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Title:
SN 1994D -- an Overluminous Type IA Supernova ?
Authors:
Drenkhahn, G.; Richtler, T.
Affiliation:
AA(Sternwarte der Universitaet Bonn, Auf dem Huegel 71, D-53121 Bonn, Germany), AB(Sternwarte der Universitaet Bonn, Auf dem Huegel 71, D-53121 Bonn, Germany)
Publication:
Astronomische Gesellschaft Meeting Abstracts, Abstracts of Contributed Talks and Posters presented at the Annual Scientific Meeting of the Astronomische Gesellschaft at Heidelberg, September 14--19, 1998, poster #P95
Publication Date:
00/1998
Origin:
AG
Bibliographic Code:
1998AGM....14..P95D

Abstract

The S0 galaxy NGC 4526 in the Virgo Cluster hosted the well observed type Ia supernova 1994D. Richmond et al. (1995, AJ 109,2121) quote a brightness excess of ~ 0.5 mag with respect to SN 1980N and SN 1989B, thus questioning the standard candle paradigm for type Ia SNe. Tammann & Sandage (1996, ApJ 452,16) compare SN 1994D with other Virgo Cluster SNe and find it too bright by only ~ 0.25 mag, rendering the decline-rate-luminosity relation (Hamuy et al. 1996, AJ 112,2398) unreliable, because correcting for this effect would enlarge the difference to other SNe. However, an individual distance determination has not yet published. In this work we analyse archival HST images in order to determine the distance using the Globular Cluster Luminosity Function (GCLF). We identify 110 cluster candidates by applying colour and shape selection criteria. A maximum likelihood analysis is carried out and limits the turn-over magnitude to m^0_V <= 23.16+/- 0.11 (internal error). Taking the absolute turn-over magnitude of the galactic globular cluster system of M^0_V=-7.54+/- 0.11, we find a distance modulus of \mu <= 30.7+/- 0.16. Adopting for SN 1992A and SN 1980N the Fornax cluster distance derived with GCLFs (Kohle et al. 1998, A&A 309,L39; Della Valle et al. 1998, MNRAS in press) results in excellent agreement between the decline-rate and colour corrected absolute magnitudes of SN 1994D and the Fornax SNe. Thus, SN 1994D fits both the GCLF distance scale as well as the decline rate-luminosity relation.
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