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Short-term spectroscopic monitoring of two cool dwarfs with strong magnetic fields
Context: There is now growing evidence that some brown dwarfs (BDs) havevery strong magnetic fields, and yet their surface temperatures are solow that the coupling is expected to be small between the matter and themagnetic field in the atmosphere. In the deeper layers, however, thecoupling is expected to be much stronger. Aims: This raises thequestion of whether the magnetic field still leads to the formation ofstructures in the photosphere and of a solar-like chromosphere andcorona. Methods: We carried out a spectroscopic monitoring campaign inwhich we observed ultracool dwarfs that have strong magnetic fields: theBD LP944-20 and 2MASSW J0036159+182110. The objects were monitored overseveral rotation periods spectroscopically. LP944-20 was observedsimultaneously in the optical and in the near infrared regime, 2MASSWJ0036159+182110 only in the infrared. From the spectra, we determinedthe temperature of the objects in each spectrum, and measured theequivalent width in a number of diagnostically important lines.Temperature variations would indicate the presence of warm and coldregions, variations in the equivalent widths of photospheric lines aresensitive to the structure of cloud layers, and Hα is a diagnosticfor chromospheric structures. Results: Both dwarfs turned out to beremarkably constant. In the case of LP944-20, the T_eff-variations are≤50 K, and the rms-variations in the equivalent widths of Hαsmall. We also find that the equivalent widths of photospheric lines areremarkably constant. We did not find any significant variations in thecase of 2MASSW J0036159+182110 either. Thus the most important result isthat no significant variability was found at the time of ourobservations. We find that Hα-line is in emission but theequivalent width is only -4.4±0.3 Å. When comparing ourspectra with spectra taken over the past 11 years, we recognizesignificant changes during this time. Conclusions: We interpret theseresults as evidence that the photosphere of these objects are remarkablyhomogeneous, with only little structure in them, and despite the strongmagnetic fields. Thus, unlike active stars, there are no prominent spotson these objects.Partly based on observations obtained at the European SouthernObservatory at La Silla, Chile in programs 078.C-0161(A) and078.C-0161(B), and partly based on observations collected at the CentroAstronómico Hispano Alemán /CAHA) at Calar Alto, operatedjointly by the Max-Planck-Institut für Astronomie and the theInsituto de Astrofísica de Andalucía (CSIC).
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| 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
| The Montreal-Cambridge-Tololo Survey of Southern Subluminous Blue Stars: The South Galactic Cap
Results for the south Galactic cap region of theMontréal-Cambridge-Tololo survey of blue subluminous stars arepresented. This region overlaps the 840 deg2 region studiedalmost three decades ago by Slettebak & Brundage. We present a list ofequatorial coordinates, photographic photometry, and spectroscopicidentifications, as well as finding charts, for 188 blue objects[(U-B)pg<=-0.6] brighter than Bpg=16.5 in thisarea. Completeness of the survey and comparisons with other similarefforts are discussed.
| Classification of Population II Stars in the Vilnius Photometric System. II. Results
The results of photometric classification of 848 true and suspectedPopulation II stars, some of which were found to belong to Population I,are presented. The stars were classified using a new calibrationdescribed in Paper I (Bartkevicius & Lazauskaite 1996). We combinethese results with our results from Paper I and discuss in greaterdetail the following groups of stars: UU Herculis-type stars and otherhigh-galactic-latitude supergiants, field red horizontal-branch stars,metal-deficient visual binaries, metal-deficient subgiants, stars fromthe Catalogue of Metal-deficient F--M Stars Classified Photometrically(MDPH; Bartkevicius 1993) and stars from one of the HIPPARCOS programs(Bartkevicius 1994a). It is confirmed that high galactic latitudesupergiants from the Bartaya (1979) catalog are giants or even dwarfs.Some stars, identified by Rose (1985) and Tautvaisiene (1996a) as fieldRHB stars, appear to be ordinary giants according to our classification.Some of the visual binaries studied can be considered as physical pairs.Quite a large fraction of stars from the MDPH catalog are found to havesolar metallicity. A number of new possible UU Herculis-type stars, RHBstars and metal-deficient subgiants are identified.
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| The Southern Vilnius Photometric System. III. Observations of E and F Harvard Standard Regions, 47 TUC and Some Metal-Deficient Stars
The results of photoelectric photometry in the Vilnius system of 101southern stars in the areas E1--E4, E8, E9 and F1 as well as of somemetal deficient stars are presented. Photometrically determined spectraltypes and luminosity classes of these stars are also given.
| The galactic reddening law - The evidence from uvby-beta photometry of B stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1985A&A...142..189T&db_key=AST
| Four-colour photometry of B stars north of B = + 45 deg and comparison with the south
Four-color photometry of 33 Henry Draper B stars north of b = + 45 degis presented. Most are little-reddened B or intermediate-A stars. A newAm star is discovered. The new measures essentially complete uvbyphotometry of all HD B stars within 45 deg of either galactic pole. Thenorthern and southern cones of HD B stars are compared, and selectioneffects deduced. Far from the galactic plane, it appears that B starsmay be equally distributed north and south of the plane; closer to thesun, an asymmetry associated with Gould's Belt is evident.
| H-beta photometry of southern early-type stars
H-beta photoelectric photometry is presented for 209 southern hemisphereearly-type stars from the HD catalog with galactic latitudes /b/ greaterthan 6 deg. Four-color photometry exists for all these stars and MKtypes for most of them. Absolute magnitudes have been estimated for allbut the emission-line stars and distances from the sun and the galacticplane determined.
| Four colour photometry of southern early-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978MNRAS.182..629K&db_key=AST
| Spectroscopically peculiar stars near the south galactic pole.
Abstract image available at:http://adsabs.harvard.edu/abs/1973AJ.....78..295G
| Radial Velocities and Spectral Classification of A-Type Stars Near the South Galactic Pole
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971PASP...83..643B&db_key=AST
| A finding list of early-type stars near the south galactic pole.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971AJ.....76..338S&db_key=AST
| Stellar-Population Samples at the Galactic Poles. II. UBVRI Photometry of M Stars Near the South Pole
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJS...22..289E&db_key=AST
| Line strengths for southern OB stars-II. Observations with moderate dispersion
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969MNRAS.144...31B&db_key=AST
| Three-colour photometry of early-type stars near the galactic poles
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1963MNRAS.127...83W&db_key=AST
| Radial velocities of bright southern stars, III
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1963MNRAS.126...29B&db_key=AST
| Faint blue stars in the region near the South Galactic Pole.
Not Available
| The Radial Velocities of Faint Class B Stars in the Declination Zone 0° to -23°.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1943ApJ....97..300N&db_key=AST
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Observation and Astrometry data
| Constellation: | Cetus |
| Right ascension: | 00h13m55.60s |
| Declination: | -17°32'43.3" |
| Apparent magnitude: | 7.35 |
| Distance: | 308.642 parsecs |
| Proper motion RA: | 15.4 |
| Proper motion Dec: | 5 |
| B-T magnitude: | 7.162 |
| V-T magnitude: | 7.335 |
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