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Tiny H I clouds in the local ISM
We report deep, high spectral resolution WSRT H I 21 cm observations offour high latitude compact radio sources, that have revealed a newpopulation of tiny, discrete clouds in the diffuse ISM, with peakoptical depths τ ˜ 0.1 - 2%, H I column densities of 0.4-8× 1018 cm-2 and core temperatures of 20-80K. Imaging detections confirm these low column densities and implylinear core dimensions of a few thousand AU, assuming a distance of 100pc. The physical origin of these tiny H I structures and theirdistribution in the ISM is at present unknown. Further observations willbe required to determine whether they are a ubiquitous component of theISM.
| Further Studies of A-Stars and F-Stars in the Region of the North Galactic Pole - Part Three - a Catalogue of Star Names and Positions
Not Available
| UVBY beta photometry of 210 B, A, and F stars in ten areas centered on extragalactic radio sources at high northern galactic latitudes
As part of a study of the reddening properties of the interstellarmedium at the South Galactic pole and particularly along the southernpart of the galactic plane, a catalog of ubvy beta photometry of 210 B,A, and F stars in 10 areas of equal size covering 160 sq deg atlatitudes higher than +30 deg is presented. Each of the observed areasis centered at radio sources that have emission or absorption in the21-cm line; and the main aim of the study is to obtain color excessesfor a comparison of neutral hydrogen column densities, tentativelyassociated with distinct clouds and with the occurrence of dust in theseclouds. V, (b-y), m1, c1, and beta are presented for the 210 stars.
| Stars with large proper motions in the astrographic zones+ 32° and + 33° (List I)
Not Available
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Av Kopekleri |
| Sað Açýklýk: | 13h25m55.84s |
| Yükselim: | +31°51'40.6" |
| Görünürdeki Parlaklýk: | 8.256 |
| Uzaklýk: | 104.932 parsek |
| özdevim Sað Açýklýk: | 15.8 |
| özdevim Yükselim: | -45.8 |
| B-T magnitude: | 8.908 |
| V-T magnitude: | 8.31 |
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