%R 2010RMxAA..46..191R
%A Richer, M. G.; López, J. A.; Díaz-Méndez, E.; Riesgo, H.; Báez, S.-H.; García-Díaz, Ma. T.; Meaburn, J.; Clark, D. M.; Calderón Olvera, R. M.; López Soto, G.; Toledano Rebolo, O.
%F AA(Based on observations obtained at the Observatorio Astronómico Nacional at San Pedro Mártir, Baja California, Mexico.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 191-214 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 214
%T The San Pedro Mártir Planetary Nebula Kinematic
Catalogue: Extragalactic Planetary Nebulae
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_mricher.pdf
%K ISM: kinematics and dynamics, Local Group, planetary nebulae: general, stars: evolution
%B We present kinematic data for 211 bright planetary nebulae in eleven Local Group galaxies: M31 (137 PNe), M32 (13), M33 (33), Fornax (1), Sagittarius (3), NGC 147 (2), NGC 185 (5), NGC 205 (9), NGC 6822 (5), Leo A (1), and Sextans A (1). The data were acquired at the Observatorio Astronómico Nacional in the Sierra de San Pedro Mártir using the 2.1 m telescope and the Manchester Echelle Spectrometer in the light of [O III]$\lambda$ mathend000#5007 at a resolution of 11^-1 mathend000#. A few objects were observed in H$\alpha$ mathend000#. The internal kinematics of bright planetary nebulae do not depend strongly upon the metallicity or age of their progenitor stellar populations, though small systematic differences exist. The nebular kinematics and H$\beta$ mathend000# luminosity require that the nebular shells be accelerated during the early evolution of their central stars. Thus, kinematics provides an additional argument favoring similar stellar progenitors for bright planetary nebulae in all galaxies.
%Z

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%R 2010RMxAA..46..215R
%A Rodríguez, L. F.; Gómez, Y.; Loinard, L.; Mioduszewski, A. J.
%F AA(Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, Mexico.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 215-219 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 219
%T On the Size of the Non-Thermal Component in
the Radio Emission from Cyg OB2 #5
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_lfrodriguez.pdf
%K radio continuum: stars, stars: individual (Cyg OB2 #5)
%B Cyg OB2 #5 is a contact binary system with variable radio continuum emission. This emission has a low-flux state where it is dominated by thermal emission from the ionized stellar wind and a high-flux state where an additional non-thermal component appears. The variations are now known to have a period of 6.7±0.2 mathend000# yr. The non-thermal component has been attributed to different agents: an expanding envelope ejected periodically from the binary, emission from a wind-collision region, or a star with non-thermal emission in an eccentric orbit around the binary. The determination of the angular size of the non-thermal component is crucial to discriminate between these alternatives. We present the analysis of VLA archive observations made at 8.46 GHz in 1994 (low state) and 1996 (high state), that allow us to subtract the effect of the persistent thermal emission and to estimate an angular size of $\leq$ 0to$\z$@.$\hss$''02 mathend000# for the non-thermal component. This compact size favors the explanation in terms of a star with non-thermal emission or of a wind-collision region.
%Z

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%R 2010RMxAA..46..221T
%A Torres-Peimbert, S.; Arrieta, A.; Bautista, M.
%F AA(Based on observations obtained at the Observatorio Astronómico Nacional at San Pedro Mártir, Baja California, Mexico.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 221-243 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 243
%T Echelle spectroscopy of the nuclei of the highly collimated bipolar planetary nebulae M-9 and M-91
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_storres.pdf
%K planetary nebulae: individual (M 2-9, M 1-91)
%B We present echelle spectroscopy of the unresolved nuclei of the bipolar planetary nebulae M-9 and M-91. The spectrum is dominated by emission lines emitted under a wide range of physical conditions. From the observations we identify the emission lines, derive physical conditions and relative motions of the different ionized species in the circumstellar region of both objects. We propose that the observed forbidden lines arise in the inner part of the extended torus that surrounds each object.
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%R 2010RMxAA..46..245O
%A Orlov, V. G.; Voitsekhovich, V. V.; Rivera, J. L.; Guerrero, C. A.; Ortiz, F.
%F AA(Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 245-251 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 251
%T Speckle Interferometry at the Observatorio
Astronómico Nacional. II
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_vorlov.pdf
%K binaries: visual, stars: fundamental parameters, techniques: high angular resolution, techniques: interferometric
%B We present speckle interferometric measurements of binary stars made during June of 2009 with the 1.5telescope of the Observatorio Astronómico Nacional at SPM (Mexico). The data contain 189 position angle and separation measures of 144 systems. The measured angular separations range from 0$\arcsec.16$ mathend000# to 3$\arcsec.64$ mathend000#. The maximum magnitude of the brighter component is 10.96. The mean error in separation is 0$\arcsec.02$ mathend000# and in the position angles $1.5°$ mathend000#. Some of the position angles were determined with the usual $180°$ mathend000# ambiguity.
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%R 2010RMxAA..46..253N
%A Neria, C.; Gómez, Y.; Rodríguez, L. F.
%F AA(Centro de Radioastronomía y Astrofísica
Universidad Nacional Autónoma de México, Morelia, Mexico)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 253-262 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 262
%T Compact radio sources in the vicinity of the ultracompact HII region G78.4+2.6
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_cneria.pdf
%K HII regions, ISM: individual (G78.4+2.6, IRAS0178+4046), radio continuum: stars
%B Using the Very Large Array (VLA) at 3.6we identify four new compact radio sources in the vicinity of the cometary HII region G78.4+2.6 (VLA). The four compact radio sources (named VLA to VLA), have near-infrared counterparts, as seen in the 3.6SPAN CLASS="MATH">$\mu$ mathend000#m Spitzer image. One of them (VLA) clearly shows evidence of radio variability in a timescale of hours. We explore the possibility that these radio sources are associated with pre-main sequence (PMS) stars in the vicinity of the UC HII region G78.4+2.6. Our results favor the smaller distance value of 1.7 kpc for G78.4+2.6. In addition to the detection of the radio sources in the vicinity of G78.4+2.6, we detected another group of five sources which appear located about 3' mathend000# to the northwest of the HII region. Some of them exhibit extended emission.
%Z

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%R 2010RMxAA..46..263R
%A Rica Romero, F. M.
%F AA(Agrupación Astronómica de Mérida, Spain.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 263-277 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 277
%T Orbital elements for eight binaries.
Study of the nature of wide components. I
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_frica.pdf
%K binaries: general, binaries: visual, instrumentation: high angular resolution, techniques: high angular resolution
%B New orbital parameters and masses for eight binaries were determined. Most of these were noted as being in need of correction due to large residuals to the previous best orbit. A modified Thiele-van den Bos method was used to obtain initial orbits which were improved using the differential correction method of Heintz. The Thiele-van den Bos method was modified so that an approximate value of the areal constant allowed good results to be obtained. The nature of wide components was studied using BVIJHK mathend000# photometry, historical astrometry and kinematical data. A search for new unreported companions around the binaries was carried out.
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%R 2010RMxAA..46..279M
%A Maryeva, O.; Abolmasov, P.
%F AA(Stavropol State University, Russia.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 279-290 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 290
%T Spectral Variability of Romano's Star
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_omaryeva.pdf
%K galaxies: individual (M33), stars: individual (Romano's star), stars: Wolf-Rayet, supergiants
%B We combine archival spectral observations of the LBV star V532 (Romano's star) together with existing photometric data in the B mathend000# band. Spectroscopic data cover 15 years of observations (from 1992 to 2007). We show that the object in maximum of brightness behaves as an emission line supergiant while in minimum V532 moves along the sequence of late WN stars. In this sense, the object behaves similarly to the well-known Luminous Blue Variable (LBV) stars AG Car and R127, but is somewhat hotter at the minima. We identify about 100 spectral lines in the 3700 - 7300 mathend000#
r Arange. As of today, our spectroscopy is the most comprehensive for this object. The velocity of the wind is derived using the Hetriplet lines (360±30 mathend000#^-1 mathend000#). Physical parameters of the nebula around V532 are estimated.
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%R 2010RMxAA..46..291P
%A Peña, J. H.; Arellano Ferro, A.; Peña-Miller, R.; Álvarez, M.; Rosas, Y.; García, H.; Muñoz, G.; Vargas, B.; Sareyan, J. P.; Guerrero, C. A.; Rentería, A.
%F AA(Based on observations collected at the San Pedro Mártir Observatory, Mexico.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 291-308 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 308
%T uvby - $\beta$ mathend000# photoelectric photometry of Cepheid stars
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_jpena-online.pdf
%K stars: variables: Cepheids, techniques: photometric
%B We present time-series uvby - $\beta$ mathend000# photometry of 41 classical Cepheid stars. A brief discussion of a comparison between the present data and previous photometric observations is included.
%Z

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%R 2010RMxAA..46..309B
%A Bernal, C. G.; Lee, W. H.; Page, D.
%F AA(Instituto de Astronomía
Universidad Nacional Autónoma de México, Mexico)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 309-322 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 322
%T Hypercritical accretion onto a magnetized
neutron star surface: a numerical approach
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_cgbernal-online.pdf
%K accretion, accretion disks, hydrodynamics, magnetic fields, stars: neutron, supernovae: individual (SN1987A)
%B The properties of a new-born neutron star, produced in a core-collapse supernova, can be strongly affected by the possible late fallback which occurs several hours after the explosion. This accretion occurs in the regime dominated by neutrino cooling, explored initially in this context by Chevalier:1989jk. Here we revisit this approach in a 1D spherically symmetric model and carry out numerical simulations in 2D in an accretion column onto a neutron star, considering detailed microphysics, neutrino cooling and the presence of magnetic fields in ideal MHD. We compare our numerical results with the analytic solutions and explore how the purely hydrodynamical as well as the MHD solutions differ from them, and begin to explore how this may affect the appearance of the remnant as a typical radio pulsar.
%Z

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%R 2010RMxAA..46..323M
%A Molina, A.
%F AA(Departamento de Física Aplicada, Facultad de Ciencias, Universidad de Granada, Granada, Spain.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 323-330 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 330
%T The importance of nucleus rotation in determining
the largest grains ejected from comets
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_amolina.pdf
%K comets: general, comets: individual (Halley, Wirtanen, Hyakutake, C/2001 A2 LINEAR, IRAS-Araki-Alcock, Churyumov-Gerasimenko), interplanetary medium, meteoroids
%B The maximum diameter of large boulders ejected from the cometary nuclei is investigated using the classical model of dust grain as dragged out by radially expanding cometary gases. The importance of the inertial forces, and particularly those due to the rotation of the comet is shown. Although a larger dust grain can be lifted from the nucleus surface if the rotation is faster, the rotation period has to be larger than a certain value. A simple expression for this critical value of rotation period is given. Our results are applied to different comets and a comparison with the maximum radius values obtained by radar measurements is made. Finally, comet Churyumov-Gerasimenko, the target of the ROSETTA mission to arrive on 2014, is going to be analyzed and a range for the maximum diameter of the dust grains that can be lifted is proposed.
%Z

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%R 2010RMxAA..46..331A
%A Arellano Ferro, A.
%F AA(Instituto de Astronomía
Universidad Nacional Autónoma de México, Mexico)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 331-338 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 338
%T Functional relationships for T_eff mathend000# and logtex2html_verbatim_mark>#math15#g mathend000# in
F-G supergiants from uvby - $\beta$ mathend000# photometry
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_aarellano.pdf
%K stars: AGB and post-AGB, supergiants, techniques: photometric
%B From photoelectric uvby - $\beta$ mathend000# data and recent accurate synthetic and spectroscopic values of T_eff mathend000# and logSPAN CLASS="MATH">g mathend000# for 50 F-G supergiants, we have calculated functional relationships that lead to initial estimates of effective temperature and gravities for these types of stars. It is shown that while the T_eff mathend000# relationships are calculated using the data on young massive supergiants, they are also valid for evolved stars of similar temperatures like post-AGB and RV Tau stars. The gravity can also be predicted from the $\Delta$[c₁] mathend000# index with an uncertainty of about 0.26 dex. Although a clear and significant trend between M_V mathend000# and $\Delta$[c₁] mathend000# is seen, no calibration is found that predicts accurate values of M_V mathend000#.
%Z

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%R 2010RMxAA..46..339M
%A Maza, N. L.; Levato, H.; López-García, Z.
%F AA(Instituto de Ciencias Astronómicas, de la Tierra y del Espacio, San Juan, Argentina.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 339-348 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 348
%T Atomic species in the spectrum of the Hg-Mn star HD 53244
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_nmaza.pdf
%K stars: chemically peculiar, stars: line identification, stars: individual (HD 53244)
%B Line identifications are presented for the Hg-Mn Bp star HD 53244 ($\gamma$ mathend000#CMa), in the spectral region $\lambda$$\lambda$3750 - 6700 mathend000#
r A. This object is a member of the southern open cluster Cr 121. Comparison of the spectrum of HD 53244 with other field Hg-Mn stars shows that it shares many of their spectral anomalies but that also some differences exist.
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%R 2010RMxAA..46..349T
%A Trejo, A.; Rodríguez, L. F.
%F AA(Centro de Radioastronomía y Astrofísica
Universidad Nacional Autónoma de México, Morelia, Michoacán, Mexico)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 349-356 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 356
%T Compact Radio Sources Apparently Associated
with Extended Galactic Sources
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_atrejo.pdf
%K ISM: individual (SNR G3.8+0.3), ISM: supernova remnants, planetary nebulae: individual (PHR 1735-333), radio lines: ISM
%B We report VLA radio observations of the 21 cm HI line toward two compact radio sources that could be associated with extended Galactic sources. In the case of the planetary nebula PHR 1735-333 we observed HI absorption against a non-thermal radio source recently discovered in the region, which was proposed to be physically associated with the planetary nebula. However, from the analysis of the HI absorption spectrum, we suggest a larger distance for this non-thermal source. In the case of the supernova remnant candidate SNR G3.8+0.3 we obtained HI absorption spectra towards it and towards a compact radio source located at its center. We conclude that SNR G3.8+0.3 is more distant than the compact radio source and that they are not physically associated.
%Z

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%R 2010RMxAA..46..357T
%A Trejo, A.; Rodríguez, L. F.
%F AA(Centro de Radioastronomía y Astrofísica
Universidad Nacional Autónoma de México, Morelia, Michoacán, Mexico)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 357-361 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 361
%T On the Nature of the Non-Thermal Radio Source
at the Center of the Orion Streamers
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_atrejo2.pdf
%K ISM: individual (Orion Streamers, HH 222), radiation mechanisms: non-thermal, radio continuum: ISM
%B We present VLA continuum observations at 20 and 6toward a non-thermal radio source located at the Streamers region in Orion. We compare 1991 archive observations with new ones taken by us in 2008. The radio source could be a young stellar source or an evolved object like a microquasar or even a jet from a radio galaxy. Our analysis shows that there is no evidence of changes in the flux densities between both epochs at a level higher than 10%. Also, we set an upper limit at a 3$\sigma$ mathend000# level of 23^-1 mathend000# for the proper motions. At the distance of Orion this implies an upper limit to the velocity in the plane of the sky of 45^-1 mathend000#. At 6, we detect linearly polarized emission at a level of 5
endtex2html_deferred% mathend000#, while at 20we do not detect this emission above a level of 2
endtex2html_deferred% mathend000#. We conclude that the non-thermal radio source most probably is a radio galaxy aligned by chance with the line of sight to the Streamers in Orion.
%Z

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%R 2010RMxAA..46..363¸
%A Çakirli, Ö; Ibanoglu, C.; Dervisoglu, A.
%F AA(Based on spectroscopic observations collected at TÜBITAK National Observatory, Turkey.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 363-373 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 373
%T The Absolute Parameters for NSVS 11868841 and the Oversized Stars in Low-Mass Eclipsing Binaries
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_ocakirli.pdf
%K binaries: eclipsing, stars: activity, stars: fundamental parameters, stars: low-mass
%B Spectroscopic observations of the low-mass eclipsing binary NSVS 11868841 have been obtained and the radial velocities were derived for both components. The masses and radii determined for the components are M₁ = 0.870±0.074
endtex2html_deferredM mathend000#, M₂ = 0.607±0.053
endtex2html_deferredM mathend000# and R₁ = 0.983±0.030
endtex2html_deferredR mathend000#, R₂ = 0.901±0.026
endtex2html_deferredR mathend000#. Both the primary and secondary stars' radii are 10% and 57% larger than those of zero-age-main-sequence stars with the same masses. This discrepancy may arise from the large spot coverage of both stars. We collected absolute parameters of 21 low mass double-lined eclipsing binaries and compared their positions in the mass-radius and mass-effective temperature panels. The large radii and lower effective temperatures found for NSV 11868841 are solved neither with differences in metallicity nor in mixing length parameters. These discrepancies for low mass stars may be due to magnetic fields inhibiting the convective energy transport, which lead to a large magnetic spot coverage of the surface of such low mass stars.
%Z

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%R 2010RMxAA..46..375L
%A Loinard, L.; Rodríguez, L. F.; Gómez, L.; Cantó, J.; Raga, A. C.; Goodman, A. A.; Arce, H. G.
%F AA(Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Mexico.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 375-383 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 383
%T A reassessment of the kinematics of PV Cephei based
on accurate proper motion measurements
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_lloinard.pdf
%K astrometry, ISM: individual (PV Cep), ISM: jets and outflows, stars: pre-main sequence
%B We present two Very Large Array observations of the pre-main-sequence star PV Cephei, taken with a separation of 10.5. These data show that the proper motions of this star are cos = + 10.9±3.0 mathend000#^-1 mathend000#; = + 0.2±1.8 mathend000#^-1 mathend000#, very similar to those -previously known- of HD 200775, the B2Ve star that dominates the illumination of the nearby reflection nebula NGC023. This result suggests that PV Cephei is not a rapidly moving runaway star as suggested by previous studies. The large velocity of PV Cephei had been inferred from the systematic eastward displacement of the bisectors of successive pairs of Herbig Haro knots along its flow. These systematic shifts might instead result from an intrinsic asymmetry in the ejection mechanisms, or in the distribution of the circumstellar material.
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%R 2010RMxAA..46..385A
%A Akkaya, I.; Schuster, W. J.; Michel, R.; Chavarría-K, C.; Moitinho, A.; Vázquez, R.; Karatas, Y.
%F AA(Based on observations carried out at the San Pedro Mártir National Astronomical Observatory (SPM), operated by Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, B. C., Mexico.)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 385-430 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 430
%T CCD U - BV - RI mathend000# Photometry of the Galactic open
clusters: Be9, Ru35, and Be0
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_iakkaya-online.pdf
%K open clusters and associations: individual (Be10, Be89, Ru135), stars: fundamental parameters, stars: Hertzsprung-Russell and C-M diagrams, techniques: photometric
%B The fundamental parameters of reddening, metallicity, age, and distance are presented for the poorly studied open clusters Be9, Ru35, and Be0, derived from their CCD U - BV - RI mathend000# photometry. The interstellar reddenings, E(B mathend000#-V) mathend000#, were measured in the two-color diagram, and the photometric metallicities, [Fe/H], from the ultraviolet excesses of the F-type stars. By fitting isochrones to the observed sequences of the clusters in five different color-magnitude diagrams, the weighted averages of distance moduli and heliocentric distances [(V₀ mathend000#-M_V), d mathend000#(kpc)] are (11^m.90±0^m.06, 2.4±0.06 mathend000#) for Be9, (9^m.58±0^m.07, 0.81±0.03 mathend000#) for Ru35, and (11^m.16±0^m.06, 1.7±0.05 mathend000#) for Be0, and the weighted averages of the ages [ log(A), A mathend000#(Gyr)] are (9.58±0.06, 3.8±0.6) mathend000# for Be9, (9.58±0.06, 3.8±0.7) mathend000# for Ru35, and (9.06±0.05, 1.08±0.08) mathend000# for Be0.
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%R 2010RMxAA..46..431C
%A Cardona, O.; Cornejo+Rodríguez, A.; García-Flores, P. C.
%F AA(Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla, Mexico)
%J Revista Mexicana de Astronomía y Astrofísica Vol. 46, pp. 431-438 (2010) (http://www.astroscu.unam.mx/~rmaa/)
%D 10/2010
%L 438
%T Star Image Shape Transformer for Astronomical
Slit Spectroscopy
%C (C) 2010; Instituto de Astronomía, Universidad Nacional Autónoma de México
%U http://www.astrosmo.unam.mx/rmaa/RMxAA..46-2/PDF/RMxAA..46-2_ocardona.pdf
%K instrumentation: miscellaneous, stars: imaging, techniques: imaging spectroscopy, techniques: spectroscopic
%B We present a new star image shape transformer for astronomical slit spectroscopy that consists of a plano-convex lens attached to a plane-parallel rectangular glass plate on one of the small sides, with the aim of improving the performance of spectrometric systems. The system transforms the shape of the objects into a rectangular form with the purpose of filling with light the entrance slit aperture in spectroscopic systems. The plate is set sidewise with the lens as the entrance aperture and the exit aperture of the plate is the illuminated slit seen by the spectrometric system. The aim of this transformer is also to maintain the beam characteristics, the intrinsic resolution of the spectrometers and to improve the throughput of the spectrometer and detector systems.
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