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We present an analysis of ultraviolet (UV) to near-infrared observations ofthe fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by theFornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN2011iv are characterised by dm_15(B) decline-rate values of 1.96 mag and 1.77mag, respectively. Although they have similar decline rates, their peak B- andH-band magnitudes differ by ~0.60 mag and ~0.35 mag, respectively. Aftercorrecting for the luminosity vs. decline rate and the luminosity vs. colourrelations, the peak B-band and H-band light curves provide distances thatdiffer by ~14% and ~9%, respectively. These findings serve as a cautionary talefor the use of transitional SNe Ia located in early-type hosts in the quest tomeasure cosmological parameters. Interestingly, even though SN 2011iv isbrighter and bluer at early times, by three weeks past maximum and extendingover several months, its B-V colour is 0.12 mag redder than that of SN 2007on.To reconcile this unusual behaviour, we turn to guidance from a suite ofspherical one-dimensional Chandrasekhar-mass delayed-detonation explosionmodels. In this context, 56Ni production depends on both the so-calledtransition density and the central density of the progenitor white dwarf. Tofirst order, the transition density drives the luminosity-width relation, whilethe central density is an important second-order parameter. Within thiscontext, the differences in the B-V color evolution along the Lira regimesuggests the progenitor of SN~2011iv had a higher central density thanSN~2007on.

Two transitional type~Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv