%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 Acker, A., Marcout, J., Ochsenbein, F., Stenholm, B., & Tylenda, R. 1992, Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Garching: ESO) Aller, L. H., Keyes, C. D., Maran, S. P., Gull, T. 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R., Whiteoak, J. B., Hughes, S. M. G., Bessell, M. S., Gardner, F. F., & Hyland, A. R. 1992, \apj mathend000#, 397, 552 Zijlstraa, A. A., Gesicki, K., Walsh, J. R., Péquignot, D., van Hoof, P. A. M., & Minniti, D. 2006, \mnras mathend000#, 369, 875 %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. 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H. 1982, \apj mathend000#, 262, 657 \ibidrule 1995, \apj mathend000#, 451, 352 %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. 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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. %Z 0.92 Alzner, A. 2001, IAUDS, Inf. 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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. 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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. 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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. 331-340 (2010) (http://www.astroscu.unam.mx/~rmaa/) %D 10/2010 %L 340 %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. %Z Abt, H. 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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. 341-348 (2010) (http://www.astroscu.unam.mx/~rmaa/) %D 10/2010 %L 348 %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. 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L., & Perley, R. A. 1990, \apjs mathend000#, 74, 181 %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. 349-353 (2010) (http://www.astroscu.unam.mx/~rmaa/) %D 10/2010 %L 353 %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 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[d]eferred% mathend000#, while at 20we do not detect this emission above a level of 2 endtex2html[d]eferred% 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 Bridle, A. H., & Perley, R. A. 1984, \araa mathend000#, 22, 319 Castets, A., Reipurth, B., & Loinard, L. 2004, A&A, 427, 895 Cohen, M., & Schwartz, R. 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J., Reipurth, B., & Roth, M. 1990, ApJ, 348, L61 %R 2010RMxAA..46..355¸ %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. 355-365 (2010) (http://www.astroscu.unam.mx/~rmaa/) %D 10/2010 %L 365 %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 M[1] = 0.870±0.074 endtex2html[d]eferredM[] mathend000#, M[2] = 0.607±0.053 endtex2html[d]eferredM[] mathend000# and R[1] = 0.983±0.030 endtex2html[d]eferredR[] mathend000#, R[2] = 0.901±0.026 endtex2html[d]eferredR[] 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. 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