Miracle-dz/UniFAR-FTUs huggingface dataset:
RELATIVISTIC JETS IN THE RADIO REFERENCE FRAME IMAGE DATABASE. II. BLAZAR JET ACCELERATIONS FROM THE FIRST 10 YEARS OF DATA (1994–2003)

We analyze blazar jet apparent speeds and accelerations from the RDV series of astrometric and geodetic very long baseline interferometry (VLBI) experiments. From these experiments, we have produced and analyzed 2753 global VLBI images of 68 sources at 8 GHz with a median beam size of 0.9 milliarcseconds (mas) and a median of 43 epochs per source. From this sample, we analyze the motions of 225 jet components in 66 sources. The distribution of the fastest measured apparent speed in each source has a median of 8.3c and a maximum of 44c. Sources in the 2FGL Fermi LAT catalog display higher apparent speeds than those that have not been detected. On average, components farther from the core in a given source have significantly higher apparent speeds than components closer to the core; for example, for a typical source, components at ∼3 mas from the core (∼15 pc projected at z ∼ 0.5) have apparent speeds about 50% higher than those of components at ∼1 mas from the core (∼5 pc projected at z ∼ 0.5). We measure accelerations of components in orthogonal directions parallel and perpendicular to their average velocity vector. Parallel accelerations have significantly larger magnitudes than perpendicular accelerations, implying that observed accelerations are predominantly due to changes in the Lorentz factor (bulk or pattern) rather than projection effects from jet bending. Positive parallel accelerations are significantly more common than negative ones, so the Lorentz factor (bulk or pattern) tends to increase on the scales observed here. Observed parallel accelerations correspond to modest source frame increases in the bulk or pattern Lorentz factor.
How Many Radio-loud Quasars Can Be Detected by the Gamma-Ray Large Area Space Telescope?

In the unification scheme, radio quasars and FR II radio galaxies come from the same parent population, but viewed at different angles. Based on the Comptonization models for the γ-ray emission from active galactic nuclei (AGNs), we estimate the number of radio quasars and FR II radio galaxies to be detected by the Gamma-Ray Large Area Space Telescope (GLAST) using the luminosity function (LF) of their parent population derived from the flat-spectrum radio quasar (FSRQ) LF. We find that ~1200 radio quasars will be detected by GLAST, if the soft seed photons for Comptonization come from the regions outside the jets. We also consider the synchrotron self-Comptonization (SSC) model, and find it unlikely to be responsible for γ-ray emission from radio quasars. We find that no FR II radio galaxies will be detected by GLAST. Our results show that most radio AGNs to be detected by GLAST will be FSRQs (~99% for the external Comptonization [EC] model), while the remainder (~1%) will be steep-spectrum radio quasars (SSRQs). This implies that FSRQs will still be good candidates for identifying γ-ray AGNs even for the GLAST sources. The contribution of all radio quasars and FR II radio galaxies to the extragalactic γ-ray background (EGRB) is calculated, which accounts for ~30% of the EGRB.
A DIRECT MEASUREMENT OF THE HEAT RELEASE IN THE OUTER CRUST OF THE TRANSIENTLY ACCRETING NEUTRON STAR XTE J1709−267

The heating and cooling of transiently accreting neutron stars provides a powerful probe of the structure and composition of their crust. Observations of superbursts and cooling of accretion-heated neutron stars require more heat release than is accounted for in current models. Obtaining firm constraints on the depth and magnitude of this extra heat is challenging and therefore its origin remains uncertain. We report on Swift and XMM-Newton observations of the transient neutron star low-mass X-ray binary XTE J1709−267, which were made in 2012 September–October when it transitioned to quiescence after a ≃10 week long accretion outburst. The source is detected with XMM-Newton at a 0.5–10 keV luminosity of LX ≃ 2 × 1034(D/8.5 kpc)2 erg s−1. The X-ray spectrum consists of a thermal component that fits to a neutron star atmosphere model and a non-thermal emission tail, each of which contribute ≃50% to the total flux. The neutron star temperature decreases from ≃158 to ≃152 eV during the ≃8 hr long observation. This can be interpreted as cooling of a crustal layer located at a column density of y ≃ 5 × 1012 g cm−2 (≃50 m inside the neutron star), which is just below the ignition depth of superbursts. The required heat generation in the layers on top would be ≃0.06–0.13 MeV per accreted nucleon. The magnitude and depth rule out electron captures and nuclear fusion reactions as the heat source, but it may be accounted for by chemical separation of light and heavy nuclei. Low-level accretion offers an alternative explanation for the observed variability.
Madelung energy of the valence-skipping compound Ba Bi O 3

Several elements show valence skip fluctuation, for instance, Tl forms the compounds in valence states $+1$ and $+3$ and Bi forms in $+3$ and $+5$ states. This kind of fluctuation gives rise to a negative effective attractive interaction and the Kondo effect. In the compounds of valence-skipping elements, the carrier doping will induce superconductivity with high critical temperature. For example, ${\mathrm{Ba}}_{1\ensuremath{-}x}{\mathrm{K}}_{x}\mathrm{Bi}{\mathrm{O}}_{3}$ shows high ${T}_{c}$ which is unlikely from the conventional electron-phonon mechanism. The reason for missing of some valence states in such valence skip compounds remains a mystery. We have performed the evaluation of the Madelung potential for $\mathrm{Ba}\mathrm{Bi}{\mathrm{O}}_{3}$ and have shown that the charge-ordered state is stabilized if we take into account the polarization of the oxygen charge. We argue that the effective Coulomb interaction energy $U$ may be negative evaluating the local excitation energy.
WHERE ARE MOST OF THE GLOBULAR CLUSTERS IN TODAY’S UNIVERSE?

The total number of globular clusters (GCs) in a galaxy rises continuously with the galaxy luminosity L, while the relative number of galaxies decreases with L following the Schechter function. The product of these two very nonlinear functions gives the relative number of GCs contained by all galaxies at a given L. It is shown that GCs, in this universal sense, are most commonly found in galaxies within a narrow range around L⋆. In addition, blue (metal-poor) GCs outnumber the red (metal-richer) ones globally by 4 to 1 when all galaxies are added, pointing to the conclusion that the earliest stages of galaxy formation were especially favorable to forming massive, dense star clusters.
The relationship between the morphology and kinematics of galaxies and its dependence on dark matter halo structure in EAGLE

We investigate the connection between the morphology and internal kinematics of the stellar component of central galaxies with mass M⋆ > 109.5 M⊙ in the EAGLE simulations. We compare several kinematic diagnostics commonly used to describe simulated galaxies, and find good consistency between them. We model the structure of galaxies as ellipsoids and quantify their morphology via the ratios of their principal axes. We show that the differentiation of blue star-forming and red quiescent galaxies using morphological diagnostics can be achieved with similar efficacy to the use of kinematical diagnostics, but only if one is able to measure both the flattening and the triaxiality of the galaxy. Flattened oblate galaxies exhibit greater rotational support than their spheroidal counterparts, but there is significant scatter in the relationship between morphological and kinematical diagnostics, such that kinematically-similar galaxies can exhibit a broad range of morphologies. The scatter in the relationship between the flattening and the ratio of the rotation and dispersion velocities (v/σ) correlates strongly with the anisotropy of the stellar velocity dispersion: at fixed v/σ, flatter galaxies exhibit greater dispersion in the plane defined by the intermediate and major axes than along the minor axis, indicating that the morphology of simulated galaxies is influenced significantly by the structure of their velocity dispersion. The simulations reveal that this anisotropy correlates with the intrinsic morphology of the galaxy’s inner dark matter halo, i.e. the halo’s morphology that emerges in the absence of dissipative baryonic physics. This implies the existence of a causal relationship between the morphologies of galaxies and that of their host dark matter haloes.
Nursing Staff Perspectives Regarding Career Plateau Management Strategies and its Relation to Job Satisfaction

Background: Career plateau is a significant decisive factor that led to negative work outcomes as decrease in job satisfaction and increase nursing staff turnover intentions when continuing to work in the same job over a long period. Aim: to assess nursing staff perspective regarding career plateau management strategies and their relation to job satisfaction. Subjects and Method: Setting: This study was conducted at Tanta University Main, Emergency, and International Teaching Hospitals. Subjects: consisted of a representative sample (n= 263) of Baccalaureate nursing staff who have more than three years of experience. Tools: two tools were used. Nurses’ career plateau management structured questionnaire and nursing staff satisfaction structured questionnaire. Results: 63% of nursing staff had moderate and high levels of career plateau. 65.0% of nursing staff had moderate double plateau. 46.4% and 43.0% of them had moderate content and structural plateau respectively and 41.1% of them had low professional plateau. 55.5% of nursing staff had high defense, 53.2% of them had moderate reevaluation management strategy and 53.2%of them had low transition management strategy.81. 7% of nursing staff were unsatisfied with their job. Conclusions: There were no statistically significant difference among Main, Emergency, and international Teaching Hospitals according to levels of career plateau. There was a statistically significant negative correlation between total nursing staff career plateau and their total job satisfaction . Recommendations: Be on the lookout for early signs of plateauing and take preventive measures such as upgrading skills, diversifying interests, and making long-term career plans. Develop a clear job description and road map for career advancement of nursing staff to reduce career plateauing.
EVOLUTION OF GROUP GALAXIES FROM THE FIRST RED-SEQUENCE CLUSTER SURVEY

We study the evolution of the red-galaxy fraction (fred) in 905 galaxy groups with 0.15 ⩽ z < 0.52. The galaxy groups are identified by the “probability friends-of-friends” algorithm from the first Red-Sequence Cluster Survey (RCS1) photometric-redshift sample. There is a high degree of uniformity in the properties of the red sequence of the group galaxies, indicating that the luminous red-sequence galaxies in the groups are already in place by z ∼ 0.5 and that they have a formation epoch of z ≳ 2. In general, groups at lower redshifts exhibit larger fred than those at higher redshifts, showing a group Butcher–Oemler effect. We investigate the evolution of fred by examining its dependence on four parameters, one of which can be classified as intrinsic and three of which can be classified as environmental: galaxy stellar mass (M*), total group stellar mass (M*, grp, a proxy for group halo mass), normalized group-centric radius (rgrp), and local galaxy density (Σ5). We find that M* is the dominant parameter such that there is a strong correlation between fred and galaxy stellar mass. Furthermore, the dependence of fred on the environmental parameters is also a strong function of M*. Massive galaxies (M* ≳ 1011 M☉) show little dependence of fred on rgrp, M*, grp, and Σ5 over the redshift range. The dependence of fred on these parameters is primarily seen for galaxies with lower masses, especially for M* ≲ 1010.6 M☉. We observe an apparent “group down-sizing” effect, in that galaxies in lower-mass halos, after controlling for galaxy stellar mass, have lower fred. We find a dependence of fred on both rgrp and Σ5 after the other parameters are controlled. At a fixed rgrp, there is a significant dependence of fred on Σ5, while rgrp gradients of fred are seen for galaxies in similar Σ5 regions. This indicates that galaxy group environment has a residual effect over that of local galaxy density (or vice versa), and both parameters need to be considered. This result suggests that processes identified with local galaxy density, such as galaxy harassment and mergers, and those associated with accretion into a larger group halo, such as ram pressure and strangulation, are both partaking in driving galaxies to their final red quiescent state. We discuss these results in the context of the “nature versus nurture” scenario of galaxy evolution.
A DYNAMICALLY DRIVEN, UNIVERSAL THERMAL PROFILE OF GALAXY GROUPS AND CLUSTERS

Large scale structures such as groups and clusters of galaxies show a universal, nearly linear entropy radial profile K(r). Using deprojected 16 clusters and 12 groups from the literature, we find that K ∝ r 0.96 ± 0.01 ? > , consistent with the mean power-law index (0.9–1.1) of previous studies. A similarly good fit is given by a τ ∝ r 0.72 ± 0.01 ? > ratio between cooling and free-fall times. Both profiles slightly flatten at small radii, as τ becomes of order unity. The entropy profile is usually attributed to self-similar shock accretion (shown to be inconsistent with the data), to non-standard heat conduction, or to turbulent heating. We argue that a dynamical mechanism is needed to sustain such a universal profile, oblivious to the temperature peak at the edge of the core and to the virial shock at the outskirts, and robust to the presence of ongoing cooling, merger, and active galactic nucleus activity. In particular, we show that such a profile can be naturally obtained in a spiral flow, which is likely to underlie most galaxy aggregates according to the ubiquitous spiral patterns and cold fronts observed. Generalizing a two-phase spiral flow model out to the virial radius surprisingly reproduces the thermal profile. A generalized Schwarzschild criterion indicates that observed spiral patterns must involve a convective layer, which may regulate the thermal profile.
Renormalization of high-energy Lorentz-violating QED

We study a QED extension that is unitary, CPT invariant, and super-renormalizable, but violates Lorentz symmetry at high energies, and contains higher-dimension operators (LVQED). Divergent diagrams are only one- and two-loop. We compute the one-loop renormalizations at high and low energies and analyze the relation between them. It emerges that the powerlike divergences of the low-energy theory are multiplied by arbitrary constants, inherited by the high-energy theory, and therefore can be set to zero at no cost, bypassing the hierarchy problem.
ON THE ORIGIN OF C4H AND CH3OH IN PROTOSTELLAR ENVELOPES

The formation pathways of different types of organic molecules in protostellar envelopes and other regions of star formation are subjects of intense current interest. We present here observations of C4H and CH3OH, tracing two distinct groups of interstellar organic molecules, toward 16 protostars in the Ophiuchus and Corona Australis molecular clouds. Together with observations in the literature, we present C4H and CH3OH data from single-dish observations of 40 embedded protostars. We find no correlation between the C4H and CH3OH column densities in this large sample. Based on this lack of correlation, a difference in line profiles between C4H and CH3OH, and previous interferometric observations of similar sources, we propose that the emission from these two molecules is spatially separated, with the CH3OH tracing gas that has been transiently heated to high (∼70–100 K) temperatures and the C4H tracing the cooler large-scale envelope where CH4 molecules have been liberated from ices. These results provide insight in the differentiation between hot corino and warm carbon-chain chemistry in embedded protostars.
Do we expect to detect electromagnetic radiation from merging stellar mass black binaries like GW150914? No

Context. The LIGO consortium announced the first direct detection of g ravitation wave event GW150914 from two merging black holes; however the nature of the black holes are still not cle ar. Aims. We study whether electromagnetic radiation can be detected from merging stellar mass black binaries like GW150914. Methods. We briefly investigate the possible growth and merging proce sses of the two stellar mass black holes in the merging event of GW150914 detected by aLIGO, as clocked by a distant external observer. Results. Our main results are: (1) The description of the black hole growth using stationary metric of a pre-existing black hole pre- dicts strong electromagnetic radiation from merging black holes, which is inconsistent with GW150914; (2) Only gravitational wave radiation can be produced in the coalescence of two black holes such as that in the GW150914 event, if the black hole growth is described using time-dependent metric considering the infl uence of the in-falling matter onto a pre-existing black hol e, as clocked by a distant external observer. Conclusions. Future high sensitivity detections of gravitational waves from merging black holes might be used to probe matter dis- tribution and space-time geometry in the vicinity of the horizon. Perhaps the GW150914-like events can be identified wit h traditional astronomy observations only if the black holes are embedded in extremely dense medium before their final merge, when very strong electromagnetic radiation is produced and can escape from the system.
Effect of Different Ratios of Cow Manure and Chemical Fertilizers on Fruit Quality of Gala Apples

Nutrient patterns can significantly influence the growth and development of fruit trees, especially fruit quality. In order to clarify the appropriate ratio of inorganic and organic fertilizers, six treatments with different ratios of cow manure and chemical fertilizers were set up in this study to evaluate the effects of different treatments on fruit yield, appearance quality, intrinsic quality and volatile substances. The results showed that, after replacing some chemical fertilizers with cow manure, the content of sugar, titratable acid, organic acid and aroma substance in the fruit increased, the fruit yield and colour did not change significantly, and the fruit weight per fruit decreased. Among the treatments of cow manure with chemical fertilizer, the fruits of 50% chemical fertilizer with 50% cow manure treatment had higher titratable acid (0.4%), malic acid (4.15 mg/g), sorbitol (0.51%), glucose (1.30%), fructose (5.81%) content and total aroma substance content (1047.82 μg/g) than chemical fertilizer alone. Compared to the fertilizer treatment alone, the application of cow manure instead of 50% of the chemical fertilizer had a positive effect on fruit quality.
Gas kinematics and excitation in the filamentary IRDC G035.39-00.33

Some theories of dense molecular cloud formation involve dynamical environments driven by converging atomic flows or collisions between preexisting molecular clouds. The determination of the dynamics and physical conditions of the gas in clouds at the early stages of their evolution is essential to establish the dynamical imprints of such collisions, and to infer the processes involved in their formation. We present multi-transition 13CO and C18O maps toward the IRDC G035.39-00.33, believed to be at the earliest stages of evolution. The 13CO and C18O gas is distributed in three filaments (Filaments 1, 2 and 3), where the most massive cores are preferentially found at the intersecting regions between them. The filaments have a similar kinematic structure with smooth velocity gradients of ~0.4-0.8 km s-1 pc-1. Several scenarios are proposed to explain these gradients, including cloud rotation, gas accretion along the filaments, global gravitational collapse, and unresolved sub-filament structures. These results are complemented by HCO+, HNC, H13CO+ and HN13C single-pointing data to search for gas infall signatures. The 13CO and C18O gas motions are supersonic across G035.39-00.33, with the emission showing broader linewidths toward the edges of the IRDC. This could be due to energy dissipation at the densest regions in the cloud. The average H2 densities are ~5000-7000 cm-3, with Filaments 2 and 3 being denser and more massive than Filament 1. The C18O data unveils three regions with high CO depletion factors (f_D~5-12), similar to those found in massive starless cores.
Four phases of angular-momentum buildup in high-z galaxies: from cosmic-web streams through an extended ring to disc and bulge

We study the angular-momentum (AM) buildup in high-$z$ massive galaxies using high-resolution cosmological simulations. The AM originates in co-planar streams of cold gas and merging galaxies tracing cosmic-web filaments, and it undergoes four phases of evolution. (I) Outside the halo virial radius ($R_{\rm v}\! \sim\! 100\,{\rm kpc}$), the elongated streams gain AM by tidal torques with a specific AM (sAM) $\sim\! 1.7$ times the dark-matter (DM) spin due to the gas' higher quadrupole moment. This AM is expressed as stream impact parameters, from $\sim\! 0. 3R_{\rm v}$ to counter rotation. (II) In the outer halo, while the incoming DM mixes with the existing halo of lower sAM to a spin $\lambda_{\rm dm}\! \sim\! 0.04$, the cold streams transport the AM to the inner halo such that their spin in the halo is $\sim\! 3\lambda_{\rm dm}$. (III) Near pericenter, the streams dissipate into an irregular rotating ring extending to $\sim\! 0. 3R_{\rm v}$ and tilted relative to the inner disc. Torques exerted partly by the disc make the ring gas lose AM, spiral in, and settle into the disc within one orbit. The ring is observable with 30\% probability as a damped Lyman-$\alpha$ absorber. (IV) Within the disc, $<\! 0. 1R_{\rm v}$, torques associated with violent disc instability drive AM out and baryons into a central bulge, while outflows remove low-spin gas, introducing certain sensitivity to feedback strength. Despite the different AM histories of gas and DM, the disc spin is comparable to the DM-halo spin. Counter rotation can strongly affect disc evolution.
Demystifying the coronal-line region of active galactic nuclei: spatially resolved spectroscopy with the Hubble Space Telescope

We present an analysis of Space Telescope Imaging Spectrograph (STIS)/Hubble Space Telescope optical spectra of a sample of 10 Seyfert galaxies aimed at studying the structure and physical properties of the coronal-line region (CLR). The high spatial resolution provided by STIS allowed us to resolve the CLR and obtain key information about the kinematics of the CL gas, measure directly its spatial scale, and study the mechanisms that drive the high-ionization lines. We find CLRs extending from just a few parsecs (∼10 pc) up to 230 pc in radius, consistent with the bulk of the coronal lines (CLs) originating between the broad-line region and narrow-line region (NLR), and extending into the NLR in the case of [Fe VII] and [Ne V] lines. The CL profiles strongly vary with the distance to the nucleus. We observed line splitting in the core of some of the galaxies. Line peak shifts, both redshift and blueshift, typically reached 500 km s −1 , and even higher velocities (1000 km s −1 )i n some of the galaxies. In general, CLs follow the same pattern of rotation curves as low-ionization lines like [O III]. From a direct comparison between the radio and the CL emission we find that neither the strength nor the kinematics of the CLs scales in any obvious and strong way with the radio jets. Moreover, the similarity of the flux distributions and kinematics of the CLs and low-ionization lines, the low temperatures derived for the gas, and the success of photoionization models to reproduce, within a factor of a few, the observed line ratios, point towards photoionization as the main driving mechanism of CLs.