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3D mapping of the dense interstellar gas around the Local Bubble
We present intermediate results from a long-term program of mapping theneutral absorption characteristics of the local interstellar medium,motivated by the availability of accurate and consistent parallaxes fromthe Hipparcos satellite. Equivalent widths of the interstellar NaID-line doublet at 5890 Å are presented for the lines-of-sighttowards some 311 new target stars lying within ~ 350 pc of the Sun.Using these data, together with NaI absorption measurements towards afurther ~ 240 nearby targets published in the literature (for many ofthem, in the directions of molecular clouds), and the ~ 450lines-of-sight already presented by (Sfeir et al. \cite{sfeir99}), weshow 3D absorption maps of the local distribution of neutral gas towards1005 sight-lines with Hipparcos distances as viewed from a variety ofdifferent galactic projections.The data are synthesized by means of two complementary methods, (i) bymapping of iso-equivalent width contours, and (ii) by densitydistribution calculation from the inversion of column-densities, amethod devised by Vergely et al. (\cite{vergely01}). Our present dataconfirms the view that the local cavity is deficient in cold and neutralinterstellar gas. The closest dense and cold gas ``wall'', in the firstquadrant, is at ~ 55-60 pc. There are a few isolated clouds at closerdistance, if the detected absorption is not produced by circumstellarmaterial.The maps reveal narrow or wide ``interstellar tunnels'' which connectthe Local Bubble to surrounding cavities, as predicted by the model ofCox & Smith (1974). In particular, one of these tunnels, defined bystars at 300 to 600 pc from the Sun showing negligible sodiumabsorption, connects the well known CMa void (Gry et al. \cite{gry85}),which is part of the Local Bubble, with the supershell GSH 238+00+09(Heiles \cite{heiles98}). High latitude lines-of-sight with the smallestabsorption are found in two ``chimneys'', whose directions areperpendicular to the Gould belt plane. The maps show that the LocalBubble is ``squeezed'' by surrounding shells in a complicated patternand suggest that its pressure is smaller than in those expandingregions.We discuss the locations of several HI and molecular clouds. Usingcomparisons between NaI and HI or CO velocities, in some cases we areable to improve the constraints on their distances. According to thevelocity criteria, MBM 33-37, MBM 16-18, UT 3-7, and MBM 54-55 arecloser than ~ 100 pc, and MBM 40 is closer than 80 pc. Dense HI cloudsare seen at less than 90 pc and 85 pc in the directions of the MBM 12and MBM 41-43 clouds respectively, but the molecular clouds themselvesmay be far beyond. The above closest molecular clouds are located at theneutral boundary of the Bubble. Only one translucent cloud, G192-67, isclearly embedded within the LB and well isolated.These maps of the distribution of local neutral interstellar NaI gas arealso briefly compared with the distribution of both interstellar dustand neutral HI gas within 300 pc.Tables 1 and 2 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp:cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/411/447
| Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS
Radial velocities have been determined for a sample of 2930 B2-F5 stars,95% observed by the Hipparcos satellite in the north hemisphere and 80%without reliable radial velocity up to now. Observations were obtainedat the Observatoire de Haute Provence with a dispersion of 80Ä,mm(-1) with the aim of studying stellar and galactic dynamics.Radial velocities have been measured by correlation with templates ofthe same spectral class. The mean obtained precision is 3.0 km s(-1)with three observations. A new MK spectral classification is estimatedfor all stars. Based on observations made at the Haute ProvenceObservatory, France and on data from The Hipparcos Catalogue, ESA.Tables 4, 5 and 6 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr or viahttp://cdsweb.u-strasbg.fr/Abstract.htm
| Scattering and absorption in soft X-ray selected AGN: an optical polarization survey
We have surveyed the optical linear polarization of a completelyidentified sample of 43 bright soft-X-ray-selected ROSAT AGN. Most (40)of these AGN show low polarization (~1%), and no clear opticalreddening. This supports the suggestion from rapid X-ray variability,disk-like spectral energy distributions, and lack of cold X-rayabsorption, that we are viewing a bare AGN disk. IRASF12397+3333 andIRAS13349+2438 show high polarization increasing to the UV - clearevidence for scattering. As well as steep, soft-X-ray spectra, they showoptical reddening and rapid X-ray variability, but almost no cold X-rayabsorption - a combination that suggests dusty ionized gas along theline-of-sight. Brandt et al. suggested and found these `warm absorbers'for IRAS13349+2438. IRASF12397+3333 is a new candidate. Combining ourdata with the optical and X-ray spectra of the high polarizationnarrow-line Seyfert 1 nuclei (NLSy1s) investigated by Goodrich revealsstrong correlations among optical reddening indicators (alpha_opt andHα /Hβ ), [OIII]/Hβ_b , and cold intrinsic X-rayabsorption Delta N_H. Optical reddening underpredicts the cold X-rayabsorption, suggesting dusty warm absorbers in all the highly polarizedAGN. The existence of these scattering-polarized and reddened NLSy1ssuggests an orientation Unified Scheme within the class of NLSy1s,analogous to that linking Seyfert 1 and Seyfert 2 nuclei. For somehighly polarized and optically selected AGN we present new analysis ofarchival X-ray data, and for the highly polarized AGN new opticalspectroscopy is presented in an appendix.
| Radial velocity measurements. I - Ground-based observations of the program stars for the HIPPARCOS satellite
The radial velocities of 272 stars brighter than m(pg) = 8.5 aredetermined by digital microphotometric measurement of plates obtainedwith dispersion 80 A/mm using the Marly slit spectrograph on the 120-cmtelescope of the Observatoire de Haute Provence. The objects wereselected as probable members of the input catalog for the ESA Hipparcosastrometric satellite. The measurement techniques and data-reductionprocedures are described in detail, and the results are presented inextensive tables and graphs and briefly characterized.
| Positions moyennes et mouvements propres de 355 etoiles DU GC de la zone de declinaison +33 +36.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976A&AS...26..219M&db_key=AST
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Datos observacionales y astrométricos
| Constelación: | León Menor |
| Ascensión Recta: | 10h16m09.36s |
| Declinación: | +35°09'52.1" |
| Magnitud Aparente: | 7.343 |
| Distancia: | 186.916 parsecs |
| Movimiento Propio en Ascensión Recta: | -28.3 |
| Movimiento Propio en Declinación: | -16.4 |
| B-T magnitude: | 7.554 |
| V-T magnitude: | 7.361 |
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