Takáts, K.Pignata, G.Pumo, M.L.Paillas, E.Zampieri, L.Elias-Rosa, N.Benetti, S.Bufano, F.Cappellaro, E.Ergon, M.Fraser, M.Hamuy, M.Inserra, C.Kankare, E.Smartt, S.J.Stritzinger, M.D.Van Dyk, S.D.Haislip, J.B.LaCluyze, A.P.Moore, J.P.Reichart, D.2023-06-062023-06-062015-05Monthly Notices of the Royal Astronomical Society Volume 450, Issue 3, Pages 3137 - 315412 May 20150035-8711https://repositorio.unab.cl/xmlui/handle/ria/50371Indexación: ScopusWe present optical and near-infrared photometry and spectroscopy of SN 2009ib, a Type II-P supernova in NGC 1559. This object has moderate brightness, similar to those of the intermediate-luminosity SNe 2008in and 2009N. Its plateau phase is unusually long, lasting for about 130 d after explosion. The spectra are similar to those of the subluminous SN 2002gd, with moderate expansion velocities.We estimate the 56Ni mass produced as 0.046±0.015M⊙. We determine the distance to SN 2009ib using both the expanding photosphere method (EPM) and the standard candle method. We also apply EPM to SN 1986L, a Type II-P SN that exploded in the same galaxy. Combining the results of different methods, we conclude the distance to NGC 1559 as D = 19.8 ± 3.0 Mpc. We examine archival, pre-explosion images of the field taken with the Hubble Space Telescope, and find a faint source at the position of the SN, which has a yellow colour [(V - I)0 = 0.85 mag]. Assuming it is a single star, we estimate its initial mass as MZAMS = 20M⊙. We also examine the possibility, that instead of the yellow source the progenitor of SN 2009ib is a red supergiant star too faint to be detected. In this case, we estimate the upper limit for the initial zero-age main sequence (ZAMS) mass of the progenitor to be ~14-17M⊙. In addition, we infer the physical properties of the progenitor at the explosion via hydrodynamical modelling of the observables, and estimate the total energy as ~0.55 × 1051 erg, the pre-explosion radius as ~400 R⊙, and the ejected envelope mass as ~15M⊙, which implies that the mass of the progenitor before explosion was ~16.5-17M⊙. © 2015 The Authors.enArtículoAtribución 4.0 Internacional (CC BY 4.0)10.1093/mnras/stv857