Miracle-dz/UniFAR-FTUs huggingface dataset:
On some properties of Banach spaces. (Spanish: Sobre algunas propiedades de espacios de Banach)

This paper is devoted to an exposition of the two main methods used to introduce isomorphic properties of Banach spaces. The first one consists in the comparison of different classes of operators; the second in the comparison of different classes of subsets. For instance, it is well known that a Banach space E is finite-dimensional if and only if every bounded linear operator on E is compact if and only if every closed, bounded subset of E is compact. The first method, introduced by Grothendieck, is based upon the following general scheme: Let Φ,Ψ be two classes of bounded linear operators between Banach spaces and E a class of Banach spaces. Then E is said to have property P(Φ,Ψ,E) if Φ(E,F)⊆Ψ(E,F) for all F∈E ; if E is the class of all Banach spaces one simply writes E∈P(Φ,Ψ) . The author considers the following classes of operators: K(E,F)= compact operators; W(E,F)= weakly compact operators; DP(E,F)= Dunford-Pettis operators; D(E,F)= Dieudonne operators; UC(E,F)= unconditionally convergent operators; L(E,F)= bounded linear operators. Then he gives the following definition: A Banach space E (i) has the Dunford-Pettis property if E∈P(W,DP) ; (ii) has the reciprocal Dunford-Pettis property if E∈P(DP,W) ; (iii) has the Dieudonne property if E∈P(D,W) ; (iv) has property (V) if E∈P(UC,W) ; (v) has the Schur property if E∈P(L,DP) ; (vi) is weakly sequentially complete if E∈P(L,D) ; (vii) does not contain copies of c 0 if E∈P(L,UC) ; (viii) does not contain copies of l 1 if E∈P(DP,K) ; (ix) has the Grothendieck property if E∈P(L,W,c 0 ) . The author also shows that the above properties are always inherited by finite products and complemented subspaces, whereas quotients or closed subspaces inherit them just in special cases. Then the author treats the second method of introducing isomorphic properties, by considering several classes of subsets of a Banach space E , namely: K(E)= relatively compact subsets; W(E)= weakly relatively compact subsets; WC(E)= weakly conditionally compact subsets; B(E)= bounded subsets; L ∗ (E)= limited subsets; DP(E)= Dunford-Pettis subsets; V ∗ (E)=V ∗ subsets. He shows that the inclusion of one of them into another is useful for giving a different formulation of the above definition (example: E has the Dunford-Pettis property if W(E)⊆DP(E) ) as well as for introducing new properties (example: E is said to have the Gelʹfand-Phillips property if L ∗ (E)⊆K(E) ). Several results about this second method are then presented.
Reconciling extremely different concentration-mass relations

The concentration-mass relations proposed by Prada et al. (2012) and by Duffy et al. (2008) on the scales of galaxy clusters show some of the largest discrepancies among all the works present in literature. This is surprising because they are both derived from the analysis of dark-matter halos forming in LCDM simulations with similar set-ups. With the help of analytic models and numerical simulations we investigate the origin of this discrepancy focusing on the procedures used to derive the concentrations (circular velocity ratios versus density profile fitting) and on the selection criteria used to bin the halos (binning in maximum circular velocity versus binning in mass). We find that both steps of the analysis have a large impact on the resulting c-M relation. In particular, we show that the two c-M relations can be entirely reconciled, if we account for these methodological differences. Our analysis demonstrates that the concentration estimates are sensitive to the largely different radial scales probed by a particular measurement method. This implies that concentrations derived with different techniques (both in observations and in simulations) must be compared over the same radial range.
The mass spectrum of compact remnants from the parsec stellar evolution tracks

The mass spectrum of stellar-mass black holes (BHs) is highly uncertain. Dynamical mass measurements are available only for few ( 10) BHs in X-ray binaries, while theoretical models strongly depend on the hydrodynamics of supernova (SN) explosions and on the evolution of massive stars. In this paper, we present and discuss the mass spectrum of compact remnants that we obtained with SEVN, a new public populationsynthesis code, which couples the PARSEC stellar evolution tracks with up-to-date recipes for SN explosion (depending on the Carbon-Oxygen mass of the progenitor, on the compactness of the stellar core at pre-SN stage, and on a recent two-parameter criterion based on the dimensionless entropy per nucleon at pre-SN stage). SEVN can be used both as a stand-alone code and in combination with direct-summation N-body codes (Starlab, HiGPUs). The PARSEC stellar evolution tracks currently implemented in SEVN predict signicantly larger values of the Carbon-Oxygen core mass with respect to previous models. For most of the SN recipes we adopt, this implies substantially larger BH masses at low metallicity (6 2 10 3 ), than other populationsynthesis codes. The maximum BH mass found with SEVN is 25, 60 and 130 M at metallicity Z = 2 10 2 , 2 10 3 and 2 10 4 , respectively. Mass loss by stellar winds plays a major role in determining the mass of BHs for very massive stars (> 90 M ), while the remnant mass spectrum depends mostly on the adopted SN recipe for lower progenitor masses. We discuss the implications of our results for the transition between NS and BH mass, and for the expected number of massive BHs (with mass > 25 M ) as a function of metallicity.
Quantification of the spin-Hall anti-damping torque with a resonance spectrometer

We present a simple technique using a cavity-based resonance spectrometer to quantify the anti-damping torque due to the spin Hall effect. Modification of ferromagnetic resonance is observed as a function of small DC current in sub-mm-wide strips of bilayers, consisting of magnetically soft FeGaB and strong spin-Hall metal Ta. From the detected current-induced linewidth change, we obtain an effective spin Hall angle of 0.08-0.09 independent of the magnetic layer thickness. Our results demonstrate that a sensitive resonance spectrometer can be a general tool to investigate spin Hall effects in various material systems, even those with vanishingly low conductivity and magnetoresistance.
DETECTION OF IRON Kα EMISSION FROM A COMPLETE SAMPLE OF SUBMILLIMETER GALAXIES

We present an X-ray stacking analysis of a sample of 38 submillimeter galaxies (SMGs) with 〈z〉 = 2.6 discovered at ⩾4σ significance in the Lockman Hole North with the MAMBO array. We find a 5σ detection in the stacked soft band (0.5–2.0 keV) image, and no significant detection in the hard band (2.0–8 keV). We also perform rest-frame spectral stacking based on spectroscopic and photometric redshifts and find a ∼4σ detection of Fe Kα emission with an equivalent width of EW ≳ 1 keV. The centroid of the Fe Kα emission lies near 6.7 keV, indicating a possible contribution from highly ionized Fe xxv or Fe xxvi; there is also a slight indication that the line emission is more spatially extended than the X-ray continuum. This is the first X-ray analysis of a complete, flux-limited sample of SMGs with statistically robust radio counterparts.
The astrometric Gaia-FUN-SSO observation campaign of 99942 Apophis

Aims. Astrometric observations performed by the Gaia Follow-Up Network for Solar System Objects (Gaia-FUN-SSO) play a key role in ensuring that moving objects first detected by ESA’s Gaia mission remain recoverable after their discovery. An observation campaign on the potentially hazardous asteroid (99 942) Apophis was conducted during the asteroid’s latest period of visibility, from 12/21/2012 to 5/2/2013, to test the coordination and evaluate the overall performance of the Gaia-FUN-SSO . Methods. The 2732 high quality astrometric observations acquired during the Gaia-FUN-SSO campaign were reduced with the Platform for Reduction of Astronomical Images Automatically (PRAIA), using the USNO CCD Astrograph Catalogue 4 (UCAC4) as a reference. The astrometric reduction process and the precision of the newly obtained measurements are discussed. We compare the residuals of astrometric observations that we obtained using this reduction process to data sets that were individually reduced by observers and accepted by the Minor Planet Center. Results. We obtained 2103 previously unpublished astrometric positions and provide these to the scientific community. Using these data we show that our reduction of this astrometric campaign with a reliable stellar catalog substantially improves the quality of the astrometric results. We present evidence that the new data will help to reduce the orbit uncertainty of Apophis during its close approach in 2029. We show that uncertainties due to geolocations of observing stations, as well as rounding of astrometric data can introduce an unnecessary degradation in the quality of the resulting astrometric positions. Finally, we discuss the impact of our campaign reduction on the recovery process of newly discovered asteroids.
ISOTROPIC HEATING OF GALAXY CLUSTER CORES VIA RAPIDLY REORIENTING ACTIVE GALACTIC NUCLEUS JETS

Active galactic nucleus (AGN) jets carry more than sufficient energy to stave off catastrophic cooling of the intracluster medium (ICM) in the cores of cool-core clusters. However, in order to prevent catastrophic cooling, the ICM must be heated in a near-isotropic fashion and narrow bipolar jets with Pjet = 1044 − 45 erg s−1, typical of radio AGNs at cluster centers, are inefficient in heating the gas in the transverse direction to the jets. We argue that due to existent conditions in cluster cores, the supermassive black holes (SMBHs) will, in addition to accreting gas via radiatively inefficient flows, experience short stochastic episodes of enhanced accretion via thin disks. In general, the orientation of these accretion disks will be misaligned with the spin axis of the black holes (BHs) and the ensuing torques will cause the BH's spin axis (and therefore the jet axis) to slew and rapidly change direction. This model not only explains recent observations showing successive generations of jet–lobes–bubbles in individual cool-core clusters that are offset from each other in the angular direction with respect to the cluster center, but also shows that AGN jets can heat the cluster core nearly isotropically on the gas cooling timescale. Our model does require that the SMBHs at the centers of cool-core clusters be spinning relatively slowly. Torques from individual misaligned disks are ineffective at tilting rapidly spinning BHs by more than a few degrees. Additionally, since SMBHs that host thin accretion disks will manifest as quasars, we predict that roughly 1–2 rich clusters within z < 0.5 should have quasars at their centers.
The nature-based school curriculum: A solution to learning-teaching that promotes students’ freedom

This research aims to describe the nature-based school curriculum as a solution to the learning-teaching that promotes students’ freedom. The implementation of the learning-teaching is designed to be fun based on the natural characteristics of children. This research utilized a qualitative-descriptive method involving students, teachers, and parents as participants. Data were collected through observations, questionnaires, and interviews. The data analysis consisted of four stages: data collection, data reduction, data presentation and drawing conclusions. The results of this research indicate that the curriculum developed at the nature-based school is implemented by integrating the national curriculum with the natural school curriculum consisting of four pillars: morality, scientific logic, leadership, and entrepreneurship. The positive impact of this research is that the innovation of natural curriculum has been in line with the implementation of independent curriculum by implementing four pillars in learning-teaching process and are carried out through experience-based learning and project-based learning methods. Students are facilitated to express their opinions in different activities and are given the freedom to choose a place to learn in several activities. For example, in some activities, students are free to choose learning places which can be in the prayer room, in the school yard, in the library, or in other places. The learning-teaching can increase students’ enthusiasm to go to school, be happy, feel valued and feel free when they are at schools. With this nature-based school curriculum, children develop according to their nature and grow into meaningful, independent, and beneficial human beings in the surrounding environment who have noble character, have logical abilities, have a good leadership spirit, and have an entrepreneurial spirit.
The effect of liquidity ratio, activity ratio, and profitability ratio on accounting profit with firm size as a mediation

One of the important parameters in the financial statements used to measure management performance is profit. Financial ratios as one of the information in the financial statements are used to measure the company's financial performance as proxied by profit. This study aims to analyze the effect of liquidity ratios, activity, and profitability on accounting profit with firm size as a mediating variable on issuers of the consumer goods sector in 2016 - 2020. The research method used is path analysis with the AMOS 23.00 software analysis tool. The results show that the liquidity ratio has no effect on accounting profit, the activity ratio has a significant effect on accounting profit, the profitability ratio has a significant effect on accounting profit, and company size only mediates the liquidity ratio on accounting profit.
Young accreted globular clusters in the outer halo of M31

ABSTRACT We report on Gemini/GMOS observations of two newly discovered globular clusters inthe outskirts of M31. These objects, PAndAS-7 and PAndAS-8, lie at a galactocentricradius of ≈ 87 kpc and are projected, with separation ≈ 19 kpc, onto a ﬁeld halosubstructure known as the South-West Cloud. We measure radial velocities for the twoclusters which conﬁrm that they are almost certainly physically associated with thisfeature. Colour-magnitude diagrams reveal strikingly short, exclusively red horizontalbranchesin both PA-7 and PA-8; both also havephotometric [Fe/H] = −1.35±0.15. Atthis metallicity, the morphology of the horizontal branch is maximally sensitive to age,and we use the distinctive conﬁgurations seen in PA-7 and PA-8 to demonstrate thatboth objects are very likely to be at least 2 Gyr younger than the oldest Milky Wayglobular clusters. Our observations provide strong evidence for young globular clustersbeing accreted into the remote outer regions of M31 in a manner entirely consistentwith the established picture for the Milky Way, and add credence to the idea thatsimilar processes play a central role in determining the composition of globular clustersystems in large spiral galaxies in general.Key words: globular clusters: general, galaxies: individual: M31
Chenier Formation Through Wave Winnowing and Tides

Cheniers are ridges consisting of coarse‐grained sediments, resting on top of the fine sediment that forms the otherwise muddy coast. In this paper, we use Delft3D to explore how cheniers are formed through wave winnowing. We identify three phases of chenier development: (a) a winnowing phase, during which mud is washed out of the seabed initially consisting of a mixture of sand and mud, (b) a sand transport phase, when the sand in the upper layer is transported onshore, and (c) a crest formation phase, during which a chenier crest rapidly develops at the landward limit of onshore sediment transport. The main mechanism driving onshore sand transport is wave asymmetry. During calm conditions, sand transport takes place within a narrow band limiting the volume of sand delivered nearshore, and therefore no chenier develops. In contrast, average storm conditions mobilize sufficient sand for a crest to develop. Our results thus reveal that chenier formation through wave winnowing does not require extreme storm conditions. Furthermore, our study showed that chenier formation through wave winnowing is a relatively slow process, with the largest time scales associated with the winnowing and sand transport. Once sufficient sand is available in the intertidal zone, the crest develops rapidly.
THERMAL INSTABILITY AND MULTI-PHASE INTERSTELLAR MEDIUM IN THE FIRST GALAXIES

We examine the linear stability and nonlinear growth of the thermal instability in isobarically contracting background gas with various metallicities and far-UV (FUV) field strengths. Such a background medium can be expected for protogalactic clouds and shocked gas with metallicity Z / Z ⊙ > 10 − 4 ? > . When the H2 cooling is suppressed by FUV fields ( G 0 > 10 − 3 ? > ) or the metallicity is high enough ( Z / Z ⊙ > 10 − 3 ? > ), the interstellar medium (ISM) is thermally unstable in the temperature range 100–7000 K owing to the cooling by C ii and O i fine-structure lines. In this case, a bi-phasic medium with a bimodal density probability distribution is formed as a consequence of the thermal instability. The characteristic scales of the thermal instability become smaller with increasing metallicity. Comparisons of the nonlinear simulations with different resolution indicates that the maximum scale of the thermal instability should be resolved with more than 60 cells to follow runaway cooling driven by the thermal instability. Under sufficiently weak FUV fields and with low metallicity, the density range of the thermal instability shrinks owing to the dominance of H2 cooling. As the FUV intensity is reduced, the bi-phasic structure becomes less remarkable and eventually disappears. Our basic results suggest that, in early galaxies, (i) fragmentation by the nonlinear growth of thermal instability could determine the mass spectrum of star clusters for Z / Z ⊙ ≲ 0.04 ? > , and (ii) a thermally bistable turbulent ISM like our galaxy becomes ubiquitous for Z / Z ⊙ ≳ 0.04 ? > , although the threshold metallicity depends on conditions such as thermal pressure, FUV strength, and redshift.
Evaluation of Hash Join Operations Performance Executing on SDN Switches: A Cost Model Approach

Distributed database systems store and manipulate data on multiple machines. In these systems, the processing cost of query operations is mainly impacted by the data access latency between machines over the network. With recent technology advances in programmable network devices, the network switches provide new opportunities for dynamically managing the network topology, enabling the data processing on these devices with the same network throughput. In this paper, we explore the programmable network switches in query processing, evaluating the processing performance of a cost model in executing the hash join operation. We assume the storage of the hash table built from outer relation and the materialization of the join probing are made in switches using advanced matching techniques similar to package inspections enabled by Ternary Content-Addressable Memories (TCAM) or SRAM via hashing. Our results show that processing the hash join operation using network switches achieved the best results compared to traditional servers, with an average time reduction of 91.82% (Query-10 from TPC-H) and 96.52% (Query-11 from TPC-H).
Far-Infrared Surveys of Galaxy Evolution

Roughly half of the radiation from evolving galaxies in the early Universe reaches us in the far-infrared and submillimeter wavelength ranges. Recent major advances in observing capabilities, in particular the launch of the Herschel Space Observatory in 2009, have dramatically enhanced our ability to use this information in the context of multiwavelength studies of galaxy evolution. Near its peak, three-quarters of the cosmic infrared background is now resolved into individually detected sources. The use of far-infrared diagnostics of dust-obscured star formation and of interstellar medium conditions has expanded from extreme and rare extreme high-redshift galaxies to more typical main-sequence galaxies and hosts of active galactic nuclei out to z≳2. These studies shed light on the evolving role of steady equilibrium processes and of brief starbursts at and since the peak of cosmic star formation and black hole accretion. This review presents a selection of recent far-infrared studies of galaxy evolution .
Combining physical galaxy models with radio observations to constrain the SFRs of high-z dusty star-forming galaxies

We complement our previous analysis of a sample of z similar to 1-2 luminous and ultraluminous infrared galaxies [(U)LIRGs], by adding deep Very Large Array radio observations at 1.4 GHz to a large data set from the far-UV to the submillimetre, including Spitzer and Herschel data. Given the relatively small number of (U)LIRGs in our sample with high signal-to-noise (SIN) radio data, and to extend our study to a different family of galaxies, we also include six well-sampled near-infrared (near-IR)-selected BzK galaxies at z similar to 1.5. From our analysis based on the radtran spectral synthesis code GRASIL, we find that, while the IR luminosity may be a biased tracer of the star formation rate (SFR) depending on the age of stars dominating the dust heating, the inclusion of the radio flux offers significantly tighter constraints on SFR. Our predicted SFRs are in good agreement with the estimates based on rest-frame radio luminosity and the Bell calibration. The extensive spectrophotometric coverage of our sample allows us to set important constraints on the star formation (SF) history of individual objects. For essentially all galaxies, we find evidence for a rather continuous SFR and a peak epoch of SF preceding that of the observation by a few Gyr. This seems to correspond to a formation redshift of z similar to 5-6. We finally show that our physical analysis may affect the interpretation of the SFR-M-* diagram, by possibly shifting, with respect to previous works, the position of the most dust obscured objects to higher M-*, and lower SFRs.
Positivity of Legendrian Thom polynomials

We study Legendrian singularities arising in complex contact geometry. We define a one-parameter family of bases in the ring of Legendrian characteristic classes such that any Legendrian Thom polynomial has nonnegative coefficients when expanded in these bases. The method uses a suitable Lagrange Grassmann bundle on the product of projective spaces. This is an extension of a nonnegativity result for Lagrangian Thom polynomials obtained by the authors previously. For a fixed specialization, other specializations of the parameter lead to upper bounds for the coefficients of the given basis. One gets also upper bounds of the coefficients from the positivity of classical Thom polynomials (for mappings), obtained previously by the last two authors.