Pulsars, transients and relativistic astrophysics

Research group

Research theme

Sub department

About

Inverse Compton X-ray halos around high-z radio galaxies: A feedback mechanism powered by far-infrared starbursts or the CMB?

(2012)

Authors:

Ian Smail, Katherine M Blundell, BD Lehmer, DM Alexander

Stellar transits in active galactic nuclei

(2012)

Authors:

Bence B茅ky, Bence Kocsis

The host galaxy of the super-luminous SN 2010gx and limits on explosive nickel-56 production

(2012)

Authors:

Ting-Wan Chen, Stephen J Smartt, Fabio Bresolin, Andrea Pastorello, Rolf-Peter Kudritzki, Rubina Kotak, Matt McCrum, Morgan Fraser, Stefano Valenti

Interacting Supernovae and Supernova Impostors. SN 2009ip, is this the end?

(2012)

Authors:

A Pastorello, E Cappellaro, C Inserra, SJ Smartt, G Pignata, S Benetti, S Valenti, M Fraser, K Takats, S Benitez, MT Botticella, J Brimacombe, F Bufano, F Cellier-Holzem, MT Costado, G Cupani, I Curtis, N Elias-Rosa, M Ergon, JPU Fynbo, F-J Hambsch, M Hamuy, A Harutyunyan, KM Ivarson, E Kankare, JC Martin, R Kotak, AP LaCluyze, K Maguire, S Mattila, J Maza, M McCrum, M Miluzio, HU Norgaard-Nielsen, MC Nysewander, P Ochner, Y-C Pan, ML Pumo, DE Reichart, TG Tan, S Taubenberger, L Tomasella, M Turatto, D Wright

The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling

Astronomy and Astrophysics 546 (2012)

Authors:

A Jerkstrand, C Fransson, K Maguire, S Smartt, M Ergon, J Spyromilio

Abstract:

SN 2004et is one of the nearest and best-observed Type IIP supernovae, with a progenitor detection as well as good photometric and spectroscopic observational coverage well into the nebular phase. Based on nucleosynthesis from stellar evolution/explosion models we apply spectral modeling to analyze its 140-700 day evolution from ultraviolet to mid-infrared. We find a M ZAMS = 15 M 芒艩(tm) progenitor star (with an oxygen mass of 0.8 M 芒艩(tm)) to satisfactorily reproduce [O芒鈥癷] 位位6300, 6364 and other emission lines of carbon, sodium, magnesium, and silicon, while 12 M 芒艩(tm) and 19 M 芒艩(tm) models under-and overproduce most of these lines, respectively. This result is in fair agreement with the mass derived from the progenitor detection, but in disagreement with hydrodynamical modeling of the early-time light curve. From modeling of the mid-infrared iron-group emission lines, we determine the density of the "Ni-bubble" to 蟻(t) 芒鈥7 脳 10 -14 脳 (t/100 d) -3 g cm -3, corresponding to a filling factor of f = 0.15 in the metal core region (V = 1800 km芒鈥 s -1). We also confirm that silicate dust, CO, and SiO emission are all present in the spectra. 漏2012 ESO.