205,523 research outputs found

    ARELLANO, Pedro M.

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    Telegram from Mr. Pedro M. Arellano to General Alvaro Obregón, requesting a hearing for the delegation of the City Council of Aguascalientes. Reply setting the date. / Telegrama del Sr. Pedro M. Arellano al Gral. Alvaro Obregón, solicitando audiencia para la delegación del Ayuntamiento de Aguascalientes. Respuesta fijando la fecha

    Retrato del teniente general de la Armada Carlos Antonio de Torres Ramírez de Arellano, marqués de Arellano. Retrato militar

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    Retrato del teniente general de la Real Armada Española y Marqués de Arellano, Carlos Antonio de Torres Ramírez de Arellano. Se desconoce la autoría del retrato.Inscripciones - Transcripción: “D. CARLOS ANTONIO DE TORRES RAMIREZ D ARE/ LLANO ANGVLO Y VI LLAVICENCIA MARO./ DE ARELLANO, TENIEN TE GRAL D LAREAL/ ARMADA, INSPECTOR Y COMANDTE. GRALD/ LOS BATALLONES DE MARINA SIRVE A.S.M./ DESDE XXVI. D NOVI EMBRE D M DCCXLL/ Q EMPEZO DE GVAR- DIAMARINA” . Inscripciones - Localización: Inf

    ABLAGS: RATS procedure to generate Arellano-Bond set of instruments

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    ABLags generates a VECT[SERIES] with the expanded panel data instruments for doing Arellano-Bond instrumental variables estimation. Arellano, M. and S. Bond (1991). "Some Tests of Specification for Panel Data: Monte Carlo Evidence and an Application to Employment Equations." Review of Economic Studies, Vol. 58, 277-297.Arellano-Bond;GMM

    Resulta de don Carlos de Arellano [Manuscrito]

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    Contiene una relación de los papeles contra Carlos de Arellano, en la causa del duque de OsunaFecha tomada del principio del document

    Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry

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    Aims. We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to derive values for the cluster's parameters. Methods. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also derived an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD). Results. Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables, and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]ZW =-2.01 ± 0.04, or [Fe/H]UVES =-2.11 ± 0.06, and a distance of 8.32 ± 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 ± 0.42 kpc (using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 ± 1.0 Gyr for M 30. © 2013 ESO
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