J/MNRAS/395/1409 Type II-P SN progenitor constraints (Smartt+, 2009)
The death of massive stars.
I. Observational constraints on the progenitors of type II-P supernovae.
Smartt S.J., Eldridge J.J., Crockett R.M., Maund J.R.
<Mon. Not. R. Astron. Soc., 395, 1409-1437 (2009)>
=2009MNRAS.395.1409S 2009MNRAS.395.1409S
ADC_Keywords: Supernovae
Keywords: stars: evolution - supergiants - supernovae: general -
galaxies: stellar content
Abstract:
We present the results of a 10.5-yr, volume-limited (28-Mpc) search
for supernova (SN) progenitor stars. In doing so we compile all SNe
discovered within this volume (132, of which 27 per cent are Type Ia)
and determine the relative rates of each subtype from literature
studies. The core-collapse SNe break down into 59 per cent II-P and 29
per cent Ib/c, with the remainder being IIb (5 per cent), IIn (4 per
cent) and II-L (3 per cent). There have been 20 II-P SNe with
high-quality optical or near-infrared pre-explosion images that allow
a meaningful search for the progenitor stars. In five cases they are
clearly red supergiants, one case is unconstrained, two fall on
compact coeval star clusters and the other twelve have no progenitor
detected. We review and update all the available data for the host
galaxies and SN environments (distance, metallicity and extinction)
and determine masses and upper mass estimates for these 20 progenitor
stars using the stars stellar evolutionary code and a single
consistent homogeneous method. A maximum likelihood calculation
suggests that the minimum stellar mass for a Type II-P to form is
mmin= 8.5+1-1.5M☉ and the maximum mass for II-P
progenitors is mmax= 16.5±1.5M☉, assuming a Salpeter
initial mass function holds for the progenitor population (in the
range Γ=-1.35+0.3-0.7). The minimum mass is consistent
with current estimates for the upper limit to white dwarf progenitor
masses, but the maximum mass does not appear consistent with massive
star populations in Local Group galaxies. Red supergiants in the Local
Group have masses up to 25M☉ and the minimum mass to produce a
Wolf-Rayet star in single star evolution (between solar and LMC
metallicity) is similarly 25-30M☉. The reason we have not
detected any high-mass red supergiant progenitors above 17M☉ is
unclear, but we estimate that it is statistically significant at
2.4σ confidence. Two simple reasons for this could be that we
have systematically underestimated the progenitor masses due to dust
extinction or that stars between 17-25M☉produce other kinds of
SNe which are not II-P. We discuss these possibilities and find that
neither provides a satisfactory solution. We term this discrepancy the
'red supergiant problem' and speculate that these stars could have
core masses high enough to form black holes and SNe which are too
faint to have been detected. We compare the 56Ni masses ejected in
the SNe to the progenitor mass estimates and find that low-luminosity
SNe with low 56Ni production are most likely to arise from
explosions of low-mass progenitors near the mass threshold that can
produce a core-collapse.
Description:
The observational data for this paper are compiled from many sources
in the recent literature but the sample selection requires some
justification and explanation if the later comparisons and discussions
of physical parameters are to be meaningful. We have selected SNe for
inclusion based on the following selection criteria, and we justify
the choice of criteria where appropriate.
We consider all core collapse SNe discovered in the 10.5 yr period
between 1998 January 1 and 2008 June 30.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 157 141 SNe discovered between 1998-2008.5 in galaxies
with recessional velocities less than 2000km/s
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
II/256 : Sternberg Supernova Catalogue, 2004 version (Tsvetkov+, 2004)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Class Type of supernovae: "Core-collapse", "Type Ia",
"Unclassified" or "Uncertain")
15- 29 A15 --- SN Supernova name
32- 42 A11 --- Gal Host galaxy name
45- 50 F6.1 km/s Vvir [-79/2283] Radial velocity of the host galaxy,
corrected for the local group infall into Virgo
52- 61 A10 --- Type Type of supernovae (or LBV)
64- 66 A3 --- HST Notes if the host galaxy has been observed by HST
prior to explosion and if the position of the SN
is "in" or "out" of the camera field-of-view
68-157 A90 --- Com Comments (1)
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Note (1): Individual notes:
a = http://etacar.umn.edu/etainfo/related/
b = SNe 2002ao and 2006jc have been termed Ibn as they show narrow He lines
due to circumstellar He rich shells. We discuss in Sect. 2.1 why we
use Ic rather than Ibn
c = http://www.supernovae.net/sn2004/sn2004gn.jpg
d = Although Vvir outside limit, the TF/SBF distance from Tonry et al.
(2000ApJ...530..625T 2000ApJ...530..625T) puts it within our distance limit and it will be
included in the stripped progenitor study of Crockett et al. in prep
e = SNe 2002ao and 2006jc have been termed Ibn as they show narrow He lines
due to circumstellar He rich shells. We discuss in Sect. 2.1 why we use
Ic rather than Ibn
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 13-Jul-2015