Details

Autor(en) / Beteiligte

• Hakobyan, A. A
• Karapetyan, A. G
• Barkhudaryan, L. V
• Mamon, G. A
• Kunth, D
• Petrosian, A. R
• Adibekyan, V
• Aramyan, L. S
• Turatto, M

Titel

Supernovae and their host galaxies – III. The impact of bars and bulges on the radial distribution of supernovae in disc galaxies

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2016-03, Vol.456 (3), p.2848-2860

Ort / Verlag

London: Oxford University Press

Erscheinungsjahr

2016

Link zum Volltext

Quelle

Elektronische Zeitschriftenbibliothek (Open access)

Beschreibungen/Notizen

• We present an analysis of the impact of bars and bulges on the radial distributions of the different types of supernovae (SNe) in the stellar discs of host galaxies with various morphologies. We use a well-defined sample of 500 nearby (≤100 Mpc) SNe and their low-inclined (i ≤ 60°) and morphologically non-disturbed S0–Sm host galaxies from the Sloan Digital Sky Survey. We find that in Sa–Sm galaxies, all core-collapse (CC) and vast majority of SNe Ia belong to the disc, rather than the bulge component. The radial distribution of SNe Ia in S0–S0/a galaxies is inconsistent with their distribution in Sa–Sm hosts, which is probably due to the contribution of the outer bulge SNe Ia in S0–S0/a galaxies. In Sa–Sbc galaxies, the radial distribution of CC SNe in barred hosts is inconsistent with that in unbarred ones, while the distributions of SNe Ia are not significantly different. At the same time, the radial distributions of both types of SNe in Sc–Sm galaxies are not affected by bars. We propose that the additional mechanism shaping the distributions of Type Ia and CC SNe can be explained within the framework of substantial suppression of massive star formation in the radial range swept by strong bars, particularly in early-type spirals. The radial distribution of CC SNe in unbarred Sa–Sbc galaxies is more centrally peaked and inconsistent with that in unbarred Sc–Sm hosts, while the distribution of SNe Ia in unbarred galaxies is not affected by host morphology. These results can be explained by the distinct distributions of massive stars in the discs of early- and late-type spirals.