Miracle-dz/UniFAR-FTUs huggingface dataset:
The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: testing deviations from Λ and general relativity using anisotropic clustering of galaxies

We use the joint measurement of geometry and growth from anisotropic galaxy clustering in the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) CMASS sample reported by Reid et al. to constrain dark energy (DE) properties and possible deviations from the general relativity (GR). Assuming GR and taking a prior on the linear matter power spectrum at high redshift from the cosmic microwave background (CMB), anisotropic clustering of the CMASS DR9 galaxies alone constrains Ωm = 0.308 ± 0.022 and 100Ωk = 5.9 ± 4.8 for w = −1, or w = −0.91 ± 0.12 for Ωk = 0. When combined with the full CMB likelihood, the addition of the anisotropic clustering measurements to the spherically averaged baryon acoustic oscillation location increases the constraining power on DE by a factor of 4 in a flat cold dark matter (CDM) cosmology with constant DE equation of state w (giving w = −0.87 ± 0.05). This impressive gain depends on our measurement of both the growth of structure and the Alcock–Paczynski effect, and is not realized when marginalizing over the amplitude of redshift-space distortions. Combining with both the CMB and Type Ia supernovae, we find Ωm = 0.281 ± 0.014 and 1000Ωk = −9.2 ± 5.0 for w = −1, or w0 = −1.13 ± 0.12 and wa = 0.65 ± 0.36 assuming Ωk = 0. Finally, when a ΛCDM background expansion is assumed, the combination of our estimate of the growth rate with previous growth measurements provides tight constraints on the parameters describing possible deviations from GR giving γ = 0.64 ± 0.05. For one-parameter extensions of the flat ΛCDM model, we find a ∼2σ preference either for w > −1 or slower growth than in GR. However, the data are fully consistent with the concordance model, and evidence for these additional parameters is weaker than 2σ.
AN XMM-NEWTON SURVEY OF THE SOFT X-RAY BACKGROUND. I. THE O vii AND O viii LINES BETWEEN l = 120° AND l = 240°

We present measurements of the soft X-ray background (SXRB) O vii and O viii intensity between l = 120° and l = 240°, the first results of a survey of the SXRB using archival XMM-Newton observations. We do not restrict ourselves to blank-sky observations, but instead use as many observations as possible, removing bright or extended sources by hand if necessary. In an attempt to minimize contamination from near-Earth solar wind charge exchange (SWCX) emission, we remove times of high solar wind proton flux from the data. Without this filtering we are able to extract measurements from 586 XMM-Newton observations. With this filtering, ∼1/2 of the observations are rendered unusable, and we are able to extract measurements from 303 observations. The oxygen intensities are typically ∼0.5–10 photons cm−2 s−1 sr−1 (line units, L.U.) for O vii and ∼0–5 L.U. for O viii. The proton flux filtering does not systematically reduce the oxygen intensities measured from a given observation. However, the filtering does preferentially remove the observations with higher oxygen intensities. Our data set includes 69 directions with multiple observations, whose oxygen intensity variations can be used to constrain SWCX models. One observation exhibits an O vii enhancement of ∼25 L.U. over two other observations of the same direction, although most SWCX enhancements are ≲4 L.U. for O vii and ≲2 L.U. for O viii. We find no clear tendency for the O vii centroid to shift toward the forbidden line energy in observations with bright SWCX enhancements. There is also no universal association between enhanced SWCX emission and increased solar wind flux or the closeness of the sightline to the sub-solar region of the magnetosheath. After removing observations likely to be contaminated by heliospheric SWCX emission, we use our results to examine the Galactic halo. There is some scatter in the halo intensity about the predictions of a simple plane-parallel model, indicating a patchiness to the halo emission. The O vii/O viii intensity ratio implies a halo temperature of ∼2.0–2.5 × 106 K, in good agreement with previous studies.
Long-lived nonthermal states realized by atom losses in one-dimensional quasicondensates

We investigate the cooling produced by a loss process non selective in energy on a one-dimensional (1D) Bose gas with repulsive contact interactions in the quasi-condensate regime. By performing nonlinear classical field calculations for a homogeneous system, we show that the gas reaches a non-thermal state where different modes have acquired different temperatures. After losses have been turned off, this state is robust with respect to the nonlinear dynamics, described by the Gross-Pitaevskii equation. We argue that the integrability of the Gross-Pitaevskii equation is linked to the existence of such long-lived non-thermal states, and illustrate this by showing that such states are not supported within a non-integrable model of two coupled 1D gases of different masses. We go beyond a classical field analysis, taking into account the quantum noise introduced by the discreteness of losses, and show that the non-thermal state is still produced and its non-thermal character is even enhanced. Finally, we extend the discussion to gases trapped in a harmonic potential and present experimental observations of a long-lived non-thermal state within a trapped 1D quasi-condensate following an atom loss process.
Nurses’ Adherence to Surgical Safety Guidelines for Patients Undergoing Abdominal Surgery

Background: Patient's safety events at the operating room can be completely avoidable by adhering to surgical safety practices that aims to improve adherence to evidence-based safety practices, communication and team work during critical time points as during surgical procedure, before induction of anesthesia, before incision and before the patient leaves the room. Objective: This study aimed to assess nurses' adherence to surgical safety guidelines for patients undergoing abdominal surgery. Subjects and methods: Design: A descriptive exploratory research design was used to achieve the aim of this study. Setting: This study was conducted at the Operating Departments affiliated to El-Saff General Hospital and Atfeh Central Hospital. Study subjects: A convenient sample of all available nurses (75) from the previously mentioned departments was included in the study. Tools of data collection: Structured interview questionnaire included two parts: demographic characteristics of the studied nurses and surgical safety guidelines checklist. Result: This study presented that less than half of the studied scrub nurses and only minority of the circulating nurses and anesthesia nurses had competent practices at the operating room respectively. Conclusion: The study concluded there were statistically significant relations between competent practices of scrub nurses and their attendance of training courses related to surgical safety and between competent practices of circulating nurses, their age and years of experience, while, there were no statistically significant relations between competent practices of anesthesia nurses, their gender and attendance of training course. Recommendation: Ongoing staff development programs and continuing education are important for improving staff performance and maintaining patients' safety.
PROBING THE UNIVERSE'S TILT WITH THE COSMIC INFRARED BACKGROUND DIPOLE

Conventional interpretation of the observed cosmic microwave background (CMB) dipole is that all of it is produced by local peculiar motions. Alternative explanations requiring part of the dipole to be primordial have received support from measurements of large-scale bulk flows. A test of the two hypotheses is whether other cosmic dipoles produced by collapsed structures later than the last scattering coincide with the CMB dipole. One background is the cosmic infrared background (CIB) whose absolute spectrum was measured to ∼30% by the COBE satellite. Over the 100–500 μm wavelength range its spectral energy distribution can provide a probe of its alignment with the CMB. This is tested with the COBE FIRAS data set which is available for such a measurement because of its low noise and frequency resolution which are important for Galaxy subtraction. Although the FIRAS instrument noise is in principle low enough to determine the CIB dipole, the Galactic foreground is sufficiently close spectrally to keep the CIB dipole hidden. A similar analysis is performed with DIRBE, which—because of the limited frequency coverage—provides a poorer data set. We discuss strategies for measuring the CIB dipole with future instruments to probe the tilt and apply it to the Planck, Herschel, and the proposed Pixie missions. We demonstrate that a future FIRAS-like instrument with instrument noise a factor of ∼10 lower than FIRAS would make a statistically significant measurement of the CIB dipole. We find that the Planck and Herschel data sets will not allow a robust CIB dipole measurement. The Pixie instrument promises a determination of the CIB dipole and its alignment with either the CMB dipole or the dipole galaxy acceleration vector.
Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence

We developed angular momentum evolution models for 0.5 and 0.8 $M_{\odot}$ stars. The parametric models include a new wind braking law based on recent numerical simulations of magnetised stellar winds, specific dynamo and mass-loss rate prescriptions, as well as core/envelope decoupling. We compare model predictions to the distributions of rotational periods measured for low mass stars belonging to star forming regions and young open clusters. Furthermore, we explore the mass dependence of model parameters by comparing these new models to the solar-mass models we developed earlier. Rotational evolution models are computed for slow, median, and fast rotators at each stellar mass. The models reproduce reasonably well the rotational behaviour of low-mass stars between 1 Myr and 8-10 Gyr, including pre-main sequence to zero-age main sequence spin up, prompt zero-age main sequence spin down, and early-main sequence convergence of the surface rotation rates. Fast rotators are found to have systematically shorter disk lifetimes than moderate and slow rotators, thus enabling dramatic pre-main sequence spin up. They also have shorter core-envelope coupling timescales, i.e., more uniform internal rotation. As to the mass dependence, lower mass stars require significantly longer core-envelope coupling timescale than solar-type ones, which results in strong differential rotation developing in the stellar interior on the early main sequence. Lower mass stars also require a weaker braking torque to account for their longer spin down timescale on the early main sequence, while they ultimately converge towards lower rotational velocities than solar-type stars on the longer term due to their reduced moment of inertia. We also find evidence that the mass-dependence of the wind braking efficiency may be related to a change of the magnetic topology in lower mass stars.
Probing the Local Bubble with Diffuse Interstellar Bands. I. Project overview and Southern hemisphere survey

We have conducted a high signal-to-noise spectroscopic survey of 670 nearby early-type stars, to map Diffuse Interstellar Band (DIB) absorption in and around the Local Bubble. The project started with a Southern hemisphere survey conducted at the European Southern Observatory's New Technology Telescope and has since been extended to an all-sky survey using the Isaac Newton Telescope. In this first paper in the series, we introduce the overall project and present the results from the Southern hemisphere survey. We make available a catalogue of equivalent-width measurements of the DIBs at 5780, 5797, 5850, 6196, 6203, 6270, 6283 \& 6614 \AA, the interstellar Na\,{\sc i} D lines at 5890 \& 5896 \AA, and the stellar He\,{\sc i} line at 5876 \AA. We find that the 5780 \AA\ DIB is relatively strong throughout, as compared to the 5797 \AA\ DIB, but especially within the Local Bubble and at the interface with more neutral medium. The 6203 \AA\ DIB shows a similar behaviour, but with respect to the 6196 \AA\ DIB. Some nearby stars show surprisingly strong DIBs whereas some distant stars show very weak DIBs, indicating small-scale structure within as well as outside the Local Bubble. The sight-lines with non-detections trace the extent of the Local Bubble especially clearly, and show it opening out into the Halo. The Local Bubble has a wall which is in contact with hot gas and/or a harsh interstellar radiation field. That wall is perforated though, causing leakage of radiation and possibly hot gas. On the other hand, compact self-shielded cloudlets are present much closer to the Sun, probably within the Local Bubble itself. As for the carriers of the DIBs, our observations confirm the notion that these are large molecules, whose differences in behaviour are mainly governed by their differing resilience and/or electrical charge, with more subtle differences possibly related to varying excitation.
A review on Loop Quantum Gravity

The aim of this dissertation is to review `Loop Quantum Gravity', explaining the main structure of the theory and indicating its main open issues. We will develop the two main lines of research for the theory: the canonical quantization (first two chapters) and spin foams (third). The final chapter will be devoted to studying some of the problems of the theory and what things remain to be developed. In chapter 3 we will also include an example of a simple calculation done in the frame of LQG: Schwarzschild black hole entropy.
Angular Velocity Estimation of Image Motion Mimicking the Honeybee Tunnel Centring Behaviour

Insects use visual information to estimate angular velocity of retinal image motion, which determines a variety of flight behaviours including speed regulation, tunnel centring and visual navigation. For angular velocity estimation, honeybees show large spatial-independence against visual stimuli, whereas the previous models have not fulfilled such an ability. To address this issue, we propose a bio-plausible model for estimating the image motion velocity based on behavioural experiments of the honeybee flying through patterned tunnels. The proposed model contains mainly three parts, the texture estimation layer for spatial information extraction, the delay-and-correlate layer for temporal information extraction and the decoding layer for angular velocity estimation. This model produces responses that are largely independent of the spatial frequency in grating experiments. And the model has been implemented in a virtual bee for tunnel centring simulations. The results coincide with both electro-physiological neuron spike and behavioural path recordings, which indicates our proposed method provides a better explanation of the honeybee’s image motion detection mechanism guiding the tunnel centring behaviour.
Three-dimensional Aquila Rift: magnetized H i arch anchored by molecular complex

Three dimensional structure of the Aquila Rift of magnetized neutral gas is investigated by analyzing HI and CO line data. The projected distance on the Galactic plane of the HI arch of the Rift is ~250 pc from the Sun. The HI arch emerges at l~ 30 deg, reaches to altitudes as high as ~ 500 pc above the plane at l~ 350deg, and returns to the disk at l~270 deg. The extent of arch at positive latitudes is ~1 kpc and radius is ~100 pc. The eastern root is associated with the giant molecular cloud complex, which is the main body of the optically defined Aquila Rift. The HI and molecular masses of the Rift are estimated to be M_HI~1.4x10^5Msun and M_H2 ~3x10^5 Msun. Gravitational energies to lift the gases to their heights are E_grav: HI ~1.4x10^51 and E_grav: H_2 ~0.3x10^51 erg, respectively. Magnetic field is aligned along the HI arch of the Rift, and the strength is measured to be B~10 microG using Faraday rotation measures of extragalactic radio sources. The magnetic energy is estimated to be E_mag~1.2x10^51 erg. A possible mechanism of formation of the Aquila Rift is proposed in terms of interstellar magnetic inflation by a sinusoidal Parker instability of wavelength of ~2.5 kpc and amplitude ~500 pc.
Semiparametric approach to the detection of non-Gaussian gravitational wave stochastic backgrounds

Using a semiparametric approach based on the fourth-order Edgeworth expansion for the unknown signal distribution, we derive an explicit expression for the likelihood detection statistic in the presence of a non-normally distributed gravitational wave stochastic background. Numerical likelihood maximization exercises based on Monte Carlo simulations for a set of large tail symmetric non-Gaussian distributions suggest that the fourth cumulant of the signal distribution can be estimated with reasonable precision when the ratio between the signal and the noise variances is larger than 0.01. The estimation of higher-order cumulants of the observed gravitational wave signal distribution is expected to provide additional constraints on astrophysical and cosmological models.
Prediction of beam losses during crab cavity quenches at the high luminosity LHC

Studies of the crab cavities at KEKB revealed that the RF phase could shift by up to 50o within ~50 us during a quench; while the cavity voltage is still at approximately 75% of its nominal amplitude. If such a failure were to occur on the HL-LHC crab cavities, it is likely that the machine would sustain substantial damage to the beam line and surrounding infrastructure due to uncontrolled beam loss before the machine protection system could dump the beam. We have developed a low-level RF system model, including detuning mechanisms and beam loading, and use this to simulate the behaviour of a crab cavity during a quench, modeling the low-level RF system, detuning mechanisms and beam loading. We supplement this with measurement data of the actual RF response of the proof of principle Double-Quarter Wave Crab Cravity during a quench. Extrapolating these measurements to the HL-LHC, we show that Lorentz Force detuning is the dominant effect leading to phase shifts in the crab cavity during quenches; rather than pressure detuning which is expected to be dominant for the KEKB crab cavities. The total frequency shift for the HL-LHC crab cavities during quenches is expected to be about 460 Hz, leading to a phase shift of no more than 3o. The results of the quench model are read into a particle tracking simulation, SixTrack, and used to determine the effect of quenches on the HL-LHC beam. The quench model has been benchmarked against the KEKB experimental measurements. In this paper we present the results of the simulations on a crab cavity failure for HL-LHC as well as for the SPS and show that beam loss is negligible when using a realistic low-level RF response.
Intra-night optical monitoring of three γ-ray detected narrow-line Seyfert 1 galaxies

For 3 radio-loud $\gamma$-ray detected Narrow-Line Seyfert 1 ($\gamma$-ray NLSy1) galaxies, we report optical variability on intra-night and/or week-like time scales, based on five $\geq$ 3 hours long monitoring sessions for each galaxy. The radio-loudness factors (R$_{1.4 GHz}$) for these galaxies, namely 1H 0323$+$342 (z = 0.0629), PKS J1222$+$0413 (z = 0.966) and PKS J1505$+$0326 (z = 0.408) are $\sim$318, $\sim$1534 and $\sim$3364 at 1.4 GHz, respectively. For the most distant $\gamma$-ray NLSy1, PKS J1222$+$0413, Intra-Night Optical Variability (INOV) characterisation is presented for the first time. The blazar-like behaviour of the nearest $\gamma$-ray NLSy1 1H 0323$+$342, which showed strong INOV on 4 of the 5 nights, was unexpected in view of its recent reclassification as `radio intermediate' (R$_{5 GHz}$ $\lesssim$ 25). Its particularly violent INOV is manifested by two optical outbursts lasting $\sim$ 1 hour, whose rapid brightening phase is shown to imply a doubling time of $\sim$ 1 hour for the optical synchrotron flux, after (conservatively) deducting the thermal optical emission contributed by the host galaxy and the Seyfert nucleus. A more realistic `decontamination' could well reduce substantially the flux doubling time, bringing it still closer in rapidity to the ultra-fast VHE ($>$ 100 GeV) flares reported for the blazars PKS 1222$+$216 and PKS 2155$-$304. A large contamination by thermal optical emission may, in fact, be common for NLSy1s as they are high Eddington rate accretors. The present study further suggests that superluminal motion in the radio jet could be a robust diagnostic of INOV.
Astrometry of mutual approximations between natural satellites. Application to the Galilean moons

Typically we can deliver astrometric positions of natural satellites with errors in the 50-150 mas range. Apparent distances from mutual phenomena, have much smaller errors, less than 10 mas. However, this method can only be applied during the equinox of the planets. We developed a method that can provide accurate astrometric data for natural satellites -- the mutual approximations. The method can be applied when any two satellites pass close by each other in the apparent sky plane. The fundamental parameter is the central instant $t_0$ of the passage when the distances reach a minimum. We applied the method for the Galilean moons. All observations were made with a 0.6 m telescope with a narrow-band filter centred at 889 nm with width of 15 nm which attenuated Jupiter's scattered light. We obtained central instants for 14 mutual approximations observed in 2014-2015. We determined $t_0$ with an average precision of 3.42 mas (10.43 km). For comparison, we also applied the method for 5 occultations in the 2009 mutual phenomena campaign and for 22 occultations in the 2014-2015 campaign. The comparisons of $t_0$ determined by our method with the results from mutual phenomena show an agreement by less than 1-sigma error in $t_0$, typically less than 10 mas. This new method is particularly suitable for observations by small telescopes.
THE GENERATION OF STRONG MAGNETIC FIELDS DURING THE FORMATION OF THE FIRST STARS

Cosmological hydrodynamical simulations of primordial star formation suggest that the gas within the first star-forming halos is turbulent. This has strong implications on the subsequent evolution, in particular on the generation of magnetic fields. Using high-resolution numerical simulations, we show that in the presence of turbulence, weak seed magnetic fields are exponentially amplified by the small-scale dynamo during the formation of the first stars. We conclude that strong magnetic fields are generated during the birth of the first stars in the universe, potentially modifying the mass distribution of these stars and influencing the subsequent cosmic evolution. We find that the presence of the small-scale turbulent dynamo can only be identified in numerical simulations in which the turbulent motions in the central core are resolved with at least 32 grid cells.