Miracle-dz/UniFAR-FTUs huggingface dataset:
HALO MASS DEPENDENCE OF H i AND O vi ABSORPTION: EVIDENCE FOR DIFFERENTIAL KINEMATICS

We studied a sample of 14 galaxies (0.1 < z < 0.7) using HST/WFPC2 imaging and high-resolution HST/COS or HST/STIS quasar spectroscopy of Lyα, Lyβ, and O vi λλ1031, 1037 absorption. The galaxies, having 10.8 ⩽ log (M h/M☉) ⩽ 12.2, lie within D = 300 kpc of quasar sightlines, probing out to D/Rvir = 3. When the full range of M h and D/Rvir of the sample are examined, ∼40% of the H i absorbing clouds can be inferred to be escaping their host halo. The fraction of bound clouds decreases as D/Rvir increases such that the escaping fraction is ∼15% for D/Rvir < 1, ∼45% for 1 ⩽ D/Rvir < 2, and ∼90% for 2 ⩽ D/Rvir < 3. Adopting the median mass log M h/M☉ = 11.5 to divide the sample into “higher” and “lower” mass galaxies, we find a mass dependency for the hot circumgalactic medium kinematics. To our survey limits, O vi absorption is found in only ∼40% of the H i clouds in and around lower mass halos as compared to ∼85% around higher mass halos. For D/Rvir < 1, lower mass halos have an escape fraction of ∼65%, whereas higher mass halos have an escape fraction of ∼5%. For 1 ⩽ D/Rvir < 2, the escape fractions are ∼55% and ∼35% for lower mass and higher mass halos, respectively. For 2 ⩽ D/Rvir < 3, the escape fraction for lower mass halos is ∼90%. We show that it is highly likely that the absorbing clouds reside within 4Rvir of their host galaxies and that the kinematics are dominated by outflows. Our finding of “differential kinematics” is consistent with the scenario of “differential wind recycling” proposed by Oppenheimer et al. We discuss the implications for galaxy evolution, the stellar to halo mass function, and the mass–metallicity relationship of galaxies.
Study of star-forming galaxies in SDSS up to redshift 0.4: I. Metallicity evolution

Context. The chemical composition of the gas in galaxies over cosmic time provides a very important tool for understanding galaxy evolution. Although there are many studies at high redshift, they are rather scarce at lower redshifts. However, low redshift studies can provide important clues about the evolution of galaxies, furnishing the required link between the local and high redshift universe. In this work, we focus on the metallicity of the gas of star-forming galaxies at low redshift, looking for signs of chemical evolution. Aims. We aim to analyze the metallicity contents star-forming galaxies of similar luminosities and masses at different redshifts. With this purpose, we present a study of the metallicity of relatively massive (log(Mstar/M� ) 10.5) star forming galaxies from SDSS–DR5 (Sloan Digital Sky Survey-data release 5), using different redshift intervals from 0.04 to 0.4. Methods. We used data processed with the STARLIGHT spectral synthesis code, correcting the fluxes for dust extinction, estimating metallicities using the R23 method, and segregating the samples with respect to the value of the [N ii] λ6583/[O ii] λ3727 line ratio in order to break the R23 degeneracy selecting the upper branch. We analyze the luminosity and mass-metallicity relations, and the effect of the Sloan fiber diameter looking for possible biases. Results. By dividing our redshift samples in intervals of similar magnitude and comparing them, significant signs of metallicity evolution are found. Metallicity correlates inversely with redshift: from redshift 0 to 0.4 a decrement of ∼0.1 dex in 12 + log(O/H) is found.
Spectro-astrometry of LkCa 15 with X-Shooter: Searching for emission from LkCa 15b ?

Planet formation is one explanation for the partial clearing of dust observed in the disks of some T Tauri stars. Indeed studies using state-of-the-art high angular resolution techniques have very recently begun to observe planetary companions in these so-called transitional disks. The goal of this work is to use spectra of the transitional disk object LkCa 15 obtained with X-Shooter on the Very Large Telescope to investigate the possibility of using spectro-astrometry to detect planetary companions to T Tauri stars. It is argued that an accreting planet should contribute to the total emission of accretion tracers such as Hα and therefore planetary companions could be detected with spectro-astrometry in the same way as it has been used to detect stellar companions to young stars. A probable planetary-mass companion was recently detected in the disk of LkCa 15. Therefore, it is an ideal target for this pilot study. We studied several key accretion lines in the wavelength range 300 nm to 2.2 μm with spectro-astrometry. While no spectro-astrometric signal is measured for any emission lines, the accuracy achieved in the technique is used to place an upper limit on the contribution of the planet to the flux of the Hα, Paγ, and Paβ lines. The derived upper limits on the flux allow an upper limit of the mass accretion rate, log (Ṁacc) = −8.9 to −9.3 for the mass of the companion between 6 MJup and 15 MJup, respectively, to be estimated (with some assumptions).
Omicron variant of COVID-19: A focused review of biologic, clinical, and epidemiological changes

On 25 November 2021, the world health organization listed Omicron as a newly arisen and the fifth variant of concern (VoC) of severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2). The genome sequence of Omicron showed the utmost number of mutations compared to other known VoCs up to now, and it was regarded as the only SARS-CoV-2 variant with changes in the receptor-binding domain (RBD). However, the Omicron is still detectable via previous polymerase chain reaction (PCR) tests. Clinical presentation of the disease is identical to previous VoCs, however in vitro and in vivo studies revealed a higher transmission rate. The biggest obstacles posed by Omicron are the immune escape and reduction in vaccine effectiveness, as indicated by many simulations and real-world studies. Although the efficacy of the two-dose vaccinations is suboptimal for Omicron, preliminary studies have considered the injection of a booster shot is beneficial and can decrease the risk of severe disease. All these new features of Omicron warranted close investigation of this VoC as a new chapter in the pandemic, especially with emersion of subvariants BA.4 and BA.5. This review presents a conspectus of the current knowledge on the COVID-19 Omicron variant biological, clinical, and epidemiological changes.
How well will ton-scale dark matter direct detection experiments constrain minimal supersymmetry?

Weakly interacting massive particles (WIMPs) are amongst the most interesting dark matter (DM) candidates. Many DM candidates naturally arise in theories beyond the standard model (SM) of particle physics, like weak-scale supersymmetry (SUSY). Experiments aim to detect WIMPs by scattering, annihilation or direct production, and thereby determine the underlying theory to which they belong, along with its parameters. Here we examine the prospects for further constraining the Constrained Minimal Supersymmetric Standard Model (CMSSM) with future ton-scale direct detection experiments. We consider ton-scale extrapolations of three current experiments: CDMS, XENON and COUPP, with 1000 kg-years of raw exposure each. We assume energy resolutions, energy ranges and efficiencies similar to the current versions of the experiments, and include backgrounds at target levels. Our analysis is based on full likelihood constructions for the experiments. We also take into account present uncertainties on hadronic matrix elements for neutralino-quark couplings, and on halo model parameters. We generate synthetic data based on four benchmark points and scan over the CMSSM parameter space using nested sampling. We construct both Bayesian posterior PDFs and frequentist profile likelihoods for the model parameters, as well as the mass and various cross-sections of the lightest neutralino. Future ton-scale experiments will help substantially in constraining supersymmetry, especially when results of experiments primarily targeting spin-dependent nuclear scattering are combined with those directed more toward spin-independent interactions.
INSENTIF PAJAK MASA PANDEMI COVID-19 UNTUK UMKM : STUDI KASUS KANTOR PELAYANAN PAJAK PRATAMA TULUNGAGUNG

Tujuan penelitian adalah untuk mengetahui dan memahami sejauh mana pemanfaatan dan pelaksanaan insentif pajak ini di KPP Pratama Tulungagung. Metode penelitian yang digunakan adalah metode stud iliteratur dengan mengkaji berbagai peraturan terkait, pengumpulan data primer melalui wawancara, serta pengumpulan data sekunder. Pandemi Covid-19 yang melanda seluruh dunia, termasuk Indonesia, memberikan dampak tidak hanya di bidang kesehatan namun juga perekonomian. UMKM sebagai salah satu penopang ekonomi Indonesia juga merasakan dampak dari pandemi ini. Pemerintah memberikan insentif pajak bagi UMKM yang tertuang di dalam PMK Nomor 86 Tahun 2020 sebagaimana telah diubah dalam PMK Nomor 110 Tahun2020. Pemerintah memiliki harapan agar banyak UMKM yang berpartisipasi dalam program ini. Fakta di lapangan ternyata hanya sebagian kecil saja UMKM yang berpartisipasi dalam program ini. Penelitian meninjau kondisi di lapangan ini dan mengkaji apa yang sebenarnya terjadi mengingat adanya gap antara kebijakan dengan pelaksanaan. Penelitian mengambil studi kasus di KPP Pratama Tulungagung dengan alasan banyaknya UMKM di kabupaten tersebut serta mudahnya akses ke objek penelitian, mengingat pandemi ini membatasi ruang gerak untuk mengambil objek di luar domisili. Hasil penelitian menemukan adanya keengganan wajib pajak UMKM dalam memanfaatkan insentif karena akses teknologi yang sulit sertakurangnya manfaat langsung yang dirasakan.
The intrinsic line width of the Fe K α line of AGN

X-ray fluorescent lines are unique features of the reflection spectrum of the cold torus when irradiated by the central AGN. Their intrinsic line widths can be used to probe the line-emitting region. The line widths of the Fe \Ka line measured from the first order Chandra High Energy Grating (HEG) spectra are $3-5$ times larger than those measured with the Si \Ka line for Circinus, Mrk 3, and NGC 1068. Because the observed Si \Ka and Fe \Ka lines are not necessarily coming from the same physical region, it is uncertain whether the line widths of the Fe \Ka line are over-estimated or not. We measured the intrinsic line widths of the Fe \Ka line of several nearby bright AGN using the second and third order Chandra HEG spectra, whose spectral resolutions are better than the first order data. We found the measured widths are all smaller than those from the first order data. The results clearly show that the widths of the Fe \Ka line measured from the first order HEG data are over-estimated. It indicates that the Fe \Ka lines of the studied sources are originating from regions around the cold dusty torus.
Experimental Evidence on Group-based Attendance Bonuses in Team Production

We test the effectiveness of a group-based attendance bonus in a field experiment in a factory in Pakistan, where workers manufacture electric fans in stages using batch-production methods. We find that the group-based attendance bonus increased by more than a quarter the average number of days that the team’s attendance target was met. This effect was larger for junior and mid-level workers as compared to senior workers. We find that the bonus incentivized better coordination among workers, especially in the latter part of the month, rather than through higher average attendance. Our experiment’s results suggest that temporary incentive programmes may help workers in the transition period to new ways of organizing production and may prove to be a valuable tool for change management. Group-based bonuses offer an alternative to individual or tournament-based incentives based on one’s own or relative performance, which may have deleterious effects on intrinsic motivation and pro-social behaviour.
Emission line diagnostics to constrain high temperature populations in early-type galaxies

Once thought to be devoid of warm and cold interstellar matter, elliptical galaxies are now commonly observed to host extended regions of neutral and ionized gas. Outside of the innermost nuclear regions of these galaxies, the favoured candidate ionizing source remains some component of the stellar population, with mounting evidence suggesting post-asymptotic-giant-branch stars (pAGBs). In a recent paper, we demonstrated that observations of recombination lines of He II (or upper limits thereof) may provide a strong constraint on the presence of any other, higher temperature ionizing sources, in particular nuclear-burning white dwarfs in the context of the single degenerate (SD) scenario for type Ia supernovae. The sensitivity of the HeII test is greatest for WD effective temperatures � 2 · 10 5 K. Here we extend our analysis to include predictions for all of the “classical” strong optical lines, as well as UV, optical, and infra-red lines of neutral Oxygen, Nitrogen, and singly-ionized Carbon. This allows us to extend the temperature range over which we can meaningfully constrain the collective luminosity of nuclear-burning WDs to 10 5 K . T . 10 6 K. We then demonstrate how observations of nearby early-type and post-starburst galaxies can place strong limits on the origin of type Ia supernovae.
Suzaku Observations of Iron K-Lines from the Intracluster Medium of the Coma Cluster

The Coma cluster was observed with an X-ray Imaging Spectrometer (XIS) onboard Suzaku in six pointings, including the central X-ray peak region, the 14'west offset region, 30'and 34'north-west offset regions, and 44'and 60'south-west offset regions. Owing to its lower background level, Suzaku has better sensitivity to Fe K-alpha lines than other satellites. Using precise Fe line measurements, we studied the temperature structure, possible bulk motions, and iron abundance distributions in the intracluster medium (ICM). The observed spectra were well-represented by a single-temperature model, and two- or three- temperature model did not improve chi-square substantially. The temperature, derived from K-alpha line ratios of H-like and He-like Fe, agree with those derived from the single-temperature model. Because the line ratio is a steep function of temperature, the consistency supports the accuracy of temperature measurements conducted with Suzaku. Within the 34'region, the redshift derived from the central energy of the He-like Fe line is consistent with that from optical observations, within a calibration error of 18 eV or 818 km/s in the line of sight. This value is smaller than the sound velocity of ICM, which is 1500 km/s. The central energy of Fe lines at the 44'offset region around the NGC 4839 subcluster is also consistent with those within the 34'region. These results on the temperature and velocity structure suggest that the core of the cluster is in a relaxed state, and non-thermal electrons relevant to the radio halo are accelerated by intracluster turbulence rather than large-scale shocks. Fe abundance is almost constant at 0.4 solar within the 34'region, and decreases with radius. This value is slightly lower than those of other clusters, which means the gas have been mixed well during a past merger associated with the growth of the cluster.
Decreased functional connectivity in salience network is associated with symptom severity in betel quid‐dependent chewers

Betel quid (BQ) is the fourth most popular psychoactive agent worldwide. Neuroimaging studies have showed that substance‐addicted individuals including alcohol, heroin, nicotine and other addictive substance exhibit altered activity patterns of the salience network (SN). However, no study has yet investigated the neural correlates of the resting‐state SN and BQ dependence (BQD)‐related physiopathological characteristics.
The effects of a hot gaseous halo on disc thickening in galaxy minor mergers

We employ hydrodynamical simulations to study the effects of dissipational gas physics on the vertical heating and thickening of disc galaxies during minor mergers. For the first time we present a suite of simulations that includes a diffuse, rotating, cooling, hot gaseous halo, as predicted by cosmological hydrodynamical simulations as well as models of galaxy formation. We study the effect of this new gaseous component on the vertical structure of a Milky Way-like stellar disc during 1:10 and 1:5 mergers. For 1:10 mergers, we find no increased final thin disc scale height compared to the isolated simulation, leading to the conclusion that thin discs can be present even after a 1:10 merger if a reasonable amount of hot gas is present. The reason for this is the accretion of new cold gas, leading to the formation of a massive new thin stellar disc that dominates the surface brightness profile. In a previous study, in which we included only cold gas in the disc, we showed that the presence of cold gas decreased the thickening by a minor merger relative to the no-gas case. Here, we show that the evolution of the scale height in the presence of a cooling hot halo is dominated by the formation of the new stellar disc. In this scenario, the thick disc is the old stellar disc that has been thickened in a minor merger at z≳ 1, while the thin disc is the new stellar disc that reforms after this merger. When galactic winds are also considered, the final scale height is larger due to two effects. First, the winds reduce the star formation rate, leading to a less massive new stellar disc, such that the thickened old disc still dominates. Secondly, the winds exert a pressure force on the gas in the disc, leading to a shallower gas profile and thus to a thicker new stellar disc. In addition, we study the evolution of the scale height during a 1:5 merger and find that a thin disc can be present even after this merger, provided enough hot gas is available. The final scale height in our simulations depends on the mass of the hot gaseous halo, the efficiency of the winds and the merger mass ratio. We find post-merger values in the range 0.5 ≲z0≲ 1.0 kpc in good agreement with observational constraints by local galaxies.
COMPARING SINGLE-EPOCH VIRIAL BLACK HOLE MASS ESTIMATORS FOR LUMINOUS QUASARS

Single-epoch virial black hole (BH) mass estimators utilizing broad emission lines have been routinely applied to high-redshift quasars to estimate their BH masses. Depending on the redshift, different line estimators (Hα, Hβ, Mg ii λ2798, C iv λ1549) are often used with optical/near-infrared spectroscopy. Here, we use a homogeneous sample of 60 intermediate-redshift (z ∼ 1.5–2.2) Sloan Digital Sky Survey quasars with optical and near-infrared spectra covering C iv through Hα to investigate the consistency between different single-epoch virial BH mass estimators. We critically compare rest-frame UV line estimators (C iv λ1549, C iii] λ1908, and Mg ii λ2798) with optical estimators (Hβ and Hα) in terms of correlations between line widths and between continuum/line luminosities, for the high-luminosity regime (L5100 > 1045.4 erg s−1) probed by our sample. The continuum luminosities of L1350 and L3000, and the broad-line luminosities are well correlated with L5100, reflecting the homogeneity of quasar spectra in the rest-frame UV–optical, among which L1350 and the line luminosities for C iv and C iii] have the largest scatter in the correlation with L5100. We found that the Mg ii FWHM correlates well with the FWHMs of the Balmer lines and that the Mg ii line estimator can be calibrated to yield consistent virial mass estimates with those based on the Hβ/Hα estimators, thus extending earlier results on less luminous objects. The C iv FWHM is poorly correlated with the Balmer line FWHMs, and the scatter between the C iv and Hβ FWHMs consists of an irreducible part (∼0.12 dex), and a part that correlates with the blueshift of the C iv centroid relative to that of Hβ, similar to earlier studies comparing C iv with Mg ii. The C iii] FWHM is found to correlate with the C iv FWHM, and hence is also poorly correlated with the Hβ FWHM. While the C iv and C iii] lines can be calibrated to yield consistent virial mass estimates as Hβ on average, the scatter is substantially larger than Mg ii, and the usage of C iv/C iii] FWHM in the mass estimators does not improve the agreement with the Hβ estimator. We discuss controversial claims in the literature on the correlation between C iv and Hβ FWHMs, and suggest that the reported correlation is either a result based on small samples or only valid for low-luminosity objects.
Relativistic corrections to the exclusive decays of C-even bottomonia into S-wave charmonium pairs

Within the nonrelativistic quantum chromodynamics (NRQCD) factorization formalism, we compute the relativistic corrections to the exclusive decays of bottomonia with even charge conjugation parity into S-wave charmonium pairs at leading order in the strong coupling constant. Relativistic corrections are resummed for a class of color-singlet contributions to all orders in the charm-quark velocity v(c) in the charmonium rest frame. Almost every process that we consider in this work has negative relativistic corrections ranging from -20 to -35%. Among the various processes, the relativistic corrections of the next-to-leading order in v(c) to the decay rate for chi(b2) -> eta(c)(mS) + eta(c)(nS) with m, n = 1 or 2 are very large. In every case, the resummation of the relativistic corrections enhances the rate in comparison with the next-to-leading-order results. We compare our results with available predictions based on the NRQCD factorization formalism. The NRQCD predictions are significantly smaller than those based on the light-cone formalism by 1 or 2 orders of magnitude.
Transport enhancement and suppression in turbulent magnetic reconnection: A self-consistent turbulence modela)

Through the enhancement of transport, turbulence is expected to contribute to the fast reconnection. However, the effects of turbulence are not so straightforward. In addition to the enhancement of transport, turbulence under some environment shows effects that suppress the transport. In the presence of turbulent cross helicity, such dynamic balance between the transport enhancement and suppression occurs. As this result of dynamic balance, the region of effective enhanced magnetic diffusivity is confined to a narrow region, leading to the fast reconnection. In order to confirm this idea, a self-consistent turbulence model for the magnetic reconnection is proposed. With the aid of numerical simulations where turbulence effects are incorporated in a consistent manner through the turbulence model, the dynamic balance in the turbulence magnetic reconnection is confirmed.
Universal Fluctuation-Driven Eccentricities in Proton-Proton, Proton-Nucleus, and Nucleus-Nucleus Collisions

We show that the statistics of fluctuation-driven initial-state anisotropies in proton-proton, proton nucleus and nucleus-nucleus collisions is to a large extent universal. We propose a simple parametrization for the probability distribution of the Fourier coefficient ${ϵ}_{n}$ in harmonic $n$, which is in good agreement with Monte Carlo simulations. Our results provide a simple explanation for the 4-particle cumulant of triangular flow measured in Pb-Pb collisions and for the 4-particle cumulant of elliptic flow recently measured in $p\text{\ensuremath{-}}\mathrm{Pb}$ collisions. Both arise as natural consequences of the condition that initial anisotropies are bounded by unity. We argue that the initial rms anisotropy in harmonic $n$ can be directly extracted from the measured ratio ${v}_{n}{4}/{v}_{n}{2}$: this gives direct access to a property of the initial density profile from experimental data. We also make quantitative predictions for the small lifting of degeneracy between ${v}_{n}{4}$, ${v}_{n}{6}$, and ${v}_{n}{8}$. If confirmed by future experiments, they will support the picture that long-range correlations observed in $p\text{\ensuremath{-}}\mathrm{Pb}$ collisions at the LHC originate from collective flow proportional to the initial anisotropy.