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To see or not to see a bow shock. Identifying bow shocks with Hα allsky surveys
OB-stars have the highest luminosities and strongest stellar winds ofall stars, which enables them to interact strongly with theirsurrounding ISM, thus creating bow shocks. These offer us an idealopportunity to learn more about the ISM. They were first detected andanalysed around runaway OB-stars using the IRAS allsky survey by vanBuren et al. (1995, AJ, 110, 2614). Using the geometry of such bowshocks information concerning the ISM density and its fluctuations canbe gained from such infrared observations. As to help to improve the bowshock models, additional observations at other wavelengths, e.g.Hα, are most welcome. However due to their low velocity these bowshocks have a size of 1°, and could only be observed as awhole with great difficulties. In the light of the new Hα allskysurveys (SHASSA/VTSS) this is no problem any more. We developeddifferent methods to detect bow shocks, e.g. the improved determinationof their symmetry axis with radial distance profiles. Using twoHα-allsky surveys (SHASSA/VTSS), we searched for bow shocks andcompared the different methods. From our sample we conclude, that thecorrelation between the direction of both proper motion and the symmetryaxis determined with radial distance profile is the most promisingdetection method. We found eight bow shocks around HD17505, HD 24430, HD48099, HD 57061, HD92206, HD 135240, HD149757, and HD 158186 from 37 candidatestaken from van Buren et al. (1995, AJ, 110, 2614). Additionally to thetraditional determination of ISM parameters using the standoff distanceof the bow shock, another approach was chosen, using the thickness ofthe bow-shock layer. Both methods lead to the same results, yieldingdensities ( 1 cm-3) and the maximal temperatures (104 K), that fit well to the up-to-date picture of the WarmIonised Medium.
| Mean positions and proper motions of 224 stars based on PZT observations at Ondrejov in 1973-1986
An improvement of the positions and proper motions for the Ondrejov PZTstar list based on observations of 224 stars in the period 1973-1986 ispresented. The mean epoch of the PZT 86 catalogue is found to be 1981.56with a standard error in right ascension equal to + or - 0.0015 s/ andin delination equal to + or - 0.017 arcsec. The proper motions in rightascension and declination were obtained with an accuracy characterizedby the average standard errors of + or - 0.051 s/cy and + or - 0.57arcsec/cy, respectively. The PZT 86 catalogue is compared with theprevious PZT (1978 and 1983) catalogues, and with the AGK 3 (Dieckvoss,1975) catalogue.
| Mean positions and proper motions of 305 stars obtained from the combination of PZT observations at Ondrejov with AGK positions
Observations of 305 stars carried out at the Ondrejov Observatory in theperiod 1973-1983 were compared to the positions of the same stars in theAGK 2 and AGK 3 catalogs in order to obtain their mean positions andproper motions. The observations were performed in the course of 1140nights using the PZT telescope and comprise more than 32 thousand startransits. The average mean errors in the right ascension and declinationof a star that was observed thoughout the whole period were + or -0.0019 s and + or - 0.019 arcsec in the epoch around 1979. It ispredicted that the errors will increase + or - 0.0055 sec and + or -0.059 arcsec in the year 2000. A table listing the errors in the rightascension and declination is provided.
| The determination of mean positions and proper motions of 304 stars from PZT observations at Ondrejov
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Observation and Astrometry data
| Constellation: | やまねこ座 |
| Right ascension: | 07h24m35.94s |
| Declination: | +49°53'49.4" |
| Apparent magnitude: | 9.46 |
| Proper motion RA: | -3 |
| Proper motion Dec: | -1.3 |
| B-T magnitude: | 9.593 |
| V-T magnitude: | 9.471 |
Catalogs and designations:
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