Miracle-dz/UniFAR-FTUs huggingface dataset:
Improvements in the identification of CTIA saturation in NASA VIIRS L1B

The two VIIRS instruments onboard the Suomi NPP and NOAA-20 spacecraft collect data in 22 spectral bands from 0.4 μm to 12.5 μm. Both instruments have exhibited a known artifact in the behavior of the capacitive transimpedance amplifier (CTIA) that manifests in a double-valued (rollover) response in the Earth view imagery. This behavior was identified and well characterized prelaunch and is predominant for the single-gain band M6. The rollover phenomenon is also observed in the low-gain stages of the dual-gain reflective solar bands and thermal bands M12 and I4. The NASA VIIRS L1B processing currently has a rollover flagging scheme that is based on fixed thresholds in the digital numbers (DN) that approximately correspond to the designed maximum radiance of the band. In this work, we briefly review the prelaunch results, current on-orbit flagging methodology, and propose improvements for future implementation in the NASA Level 1B products. Results indicate significant improvement via more accurate flagging for the rollover pixels in band M6 as well as other RSB. The methodologies developed in this work could also be applicable to future VIIRS instruments to be launched aboard the JPSS-2-4 spacecrafts.
On the redshift distribution and physical properties of ACT-selected DSFGs.

We present multi-wavelength detections of nine candidate gravitationally-lensed dusty star-forming galaxies (DSFGs) selected at 218GHz (1.4mm) from the ACT equatorial survey. Among the brightest ACT sources, these represent the subset of the total ACT sample lying in Herschel SPIRE fields, and all nine of the 218GHz detections were found to have bright Herschel counterparts. By fitting their spectral energy distributions (SEDs) with a modified blackbody model with power-law temperature distribution, we find the sample has a median redshift of z = 4.1 - 1.0 + 1.1 (68 per cent confidence interval), as expected for 218GHz selection, and an apparent total infrared luminosity of log 10 ( μ L IR / L ⊙ ) = 13.86 - 0.30 + 0.33 , which suggests that they are either strongly lensed sources or unresolved collections of unlensed DSFGs. The effective apparent diameter of the sample is μ d = 4.2 - 1.0 + 1.7 kpc , further evidence of strong lensing or multiplicity, since the typical diameter of dusty star-forming galaxies is 1.0-2.5 kpc. We emphasize that the effective apparent diameter derives from SED modelling without the assumption of optically thin dust (as opposed to image morphology). We find that the sources have substantial optical depth. ( τ = 4.2 - 1.9 + 3.7 ) to dust around the peak in the modified blackbody spectrum (λ obs ⩽ 500μm), a result that is robust to model choice.
Predicting contamination accumulation in facilities with limited data

In preparation for the James Webb Space Telescope (JWST) launch at the Centre Spatial Guyanias (CSG) in French Guiana, particulate contamination accumulation predictions were necessary for each facility in which the hardware would be exposed because the Telescope would be uncovered in each of the facilities and had strict particulate requirements. These included facilities for final integration and testing, fueling, transportation and encapsulation. Minimal heritage data existed from CSG and previous launch campaigns to use as a basis for contamination predictions. Data from the Automatic Transfer Vehicle and Herschel-Planck launch campaigns were used in conjunction with facility monitoring data provided by the European Space Agency (ESA) and data collected during a JWST working group visit to CSG. These campaigns were conducted at varying cleanliness levels that were typically less stringent than JWST requirements. Each facility was evaluated using the data provided and likely performance improvement with the addition of High Efficiency Particulate Air filter (HEPA) banks operating when possible. Once the launch campaign was completed, the predicted fallout was compared with actual data collected throughout the campaign. Based on the actual measurements, JWST’s primary and secondary mirrors turned out to be much cleaner than what was predicted.
Tracking analysis of augmented complex least mean square algorithm

The augmented complex least mean‐square (ACLMS) algorithm is a suitable algorithm for the processing of both second‐order circular (proper) and noncircular (improper) signals. In this paper, we provide tracking analysis of the ACLMS algorithm in the non‐stationary environments. Using the established energy conservation argument, we derive a variance relation that contains moments that represent the effects of non‐stationary environment. We evaluate these moments and derive closed‐form expressions for the excess mean‐square error (EMSE) and mean‐square error (MSE). The derived expressions, supported by simulations, reveal that unlike the stationary case, the steady‐state EMSE, and MSE curves are not monotonically increasing functions of the step‐size parameter. We also use this observation to optimize the step‐size learning parameter. Simulation results illustrate the theoretical findings and match well with theory. Copyright © 2015 John Wiley & Sons, Ltd.
Hubble imaging of V1331 Cygni: Proper motion study of its circumstellar structures

The young star V1331 Cyg received previous attention because it is surrounded by an optical, arc-like reflection nebula. V1331 Cyg is commonly considered to be a candidate for an object that has undergone an FU-Ori (FUOR) the outbreak in the past. This in turn could lead to a time-varying appearance of the dusty arcs that may be revealed by multi-epoch imaging. In particular, a radial colour analysis of the dust arcs can then be attempted to check whether radial grain size distribution was modified by a previous FUOR wind. Second-epoch imaging of V1331 Cyg was obtained by us in 2009 using the Hubble Space Telescope (HST). By comparing this to archival HST data from 2000, we studied the time evolution of the circumstellar nebulae. After a point spread function subtraction using model point spread functions, we used customised routines to perform a proper motion analysis. The nebula expansion was first derived by deconvolving and correlating the two-epoch radial brightness profiles. Additional data from other facilities TLS, UKIDSS, SPITZER, and HERSCHEL were also incorporated to improve our understanding of the star in terms of environment, viewing angle, bipolar outflow length, and the FUOR phenomenon. The derived radial colour profiles do not indicate a spatial separation of the dust grain sizes. The HERSCHEL 160 micron images show for the time thermal emission from dust probably residing in the outer arc. By viewing V1331 Cyg almost pole-on, the length of the bipolar outflow exceeds previous estimates by far. The outer arc expansion timescale is consistent with the implantation time of the CO torus, which supports the hypothesis of an outburst that occurred a few thousand years ago. The azimuthal colour variation of the outer arc is probably due to changes of the scattering angle, imposed by a tilt or helical geometry of the dust configuration.
A review on recent results on on/off reconstruction of optical states

The knowledge of the density matrix of a quantum state plays a fundamental role in several applications, from quantum information to Standard Quantum Mechanics foundations investigation. Recently, a method has been implemented in order to obtain the reconstruction of the (diagonal) elements of the density matrix exploiting the information achievable with realistic on/off detectors (e.g. silicon avalanche photo-diodes). Purpose of this paper is to introduce this on/off method and present the last experimental results obtained with it in several different cases.
INHOMOGENEITIES IN TYPE Ib/c SUPERNOVAE: AN INVERSE COMPTON SCATTERING ORIGIN OF THE X-RAY EMISSION

Inhomogeneities in a synchrotron source can severely affect the conclusions drawn from observations regarding the source properties. However, their presence is not always easy to establish, since several other effects can give rise to similar observed characteristics. It is argued that the recently observed broadening of the radio spectra and/or light curves in some Type Ib/c supernovae is a direct indication of inhomogeneities. As compared to a homogeneous source, this increases the deduced velocity of the forward shock and the observed correlation between total energy and shock velocity could in part be due to a varying covering factor. The X-ray emission from at least some Type Ib/c supernovae is unlikely to be synchrotron radiation from an electron distribution accelerated in a nonlinear shock. Instead it is shown that the observed correlation during the first few hundred days between the radio, X-ray, and bolometric luminosities indicates that the X-ray emission is inverse Compton scattering of the photospheric photons. Inhomogeneities are consistent with equipartition between electrons and magnetic fields in the optically thin synchrotron emitting regions.
Rutin Potentially Binds the Gamma Secretase Catalytic Site, Down Regulates the Notch Signaling Pathway and Reduces Sphere Formation in Colonospheres

Rutin, a natural flavonol, can modulate molecular signaling pathways and has considerable potential in cancer treatment. However, little is known about the effect of rutin on the notch signaling pathway (NSP) in cancer and cancer stem-like cells. In this study, we explored the effect of rutin on gamma secretase (GS, a putative notch signaling target) inhibition mediated NICD (Notch Intracellular Domain) production in colon cancer cells. Molecular docking, MM-GBSA, and Molecular dynamics (MD) simulation experiments were performed to check rutin’s GS catalytic site binding potential. The HCT-116 colon cancer and cancer stem-like cells (colonospheres) were utilized to validate the in silico findings. The NICD production, notch promoter assay, expression of notch target genes, and cancer stemness/self-renewal markers were studied at molecular levels. The results were compared with the Notch-1 siRNA transfected test cells. The in silico study revealed GS catalytic site binding potential in rutin. The in vitro results showed a decreased NICD formation, an altered notch target gene (E-cad, Hes-1, and Hey-1) expression, and a reduction in stemness/self-renewal markers (CD44, c-Myc, Nanog, and Sox2) in test cells in a time and dose-dependent manner. In conclusion, rutin inhibits the notch signaling pathway and reduces the stemness/self-renewal property in colon cancer cells and the colonospheres by targeting gamma secretase. The clinical efficacy of rutin in combination therapy in colon cancer may be studied in the future.
Note on the helicity decomposition of spin and orbital optical currents

In the helicity representation, the Poynting vector (current) for a monochromatic optical field, when calculated using either the electric or the magnetic field, separates into right-handed and left-handed contributions, with no cross-helicity contributions. Cross-helicity terms do appear in the orbital and spin contributions to the current. But when the electric and magnetic formulas are averaged (‘electric–magnetic democracy’), these terms cancel, restoring the separation into right-handed and left-handed currents for orbital and spin separately.
Near-Infrared Spectroscopic Monitoring Observations of Three Yellow Hypergiants and Time Variation of 2.3 $\mu$m CO Features of $\rho $ Cassiopeia

We made spectroscopic monitoring observations of the three yellow hypergiants ( Cassiopeia, HR 8752, and IRC+10420) in the 0.9–2.4 m wavelength range with a resolution of 2600 over a fifteen month period. The spectra of HR 8752 and IRC+10420 showed no time variations. On the other hand, those of Cas showed just a series of time variation in 2.3 m CO features from nondetection to absorption through emission during 2002–2004. We interpret this variation as being a result of an expanding gas shell whose excitation temperature was being cooled down to 800 K. The CO column densities were estimated from the CO absorption depths. Moreover, assuming spherical symmetry of the expanding shell with a constant expansion velocity of 35 km s , a stellar effective temperature of 7000 K, a stellar radius of 400 Rˇ, solar abundance, and all carbon atoms forming CO molecules, we estimated the mass of the shell to be 2 10 Mˇ for a model with a single shell expanding from the photosphere, or 5 10 Mˇ for another model with an expanding shell and a static envelope. These estimates of the released mass strongly depend on assumptions of the expansion velocity, the abundance, and the dissociation of the CO molecules.
ROTATION OF THE NGC 1333 IRAS 4A2 PROTOSTELLAR JET

The bipolar jet of the NGC 1333 IRAS 4A2 protostar shows a velocity gradient in the direction perpendicular to the jet axis. This lateral velocity gradient can be seen throughout the jet imaged in a silicon monoxide line, 2500–8700 AU from the driving source, and is consistent with the rotation of the accretion disk. If this gradient is caused by the rotation of the jet around its axis, the average specific angular momentum is about 1.5 × 1021 cm2 s−1. Comparison of the kinematics between the jet and the disk suggests that the jet-launching region on the disk has a radius of about 2 AU, which supports the disk-wind models. The angular momentum transported away by the jet seems to be large enough for the protostar to accrete matter from the disk, confirming the crucial role of jets in the early phase of the star formation process.
First Successful Transport and Short-term Rearing of the Endangered Sardinella tawilis (Herre, 1927) in Ex Situ Captivity

The Taal Lake endemic freshwater sardine Sardinella tawilis (Herre, 1927), an important fisheries species, has been recently placed in the Endangered category by the International Union for Conservation of Nature due to its high endemicity and population declines, coupled with potential threats from natural volcanic and geologic events. We examined the survivorship of S. tawilis in short-term ex situ captivity (~ 30 d) and determined water quality parameters that influence survival. Collection, transport, and ex situ captivity trials for a total of 333 S. tawilis individuals were conducted from February–May 2021. The survival rate ranged from 2.6–26.9% after 30 d across the four trials. Principal component analyses showed that salinity, conductivity, and dissolved oxygen (DO) influenced S. tawilis survival. Generalized linear mixed models revealed that the combination of conductivity and DO have a significant effect on survival. Manifestations of handling stress observed in captive individuals include scale loss, hemorrhaging at fin base, swelling of eyes, and possible fungal infections. This study documents the first attempt at rearing S. tawilis via ex situ captivity. The findings of this study will serve as a basis to improve the survival of S. tawilis in captivity and will open possibilities of captive breeding or larval rearing for this endemic freshwater sardine.
Low-cost dielectric sheets for large-area floor sensing applications

Sensitivity response is a critical parameter that decides the domain of dielectric materials to be implemented as piezocapacitive sensors for low- or high-pressure sensing applications. Here, we have clarified the sensitivity response behavior of three low-cost dielectric materials, two biodegradable paperboards, and one acoustic polymeric foam. The devices are fabricated in the form of a metal–insulator–metal structure, and the capacitive response of the devices is measured using the charge extraction by linearly increasing voltage technique. The sensitivity response curve (ΔC/C o vs. pressure) reveals that the paperboard materials are sensitive enough to detect low-pressure regimes (45 kPa), whereas the acoustic foam is quite promising for high-pressure monitoring (above 150 kPa). Using a multiplexer circuit, we demonstrated the sensitivity response via 2 by 2 matrix structure both as a steady-state and transient response. Our results show that the passive matrix structure interference between different pixels can be minimized after increasing the spacing between electrodes strip. Finally, a full-scale demonstrator (dimension 120 cm × 400 cm) with a 2 × 8 matrix structure laminated under floor tiling has been demonstrated. We show how such a floor sensor utilizing the low-cost substrates can be used to recognize single-stepping, walking, and falling.
Modeling of contamination vent path for outgassing components underneath thermal blankets on Europa Clipper

NASA’s Europa Clipper mission will conduct a detailed reconnaissance of Jupiter’s moon Europa and investigate whether the icy moon could host conditions suitable for life. To perform these tasks, the spacecraft will carry several scientific instruments, including cameras, mass spectrometers, radars, magnetometers, plasma sensors and dust analyzer. These state-of-the-art instruments are very sensitive to molecular contamination; hence it is important to properly design preferential venting paths that minimize the transport of contaminants to the instruments sensitive surfaces. The JPL Contamination Control Group developed a physics-based approach to quantify the amount of contaminants escaping from the thermal blankets vents. This approach includes a thorough design of the thermal blankets and vents in the Europa Clipper geometrical model and a detailed analysis of the transport of contaminants from outgassing components underneath the thermal blankets to the vents. The physics-based thermal blankets venting model enhances the ability to assess and control outgassing contamination on Europa Clipper, and subsequently to properly design venting locations that provide a preferential escape path for outgassed molecules. The model also provides more accurate results compared to the historic approach (area ratio) widely used in literature to estimate outgassing from thermal blankets vents.
Spectroscopy Made Easy: Evolution

Context. The Spectroscopy Made Easy (SME) package has become a popular tool for analyzing stellar spectra, often in connection with large surveys or exoplanet research. SME has evolved significantly since it was first described in 1996, but many of the original caveats and potholes still haunt users. The main drivers for this paper are complexity of the modeling task, the large user community, and the massive effort that has gone into SME. Aims. We do not intend to give a comprehensive introduction to stellar atmospheres, but will describe changes to key components of SME: the equation of state, opacities, and radiative transfer. We will describe the analysis and fitting procedure and investigate various error sources that affect inferred parameters. Methods. We review the current status of SME, emphasizing new algorithms and methods. We describe some best practices for using the package, based on lessons learned over two decades of SME usage. We present a new way to assess uncertainties in derived stellar parameters. Results. Improvements made to SME, better line data, and new model atmospheres yield more realistic stellar spectra, but in many cases systematic errors still dominate over measurement uncertainty. Future enhancements are outlined.
BREAKOUT RECONNECTION OBSERVED BY THE TESIS EUV TELESCOPE

We present experimental evidence of the coronal mass ejection (CME) breakout reconnection, observed by the TESIS EUV telescope. The telescope could observe solar corona up to 2 R⊙ from the Sun center in the Fe 171 Å line. Starting from 2009 April 8, TESIS observed an active region (AR) that had a quadrupolar structure with an X-point 0.5 R⊙ above photosphere. A magnetic field reconstructed from the Michelson Doppler Imager data also has a multipolar structure with an X-point above the AR. At 21:45 UT on April 9, the loops near the X-point started to move away from each other with a velocity of ≈7 km s−1. At 01:15 UT on April 10, a bright stripe appeared between the loops, and the flux in the GOES 0.5–4 Å channel increased. We interpret the loops’ sideways motion and the bright stripe as evidence of the breakout reconnection. At 01:45 UT, the loops below the X-point started to slowly move up. At 15:10 UT, the CME started to accelerate impulsively, while at the same time a flare arcade formed below the CME. After 15:50 UT, the CME moved with constant velocity. The CME evolution precisely followed the breakout model scenario.
The spatial and velocity bias of linear density peaks and protohaloes in the Λ cold dark matter cosmology

We use high-resolution N-body simulations to investigate the Lagrangian bias of cold dark matter haloes within the Λ cold dark matter cosmology. Our analysis focuses on ‘protohaloes’ that we identify in the simulation initial conditions with the subsets of particles belonging to individual redshift-zero haloes. We then calculate the number density and velocity divergence fields of protohaloes and estimate their autospectral densities. We also measure the corresponding cross-spectral densities with the linear matter distribution. We use our results to test a Lagrangian bias model presented by Desjacques & Sheth which is based on the assumption that haloes form out of local density maxima of a specific height. Our comparison validates the predicted functional form for the scale dependence of the bias for both the density and the velocity fields. We also show that the bias coefficients are accurately predicted for the velocity divergence. In contrast, the theoretical values for the density bias parameters do not accurately match the numerical results as a function of halo mass. This is likely due to the simplistic assumptions that relate virialized haloes to density peaks of a given height in the model. We also detect appreciable stochasticity for the Lagrangian density bias, even on very large scales. These are not included in the model at leading order but correspond to higher order corrections.
BeamR: Beam Reweighing with Attribute Discriminators for Controllable Text Generation

Recent advances in natural language process-001 ing have led to the availability of large pre-002 trained language models (LMs), with rich gen-003 erative capabilities. Although these models 004 are able to produce ﬂuent and coherent text, 005 it remains a challenge to control various at-006 tributes of the generation, including sentiment, 007 formality, topic and many others. We propose a 008 Beam Reweighing (B EAM R) method, building 009 on top of standard beam search, in order to con-010 trol different attributes. B EAM R combines any 011 generative LM with any attribute discrimina-012 tor, offering full ﬂexibility of generation style 013 and attribute, while the beam search backbone 014 maintains ﬂuency across different domains. No-015 tably, B EAM R allows practitioners to leverage 016 pre-trained models without the need to train 017 generative LMs together with discriminators. 018 We evaluate B EAM R in two diverse tasks: senti-019 ment steering, and machine translation formal-020 ity. Our results show that B EAM R performs 021 on par with or better than existing state-of-the-022 art approaches (including ﬁne-tuned methods), 023 and highlight the ﬂexiblity of B EAM R in both 024 causal and seq2seq language modeling tasks. 025
Increasing supercycle lengths of active SU UMa-type dwarf novae

We present observational evidence that supercycle lengths of the most active SU UMa-type stars are increasing during the past decades. We analysed a large number of photometric measurements from available archives and found that this effect is generic for this class of stars, independently of their evolutionary status. This finding is in agreement with previous predictions and the most recent work of Patterson et al. (2012) on BK Lyn.