Miracle-dz/UniFAR-FTUs huggingface dataset:
The Nature of Star Formation in Distant Ultraluminous Infrared Galaxies Selected in a Remarkably Narrow Redshift Range

We present mid-infrared spectra of 32 high-redshift ultraluminous infrared galaxies, selected via the stellar photospheric feature at rest-frame 1.6 μm, and an observed-frame 24 μm flux of >500 μJy. Nearly all the sample reside in a redshift range of ⟨ z⟩ = 1.71 ± 0.15 and have rest-frame 1-1000 μm luminosities of 1012.9-1013.8 L☉. Most of the spectra exhibit prominent polycyclic aromatic hydrocarbon emission features and weak silicate absorption, consistent with a starburst origin for the IR emission. Our selection method appears to be a straightforward and efficient way of finding distant, IR-luminous, star-forming galaxies in narrow redshift ranges. There is, however, evidence that the mid-IR spectra of our sample differ systematically from those of local ULIRGs; our sample have comparable PAH equivalent widths but weaker apparent silicate absorption, and (possibly) enhanced PAH 6.2 μm/7.7 μm and 6.2 μm/11.2 μm flux ratios. Furthermore, the composite mid-IR spectrum of our sample is almost identical to that of local starbursts with IR luminosities of 1010-1011 L☉, rather than that of local ULIRGs. These differences are consistent with a reduced dust column, which can plausibly be obtained via some combination of (1) star formation that is extended over spatial scales of 1-4 kpc and (2) star formation in unusually gas-rich regions.
Separation of Energy Scales in Undoped YbRh2Si2 Under Hydrostatic Pressure

The temperature–magnetic field ( T – H ) phase diagram of YbRh 2 Si 2 in the vicinity of its quantum critical point is investigated by low- T magnetization measurements. Our analysis reveals that the energy scale \(T^{\star}(H)\), previously related to the Kondo breakdown and terminating at 0.06 T for T →0, remains unchanged under pressure, whereas the antiferromagnetic critical field increases from 0.06 T ( P =0) to 0.29 T ( P =1.28 GPa), resulting in a crossing of T N ( H ) and \(T^{\star}(H)\). Our results are very similar to those on Yb(Rh 1- x Co x ) 2 Si 2 , proving that the Co-induced disorder can not be the reason for the detachment of both scales under chemical pressure.
β-Ensembles for Toric Orbifold Partition Function

We investigate combinatorics of the instanton partition function for the generic four dimensional toric orbifolds. It is shown that the orbifold projection can be implemented by taking the inhomogeneous root of unity limit of the q-deformed partition function. The asymptotics of the combinatorial partition function yields the multi-matrix model for a generic β. Subject Index: 135, 183
Decentralized State Estimation-Based Optimal Integral Model Predictive Control of Voltage and Frequency in the Distribution System Microgrids

The power distribution system is undergoing a shift from centralized to decentralized operation due to the large-scale integration of distributed energy resources (DER). To increase the scalability and reduce the dependency on communication networks, there is a strong need for a decentralized control framework that can maintain the nominal voltage and frequency in a microgrid. In this article, a novel decentralized state estimation-based optimal voltage and frequency restoration strategy is proposed. The framework computes the optimal integral model predicted control reference signal to the primary controller, that is unaffected by the local measurement noise, hence, ensuring stable power-sharing among the DERs. The proposed framework is built on a first-order DER model and a local/global measurements-based local state estimation technique, facilitating deployability to the grid edge devices. The capabilities of the proposed framework are tested and validated on a real-time simulator with a full system dynamic model considering an islanded section of the IEEE 123 node distribution network for the various grid events. It is observed that the framework offers significant transient performance improvement in comparison to the Linear Quadratic Regulator method, with around 70% faster voltage restoration when the communication latency is considered.
Cosmic microwave background observables of small field models of inflation

We construct a class of single small field models of inflation that can predict, contrary to popular wisdom, an observable gravitational wave signal in the cosmic microwave background anisotropies. The spectral index, its running, the tensor to scalar ratio and the number of e-folds can cover all the parameter space currently allowed by cosmological observations. A unique feature of models in this class is their ability to predict a negative spectral index running in accordance with recent cosmic microwave background observations. We discuss the new class of models from an effective field theory perspective and show that if the dimensionless trilinear coupling is small, as required for consistency, then the observed spectral index running implies a high scale of inflation and hence an observable gravitational wave signal. All the models share a distinct prediction of higher power at smaller scales, making them easy targets for detection.
ON THE GAS TEMPERATURE OF MOLECULAR CLOUD CORES

We investigate the uncertainties affecting the temperature profiles of dense cores of interstellar clouds. In regions shielded from external ultraviolet radiation, the problem is reduced to the balance between cosmic ray heating, line cooling, and the coupling between gas and dust. We show that variations in the gas phase abundances, the grain size distribution, and the velocity field can each change the predicted core temperatures by 1 or 2 K. We emphasize the role of non-local radiative transfer effects that often are not taken into account, for example, when modeling the core chemistry. These include the radiative coupling between regions of different temperature and the enhanced line cooling near the cloud surface. The uncertainty of the temperature profiles does not necessarily translate to a significant error in the column density derived from observations. However, depletion processes are very temperature sensitive and a 2 K difference can mean that a given molecule no longer traces the physical conditions in the core center.
Effective field theory for Higgs boson plus jet production

We use an effective field theory (EFT) which includes all possible gluon-Higgs dimension-5 and dimension-7 operators to study Higgs boson plus jet production in next-to-leading order QCD. The EFT sheds light on the effect of a finite top quark mass as well as any Beyond-the-Standard Model (BSM) modifications of Higgs-gluon effective couplings. In the gluon channel, the accuracy of the heavy-top approximation for differential distributions arises from the non-interference between the helicity amplitudes of the G^3 h and G^2 h operators in the m_h < p_T limit at lowest order. One dimension-7 operator involving quark bilinears, however, contributes significantly at high p_T, and potentially offers a channel for seeing BSM effects. One-loop renormalization of these operators is determined, allowing resummation of large logarithms via renormalization group running. NLO numerical results at the LHC are presented, which include O(1/m_t^2) contributions in the SM limit.
The risks of attrition bias in longitudinal surveys of the impact of COVID-19

Abstract As the COVID-19 pandemic continues, interest in mental health impacts is shifting from short-term to long-term outcomes. As part of a longitudinal online survey study examining mental health impacts of the pandemic, we assessed the risk of attrition bias related to a history of depression—a condition research shows can increase challenges of recruitment and retention. Among 5023 participants who completed the baseline survey, significantly more reporting a history of depression were lost to follow-up: baseline to 3 months: 497/760 (65.4%) vs 2228/4263 (52.3%), P < 0.001; 3 to 6 months: 179/263 (68.1%) vs 1183/2035 (58.1%), P = 0.002. Participants reporting a history of depression also had greater adjusted odds of a Patient Health Questionnaire-8 score ≥10 (odds ratio [OR] = 3.97, 95% confidence interval [CI] 3.27, 4.84), Generalized Anxiety Disorder-7 score ≥10 (OR = 3.77, 95% CI 3.07, 4.62), and Posttraumatic Diagnostic Scale for DSM V score ≥ 28 (OR = 7.17, 95% CI 4.67, 11.00) at baseline, indicating a need to account for attrition bias when examining these outcomes. Similar considerations likely apply to other longitudinal survey studies and are important to address to ensure accurate evidence is available to support policy decisions regarding resource allocation and funding.
Smooth X-ray variability from Ophiuchi A+B. A strongly magnetized primary B2 star?

X-rays from massive stars are ubiquitous yet not clearly understood. In an XMM-Newton observation devoted to observe the first site of star formation in the Ophiuchi dark cloud, we detect smoothly variable X-ray emission from the B2IV+B2V system of Ophiuchi. Tentatively we assign the emission to the primary component. The light curve of the pn camera shows a first phase of low, almost steady rate, then a rise phase of duration of 10 ks, followed by a high rate phase. The variability is seen primarily in the band 1.0-8.0 keV while little variability is detected below 1 keV. The spectral analysis of the three phases reveals the presence of a hot component at 3.0 keV that adds up to two relatively cold components at 0.9 keV and 2.2 keV. We explain the smooth variability with the emergence of an extended active region on the surface of the primary star due to its fast rotation (vsin i 315 km/s). We estimate that the region has diameter in the range 0:5 0:6 R . The hard X-ray emission and its variability hint a magnetic origin, as suggested for few other late-O early-B type stars. We also discuss an alternative explanation based on the emergence from occultation of a young (5-10 Myr) low mass companion bright and hot in X-rays.
A LUMINOUS BLUE VARIABLE STAR INTERACTING WITH A NEARBY INFRARED DARK CLOUD

G79.29+0.46 is a nebula created by a luminous blue variable (LBV) star candidate characterized by two almost circular concentric shells. In order to investigate whether the shells are interacting with the infrared dark cloud (IRDC) G79.3+0.3 located at the southwestern border of the inner shell, we conducted Jansky Very Large Array observations of NH3(1, 1), (2, 2) and c-C3H2, and combined them with previous Effelsberg data. The overall NH3 emission consists of one main clump, named G79A, elongated following the shape of the IRDC, plus two fainter and smaller cores to the north, which spatially match the inner infrared shell. We analyzed the NH3 spectra at each position with detected emission and inferred linewidth, rotational temperature, column density, and abundance maps, and find that: (1) the linewidth of NH3(1, 1) in the northern cores is 0.5 km s−1, slightly larger than in their surroundings; (2) the NH3 abundance is enhanced by almost one order of magnitude toward the northwestern side of G79A; (3) there is one “hot slab” at the interface between the inner infrared shell and the NH3 peak of G79A; and (4) the western and southern edges of G79A present chemical differentiation, with c-C3H2 tracing more external layers than NH3, similar to what is found in photon-dominated regions. Overall, the kinematics and physical conditions of G79A are consistent with both shock-induced and UV radiation-induced chemistry driven by the LBV star. Therefore, the IRDC is not likely associated with the star-forming region DR15, but located farther away, near G79.29+0.46 at 1.4 kpc.
Natural inflation with multiple sub-Planckian axions

We extend the Kim-Nilles-Peloso (KNP) alignment mechanism for natural inflation to models with N > 2 axions, which obtains super-Planckian effective axion decay constant f eff ≫ M Pl through an alignment of the anomaly coefficients of multiple axions having sub-Planckian fundamental decay constants f 0 ≪ M Pl . The original version of the KNP mechanism realized with two axions requires that some of the anomaly coefficients should be of the order of f eff / f 0 , which would be uncomfortably large if f eff / f 0 ≳ O ( 100 ) as suggested by the recent BICEP2 results. We note that the KNP mechanism can be realized with the anomaly coefficients of O ( 1 ) if the number of axions N is large as N ln N ≳ 2 ln ( f eff / f 0 ) , in which case the effective decay constant can be enhanced as f eff / f 0 ∼ N ! n N − 1 for n denoting the typical size of the integer-valued anomaly coefficients. Comparing to the other multiple axion scenario, the N -flation scenario which requires N ∼ f eff 2 / f 0 2 , the KNP mechanism has a virtue of not invoking to a too large number of axions, although it requires a specific alignment of the anomaly coefficients, which can be achieved with a probability of O ( f 0 / f eff ) under a random choice of the anomaly coefficients. We also present a simple model realizing a multiple axion monodromy along the inflaton direction.
Renormalization group properties of scalar field theories using gradient flow

Gradient flow has proved useful in the definition and measurement of renormalized quantities on the lattice. Recently, the fact that it suppresses high-modes of the field has been used to construct new, continuous RG transformations both analytically and on the lattice, distinct from the usual blocking techniques in spin models and gauge theories. In this work, we discuss such a formulation for scalar field theory, and we present preliminary numerical results for its application to the determination of critical exponents at the Wilson-Fisher fixed point of three-dimensional $\phi^4$ theory.
Students' Critical Thinking on Argumentative Essay Writing through Cooperative Learning

Carried on in non-English major freshman students setting, this study aims to examine how critical thinking skills can be developed through cooperative learning in their argumentative essay writing. An experimental group (n=20) and a control group (n=20) were randomly set up, the students were pre-tested and post-tested to see if there is a significant difference in their assigned essay through the Illinois Critical Thinking Essay Scoring Rubric. The implementation of critical thinking rubrics was carried out by 1) supporting students in cooperation, 2) offering the objective 3) fostering students to develop their ideas in writing. The Paired Sample T-test was used to calculate the difference between the pre-and post-test results. Results confirmed that in the Paired Sample t-test, the mean score (-5000) of the experimental group is statistically higher than the mean of the control group’s (-3900). It indicates that the implementation of the critical thinking strategy effectively develops and promotes students’ critical thinking skills in argumentative essay writing. Through the implementation of five key elements of critical thinking by Sadeghi (2012), students were more open-minded, tolerant, objective, honest and concise, respecting others, and interpreting situations differently. The research offered a different perspective on developing students’ critical thinking strategy use by focusing on longer periods of research and the larger number of participants and also implied the integration of critical thinking scoring rubric and argumentative essay skill performance for future research.
SWEETSPOT: NEAR-INFRARED OBSERVATIONS OF 13 TYPE Ia SUPERNOVAE FROM A NEW NOAO SURVEY PROBING THE NEARBY SMOOTH HUBBLE FLOW

We present 13 Type Ia supernovae (SNe Ia) observed in the rest-frame near-infrared (NIR) from 0.02 < z < 0.09 with the WIYN High-resolution Infrared Camera on the WIYN 3.5 m telescope. With only one to three points per light curve and a prior on the time of maximum from the spectrum used to type the object, we measure an H-band dispersion of spectroscopically normal SNe Ia of 0.164 mag. These observations continue to demonstrate the improved standard brightness of SNe Ia in an H band, even with limited data. Our sample includes two SNe Ia at z ∼ 0.09, which represent the most distant rest-frame NIR H-band observations published to date. This modest sample of 13 NIR SNe Ia represent the pilot sample for “SweetSpot”—a 3 yr NOAO Survey program that will observe 144 SNe Ia in the smooth Hubble flow. By the end of the survey we will have measured the relative distance to a redshift of z ∼ 0.05%–1%. Nearby Type Ia supernova (SN Ia) observations such as these will test the standard nature of SNe Ia in the rest-frame NIR, allow insight into the nature of dust, and provide a critical anchor for future cosmological SN Ia surveys at higher redshift.
SIGNS OF EARLY-STAGE DISK GROWTH REVEALED WITH ALMA

We present ALMA 1.3 mm continuum, 12CO, C18O, and SO data for the Class 0 protostars Lupus 3 MMS, IRAS 15398−3559, and IRAS 16253−2429 at resolutions of ∼100 au. By measuring a rotational profile in C18O, a 100 au Keplerian disk around a 0.3 M⊙ protostar is observed in Lupus 3 MMS. No 100 au Keplerian disks are observed in IRAS 15398−3559 and IRAS 16253−2429. Nevertheless, embedded compact (<30 au) continuum components are detected. The C18O emission in IRAS 15398−3559 shows signatures of infall with a constant angular momentum. IRAS 16253−2429 exhibits signatures of infall and rotation, but its rotational profile is unresolved. By fitting the C18O data with our kinematic models, the protostellar masses and the disk radii are inferred to be 0.01 M⊙ and 20 au in IRAS 15398−3559, and 0.03 M⊙ and 6 au in IRAS 16253−2429. By comparing the specific angular momentum profiles from 10,000 au to 100 au in eight Class 0 and I protostars, we find that the evolution of envelope rotation can be described with conventional inside-out collapse models. In comparison with a sample of 18 protostars with known disk radii, our results reveal signs of disk growth, with the disk radius increasing as M * 0.8 ± 0.14 or t 1.09 ± 0.37 in the Class 0 stage, where M* is the protostellar mass and t is the age. The disk growth rate slows down in the Class I stage. In addition, we find a hint that the mass accretion rate declines as t − 0.26 ± 0.04 from the Class 0 to the Class I stages.
Observations of Low-frequency Radio Emission from Millisecond Pulsars and Multipath Propagation in the Interstellar Medium

Studying the gravitational-wave sky with pulsar timing arrays (PTAs) is a key science goal for the Square Kilometre Array (SKA) and its pathfinder telescopes. With current PTAs reaching sub-microsecond timing precision, making accurate measurements of interstellar propagation effects and mitigating them effectively has become increasingly important to realize PTA goals. As these effects are much stronger at longer wavelengths, low-frequency observations are most appealing for characterizing the interstellar medium (ISM) along the sight lines toward PTA pulsars. The Murchison Widefield Array (MWA) and the Engineering Development Array (EDA), which utilizes MWA technologies, present promising opportunities for undertaking such studies, particularly for PTA pulsars located in the southern sky. Such pulsars are also the prime targets for PTA efforts planned with the South African MeerKAT, and eventually with the SKA. In this paper we report on observations of two bright southern millisecond pulsars, PSR J0437−4715 and PSR J2145−0750, made with these facilities; MWA observations sampled multiple frequencies across the 80–250 MHz frequency range, while the EDA provided direct-sampled baseband data to yield a large instantaneous usable bandwidth of ∼200 MHz. Using these exploratory observations, we investigate various aspects relating to pulsar emission and ISM properties, such as spectral evolution of the mean pulse shape, scintillation as a function of frequency, chromaticity in interstellar dispersion, and flux density spectra at low frequencies. Systematic and regular monitoring observations will help ascertain the role of low-frequency measurements in PTA experiments, while simultaneously providing a detailed characterization of the ISM toward the pulsars, which will be useful in devising optimal observing strategies for future PTA experiments.
Ureterovesical Anastomosis Complications in Kidney Transplantation: Definition, Risk Factor Analysis, and Prediction by Quantitative Fluorescence Angiography with Indocyanine Green

Ureteral stenosis and urinary leakage are relevant problems after kidney transplantation. A standardized definition of ureterovesical anastomosis complications after kidney transplantation has not yet been established. This study was designed to demonstrate the predictive power of quantitative indocyanine green (ICG) fluorescence angiography. This bicentric historic cohort study, conducted between November 2015 and December 2019, included 196 kidney transplantations. The associations between quantitative perfusion parameters of near-infrared fluorescence angiography with ICG and the occurrence of different grades of ureterovesical anastomosis complications in the context of donor, recipient, periprocedural, and postoperative characteristics were evaluated. Post-transplant ureterovesical anastomosis complications occurred in 18%. Complications were defined and graded into three categories. They were associated with the time on dialysis (p = 0.0025), the type of donation (p = 0.0404), and the number of postoperative dialysis sessions (p = 0.0173). Median ICG ingress at the proximal ureteral third was 14.00 (5.00–33.00) AU in patients with and 23.50 (4.00–117.00) AU in patients without complications (p = 0.0001, cutoff: 16 AU, sensitivity 70%, specificity 70%, AUC = 0.725, p = 0.0011). The proposed definition and grading of post-transplant ureterovesical anastomosis complications is intended to enable valid comparisons between studies. ICG Fluorescence angiography allows intraoperative quantitative assessment of ureteral microperfusion during kidney transplantation and is able to predict the incidence of ureterovesical anastomosis complications. Registration number: NCT-02775838.
The energy and momentum input of supernova explosions in structured and ionized molecular clouds

We investigate the early impact of single and binary supernova (SN) explosions on dense gas clouds with three-dimensional, high-resolution, hydrodynamic simulations. The effect of cloud structure, radiative cooling, and ionising radiation from the progenitor stars on the net input of kinetic energy, f_kin=E_kin/E_SN, thermal energy, f_therm=E_therm/E_SN, and gas momentum f_P=P/P_SN to the interstellar medium (ISM) is tested. For clouds with n=100 cm^{-3}, the momentum generating Sedov and pressure-driven snowplough phases are terminated early (~ 0.01 Myr) and radiative cooling limits the coupling to f_therm ~ 0.01, f_kin ~ 0.05, and f_P ~ 9, significantly lower than for the case without cooling. For pre-ionised clouds these numbers are only increased by ~ 50%, independent of the cloud structure. This only suffices to accelerate ~ 5% of the cloud to radial velocities >30km/s. A second SN might further enhance the coupling efficiencies if delayed past the Sedov phase of the first explosion. Such very low coupling efficiencies cast doubts on many galaxy-scale sub-resolution models for supernova feedback, most of which are validated a posteriori by qualitative agreement of galaxy properties with observations. Ionising radiation appears not to significantly enhance the immediate coupling of SNe to the surrounding gas as it drives the ISM into inert dense shells and cold clumps, a process which is unresolved in galaxy scale simulations. Our results support previous conclusions that supernovae might only drive a wind if a significant fraction explodes in low-density environments or if they are supported by processes other than ionising radiation.