Overcoming ambiguities in classical and quantum correlation measures

We identify ambiguities in the available frameworks for defining quantum, classical, and total correlations as measured by discordlike quantifiers. More specifically, we determine situations for which either classical or quantum correlations are not uniquely defined due to degeneracies arising from the optimization procedure over the state space. In order to remove such degeneracies, we introduce a general approach where correlations are independently defined, escaping therefore from a degenerate subspace. As an illustration, we analyze the trace-norm geometric quantum discord for two-qubit Bell-diagonal states.Comment: 5 pages, 2 figures. v2: Minor corrections. Published versio

A grid of Synthetic Spectra for Hot DA White Dwarfs and Its Application in Stellar Population Synthesis

In this work we present a grid of LTE and non-LTE synthetic spectra of hot DA white dwarfs (WDs). In addition to its usefulness for the determination of fundamental stellar parameters of isolated WDs and in binaries, this grid will be of interest for the construction of theoretical libraries for stellar studies from integrated light. The spectral grid covers both a wide temperature and gravity range, with 17,000 K <= T_eff <= 100,000 K and 7.0 <= log(g) <= 9.5. The stellar models are built for pure hydrogen and the spectra cover a wavelength range from 900 A to 2.5 microns. Additionally, we derive synthetic HST/ACS, HST/WFC3, Bessel UBVRI and SDSS magnitudes. The grid was also used to model integrated spectral energy distributions of simple stellar populations and our modeling suggests that DAs might be detectable in ultraviolet bands for populations older than ~8 Gyr.Comment: to be published in The Astrophysical Journal Supplement Serie

Geometric classical and total correlations via trace distance

We introduce the concepts of geometric classical and total correlations through Schatten 1-norm (trace norm), which is the only Schatten p-norm able to ensure a well-defined geometric measure of correlations. In particular, we derive the analytical expressions for the case of two-qubit Bell-diagonal states, discussing the superadditivity of geometric correlations. As an illustration, we compare our results with the entropic correlations, discussing both their hierarchy and monotonicity properties. Moreover, we apply the geometric correlations to investigate the ground state of spin chains in the thermodynamic limit. In contrast to the entropic quantifiers, we show that the classical correlation is the only source of 1-norm geometric correlation that is able to signaling an infinite-order quantum phase transition.Comment: v2: published versio

Angular Correlation Function from sample covariance with BOSS and eBOSS LRG

The Baryon Acoustic Oscillations (BAO) are one of the most used probes to understand the accelerated expansion of the Universe. Traditional methods rely on fiducial model information within their statistical analysis, which may be a problem when constraining different families of models. The aim of this work is to provide a method that constrains $\theta_{BAO}$ through a model-independent and compare parameter estimation of the angular correlation function polynomial approach, using the covariance matrix from the galaxy sample from thin redshift bins, with the usual mock sample covariance matrix. We proposed a different approach to finding the BAO angular feature revisiting previous work in the literature, we take the bias between the correlation function between the bins and the whole sample. We used widths of $\delta z = 0.002$ separation for all samples as the basis for a sample covariance matrix weighted by the statistical importance of the redshift bin. We propose a different weighting scheme based only on random pair counting. We also propose an alternate shift parameter based only on the data. Each sample belongs to the Sloan Digital Sky Survey Luminous Red Galaxies (LRG): BOSS1, BOSS2, and eBOSS, with effective redshift $z_{eff}$: 0.35, 0.51, 0.71, respectively, and different numbers of bins with 50, 100, and 200 respectively. In addition, we correct the angular separation from the polynomial fit ($\theta_{fit}$) that encodes the BAO feature with a bias function obtained by comparing each bin correlation function with the correlation function of the whole set. We also tested the same correction choosing the bin at $z_{eff}$ and found that for eBOSS $\theta_{BAO}$ is in $1 \sigma$ agreement with the Planck 18 model. BOSS1 and BOSS2 $\theta_{BAO}$ agreed in $1\sigma$ with the Pantheon+ & S$H_0$ES Flat$\Lambda$CDM model, in tension with Planck 18.Comment: 18 page

O uso da argumentação na montagem de um modelo

Trabalhos recentes na área de Ensino de ciência têm tratado a argumentação como parte imprescindível das aulas de ciência, pois argumentar seria uma das características da ciência. A forma de análise recorrente em tais trabalhos é o padrão criado por Toulmin, que permite uma divisão do argumento e a identificação de seus elementos constituintes. Foi analisada uma seqüência didática com as turmas de 3º ano da escola de Aplicação da Universidade de São Paulo que culminou na montagem de um modelo de DNA. Tal montagem foi feita em grupos e as discussões ocorridas durante a tarefa foram gravadas e transcritas. A análise dos discursos mostrou argumentos simples compostos basicamente por dados e conclusão. A atividade se mostra diferente da ciência já que não são defendidos pontos de vista sobre uma questão aberta, mas sim opiniões sobre algo já estabelecido

Observations of the SW Sextantis star DW Ursae Majoris with the Far Ultraviolet Spectroscopic Explorer

We present an analysis of the first far-ultraviolet observations of the SW Sextantis-type cataclysmic variable DW Ursae Majoris, obtained in November 2001 with the Far Ultraviolet Spectroscopic Explorer. The time-averaged spectrum of DW UMa shows a rich assortment of emission lines (plus some contamination from interstellar absorption lines including molecular hydrogen). Accretion disk model spectra do not provide an adequate fit to the far-ultraviolet spectrum of DW UMa. We constructed a light curve by summing far-ultraviolet spectra extracted in 60-sec bins; this shows a modulation on the orbital period, with a maximum near photometric phase 0.93 and a minimum half an orbit later. No other periodic variability was found in the light curve data. We also extracted spectra in bins spanning 0.1 in orbital phase; these show substantial variation in the profile shapes and velocity shifts of the emission lines during an orbital cycle of DW UMa. Finally, we discuss possible physical models that can qualitatively account for the observed far-ultraviolet behavior of DW UMa, in the context of recent observational evidence for the presence of a self-occulting disk in DW UMa and the possibility that the SW Sex stars may be the intermediate polars with the highest mass transfer rates and/or weakest magnetic fields.Comment: accepted by the Astronomical Journal; 36 pages, including 12 figures and 4 table