2013A&A...558A.131G


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.21CEST16:15:02

2013A&A...558A.131G - Astronomy and Astrophysics, volume 558A, 131-131 (2013/10-1)

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

GROH J.H., MEYNET G., GEORGY C. and EKSTROEM S.

Abstract (from CDS):

We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of Mini=20-120M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with Mini=9-20M, 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 classification and find that, depending on their initial mass and rotation, massive stars 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 obtained the following types of SN progenitors: WO1-3 (Mini≥32M), WN10-11 (25<Mini<32M), LBV (20≤Mini≤25M), G1 Ia+ (18<Mini<20M), and RSGs (9≤Mini≤18M). For non-rotating models, we found spectral types WO1-3 (Mini>40M), WN7-8 (25<Mini≤40M), WN11h/LBV (20<Mini≤25M), and RSGs (9≤Mini≤20M). 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 the most massive and luminous SN progenitors are not necessarily the brightest ones in a given filter, since this depends on their luminosity, temperature, wind density, and the way the spectral energy distribution compares to a filter bandpass. We find that SN IIP progenitors (RSGs) are bright in the RIJHKS filters and faint in the UB 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 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.

Abstract Copyright:

Journal keyword(s): stars: evolution - supernovae: general - stars: massive - stars: winds, outflows - gamma-ray burst: general - stars: rotation

VizieR on-line data: <Available at CDS (J/A+A/558/A131): listsp.dat sp/* spn/*>

Simbad objects: 60

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Number of rows : 60

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 SN 2005gl SN* 00 49 50.02 +32 16 56.8       17.0   SN.IIn 120 2
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9092 1
3 SN 2002ap SN* 01 36 23.85 +15 45 13.2   13.11 14.54     SN.Ic-bl 482 1
4 SN 2003gd SN* 01 36 42.65 +15 44 19.9     13.2     SN.IIP 211 2
5 SN 2006gy SN* 03 17 27.06 +41 24 19.5       14.20   SN.IIn 272 1
6 SN 2001du SN* 03 33 29.11 -36 08 32.5     14.0     SN.IIP 46 1
7 SN 2003bg SN* 04 10 59.42 -31 24 50.3     15.0     SNIc 121 1
8 SN 1999em SN* 04 41 27.04 -02 51 45.2   13.79 13.7     SN.IIP 556 1
9 SN 2001B SN* 04 57 19.24 +78 11 16.5     15.0     SNIb 37 1
10 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14327 1
11 SN 2006bc SN* 07 21 16.50 -68 59 57.3   17.6 16.0     SN.IIP 37 1
12 SN 2006jc SN* 09 17 20.78 +41 54 32.7     13.8     SN.Ib-n 252 1
13 SN 2010jl SN* 09 42 53.33 +09 29 41.8           SN.IIn 174 1
14 SN 1999gi SN* 10 18 16.66 +41 26 28.2   14.8       SN.IIP 195 1
15 HD 90177 s*b 10 22 53.8426931454 -59 37 28.361118869 9.16 9.66 8 8.15   LBV 300 0
16 SN 2012aw SN* 10 43 53.735 +11 40 17.63       15   SNIIP 127 1
17 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2148 0
18 SN 2009md SN* 10 48 26.28 +12 32 02.8           SN.IIP 45 2
19 WRAY 15-682 WR* 10 53 59.5776214569 -60 26 44.358376205   11.64 10.85 10.56   WN11h 133 3
20 V* AG Car WR* 10 56 11.5779283438 -60 27 12.809532379 7.00 7.57 6.96 7.73   WN11h 580 0
21 SN 2009hd SN* 11 20 16.99 +12 58 46.3           SN.II 45 1
22 SN 2007aa SN* 12 00 27.69 -01 04 51.6 16.9 16.4 5.8     SN.IIP 46 1
23 SN 2004gt SN* 12 01 50.37 -18 52 12.7   19.42 14.9     SNIc 61 1
24 SN 2010br SN* 12 03 10.95 +44 31 43.1           SN.Ib/c 16 1
25 SN 2003ie SN* 12 03 18.15 +44 31 34.6     15.2     SN.IIP 31 1
26 SN 2011am SN* 12 16 26.00 -43 19 20.0           SNIb 7 1
27 SN 2008ax SN* 12 30 40.80 +41 38 16.1   23.6 23.5 14.1 22.6 SN.IIb 199 1
28 SN 2006my SN* 12 43 40.74 +16 23 14.1     15.3     SN.IIP 40 1
29 SN 2012au SN* 12 54 52.18 -10 14 50.2           SNIb 32 2
30 SN 1999br SN* 13 00 41.80 +02 29 45.8     17.5     SN.IIPp 145 1
31 SN 2005cs SN* 13 29 53.37 +47 10 28.2   14.5       SN.IIP 313 1
32 SN 2004dg SN* 14 59 58.96 +01 53 25.6     17.1     SN.IIP 25 1
33 Cl* Westerlund 1 BKS H * 16 47 01.4273629136 -45 50 37.260634424   18.781 14.47     F3Ia+ 21 0
34 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 442 0
35 Cl* Westerlund 1 W 243 s*b 16 47 07.5028508821 -45 52 29.152464693   19.873 15.730     LBV 48 0
36 HD 326823 Be* 17 06 53.9048235955 -42 36 39.705015741 9.68 9.87 9.03 9.51   O 70 0
37 WR 93b WR* 17 32 03.3085935721 -35 04 32.618191778           WO3 14 0
38 [B61] 2 s*b 17 41 35.4374195439 -30 06 38.782935913   18.0 15.00 14.23 10.30 LBV_B[e]: 43 0
39 HD 160529 sg* 17 41 59.0257256544 -33 30 13.702939546 8.17 7.87 6.66 5.50 4.51 A2Ia 182 1
40 V* V3893 Sgr WR* 17 45 47.5403190596 -26 10 26.777772852   15.13 14.20 14.23   WR 105 1
41 [FMM95] 3 Em* 17 46 15.240 -28 50 03.58           ~ 133 1
42 [GMC99] D6 * 17 46 17.982 -28 49 03.46           ~ 51 0
43 WR 102ka WR* 17 46 18.12 -29 01 36.6           WN10 27 0
44 HD 316285 s*b 17 48 14.0369781568 -28 00 53.124817157 11.88 11.27 9.60 9.28   B0Ieq 177 2
45 HD 168607 s*b 18 21 14.8855350307 -16 22 31.760520819 10.23 9.82 8.28 8.55   B9Iaep 171 1
46 HD 168625 s*b 18 21 19.5486475779 -16 22 26.077308888 10.15 9.78 8.37 8.76   B6Iap 246 2
47 V* V481 Sct s*b 18 33 55.2778598542 -06 58 38.634278867           LBV_B[e]: 42 0
48 MR 89 WR* 18 41 00.8669826586 -04 26 14.473452479 13.1 12.97 11.93 11.67   WN7 64 2
49 IRAS 18576+0341 s*b 19 00 10.89456 +03 45 47.1096           B8I 80 1
50 HD 177230 WR* 19 03 59.0232385542 -04 19 01.911120922 11.32 11.60 11.12     WN8 156 0
51 BD+14 3887 Em* 19 21 33.9773483922 +14 52 56.908316938 11.86 11.3 9.89     B3Ibe 76 0
52 [OMN2000] LS1 Em* 19 23 47.6416797701 +14 36 39.064626755     15.1     O4I 17 0
53 IRC +10420 pA* 19 26 48.0981288433 +11 21 16.756524951   13.98 11.66     F8Ia+e 448 0
54 * P Cyg s*b 20 17 47.2020844 +38 01 58.552724 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1125 1
55 WR 142 WR* 20 21 44.3438534563 +37 22 30.543604467   14.39 12.99 12.73 11.04 WO2 119 0
56 IRAS 20298+4011 Em* 20 31 42.2841507943 +40 21 59.061205285     15.1     B:I[e] 82 0
57 SN 2002hh SN* 20 34 44.29 +60 07 19.0     17.18     SN.IIP 128 1
58 SN 2009ip s*b 22 23 08.26 -28 56 52.4           LBV 245 0
59 SN 2001ig SN* 22 57 30.69 -41 02 25.9     14.5     SN.IIb 134 1
60 * rho Cas LP* 23 54 23.0339951270 +57 29 57.766930774 7.00 5.85 4.59 3.63 2.89 G2_0 357 0

    Equat.    Gal    SGal    Ecl

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2019.10.21-16:15:02

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