Miracle-dz/UniFAR-FTUs huggingface dataset:
The Relationship Between Eastern Equatorial Pacific Sea Surface Temperatures and Rainfall over India and Sri Lanka

Abstract Monsoon season (June–September) precipitation data from 31 Indian subdivisions and mean monthly precipitation data from 35 Indian and Sri Lanka stations, spanning the period 1875–79, were analyzed to determine the relationship between equatorial Pacific warm episodes (El Nino events) and interannual fluctuations in precipitation over India and Sri Lanka. The data reveal a strong tendency for a below normal summer monsoon during the 25 moderate/strong warm episodes which occurred during the period. For example, area-averaged June–September rainfall over India was below the median value in 21 of the 25 warm episode years. These years include the five largest, and nine of the eleven largest, negative monsoon season anomalies. Considerably smaller average departures occurred during the monsoon seasons of the year preceding and the year following the warm episode, and during the remaining months of the warm episode year. The anomaly pattern over Sri Lanka and extreme southern India is quite different,.
Probing evolutionary population synthesis models in the near infrared with early-type galaxies

LGDH thanks CAPES and CNPq. RR thanks CNPq and FAPERGS for partial funding of this project. ARA thanks CNPq for partial support to this work. LPM thanks CNPQ and FAPESP for partial funding of this project. CK acknowledges support through the research project AYA2017-79724-C4-4-P from the Spanish PNAYA. This research made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This study uses data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://califa.caha.es/). Based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). We thank the referee Reynier Peletier for carefully reading our paper and for giving such constructive comments which substantially helped improving the quality of the paper.
Renormalization group flow, stability, and bulk viscosity in a large N thermal QCD model

The ultraviolet completion of a large N QCD model requires introducing new degrees of freedom at certain scale so that the UV behavior may become asymptotically conformal with no Landau poles and no UV divergences of Wilson loops. These UV degrees of freedom are represented by certain antibranes arranged on the blown-up sphere of a warped resolved conifold in a way that they are separated from the other set of branes that control the IR behavior of the theory. This separation of the branes and the antibranes creates instability in the theory. Further complications arise from the curvature of the ambient space. We show that, despite these analytical hurdles, stability may still be achieved by switching on appropriate world-volume fluxes on the branes. The UV degrees of freedom, on the other hand, modify the RG flow in the model. We discuss this in details by evaluating the flow from IR confining to UV conformal. Finally we lay down a calculational scheme to study bulk viscosity which, in turn, would signal the inherent nonconformality in this model.
Hubble Space Telescope Far‐Ultraviolet Spectroscopy of the Dwarf Nova VW Hydri in Superoutburst

We obtained three consecutive Hubble Space Telescope spectroscopic observations of a single superoutburst of the dwarf nova VW Hydri. The spectra cover the beginning, middle, and end of the superoutburst. All of the spectra are dominated by strong absorption lines due to C iii (1175 Å), Lyα (1216 Å), N iv (1238 and 1242 Å), S ii (1260–1565 Å), S iii (1300 Å), C ii (1335 Å), S iv (1394 and 1402 Å), and C iv (1548 and 1550 Å). We discuss the evolution of the far‐UV energy distribution and line structure during the superoutburst. We note the absence of any P Cygni line structure in the Space Telescope Imaging Spectrograph spectra. Using state‐of‐the‐art accretion disk models by Wade & Hubeny, we have determined for all three spectra accretion rates for two white dwarf masses, 0.55 and 0.8 M⊙. For both white dwarf masses, the accretion rate during superoutburst decreased by a factor of 2 from early to late in the superoutburst. The average accretion rate during superoutburst is (3–6) × 10−9 M⊙ yr−1, depending on the white dwarf mass.
Chiral Dynamics of the Two Λ(1405) States

The Λ(1405) resonance is studied by a chiral unitary approach, in which the reso- nance is dynamically generated in coupled-channel meson-baryon scattering. Inves-tigating the analytic structure of the scattering amplitudes obtained by the chiral unitary approach, we ﬁnd two poles around the energies of the Λ(1405) coupling diﬀerently to the meson-baryon states. We reach the conclusion that the Λ(1405) resonance seen in experiments is not just one single resonance, but a superposition of these two states.
Fractionalization of a flux quantum in a one-dimensional parallel Josephson junction array with alternating π junctions

We study numerically and analytically the properties of a one-dimensional array of parallel Josephson junctions in which every alternate junction is a $\ensuremath{\pi}$ junction. In the ground state of the array, each cell contains spontaneous magnetic flux $\ensuremath{\Phi}l~{\ensuremath{\Phi}}_{0}/2$ which shows antiferromagnetic ordering along the array. We find that an externally introduced $2\ensuremath{\pi}$ fluxon ${\ensuremath{\Phi}}_{0}$ in such an array is unstable and fractionalizes into two $\ensuremath{\pi}$ fluxons of magnitude $\frac{1}{2}{\ensuremath{\Phi}}_{0}. $ We attribute this fractionalization to the degeneracy of the ground state of the array. The magnitude of the flux in the fractional fluxons can be controlled by changing the critical current of the $\ensuremath{\pi}$ junctions relative to the 0 junctions. In the presence of an external current, the fluxon lattice in the antiferromagnetic ground state can be depinned. We also observe a resonant structure in the $V\ensuremath{-}I$ characteristics above the depinning current due to the interaction between the fluxon lattice and the array.
SHOCK-EXCITED MASER EMISSION FROM THE SUPERNOVA REMNANT W28

We present VLA observations in the hydroxyl line OH(1720 MHz) towards the supernova remnant W28. These high resolution images show a more extensive distribution of 1720 MHz emission than had previously been suspected from earlier single-dish observations. A total of 26 distinct maser spots were detected which lie on the edge of the radio continuum emission from W28 and are unresolved with our 12 arcsec resolution. Significant detection of linear and circular polarization in the maser spots is also made. The location of the maser spots, together with the physical conditions in the SNR and the adjacent molecular cloud, argue for a shock excitation mechanism. The possibilities of using the OH(1720 MHz) as a powerful diagnostic of the interaction of supernova remnants with molecular clouds is discussed.
A Comparison of cosmological models using recent supernova data

We study the expansion history of the universe up to a redshift of $\mathrm{z}=1.75$ using the 194 recently published SnIa data by Tonry et al. and Barris et al. In particular we find the best fit forms of several cosmological models and $H(z)$ ansatze, determine the best fit values of their parameters and rank them according to increasing value of ${\ensuremath{\chi}}_{\mathrm{min}}^{2}$ [the minimum value of ${\ensuremath{\chi}}^{2}$ for each $H(z)$ ansatz]. We treat ${\ensuremath{\Omega}}_{0m}$ as a parameter using a reasonable prior and assume flat geometry of the universe. No prior assumptions are made about validity of energy conditions. The fitted models are fourteen and include standard cold dark matter (SCDM), cold dark matter with cosmological constant \ensuremath{\Lambda} (LCDM), dark energy with constant equation of state parameter w (quiessence), third order polynomial for $H(1+z),$ Chaplygin gas, Cardassian model, ${w(z)=w}_{0}{+w}_{1}z,$ ${w(z)=w}_{0}{+zw}_{1}/(1+z),$ an oscillating ansatz for $H(z),$ etc. All these models with the exception of SCDM are consistent with the present data. However, the quality of the fit differs significantly among them and so do the predicted forms of $w(z)$ and $H(z)$ at best fit. The worst fit among the data-consistent models considered corresponds to the simplest model LCDM $({\ensuremath{\chi}}_{\mathrm{min}}^{2}=198.7$ for ${\ensuremath{\Omega}}_{0m}=0.34)$ while the best fit is achieved by the three parameter oscillating ansatz $({\ensuremath{\chi}}_{\mathrm{min}}^{2}=193.8). $ Most of the best fit ansatze have an equation of state parameter $w(z)$ that varies between $w(z)\ensuremath{\simeq}\ensuremath{-}1$ for $zl0.5$ to $w(z)g0$ for $zg1. $ This implies that the sign of the pressure of the dark energy may be alternating as the redshift increases. The goodness of fit of the oscillating $H(z)$ ansatz lends further support to this possibility.
The Location and Environments of Neutron Star Mergers in an Evolving Universe

The simultaneous detection of gravitational and electromagnetic waves from a binary neutron star merger has both solidified the link between neutron star mergers and short-duration gamma-ray bursts (GRBs), and demonstrated the ability of astronomers to follow-up the gravitational wave detection to place constraints on the ejecta from these mergers, as well as the nature of the GRB engine and its surroundings. As the sensitivity of aLIGO and VIRGO increases, it is likely that a growing number of such detections will occur in the next few years, leading to a sufficiently large number of events to constrain the populations of these GRB events. While long-duration GRBs originate from massive stars and thus are located near their stellar nurseries, binary neutron stars may merge on much longer timescales, and thus may have had time to migrate appreciably. The strength and character of the electromagnetic afterglow emission of binary neutron star mergers is a sensitive function of the circum-merger environment. Though the explosion sites of short GRBs have been explored in the literature, the question has yet to be fully addressed in its cosmological context. We present cosmological simulations following the evolution of a galaxy cluster, including star formation combined with binary population synthesis models, to self-consistently track the locations and environmental gas densities of compact binary merger sites throughout the cosmic web. We present probability distributions for densities as a function of redshift and discuss model sensitivity to population synthesis model assumptions.
SDSS-IV MaNGA: Star Formation Cessation in Low-redshift Galaxies. I. Dependence on Stellar Mass and Structural Properties

We investigate radial gradients in the recent star formation history (SFH) of 1917 galaxies with 0.01 < z < 0.14 from the Mapping Nearby Galaxies at Apache Point Observatory project. For each galaxy, we obtain two-dimensional maps and radial profiles for three spectroscopically measured parameters that are sensitive to the recent SFH: Dn(4000) (the 4000 Å break), EW(HδA), and EW(Hα) (the equivalent width of the Hδ absorption and the Hα emission line). The majority of the spaxels are consistent with models of a continuously declining star formation rate, indicating that starbursts occur rarely in local galaxies with regular morphologies. We classify the galaxies into three classes: fully star-forming (SF), partly quenched (PQ), and totally quenched (TQ). The galaxies that are less massive than 1010 M⊙ present at most weak radial gradients in the diagnostic parameters. In contrast, massive galaxies with a stellar mass above 1010 M⊙ present significant gradients in the three diagnostic parameters if they are classified as SF or PQ but show weak gradients in Dn(4000) and EW(HδA) and no gradients in EW(Hα) if they are in the TQ class. This implies the existence of a critical stellar mass (∼1010 M⊙) above which the star formation in a galaxy is shut down from the inside out. Galaxies tend to evolve synchronously from the inner to the outer regions before their mass reaches the critical value. We have further divided the sample at a fixed mass by both bulge-to-total luminosity ratio and morphological type, finding that our conclusions hold regardless of these factors; it appears that the presence of a central dense object is not a driving parameter but rather a by-product of the star formation cessation process.
The Hard X-Ray Spectral Slope as an Accretion Rate Indicator in Radio-quiet Active Galactic Nuclei

We present new XMM-Newton observations of two luminous and high accretion rate radio-quiet active galactic nuclei (AGNs) at z ~ 2. Together with archival X-ray and rest-frame optical spectra of three sources with similar properties, as well as 25 moderate-luminosity radio-quiet AGNs at z < 0.5, we investigate, for the first time, the dependence of the hard (≳2 keV) X-ray power-law photon index on the broad Hβ emission-line width and on the accretion rate across ~3 orders of magnitude in AGN luminosity. Provided that the accretion rates of the five luminous sources can be estimated by extrapolating the well-known relation between the broad-line region size and luminosity to high luminosities, we find that the photon indices of these sources, while consistent with those expected from their accretion rates, are significantly higher than expected from the widths of their Hβ lines. We argue that within the limits of our sample, the hard X-ray photon index depends primarily on the accretion rate.
Detection of a giant white-light flare on an L2.5 dwarf with the Next Generation Transit Survey

We present the detection of a ΔV ∼ −10 flare from the ultracool L2.5 dwarf ULAS J224940.13−011236.9 with the Next Generation Transit Survey (NGTS). The flare was detected in a targeted search of late-type stars in NGTS full-frame images and represents one of the largest flares ever observed from an ultracool dwarf. This flare also extends the detection of white-light flares to stars with temperatures below 2000 K. We calculate the energy of the flare to be $3.4^{+0.9}_{-0.7}\times 10^{33}$ erg, making it an order of magnitude more energetic than the Carrington event on the Sun. Our data show how the high-cadence NGTS full-frame images can be used to probe white-light flaring behaviour in the latest spectral types.
A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5: Gas Mass and Its Fraction Revealed with ALMA

We investigate gas contents of star-forming galaxies associated with protocluster 4C23.56 at z = 2.49 by using the redshifted CO (3–2) and 1.1 mm dust continuum with the Atacama Large Millimeter/submillimeter Array. The observations unveil seven CO detections out of 22 targeted Hα emitters (HAEs) and four out of 19 in 1.1 mm dust continuum. They have high stellar mass ( M⊙) and exhibit a specific star-formation rate typical of main-sequence star-forming galaxies at . Different gas-mass estimators from CO (3–2) and 1.1 mm yield consistent values for simultaneous detections. The gas mass ( ) and gas fraction ( ) are comparable to those of field galaxies, with )) , where is the CO-to-H2 conversion factor and A(Z) is the additional correction factor for the metallicity dependence of , and from CO (3–2). Our measurements place a constraint on the cosmic gas density of high-z protoclusters, indicating that the protocluster is characterized by a gas density higher than that of the general fields by an order of magnitude. We found with the CO(3–2) detections. The five ALMA CO detections occur in the region of highest galaxy surface density, where the density positively correlates with global star-forming efficiency (SFE) and stellar mass. Such correlations possibly indicate a critical role of the environment on early galaxy evolution at high-z protoclusters, though future observations are necessary for confirmation.
Discovery of an Edge-On Disk in the MBM 12 Young Association

We report the discovery of a spatially resolved edge-on protoplanetary disk in the ~2 Myr old MBM 12 young association. Our near-infrared images of LkHα 263C (MBM 12A 3C), obtained with the Hokupa`a adaptive optics system on the Gemini North telescope, clearly show two elongated reflection nebulosities separated by a dark lane, a morphology well matched by scattered-light models of an optically thick (at near-infrared wavelengths) edge-on disk. An optical spectrum of the scattered-light nebulosity obtained with the Keck II telescope exhibits a spectral type of M0 ± 0.5 (Teff = 3850 ± 100 K) for the central star and contains Hα and forbidden emission lines, which may indicate the presence of a jet. The absence of a near-infrared point source implies AK > 9.5 toward the unseen central star. The disk is flared and has a radius of ~150 AU (at a distance of 275 pc) and an inclination of 87°. The aspect ratio of the model disk in the J band is 0.72. There is possible evidence of dust settling to the disk midplane. LkHα 263C is 4. ″115 from the 0. ″415 binary LkHα 263 A and B (MBM 12A 3A and 3B), which is itself 15. ″5 from LkHα 262 (MBM 12A 2). Thus, LkHα 263C may be the first disk to be clearly resolved around an individual star in a young quadruple system. The detection of a faint edge-on disk near a bright star demonstrates both the high angular resolution and the high sensitivity that can be achieved with adaptive optics imaging on large telescopes.
Momentum distribution in the decay B-->J/ψ+X

We combine the NRQCD formalism for the inclusive color singlet and octet production of charmonium states with the parton and the ACCMM model, respectively, and calculate the momentum distribution in the decay B{r_arrow}J/{psi}+X. Neglecting the kinematics of soft gluon radiation, we find that the motion of the b quark in the bound state can account, to a large extent, for the observed spectrum. The parton model gives a satisfactory presentation of the data, provided that the heavy quark momentum distribution is taken to be soft. To be explicit, we obtain {var_epsilon}{sub p}{approximately}0.008{endash}0.012 for the parameter of the distribution function of Peterson {ital et al.} The ACCMM model can account for the data more accurately. The preferred Fermi momentum p{sub F}{congruent}0.57GeV is in good agreement with recent studies of the heavy quark{close_quote}s kinetic energy. {copyright} {ital 1997} {ital The American Physical Society}
Magnetic topology and surface differential rotation on the K1 subgiant of the RS CVn system HR 1099

We present here spectropolarimetric observations of the RS CVn system HR 1099 (V711 Tau) secured from 1998 February to 2002 January with the spectropolarimeter MuSiCoS at the Telescope Bernard Lyot (Observatoire du Pic du Midi, France). We apply Zeeman–Doppler imaging and reconstruct surface brightness and magnetic topologies of the K1 primary subgiant of the system, at five different epochs. We confirm the presence of large, axisymmetric regions where the magnetic field is mainly azimuthal, providing further support to the hypothesis that dynamo processes may be distributed throughout the whole convective zone in this star. We study the short-term evolution of surface structures from a comparison of our images with observations secured at close-by epochs by Donati et al. at the Anglo-Australian Telescope. We conclude that the small-scale brightness and magnetic patterns undergo major changes within a time-scale of 4–6 weeks, while the largest structures remain stable over several years. We report the detection of a weak surface differential rotation (both from brightness and magnetic tracers) indicating that the equator rotates faster than the pole with a difference in rotation rate between the pole and the equator about four times smaller than that of the Sun. This result suggests that tidal forces also affect the global dynamic equilibrium of convective zones in cool active stars.
Hyperon polarization in heavy-ion collisions and holographic gravitational anomaly

We study the energy dependence of global polarization of $\Lambda$ hyperons in peripheral $Au-Au$ collisions. We combine the calculation of vorticity and strange chemical potential in the framework of kinetic Quark-Gluon String Model with the anomalous mechanism related to axial vortical effect. We pay special attention to the temperature dependent contribution related to gravitational anomaly and found that the preliminary RHIC data are compatible with its suppression discovered earlier in lattice calculations.
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations

We model the galaxy formation in a series of high-resolution N-body simulations using the semianalytical approach. Unlike many earlier investigations based on semianalytical models, we make use of the subhalos resolved in the N-body simulations to follow the mergers of galaxies in dark halos, and we show that this is pivotal in modeling correctly the galaxy luminosity function at the bright end and the bimodal nature of galaxy color distribution. Mergers of galaxies based on subhalos also result in many more bright red galaxies at high z. The semianalytical model we adopt is similar to those used in earlier semianalytical studies, except that we consider the effect of a prolonged cooling in small halos and that we explicitly follow the chemical enrichment in the interstellar medium. We use our model to make predictions for the properties of the galaxy population at low redshift and compare them with various current observations. We find that our model predictions can match the luminosity functions of galaxies in various wavebands redder than the u band. The shape of the luminosity function at the bright end is well reproduced if galaxy mergers are modeled with the merger trees of subhalos, and the steep faint-end slope can be moderated if the gas cooling time in low-mass halos is comparable to the age of the universe. The model with subhalos resolved can reproduce the main features in the observed color bimodal distribution, although it still predicts too many bright blue galaxies. The same model can also match the color-magnitude relation for elliptical galaxies in clusters, the metallicity-luminosity relation and metallicity-rotation velocity relation of spiral galaxies, and the gas fraction in present-day spiral galaxies. We also identify areas where further improvements of the model are required.