Miracle-dz/UniFAR-FTUs huggingface dataset:
A minimum mass nebula for M dwarfs

Recently revealed differences in planets around M dwarf vs. solar-type stars could arise from differences in their primordial disks, and surveys of T Tauri stars find a correlation between stellar mass and disk mass. "Minimum" disks have been reconstructed for the Solar System and solar-type stars and here this exercise is performed for M dwarfs using Kepler-detected planets. Distribution of planet mass between current orbits produces a disk with total mass of ~0.009Msun and a power-law profile with index 2.2. Disk reconstruction from the output of a forward model of planet formation indicates that the effect of detection bias on disk profile is slight and that the observed scatter in planet masses and semi-major axes is consistent with a universal disk profile. This nominal M dwarf disk is more centrally concentrated than those inferred around the solar-type stars observed by Kepler, and the mass surface density beyond 0.02 AU is sufficient for in situ accretion of planets as single embryos. The mass of refractory solids within 0.5 AU is 5.6Mearth compared to 4Mearth for solar-type stars, in contrast with the trend with total disk mass. The total solids beyond 0.5 AU is sufficient for the core of at least one giant planet.
DUSTY QUASARS AT HIGH REDSHIFTS

A population of quasars at z ∼ 2 is determined based on dust luminosities νLν(7.8 μm) that includes unobscured, partially obscured, and obscured quasars. Quasars are classified by the ratio νLν(0.25 μm)/νLν(7.8 μm) = UV/IR, assumed to measure obscuration of UV luminosity by the dust that produces IR luminosity. Quasar counts at rest-frame 7.8 μm are determined for quasars in the Boötes field of the NOAO Deep Wide Field Survey using 24 μm sources with optical redshifts from the AGN and Galaxy Evolution Survey (AGES) or infrared redshifts from the Spitzer Infrared Spectrograph. Spectral energy distributions are extended to far-infrared wavelengths using observations from the Herschel Space Observatory Spectral and Photometric Imaging Receiver (SPIRE), and new SPIRE photometry is presented for 77 high-redshift quasars from the Sloan Digital Sky Survey. It is found that unobscured and obscured quasars have similar space densities at rest-frame 7.8 μm, but the ratio Lν(100 μm)/Lν(7.8 μm) is about three times higher for obscured quasars than for unobscured, so that far-infrared or submillimeter quasar detections are dominated by obscured quasars. We find that only ∼5% of high-redshift submillimeter sources are quasars and that existing 850 μm surveys or 2 mm surveys should already have detected sources at z ∼ 10 if quasar and starburst luminosity functions remain the same from z = 2 until z = 10.
The Chandra-COSMOS survey – IV. X-ray spectra of the bright sample

We present the X-ray spectral analysis of the 390 brightest extragalactic sources in the Chandra-COSMOS catalog, showing at least 70 net counts in the 0.5-7 keV band. This sample has a 100% completeness in optical-IR identification, with 75% of the sample having a spectroscopic redshift and 25% a photometric redshift. Our analysis allows us to accurately determine the intrinsic absorption, the broad band continuum shape ({\Gamma}) and intrinsic L(2-10) distributions, with an accuracy better than 30% on the spectral parameters for 95% of the sample. The sample is equally divided in type-1 (49.7%) and type-2 AGN (48.7%) plus few passive galaxies at low z. We found a significant difference in the distribution of {\Gamma} of type-1 and type-2, with small intrinsic dispersion, a weak correlation of {\Gamma} with L(2-10) and a large population (15% of the sample) of high luminosity, highly obscured (QSO2) sources. The distribution of the X ray/Optical flux ratio (Log(FX /Fi)) for type-1 is narrow (0 < X/O < 1), while type-2 are spread up to X/O = 2. The X/O correlates well with the amount of X-ray obscuration. Finally, a small sample of Compton thick candidates and peculiar sources is presented. In the appendix we discuss the comparison between Chandra and XMM-Newton spectra for 280 sources in common. We found a small systematic difference, with XMM-Newton spectra that tend to have softer power-laws and lower obscuration.
Versatile relative entropy bounds for quantum networks

We provide a versatile upper bound on the number of maximally entangled qubits, or private bits, shared by two parties via a generic adaptive communication protocol over a quantum network when the use of classical communication is not restricted. Although our result follows the idea of Azuma et al (2016 Nat. Commun. 7 13523) of splitting the network into two parts, our approach relaxes their strong restriction, consisting of the use of a single entanglement measure in the quantification of the maximum amount of entanglement generated by the channels. In particular, in our bound the measure can be chosen on a channel-by-channel basis, in order to make it as tight as possible. This enables us to apply the relative entropy of entanglement, which often gives a state-of-the-art upper bound, on every Choi-simulable channel in the network, even when the other channels do not satisfy this property. We also develop tools to compute, or bound, the max-relative entropy of entanglement for channels that are invariant under phase rotations. In particular, we present an analytical formula for the max-relative entropy of entanglement of the qubit amplitude damping channel.
A kinematic study of the irregular dwarf galaxy NGC 4861 using H I and Hα observations

Context. Outflows powered by the injection of kinetic energy from massive stars can strongly affect the chemical evolution of galaxies, in particular of dwarf galaxies, as their lower gravitational potentials enhance the chance of a galactic wind. Aims. We therefore performed a detailed kinematic analysis of the neutral and ionised gas components in the nearby star-forming irregular dwarf galaxy NGC 4861. Similar to a recently published study of NGC 2366, we want to make predictions about the fate of the gas and to discuss some general issues about this galaxy. Methods. Fabry-Perot interferometric data centred on the Hα line were obtained with the 1.93 m telescope at the Observatoire de Haute-Provence. They were complemented by H i synthesis data from the VLA. We performed a Gaussian decomposition of both the Hα and the H i emission lines in order to search for multiple components indicating outflowing gas. The expansion velocities of the detected outflows were compared to the escape velocity of NGC 4861, which was modelled with a pseudo-isothermal halo. Results. Both in Hα and H i the galaxy shows several outflows, three directly connected to the disc and probably forming the edges of a supergiant shell, and one at kpc-distance from the disc. We measured velocity offsets of 20 to 30 km s −1 , which are low in comparison to the escape velocity of the galaxy and therefore minimise the chance of a galactic wind.
Running Spectral Index from Inflation with Modulations

We argue that a large negative running spectral index, if confirmed, might suggest that there are abundant structures in the inflaton potential, which result in a fairly large (both positive and negative) running of the spectral index at all scales. It is shown that the center value of the running spectral index suggested by the recent CMB data can be easily explained by an inflaton potential with superimposed periodic oscillations. In contrast to cases with constant running, the perturbation spectrum is enhanced at small scales, due to the repeated modulations. We mention that such features at small scales may be seen by 21 cm observations in the future.
Extending virial black hole mass estimates to low-luminosity or obscured AGN: the cases of NGC 4395 and MCG -01-24-012

In the last decade, using single epoch (SE) virial based spectroscopic optical observations, it has been possible to measure the black hole (BH) mass on large type 1 Active Galactic Nuclei (AGN) samples. However this kind of measurements can not be applied on those obscured type 2 and/or low luminosity AGN where the nuclear component does not dominate in the optical. We have derived new SE relationships, based on the FWHM and luminosity of the broad line region component of the Pa emission line and/or the hard X-ray luminosity in the 14-195 keV band, which have the prospect of better working with low luminosity or obscured AGN. The SE relationships have been calibrated in the 10 5 10 9 M mass range, using a sample of AGN whose BH masses have been previously measured using reverberation mapping techniques. Our tightest relationship between the reverberation-based BH mass and the SE virial product has an intrinsic spread of 0.20 dex. Thanks to these SE relations, in agreement with previous estimates, we have measured a BH mass of MBH=1:7 +1:3
An Empirical Study of Volatility in Cryptocurrency Market

Cryptocurrencies have gained a lot of attraction across the globe. Most observers of the cryptocurrency market will agree that crypto volatility is in a different league altogether. There has been a growing need to understand the nature of volatility in cryptocurrency. This paper analyzes the performance of four mostly traded, different cryptocurrencies in terms of their risk and return. The relationship between the return and returns volatility among different currencies has been examined considering the daily closing prices from 1 January 2017 to 30 June 2022, using the family of the GARCH model. The study has explored the spillover and asymmetric effect of volatility by using the DCC GARCH model and EGARCH model, respectively. The causal behavior among different cryptocurrencies has also been examined using Granger causality. There has been a strong spillover effect among different cryptocurrencies, Bitcoin and Ether, which are the top two cryptocurrencies with the highest market capitalization which have exhibited an asymmetric impact in their volatility as compared to the other two currencies, which are Litecoin and XRP.
Disparities in Prevalence and Barriers to Hypertension Control: A Systematic Review

Controlling hypertension (HTN) remains a challenge, as it is affected by various factors in different settings. This study aimed to describe the disparities in the prevalence and barriers to hypertension control across countries of various income categories. Three scholarly databases—ScienceDirect, PubMed, and Google Scholar—were systematically examined using predefined search terms to identify potentially relevant studies. Original research articles published in English between 2011 and 2022 that reported the prevalence and barriers to HTN control were included. A total of 33 studies were included in this systematic review. Twenty-three studies were conducted in low and middle-income countries (LMIC), and ten studies were from high-income countries (HIC). The prevalence of hypertension control in the LMIC and HIC studies ranged from (3.8% to 50.4%) to (36.3% to 69.6%), respectively. Concerning barriers to hypertension control, patient-related barriers were the most frequently reported (n = 20), followed by medication adherence barriers (n = 10), lifestyle-related barriers (n = 8), barriers related to the affordability and accessibility of care (n = 8), awareness-related barriers (n = 7), and, finally, barriers related to prescribed pharmacotherapy (n = 6). A combination of more than one category of barriers was frequently encountered, with 59 barriers reported overall across the 33 studies. This work reported disparities in hypertension control and barriers across studies conducted in LMIC and HIC. Recognizing the multifactorial nature of the barriers to hypertension control, particularly in LMIC, is crucial in designing and implementing customized interventions.
Spin-orbit evolution of the GJ 667C system: the effect of composition and other planets’ perturbations

Potentially habitable planets within the habitable zone of M-dwarfs are affected by tidal interaction. We studied the tidal evolution in GJ 667C using a numerical code we call TIDEV. We reviewed the problem of the dynamical evolution focusing on the effects that a rheological treatment, different compositions and the inclusion of orbital perturbations, have on the spin-down time and the probability to be trapped in a low spin-orbit resonance. Composition have a strong effect on the spin-down time, changing, in some cases, by almost a factor of 2 with respect to the value estimated for a reference Earth-like model. We calculated the time to reach a low resonance value (3:2) for the configuration of 6 planets. Capture probabilities are affected when assuming different compositions and eccentricities variations. We chose planets b and c to evaluate the probabilities of capture in resonances below 5:2 for two compositions: Earth-like and Waterworld planets. We found that perturbations, although having a secular effect on eccentricities, have a low impact on capture probabilities and noth- ing on spin-down times. The implications of the eccentricity variations and actual habitability of the GJ 667C system are discussed.
The RoboPol Program: Optical Polarimetric Monitoring of Blazars

After three years of polarimetric monitoring of blazars, the RoboPol project has uncovered several key characteristics of polarimetric rotations in the optical for these most variable sources. The most important of these is that polarization properties of the synchrotron emission in the optical appear to be directly linked with gamma-ray activity. In this paper, we discuss the evidence for this connection, as well as the broader features of polarimetric behavior in blazars that are key in making progress with theoretical modeling of blazar emission.
Involvement of M1/M2 Macrophage Polarization in Reparative Dentin Formation

In cases in which dental pulp tissue is accidentally exposed, direct pulp capping is often performed to induce reparative dentin formation. Although macrophages are essential for the inflammatory response and tissue repair, the emergence pattern and the role of macrophages in dental pulp tissue have not been clarified. Here, we investigated the emergence of M1/M2 macrophages in dental pulp tissue after a direct pulp capping and the effects of M2 macrophages on odontoblastic differentiation of the dental pulp stem cell (DPSC) clones. The emergence of macrophages in dental pulp tissue was investigated using a rat direct pulp capping model. Alizarin Red S staining and quantitative RT-PCR was performed to examine the effect of M2 macrophages on the mineralization and odontoblastic differentiation of DPSC clones. Immunohistochemical staining revealed that M1 macrophages were detected in dental pulp tissue after treatment and increased in number at three days after treatment. However, M2 macrophages gradually increased in number in dental pulp tissue after treatment, with the highest level recorded at seven days post-operation. Additionally, conditioned medium from M2 macrophages induced odontoblast-like differentiation of DPSC clones. These results suggest that macrophages play a role in the inflammatory response and reparative dentin formation after dental pulp exposure.
Step Bunching In Conserved Systems: Scaling And Universality

We study the step bunching process in three different 1D step flow models and obtain scaling relations for the step bunches formed in the long times limit. The first one was introduced by S.Stoyanov [Jap. J.Appl. Phys. 29, (1990) L659] as the simplest 'realistic' model of step bunching due to drift of the adatoms. Here we show that it could lead to (at least) two different types of step bunching, depending on the magnitude of the drift. The other two models are minimal models: the equations for step velocity are constructed ad hoc from two terms with opposite effects - destabilizing and, respectively, stabilizing the regular step train.
Two-color quark matter: U(1) A restoration, superfluidity, and quarkyonic phase

We discuss the phase structure of quantum chromodynamics (QCD) with two colors and two flavors of light quarks. This is motivated by the increasing interest in the QCD phase diagram as follows: (1) The QCD critical point search has been under intensive dispute and its location and existence suffer from uncertainty of effective U(1){sub A} symmetry restoration. (2) A new phase called quarkyonic matter is drawing theoretical and experimental attention but it is not clear whether it can coexist with diquark condensation. We point out that two-color QCD is nontrivial enough to contain essential ingredients for (1) and (2) both, and most importantly, is a system without the sign problem in numerical simulations on the lattice. We adopt the two-flavor Nambu-Jona-Lasinio model extended with the two-color Polyakov loop and make quantitative predictions that can be tested by lattice simulations.
AN ANALYSIS OF GENDER REPRESENTATION IN I LOVE JAKARTA, AN ELEMENTARY TEXTBOOK

Klein (1985) believes that appropriate gender-unbiased material mostly gives students the chance to accommodate more compliant mindsets towards gender roles. This study was conducted to observe the way genders are represented in local elementary textbooks in Indonesia, especially the textbook entitled "I Love Jakarta. " The method applied in this study was qualitative research that used content analysis. The approach was used to describe the content of the textbook, by using the checklist adapted from Shallaita, et al. (2021), which includes all the texts, illustrations, vocabularies, and exercises, in every chapter of the book. The writers assessed the gender representation in the first grade of an elementary school textbook according to five categories adopted from Amini and Birjandi (2012); Visibility, Firstness, Feminine/Masculine Generic Construction, Activity, Occupation on every text and pictures in the book from unit one until sixteen. The results showed that (1) in terms of visibility, male (54%) was represented more than female (46%), (2) in terms of firstness, male (around nine mentions) in the majority of the cases was mentioned first than female (around five mentions), (3) in the category of feminine/masculine generic construction, there was no case found, (4) regarding the activities portrayed in the book, both male and female characters shared their parts of doing some of the general activities; however, there were cases where some activities were portrayed of being intended mainly for males, such as doing pencak silat and lifting heavy objects. On the other hand, there were portrayals of some of the activities which were mostly intended for females because of their less-aggressive nature, such as dancing and reading a book, (5) in terms of occupations depicted in the book, some of them were represented equally by both male and female characters; however, there were occupations which were considered more manly, such as fisherman and pedicab driver, therefore portrayed by male characters. To sum up, both genders were not represented equally in terms of the five categories.
Long-term X-ray variability characteristics of the narrow-line Seyfert 1 galaxy RE J1034+396

This publication uses data from the AstroSat mission of the Indian Space Research Organisation (ISRO). AstroSat observed this source as part of its SXT-guaranteed time program for AGN studies (PI: K. P. Singh). This work has used the data from the Soft X-ray Telescope (SXT) developed in a collaboration between TIFR, Mumbai, and the University of Leicester and the Large X-ray Proportional Counter Array (LAXPC) developed at TIFR, Mumbai. The SXT and LAXPC POCs at TIFR are thanked for verifying and releasing the data via the ISSDC data archive and providing the necessary software tools. This research has made use of the data and software obtained from NASAs High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. The use of the XRT DATA ANALYSIS SOFTWARE (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC) is gratefully acknowledged. This work has made use of observations obtained with XMM–Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the USA (NASA). Partial support for the SXT UK–Indian collaboration was provided by the UKIERI programme of the British Council and Royal Society. Kishor Chaudhury expresses his profound gratitude to Dr. Samir Kumar Sarkar for teaching the data analysis procedure and special thanks to Dr. Arunava Bhadra for his valuable suggestions.
Relativistic low angular momentum accretion in 3D

We study the low angular momentum accretion of matter onto Schwarzschild or Kerr black hole using fully relativistic numerical simulations. Our aim is to include the rotation of both the gas and the black hole and the presence of the magnetic field into the picture. We compare resulting structure of transonic flow with results of 1D pseudo-Newtonian semi-analytical computations of non-magnetized flow.
HIGH-RESOLUTION SPECTROSCOPY OF Ne ii EMISSION FROM YOUNG STELLAR OBJECTS

Constraining the spatial and thermal structure of the gaseous component of circumstellar disks is crucial for understanding star and planet formation. Models predict that the [Ne ii] line at 12.81 μm detected in young stellar objects (YSOs) with Spitzer traces disk gas and its response to high-energy radiation, but such [Ne ii] emission may also originate in shocks within powerful outflows. To distinguish between these potential origins for mid-infrared [Ne ii] emission and to constrain disk models, we observed 32 YSOs using the high-resolution (R ∼ 30,000) mid-infrared spectrograph VISIR at the Very Large Telescope. We detected the 12.81 μm [Ne ii] line in 12 objects, tripling the number of detections of this line in YSOs with high spatial and spectral resolution spectrographs. We obtain the following main results. (1) In Class I objects the [Ne ii] emission observed from Spitzer is mainly due to gas at a distance of more than 20–40 AU from the star, where neon is, most likely, ionized by shocks due to protostellar outflows. (2) In transition and pre-transition disks, most of the emission is confined to the inner disk, within 20–40 AU from the central star. (3) Detailed analysis of line profiles indicates that, in transition and pre-transition disks, the line is slightly blueshifted (2–12 km s−1) with respect to the stellar velocity, and the line width is directly correlated with the disk inclination, as expected if the emission is due to a disk wind. (4) Models of EUV/X-ray-irradiated disks reproduce well the observed relation between the line width and the disk inclination, but underestimate the blueshift of the line.
Numerical evaluation of the tensor bispectrum in two field inflation

We evaluate the dimensionless non-Gaussianity parameter hNL, that characterizes the amplitude of the tensor bispectrum, numerically for a class of two field inflationary models such as double inflation, hybrid inflation and aligned natural inflation. We compare the numerical results with the slow roll results which can be obtained analytically. In the context of double inflation, we also investigate the effects on hNL due to curved trajectories in the field space. We explicitly examine the validity of the consistency relation governing the tensor bispectrum in the squeezed limit. Lastly, we discuss the contribution to hNL due to the epoch of preheating in two field models.