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High Ionization Species in the Nearby Interstellar Medium from an Exhaustive Analysis of the IUE INES Database
Main-sequence (MS) and giant late-B and early-A type stars are the besttargets for searching for nearby interstellar (IS) Si IV and C IVresonance lines because they are not able to produce them, either inatmospheric layers or in their circumstellar environment, and becausemany stars of these spectral types are nearby and located in the localinterstellar medium (LISM). In addition, the use of certain stars hotterthan B6 can lead to misinterpretations (e.g., alpha Arae). This workanalyzes the reliable Short-Wavelength Prime high-resolution UV spectraof 558 B6-A9 type stars observed by the International UltravioletExplorer at distances lower than 400 pc from the Sun. For the firsttime, this work utilizes the entire INES database to extract stellar andIS information in a systematic way from homogeneous data. Stars wereclassified into seven groups: normal (MS and subgiant), giant, peculiar,emission line, Algols, pre-main sequence or Herbig Ae/Be, and shellstars. Only 10 normal stars, located beyond 90 pc, show weak Si IV and CIV absorptions and are clustered around the direction of Sco-Cen, while85 located closer than 90 pc, as well as another 89 beyond 90 pc, do notshow any absorptions at all. We conclude that these highly ionizedspecies originate most probably in the LISM, at 90 pc from the Sun,corresponding to the warm interaction zone (IZ), where the expandingLoop I super-shell and the Local Bubble collide. We base our results ona robust statistical analysis of both spectral types and spatialdistributions of the different stellar groups we defined. Our estimatedcolumn densities N of both ions are similar to those obtained by otherauthors for distant stars, suggesting that these absorptions concentratefundamentally in the IZ. A logarithmic correlation between N and thedistance D confirms these results.
| The star catalogue of Hevelius. Machine-readable version and comparison with the modern Hipparcos Catalogue
The catalogue by Johannes Hevelius with the positions and magnitudes of1564 entries was published by his wife Elisabeth Koopman in 1690. Weprovide a machine-readable version of the catalogue, and briefly discussits accuracy on the basis of comparison with data from the modernHipparcos Catalogue. We compare our results with an earlier analysis byRybka (1984), finding good overall agreement. The magnitudes given byHevelius correlate well with modern values. The accuracy of his positionmeasurements is similar to that of Brahe, with ? = 2´ forlongitudes and latitudes, but with more errors >5´ thanexpected for a Gaussian distribution. The position accuracy decreasesslowly with magnitude. The fraction of stars with position errors largerthan a degree is 1.5%, rather smaller than the fraction of 5% in thestar catalogue of Brahe.Star catalogue of Hevelius is only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A29
| Three editions of the star catalogue of Tycho Brahe. Machine-readable versions and comparison with the modern Hipparcos Catalogue
Tycho Brahe completed his catalogue with the positions and magnitudes of1004 fixed stars in 1598. This catalogue circulated in manuscript form.Brahe edited a shorter version with 777 stars, printed in 1602, andKepler edited the full catalogue of 1004 stars, printed in 1627. Weprovide machine-readable versions of the three versions of thecatalogue, describe the differences between them and briefly discusstheir accuracy on the basis of comparison with modern data from theHipparcos Catalogue. We also compare our results with earlier analysesby Dreyer (1916, Tychonis Brahe Dani Scripta Astronomica, Vol. II) andRawlins (1993, DIO, 3, 1), finding good overall agreement. Themagnitudes given by Brahe correlate well with modern values, hislongitudes and latitudes have error distributions with widths of2´, with excess numbers of stars with larger errors (as comparedto Gaussian distributions), in particular for the faintest stars. Errorsin positions larger than ?10´, which comprise about 15% ofthe entries, are likely due to computing or copying errors.The full tables KeplerE and Variants (see Table 4) and the table withthe latin descriptions of the stars are available in electronic formonly at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A28
| Speckle Interferometry at the US Naval Observatory. XIII.
The results of 1424 speckle interferometric observations of doublestars, made with the 26 inch (66 cm) refractor of the US NavalObservatory, are presented. Each speckle interferometric observation ofa system represents a combination of over 2000 short-exposure images.These observations are averaged into 1053 mean relative positions andrange in separation from 0.36″ to 61.92″, with a medianseparation of 10.31″. This is the 13th in a series of paperspresenting measurements obtained with this system and covers the period2006 January 12-December 29. Included in these data are nine oldermeasurements whose positions were previously deemed possibly aberrantbut are no longer classified this way following a confirmingobservation. This paper also includes the first data obtained using anew "secondary" camera, designed and built at USNO.
| Speckle observations with PISCO in Merate - III. Astrometric measurements of visual binaries in 2005 and scale calibration with a grating mask
We present relative astrometric measurements of visual binaries madeduring the first semester of 2005, with the Pupil Interferometry SpeckleCamera and Coronagraph (PISCO) at the 102-cm Zeiss telescope of theBrera Astronomical Observatory, in Merate. We performed 214 newobservations of 192 objects, with angular separations in the range0.2-4.3arcsec, and with an average accuracy of 0.01arcsec. Most of theposition angles could be determined without the usual 180°ambiguity, and their mean error is . Our sample contains orbital couplesas well as binaries whose motion is still uncertain. The purpose of thislong-term programme is to improve the accuracy of the orbits andconstrain the masses of the components.For the first time with PISCO, the astrometric calibration was made witha grating mask mounted at the entrance of the telescope. The advantageof this procedure is to provide a reliable and fully independent scaledetermination.We have found two possible new triple systems: ADS 7871 and KUI 15. Wepropose a preliminary orbit for ADS 4208.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| A Spectroscopic and Photometric Survey of Stars in the Field of L1457: A New Distance Determination
We present a spectroscopic and photometric survey of a sample of fieldstars in the region of the molecular cloud L1457. High-qualitycoudé feed spectra, together with five-band photometry in theSloan Digital Sky Survey system and near-infrared archival data from theTwo Micron All Sky Survey, are used to derive color excesses anddistances for the stars. Based on these data, a new distance estimate of360+/-30 pc is derived for the cloud, supporting recent results by K. L.Luhman. The data further indicate that the north-south velocity gradientseen in the millimeter-wave CO data is mirrored in a distance gradient,with the northern part of the cloud being closer to us. A second, lessopaque, layer of extinction is detected at ~80 pc. This distance isconsistent with the earlier distance estimates to the cloud, based on NaI absorption. We identify this layer with the wall of the hot LocalBubble. Hence, the dense cloud is not, as previously thought, associatedwith the Local Bubble.
| Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i
This work is the second part of the set of measurements of v sin i forA-type stars, begun by Royer et al. (\cite{Ror_02a}). Spectra of 249 B8to F2-type stars brighter than V=7 have been collected at Observatoirede Haute-Provence (OHP). Fourier transforms of several line profiles inthe range 4200-4600 Å are used to derive v sin i from thefrequency of the first zero. Statistical analysis of the sampleindicates that measurement error mainly depends on v sin i and thisrelative error of the rotational velocity is found to be about 5% onaverage. The systematic shift with respect to standard values fromSlettebak et al. (\cite{Slk_75}), previously found in the first paper,is here confirmed. Comparisons with data from the literature agree withour findings: v sin i values from Slettebak et al. are underestimatedand the relation between both scales follows a linear law ensuremath vsin inew = 1.03 v sin iold+7.7. Finally, thesedata are combined with those from the previous paper (Royer et al.\cite{Ror_02a}), together with the catalogue of Abt & Morrell(\cite{AbtMol95}). The resulting sample includes some 2150 stars withhomogenized rotational velocities. Based on observations made atObservatoire de Haute Provence (CNRS), France. Tables \ref{results} and\ref{merging} are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.125.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/393/897
| On the MBM 12 Young Association
I present a comprehensive study of the MBM 12 young association (MBM12A). By combining infrared (IR) photometry from the Two-Micron All-SkySurvey (2MASS) survey with new optical imaging and spectroscopy, I haveperformed a census of the MBM 12A membership that is complete to 0.03Msolar (H~15) for a 1.75d×1.4d field encompassing theMBM 12 cloud. I find five new members with masses of 0.1-0.4Msolar and a few additional candidates that have not beenobserved spectroscopically. From an analysis of optical and IRphotometry for stars in the direction of MBM 12, I identify M dwarfs inthe foreground and background of the cloud. By comparing the magnitudesof these stars to those of local field dwarfs, I arrive at a distancemodulus 7.2+/-0.5 (275 pc) to the MBM 12 cloud; it is not the nearestmolecular cloud and is not inside the local bubble of hot ionized gas ashad been implied by previous distance estimates of 50-100 pc. I havealso used Li strengths and H-R diagrams to constrain the absolute andrelative ages of MBM 12A and other young populations; these dataindicate ages of 2+3-1 Myr for MBM 12A and ~10 Myrfor the TW Hya and η Cha associations. MBM 12A may be a slightlyevolved version of the aggregates of young stars within the Taurus darkclouds (~1 Myr) near the age of the IC 348 cluster (~2 Myr).
| Speckle Interferometry of New and Problem Hipparcos Binaries. II. Observations Obtained in 1998-1999 from McDonald Observatory
The Hipparcos satellite made measurements of over 9734 known doublestars, 3406 new double stars, and 11,687 unresolved but possible doublestars. The high angular resolution afforded by speckle interferometrymakes it an efficient means to confirm these systems from the ground,which were first discovered from space. Because of its coverage of adifferent region of angular separation-magnitude difference(ρ-Δm) space, speckle interferometry also holds promise toascertain the duplicity of the unresolved Hipparcos ``problem'' stars.Presented are observations of 116 new Hipparcos double stars and 469Hipparcos ``problem stars,'' as well as 238 measures of other doublestars and 246 other high-quality nondetections. Included in these areobservations of double stars listed in the Tycho-2 Catalogue andpossible grid stars for the Space Interferometry Mission.
| Speckle Interferometry at the US Naval Observatory. V.
The results of 1544 speckle interferometric observations of 637 binarystars, ranging in separation from 0.25" to 5.25", are tabulated. Theseobservations were obtained using the 66 cm refractor at the US NavalObservatory in Washington, DC, with an intensified CCD detector. This isthe fifth in a series of papers presenting measures obtained with thissystem and covers the period 1998 January 1 through December 31. Randomerrors for all measures are estimated to be 17.6 mas in separation and0.55d/ρ in position angle, where ρ is the separation inarcseconds.
| The distance to the nearest star-forming clouds: MBM12 and MBM20
We present high-resolution spectra (R ~ 49,000) of stars that haveparallax measurements from the Hipparcos satellite and are projectedalong the line of sight to the two nearest known star forming clouds tothe Sun: MBM12 and MBM20. The spectra were obtained with the FOCESEchelle Spectrograph at the 2.2 meter telescope in Calar Alto, Spain andthe wavelength range was chosen to include the interstellar Na I D linesat lambda 5889.950 Ä and lambda 5895.924 Ä. Since the starsare at a range of distances, we use their spectra along with theirparallaxes from Hipparcos to determine the distance to the moleculargas. The stars in front of the cloud do not show interstellar Na I Dabsorption features while the stars behind the cloud do showinterstellar absorption features. We find that both clouds are somewhatmore distant than previously estimated. The revised distance to MBM12 is58+/-5 pc < d < 90+/-12 pc and the distance to MBM20 is 112+/-15pc < d < 161+/-21 pc.
| Two-colour photometry for 9473 components of close Hipparcos double and multiple stars
Using observations obtained with the Tycho instrument of the ESAHipparcos satellite, a two-colour photometry is produced for componentsof more than 7 000 Hipparcos double and multiple stars with angularseparations 0.1 to 2.5 arcsec. We publish 9473 components of 5173systems with separations above 0.3 arcsec. The majority of them did nothave Tycho photometry in the Hipparcos catalogue. The magnitudes arederived in the Tycho B_T and V_T passbands, similar to the Johnsonpassbands. Photometrically resolved components of the binaries withstatistically significant trigonometric parallaxes can be put on an HRdiagram, the majority of them for the first time. Based on observationsmade with the ESA Hipparcos satellite.
| ROSAT PSPC observations of T Tauri stars in MBM12 PSPC observations of T Tauri stars in MBM12
We present the ROSAT PSPC pointed and ROSAT All-Sky Survey (RASS)observations and the results of our low and high spectral resolutionoptical follow-up observations of the T Tauri stars (TTS) and X-rayselected T Tauri star candidates in the region of the high galacticlatitude dark cloud MBM12 (L1453-L1454, L1457, L1458). Previousobservations have revealed 3 ``classical'' T Tauri stars and 1``weak-line'' T Tauri star along the line of sight to the cloud. Becauseof the proximity of the cloud to the sun, all of the previously knownTTS along this line of sight were detected in the 25 ks ROSAT PSPCpointed observation of the cloud. We conducted follow-up opticalspectroscopy at the 2.2-meter telescope at Calar Alto to look forsignatures of youth in additional X-ray selected T Tauri starcandidates. These observations allowed us to confirm the existence of 4additional TTS associated with the cloud and at least 2 young mainsequence stars that are not associated with the cloud and place an upperlimit on the age of the TTS in MBM12 ~ 10 Myr. The distance to MBM12 hasbeen revised from the previous estimate of 65+/-5 pc to 65+/-35 pc basedon results of the Hipparcos satellite. At this distance MBM12 is thenearest known molecular cloud to the sun with recent star formation. Weestimate a star-formation efficiency for the cloud of 2-24%. We havealso identified a reddened G9 star behind the cloud with A_v ~ 8.4-8.9mag. Therefore, there are at least two lines of sight through the cloudthat show larger extinctions (A_v > 5 mag) than previously thoughtfor this cloud. This higher extinction explains why MBM12 is capable ofstar-formation while most other high-latitude clouds are not. Table~4 isonly available in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html.}
| Speckle Interferometry at the US Naval Observatory. IV.
The results of 1314 speckle interferometric observations of 625 binarystars, ranging in separation from 0.2" to 5.2" with a limiting secondarymagnitude of V=11, are tabulated. These observations were obtained usingthe 66 cm refractor at the US Naval Observatory in Washington, DC, withan intensified CCD detector. This is the fourth in a series of paperspresenting measures obtained with this equipment and covers the period1997 January 1 through December 31. Random errors for all measures areestimated to be 18 mas in separation and 0.57d/rho in position angle,where rho is the separation in arcseconds.
| Speckle Interferometry at the US Naval Observatory. III.
Position angles and separations resulting from 2578 speckleinterferometric observations of 590 binary stars are tabulated. This isthe third in a series of papers presenting measures obtained using the66 cm refractor at the US Naval Observatory in Washington, DC, andcovers the period from 1995 June through 1996 December. Program starsrange in separation from 0.2" to 4.3", with a limiting magnitude ofV=11. Random errors are estimated to be 17.0 mas in separation and0.56d/rho in position angle, where rho is the separation in arcseconds.These are the first results acquired using an improved intensified CCDdetector. The new detector, in concert with an intensity-filteringtechnique applied in software, has permitted a 1 mag increase in dynamicrange, to 3.5 mag, for pairs separated by about 2". The instrumentationand calibration are briefly described, with an emphasis on thecharacteristics of the new detector. The software filter used toincrease the dynamic range is also described.
| Speckle Interferometry at the US Naval Observatory. II.
Position angles and separations resulting from 2406 speckleinterferometric observations of 547 binary stars are tabulated. This isthe second in a series of papers presenting measures obtained using the66 cm refractor at the US Naval Observatory in Washington, DC, with anintensified CCD detector. Program stars range in separation from 0.2" to3.8", with Deltam<=2.5 mag and a limiting magnitude of V=10.0. Theobservation epochs run from 1993 January through 1995 August. Randomerrors are estimated to be 14 mas in separation and 0.52d/rho inposition angle, where rho is the separation in arcseconds. Theinstrumentation and calibration are briefly described. Aspects of thedata analysis related to the avoidance of systematic errors are alsodiscussed.
| Speckle Observations of Binary Stars with the WIYN Telescope. I. Measures During 1997
Two hundred seventy-seven position angle and separation measures of 154double stars are presented. Three of the systems were previously unknownto be double, and 16 other systems were discovered earlier this decadeby the Hipparcos satellite. Measures are derived from speckleobservations taken with the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5 mtelescope located at Kitt Peak, Arizona. Speckle images were obtainedusing two different imaging detectors, namely, a multianode microchannelarray (MAMA) detector and a fast-readout CCD. A measurement precisionstudy was performed on a sample of binaries with extremely well knownorbits by comparing the measures obtained here to the ephemerispredictions. For the CCD, the root mean square (rms) deviation ofresiduals was found to be 3.5 milliarcseconds (mas) in separation and1.2d in position angle, while the residuals of the MAMA data varieddepending on the magnification used and seeing conditions but can becomparable or superior to the CCD values. In addition, the two cameraswere compared in terms of the detection limit in total magnitude andmagnitude difference of the systems under study. The MAMA system has theability to detect some systems with magnitude differences larger than3.5, although reliable astrometry could not be obtained on theseobjects. Reliable astrometry was obtained on a system of magnitudedifference of 5.3 with the CCD system.
| Measurements of double stars 1993.67 - 1998.13
624 Micrometer Measurements of 224 pairs with a 32.5 cm Cassegrain, 719Measurements of 310 double stars with a 360 mm Newtonian are given.Tables 1 to 4 are available in electronic form only at the CDS130.79.128.5 or via http://cdsweb.u-strasbg.fr/Abstract.html
| Micrometer Measures of Double Stars
Micrometer measures of 795 double stars made with the 26 inch (0.66 m)refractor of the US Naval Observatory from 1984 to 1990 are presented.
| ICCD Speckle Observations of Binary Stars. XVII. Measurements During 1993-1995 From the Mount Wilson 2.5-M Telescope.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.1639H&db_key=AST
| Speckle Interferometry at the US Naval Observatory. I.
We present speckle interferometer measurements of 467 binary stars takenat the US Naval Observatory in Washington, DC, using the 66 cmrefractor, from 1990 October through 1992 December. The observingprogram is designed to provide high-quality observations of binaries inthe 0."3--3."5 range of separations and as faint as 10.0 mag. More than8000 measurements have been made to date, of which we report the resultsfor 2329. Not only is it our intent to provide accurate data forinteresting binary stars, but also, by careful calibration, to firmlyrelate the "classical" astrometry of binary stars to that being obtainedtoday by speckle and that which will soon be obtained by other moderntechniques such as long-baseline optical interferometry.
| ICCD speckle observations of binary stars. 11: Measurements during 1991-1993 from the Kitt Peak 4 M telescope
One-thousand one-hundred ninety-seven observations of 730 binary starsystems, observed by means of speckle interferometry with the 4 mtelescope on Kitt Peak, are presented. Included in these binary starsare new interferometric companions to five visual binaries. Thesemeasurements, made mostly during the period 1991 to 1993, comprise the11th installment of results stemming from our speckle program at the 4 mclass telescopes on Kitt Peak, Cerro Tololo, and Mauna Kea.
| Speckle interferometric measurements of binary stars. VII
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1982ApJS...49..267M&db_key=AST
| Photographische Doppelsternmessungen mit Okularprojektion.
Not Available
| Mikrometermessungen von Doppelsternen. V.
Not Available
| Mikrometermessungen von Doppelsternen
Not Available
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| Сазвежђа: | Ован |
| Ректацензија: | 02h59m12.71s |
| Deклинација: | +21°20'25.1" |
| Apparent магнитуда: | 5.163 |
| Proper motion RA: | -9.4 |
| Proper motion Dec: | -5 |
| B-T magnitude: | 5.227 |
| V-T magnitude: | 5.169 |
Каталог и designations:
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