Bibcode
Vinkó, J.; Takáts, K.; Szalai, T.; Marion, G. H.; Wheeler, J. C.; Sárneczky, K.; Garnavich, P. M.; Kelemen, J.; Klagyivik, P.; Pál, A.; Szalai, N.; Vida, K.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 540, id.A93, 7 pp.
Fecha de publicación:
4
2012
Revista
Número de citas
46
Número de citas referidas
42
Descripción
Aims: The appearance of two recent supernovae, SN 2011dh and
2005cs, both in M 51, provides an opportunity to derive an improved
distance to their host galaxy by combining the observations of both SNe.
Methods: We apply the Expanding Photosphere Method to get the
distance to M 51 by fitting the data of these two SNe simultaneously. In
order to correct for the effect of flux dilution, we use correction
factors (ζ) appropriate for standard type II-P SNe atmospheres for
2005cs, but find ζ ~ 1 for the type IIb SN 2011dh, which may be due
to the reduced H-content of its ejecta. Results: The EPM analysis
resulted in DM 51 = 8.4 ± 0.7 Mpc. Based on this
improved distance, we also re-analyze the HST observations of the
proposed progenitor of SN 2011dh. We confirm that the object detected on
the pre-explosion HST-images is unlikely to be a compact stellar
cluster. In addition, its derived radius (~277 R⊙) is too
large for being the real (exploded) progenitor of SN 2011dh.
Conclusions: The supernova-based distance, D = 8.4 Mpc, is in good
agreement with other recent distance estimates to M 51.