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Statistical Constraints for Astrometric Binaries with Nonlinear Motion
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| Discovery of an Extremely Red Object in the Field of HD 155826
We have discovered an extremely red object, LSF 1, located 7" southwest(P.A. 217°) of the bright spectroscopic binary system HD 155826.Originally reported by IRAS as one source detected at 12-60 μm, andfound as a single 6-25 μm source of similar flux in the MidcourseSpace Experiment Galactic plane survey, two bright point sources werefound in arcsecond resolution infrared images obtained with the MIRLINcamera at the Infrared Telescope Facility and confirmed by the LongWavelength Spectrometer camera on Keck I. While HD 155826 itself waseasily detected in all the broadband and narrowband filters from 0.9 to12 μm that we used, the new counterpart, LSF 1, is only visible at 10μm. In Gunn z, J, H, and K', the upper limit to the new object'smagnitude is ~14. The detection of the new bright IR source explains theconfusing [K]-[N] IRAS colors that originally implied that HD 155826 wasa possible Vega-like system. The ``anomalous long-wavelength emission''is found to arise entirely from the new source. Without mid-IR extensionor excess long-wavelength emission, HD 155826 should no longer beclassified as a Vega-like system. We suspect LSF 1 to be either a highlyreddened carbon star or a Class II YSO, with no association with thehigh proper motion HD 155826 system.
| MK classification and photometry of stars used for time and latitude observations at Mizusawa and Washington
MK spectral classifications are given for 591 stars which are used fortime and latitude observations at Mizusawa and Washington. Theclassifications in the MK system were made by slit spectrograms ofdispersion 73 A/mm at H-gamma which were taken with the 91 cm reflectorat the Okayama Astrophysical Observatory. Photometric observations in UBV were made with the 1-meter reflector at the Flagstaff Station of U.S.Naval Observatory. The spectrum of HD 139216 was found to show a strongabsorption line of H-beta. The following new Am stars were found:HD9550, 25271, 32784, 57245, 71494, and 219109. The following new Apstars were found: HD6116, 143806, 166894, 185171, and 209260. The threestars, HD80492, 116204, and 211376, were found to show the emission inCaII H and K lines.
| Preliminary catalog of the declinations of 96 stars of the international program, compiled from Kitab PZT observations
Not Available
| UBV Photoelectric Photometry of 259 PZT Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980PASP...92..215G&db_key=AST
| Possible nearby stars brighter than tenth magnitude
Basic data are compiled for 447 stars brighter than 10th visualmagnitude which may be within 25 pc of the sun and are missing from boththe Gliese (1969) and the Woolley et al. (1970) catalogs of nearbystars. The list includes 245 stars with photometric parallaxes, 17 starswith trigonometric parallaxes, and nine stars with dynamical parallaxes,all of which parallaxes are at least 0.040 arcsec, as well as 176 likelycandidates. The stars are grouped into six categories according to thereliability of absolute-magnitude estimates and ranked within each groupon the basis of calculated distance. The distance estimates incorporatea kinematic correction to the photometric parallaxes which is based onthe size of a star's proper motion. A list of stars brighter than 10thmag which appear in the Gliese but not in the Woolley et al. catalog isalso provided to facilitate cross-reference with existing catalogs ofnearby stars.
| Trigonometric parallaxes of 36 stars determined by photography with the MC Cormick 26-inch refractor.
Not Available
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| Takýmyýldýz: | Kertenkele |
| Sað Açýklýk: | 22h24m37.85s |
| Yükselim: | +39°25'50.6" |
| Görünürdeki Parlaklýk: | 8.013 |
| Uzaklýk: | 45.704 parsek |
| özdevim Sað Açýklýk: | 173 |
| özdevim Yükselim: | 83.2 |
| B-T magnitude: | 8.838 |
| V-T magnitude: | 8.082 |
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