Miracle-dz/UniFAR-FTUs huggingface dataset:
The XXL Survey

Context. The fraction of galaxies bound in groups in the nearby Universe is high (50% at z ~ 0). Systematic studies of galaxy properties in groups are important in order to improve our understanding of the evolution of galaxies and of the physical phenomena occurring within this environment. Aims. We have built a complete spectrophotometric sample of galaxies within X-ray detected, optically spectroscopically confirmed groups and clusters (G&C), covering a wide range of halo masses at z ≤ 0.6. Methods. In the context of the XXL survey, we analyse a sample of 164 G&C in the XXL-North region (XXL-N), at z ≤ 0.6, with a wide range of virial masses (1.24 × 1013 ≤ M500,scal(M⊙) ≤ 6.63 × 1014) and X-ray luminosities ((2.27 × 1041 ≤ L500,scalXXL(erg s−1) ≤ 2.15 × 1044)). The G&C are X-ray selected and spectroscopically confirmed. We describe the membership assignment and the spectroscopic completeness analysis, and compute stellar masses. As a first scientific exploitation of the sample, we study the dependence of the galaxy stellar mass function (GSMF) on global environment. Results. We present a spectrophotometric characterisation of the G&C and their galaxies. The final sample contains 132 G&C, 22 111 field galaxies and 2225 G&C galaxies with r-band magnitude <20. Of the G&C, 95% have at least three spectroscopic members, and 70% at least ten. The shape of the GSMF seems not to depend on environment (field versus G&C) or X-ray luminosity (used as a proxy for the virial mass of the system). These results are confirmed by the study of the correlation between mean stellar mass of G&C members and L500,scalXXL. We release the spectrophotometric catalogue of galaxies with all the quantities computed in this work. Conclusions. As a first homogeneous census of galaxies within X-ray spectroscopically confirmed G&C at these redshifts, this sample will allow environmental studies of the evolution of galaxy properties.
Two-gap model for underdoped cuprate superconductors

Various properties of underdoped superconducting cuprates, including the momentum-dependent pseudogap opening, indicate a behavior which is neither BCS- nor Bose-Einstein condensation (BEC)\char21{} like. To explain this issue we introduce a two-gap model. This model assumes an anisotropic pairing interaction among two kinds of fermions with small and large Fermi velocities representing the quasiparticles near the M and the nodal points of the Fermi surface, respectively. We find that a gap forms near the M points resulting in incoherent pairing due to strong fluctuations. Instead, the pairing near the nodal points sets in with phase coherence at lower temperature. By tuning the momentum-dependent interaction, the model allows for a continuous evolution from a pure BCS pairing (in the overdoped and optimally doped regime) to a mixed boson-fermion picture (in the strongly underdoped regime).
Edge magnetization and spin transport in an SU(2)-symmetric Kitaev spin liquid

We investigate the edge magnetism and the spin transport properties of an SU(2)-symmetric Kitaev spin liquid (KSL) model put forward by Yao and Lee [Phys. Rev. Lett. \textbf{107}, 087205 (2011)] on the honeycomb lattice. In this model, the spin degrees of freedom fractionalize into a $\mathbb{Z}_{2}$ static gauge field and three species of either gapless (Dirac) or gapped (chiral) Majorana fermionic excitations. We find that, when a magnetic field is applied to a zigzag edge, the Dirac KSL exhibits a nonlocal magnetization associated with the existence of zero-energy edge modes. The application of a spin bias $V=\mu_{\uparrow}-\mu_{\downarrow}$ at the interface of the spin system with a normal metal produces a spin current into the KSL, which depends, in the zero-temperature limit, as a power-law on $V$ for both Dirac and chiral KSLs, but with different exponents. Lastly, we study the longitudinal spin Seebeck effect, in which a spin current is driven by the combined action of a magnetic field perpendicular to the plane of the honeycomb lattice and a thermal gradient at the interface of the KSL with a metal. Our results suggest that edge magnetization and spin transport can be used to probe the existence of charge-neutral edge states in quantum spin liquids.
Pure fluorescent H2 emission from Hubble 12

An improved K-band (2.0-2.4 μm) spectrum of the planetary nebula Hubble 12 has been obtained at a position near where Dinerstein et al. found the H 2 line emission to be fluorescent. The new spectrum is consistent with the conclusion of Dinerstein et al. and, in addition, provides further evidence that the emission is essentially purely fluorescent, through the presence of several weak H 2 lines of higher excitation than have been detected previously and a measured ortho/para ratio of 1.7. Analysis of the spectrum demonstrates that the gas density is ∼ 10 4 -10 5 cm −3
Stochastic approximation algorithm for industrial process optimisation

Stochastic approximation algorithms are alternative linear search methods for optimising control systems where the functional relationship between the response variable and the controllable factors in a process and its analytical model remain unknown. These algorithms have no criteria for selecting succession measurements ensuring convergence, meaning that, when implemented in practice, they may diverge with consequent waste of resources. The objective of this research was to determine industrial processes’ optimum operating conditions by using a modified stochastic approximation algorithm, where its succession measurements were validated by obtaining response variable values for each iteration through simulation. The algorithm is presented in nine stages; its first six describe which are process independent and dependent variables, the type of experimental design selected, the experiments assigned and developed and the second order models obtained. The last three stages describe how the algorithm was developed, and the optimal values of the independent variables obtained. The algorithm was validated in 3 industrial processes which it was shown to be efficient for determining independent variables’ optimum operating conditions (temperature and time): the first three iterations were obtained at 66°C in 3 hours 42 minutes for process 1, unlike processes 2 and 3 where the first iteration was obtained at 66°C in 6 hours 06 minutes and 80°C in 5 hours 06 minutes, respectively.
Slightly generalized Generalized Contagion: Unifying simple models of biological and social spreading

We motivate and explore the basic features of generalized contagion, a model mechanism that unifies fundamental models of biological and social contagion. Generalized contagion builds on the elementary observation that spreading and contagion of all kinds involve some form of system memory. We discuss the three main classes of systems that generalized contagion affords, resembling: simple biological contagion; critical mass contagion of social phenomena; and an intermediate, and explosive, vanishing critical mass contagion. We also present a simple explanation of the global spreading condition in the context of a small seed of infected individuals.
Systematic generation of finite-range atomic basis sets for linear-scaling calculations

Basis sets of atomic orbitals are very efficient for density functional calculations but lack a systematic variational convergence. We present a method to optimize numerical atomic orbitals variationally, using a single parameter to control their range. The efficiency of the basis generation scheme is tested and compared with other schemes for multiple $\ensuremath{\zeta}$ basis sets. The scheme is shown to be comparable in quality to other widely used schemes albeit offering better performance for linear-scaling computations.
A Search for Variable Stars and Planetary Occultations in NGC 2301. I. Techniques

We observed the young open cluster NGC 2301 for 14 nights in 2004 February using the orthogonal transfer CCD camera OPTIC. We used point‐spread function shaping techniques (“square stars”) during the observations, allowing us to obtain a larger dynamic range (4.5 mag) of high photometric precision results (≤2 mmag). These results are better than similar observing campaigns using standard CCD imagers. This paper discusses our observational techniques and presents initial results for the variability statistics found in NGC 2301. Details of the variability statistics as functions of color, variability type, stellar type, and cluster location will appear in Paper II.
Effective Interaction between Molecules in the Strong-Coupling BEC Regime of a Superfluid Fermi Gas

We investigate the effective interaction between Cooper-pair molecules in the strong-coupling BEC regime of a superfluid Fermi gas with a Feshbach resonance. Our work uses a path integral formulation and a renormalization group (RG) analysis of fluctuations in a single-channel model. We show that a physical cutoff energy ω c originating from the finite molecular binding energy is the key to understanding the interaction between molecules in the BEC regime. Our work thus clarifies recent results by showing that a M =2 a F is a bare molecular scattering length while a M =(0.6–0.75) a F is the low-energy molecular scattering length renormalized to include high-energy scattering up to ω c (here, a F is the scattering length between Fermi atoms). We also include many-body effects at finite temperatures. We find that a M is strongly dependent on temperature, vanishing at T c , consistent with the earlier Bose gas results of Bijlsma and Stoof.
All-electron GW calculation based on the LAPW method: Application to wurtzite ZnO

We present a new, all-electron implementation of the GW approximation and apply it to wurtzite ZnO. Eigenfunctions computed in the local-density approximation (LDA) by the full-potential linearized augmented-plane-wave (LAPW) or the linearized muffin-tin-orbital (LMTO) method supply the input for generating the Green function G and the screened Coulomb interaction W. A mixed basis is used for the expansion of W, consisting of plane waves in the interstitial region and augmented-wavefunction products in the augmentation-sphere regions. The frequency-dependence of the dielectric function is computed within the random-phase approximation (RPA), without a plasmon-pole approximation. The Zn 3d orbitals are treated as valence states within the LDA; both core and valence states are included in the self-energy calculation. The calculated bandgap is smaller than experiment by about 1eV, in contrast to previously reported GW results. Self-energy corrections are orbital-dependent, and push down the deep O 2s and Zn 3d levels by about 1eV relative to the LDA. The d level shifts closer to experiment but the size of shift is underestimated, suggesting that the RPA overscreens localized states.
3-omega method for thermal properties of thin film multilayers

Short review on the different models for the electro-thermal 3-omega method. We present the deduction of the fundamental relation between the 3-omega voltage with the temperature rise to determine the thermal conductivity. The usage of the anisotropy of the films allows a smooth transition between 1D and 2D models. A comparison between the multilayer methods and analytical solutions are presented.
Superfluid density and competing orders in d -wave superconductors

We derive expressions for the superfluid density ${\ensuremath{\rho}}_{s}$ in the low-temperature limit $T\ensuremath{\rightarrow}0$ in $d$-wave superconductors, taking into account the presence of competing orders such as spin-density waves, $i{d}_{xy}$ pairing, etc. Recent experimental data for the thermal conductivity and for elastic neutron scattering in ${\mathrm{La}}_{2\ensuremath{-}x}{\mathrm{Sr}}_{x}\mathrm{Cu}{\mathrm{O}}_{4}$ suggest there are magnetic field induced anomalies that can be interpreted in terms of competing orders. We consider the implications of these results for the superfluid density and show in the case of competing spin-density wave order that the usual Volovik-like $\sqrt{H}$ depletion of ${\ensuremath{\rho}}_{s}(H)$ is replaced by a slower dependence on applied magnetic field. We find that it is crucial to include the competing order parameter in the self-consistent equation for the impurity scattering rate.
A Search for Stellar Populations in High-Velocity Clouds

We report the results of a photometric search for giant stars associated with the cores of four high-velocity clouds (HVCs)—two of which are compact HVCs—using the Las Campanas du Pont 2.5 m and Cerro Tololo Blanco 4 m telescopes in combination with a system of filters (Washington M, T2 + DDO51) useful for identifying low surface gravity, evolved stars. Identical observations of nearby control fields provide a measure of the "giant star" background. Our data reach M0 = 22 for three of the HVCs and M0 = 21.25 for the fourth, depths that allow the detection of any giant stars within 600 kpc. Although we identify a number of faint late-type giant star candidates, we find neither a coherent red giant branch structure nor a clear excess of giant candidate counts in any HVC. This indicates that the giant candidates are probably not related to the HVCs and are more likely to be either random Milky Way giant stars or one of several classes of potential survey contaminants. Echelle spectroscopy of the brightest giant candidates in one HVC and its control field reveals radial velocities representative of the canonical Galactic stellar populations. In addition to these null results, no evidence of any young HVC stellar populations (represented by blue main-sequence stars) is found, a result consistent with previous searches. Our methodology, specifically designed to find faint diffuse stellar populations, places the tightest upper limit yet on the total stellar mass of HVCs of a few times 105 M☉.
Inhibition of Neuronal Nicotinic Acetylcholine Receptor Subtypes by (cid:1) -Conotoxin GID and Analogues * □ S

(cid:1) -Conotoxins are small disulfide-rich peptides from the venom of the Conus species that target the nicotinic acetylcholine receptor (nAChR). They are valuable pharmacological tools and also have potential therapeutic applications particularly for the treatment of chronic pain. (cid:1) -Conotoxin GID is isolated from the venom of Conus geographus and has an unusual N-ter-minal tail sequence that has been shown to be important for binding to the (cid:1) 4 (cid:2) 2 subtype of the nAChR. To date, only four conotoxins that inhibit the (cid:1) 4 (cid:2) 2 subtype have been character-ized, but they are of considerable interest as it is the most abun-dant nAChR subtype in the mammalian brain and has been implicated in a range of diseases. In this study, analysis of ala-nine-scan and truncation mutants of GID reveals that a conserved proline in (cid:1) -conotoxins is important for activity at the (cid:1) 7, (cid:1) 3 (cid:2) 2, and (cid:1) 4 (cid:2) 2 subtypes. Although the proline residue was the most critical residue for activity at the (cid:1) 3 (cid:2) 2 subtype, Asp 3 12 , and Asn 14 are also critical at the (cid:1) 7 subtype. Interest-ingly, very few of the mutations tested retained activity at the 4 (cid:2) 2 subtype indicating a tightly defined binding site. This lack of tolerance to sequence variation may explain the lack of selec-tive ligands discovered for the (cid:1) 4 (cid:2) 2 subtype to date. Overall, our findings contribute to the understanding of the structure-activity relationships of (cid:1) -conotoxins and may be beneficial for the ongoing attempts to exploit modulators of the neuronal nAChRs as therapeutic agents.
A countable representation of the Fleming-Viot measure-valued diffusion

The Fleming-Viot measure-valued diffusion arises as the infinite population limit of various discrete genetic models with general type space. The paper gives a countable construction of the process as the empirical measure carried by a certain interactive particle system. This explicit representation facilitates the study of various properties of the Fleming-Viot process. The construction also carries versions of the familiar genealogical processes from population genetics, in particular, Kingman's coalescent, thus unifying the genealogical and measure-valued approaches to the subject.
Star formation studies using the Herschel-SPIRE Imaging FTS

The study of low mass star formation in our local Galaxy is particularly suited to HERSCHEL. The SPIRE spectrometer and photometer aboard the spacecraft operate in the ~ 200 - 600�m range and are well suited to probe the cold, dusty environments in molecular clouds where prestellar cores reside. The SPIRE FTS spectrometer is an interferometer, and this instrument design has strengths and weaknesses which are im- portant to understand when using data from the instrument. Herschel is set to continue groundbreaking work in the infrared, building upon earlier work from ISO, IRAS, and SPITZER, probing deep into star forming regions and improving our knowledge of the processes within. In this PhD thesis, we outline the current body of knowledge in low mass star formation. We examine the properties of the SPIRE FTS as a spectrometerusing a small, laboratory designed desktop FTS. We study the intrinsic properties of the instrument, as a way of understanding issues we are likely to see when using the SPIRE FTS in ight. With these issues firmly in mind, we examine the creation and use of SLIDE - an interactive IDL-based tool for processing SPIRE FTS data. SLIDE can extract line and continuum information from SPIRE FTS SEDs. We outline the creation, testing and use of SLIDE and provide examples of the use of SLIDE in astronomy with some examples from the literature. We then use the line information we extract from a variety of sources with the spectrometer, to examine how SED fitting from photometer data could be affected by line contamination. We simulate a wide range of greybodies with noise and line con- tamination and examine how SED fitting is affected. Our simulations conclude that line contamination is not enough to affect the recovery of temperature and spectral index B significantly. Finally we use the information we have deduced to examine SPIRE FTS SEDs of L1689B - a prestellar core located in Ophiuchus. Our SED fitting of the core confirms that this core is starless with no internal heating source, and the spectral index profile over the core morphology is consistent with an increasing density of fractal aggregrate grains towards the centre. The increase in grain density and spectral index profile is also in agreement with previous CO depletion data. Fractal grain growth of this nature is consistent with dust grain models.
A spectroscopic study of the Dr 21 outflow source. III - The CO line emission

New, high-angular resolution observations of 12 CO, 13 CO, C 18 O J = 1-0 and H 33 α hydrogen recombination line emission from the energetic DR 21 outflow are presented and discussed. The high-velocity CO emission is clearly bipolar with the blueshifted outflow lobe lying to the west and the redshifted lobe to the east of the DR 21 cloud core. These observations suggest that the DR 21 outflow is probably the most massive and energetics young-stellar outflow yet discovered in the Galaxy. In addition to the main outflow, the CO maps reveal a second high-velocity bipolar flow which also originates from within the DR 21 cloud core but extends along a N-S axis, perpendicular to the E-W axis of the main outflow
Product and quality assurance processes and ECSS compliance within a science ground segment using Gaia as an example

The ESA satellite Gaia aims to measure the main astrometric parameters and generate an astrometric catalogue of 109 objects with an accuracy on the micro-arcsec level. To reach this goal the European scientific community has formed the Gaia Data Processing and Analysis Consortium (DPAC). DPAC includes the Science Operation Centre (SOC) at ESAC and together they constitute the Gaia science ground segment, including a total of more than 400 scientists and engineers. Such a large group of developers represent a massive development effort which requires effective quality monitoring and assurance mechanisms and reporting structures to be in place. In this paper we will outline the procedures and mechanisms setup within the consortium to assure that DPAC software products and the necessary hardware will be ready when they are needed and fulfill their expectations. The experiences gathered in the employed PA/QA process, which is based on the relevant ECSS standards, will be described and will prove useful for other projects of similarly large scale.
Quantum–classical transition in the electron dynamics of thin metal films

The quantum electrons dynamics in a thin metal film is studied numerically using the self-consistent Wigner–Poisson equations. The initial equilibrium is computed from the Kohn–Sham equations at finite temperature, and then mapped into the phase-space Wigner function. The time-dependent results are compared systematically with those obtained previously with a classical approach (Vlasov–Poisson equations). It is found that, for large excitations, the quantum and classical dynamics display the same low-frequency oscillations due to ballistic electrons bouncing back and forth on the film surfaces. However, below a certain excitation energy (roughly corresponding to one quantum of plasmon energy ), the quantum and classical results diverge, and the ballistic oscillations are no longer observed. These results provide an example of a quantum–classical transition that may be observed with current pump–probe experiments on thin metal films.
Polarized scattered light from self-luminous exoplanets

Direct imaging has paved the way for atmospheric characterization of young and self-luminous gas giants. Scattering in a horizontally-inhomogeneous atmosphere causes the disk-integrated polarization of the thermal radiation to be linearly polarized, possibly detectable with the newest generation of high-contrast imaging instruments. We aim to investigate the effect of latitudinal and longitudinal cloud variations, circumplanetary disks, atmospheric oblateness, and cloud particle properties on the integrated degree and direction of polarization in the near-infrared. We have developed a three-dimensional Monte Carlo radiative transfer code (ARTES) for scattered light simulations in (exo)planetary atmospheres. The code is applicable to calculations of reflected light and thermal radiation in a spherical grid with a parameterized distribution of gas, clouds, hazes, and circumplanetary material. The disk-integrated degree of polarization of a horizontally-inhomogeneous atmosphere is maximal when the planet is flattened, the optical thickness of the equatorial clouds is large compared to the polar clouds, and the clouds are located at high altitude. For a flattened planet, the integrated polarization can both increase or decrease with respect to a spherical planet which depends on the horizontal distribution and optical thickness of the clouds. The direction of polarization can be either parallel or perpendicular to the projected direction of the rotation axis when clouds are zonally distributed. Rayleigh scattering by submicron-sized cloud particles will maximize the polarimetric signal whereas the integrated degree of polarization is significantly reduced with micron-sized cloud particles as a result of forward scattering. The presence of a cold or hot circumplanetary disk may also produce a detectable degree of polarization ($\lesssim$1%) even with a uniform cloud layer in the atmosphere.