Parametrització de contorns oberts

Un dels principals problemes quan es realitza un anàlisi de contorns és la gran quantitat de dades implicades en la descripció de la figura. Per resoldre aquesta problemàtica, s’aplica la parametrització que consisteix en obtenir d’un contorn unes dades representatives amb els mínims coeficients possibles, a partir dels quals es podrà reconstruir de nou sense pèrdues molt evidents d’informació. En figures de contorns tancats, la parametrització més estudiada és l’aplicació de la transformada discreta de Fourier (DFT). Aquesta s’aplica a la seqüència de valors que descriu el comportament de les coordenades x i y al llarg de tots els punts que formen el traç. A diferència, en els contorns oberts no es pot aplicar directament la DFT ja que per fer-ho es necessita que el valor de x i de y siguin iguals tan en el primer punt del contorn com en l’últim. Això és degut al fet que la DFT representa sense error senyals periòdics. Si els senyals no acaben en el mateix punt, representa que hi ha una discontinuïtat i apareixen oscil·lacions a la reconstrucció. L’objectiu d’aquest treball és parametritzar contorns oberts amb la mateixa eficiència que s’obté en la parametrització de contorns tancats. Per dur-ho a terme, s’ha dissenyat un programa que permet aplicar la DFT en contorns oberts mitjançant la modificació de les seqüencies de x i y. A més a més, també utilitzant el programari Matlab s’han desenvolupat altres aplicacions que han permès veure diferents aspectes sobre la parametrització i com es comporten els Descriptors El·líptics de Fourier (EFD). Els resultats obtinguts han demostrat que l’aplicació dissenyada permet la parametrització de contorns oberts amb compressions òptimes, fet que facilitarà l’anàlisi quantitatiu de formes en camps com l’ecologia, medicina, geografia, entre d’altres.

Consultoria del procés de logística interna del laboratori d'anàlisis clíniques a l'Hospital General de Vic

Com a resultat de les politiques i estratègies de col·laboració entre la universitat de Vic i de l’hospital i de la voluntat de realitzar activitats formatives conjuntes , s’estableix un línia de treball orientada a l’estudi i anàlisi de la situació logística interna actual del laboratori d’anàlisis clíniques de l’Hospital General de Vic. El treball es centra en el procés intern del laboratori i l’abast de l’estudi es troba limitat a les àrees especifiques d’hematologia i coagulació i bioquímica. D’aquestes dues àrees el treball realitza un estudi exhaustiu del seu procés intern, identifica les seves activitats i la seva metodologia de treball amb l’objectiu d’elaborar el Value Stream Map de cadascuna de les àrees. Les àrees de Microbiologia, Banc de Sang i Urgències resten fora d’aquest estudi exhaustiu tot i que són presents en el treball per la inevitable interacció que tenen en la globalitat del procés. El treball es centra bàsicament en els processos automatitzats tot i que els processos que es duen a terme en el laboratori són tant automatitzats com manuals. També es limita al sistema productiu intern del laboratori tot i la interacció que té aquest sistema intern amb altres centres productius del sistema com ara són els centres d’atenció primària, els diversos hospitals i centres d’atenció sociosanitària. El laboratori es troba immers en el moment de l’elaboració d’aquest treball en un situació de canvi i millora del seus processos interns que consisteixen principalment en la substitució de part la maquinària actual que obliguen a la definició d’un nou layout i d’una nova distribució de la producció a cada màquina. A nivell extern també s’estan produint millores en el sistema informàtic de gestió que afecten a part del seu procés. L’objectiu del treball és donar visibilitat total al procés de logística interna actual del laboratori, identificant clarament com són i quina seqüència tenen els processos logístics interns i els mètodes de treball actuals, tant de recursos màquina com recursos persona, per poder identificar sota una perspectiva de generació de valor, aquells punts concrets de la logística interna que poden ser millorats en quant a eficiència i productivitat amb l’objectiu que un cop identificats es puguin emprendre accions i/o projectes de millora. El treball finalitza amb un anàlisis final del procés logística interna des d’una òptica Lean. Per fer-ho, identifica aquelles activitats que no aporten valor al procés o MUDA i les classifica en set categories i es realitzen diverses propostes de millora com són la implantació d’un flux continu , anivellat i basat en un concepte pull , identifica activitats que poden ser estandarditzades i/o simplificades i proposa modificacions en les infraestructures físiques per donar major visibilitat al procés. L’aspecte humà del procés es planteja des d’un punt de vist de metodologia, formació, comunicació i aplicació de les 5S.

UBVRI photoelectric photometry of nearby stars. II.

A second set of UBVRI photometry results for nearby stars of Gliese's (1969) catalog and its supplements, including in this case some multiple systems, are presented. Most of the observations were carried out between July 1984 and December 1985 at Calar Alto with the 1.23-m Centro Astronomico Hispano-Aleman telescope and the 1.52-m Observatorio Astronomico Nacional telescope. The number of observations of program and standard stars for the six runs and the final results for 60 stars are presented.

Microquasars as high energy gamma-ray sources

Galactic microquasars are certainly one of the most recent additions to the field of high energy astrophysics and have attracted increasing interest over the last decade. However, the high energy part of the spectrum of microquasars is the most poorly known, mainly due the lack of sensitive instrumentation in the past. Microquasars are now primary targets for all of the observatories working in the X-ray and gamma-ray domains. They also appear as the possible counterparts for some of the unidentified sources of high-energy gamma-rays detected by the experiment EGRET on board the satellite COMPTON-GRO. This paper provides a general review of the main observational results obtained up to now as well as a summary of the scenarios for production of high-energy gamma-rays at the present moment.

Exploring the high frequency emission of radio loud X-ray binaries

We report millimetre-wave continuum observations of the X-ray binaries Cygnus X-3, SS 433, LSI+61 303, Cygnus X-1 and GRS 1915+105. The observations were carried out with the IRAM 30 m-antenna at 250 GHz (1.25 mm) from 1998 March 14 to March 20. These millimetre measurements are complemented with centimetre observations from the Ryle Telescope, at 15 GHz (2.0 cm) and from the Green Bank Interferometer at 2.25 and 8.3 GHz (13 and 3.6 cm). Both Cygnus X-3 and SS 433 underwent moderate flaring events during our observations, whose main spectral evolution properties are described and interpreted. A significant spectral steepening was observed in both sources during the flare decay, that is likely to be caused by adiabatic expansion, inverse Compton and synchrotron losses. Finally, we also report 250 GHz upper limits for three additional undetected X-ray binary stars: LSI+65 010, LSI+61 235 and X Per.

CP2 stars as viewed by the uvby Hbeta system

A new statistical parallax method using the Maximum Likelihood principle is presented, allowing the simultaneous determination of a luminosity calibration, kinematic characteristics and spatial distribution of a given sample. This method has been developed for the exploitation of the Hipparcos data and presents several improvements with respect to the previous ones: the effects of the selection of the sample, the observational errors, the galactic rotation and the interstellar absorption are taken into account as an intrinsic part of the formulation (as opposed to external corrections). Furthermore, the method is able to identify and characterize physically distinct groups in inhomogeneous samples, thus avoiding biases due to unidentified components. Moreover, the implementation used by the authors is based on the extensive use of numerical methods, so avoiding the need for simplification of the equations and thus the bias they could introduce. Several examples of application using simulated samples are presented, to be followed by applications to real samples in forthcoming articles.

Detection of moving groups among early type stars

Our procedure to detect moving groups in the solar neighbourhood (Chen et al., 1997) in the four-dimensional space of the stellar velocity components and age has been improved. The method, which takes advantadge of non-parametric estimators of density distribution to avoid any a priori knowledge of the kinematic properties of these stellar groups, now includes the effect of observational errors on the process to select moving group stars, uses a better estimation of the density distribution of the total sample and field stars, and classifies moving group stars using all the available information. It is applied here to an accurately selected sample of early-type stars with known radial velocities and Strömgren photometry. Astrometric data are taken from the HIPPARCOS catalogue (ESA, 1997), which results in an important decrease in the observational errors with respect to ground-based data, and ensures the uniformity of the observed data. Both the improvement of our method and the use of precise astrometric data have allowed us not only to confirm the existence of classical moving groups, but also to detect finer structures that in several cases can be related to kinematic properties of nearby open clusters or associations.

Secondary UBVRI-CCD standard stars in the neighbourhood of Landolt standard stars

A list of 681 UBVRI secondary standard stars for CCD photometry is presented. Visual magnitude ranges from 9.7 to 19.4, and the B-V colour index varies from 1.15 to 1.97. The stars are grouped into 11 different fields, each of them is generally observable in a single CCD frame. The stars are located near Landolt UBVRI equatorial standards, accessible to telescopes in both hemispheres, and mainly within the 5 - 8 hours range of right ascension. Photometry, equatorial coordinates and finding charts are provided.

UBVRI photoelectric photometry of nearby stars

In order to complete the photometric data of the Gliese (1969) 'Catalog of Nearby Stars', and in addition use these data for the Hipparcos space astrometry mission, program stars have been selected from the catalog and its supplements on the basis of their having an incomplete set of UBVRI photometric data of magnitude lower than 13. The program developed rejects determinations of any magnitude or color index having a residual greater than 2(sigma-prime), where sigma-prime is the standard deviation for the determinations of unit weight.

UBVRI photoelectric photometry of high proper motion stars

UBVRI photoelectric photometry is presented for 269 late spectral type, high proper motion stars belonging to the 'Lowell Proper Motion Survey' and included in the present version of the Hipparcos Input Catalogue. The observations and data reduction are described. The external errors obtained by comparison of the results with those obtained in other studies are presented.

UBVRI photometry of G, K, M Hipparcos stars

UBVRI data are presented for a set of 229 late-type stars, most of them being high proper motion stars. All these data are part of the Input Catalog planned observations for the Hipparcos mission.

UVBY-Beta Photometry for 67 Stars in the Region of Alpha-Persei

UVBY-Beta photometric data are presented for 67 stars in the region of alpha-Persei and their relationship to the cluster is analyzed. These data allowed us to confirm at least 16 new members of the alpha-Persei open cluster.

UBVRI photometry of G, K, M Hipparcos stars. II.

As indicated by Grenon (1989), the data of the present series of reports on the UBVRI photometry of late-type stars in the Hipparcos Input Catalog are to be employed in computations of Hipparcos observing time, as well as in evaluating the observability of faint stars by the satellite. Attention is here given to late type stars in the V = 8-12 range, including distant red giants in the Galactic plane (Hipparcos proposal 189), as well as high proper motion stars included in the G, LTT, LP, and MCC catalogs.

On the binary nature of the γ-ray sources AGL J2241+4454 (= MWC 656) and HESS J0632+057 (= MWC 148)

We present optical spectroscopy of MWC 656 and MWC 148, the proposed optical counterparts of the gamma-ray sources AGL J2241+4454 and HESS J0632+0 57, respectively. The main parameters of the Halpha emission line (EW, FWHM and centroid velocity) in these stars are modulated on the proposed orbital periods of 60.37 and 321 days, respectively. These modulations are likely produced by the resonant interaction of the Be discs with compact stars in eccentric orbits. We also present radial velocity curves of the optical stars folded on the above periods and obtain the first orbital elements of the two gamma-ray sources thus confirming their binary nature. Our orbital solution support eccentricities e~0.4 and 0.83+-0.08 for MWC 656 and MWC 148, respectively. Further, our orbital elements imply that the X-ray outbursts in HESS J0632+057/MWC 148 are delayed ~0.3 orbital phases after periastron passage, similarly to the case of LS I +61 303. In addition, the optical photometric light curve maxima in AGL J2241+4454/MWC 656 occur ~0.25 phases passed periastron, similar to what is seen in LS I +61 303. We also find that the orbital eccentricity is correlated with orbital period for the known gamma-ray binaries. This is explained by the fact that small stellar separations are required for the efficient triggering of VHE radiation. Another correlation between the EW of Halpha and orbital period is also observed, similarly to the case of Be/X-ray binaries. These correlations are useful to provide estimates of the key orbital parameters Porb and e from the Halpha line in future Be gamma-ray binary candidates.