Miracle-dz/UniFAR-FTUs huggingface dataset:
Radio-mode feedback in local AGNs: dependence on the central black hole parameters

Radio mode feedback, in which most of the energy of an active galactic nucleus (AGN) is released in a kinetic form via radio-emitting jets, is thought to play an important role in the maintenance of massive galaxies in the present-day Universe. We study the link between radio emission and the properties of the central black hole in a large sample of local radio galaxies drawn from the Sloan Digital Sky Survey (SDSS), based on the catalogue of Best and Heckman (2012). Our sample is mainly dominated by massive black holes (mostly in the range $10^8-10^9 M_{\odot}$) accreting at very low Eddington ratios (typically $\lambda < 0.01$). In broad agreement with previously reported trends, we find that radio galaxies are preferentially associated with the more massive black holes, and that the radio loudness parameter seems to increase with decreasing Eddington ratio. We compare our results with previous studies in the literature, noting potential biases. The majority of the local radio galaxies in our sample are currently in a radiatively inefficient accretion regime, where kinetic feedback dominates over radiative feedback. We discuss possible physical interpretations of the observed trends in the context of a two-stage feedback process involving a transition in the underlying accretion modes.
THE CANADA–FRANCE HIGH-z QUASAR SURVEY: NINE NEW QUASARS AND THE LUMINOSITY FUNCTION AT REDSHIFT 6

We present discovery imaging and spectroscopy for nine new z ∼ 6 quasars found in the Canada–France High-z Quasar Survey (CFHQS) bringing the total number of CFHQS quasars to 19. By combining the CFHQS with the more luminous Sloan Digital Sky Survey sample, we are able to derive the quasar luminosity function from a sample of 40 quasars at redshifts 5.74 < z < 6.42. Our binned luminosity function shows a slightly lower normalization and flatter slope than found in previous work. The binned data also suggest a break in the luminosity function at M1450 ≈ −25. A double power-law maximum likelihood fit to the data is consistent with the binned results. The luminosity function is strongly constrained (1σ uncertainty <0.1 dex) over the range −27.5 < M1450 < −24.7. The best-fit parameters are Φ(M*1450) = 1.14 × 10−8 Mpc−3 mag−1, break magnitude M*1450 = −25.13, and bright end slope β = −2.81. However, the covariance between β and M*1450 prevents strong constraints being placed on either parameter. For a break magnitude in the range −26 < M*1450 < −24, we find −3.8 < β < −2.3 at 95% confidence. We calculate the z = 6 quasar intergalactic ionizing flux and show it is between 20 and 100 times lower than that necessary for reionization. Finally, we use the luminosity function to predict how many higher redshift quasars may be discovered in future near-IR imaging surveys.
DYNAMIC EVOLUTION OF AN X-SHAPED STRUCTURE ABOVE A TRANS-EQUATORIAL QUADRUPOLE SOLAR ACTIVE REGION GROUP

In the solar corona, magnetic reconnection usually takes place at the singular configuration of the magnetic field, in particular near a magnetic null, owing to its high susceptibility to perturbations. In this Letter, we report a rare X-shaped structure, encompassing a magnetic null, above a trans-equatorial quadrupole active region group that is well observed by the Atmospheric Imaging Assembly (AIA). The observations show that this X-shaped structure is visible in all AIA EUV passbands and stably exists for days. However, possibly induced by flare activities at the northern part of the quadrupole active region group, the X-shaped structure starts to destabilize while a jet erupts near its center at ∼15:05 UT on 2013 October 7. Through nonlinear force-free field modeling, we identify a magnetic null that is above the quadrupole polarities and well corresponds to the X-shaped structure. After the jet eruption, the temperature and emission measure of the plasma near the X-shaped structure rise from ∼2.3 MK and ∼1.2 × 1027 cm−5 at 15:01 UT to ∼5.4 MK and ∼3.7 × 1027 cm−5 at 15:36 UT, respectively, revealed by the differential emission measure analysis, indicating that magnetic reconnection most likely takes place there to heat the plasma. Moreover, the height of the null increases ∼10 Mm, which is most likely due to the partial opening of the field lines near the fan surface that makes the null underneath rise to seek a new equilibrium.
Evaluating the Prevalence and Distribution of Dental Anomalies in the Permanent Dentition of Patients Seeking Dental Care

Background: Disturbances seen during tooth formation result in developmental dental anomalies presenting in the oral cavity. These anomalies manifest as discrepancies in the number, color, size, and shape of the teeth. These dental anomalies can either be acquired, congenital, or developmental. Their early detection and management are necessary as they affect aesthetics and occlusion. The study had the aim of gauging the prevalence of developmental anomalies in the permanent dentition of Indian subjects. Methods: A total of 1192 participants recruited from the institute for study purposes, comprising males and females, were examined clinically and radiographically, and their dental casts were also evaluated. These subjects were assessed for anomalies in position, structure, number, and/or shape. Anomalies in the position include transmigration, transportation, and/or ectopic position; anomalies in the structure, including dentinogenesis imperfecta or amelogenesis imperfecta; anomalies in number, including hyperdontia or hypodontia; and anomalies in shape, including peg laterals, taurodontism, fusion, dens evaginatus, talon cusp, and/or microdontia. Results: A statistically significant difference was seen in unilateral microdontia and dentinogenesis imperfecta between males and females, with attained p-values of 0.003 and 0.06, respectively. The results of the present study showed that 9.89% (n = 118) study subjects, whereas 1% (n = 12) study subjects had two dental anomalies in their permanent dentitions, with no subject presenting more than two dental anomalies, showing that various dental anomalies have a low prevalence in the Indian population. Conclusion: The present study has led to the conclusion that the prevalence of dental anomalies is low in Indian subjects. However, these anomalies should be detected and treated early to prevent them from causing further complications.
Strong converse theorems in the quantum information theory

Strong converse theorems for two different subjects in quantum information theory are presented. First, we show a lower bound on the probability of decoding error for a quantum communication channel, from which the strong converse to the quantum channel coding theorem is obtained. Second, we give the strong converse theorem for the quantum hypothesis testing as an application of a new inequality on the error probabilities. This inequality is also used to establish the quantum Stein's lemma.
Anomalous Pressure Dependence of the Superconducting Transition Temperature in FeSe1-x Studied by DC Magnetic Measurements

The pressure dependence of superconducting transition temperature $T_{\rm c}$ has been investigated through the DC magnetic measurements for FeSe$_{0.8}$ and FeSe$_{1.0}$. For both samples, with increasing pressure $P$, the $T_{\rm c}$$-$$P$ curve exhibits a two-step increase, showing a local maximum of $\sim$11 K at $P$$\sim$1.0 GPa and a rapid increase with an extremely large pressure coefficient for $P$$>$1.5 GPa. $T_{\rm c}$ saturates at $\sim$25 K (21 K) in FeSe$_{1.0}$ (FeSe$_{0.8}$) for $P$$>$3 GPa. A rapid decrease in superconducting volume fraction is observed with an increase in $T_{\rm c}$ above 1.5 GPa, suggesting the presence of electronic inhomogeneity.
ESTIMATING BLACK HOLE MASSES IN HUNDREDS OF QUASARS

We explore the practical feasibility of active galactic nucleus (AGN) broadband reverberation mapping and present first results. We lay out and apply a rigorous approach for the stochastic reverberation mapping of unevenly sampled multi-broadband flux measurements, assuming that the broad-line region (BLR) line flux is contributing up to 15% in some bands, and is directly constrained by one spectroscopical epoch. The approach describes variations of the observed flux as the continuum, modeled as a stochastic Gaussian process, and emission line contribution, modeled as a scaled, smoothed, and delayed version of the continuum. This approach can be used not only to interpolate in time between measurements, but also to determine confidence limits on continuum—line emission delays. This approach is applied to Sloan Digital Sky Survey observations in Stripe 82 (S82), providing flux measurements that are precise to 2% at ∼60 epochs over ∼10 yr. The strong annual variations in the epoch sampling prove a serious limitation in practice. In addition, suitable redshift ranges must be identified where strong, broad emission lines contribute to one filter, but not to another. By generating and evaluating problem-specific mock data, we verify that S82-like data can constrain τdelay for a simple transfer function model. In application to real data, we estimate τdelay for 323 AGNs with 0.225 < z < 0.846, combining information for different objects through the ensemble-scaling relationships for BLR size and black hole mass. Our analysis tentatively indicates a 1.7 times larger BLR size of Hα and Mg ii compared to Kaspi et al. and Vestergaard, but the seasonal data sampling casts doubt on the robustness of the inference.
Small Impact of Stratospheric Dynamics and Chemistry on the Surface Temperature of the Last Glacial Maximum in CESM2(WACCM6ma)

Stratospheric dynamics and chemistry can impact the tropospheric climate through changing radiatively active atmospheric constituents and stratosphere‐troposphere interactions. The impact of stratospheric dynamics and chemistry on the Last Glacial Maximum (LGM) climate is not well‐studied and remains an uncertain aspect of glacial‐interglacial climate change. Here we perform coupled LGM simulations using the Community Earth System Model version 2 (CESM2), with a high‐top atmosphere—the Whole Atmosphere Community Climate Model version 6 with a middle atmosphere chemistry mechanism (WACCM6ma). The CESM2(WACCM6ma) LGM simulations show a weaker stratospheric circulation than the preindustrial, 10%–35% less tropospheric ozone and 10%–50% more ozone in the lower stratosphere. These dynamical and chemical changes cause slightly more cooling (<5%) in LGM surface and tropospheric temperatures than parallel simulations using a low‐top atmosphere without active chemistry. Results from our model suggest that stratospheric dynamics and chemistry may have little direct effect on the glacial‐interglacial climate change.
Emissions of Fungal Volatile Organic Compounds in Residential Environments and Temporal Emission Patterns: Implications for Sampling Methods

Currently, little is known about the occurrences of fungi-derived microbial volatile organic compounds (mVOCs) in various indoor materials and their detection in residential environments, despite mVOCs being linked to several acute health effects. We identified various mVOCs emitted from fungi grown on PVC wallpaper, silicone rubber, and malt extract agar. We also investigated mVOCs temporal emission and whether fungi-derived VOCs concentration can be used to estimate fungal concentration in the air using active and passive air sampling methods. Among the three fungal growth media included in this study, silicone rubber produced the most variety of mVOCs: 106 compounds (from Aspergillus niger), 35 compounds (from Alternaria alternata), and 85 compounds (from Penicillium chrysogenum). We also found the emission patterns of eight chemical classes (i.e., aromatics, ethers, aliphatics, alcohols, ketones, aldehydes, chlorides, and nitrides) from the three different fungi. From the results of our field experiments in 11 residential environments, passive air samplers led to higher correlations coefficients (0.08 to 0.86) between mVOCs’ air concentrations and airborne fungal concentrations, compared with active air samplers, which showed negative correlation coefficients (−0.99 to −0.02) for most compounds. This study elucidated the occurrence and temporal emission patterns of fungal VOCs in residential environments.
Astrometry of H2O Masers in the Massive Star-Forming Region IRAS 06061+2151 with VERA

We measured the trigonometric annual parallax of an H2O maser source associated with the massive starforming region IRAS 06061+2151 with VERA. The annual parallax of 0.496 ˙ 0.031 mas, corresponding to a distance of 2.02 +0:13 � 0:12 kpc, was obtained by 10 epochs of observations during the period from 2007 October to 2009 September. This distance was obtained more accurately than the photometric one previously measured, and places IRAS 06061+2151 in the Perseus spiral arm. We found that IRAS 06061+2151 also has a peculiar motion of larger than 15 km s � 1 which is counter to the Galactic rotation. This is similar to the motions of five sources in the Perseus spiral arm, whose parallaxes and proper motions have already been measured with satisfactory accuracy. Moreover, these sources move with an average of 27 km s � 1 toward the Galactic center and counter to the Galactic rotation.
A third H i 21-cm absorption system in the sight-line of MG J0414+0534: a redshift for Object X?

We report the detection of a third H I 21-cm absorber in the sight-line towards the z = 2:64 quasar MG J0414+0534 (4C +05.19). In addition to the absorption at the host redshift and in the z = 0:96 gravitational lens, we find, through a decimetre-wave spect ral scan towards this source, strong absorption at z = 0:38. We believe this may be associated with “Object X”, an additional feature apparent in the field of the lensing galaxy and lensed images, on the basis of its close proximity to the quasar images and the possible detection of the [O III] doublet in a published optical spectrum. If real, the streng th of the [O III] emission would suggest the presence of an active galactic nucleus, or a gas- rich galaxy undergoing rapid star formation, either of which is consistent with the stron g outflows apparent in the 21-cm spectrum. Although this is the strongest intervening 21-cm absorber yet found (a column density of NHI > 10 22 cm 2 , for a modest Ts=f > 300 K), simultaneous observations failed to detect any of the 18-cm OH lines at the 21-cm redshift. This suggests that, as for the lensing galaxy, this is not the primary location of the intervening m aterial responsible for the very red colour of MG J0414+0534.
RCSLenS: a new estimator for large-scale galaxy-matter correlations

We present measurements of the galaxy bias b and the galaxy-matter cross-correlation coecient r for the BOSS LOWZ luminous red galaxy sample. Using a new statistical weak lensing analysis of the Red Sequence Cluster Lensing Survey (RCSLenS) we nd the bias properties of this sample to be higher than previously reported with b = 2:45 +0:05 0:05 and r = 1:64 +0:17 0:16 on scales between 3 0 and 20 0 . We repeat the measurement for angular scales of 20 0 6 # 6 70 0 , which yields b = 2:39 +0:07 0:07 and r = 1:24 +0:26 0:25. This is the rst application of a data compression analysis using a complete sets of discrete estimators for galaxy-galaxy lensing and galaxy clustering. As cosmological data sets grow, our new method of data compression will become increasingly important in order to interpret joint weak lensing and galaxy clustering measurements and to estimate the data covariance. In future studies this formalism can be used as a tool to study the large-scale structure of the Universe to yield a precise determination of cosmological parameters.
Influences of various pricing points: an experimental study of plastic bags in Johannesburg, South Africa

ABSTRACT Policymakers have little experience regarding designing the right levels of pricing for plastic bags. The ineffectiveness of charging for bags, in countries such as South Africa, makes it imperative that we map the demand curve. Getting the charge “right” depends on the size of the externality. Charging for bags is therefore an effective intervention to encourage consumers to carry their own bags to the stores. We employ a contingent behaviour (CB) dataset necessary to estimate the charge level that is likely to lead to a reduction in bag use over time. The results of the random effects Tobit model suggest that the current charge of US$0.03 was found to be too low, and highly inelastic. A charge of US$0.50 has potential to reduce unnecessary plastic use and is still lower than the price of alternatives; therefore, there is no danger of consumers shifting to alternatives that may cause more harm.
HIGHz: a survey of the most H i-massive galaxies at z ∼ 0.2

We present the results of the HIGHz Arecibo survey, which measured the HI content of 39 galaxies at redshift $z>0.16$ selected from the Sloan Digital Sky Survey. These are all actively star-forming, disk-dominated systems in relatively isolated environments, with stellar and HI masses larger than $10^{10}$ M$_\odot$ and redshifts $0.17\leq z\leq 0.25$. Our sample includes not only the highest-redshift detections of HI emission from individual galaxies to date, but also some of the most HI-massive systems known. Despite being exceptionally large, the HI reservoirs of these galaxies are consistent with what is expected from their ultraviolet and optical properties. This, and the fact that the galaxies lie on the baryonic Tully-Fisher relation, suggests that HIGHz systems are rare, scaled-up versions of local disk galaxies. We show that the most HI-massive galaxies discovered in the Arecibo Legacy Fast ALFA survey are the local analogues of HIGHz, and discuss the possible connection between our sample and the turbulent, gas-rich disks identified at $z\sim 1$. The HIGHz sample provides a first glimpse into the properties of the massive, HI-rich galaxies that will be detected at higher redshifts by the next-generation HI surveys with the Square Kilometer Array and its pathfinders.
NUMERICAL EXPERIMENTS ON THE DETAILED ENERGY CONVERSION AND SPECTRUM STUDIES IN A CORONA CURRENT SHEET

In this paper, we study the energy conversion and spectra in a corona current sheet (CS) by 2.5 dimensional MHD numerical simulations. Numerical results show that many Petschek-like fine structures with slow-mode shocks mediated by plasmoid instabilities develop during the magnetic reconnection process. The termination shocks can also be formed above the primary magnetic island and at the head of secondary islands. These shocks play important roles in generating thermal energy in a corona CS. For a numerical simulation with initial conditions close to the solar corona environment, the ratio of the generated thermal energy to the total dissipated magnetic energy is around 1/5 before secondary islands appear. After secondary islands appear, the generated thermal energy starts to increase sharply and this ratio can reach a value of about 3/5. In an environment with a relatively lower plasma density and plasma β, the plasma can be heated to a much higher temperature. After secondary islands appear, the one-dimensional energy spectra along the CS do not behave as a simple power law and the spectrum index increases with the wave number. The average spectrum index for the magnetic energy spectrum along the CS is about 1.8. The two-dimensional spectra intuitively show that part of the high energy is cascaded to large kx and ky space after secondary islands appear. The plasmoid distribution function calculated from numerical simulations behaves as a power law closer to f ( &psgr; ) ∼ &psgr; − 1 ? > in the intermediate ψ regime. By using &eegr; eff = v inflow · L , ? > the effective magnetic diffusivity is estimated to be about 1011 ∼ 1012 m2 s−1.
On the naming convention used for multiple star systems and extrasolar planets

The present naming convention for extrasolar planets used by the vast majority of researchers in the field is based upon an interpretation of the provisional I.A. U. standard for multiple star systems. With the existence of hundreds of exoplanets around single stars named by this convention and a handful of exoplanets around binary stars -- circumbinary planets -- it has become necessary to find a uniform and useful naming convention for the latter which is maximally compatible with the single host-star convention and which captures as much of the dynamical information about the planet as possible. We propose a simple and generic naming convention for all exoplanets which follows the provisional I.A. U. standard but more clearly indicates their dynamical status. The proposed convention is compatible with present usage and easily extendible to exoplanets around stars in systems of arbitrary multiplicity. We invite comments and discussion on the proposed convention, in the hope of a timely adoption by the I.A. U. Commissions 5, 8+24, 26, 42, 45 and 53.
The Effects of Disability Status and Employment Level in Shaping Employee Perceptions

THE EFFECTS OF DISABILITY STATUS AND EMPLOYMENT LEVEL IN SHAPING EMPLOYEE PERCEPTIONS: A VIGNETTE STUDY OF EMPLOYEES WHO ARE BLIND by Raymond A. Bennett This study sought to understand the impact of disability status and level of employment (i.e., supervisor or employee) on ratings of performance outcomes and legitimately earning one’s role. It was hypothesized that leaders with disability (LWD) would be rated as poorer performers compared to non-disabled leaders and that co-workers with disability (CWD) would be rated more favorably than LWD. It was also hypothesized that the perceived legitimacy of disability status would moderate the impact of disability status and employment level on performance outcomes. 102 participants read one of four vignettes describing an organization member they regularly interacted with and responded to items about them as well as their own beliefs. Vignettes had either a co-worker who is blind, a supervisor who is blind, a co-worker without a disability, or a supervisor without a disability. While the primary study hypotheses were not supported, results showed that people with disability (PWD) were rated higher on task performance and having legitimately earned their role compared to those without disability, and that LWD were rated as more likely to have earned their role legitimately compared to non-disabled leaders. Implications for future research are discussed, including a need to identify what moderating variables influence perceptions of legitimately earning one's role and performance for those LWD and PWD more generally.
Generation of powerful terahertz emission in a beam-driven strong plasma turbulence

The generation of terahertz electromagnetic radiation due to the coalescence of upper-hybrid waves in the long-wavelength region of strong plasma turbulence driven by a high-current relativistic electron beam in a magnetized plasma is investigated. The width of the frequency spectrum and the angular characteristics of this radiation for various values of plasma density and turbulence energy are calculated using the simple theoretical model adequately describing beam–plasma experiments at mirror traps. It is shown that the power density of electromagnetic emission at the second harmonic of plasma frequency in the terahertz range for these laboratory experiments can reach the level of 1 MW cm−3 with 1% conversion efficiency of beam energy losses to electromagnetic emission.