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Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| New Estimates of the Solar-Neighborhood Massive Star Birthrate and the Galactic Supernova Rate
The birthrate of stars of masses >=10 Msolar is estimatedfrom a sample of just over 400 O3-B2 dwarfs within 1.5 kpc of the Sunand the result extrapolated to estimate the Galactic supernova ratecontributed by such stars. The solar-neighborhood Galactic-plane massivestar birthrate is estimated at ~176 stars kpc-3Myr-1. On the basis of a model in which the Galactic stellardensity distribution comprises a ``disk+central hole'' like that of thedust infrared emission (as proposed by Drimmel and Spergel), theGalactic supernova rate is estimated at probably not less than ~1 normore than ~2 per century and the number of O3-B2 dwarfs within the solarcircle at ~200,000.
| An Atlas of Spectrophotometric Landolt Standard Stars
We present CCD observations of 102 Landolt standard stars obtained withthe Ritchey-Chrétien spectrograph on the Cerro TololoInter-American Observatory 1.5 m telescope. Using stellar atmospheremodels, we have extended the flux points to our six spectrophotometricsecondary standards, in both the blue and the red, allowing us toproduce flux-calibrated spectra that span a wavelength range from 3050Å to 1.1 μm. Mean differences between UBVRI spectrophotometrycomputed using Bessell's standard passbands and Landolt's publishedphotometry were determined to be 1% or less. Observers in bothhemispheres will find these spectra useful for flux-calibrating spectra,and through the use of accurately constructed instrumental passbands,will be able to compute accurate corrections to bring instrumentalmagnitudes to any desired standard photometric system (S-corrections).In addition, by combining empirical and modeled spectra of the Sun,Sirius, and Vega, we calculate and compare synthetic photometry toobserved photometry taken from the literature for these three stars.
| New runaway OB stars with HIPPARCOS
A Monte Carlo method for detection of runaway OB stars fromobservational data is proposed. 61 runaway OB star candidates have beendetected by an analysis of Hipparcos proper motions. The peculiartangential and total transverse velocities have been determined forthese stars. A list of the detected runaway star candidates ispresented. The evidence of a discrepancy between photometric andparallactic distances of runaway OB star candidates is presented.
| Stars with ISM Polarization Observed with HPOL. II
Polarization data are given for stars whose polarizations are mostlyinterstellar which were observed with the University of Wisconsinspectropolarimeter (HPOL) during 1995-2003. Several cases are found forwhich K in the Serkowski Law for ISM polarization is higher than allowedby published formulas.
| Catalog of Galactic OB Stars
An all-sky catalog of Galactic OB stars has been created by extendingthe Case-Hamburg Galactic plane luminous-stars surveys to include 5500additional objects drawn from the literature. This work brings the totalnumber of known or reasonably suspected OB stars to over 16,000.Companion databases of UBVβ photometry and MK classifications forthese objects include nearly 30,000 and 20,000 entries, respectively.
| Passbands and Theoretical Colors for the Washington System
The passbands of the Washington system (C, M, T1,T2) have been checked through synthetic photometry of theVilnius spectra and comparison of observed and synthetic color-colorrelations. Using the derived passbands, theoretical colors were computedusing the grid of ATLAS no-overshoot models of Castelli. These can beused for calibration of the Washington system.
| Archival searches for transient optical emission in the error box of the 1991 January 22 gamma-ray burst
We present here the results of a study carried out at the HarvardCollege Observatory Plate Collection. We examined 3995 plates coveringthe error box of the gamma-ray burst GRB 910122, over a time span of 90yr (from 1889 to 1979). The total exposure time is ~ 0.55 yr. Noconvincing evidence of optical transient emission was found within theGRB 910122 IPN error box. However, a possible OT was found outside theGRB 910122 error box. Optical ground based observations have revealed aV ~ 22.3 object consistent with the position of the new object. Thecolours of the object are typical of a K7/M0 star or a reddened galaxy,which could have caused the OT, but the fact that the object is far awayfrom the GRB error box makes both events unrelated.
| Structure analysis of edge-on spiral galaxies.
The stellar distribution of a small sample of edge-on spiral galaxies isexamined in B, V, R, and I by fitting model distributions to the lightprofiles, both perpendicular to the galaxy planes and along the majoraxes. We have developed a method to compare the fits for the modelsobtained for different galaxies by introducing a global goodness-of-fitparameter P_ij_. In general, the best fitting vertical model is morepeaked than expected for an isothermal sheet distribution, i.e. it iseither an exponential light distribution or a sech(z)-model. The mostlikely explanation for the deviations from an exponential or a sech(z)distribution at small z is dust extinction, whereas the excess lightdetected at large z for a few early-type spirals could be due to a thickdisk component. The constancy of the exponential scale height of boththe thin and the thick disks as a function of position along the majoraxis is confirmed, although it seems to lose strength in the radialouter parts. It is found that the vertical scale parameters for both thethin and the thick disks are confined within narrow ranges. We show thatthe scale lengths vary as a function of z-distance from the galaxyplanes. The smallest scale lengths were measured in the galaxy planes.This can be explained by a combination of absorption effects and a youngstellar population, that is supposed to be present in the galaxy planes.The mean ratio of the radial to the vertical scale parameter, h_R_/z_0_,is 5.9+/-0.4.
| New pulsational properties of eight `anomalous' RR Lyrae variables
CCD photometry in the V band is presented for seven field RR Lyrae starsselected from a sample of eight variables; these, according to datacollected in the literature, are expected to be ab-type pulsators, tohave short periods (and hence high metallicity), and to be located at ahigh z from the Galactic plane. New periods and epochs are derived forthem. The new periods are only slightly shorter than the valuespublished in the fourth edition of the General Catalogue of VariableStars (GCVS4). In six cases our amplitude of the light variation issignificantly smaller than that published in the GCVS4, and in at leastthree cases the actual pulsation appears to be in the first harmonicrather than in the fundamental mode. All the suggested c-type pulsatorsshow variations in the amplitude and/or quite scattered light curves.Some possible explanations are given. From a spectrophotometric analysisof the sample, only DL Com is confirmed to pulsate in the fundamentalmode, to have a short period, and to be located at a relatively high z.However, a single object cannot be taken as evidence for a significantmetal-rich population at a large distance from the Galactic plane.
| Ultraviolet FeIII lines in the spectra of high galactic latitude early-type stars
Using high resolution spectral data from the International UltravioletExplorer satellite, we present qualitative and quantitative comparisonsof blends of Fe III absorption lines in the region1890A<=λ<=1930A for a sample of fifteen high latitudeB-type and standard stars. Standard and halo stars were matched ineffective temperature and surface gravity using Stroemgren [c_1_] andHβ photometry, and LTE model atmosphere codes were used toinvestigate whether they had similar iron abundances. We conclude thatwhile most of the halo stars have Population I iron abundances and maybe young objects, one star, HD 177566, has significant iron and silicondepletions and is most probably an old, evolved star. In view of thecoincidence of the atmospheric parameters of this star with those ofyoung B-type stars, we consider a post-AGB evolutionary status to belikely for HD 177566.
| The distribution of neutral hydrogen in the interstellar medium. 1: The data
We compile, from the existing literature, the largest sample to date(842 data points) of hydrogen column density measurements, N(H I), ofthe gas in the interstellar medium. We include only results obtainedfrom absorption measurements toward individual stars (594 in our sample)in an effort to construct a three-dimensional picture of theinterstellar gas. We derive hydrogen column densities toward a fractionof the stars in the sample from published column density measurements ofmetal ions. A three-dimensional physical model derived from this dataset will be presented in a companion paper. The observed stars spandistances from a few parsecs to a few thousand parsecs, and more thanhalf of the sample serves to describe the local interstellar mediumwithin a few hundred parsecs of the Sun. Hydrogen column densities rangefrom 1017 to 1022/sq cm. We describe here thevarious observational methods used to estimate the hydrogen columndensities and present the table with the stellar and hydrogen columndensity data. The provided table is intended as a global reference work,not to introduce new results.
| A high-resolution optical and radio study of Milky Way halo gas
Optical interstellar absorption lines of Ti II and Ca II and the 21 cmemission line of H I were observed at high-resolution (6 and 1 km/s,respectively) and high detection sensitivity along 25 lines of sight inthe Galactic halo. The sample includes 16 distant halo stars matchedwith one or more nearly aligned foreground stars as well as local starsalong five extragalactic sight lines. The data show substantialinterstellar material, at both low and intermediate velocities, between250 and 1000 pc beyond the Galactic plane. As much as one-third of thetotal gas observed in Ca II absorption may be beyond 1 kpc, and thegaseous Ti II may lie in an even thicker layer. The directly determinedgaseous Ti abundance above the Galactic plane exceeds that in the disk,on the average, by a factor of 4 to 6 and, for individual cloudcomponents, is further enhanced at higher LSR velocity. Thirty threediscrete high-latitude clouds are detected in Ca II absorption, and 17discrete clouds, including three high-velocity clouds, are identified inH I emission. The kinematics of the high-latitude gas observed in Ti IIand Ca II absorption is characterized by significant peculiar velocitieswith respect to a model corotating halo.
| On the distance to the HVC-complex Hydra/Sextans.
Not Available
| A radio optical reference frame. III - Additional radio and optical positions in the Southern Hemisphere
Radio and optical positions are presented for southern hemisphereextragalactic sources from the Parkes 2.7 GHz survey. Sixty-one sourceswere observed with Mark III VLBI at 8.4 GHz between Tidbinbilla,Australia, and Hartebeesthoek, South Africa. The results presented arepart of the effort to establish a global reference frame of 400extragalactic radio sources. Radio positions with about 10 milliarcsecerrors have been estimated for 39 sources not previously in the presentradio reference frame catalog, and provisional positions were obtainedfor two additional sources, bringing the total number of catalog sourcesto 276. The principal source of error is the uncalibrated ionosphere. Ofthe remaining sources five were completely undetected, six were eithertoo faint or too resolved, and nine had previous catalog positions.Optical positions on the FK5 system have also been measured for foursouthern sources using prime focus plates from the Anglo-Australian 4 mtelescope with an accuracy of 0.06 arcsec. This raises to 40 the numberof radio sources with accurately measured positions for their opticalcounterparts.
| Uvby-beta observations of 528 type B stars with V between the 8th and 9th magnitude
The paper presents uvby-beta measurements of 528 type B stars selectedfrom the SAO Catalog on the basis of two criteria: the spectral types inthe range B3-B5 and mV between the 8th and the 9th magnitude. Reddeningindependent (c1) values are estimated from the spectral classificationand compared to the observed values. No systematic trend with observed(b-y), H-beta, or spectral type appears to be present, but the range of(c1) residuals is surprisingly large. A rather large part of the starshas small beta values, smaller than for the BIa supergiants. Only twoare classified as O stars and most of them have the suffix e, ne, ornne. Most beta values for the O type stars are slightly above the upperlimit of 2.585 m.
| Photoelectric UBV photometry of northern stars from the HK objective-prism survey. II
Photoelectric UBV photometry is presented for a sample of 165 starsdrawn from the extension of the HK objective-prism/interference-filtersurvey of Beers, Preston, and Shectman to the northern galactichemisphere. These results are part of continuing follow-up observationsof candidate metal-deficient and horizontal-branch field stars and otherinteresting stars identified in the survey. A complete set ofphotometric observations is now available for three of the25-square-degree survey fields. The complete photometric sample of 299northern HK candidates obtained to date contains on order 90main-sequence turnoff, subgiant, and giant stars with (Fe/H) of lessthan or equal to -1.0, 50 field blue horizontal-branch stars, and 30stars with the photometric properties of field-blue stragglers.
| A photometric study of the very short period eclipsing binary EH Hydrae
Recent Johnson-Cousins' B,V,Rc,Ic photoelectric observations of the veryshort period W UMa variable, EH Hya, are presented. These observationswere made, using the Yale 1M telescope and the dry-ice-cooled HamamatsuGa-As PMT at Cerro Tololo Inter-Americal Observatory. The light curvesreveal that the eclipses are total, and that the primary eclipse is anoccultation. Thus, the system is of W-type, with the larger componentbeing the cooler. Standard magnitudes were determined, and a reddeningestimate was made. A simultaneous solution of the B,V,R light curves wascomputed using the Wilson-Devinney (1971) synthetic light curve code.The solution indicates that the system consists of two late G-type starsin shallow contact with a fill-out factor of 12 percent. The differencein component temperatures is 336(8) K and the mass ratio is ratherextreme, being 0.314(2). EH Hya is compared to other very short periodbinaries of late G-type, and they are found to comprise a fairlyhomogenous group with regards to mass ratios, degree of thermal contact,and magnetic activity.
| UBV(RI)c photometry of equatorial standard stars - A direct comparison between the northern and southern systems
UBV(RI)c photometry of 212 stars from Landolt's list of equatorialstandards is presented. The observations are tied to the system definedby Cousin's E-region standards. A comparison of the present results withLandolt's reveals reasonably good agreement for (V-R)c and (V-I)c, butmarked systematic differences for (B-V) and (U-B). The UBV systems ofCousins and Landolt are evidently not the same and both probably differfrom Johnson's original system.
| Photoelectric UBV photometry of northern stars from the HK objective-prism survey
Photoelectric photometry is presented for a sample of 139 halo starsdrawn from an extension of the HK objective-prism survey of Beers,Preston, and Shectman to the northern galactic hemisphere. Thecandidates for which photometry is reported were selected to span a widerange of types, but are dominated by stars classified as type AB, A, or'metal poor'.
| Washington CCD standard fields
Twenty-two new Washington system standards have been established in fourfields suitable for observation with a CCD. Each field includes starswith a wide color range sufficiently faint to be observed with largetelescopes. The fields are (mostly) equatorial, and spaced approximatelyevery 6 hours in right ascension. All observations were obtainedphotoelectrically to ensure that they were on the standard system. Themean number of observations per star is 18, and the mean colors andmagnitudes are determined to about 0.005 mag. The existence of anextremely red star near the Landolt standard SA 98-682 is noted. Inaddition, (M-51) observations are presented for 13 traditionalCMT(1)T(2) standards that allow their use as standards for this colorindex as well.
| Empirical temperature calibrations for early-type stars
Three temperature calibrations of suitable photometric quantities havebeen derived for O and B stars. A sample of 120 stars with reliableT(eff.) determinations has been used for establishing each calibration.The different calibrations have been critically discussed and compared.Temperature determinations for 1009 program stars have been obtainedwith an accuracy of the order of 10 percent.
| IUE-IRAS studies of the infrared cirrus
The 60 and 100 micron cirrus emission around 256 lines of sight in theIRAS all-sky survey was measured, and the flux averages were used tostudy the distribution, variations, and correlations of the IRASinfrared cirrus fluxes with various interstellar parameters. It wasfound that the 60 and 100 micron fluxes correlate with the depletion ofSi and show a trend with the depletion of Fe for 51 lines of sighttoward the Galactic halo. No correlation was found with the abundancesof Si, Mn, Fe, S, or Zn or with abundance ratios for the full sample of256 stars. An abundance ratio of about 3 x 10 to the 7th by numberrelative to H was derived from 60 and 100 micron flux ratios and the Hcolumn along the line of sight; this ratio appears to decrease by afactor of 10 into the halo.
| Spectrophotometry of stars of intermediate brightness
Spectrophotometric observations of 15 stars in a magnitude range m ofbetween 8.0 and 10.9, located mostly near the equator and covering allthe range of right ascensions, are presented. The energy distributionshave been obtained in Hayes' (1970) system as revised by Hayes andLatham (1975), and in the augmented system presented by Taylor (1984).Comments about some of the standard stars are presented as well as acomparison of the results obtained with both systems.
| Galactic interstellar abundance surveys with IUE. III - Silicon, manganese, iron, sulfur, and zinc
This paper continues a survey of intestellar densities, abundances, andcloud structure in the Galaxy using the IUE satellite. A statisticaldata set of 223 O3-B2.5 stars is constructed, including 53 stars in theGalactic halo. It is found that S II lines in B stars, of luminosityclasses IV and V, have possible contamination from stellar S II,particular for stars with v sin i less than 200 km/s. The meanlogarithmic depletions are -1.00, -1.19. -0.63, and -0.23 (Si, Mn,Fe,S,Zn). Depletions of Si, Mn, and Fe correlate with the mean hydrogendensity n-bar along the line of sight, with a turnover for n-bar greaterthan 1/cm. Sulfur depletions correlate with n-bar along the line ofsight. The slight Zn depletion correlation also appears to bestatistically insignificant. No correlation of depletion is found withthe physical density derived from H2 rotational states in 21 lines ofsight. Depletion variations in the disk are consistent with a Galacticabundance gradient or with enhanced mean depletions in the anticenterregion.
| Galactic interstellar abundance surveys with IUE. II - The equivalent widths and column densities
This paper continues a survey of interstellar densities, abundances, andcloud structure in the Galaxy, using the International UltravioletExplorer (IUE) satellite. Equivalent widths of 18 ultraviolet resonancetransitions are presented and column densities for Si II, Mn II, Fe II,S II, and Zn II toward 261 early-type stars are derived. Theseequivalent widths and column densities agree within the stated errors ofearlier Copernicus, BUSS, or IUE surveys of Mn II, Fe II, S II, and ZnII for 45 stars in common. The column densities are derived fromsingle-component curves of growth with a common b-value based on that ofFe II and Si II.
| The extent of the local H I halo
Forty-five high-latitude, OB stars have been observed in the Ly alphaand 21 cm lines of HI in an effort to map out the vertical distributionand extent of the local HI halo. The 25 stars for which a reliable HIcolumn density can be obtained from Ly alpha lie between 60 and 3100 pcfrom the plane. The principal result is that the total column density ofHI at an absolute value of z greater than 1 kpc is, on the average, 5 +or - 3 x 10 to the 19th power/sq cm, or 15 percent of thetotalHI. At relatively low z the data toward some starssuggest a low effective scale height and fairly high average foregrounddensity, while toward others the effective scale height is large and theaverage density is low. This can be understood as the result ofirregularities in the interstellar medium. A model with half of the HImass in clouds having radii of a few pc and a Gaussian verticaldistribution with sigma2 = 135 pc, and half of the mass in anexponential component with a scale height of 500 pc, gives asatisfactory fit to the data. The technique of comparing Ly alpha and 21cm column densities is also used to discuss the problem of estimatingthe distance to several possibly subluminous stars.
| On optical studies of high-velocity clouds
Lists of distant objects that can be used to study physical conditionsin, and distances of, 21 cm (Oort) high-velocity clouds are presented.Recent published observations are used to compile positions, velocities,and distances of the clouds.
| Catalog of O-B stars observed with Tokyo Meridian Circle
A catalog of the O-B stars, selected from 'Blaauw-Parenago' list andRubin's catalog, has been compiled on the FK4 system by the observationsmade with Gautier 8-inch Meridian Circle at the Tokyo AstronomicalObservatory during the period, 1971 to 1979. It contains 1059 stars andwas compiled for the future establishment of high precision propermotions of O-B stars.
| Galactic interstellar abundance surveys with IUE. I - Neutral hydrogen
A survey is initiated of interstellar densities, abundances, and cloudstructure in the Galaxy, using the International Ultraviolet Explorer.From high-resolution (0.1-A) spectra, interstellar column densities arederived toward 244 early-type stars by fitting the damping wings of theLy-alpha absorption line. Published B-V photometry is used to deriveE(B-V) color excesses, stellar distances r, and the mean hydrogendensities, n-bar = N(H I)/r. The data set includes stars out to r = 8.5kpc and E(B-V) = 0.86, with 68 stars in the galactic halo (absolute bgreater than 20 deg). The statistical sample consists of 205 stars oftype O3-B2.5 within 5 kpc (53 stars in the halo). The column densities,log N(H I), range from less than 19.44 per square centimeter for alphaVir to 21.81 for HD 37061. A statistical analysis of the E(B-V)distribution suggests variations in the line-of-sight cloud density andthe mean reddening per cloud.
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| קבוצת-כוכבים: | סכסטנט |
| התרוממות ימנית: | 09h48m44.49s |
| סירוב: | -02°42'49.0" |
| גודל גלוי: | 8.62 |
| מרחק: | 10000000 פארסק |
| תנועה נכונה: | 3.6 |
| תנועה נכונה: | -12.8 |
| B-T magnitude: | 8.459 |
| V-T magnitude: | 8.607 |
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