofprints of various ungulate mammals, both wild and domestic, as well as footprints of humans, ranging from potentially as early as the fifth to sixth century to the 19th century or later. Trample grounds and horizons with high densities of tracks are associated with other signs of intensifying usage of dune habitats for pasture and farming, including constrained movement of livestock, relatively well-developed paleosols, and evidence of ploughing. The presence of such abundant life traces not only reflects the presence of individual animals and people in an area, but sheds light on the potential processes and feedbacks that the tracemakers were involved in, in terms of maintaining and modifying the habitats themselves, which were dynamic and changeable. Footprints and their associated sedimentological records can be integrated with archaeological and historical data to analyse anthropogenic influence through time on physical landscapes and on the wild biota.
Differences in Access to Health Resources: An Analysis of Disparities among Dalit Sub-castes in Uttar Pradesh, India

This essay is based on an empirical study conducted in Sonbhadra district of Uttar Pradesh. It argues for the need of sub-caste level analysis among Dalits as regards their access to health resources. Making use of both quantitative and qualitative data, the disparities in the socio-economic standing of various sub-castes within scheduled castes are discussed. The perceptions about health, illness and disease provides the contextual information about the prevalence of various health conditions while the concentration curves reflect the disparities in out-of pocket expenditure, landholding and income among various sub-castes within Dalits. The case reports of the respondents facilitate an understanding of the intersection of social identity, economic status and spatial inaccessibility of health services as barriers in accessing health care services. The essay suggests that the differences in access to health resources among various sub-caste of Dalits is a function of intersection of social identity, socio-economic status and geographic location of health care services. There is a greater need to identify the differences and challenges within sub-castes to overcome the gap between their health needs and accessibility of health care services.
Questioning the Recent Observation of Quantum Hawking Radiation

A recent article [J. Steinhauer, Nat. Phys. 2016, 12, 959] has reported the observation of quantum Hawking radiation and its entanglement in an analogue black hole. Here, the published evidence, its consistency with theoretical bounds, and the statistical significance of the results are analyzed. The analysis raises severe doubts on the observation of Hawking radiation.
Cosmological perturbations on the phantom brane

We obtain a closed system of equations for scalar perturbations in a multi-component braneworld. Our braneworld possesses a phantom-like equation of state at late times, weff < −1, but no big-rip future singularity. In addition to matter and radiation, the braneworld possesses a new effective degree of freedom—the `Weyl fluid' or `dark radiation'. Setting initial conditions on super-Hubble spatial scales at the epoch of radiation domination, we evolve perturbations of radiation, pressureless matter and the Weyl fluid until the present epoch. We observe a gradual decrease in the amplitude of the Weyl-fluid perturbations after Hubble-radius crossing, which results in a negligible effect of the Weyl fluid on the evolution of matter perturbations on spatial scales relevant for structure formation. Consequently, the quasi-static approximation of Koyama and Maartens provides a good fit to the exact results during the matter-dominated epoch. We find that the late-time growth of density perturbations on the brane proceeds at a faster rate than in ΛCDM. Additionally, the gravitational potentials Φ and Ψ evolve differently on the brane than in ΛCDM, for which Φ = Ψ. On the brane, by contrast, the ratio Φ/Ψ exceeds unity during the late matter-dominated epoch (z ≲ 50). These features emerge as smoking gun tests of phantom brane cosmology and allow predictions of this scenario to be tested against observations of galaxy clustering and large-scale structure.
Beauty is distractive: particle production during multifield inflation

We consider a two-dimensional model of inflation, where the inflationary trajectory is ``deformed'' by a grazing encounter with an Extra Species/Symmetry Point (ESP) after the observable cosmological scales have left the Hubble radius. The encounter entails a sudden production of particles, whose backreaction causes a bending of the trajectory and a temporary decrease in speed, both of which are sensitive to initial conditions. This ``modulated'' effect leads to an additional contribution to the curvature perturbation, which can be dominant if the encounter is close. We compute associated non-Gaussianities, the bispectrum and its scale dependence as well as the trispectrum, which are potentially detectable in many cases. In addition, we consider a direct modulation of the coupling to the light field at the ESP via a modulaton field, a mixed scenario whereby the modulaton is identified with a second inflaton, and an extended Extra Species Locus (ESL); all of these scenarios lead to similar additional contributions to observables. We conclude that inflaton interactions throughout inflation are strongly constrained if primordial non-Gaussianities remain unobserved in current experiments such as PLANCK. If they are observed, an ESP encounter leaves additional signatures on smaller scales which may be used to identify the model.
Attractor Flows in st2 Black Holes

Following the same treatment of Bellucci et al. we obtain, the hitherto unknown general solutions of the radial attractor flow equations for extremal black holes, both for non-BPS with non-vanishing and vanishing central charge Z for the so-called st2 model, the minimal rank-two symmetric supergravity in d = 4 space-time dimensions. We also make useful comparisons with results that already exist in literature, and introduce the fake supergravity (first-order) formalism to be used in our analysis. An analysis of the BPS bound all along the non-BPS attractor flows and of the marginal stability of corresponding D-brane charge configurations has also been presented.
SIMULATIONS OF ISOLATED DWARF GALAXIES FORMED IN DARK MATTER HALOS WITH DIFFERENT MASS ASSEMBLY HISTORIES

We present zoom-in N-body/hydrodynamics resimulations of dwarf galaxies formed in isolated cold dark matter (CDM) halos with the same virial mass (Mv ≈ 2.5 × 1010 M☉) at redshift z = 0. Our goals are to (1) study the mass assembly histories (MAHs) of the halo, stellar, and gaseous components; and (2) explore the effects of the halo MAHs on the stellar/baryonic assembly of simulated dwarfs. Overall, the dwarfs are roughly consistent with observations. More specific results include: (1) the stellar-to-halo mass ratio remains roughly constant since z ∼ 1, i.e., the stellar MAHs closely follow halo MAHs. (2) The evolution of the galaxy gas fractions, fg, are episodic, showing that the supernova-driven outflows play an important role in regulating fg—and hence, the star formation rate (SFR)—however, in most cases, a large fraction of the gas is ejected from the halo. (3) The star formation histories are episodic with changes in the SFRs, measured every 100 Myr, of factors of 2–10 on average. (4) Although the dwarfs formed in late assembled halos show more extended SF histories, their z = 0 specific SFRs are still below observations. (5) The inclusion of baryons most of the time reduces the virial mass by 10%–20% with respect to pure N-body simulations. Our results suggest that rather than increasing the strength of the supernova-driven outflows, processes that reduce the star formation efficiency could help to solve the potential issues faced by CDM-based simulations of dwarfs, such as low values of the specific SFR and high stellar masses.