J/ApJ/791/105 SNe progenitor masses probability distribution (Williams+, 2014)
Constraints for the progenitor masses of 17 historic core-collapse supernovae.
Williams B.F., Peterson S., Murphy J., Gilbert K., Dalcanton J.J.,
Dolphin A.E., Jennings Z.G.
<Astrophys. J., 791, 105 (2014)>
=2014ApJ...791..105W 2014ApJ...791..105W (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Stars, masses ; Models
Keywords: stars: evolution - stars: massive - supernovae: general
Abstract:
Using resolved stellar photometry measured from archival Hubble Space
Telescope imaging, we generate color-magnitude diagrams of the stars
within 50 pc of the locations of historic core-collapse supernovae
(SNe) that took place in galaxies within 8 Mpc. We fit these
color-magnitude distributions with stellar evolution models to
determine the best-fit age distribution of the young population. We
then translate these age distributions into probability distributions
for the progenitor mass of each SN. The measurements are anchored by
the main-sequence stars surrounding the event, making them less
sensitive to assumptions about binarity, post-main-sequence evolution,
or circumstellar dust. We demonstrate that, in cases where the
literature contains masses that have been measured from direct
imaging, our measurements are consistent with (but less precise than)
these measurements. Using this technique, we constrain the progenitor
masses of 17 historic SNe, 11 of which have no previous estimates from
direct imaging. Our measurements still allow the possibility that all
SN progenitor masses are <20 M☉. However, the large
uncertainties for the highest-mass progenitors also allow the
possibility of no upper-mass cutoff.
Description:
We selected all positively typed historic core-collapse SNe within
8 Mpc that also have ∼arcsecond accuracy in their positions from the
Asiago Supernova Catalog (Barbon et al. 1999A&AS..139..531B 1999A&AS..139..531B, cat B/sn);
higher positional accuracy is not needed, due to the large size of the
aperture within which the color-magnitude diagram (CMD) is
constructed. We cross-referenced the SN catalog with the HST archive
and identified SNe that have HST imaging in at least two broadband
filters in ACS, WFPC2, or UVIS. Even relatively shallow data can
provide constraints given that, for the most massive ∼50 M☉
progenitors, the surrounding populations are likely to have other very
massive stars with MV←5. We found 22 SNe that match these
requirements.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 85 22 SN Sample
table3.dat 34 187 Probability distributions, with associated
uncertainties, for our sample
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/MNRAS/395/1409 : Type II-P SN progenitor constraints (Smartt+, 2009)
J/MNRAS/436/774 : Core collapse supernovae (type Ibc) (Eldridge+, 2013)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- SN Name of SN
10- 14 A5 --- Type Spectral type of the SN
16- 17 I2 h RAh Hour of Right Ascension (J2000)
19- 20 I2 min RAm Minute of Right Ascension (J2000)
22- 26 F5.2 s RAs Second of Right Ascension (J2000)
28 A1 --- DE- Sign of the Declination (J2000)
29- 30 I2 deg DEd Degree of Declination (J2000)
32- 33 I2 arcmin DEm Arcminute of Declination (J2000)
35- 39 F5.2 arcsec DEs Arcsecond of Declination (J2000)
41- 53 A13 --- Galaxy Host galaxy of the SN (NGC NNNN)
55- 59 I5 --- PID Program identification number of the HST data
used for our photometry (NNNNN)
61- 64 F4.1 mag Mod Distance modulus to the galaxy
66- 69 F4.2 Mpc Dist Distance to the galaxy
71- 75 F5.3 mag ext ?=- Foreground extinction to the SN
77- 79 F3.1 mag diffext ?=- Differential extinction applied to our
model fits
81- 85 I5 --- Nstar Number of star in our photometry within
the physical radius of 50 pc
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- SN Supernova identifier
10- 13 F4.1 Msun B_Mass Upper mass limit of mass bin
15- 18 F4.1 Msun b_Mass Lower mass limit of mass bin
20- 24 F5.1 --- Prob Most likely percentage (1)
26- 29 F4.1 --- E_Prob Upper 1σ uncertainty in Prob
31- 34 F4.1 --- e_Prob Lower 1σ uncertainty in Prob
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Note (1): Of stellar mass (<50 Myr) in the mass bin.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 30-Mar-2017