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Uvbyβ photometry of all stars earlier than G0 and brighter than m_pg_~10.3mag in Selected Area 194
Four-colour and Hβ photometry is introduced for 594 stars earlierthan G0 in the Kapteyn's Selected Area 194. The results give V, b-y,m_1_, c_1_, and β on the standard systems, with overall rms errorsfor one observation of one star of 0.009mag, 0.004mag, 0.006mag,0.009mag, and 0.009mag, respectively. The data cover an area of about5deg x 5deg and is intended for an investigation of the distribution ofthe interstellar medium toward the northern part of the SouthernCoalsack and its surroundings. A comparison to earlier results obtainedby other authors has shown that the c_1_ indices obtained for the latetype stars were underestimated, in average, by 0.020mag. Since suchdifference may account for an error of little more than 10% in theestimated stellar distances, a correction was applied to the c_1_ indexof these stars.
| Stromgren and H-beta photometry of stars earlier than G0 in the Southern Coalsack direction
Four-color and H-beta photometry have been obtained for 236 starsearlier than G0 in order to study the color excess distribution in theSouthern Coalsack direction. The beta histogram of the stars reveals arelative absence of stars in the range of A4 to A9. The (b-y)distribution for B-type stars suggests the existence of three differenttypes of stars located at different distances.
| Estimation of spectral classifications for bright southern stars with interesting Stromgren indices
This paper investigates the degree of success with which uvby photometrycan be applied to predict spectral classifications for 947 A, F, and Gstars brighter than an apparent magnitude of 8.3 and with four-colorindices indicating some kind of interesting, unusual, or peculiarspectrum. One or several possible spectral classifications are estimatedfor each star from photometry alone, double stars are distinguished, andthe estimates are compared with published classifications. The resultsshow that the framework provided by uvby photometry can be extended toinclude most G and K stars, reddened stars, peculiar stars, and certaintypes of double star.
| Preferred frequency for interstellar communications
It is suggested that the 4829.659-MHz line frequency of the1(11)-to-1(10) rotational transition of formaldehyde is a plausiblefrequency to monitor for the purpose of detecting interstellarcommunications. The formaldehyde line is of interest because, as aresult of the antimaser effect, it exhibits a very low excitationtemperature. The background radiation temperature in the direction ofdark clouds is below the 3 K background temperature; the backgroundnoise temperature, lowered approximately 1 K, is lower than at any otherfrequency band.
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Dades d'Observació i Astrometria
| Constel·lació: | Crux |
| Ascensió Recta: | 12h44m56.46s |
| Declinació: | -62°12'51.3" |
| Magnitud Aparent: | 8.859 |
| Distancia: | 1666.667 parsecs |
| Moviment propi RA: | -27.7 |
| Moviment propi Dec: | -2.6 |
| B-T magnitude: | 9.942 |
| V-T magnitude: | 8.949 |
Catàlegs i designacions:
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