Miracle-dz/UniFAR-FTUs huggingface dataset:
THE STELLAR HALOS OF MASSIVE ELLIPTICAL GALAXIES. III. KINEMATICS AT LARGE RADIUS

We present a two-dimensional kinematic analysis out to ∼2–5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions σ > 150 km s−1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and σ for each galaxy extending to at least 2 Re. Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re. The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a “two-phase” picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos.
The origin of the dust in high-redshift quasars: the case of SDSS J1148+5251

We present a semi-analytical model for the formation and evolution of a high-redshift quasar (QSO). We reconstruct a set of hierarchical merger histories of a 10(13)-M-circle dot dark matter halo and model the evolution of the corresponding galaxy and of its central supermassive black hole. The code GAMETE/QSODUST consistently follows (i) the black hole assembly via both coalescence with other black holes and gas accretion; (ii) the build-up and star formation history of the quasar host galaxy, driven by binary mergers and mass accretion; (iii) the evolution of gas, stars and metals in the interstellar medium (ISM), accounting for mass exchanges with the external medium (infall and outflow processes); (iv) the dust formation in supernova (SN) ejecta and in the stellar atmosphere of asymptotic giant branch (AGB) stars, dust destruction by interstellar shocks and grain growth in molecular clouds; and (v) the active galactic nucleus feedback which powers a galactic-scale wind, self-regulating the black hole growth and eventually halting star formation. We use this model to study the case of SDSS J1148+5251 observed at redshift 6.4. We explore different star formation histories for the QSO host galaxy and find that Population III stars give a negligible contribution to the final metal and dust masses due to rapid enrichment of the ISM to metallicities >Z(cr) = 10(-6)-10(-4) Z(circle dot) in progenitor galaxies at redshifts > 10. If Population II/I stars form with a standard initial mass function (IMF) and with a characteristic stellar mass of m(ch) = 0.35 M-circle dot, a final stellar mass of (1-5) x 10(11) M-circle dot is required to reproduce the observed dust mass and gas metallicity of SDSS J1148+5251. This is a factor of 3-10 higher than the stellar mass inferred from observations and would shift the QSO closer or on to the stellar bulge-black hole relation observed in the local Universe; alternatively, the observed chemical properties can be reconciled with the inferred stellar mass, assuming that Population II/I stars form according to a top-heavy IMF with m(ch) = 5M(circle dot). We find that SNe dominate the early dust enrichment and that, depending on the shape of the star formation history and on the stellar IMF, AGB stars contribute at z <8-10. Yet, a dust mass of (2-6) x 10(8) M-circle dot estimated for SDSS J1148+ 5251 cannot be reproduced considering only stellar sources, and the final dust mass is dominated by grain growth in molecular clouds. This conclusion is independent of the stellar IMF and star formation history.
The confinement of star-forming galaxies into a main sequence through episodes of gas compaction, depletion and replenishment

Using cosmological simulations, we address the properties of high-redshift star-forming galaxies (SFGs) across their main sequence (MS) in the plane of star-formation rate (SFR) versus stellar mass. We relate them to the evolution of galaxies through phases of gas compaction, depletion, possible replenishment, and eventual quenching. We find that the high-SFR galaxies in the upper envelope of the MS are compact, with high gas fractions and short depletion times ("blue nuggets"), while the lower-SFR galaxies in the lower envelope have lower central gas densities, lower gas fractions and longer depletion times, consistent with observed gradients across the MS. Stellar-structure gradients are negligible. The SFGs oscillate about the MS ridge on timescales $\sim0.4~t_{\mathrm{Hubble}}$ ($\sim1$ Gyr at $z\sim3$). The propagation upwards is due to gas compaction, triggered, e.g., by mergers, counter-rotating streams, and/or violent disc instabilities. The downturn at the upper envelope is due to central gas depletion by peak star formation and outflows while inflow from the shrunken gas disc is suppressed. An upturn at the lower envelope can occur once the extended disc has been replenished by fresh gas and a new compaction can be triggered, namely as long as the replenishment time is shorter than the depletion time. The mechanisms of gas compaction, depletion and replenishment confine the SFGs to the narrow ($\pm0.3$ dex) MS. Full quenching occurs in massive haloes ($M_{\mathrm{vir}}>10^{11.5}~M_\odot$) and/or at low redshifts ($z<3$), where the replenishment time is long compared to the depletion time, explaining the observed bending down of the MS at the massive end.
North American Glaciations and Pacific Inputs in the Nd and Sr Isotope Pleistocene Record From the Western Arctic Ocean

Enduring questions remain regarding the transition from relatively warm and stable pre‐ and early‐Pleistocene climate to that of the high amplitude glacial‐interglacial cycles later in the Quaternary. The main shift in glacial intensity and periodicity around 1 Ma is known as the Mid‐Pleistocene Transition (MPT). Here we analyze detrital strontium (Sr) and neodymium (Nd) isotopes in a western Arctic sediment core P23 previously investigated using several litho/biostratigraphic proxies. Based on an improved age framework combining lithostratigraphic cyclicity and Sr isotope stratigraphy, the P23 record extends to ∼3.3 Ma, thus providing a rare insight into the Quaternary Arctic climate change. The distinct pre‐MPT P23 record is dominated by Pacific‐sourced sediment inputs, with little to no intra‐Arctic glacial inputs, except for a sandy interval around ∼2.5 Ma. A consistent decrease of Nd isotopic values toward North American continental signatures started in both the Arctic and Bering Sea at ∼1.5 Ma and led to a major threshold shift in P23 proxies at ∼0.9 Ma. We argue that this threshold was associated with the first prolonged closure of the Bering Strait for an entire obliquity cycle. This shift marked the expansion of the North American ice sheets to the Arctic margin, with dramatic impacts on depositional and hydrographic environments in the Arctic Ocean. These impacts intensified in the subsequent glacial intervals indicating further ice‐sheet growth, probably fed back by continuing prolonged Bering Strait closures.
IONIZED GAS KINEMATICS AT HIGH RESOLUTION. V. [Ne ii], MULTIPLE CLUSTERS, HIGH EFFICIENCY STAR FORMATION, AND BLUE FLOWS IN HE 2–10

We measured the 12.8 μm [Ne ii] line in the dwarf starburst galaxy He 2–10 with the high-resolution spectrometer TEXES on the NASA IRTF. The data cube has a diffraction-limited spatial resolution of ∼1″ and a total velocity resolution, including thermal broadening, of ∼5 km s−1. This makes it possible to compare the kinematics of individual star-forming clumps and molecular clouds in the three dimensions of space and velocity, and allows us to determine star formation efficiencies. The kinematics of the ionized gas confirm that the starburst contains multiple dense clusters. From the M/R of the clusters and the ≃30%–40% star formation efficiencies, the clusters are likely to be bound and long lived, like globulars. Non-gravitational features in the line profiles show how the ionized gas flows through the ambient molecular material, as well as a narrow velocity feature, which we identify with the interface of the H ii region and a cold dense clump. These data offer an unprecedented view of the interaction of embedded H ii regions with their environment.
Effects of Fruiting on Net Photosynthesis and Dark Respiration of ‘Hecker’ Strawberries1

During a 6-week fruiting cycle of a day-neutral strawberry, (Fragaria × ananassa Duch. cv. Hecker), net photosynthesis (Pn) was significantly greater on fruiting plants than deblossomed plants on 5 of 6 measurement dates. The presence of fruit did not affect dark respiration (Rd). Pn tended to decline during the fruiting cycle while Rd tended to increase. Removal of inflorescences from fruiting plants resulted in a significant decline in Pn while Rd was unaffected.
Notch1-Jagged1 Signaling Pathway in Oral Squamous Cell Carcinoma: Relation to Tumor Recurrence and Patient Survival

BACKGROUND: Dysregulated Jagged1/Notch1 signaling has been implicated in a variety of carcinomas, but little is known about the expression and possible role of Jagged1 and Notch1 in patients with oral squamous cell carcinoma (OSCC). AIM: We set out to examine the clinical significance of Notch1 and Jagged1 expression in OSCC. METHODS: Specimens were obtained from 44 patients who underwent surgical resection of primary OSCC. Immunostaining was done for Notch1 and Jagged1. The utilized markers’ expressions were analyzed in respect to 3 years overall survival (OS) and disease-free survival (DFS). RESULTS: Poor prognosis was significantly associated with high Notch1 expression, high Jagged1 expression, advanced TNM clinical stage (III and IV), presence of distant metastasis, presence of nodal involvement, large-sized tumors (≥4 cm), presence of lymphovascular invasion, higher grade carcinomas, high Notch1 and Jagged1 coexpression, and carcinomas aroused from tongue and palate. Notch1, Jagged1, histologic grade, and tumor site were the independent predictors of DFS, while Jagged1 expression, histologic grade, and tumor site were the independent predictors of 3 years OS. CONCLUSION: Our findings imply that either high levels of Notch1 or Jagged1 expression, or combined combination of both are related with poor prognostic outcomes.
A Density-based Clustering Approach to detect Colluding SSDF Attackers in Cognitive Radio Networks

Among the many attacks that Cognitive Radio Networks (CRN) are vulnerable to, Spectrum Sensing Data Falsification (SSDF) attack is one of the most common attacks. The current work focusses on an advanced form of SSDF attacks, called Colluding SSDF attack. The colluding attack is a collaborative well-planned and well-timed attack where a leader instructs the other attackers when and how to attack a CRN during sensing period. Needless to say, Colluding SSDF attacks are harder to detect and thus, they are more harmful. To detect this attack, we have proposed a technique based on Density-Based Spatial Clustering of Applications with Noise (DBSCAN) [1]. The density-based clustering technique separates the high-density clusters (normal SUs) from low-density clusters (attackers). Simulation results demonstrate the effectiveness of the proposed when the percentage of attackers is less than 50%. Additionally, a performance comparison of the proposed method has been done with an existing work, agglomerative clustering detection algorithm (ACD)[2].
Assessment and comparison of nutritional status of government and private school children of Muzaffarnagar city

Background: Malnutrition leads to poor cognitive performance and physical growth in children and is a major component of school health services. Imbalanced nutrition in adolescence can put them at high risk of chronic diseases particularly if combined with adverse lifestyle. Objective: This study was designed to assess and compare the nutritional status of government and private school children of Muzaffarnagar city. Material and Methods: School based, comparative Cross-sectional study. One private and one government school was selected using unistage stratified random sampling. A total of 1960 (980 each from private school and government school) school children of class 6-12 were studied for socio-epidemiological details, dietary habits, and physical activity. Information on education status, occupation, monthly income of their parents was also collected. Required anthropometric measurements were taken. Results: Of 980 children from private school, 90 (9.18%) were underweight,138 (14.08%) were overweight, and 137 (13.97%) were obese. Majority of children from government school were underweight 215 (21.94%) except for 24 (2.45%) overweight children. Conclusion: This study shows the dual nature of nutritional problem, under-nutrition among the lower socioeconomic class of govt. school at one side and worrisome epidemic of obesity among the affluent of private school.
Quasielectrons as inverse quasiholes in lattice fractional quantum Hall models

From an experimental point of view, quasielectrons and quasiholes play very similar roles in the fractional quantum Hall effect. Nevertheless, the theoretical description of quasielectrons is known to be much harder than that of quasiholes. The problem is that one obtains a singularity in the wavefunction if one tries to naively construct the quasielectron as the inverse of the quasihole. Here, we demonstrate that the same problem does not arise in lattice fractional quantum Hall models. This result allows us to make detailed investigations of the properties of quasielectrons, including their braiding statistics and density distribution on lattices on the plane and on the torus. We show that some of the states considered have high overlap with certain fractional Chern insulator states. We also derive few-body Hamiltonians, for which various states containing quasielectrons are exact ground states.
X-ray spectral properties of Seyfert galaxies and the unification scheme

Aims: The unification scheme of Seyfert galaxies predicts that the observed differences between type 1 and type 2 Seyfert galaxies are solely due to the differing orientations of the toroidal-shaped obscuring material around AGN. The observed X-ray spectra of Seyfert type 2s compared to type 1s are expected to be affected by higher absorbing column density due to the edge-on view of the obscuring torus. We study the 0.5 - 10 keV X-ray spectral properties of Seyfert type 1s and type 2s with the aim to test the predictions of Seyfert unification scheme in the X-ray regime. Methods: We use an optically selected Seyfert sample in which type 1s and type 2s have matched distributions in the orientation independent parameters of AGN and host galaxy. Results: The 0.5 - 10 keV XMM-Newton pn X-ray spectra of Seyfert galaxies are in general best fitted with a model consists of an absorbed power-law, a narrow Gaussian fitted to the Fe K{\alpha} emission line and an often seen soft excess component characterized by either a thermal plasma model with temperature kT \sim 0.1 - 1.0 keV and/or a steep power-law. The 2.0 - 10 keV hard X-ray continuum emission in several Seyfert type 2s is reflection dominated and suggests the Compton-thick obscuration. Results on the statistical comparison of the distributions of the observed X-ray luminosities in the soft (0.5 - 2.0 keV) and hard (2.0 - 10.0 keV) bands, the X-ray absorbing column densities, the equivalent widths of Fe K{\alpha} line and the flux ratios of hard X-ray to [OIII] {\lambda}5007{\AA} for the two Seyfert subtypes are consistent with the obscuration and orientation based unification scheme.
Diagnostic Accuracy of Direct Immunofluorescence Test on Paraffin-Embedded Blocks in Comparison with Frozen Section Blocks in Renal Biopsies

Background In several published research, the evaluation of renal disorders using immunofluorescence on formalin-fixed, paraffin-embedded (FFPE) tissue sections versus immunofluorescence on frozen sections was compared. Each technique's accuracy varies greatly. This study's objective was to assess IF-P as a potential replacement for IF-F in the diagnosis of renal biopsy specimens. Materials and Methods To show immunoglobulin IgA, IgG, IgM, and C3 immune deposits, proteinase K digestion of paraffin-embedded renal biopsy was standardized and used in 51 renal biopsies. Sensitivity, specificity, false-positive, and false-negative values were calculated. Results IF-P showed a sensitivity of 93.1%, 76.9%, 63.6%, and 33.3%, and a specificity of 100%, 97.3%, 95%, and 100% for IgG, IgA, IgM, and C3, respectively. Compared to cases that had both routine IF and IF-P, 50 of 51 showed either the same amount of staining for the diagnostic immunoglobulin/complement or a small amount of difference. In most of the cases (49 of 51), diagnostic findings were found. Conclusion IF-P is a sensitive and precise approach for assessing immune deposits in renal tissue biopsies. We come to the conclusion that IF-P serves as a beneficial salvage immunohistochemistry method for renal biopsies that do not contain enough cortical tissue for IF-F.
INTRACLUSTER MEDIUM REHEATING BY RELATIVISTIC JETS

Galactic jets are powerful energy sources reheating the intracluster medium in galaxy clusters. Their crucial role in the cosmic puzzle, motivated by observations, has been established by a great number of numerical simulations excluding the relativistic nature of these jets. We present the first relativistic simulations of the very long-term evolution of realistic galactic jets. Unexpectedly, our results show no buoyant bubbles, but large cocoon regions compatible with the observed X-ray cavities. The reheating is more efficient and faster than in previous scenarios, and it is produced by the shock wave driven by the jet, that survives for several hundreds of Myr. Therefore, the X-ray cavities in clusters produced by powerful relativistic jets would remain confined by weak shocks for extremely long periods and their detection could be an observational challenge.
Observational constraint on the varying speed of light theory

The varying speed of light (VSL) theory is controversial. It succeeds in explaining some cosmological problems, but on the other hand it is excluded by mainstream physics because it will shake the foundation of physics. In the present paper, we devote ourselves to test whether the speed of light is varying from the observational data of the type Ia Supernova, Baryon Acoustic Oscillation, Observational $H(z)$ data and Cosmic Microwave Background (CMB). We select the common form $c(t)=c_0a^n(t)$ with the contribution of dark energy and matter, where $c_0$ is the current value of speed of light, $n$ is a constant, and consequently construct a varying speed of light dark energy model (VSLDE). The combined observational data show a much trivial constraint $n=-0.0033 \pm 0.0045$ at 68.3\% confidence level, which indicates that the speed of light may be a constant with high significance. By reconstructing the time-variable $c(t)$, we find that the speed of light almost has no variation for redshift $z < 10^{-1}$. For high-$z$ observations, they are more sensitive to the VSLDE model, but the variation of speed of light is only in order of $10^{-2}$. We also introduce the geometrical diagnostic $Om (z)$ to show the difference between the VSLDE and $\Lambda$CDM model. The result shows that the current data are difficult to differentiate them. All the results show that the observational data favor the constant speed of light.
Flowering and Fruiting of Chinese Jujubes in Florida

Eighteen cultivars of the Chinese jujube (Zizyphus jujuba Mill.) grown in Florida comprised 2 flowering types based on the time of day when the flowers open. Flowers on 10 cultivars open each day between 0700 and 1000 hr and on the other 8 between 1400 and 1700 hr. Despite ample opportunity for cross-pollination and intense activity by pollinating insects, some cultivars set little or no fruit. Cultivars that fruit heavily and reliably are parthenocarpic. Supplemental light in the fall prolongs flowering and fruiting and could substantially increase yields.
Statistics of cosmic density profiles from perturbation theory

The joint probability distribution function (PDF) of the density within multiple concentric spherical cells is considered. It is shown how its cumulant generating function can be obtained at tree order in perturbation theory as the Legendre transform of a function directly built in terms of the initial moments. In the context of the upcoming generation of large-scale structure surveys, it is conjectured that this result correctly models such a function for finite values of the variance. Detailed consequences of this assumption are explored. In particular the corresponding one-cell density probability distribution at finite variance is computed for realistic power spectra, taking into account its scale variation. It is found to be in agreement with $\Lambda$-CDM simulations at the few percent level for a wide range of density values and parameters. Related explicit analytic expansions at the low and high density tails are given. The conditional (at fixed density) and marginal probability of the slope -- the density difference between adjacent cells -- and its fluctuations is also computed from the two-cells joint PDF; it also compares very well to simulations, in particular in under-dense regions, with a significant reduced cosmic scatter compared to over-dense regions. It is emphasized that this could prove useful when studying the statistical properties of voids as it can serve as a statistical indicator to test gravity models and/or probe key cosmological parameters.
KamLAND-Experiment and Soliton-Like Nuclear Georeactor. Part 1. Comparison of Theory with Experiment

We give an alternative description of the data produced in the KamLAND experiment, assuming the existence of a natural nuclear reactor on the boundary of the liquid and solid phases of the Earth core. Analyzing the uncertainty of antineutrino spectrum of georeactor origin, we show that the theoretical (which takes into account the soliton-like nuclear georeactor) total reactor antineutrino spectra describe with good accuracy the experimental KamLAND-data over the years of 2002-2007 and 2002-2009, respectively. At the same time, the parameters of mixing (△m221=2.5×10-5 eV2, tan2θ12=0.437) calculated within the framework of georeactor hypothesis substantially differ from the parameters of mixing ((△m221=7.49×10-5 eV2, tan2θ12=0.436) obtained in KamLAND-experiment for total exposure over the period of 2002-2009. By triangulation of KamLAND and Borexino data we have constructed the coordinate location of soliton-like nuclear georeactors on the boundary of the liquid and solid phases of the Earth core.