Miracle-dz/UniFAR-FTUs huggingface dataset:
A WISE view of novae - I. The data

We present the results of data-mining the Wide-field Infrared Survey Explorer (WISE) archive for data on classical and recurrent novae. We find that the detections are consistent with dust emission, line emission, emission by a stellar photosphere, or a combination of these. Of the 36 novae detected in one or more WISE bands, 16 are detected in all four; thirty-one known novae are not detected by WISE. We also searched for WISE data on post-WISE novae, to gain information about nova progenitors. In this first paper we consider only the WISE data. In future papers we will provide a more detailed modelling of the WISE data, and discuss WISE data on post-WISE novae - including their variability - and will complement the WISE data with data from other IR surveys.
A novel black hole mimicker: a boson star and a global monopole nonminimally coupled to gravity

A field-theoretic model for a highly compact object that mimicks a black hole is found for the gravitationally interacting system of a boson star and a global monopole which are nonminimally coupled to gravity. According to the strength of the nonlinear gravitational effects and the gravitational backreaction, three distinct coupling regimes are featured: weak, mild and strong. In the strong coupling regime we show that a repulsive monopole stabilizes an attractive boson star and the resulting configuration exhibits large energy density, large (and negative) principal pressures, large compactness, large effective potential, large local forces, and yet exhibits no event horizon. As such a composite system of a boson star and a global monopole represents a convincing microscopic candidate for a black hole mimicker.
AVERAGE METALLICITY AND STAR FORMATION RATE OF Lyα EMITTERS PROBED BY A TRIPLE NARROWBAND SURVEY

We present the average metallicity and star formation rate (SFR) of Lyα emitters (LAEs) measured from our large-area survey with three narrowband (NB) filters covering the Lyα, [O ii]λ3727, and Hα+[N ii] lines of LAEs at z = 2.2. We select 919 z = 2.2 LAEs from Subaru/Suprime-Cam NB data in conjunction with Magellan/IMACS spectroscopy. Of these LAEs, 561 and 105 are observed with KPNO/NEWFIRM near-infrared NB filters whose central wavelengths are matched to redshifted [O ii] and Hα nebular lines, respectively. By stacking the near-infrared images of the LAEs, we successfully obtain average nebular-line fluxes of LAEs, the majority of which are too faint to be identified individually by NB imaging or deep spectroscopy. The stacked object has an Hα luminosity of 1.7 × 1042 erg s−1 corresponding to an SFR of 14 M☉ yr−1. We place, for the first time, a firm lower limit to the average metallicity of LAEs of Z ≳ 0.09 Z☉ (2σ) based on the [O ii]/(Hα+[N ii]) index together with photoionization models and empirical relations. This lower limit of metallicity rules out the hypothesis that LAEs, so far observed at z ∼ 2, are extremely metal-poor (Z < 2 × 10−2 Z☉) galaxies at the 4σ level. This limit is higher than a simple extrapolation of the observed mass–metallicity relation of z ∼ 2 UV-selected galaxies toward lower masses (5 × 108 M☉), but roughly consistent with a recently proposed fundamental mass–metallicity relation when the LAEs’ relatively low SFR is taken into account. The Hα and Lyα luminosities of our NB-selected LAEs indicate that the escape fraction of Lyα photons is ∼12%–30%, much higher than the values derived for other galaxy populations at z ∼ 2.
Longitudinal muon spin relaxation in high-purity aluminum and silver

When positive muons are stopped in a high puritymetal with the muon spin along the direction of an ap-plied magnetic ﬁeld, the muons can be depolarized byinteractions with nuclear dipole moments, conductionelectrons, and paramagnetic impurities. The form ofthe resulting depolarization has been studied using theµ
Cosmological Intersecting Brane Solutions

The recent discovery of an explicit dynamical description of p-branes makes it possible to investigate the existence of intersection of such objects. We generalize the solutions depending on the overall transverse space coordinates and time to those which depend also on the relative transverse space and satisfy new intersection rules. We give classification of these dynamical intersecting brane solutions involving two branes, and discuss the application of these solutions to cosmology and show that these give Friedmann-Lemaitre-Robertson-Walker cosmological solutions. Finally, we construct the brane world models, using the (cut-)copy-paste method after compactifying the trivial spatial dimensions. We then find that interesting brane world models can be obtained from codimension-one branes and several static branes with higher codimensions. We also classify the behaviors of the brane world near the future/past singularity.
MASS-RADIUS RELATIONS AND CORE-ENVELOPE DECOMPOSITIONS OF SUPER-EARTHS AND SUB-NEPTUNES

Many exoplanets have been discovered with radii of 1–4 R⊕, between that of Earth and Neptune. A number of these are known to have densities consistent with solid compositions, while others are “sub-Neptunes” likely to have significant H2–He envelopes. Future surveys will no doubt significantly expand these populations. In order to understand how the measured masses and radii of such planets can inform their structures and compositions, we construct models both for solid layered planets and for planets with solid cores and gaseous envelopes, exploring a range of core masses, H2–He envelope masses, and associated envelope entropies. For planets in the super-Earth/sub-Neptune regime for which both radius and mass are measured, we estimate how each is partitioned into a solid core and gaseous envelope, associating a specific core mass and envelope mass with a given exoplanet. We perform this decomposition for both “Earth-like” rock-iron cores and pure ice cores, and find that the necessary gaseous envelope masses for this important sub-class of exoplanets must range very widely from zero to many Earth masses, even for a given core mass. This result bears importantly on exoplanet formation and envelope evaporation processes.
Evidence for a Zb0(10610) in Dalitz analysis of Y(5S) -> Y(nS) pi0 pi0

We report the first observation of Y(5S) -> Y(1,2S) pi0 pi0 decays. Evidence for the Zb0(10610) with 4.9sigma significance is found in a Dalitz plot analysis of Y(5S) -> Y(2S) pi0 pi0 decays. The results are obtained with a 121.4 fb^-1 data sample collected with the Belle detector at the Y(5S) resonance at the KEKB asymmetric-energy e+e- collider.
PEMANFAATAN LIMBAH CANGKANG TELUR, KULIT BAWANG DAN DAUN KERING MELALUI PROSES SAINS DAN TEKNOLOGI SEBAGAI ALTERNATIF PENGHASIL PRODUK YANG RAMAH LINGKUNGAN

The purpose of this study was to ascertain that the processing of waste egg shells, onion skins, and dried leaves can be organic fertilizer through the process of science and technology as a product that is environmentally friendly and high economic value. This research method is descriptive only quantitative. Research results showed that the waste chicken egg shells, onion skins, and dried mango leaves can be processed into organic fertilizer with high levels of nutrients for organic fertilizer from the eggshell is N 0.18% (medium), P content of 7% (medium) , and levels of C 8% (moderate), substance C - Organic 5.2% (very high), C / N of 30 (very high), for fertilizers from onion skin that is N 0.13% (moderate), the levels of P 4 % (moderate), and levels of C 5% (medium), substance C - Organic 4.8% (high), C / N 23 (high), for fertilizers from the dried leaves are N 0.16% (medium), P content of 6% (moderate), and K content of 5.8% (moderate), substance C - Organic 4% (high), C / N 25 (high), that is worth selling high and can compete, Marketing is done in a flower sales with sales revenue was approximately 8 burlap sack 5 kg of the total sales of 12 jute from each - each organic fertilizer.
SN 2011fe: A Laboratory for Testing Models of Type Ia Supernovae

Abstract SN 2011fe is the nearest supernova of Type Ia (SN Ia) discovered in the modern multi-wavelength telescope era, and it also represents the earliest discovery of an SN Ia to date. As a normal SN Ia, SN 2011fe provides an excellent opportunity to decipher long-standing puzzles about the nature of SNe Ia. In this review, we summarise the extensive suite of panchromatic data on SN 2011fe and gather interpretations of these data to answer four key questions: (1) What explodes in an SN Ia? (2) How does it explode? (3) What is the progenitor of SN 2011fe? and (4) How accurate are SNe Ia as standardisable candles? Most aspects of SN 2011fe are consistent with the canonical picture of a massive CO white dwarf undergoing a deflagration-to-detonation transition. However, there is minimal evidence for a non-degenerate companion star, so SN 2011fe may have marked the merger of two white dwarfs.
Shocked water in the Cepheus E protostellar outflow

Context. Previous far-infrared observations at low-angular resolution have reported the presence of water associated with low-velocity outflow shocks and protostellar envelopes. Aims. We want to elucidate the origin of water emission in protostellar systems. Methods. The outflow driven by the intermediate-mass class 0 protostar Cep E is among the most luminous outflows detected so far. Using the IRAM 30 m telescope, we searched for and detected the p-H 2 O 3 13 -2 20 line emission at 183 GHz in the Cep E star-forming core. The emission arises from high-velocity gas close to the protostar, which is unresolved in the main beam of the telescope. Complementary observations at 2" resolution with the Plateau de Bure interferometer helped establish the origin of the emission detected and the physical conditions in the emitting gas. The water line profile and its spatial distribution are very similar to those of SiO. We find that the H 2 O emission arises from warm (~200 K), dense ((1-2) x 10 6 cm -3 ) gas, and its abundance is enhanced by one to two orders of magnitude with respect to the protostellar envelope. Results. We detect water emission in strong shocks from the high-velocity jet at 1000 AU from the protostar. Despite the large beam size of the telescope, such emission should be detectable with Herschel.
Recovery from population III supernova explosions and the onset of second generation star formation

We use cosmological simulations to assess how the explosion of the first stars in supernovae (SNe) influences early cosmic history. Specifically, we investigate the impact by SNe on the host systems for Population III (Pop III) star formation and explore its dependence on halo environment and Pop III progenitor mass. We then trace the evolution of the enriched gas until conditions are met to trigger second-generation star formation. To this extent, we quantify the recovery timescale, which measures the time delay between a Pop III SN explosion and the appearance of cold, dense gas, out of which second-generation stars can form. We find that this timescale is highly sensitive to the Pop III progenitor mass, and less so to the halo environment. For Pop III progenitor masses M . 40M , recovery is prompt, 10 Myr. For more massive progenitors, including those exploding in pair instability SNe, second-generation star formation is delayed significantly, for up to a Hubble time. The dependence of the recovery time on the mass of the SN progenitor is mainly due to the ionizing impact of the progenitor star. Photoionization heating increases the gas pressure and initiates a hydrodynamical response that reduces the central gas density, an effect that is stronger in more massive and hence more luminous progenitors. The gas around lower mass Pop III stars remains therefore denser and hence the SN remnants cool more rapidly, facilitating the subsequent re-condensation of the gas and formation of a second generation of stars. In most cases, the second-generation stars are already metal-enriched, thus belonging to Population II. The recovery timescale is a key quantity governing the nature of the first galaxies, able to host low-mass, long-lived stellar systems. These in turn are the target of future deep-field campaigns with the James Webb Space Telescope.
A subarcsecond study of the hot molecular core in G023.01−00.41

(Abridged) METHODS: We performed SMA observations at 1.3 mm with both the most extended and compact array configurations, providing sub-arcsecond and high sensitivity maps of various molecular lines, including both hot-core and outflow tracers. We also reconstruct the spectral energy distribution of the region from millimeter to near infrared wavelengths, using the Herschel/Hi-GAL maps, as well as archival data. RESULTS: From the spectral energy distribution, we derive a bolometric luminosity of about 4x10^4 Lsun. Our interferometric observations reveal that the distribution of dense gas and dust in the HMC is significantly flattened and extends up to a radius of 8000 AU from the center of radio continuum and maser emission in the region. The equatorial plane of this HMC is strictly perpendicular to the elongation of the collimated bipolar outflow, as imaged on scales of about 0.1-0.5 pc in the main CO isotopomers as well as in the SiO(5-4) line. In the innermost HMC regions (ca. 1000 AU), the velocity field traced by the CH3CN(12_K-11_K) line emission shows that molecular gas is both expanding along the outflow direction following a Hubble-law, and rotating about the outflow axis, in agreement with the (3-D) velocity field traced by methanol masers. The velocity field associated with rotation indicates a dynamical mass of 19 Msun at the center of the core. The latter is likely to be concentrated in a single O9.5 ZAMS star, consistent with the estimated bolometric luminosity of G023.01-00.41. The physical properties of the CO(2-1) outflow emission, such as its momentum rate 6x10^-3 Msun km/s /yr and its outflow rate 2x10^-4 Msun/yr, support our estimates of the luminosity (and mass) of the embedded young stellar object.
Radiative feedback from protoplanets in self-gravitating protoplanetary discs

It is well known that massive protoplanetary disc are gravitationally unstable beyond tens of AU from their parent star. The eventual fate of the self-gravitating gas clumps born in the disc is currently not understood, although the range of uncertainty is well known. If clumps migrate inward rapidly, they are tidally disrupted, which may leave behind giant or terrestrial like planets. On the other hand, if clumps migrate less rapidly, they tend to accrete gas, becoming proto brown dwarfs or low mass companions to the parent star. Here we argue that radiative feedback of contracting clumps (protoplanets) on their discs is an important effect that has been overlooked in previous calculations. We show analytically that temperature in clump’s vicinity may be high enough to support a quasi-static atmosphere if the clump mass is below a critical value, Mcr � 6 Jupiter masses (MJ). This may arrest further gas accretion onto the clump and thus promote formation of planets rather than low mass companions. We use numerical simulations to evaluate these analytical conclusions by studying migration and accretion of gas clumps as a function of their initial mass, Mi. Simulations neglecting the radiative preheating effect show that gas clumps with mass less than � 2MJ migrate inward rapidly; more massive clumps result in low mass companions. In contrast, simulations that include radiative preheating from the clump show that clumps as massive as 8MJ migrate inward rapidly and end up tidally disrupted in the inner disc. We conclude that, with other parameters being equal, previous simulations neglecting radiative feedback from self-gravitating clumps over-estimated the population of brown dwarfs and low mass stellar companions and under-estimated the population of planets.
Comparative evaluation of antimicrobial activity of ground husk of cocoa bean with and without xylitol on Streptococcus Mutans – An in-vitro study.

Background: Dental caries is a disease that occurs when bacteria, predominantly Streptococcus mutans, colonizes the tooth surface and metabolizes the dietary carbohydrates to acids, resulting in demineralization of teeth. Interventions that can inhibit the growth and survival of streptococcus mutans are crucial to reduce dental caries. Cocoa bean husks, extracted from the shells of cocoa beans have shown to possess anti glucosyltransferase and antibacterial activities. Aim of our study was to evaluate in-vitro antimicrobial activity of ground husk of cocoa beans with and without xylitol on streptococcus mutans. Methods – The study was carried out using 96 well microtiter plate and these were divided into three groups. Group I consisted of Extracted powder of cocoa bean (CBH), Group II was of extracted powder of cocoa bean and xylitol (CBH+X) and Group III consisted of Chlorhexidine (0.12%) (CHX). Minimum Inhibitory concentration was assessed using 96 well micro-titer plate. Standardized strain of Streptococcus Mutans 25175D was used. Results – No anti-microbial activity was seen for group I (CBH) and group II (CBH+X) at concentrations of 0.3%. However, chlorhexidine (0.12%) showed its antibacterial activity at its first concentration only. Conclusions – It was found that ground husk of cocoa bean at 0.3% does not possess any antimicrobial property in in-vitro trial. Addition of xylitol had no effect on increasing antibacterial property.
New and updated convex shape models of asteroids based on optical data from a large collaboration network

Context. Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. These efforts already provided deep insight into physical properties of main-belt asteroids or large collisional families. Going into finer detail (e.g., smaller collisional families, asteroids with sizes 20 km) requires knowledge of physical parameters of more objects. Aims. We aim to increase the number of asteroid shape models and rotation states. Such results provide important input for further studies, such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides bulk density estimates incombination with known masses, but also constrains theoretical collisional and evolutional models of the solar system. Methods. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as input for the convex inversion method, and derive 3D shape models of asteroids together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that 100 observers who submittheir optical data to publicly available databases. Results. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature, or for which masses will most likely be determined from their gravitational influence on smaller bodies whose orbitaldeflections will be observed by the ESA Gaia astrometric mission. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and three near-Earth asteroids. The shape model revisions and determinations were enabled by using additional optical data from recent apparitions for shape optimization.
Home-Applied Dual-Light Photodynamic Therapy in the Treatment of Stable Chronic Periodontitis (HOPE-CP)—Three-Month Interim Results

A single-site, randomized clinical trial was designed to determine the efficacy of regular home use of Lumoral® dual-light antibacterial aPDT in periodontitis patients. For the study, 200 patients were randomized to receive non-surgical periodontal treatment (NSPT), including standardized hygiene instructions and electric toothbrush, scaling and root planing, or NSPT with adjunctive Lumoral® treatment. A complete clinical intraoral examination was conducted in the beginning, at three months, and at six months. This report presents the three-month results of the first 59 consecutive randomized subjects. At three months, bleeding on probing (BOP) was lower in the NSPT + Lumoral®-group than in the NSPT group (p = 0.045), and more patients in the NSPT + Lumoral®-group had their BOP below 10% (54% vs. 22%, respectively, p = 0.008). In addition, patients in the NSPT + Lumoral®-group improved their oral hygiene by visible-plaque-index (p = 0.0003), while the NSPT group showed no statistical improvement compared to the baseline. Both groups significantly reduced the number of deep periodontal pockets, but more patients with a reduction in their deep pocket number were found in the NSPT + Lumoral® group (92% vs. 63%, p = 0.02). Patients whose number of deep pockets was reduced by 50% or more were also more frequent in the NSPT + Lumoral®-group (71% vs. 33%, p = 0.01). Patients with initially less than ten deep pockets had fewer deep pockets at the three-month follow-up in the Lumoral® group (p = 0.01). In conclusion, adjunctive use of Lumoral® in NSPT results in improved treatment outcomes at three months post-therapy.
Mimetic Compact Stars

Modified gravity models have been constantly proposed with the purpose of evading some standard gravity shortcomings. Recently proposed by A.H. Chamseddine and V. Mukhanov, the Mimetic Gravity arises as an optimistic alternative. Our purpose in this work is to derive Tolman-Oppenheimer-Volkoff equations and solutions for such a gravity theory. We solve them numerically for quark star and neutron star cases. The results are carefully discussed.
INFRARED AND X-RAY SPECTROSCOPY OF THE Kes 75 SUPERNOVA REMNANT SHELL: CHARACTERIZING THE DUST AND GAS PROPERTIES

We present deep Chandra observations and Spitzer Space Telescope infrared (IR) spectroscopy of the shell in the composite supernova remnant (SNR) Kes 75 (G29.7-0.3). The remnant is composed of a central pulsar wind nebula and a bright partial shell in the south that is visible at radio, IR, and X-ray wavelengths. The X-ray emission can be modeled by either a single thermal component with a temperature of ∼1.5 keV, or with two thermal components with temperatures of 1.5 and 0.2 keV. Previous studies suggest that the hot component may originate from reverse-shocked supernova (SN) ejecta. However, our new analysis shows no definitive evidence for enhanced abundances of Si, S, Ar, Mg, and Fe, as expected from SN ejecta, or for the IR spectral signatures characteristic of confirmed SN condensed dust, thus favoring a circumstellar or interstellar origin for the X-ray and IR emission. The X-ray and IR emission in the shell are spatially correlated, suggesting that the dust particles are collisionally heated by the X-ray emitting gas. The IR spectrum of the shell is dominated by continuum emission from dust with little, or no line emission. Modeling the IR spectrum shows that the dust is heated to a temperature of ∼140 K by a relatively dense, hot plasma that also gives rise to the hot X-ray emission component. The density inferred from the IR emission is significantly higher than the density inferred from the X-ray models, suggesting a low filling factor for this X-ray emitting gas. The total mass of the warm dust component is at least 1.3 × 10−2 M☉, assuming no significant dust destruction has occurred in the shell. The IR data also reveal the presence of an additional plasma component with a cooler temperature, consistent with the 0.2 keV gas component. Our IR analysis therefore provides an independent verification of the cooler component of the X-ray emission. The complementary analyses of the X-ray and IR emission provide quantitative estimates of density and filling factors of the clumpy medium swept up by the SNR.