Miracle-dz/UniFAR-FTUs huggingface dataset:
H.E.S.S. observations of RX J1713.7−3946 with improved angular and spectral resolution: Evidence for gamma-ray emission extending beyond the X-ray emitting shell

Supernova remnants exhibit shock fronts (shells) that can accelerate charged particles up to very high energies. In the past decade, measurements of a handful of shell-type supernova remnants in very-high-energy gamma rays have provided unique insights into the acceleration process. Among those objects, RX J1713.7-3946 (also known as G347.3-0.5) has the largest surface brightness, allowing us in the past to perform the most comprehensive study of morphology and spatially resolved spectra of any such very-high-energy gamma-ray source. Here we present extensive new H.E. S.S. measurements of RX J1713.7-3946, almost doubling the observation time compared to our previous publication. Combined with new improved analysis tools, the previous sensitivity is more than doubled. The H.E. S.S. angular resolution of 0.048∘ (0.036∘ above 2 TeV) is unprecedented in gamma-ray astronomy and probes physical scales of 0.8 (0.6) parsec at the remnant's location. The new H.E. S.S. image of RX J1713.7-3946 allows us to reveal clear morphological differences between X-rays and gamma rays. In particular, for the outer edge of the brightest shell region, we find the first ever indication for particles in the process of leaving the acceleration shock region. By studying the broadband energy spectrum, we furthermore extract properties of the parent particle populations, providing new input to the discussion of the leptonic or hadronic nature of the gamma-ray emission mechanism.
J1649+2635: A Grand-Design Spiral with a Large Double-Lobed Radio Source

We report the discovery of a grand-design spiral galaxy associated with a double-lobed radio source. J1649+2635 (z = 0.0545) is a red spiral galaxy with a prominent bulge that it is associated with a L(1.4GHz) is approximately 10(exp24) W Hz(exp1) double-lobed radio source that spans almost 100 kpc. J1649+2635 has a black hole mass of M(BH) is approximately 3-7 10(exp8) Solar mass and SFR is approximately 0.26 - 2.6 solar mass year(exp1). The galaxy hosts a approximately 96 kpc diffuse optical halo, which is unprecedented for spiral galaxies. We find that J1649+2635 resides in an overdense environment with a mass of M(dyn) = 7.7(+7.9/4.3) 10(exp13) Solar mass, likely a galaxy group below the detection threshold of the ROSAT All-Sky Survey. We suggest one possible scenario for the association of double-lobed radio emission from J1649+2635 is that the source may be similar to a Seyfert galaxy, located in a denser-than-normal environment. The study of spiral galaxies that host large-scale radio emission is important because although rare in the local Universe, these sources may be more common at high-redshifts.
Analyzing Factors Associated with Blood Glucose Levels on Female Islamic Student (Santriwati) at Syaichona Cholil 2 Islamic Boarding School in Bangkalan Regency

This is a cross sectional study that aims to analyze the factors associated with blood glucose levels on teenage women. The researcher selected 77 female Islamic students (Santriwati) at the Syaichona Cholil 2 Islamic Boarding School as the respondents by using simple random sampling. The Data were collected by interviews, observations, and measurements which conducted on October 2019. The research variables were the education level, blood pressure status, instant drink consumption, nutritional status, and physical activity which were analyzed by using Correlation Rank Spearman with significance α = 0.05. The results showed that factors related to blood glucose levels are blood pressure status (p = 0.035) and physical activity (p = 0.023); while the level of education (p = 0.571), instant drink consumption (p = 0.955), and nutritional status (p = 0.159) are not associated with blood glucose level. The school suppose to conduct blood glucose screening test on teenagers for early detection of at-risk teenagers.
Cool core remnants in galaxy clusters

Istituto di Astroﬁsica Spaziale e Fisica Cosmica, INAF, via Bassini 15, I-20133 Milano, ItalyPreprint online version: October 26, 2009AbstractContext.X ray clusters are conventionally divided into two classes: “cool core” (CC) and “non cool core” (NCC) objects, on the bas isof the observational properties of their central regions. Recent results have shown that the cluster population is bimodal (Cavagnoloet al. 2009). Aims.We want to understand whether the observed distribution of clusters is due to a primordial division into two distinct classesrather than to diﬀerences in how these systems evolve across cosmic time.Methods. We systematically search the ICM of NCC clusters in a subsample of the B55 ﬂux limited sample of clusters for regionswhich have some characteristics typical of cool cores, namely low entropy gas and high metal abundanceResults.We ﬁnd that most NCC clusters in our sample host regions remin iscent of CC, i. e. characterized by relative low entropy gas(albeit not as low as in CC systems) and a metal abundance excess. We have dubbed these structures “cool core remnants”, si nce weinterpret them as what remains of a cool core after a heating event (AGN giant outbursts in a few cases and more commonly mergers). We infer that most NCC clusters have undergone a cool core phase during their life. The fact that most cool core remnants are foundin dynamically active objects provides strong support to scenarios where cluster core properties are not ﬁxed “ab initi o” but evolveacross cosmic time.Key words. Galaxies: clusters: general – X-rays: galaxies: clusters
Isolated and binary neutron stars in dynamical Chern-Simons gravity

We study isolated and binary neutron stars in dynamical Chern-Simons gravity. This theory modifies the Einstein-Hilbert action through the introduction of a dynamical scalar field coupled to the Pontryagin density. We here treat this theory as an effective model, working to leading order in the Chern-Simons coupling. We first construct isolated neutron star solutions in the slow-rotation expansion to quadratic order in spin. We find that isolated neutron stars acquire a scalar dipole charge that corrects its spin angular momentum to linear order in spin and corrects its mass and quadrupole moment to quadratic order in spin, as measured by an observer at spatial infinity. We then consider neutron stars binaries that are widely separated and solve for their orbital evolution in this modified theory. We find that the evolution of post-Keplerian parameters is modified, with the rate of periastron advance being the dominant correction at first post-Newtonian order. We conclude by applying these results to observed pulsars with the aim to place constraints on dynamical Chern-Simons gravity. We find that the modifications to the observed mass are degenerate with the neutron star equation of state, which prevents us from testing the theory with the inferred mass of the millisecond pulsar J1614-2230. We also find that the corrections to the post-Keplerian parameters are too small to be observable today even with data from the double binary pulsar J0737-3039. Our results suggest that pulsar observations are not currently capable of constraining dynamical Chern-Simons gravity, and thus, gravitational-wave observations may be the only path to a stringent constraint of this theory in the imminent future.
Difference in Social Anxiety among Students of Single-sex and Co-Education Schools

The purpose of the study was to understand how the classroom environment, in terms of student gender composition affects social anxiety among school students in an urban Indian context. The study aimed to examine the difference in levels of social anxiety, between students of single-sex and co-education schools. A comparative quantitative research design was adopted for this study. Convenient sampling technique was used to select the sample. The Liebowitz Social Anxiety Scale (Liebowitz, 1987) was administered to a total of 165 students (39 girls from co-education schools, 42 girls from all-girls schools, 38 boys from co-education schools and 46 boys from all-boys schools) of class IX and X across single-sex and co-education schools in Bangalore, Karnataka. Analysis of Variance (ANOVA) was done to identify differences in social anxiety among the four groups, which revealed that girls of co-education schools had significantly higher social anxiety than boys of single-sex schools. The difference among other student groups was not statistically significant. The findings indicate that boys are comfortable in an all-boys schools while girls in co-education school experience high social anxiety. Implications of the study, relevant to the education system are discussed.
A comprehensive classification of galaxies in the SDSS: How to tell true from fake AGN?

We use the W Hα versus [NII]/Hα (WHAN) diagram introduced by us in previous work to provide a comprehensive emission-line classification of Sloan Digital Sky Survey galaxies. This classification is able to cope with the large population of weak line galaxies that do not appear in traditional diagrams due to a lack of some of the diagnostic lines. A further advantage of the WHAN diagram is to allow the differentiation between two very distinct classes that overlap in the low-ionization nuclear emission-line region (LINER) region of traditional diagnostic diagrams. These are galaxies hosting a weakly active galactic nucleus (wAGN) and 'retired galaxies' (RGs), i.e. galaxies that have stopped forming stars and are ionized by their hot low-mass evolved stars. A useful criterion to distinguish true from fake AGN (i.e. the RGs) is the value of ξ, which measures the ratio of the extinction-corrected Hα luminosity with respect to the Hα luminosity expected from photoionization by stellar populations older than 10 8 yr. We find that ξ follows a markedly bimodal distribution, with a ξ≫1 population composed by systems undergoing star formation and/or nuclear activity, and a peak at ξ~1 corresponding to the prediction of the RG model. We base our classification scheme not on ξ but on a more readily available and model-independent quantity which provides an excellent observational proxy for ξ: the equivalent width of Hα. Based on the bimodal distribution of W Hα , we set the practical division between wAGN and RGs at W Hα = 3 A. Five classes of galaxies are identified within the WHAN diagram: (i) pure star-forming galaxies: log[N II]/Hα 3 A; (ii) strong AGN (i.e. Seyferts): log[NII]/Hα > -0.4 and W Hα > 6A; (iii) weak AGN: log[N n]/Hα > -0.4 and W Hα between 3 and 6 A; (iv) RGs (i.e. fake AGN): W Hα < 3 A; (v) passive galaxies (actually, lineless galaxies): W Hα and W [NII] < 0.5 A. A comparative analysis of star formation histories and of other physical and observational properties in these different classes of galaxies corroborates our proposed differentiation between RGs and wAGN in the LINER-like family. This analysis also shows similarities between strong and weak AGN on the one hand, and retired and passive galaxies on the other.
Enhanced UV light detection using wavelength-shifting properties of Silicon nanoparticles

Detection of UV photons is becoming increasingly necessary with the use of noble gases and liquids in elementary particle experiments. Cerenkov light in crystals and glasses, scintillation light in neutrino, dark matter, and rare decay experiments all require sensitivity to UV photons. New sensor materials are needed that can directly detect UV photons and/or absorb UV photons and re-emit light in the visible range measurable by existing photosensors. It has been shown that silicon nanoparticles are sensitive to UV light in a wavelength range around ∼ 200 nm. UV light is absorbed and re-emitted at wavelengths in the visible range depending on the size of the nanoparticles. Initial tests of the wavelength-shifting properties of silicon nanoparticles are presented here that indicate by placing a film of nanoparticles in front of a standard visible-wavelength detecting photosensor, the response of the sensor is significantly enhanced at wavelengths < 320 nm.
Period switching in the symbiotic star BX Mon

ABSTRACT We report on a detailed analysis of the optical light curve of the symbiotic system BXMon, the data of which were gathered from the literature. The light curve covers theperiod December 1889 March 2009, with a gap of no observations between March 1940and February 1972. The light curve is characterized by strong oscillations of peak topeak amplitude of 2 to more than 3 magnitudes. Before the gap the ﬂuctuations weremodulated mainly by a period P a =1373±4 d. After the gap the dominant periodicityis P b =1256±16. Higher harmonics as well as a few beats of the two major periodicitiescan also be identiﬁed in the light curve. We identify one of the beat periods, P r =656d, as the sidereal rotation period of the giant component of the system . The periodswitching that took place during the gap in the observations was possibly associatedwith a certain cataclysmic event, hints of which may be recognized in the LC in theﬁrst 11 years after the gap.We suggest that the origin of the major oscillations is in periodic episodes of massaccretion from the M giant onto the hot component of the system. After the gap theyare correlated with the periastron passage of the system, and therefore appear withthe binary period. Before the gap the oscillations appeared with the diurnal cycle ofan observer on the surface of the rotating M giant, whose sun is the hot component.The event of the period switching is possibly related to an intensive magnetic activityin the outer layers of the giant star.Keywords: binaries: symbiotic – stars: individual: BX Mon – stars: magnetic ﬁelds– stars: rotation.
STAR FORMATION QUENCHING IN HIGH-REDSHIFT LARGE-SCALE STRUCTURE: POST-STARBURST GALAXIES IN THE Cl 1604 SUPERCLUSTER AT z ∼ 0.9

The Cl 1604 supercluster at z ∼ 0.9 is one of the most extensively studied high-redshift large-scale structures, with more than 500 spectroscopically confirmed members. It consists of eight clusters and groups, with members numbering from a dozen to nearly a hundred, providing a broad range of environments for investigating the large-scale environmental effects on galaxy evolution. Here we examine the properties of 48 post-starburst galaxies in Cl 1604, comparing them to other galaxy populations in the same supercluster. Incorporating photometry from ground-based optical and near-infrared imaging, along with Spitzer mid-infrared observations, we derive stellar masses for all Cl 1604 members. The colors and stellar masses of the K+A galaxies support the idea that they are progenitors of red sequence galaxies. Their morphologies, residual star formation rates, and spatial distributions suggest that galaxy mergers may be the principal mechanism producing post-starburst galaxies. Interaction between galaxies and the dense intracluster medium (ICM) is also effective, but only in the cores of dynamically evolved clusters. The prevalence of post-starburst galaxies in clusters correlates with the dynamical state of the host cluster, as both galaxy mergers and the dense ICM produce post-starburst galaxies. We also investigate the incompleteness and contamination of K+A samples selected by means of Hδ and [O ii] equivalent widths. K+A samples may be up to ∼50% incomplete due to the presence of LINERs/Seyferts, and up to ∼30% of K+A galaxies could have substantial star formation activity.
THE FIRST SYSTEMATIC STUDY OF TYPE Ibc SUPERNOVA MULTI-BAND LIGHT CURVES

We present detailed optical photometry for 25 Type Ibc supernovae (SNe Ibc) within d ≈ 150 Mpc obtained with the robotic Palomar 60 inch telescope in 2004–2007. This study represents the first uniform, systematic, and statistical sample of multi-band SNe Ibc light curves available to date. We correct the light curves for host galaxy extinction using a new technique based on the photometric color evolution, namely, we show that the (V − R) color of extinction-corrected SNe Ibc at Δt ≈ 10 days after V-band maximum is tightly distributed, 〈(V − R)V10〉 = 0.26 ± 0.06 mag. Using this technique, we find that SNe Ibc typically suffer from significant host galaxy extinction, 〈E(B − V)〉 ≈ 0.4 mag. A comparison of the extinction-corrected light curves for helium-rich (Type Ib) and helium-poor (Type Ic) SNe reveals that they are statistically indistinguishable, both in luminosity and decline rate. We report peak absolute magnitudes of 〈MR〉 = −17.9 ± 0.9 mag and 〈MR〉 = −18.3 ± 0.6 mag for SNe Ib and Ic, respectively. Focusing on the broad-lined (BL) SNe Ic, we find that they are more luminous than the normal SNe Ibc sample, 〈MR〉 = −19.0 ± 1.1 mag, with a probability of only 1.6% that they are drawn from the same population of explosions. By comparing the peak absolute magnitudes of SNe Ic-BL with those inferred for local engine-driven explosions (GRB-SN 1998bw, XRF-SN 2006aj, and SN 2009bb) we find a 25% probability that relativistic SNe are drawn from the overall SNe Ic-BL population. Finally, we fit analytic models to the light curves to derive typical 56Ni masses of MNi ≈ 0.2 and 0.5 M☉ for SNe Ibc and SNe Ic-BL, respectively. With reasonable assumptions for the photospheric velocities, we further extract kinetic energy and ejecta mass values of Mej ≈ 2 M☉ and EK ≈ 1051 erg for SNe Ibc, while for SNe Ic-BL we find higher values, Mej ≈ 5 M☉ and EK ≈ 1052 erg. We discuss the implications for the progenitors of SNe Ibc and their relation to those of engine-driven explosions.
The frequency of dwarf galaxy multiples at low redshift in SDSS versus cosmological expectations

We quantify the frequency of companions of low-redshift (0.013 55 arcsec, projected separations r_p 1:4) steadily increases with decreasing Primary stellar mass, whereas the cosmological “Major Merger rate” (per Gyr) has the opposite behaviour. We conclude that cosmological simulations can be reliably used to constrain the fraction of dwarf mergers across cosmic time.
Variation in the population density of the Giant African Snail (Lissachatina fulica) in the Neotropical region

The Giant African Snail (Lissachatina fulica) is one of the 100 world’s worst invasive species and has been recorded in the Neotropical region since the 1980s. Temperature and precipitation variables affect snail population density; however, these relationships have not been investigated for L. fulica on a regional scale. Here, we made the first description of variation in population density of L. fulica in the Neotropical region using a literature search, descriptive statistics, and a Principal Component Analysis (PCA). We found 22 studies covering 36 localities in six countries. The mean snail density was 11.55 ± 28.32 ind/m2, with the lowest value recorded in Cuba (0.0002 ind/m2) and the highest value recorded in Venezuela (150 ind/m2). These values were recorded between 21 % to 93 % of Human Footprint, 710 mm to 4438 mm of Annual Precipitation, 13 ºC to 27 ºC, Mean Temperature of the Coldest Quarter, and 3 ºC to 40 ºC of Temperature Seasonality. The PCA suggested that low densities can occur in various environmental conditions, whereas medium and high densities seem to appear in more specific climatic combinations. In conclusion, increased densities of Lissachatina fulica in the Neotropics seem to be influenced by climatic variations, especially the Mean Temperature of the Coldest Quarter and Annual Precipitation, supporting previous findings in the literature regarding the snail establishment. Future monitoring of this invasive species, performed at expanded spatial and temporal scales, may provide tools to establish a relationship between snail density values and impact.
Awareness of Racism Among Social Work Students in a Challenging Era

This study focused on understanding individual (e.g., political identity and alignment of social work core values with the Black Lives Matter movement and the All Lives Matter argument) and social environmental correlates (e.g., social network composition) of awareness of racism among social work students. A convenience sample of social work students (n=98) recruited from a major Midwest land grant university completed an online anonymous survey with questions covering individual characteristics, social network information, and attitudes toward social phenomena. The Color-Blind Racial Attitudes Scale was used to assess overall awareness of racism, White privilege, institutional racism, and blatant racism. Regression models were conducted to identify correlates of these domains of racial attitudes separately. Liberal political view identification and alignment of Black Lives Matter (BLM) movement with social work core values were associated with better awareness of racism across all domains; aligning All Lives Matter with social work core values was associated with unawareness of overall racism, institutional racism, and blatant racism. Finally, discussion on racial issues with network members was associated with better awareness of overall racism, White privilege, and blatant racism. Social work programs should facilitate inter-group dialogues to build consensus on countering racism. Discussions on the mission and the context of BLM and its opposition efforts should also be incorporated in the curriculum. Finally, more emphasis on the impact of institutional racism should be included into course activities to further discussion on such topics within students’ network.
DUST HEATING BY LOW-MASS STARS IN MASSIVE GALAXIES AT z < 1 ?>

Using the Hubble Space Telescope/Wide Field Camera 3 imaging data and multi-wavelength photometric catalog, we investigated the dust temperature of passively evolving and star-forming galaxies at 0.2 < z < 1.0 ? > in the CANDELS fields. We estimated the stellar radiation field by low-mass stars from the stellar mass and surface brightness profile of these galaxies and then calculated their steady-state dust temperature. At first, we tested our method using nearby early-type galaxies with the deep far-IR data by the Herschel Virgo cluster survey and confirmed that the estimated dust temperatures are consistent with the observed temperatures within the uncertainty. We then applied the method to galaxies at 0.2 < z < 1.0 ? > , and found that most passively evolving galaxies with M star > 10 10 M ⊙ ? > have relatively high dust temperatures of T dust > 20 ? > K, for which the formation efficiency of molecular hydrogen on the surface of dust grains in the diffuse ISM is expected to be very low from the laboratory experiments. The fraction of passively evolving galaxies strongly depends on the expected dust temperature at all redshifts and increases rapidly increasing temperature around T dust ∼ 20 ? > K. These results suggest that the dust heating by low-mass stars in massive galaxies plays an important role in the continuation of their passive evolution because the lack of the shielding effect of the molecular hydrogen on the UV radiation can prevent the gas cooling and formation of new stars.
On the one-way specification property and large deviations for non-transitive systems

We introduce a weaker form of the specification property, called "one-way specification property", and give several examples of non-transitive systems satisfying this property. As an application, we show that the $(-\beta)$-transformation satisfies a level-2 large deviation principle with the Lebesgue measure and the rate function is the free energy under the condition that $\beta>1$ is a Yrrap number, that is, the orbit of $1$ under the $(-\beta)$-transformation is eventually periodic.