Miracle-dz/UniFAR-FTUs huggingface dataset:
Effects of Different Organ Metastases on the Prognosis of Stage IV Urothelial Carcinoma of the Bladder

Objective To assess the prognosis of stage IV metastatic urinary bladder urothelial carcinoma (UBUC) at initial diagnosis and determine prognostic factors based on distant organ metastasis. Methods A retrospective cohort analysis of UBUC was conducted based on the Surveillance, Epidemiology, and End Results (SEER) database. Univariate and multivariate Cox regression analyses were used to determine the variables associated with overall survival (OS). Kaplan–Meier curves were used to compare survival curves among different groups. Results A total of 3103 patients with stage IV UBUC were selected for analysis. The number of distant organ metastatic sites independently predicted the OS. The OS was not different in other metastatic sites when bone metastasis was used as a reference (P > 0.05). However, the OS was shorter for a single metastatic site (P < 0.001) and multiple metastatic sites when metastasis was not used as a reference (P < 0.001). Multivariable Cox regression analysis indicated that low survivorship was independently associated with no surgery for the entire cohort and patients with only one metastatic organ. Sex (P = 0.019) and grade (P = 0.046) were the independent risk factors for patients with only one metastatic organ. Conclusions These results show that the prognosis of stage IV metastatic UBUC is not different between any single metastatic organ. The prognosis of stage IV metastatic UBUC depends on the number of distant organ metastasis. This study determined some predictors of survival and thus may help therapists to choose appropriate treatment strategies for metastatic UBUC.
Minimal temperature of quantum refrigerators

A first-principle reciprocating quantum refrigerator is investigated to determine the limitations of cooling to absolute zero. If the energy spectrum of the working medium possesses an uncontrollable gap, then there is a minimum achievable temperature above zero. Such a gap, combined with a negligible amount of noise, prevents adiabatic following during the expansion stage which is the necessary condition for reaching Tc→0.
The ionized absorber and nuclear environment of IRAS 13349+2438: multi-wavelength insights from coordinated Chandra HETGS, HST STIS, HET and Spitzer IRS

We present results from a multiwavelength IR‐to‐X-ray campaign of the infrared bright (but highly optical-UV extincted) QSO IRAS 13349+2438 obtained with the Chandra High Energy Transmission Grating Spectrometer (HETGS), the Hubble Space Telescope Space Telescope Imaging Spectrograph (STIS), the Hobby-Eberly Telescope (HET) 8-meter, and the Spitzer Infrared Spectrometer (IRS). Based on HET optical spectra of [O III], we refine the redshift of IRAS 13349 to be z = 0.10853. The weakness of the [O III] in combination with strong Fe II in the HET spectra reveal extreme Eigenvector-1 characteristics in IRAS 13349, but the 2468 kms −1 width of the Hβ line argues against a narrow-line Seyfert 1 classification; on average, IR, optical and UV spectra show I RAS 13349 to be a typical QSO. Independent estimates based on the Hβ line width and fits to the IRAS 13349 SED both give a black hole mass of MBH = 10 9 M⊙. The heavily reddened STIS UV spectra reveal for the first time blue-shifted absorption from Ly α, N V and 4 with components at systemic velocities of 950 kms −1 and 75 kms −1 . The higher velocity UV lines are coincident with the lower-ionisation (ξ � 1.6) WA-1 warm absorber lines seen in the X-rays with the HETGS. In addition, a ξ � 3.4 WA-2 is also required by the data, while a ξ � 3 WA-3 is predicted by theory, and seen at less significance; all detected X-ray a bsorption lines are blueshifted by � 700 900kms −1 . Theoretical models comparing different ionising SEDs reveal that including the UV (i.e., the accretion disc) as part of the ion ising continuum has strong implications for the conclusions one would draw about the thermodynamic stability of the warm absorber. Specific to IRAS 13349, we find that an X-ray-UV ioni sing SED favors a continuous distribution of ionisation states in a smooth flow (this paper), versus discrete clouds in pressure equilibrium (previous work by other authors). Direct detections of dust are seen in both the IR and X-rays. We see weak PAH emission at 7. 7µm and 11. 3µm which may also be blended with forsterite, and 10 µm and 18µm silicate emission, as well as an Fe L edge at 700 eV indicative of iron-base dust with a dust-to-gas ratio > 90%. We develop a geometrical model in which we view the nuclear regions of the QSO along a line of sight that passes through the upper atmosphere of an obscuring torus. This sight line is largely transparent in Xrays since the gas is ionised, but it is completely obscured b y dust that blocks a direct view of the UV/optical emission region. In the context of our model, 20% of the intrinsic UV/optical continuum is scattered into our sight line by the far wall of a n obscuring torus. An additional 2.4% of the direct light, which likely dominates the UV emission, is Thomson-scattered into our line-of-sight by another off-plane component of highly ionized gas.
Symmetric Gapped Interfaces of SPT and SET States: Systematic Constructions

Symmetry protected topological (SPT) states have boundary 't Hooft anomalies that obstruct an effective boundary theory realized in its own dimension with UV completion and an on-site $G$-symmetry. In this work, yet we show that a certain anomalous non-on-site $G$ symmetry along the boundary becomes on-site when viewed as an extended $H$ symmetry, via a suitable group extension $1\to K\to H\to G\to1$. Namely, a non-perturbative global (gauge/gravitational) anomaly in $G$ becomes anomaly-free in $H$. This guides us to construct exactly soluble lattice path integral and Hamiltonian of symmetric gapped boundaries, always existent for any SPT state in any spacetime dimension $d \geq 2$ of any finite symmetry group, including on-site unitary and anti-unitary time-reversal symmetries. The resulting symmetric gapped boundary can be described either by an $H$-symmetry extended boundary of bulk $d \geq 2$, or more naturally by a topological emergent $K$-gauge theory with a global symmetry $G$ on a 3+1D bulk or above. The excitations on such a symmetric topologically ordered boundary can carry fractional quantum numbers of the symmetry $G$, described by representations of $H$. (Apply our approach to a 1+1D boundary of 2+1D bulk, we find that a deconfined gauge boundary indeed has spontaneous symmetry breaking with long-range order. The deconfined symmetry-breaking phase crosses over smoothly to a confined phase without a phase transition.) In contrast to known gapped interfaces obtained via symmetry breaking (either global symmetry breaking or Anderson-Higgs mechanism for gauge theory), our approach is based on symmetry extension. More generally, applying our approach to SPT, topologically ordered gauge theories and symmetry enriched topologically ordered (SET) states, leads to generic boundaries/interfaces constructed with a mixture of symmetry breaking, symmetry extension, and dynamical gauging.
Modifying unhealthy behaviors among primary school children

Background: Unhealthy behaviors among primary school children arise during childhood, which often persist into adulthood, affecting health and well-being in later life. These unhealthy behaviors are represented in the misuse use of technology, bullying, smoking and anxiety. Aim of the Study: This study aimed to evaluate the impact of the educational health program on modifying unhealthy behaviors among primary school children. Design: Quasi-experimental was utilized to achieve the aim of the study. Setting: The study was conducted in the Sharabeya area affiliated to the Sharabeya Educational Administration of the Directorate of Education in Cairo, which includes many primary schools. Sample: A Multistage sample was selected randomly it compromised of 124 primary school children. Tools: Two tools were used for data collection, first tool: An interviewing questionnaire for primary school children including two parts; Part I:Demographic characteristics of the children, Part II: children's knowledge about unhealthy behaviors. Second tool: Assessing children reported practices about unhealthy behaviors. Results: the main results of the study revealed that, significant improvement in children knowledge and their reported practices regarding unhealthy behaviors. Conclusions: the study concluded that the educational health program remarked improvement all items of knowledge and reported practice of children related to unhealthy behavior.
Generation of radiative knots in a randomly pulsed protostellar jet I. Dynamics and energetics

Context. Herbig-Haro objects are characterized by a complex knotty morphology detected mainly along the axis of protostellar jets in a wide range of bands: from radio to IR to optical bands, with X-rays knots also detected in the last few years. Evidence of intera ctions between knots formed in different epochs have been found, suggesting that jets may result from the ejection of plasma blobs from the stellar source. Aims. We aim at investigating the physical mechanism leading to the irregular knotty structure observed in protostellar jets in different wavelength bands and the complex interactions occurring among blobs of plasma ejected from the stellar source. Methods. We perform 2D axisymmetric hydrodynamic numerical simulations of a randomly ejected pulsed jet. The jet consists of a tr ain of blobs which ram with supersonic speed into the ambient medium. The initial random velocity of each blob follows an exponential distribution. We explore the ejection rate parameter in order to derive constraints on the physical properties of protostellar jets by comparison of model results with observations. Our model takes into account the effects of radiative losses and thermal conduction. Results. We find that the mutual interactions of blobs ejected at diffe rent epochs and with different speed lead to a variety of plasma components not described by current models of jets. The main features characterizing the random pulsed jet scenario are: single high speed knots, showing a measurable proper motion in nice agreement with optical and X-rays observations; irregular chains of knots aligned along the jet axis and possibly interacting with each other; rever se shocks interacting with outgoing knots; oblique shock patterns produced by the reflection of shocks at the cocoon surrounding the jet. Al l these structures concur to determine the morphology of the jet in different wavelength bands. We also find that the thermal conduction pl ays a crucial role in damping out hydrodynamic instabilities that would develop within the cocoon and that contribute to the jet breaking.
SOPHIE velocimetry of Kepler transit candidates VII. A false-positive rate of 35% for Kepler close-in giant candidates

The false-positive probability (FPP) of Kepler transiting candidates is a key value for statistical studies of candidate properties. A previous investigation of the stellar population in the Kepler field has provided an estimate for the FPP of less than 5% for most of the candidates. We report here the results of our radial velocity observations on a sample of 46 Kepler candidates with a transit depth greater than 0.4%, orbital period less than 25 days and host star brighter than Kepler magnitude 14.7. We used the SOPHIE spectrograph mounted on the 1.93-m telescope at the Observatoire de Haute-Provence to establish the nature of the transiting candidates. In this sample, we found five undiluted eclipsing binaries, two brown dwarfs, six diluted eclipsing binaries, and nine new transiting planets that complement the 11 already published planets. The remaining 13 candidates were not followed-up or remain unsolved due to photon noise limitation or lack of observations. From these results we computed the FPP for Kepler close-in giant candidates to be 34.8% +/- 6.5%. We aimed to investigate the variation of the FPP for giant candidates with the longer orbital periods and found that it should be constant for orbital periods between 10 and 200 days. This significantly disagrees with the previous estimates. We discuss the reasons for this discrepancy and the possible extension of this work toward smaller planet candidates. Finally, taking the false-positive rate into account, we refined the occurrence rate of hot Jupiters from the Kepler data.
Microbiota of Dental Abscess and their Susceptibility to Empirical Antibiotic Therapy

Context: Resistant pathogens to purulent odontogenic infections have evolved due to misuse of antibiotics. Hence, it is important to use a suitable antibacterial agent. Aim: This study aimed to identify the common bacterial species causing odontogenic infections and to determine their antibiotic susceptibility profile to amoxicillin, amoxicillin and clavulanic acid, azithromycin, and linezolid. Settings and Design: This was an in vitro cross-sectional study. Material and Methods: Fifty pus samples from odontogenic abscess were cultured and antibiotic susceptibility tests were performed as per the standard microbiological procedures. Statistical Analysis Used: Binomial test and Pearson's Chi-square test were used for statistical analysis. Results: Out of the 50 samples cultured, 30 samples showed growth. The distribution of growth among the 30 samples was Gram-positive cocci (n = 23, 67.65%) and Gram-negative bacilli (n = 11, 32.35%). Gram-positive isolates that were grown were Enterococcus faecalis (38.24%) followed by Staphylococcus aureus (29.41%) and Gram-negative bacilli that were isolated were Klebsiella pneumoniae (14.71%), Pseudomonas aeruginosa (8.82%), Escherichia coli (5.88%), and Enterobacter (2.94%). Enterococcus isolates were highly susceptible to amoxicillin (76.92%). An increase in the zone of inhibition to amoxicillin–clavulanic acid was appreciated more for Staphylococcus (50%) than Enterococcus (30.76%). Enterococcus and Staphylococcus showed high susceptibility of 92.31% and 90% to linezolid, respectively. E. coli and Enterobacter were 100% susceptible to amoxicillin. All the Gram-negative bacteria except for P. aeruginosa were 100% highly susceptible to amoxicillin–clavulanic acid. Conclusions: Culture-guided antibiotic prescriptions are necessary to prevent the emergence of antibiotic-resistant bacteria.
Proﬁnite groups with a cyclotomic p -orientation

Let p be a prime. A continuous representation θ : G → GL 1 ( Z p ) of a proﬁnite group G is called a cyclotomic p -orientation if for all open subgroups U ⊆ G and for all k, n ≥ 1 the natural maps H k ( U, Z p ( k ) /p n ) −→ H k ( U, Z p ( k ) /p ) are surjective. Here Z p ( k ) denotes the Z p -module of rank 1 with U - action induced by θ | kU . By the Rost-Voevodsky theorem, the cyclotomic character of the absolute Galois group G K of a ﬁeld K is, indeed, a cyclo-tomic p -orientation of G K . We study proﬁnite groups with a cyclotomic p -orientation. In particular, we show that cyclotomicity is preserved by several operations on proﬁnite groups, and that Bloch-Kato pro-p groups with a cyclotomic p -orientation satisfy a strong form of Tits’ alternative and decompose as semi-direct product over a canonical abelian closed normal subgroup.
Lyα COOLING EMISSION FROM GALAXY FORMATION

Recent numerical and analytical studies have shown that galaxies accrete most of their baryons via the cold mode, from streams with temperatures T ∼ 104–105 K. At these temperatures, the streams should radiate primarily in the Lyα line and have therefore been proposed as a model to power the extended, high-redshift objects known as Lyα blobs, and may also be relevant for powering a range of less luminous Lyα sources. We introduce a new Lyα radiative transfer code, αRT, and calculate the transport of the Lyα emission from cold accretion in cosmological hydrodynamical simulations. In this paper, we describe our methodology, and address physical and numerical issues that are critical to making accurate predictions for the cooling luminosity, but that have been mostly neglected or treated simplistically so far. In particular, we highlight the importance of self-shielding and of properly treating sub-resolution models in numerical simulations. Most existing simulations do not self-consistently incorporate these effects, which can lead to order-of-magnitude errors in the predicted cooling luminosity. Using a combination of post-processing ionizing radiative transfer and re-simulation techniques, we develop an approximation to the consistent evolution of the self-shielded gas. We quantify the dependence of the Lyα cooling luminosity on halo mass at z = 3 for the simplified problem of pure gas accretion embedded in the cosmic radiation background and without feedback, and present radiative transfer results for a particular system. While pure cooling in massive halos (without additional energy input from star formation and active galactic nuclei) is in principle sufficient to produce Lα ∼ 1043–1044 erg s−1 blobs, this requires including energy released in gas of density sufficient to form stars, but which is kept 100% gaseous in our optimistic estimates. Excluding emission from such dense gas yields lower luminosities by up to one to two orders of magnitude at high masses, making it difficult to explain the observed Lyα blobs with pure cooling. Resonant scattering produces diffuse Lyα halos, even for centrally concentrated emission, and broad double peaked line profiles. In particular, the emergent line widths are in general not representative of the velocity dispersion within galactic halos and cannot be directly used to infer host halo masses.
Analysis of possible systematic errors in the Oslo method

In this work, we have reviewed the Oslo method, which enables the simultaneous extraction of the level density and {gamma}-ray transmission coefficient from a set of particle-{gamma} coincidence data. Possible errors and uncertainties have been investigated. Typical data sets from various mass regions as well as simulated data have been tested against the assumptions behind the data analysis.
TWO TIMESCALE DISPERSAL OF MAGNETIZED PROTOPLANETARY DISKS

Protoplanetary disks are likely to be threaded by a weak net flux of vertical magnetic field that is a remnant of the much larger fluxes present in molecular cloud cores. If this flux is approximately conserved its dynamical importance will increase as mass is accreted, initially by stimulating magnetorotational disk turbulence and subsequently by enabling wind angular momentum loss. We use fits to numerical simulations of ambipolar dominated disk turbulence to construct simplified one-dimensional evolution models for weakly magnetized protoplanetary disks. We show that the late onset of significant angular momentum loss in a wind can give rise to “two timescale” disk evolution in which a long phase of viscous evolution precedes rapid dispersal as the wind becomes dominant. The wide dispersion in disk lifetimes could therefore be due to varying initial levels of net flux. Magnetohydrodynamic (MHD) wind triggered dispersal differs from photoevaporative dispersal in predicting mass loss from small (<1 AU) scales, where thermal winds are suppressed. Our specific models are based on a limited set of simulations that remain uncertain, but qualitatively similar evolution appears likely if mass is lost from disks more quickly than flux, and if MHD winds become important as the plasma β decreases.
Modul Nusantara: Mengembangkan Karakter Mahasiswa dalam Kelas Multikultural

Beberapa mahasiswa menjadikan agama sebagai lelucon, ada pula mahasiswa yang memotong pembicaraan disaat temannya sedang berbicara. Sebagian mahasiswa merasa bangga menggunakan produk-produk luar negeri baik pakaian, handphone, dan semua yang melekat pada kebutuhan mereka. Penelitian ini bertujuan untuk menganalisis karakter yang terdapat pada mahasiswa dalam kelas multikultural di kegiatan modul nusantara. Penelitian ini merupakan penelitian kualitatif deskriptif. Subjek penelitian merupakan mahasiswa luring yang berjumalah 9 orang. Instrumen penelitian yang digunakan adalah wawancara, observasi, dan dokumentasi. Teknik analisis data dalam penelitian ini yaitu reduksi data, penyajian data, dan kesimpulan. Keabsahan data menggunakan triangulasi sumber dengan menguji kredibilitas data dilakukan dengan cara mengecek data yang telah diperoleh melalui beberapa sumber. Hasil penelitian menunjukkan bahwa kegiatan ini sangat menekankan pada karakter toleransi dan cinta tanah air mahasiswa. Hal ini terlihat dari hasil presentasi sebesar 66% untuk karakter toleransi dan 67% untuk karakter cinta tanah air. Program modul nusantara yang mengedepankan nilai toleransi ini sangat penting bagi mahasiswa selain itu dapat mencegah terjadinya isu buruk sesama bangsa Indonesia. Program ini juga membuat mahasiswa bangga terhadap negaranya sendiri dan terciptanya nilai cinta tanah air dan rasa nasionalisme dalam diri mahasiswa.
ON THE ORIGIN OF LOPSIDEDNESS IN GALAXIES AS DETERMINED FROM THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G)

We study the m = 1 distortions (lopsidedness) in the stellar components of 167 nearby galaxies that span a wide range of morphologies and luminosities. We confirm the previous findings of (1) a high incidence of lopsidedness in the stellar distributions, (2) increasing lopsidedness as a function of radius out to at least 3.5 exponential scale lengths, and (3) greater lopsidedness, over these radii, for galaxies of later type and lower surface brightness. Additionally, the magnitude of the lopsidedness (1) correlates with the character of the spiral arms (stronger arm patterns occur in galaxies with less lopsidedness), (2) is not correlated with the presence or absence of a bar, or the strength of the bar when one is present, (3) is inversely correlated to the stellar mass fraction, f*, within one radial scale length, and (4) correlates directly with f* measured within the radial range over which we measure lopsidedness. We interpret these findings to mean that lopsidedness is a generic feature of galaxies and does not, generally, depend on a rare event, such as a direct accretion of a satellite galaxy onto the disk of the parent galaxy. While lopsidedness may be caused by several phenomena, moderate lopsidedness (〈A1〉i + 〈A1〉o)/2 < 0.3) is likely to reflect halo asymmetries to which the disk responds or a gravitationally self-generated mode. We hypothesize that the magnitude of the stellar response depends both on how centrally concentrated the stars are with respect to the dark matter and whether there are enough stars in the region of the lopsidedness that self-gravity is dynamically important.