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 metallicity. We combine Geneva stellar
evolutionary models with initial masses of Mini=20-120 Msun with
atmospheric/wind models using CMFGEN. We provide synthetic photometry and
high-resolution spectra of hot stars at the pre-SN stage. For Mini=9-20 Msun,
we supplement our analysis using publicly available MARCS model atmospheres of
RSGs. We employ observational criteria of spectroscopic classification and find
that massive stars, depending on Mini and rotation, end their lives as red
supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and
Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we
obtain the following types of SN progenitors: WO1-3 (Mini <= 32 Msun), WN10-11
(25 < Mini < 32 Msun), LBV (20 <= Mini < 25 Msun), G1 Ia+ (18 < Mini < 20
Msun), and RSGs (9 <= Mini <= 18 Msun). For non-rotating models, we find
spectral types WO1-3 (Mini>40 Msun), WN7-8 (25 < Mini <= 40 Msun), WN11h/LBV
(20 < Mini <= 25 Msun), and RSGs (9 <= Mini <= 20 Msun). 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 not necessarily the most massive and
luminous SN progenitors are the brighter ones in a given filter. We show that
SN IIP progenitors (RSGs) are bright in the RIJHK_S filters and faint in the UB
filters. SN IIL/b progenitors (LBVs and YHGs), and SN Ib progenitors (WNs) are
relatively bright in optical/IR filters, while SN Ic progenitors (WOs) are
faint in all optical filters. We argue 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.[abridged]
