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A statistical analysis of the detection limits of fast photometry
This work investigates the statistical limits for the detection ofstellar variability using ground based fast photometry. We show thatwhen sky transparency variations are very low or have been efficientlyremoved from the raw light curve, the overall noise is of a MixedPoisson (MP) nature (photon noise mixed by scintillation). As aconsequence, three regimes appear for the detection of photometricvariations depending on the star's brightness (scintillation,scintillation and photon noise, photon noise and sky background). Theproposed analysis is mainly applied to the Indian sites of Manora Peak(existing 104 cm telescope) and Devasthal (future 1 m automatedtelescope, and 3 m telescope project). As shown by some examples, it canbe applied to any site with the corresponding parameters. For 1 m classtelescopes at an altitude of about 2000 m, the frontier magnitudesbetween the different detection regimes are about 10 mag and 15 mag. Byanalysing the corresponding statistics of the MP noise periodogram, theminimum amplitude variation that one can detect with a given confidencelevel is evaluated for each observational setting. For example, with a 3m telescope at about 2500 m, ≈120 μmag variations would bedetected in 2 h with a 99% confidence level for stars brighter thanmagnitude 12. For a star of 15th magnitude, ≈400 μmag oscillationswould still be detected at that level. These detection limits arediscussed in the light of observations obtained in Manora peak, andcompared to results obtained at different astronomical sites.
| A search for rapid oscillations in chemically peculiar A-type stars
In 1995 we initiated a Northern Hemisphere survey for rapidlyoscillating Ap stars. This paper presents the results including one newroAp star (HD 122970), the confirmation of rapid oscillations of HD99563 and apparent null results for other stars. Using Hipparcos data astatistical analysis of the absolute magnitudes and galacticdistributions of all known roAp and noAp stars (also taken from theliterature) was made. A systematic trend for most of the program starsin a M_{ V} vs. beta (index of the Strömgren uvbybeta system)diagram was detected leading to the conclusion that beta issystematically influenced by the chemical peculiarity and/or magneticfield. Three roAp stars are outside the delta Scuti instability stripwhich implies that the driving mechanism of the two classes of pulsatingstar is different. This is also suggested by new pulsation models. Nostatistical difference between the galactic distribution of roAp andnoAp stars was found.
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Datos observacionales y astrométricos
| Constelación: | Can Menor |
| Ascensión Recta: | 07h23m48.97s |
| Declinación: | +06°56'45.6" |
| Magnitud Aparente: | 7.644 |
| Movimiento Propio en Ascensión Recta: | 5.5 |
| Movimiento Propio en Declinación: | 5.7 |
| B-T magnitude: | 8.097 |
| V-T magnitude: | 7.682 |
Catálogos y designaciones:
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