J/ApJ/881/54 Masses of SNR progenitors in M83 (Williams+, 2019)
The masses of supernova remnant progenitors in M83.
Williams B.F., Hillis T.J., Blair W.P., Long K.S., Murphy J.W., Dolphin A.,
Khan R., Dalcanton J.J.
<Astrophys. J., 881, 54 (2019)>
=2019ApJ...881...54W 2019ApJ...881...54W
ADC_Keywords: Supernova remnants; Photometry, HST; Reddening; Stars, masses;
Optical; X-ray sources; Cross identifications
Keywords: galaxies: individual (M83) ; stars: evolution ; stars: massive ;
supernovae: general
Abstract:
We determine the ages of the young, resolved stellar populations at
the locations of 237 optically identified supernova remnants in M83.
These age distributions put constraints on the progenitor masses of
the supernovae that produced 199 of the remnants. The other 38 show no
evidence for having a young progenitor and are therefore good Type Ia
SNR candidates. Starting from Hubble Space Telescope broadband
imaging, we measured resolved stellar photometry of seven archival
WFC3/UVIS fields in F336W, F438W, and F814W. We generate
color-magnitude diagrams of the stars within 50pc of each SNR and fit
them with stellar evolution models to obtain the population ages. From
these ages we infer the progenitor mass that corresponds to the
lifetime of the most prominent age within the past 50Myr. In this
sample, there are 47 SNRs with best-fit progenitor masses >15M☉,
and 5 of these are >15M☉ at 84% confidence. This is the largest
collection of high-mass progenitors to date, including our
highest-mass progenitor inference found so far, with a constraint of
<8Myr. Overall, the distribution of progenitor masses has a power-law
index of -3.0-0.7+0.2, steeper than Salpeter initial mass function
(-2.35). It remains unclear whether the reason for the low number of
high-mass progenitors is due to the difficulty of finding and
measuring such objects or because only a fraction of very massive
stars produce supernovae.
Description:
We analyze HST observations of seven WFC3/UVIS fields in three filters
F336W, F438W, and F814W covering most of the high surface brightness
portion of M83. These observations (taken between 2009-Aug-20 and
2012-Sep-06) are described in detail in Blair+ (2014, J/ApJ/788/55).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 64 307 M83 supernova remnants
table2.dat 52 199 SNR photometry depth, extinction, and
progenitor mass estimates
table3.dat 104 4378 Age distribution results for the 199 remnants
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
J/ApJ/695/580 : Oxygen abundance in M83 (Bresolin+, 2009)
J/ApJ/703/614 : UV star-forming regions in M31 (Kang+, 2009)
J/MNRAS/395/1409 : Type II-P SN progenitor constraints (Smartt+, 2009)
J/AJ/144/142 : HST photometry of young stellar pop. in M31 (Bianchi+, 2012)
J/ApJS/203/8 : Optical SNR candidates in M83 (Blair+, 2012)
J/ApJ/788/55 : HST/WFC3 SNR discoveries in M83 (NGC5236) (Blair+, 2014)
J/ApJ/795/170 : Sample SNRs for M31 and M33 (Jennings+, 2014)
J/ApJS/212/21 : A deep Chandra ACIS survey of M83 (Long+, 2014)
J/ApJS/215/9 : PHAT X. UV-IR photometry of M31 stars (Williams+, 2014)
J/ApJ/791/105 : SNe progenitor masses prob. distribution (Williams+, 2014)
J/A+A/593/A68 : PTF12os & iPTF13bvn spectra & light curves (Fremling+, 2016)
J/ApJ/846/145 : PHAT. XIX. Formation history of M31 disk (Williams+, 2017)
J/ApJ/839/83 : GMOS spectroscopic obs. of SNR cand. in M83 (Winkler+, 2017)
J/ApJ/860/39 : HST obs. of nearby core-collapse SNe (Williams+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- SNR Source identifier in this work
9- 12 A4 --- --- [B12-]
13- 16 A4 --- [BWL2012] Blair+ 2012, J/ApJS/203/8 identifier;
except 174a (1)
18- 21 A4 --- --- [B14-]
22- 23 I2 --- [BCD2014] ? Blair+ 2014, J/ApJ/788/55 identifier
25- 28 A4 --- --- [D10-]
29- 32 A4 --- [DBL2010] Dopita+ 2010ApJ...710..964D 2010ApJ...710..964D identifier
(<[DBL2010] M83-SNR-1-NN> or
<[DBL2010] M83-SNR-N-NN> or
<[DBL2010] M83-SRC-1-ON> in Simbad)
34- 37 A4 --- [LKB2014] Long+ 2014, J/ApJS/212/21 X-ray identifier
39- 48 F10.6 deg RAdeg [204.16/204.33] Right Ascension (J2000)
50- 59 F10.6 deg DEdeg [-29.96/-29.77] Declination (J2000)
61- 62 A2 --- Qual Quality Flag (2)
64 A1 --- Use Use Flag (3)
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Note (1): An additional young SNR that may represent an unobserved SN in the
last century, SNR 238 (B12-174a), is included in the sample
(Blair+ 2015ApJ...800..118B 2015ApJ...800..118B ; <[BWL2015] B12-174a> in Simbad).
See Section 2.1.
Note (2): Quality flag as follows:
1a = Optical imaging candidate confirmed by spectroscopy and having
X-ray emission (48 occurrences).
1b = Optical imaging candidate strongly confirmed by optical spectroscopy
(e.g. spectroscopic [SII]:Hα>0.5) but no X-ray detection
(52 occurrences).
1c = Optical imaging candidate with photometric [SII]:Hα>0.5 but no
optical spectral confirmation available and no X-ray detection
(61 occurrences).
1d = Optical imaging candidate with X-ray but no spectra available
(22 occurrences).
1e = Optical imaging candidate with X-ray but marginal spectral ratio
(likely due to HII contamination; 6 occurrences).
1f = Solid imaging candidate, no X-ray, but with clear HII contamination
in spectrum (2 occurrences).
1g = Strong HST [FeII] 1.64um candidate (9 occurrences).
1h = HST Nuclear candidates (mostly Dopita+ 2010ApJ...710..964D 2010ApJ...710..964D) with no
additional supporting evidence (11 occurrences).
1z = Special cases (3 occurrences).
2 = Optical candidate with imaging or spectroscopic ratio
0.25<[SII]:Hα<0.5. Many of these are likely SNRs, but HII
contamination causes uncertainty. Some have detectable [FeII],
which strengthens their case (87 occurrences).
h = Historical supernova (event was observed; 6 occurrences).
Note (3): Use flag which indicates how each SNR was used (p) or not used in
the analysis as follows:
p = Progenitor mass constrained from measured local young population
(199 occurrences).
n = No young population detected in the fit (Type Ia candidate).
o = Outside of the HST coverage; no measurement performed.
c = Too close to the center of M83; no measurement performed.
i = Insufficient photometry for a measurement; fitting failed.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- SNR SNR identifier in this work
9- 12 F4.1 mag F336W [25.5/26.5] The 50% completeness magnitude
in HST/WFC3 F336W filter
14- 17 F4.1 mag F438W [26.4/27.3] The 50% completeness magnitude
in HST/WFC3 F438W filter
19- 22 F4.1 mag F814W [25.1/26.3] The 50% completeness magnitude
in HST/WFC3 F814W filter
24- 26 I3 --- Ns [27/945] Number of stars extracted
in F438W filter data
28- 30 F3.1 mag dAv [0/3] Best differential reddening (1)
32- 34 F3.1 mag Av [0.2/3.2] Best reddening (1)
36- 40 F5.2 Msun MZAMS [7.5/60] Zero Age Main Sequence mass
42- 46 F5.2 Msun E_MZAMS [0.17/54] Upper uncertainty in MZAMS
48- 52 F5.2 Msun e_MZAMS [0.13/46] Lower uncertainty in MZAMS
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Note (1): Applied during the fitting process.
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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- 7 A7 --- SNR SNR identifier in this work
9- 12 F4.1 Myr T1 [4/44.7] Lower age bin value
14- 17 F4.1 Myr T2 [4.5/50.1] Upper age bin value
19- 28 E10.4 Msun/yr SFR [0/66500000] Best star formation rate
29 A1 --- f_SFR i: value "4.4844e-67" has been set
to "0" by CDS
31- 40 E10.4 Msun/yr e_SFR [0/66500000] Lower uncertainty in SFR
41 A1 --- feSFR i: value "4.4844e-67" has been set
to "0" by CDS
43- 52 E10.4 Msun/yr E_SFR [0/90575000] Upper uncertainty in SFR
54- 58 F5.3 --- PDF [0/1] Best fraction of <50Myr stellar mass
60- 64 F5.3 --- e_PDF [0/1] Lower uncertainty in PDF
66- 70 F5.3 --- E_PDF [0/1] Upper uncertainty in PDF
72- 76 F5.3 --- CDF [0/1] Best running cumulative fraction of
stellar mass
78- 82 F5.3 --- e_CDF [0/1]? Monte Carlo resampling estimate of
the 16% percentile in CDF
84- 88 F5.3 --- CDF50 [0/1]? Monte Carlo resampling estimate of
the 50% percentile in CDF
90- 94 F5.3 --- E_CDF [0/1]? Monte Carlo resampling estimate of
the 84% percentile in CDF
96- 99 F4.1 Msun M1 [7.3/52.1] Mass corresponding to T1
101-104 F4.1 Msun M2 [7.7/66.6] Mass corresponding to T2
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 22-Jan-2021