Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death

We investigate the fundamental properties of core-collapse Supernova (SN) progenitors from single stars at solar meta llicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of Mini = 20− 120 M⊙ with atmospheric/wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at t he pre-SN stage. For models with Mini = 9− 20 M⊙, we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classifi cation and find that massive stars, depending on their initial mass and rotation , end their lives as red supergiants (RSG), yellow hypergian ts (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the following types of SN progenitors: WO1‐3 (Mini ≥ 32 M⊙), WN10‐11 (25 40 M⊙), WN7‐8 (25< Mini ≤ 40 M⊙), WN11h/LBV (20< Mini ≤ 25 M⊙), and RSGs (9≤ Mini ≤ 20 M⊙). Our rotating models indicate that SN IIP progenitors are all RSG, SN IIL/b progenitors are 56% LBVs and 44% YHGs, SN Ib progenitors are 96% WN10-11 and 4% WOs, and SN Ic progenitors are all WO stars. We find that n ot necessarily the most massive and luminous SN progenitors are the brighter ones in a given filter, since this depends on t heir luminosity, temperature, wind density, and how the spectral energy distribution compares to a filter bandpass. We find that SN IIP progenitors (RSGs) are bright in the RI JHKS filters and faint in the U B filters. SN IIL /b progenitors (LBVs and YHGs), and SN Ib progenitors (WNs) are relatively bright in optical/infrared filters, while SN Ic progenitors (WOs) are faint in all optical filters. We argu e that SN Ib and Ic progenitors from single stars should be undetectable in the available pre-explosion images with the current magnitude limits, in agreement with observational results.

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