The Distance to NGC 5253 and the Absolute Magnitude of SN 1972E

Details The Distance to NGC 5253 and the Absolute Magnitude of SN 1972E The Distance to NGC 5253 and the Absolute Magnitude of SN 1972E

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.1304p&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #13.04; Bulletin of the American Astronomical Society, Vol. 24, p.749

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The amorphous irregular galaxy and Centaurus group member, NGC 5253, was the host of the well-observed type Ia supernova 1972E. With the goal of improving the calibration of absolute magnitudes for type Ia supernovae (SNe Ia), we have derived independent distance estimates for NGC 5253 using the planetary nebula luminosity function (PNLF) and surface brightness fluctuations (SBF) methods. From narrow-band [O III]lambda 5007 and Hα images, a statistically-complete sample of only 10 planetary nebulae were identified, yielding a poorly-constrained distance modulus of (m-M)_PNLF = 28.1(+.1}_{-.5) . On the other hand, the halo of NGC 5253 is incipiently resolved in broad-band V and I images, and the SBF method (applied at 60" < r < 120") provides a more accurate estimate of (m-M)_SBF = 27.1 +/- 0.1. The discrepency between these two methods is unprecedented; 14 previous comparisons give an rms dispersion of only 0.18 mag. We interpret the large differential as most likely due to ~ 0.7 mag of extinction due to dust in the inner regions (r < 70") of NGC 5253, where the planetary nebulae were found. The SBF result supports Pierce's (1992) calibration of SNe Ia, and implies MB = -18.7 +/- 0.2 at maximum light.

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