Other
Scientific paper
Sep 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mst...........f&link_type=abstract
Diploma Thesis, University of Vienna, (2000)
Other
7
Surface Brightness Fluctuations (Sbf), Galaxies, Ngc 3379, Photometry, Distances And Redshifts, Distance Scale
Scientific paper
In this work a direct method for determining extragalactic distances, the Surface Brightness Fluctuations (SBF) technique, is presented.Apart from a historical introduction the first part gives a comparison between different primary and secondary indicators of the Extragalactic Distance Scale. An extensive, current review of the five most popular indicators, Classical Cepheids, RR Lyrae stars, Globular Clusters, Novae and Supernovae of type Ia for measuring extragalactic distances is also included, whereas weight is given to the application, the associated problems and difficulties, occured uncertainties and errors, precision of the individual technique and finally the range of each method.In the second part of my work the Surface Brightness Fluctuations method is discussed in detail. Apart from the application as a distance indicator, different calibrations, uncertainties and the accuracy of the technique, in particular attention was paid to the practical implementation of measurements and analyses. Various wavelength regions the V, R, I as well as the K-band are compared with each other and their advantages and disadvantages illustrated. A preview of future improvements and upcoming Hubble Space Telescope projects closes this review.The last part contains a direct application of the SBF method to photometric Kron-Cousins I-band data of the standard E0 galaxy NGC 3379, observed with the 3.5m ESO NTT telescope, in La Silla, Chile. The zeropoint calibration was performed using I-band aperture photometry of the standard stars of the galactic cluster M67. After a smooth galaxy model for the galaxy NGC 3379 was constructed and subtracted from the original data the total signal amount of unwanted point sources, such as foreground stars, background galaxies and globular clusters, was identified and afterwards eliminated. Taking into account the measured residual variances of not detected globular clusters and background galaxies, an analysis of the power spectrum gave a mean weighted fluctuation magnitude of mI=28.65+-0.04 mag. This result stands in good agreement with the mean weighted fluctuation magnitude of Sodemann & Thomsen (1995) and other values from literature. Using the MI calibrations of Tonry (1991) and Tonry et al. (1997) together with our calculated fluctuation magnitude, distance moduli of (m-M)0=29.85+-0.17 and (m-M)0=30.23+-0.17 were derived, respectively. Adopting a distance modulus of (m-M)0=29.85+-0.17 a distance to the galaxy NGC 3379 of d=9.3 Mpc was determined. Using the distance modulus of (m-M)0=30.23+-0.17 for NGC 3379 a distance of d=11.1 Mpc follows. Both results agree very well with results of other investigations.
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