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Recent Progress in Young Galactic* SNRs
Brian J. Williams (NASA GSFC / USRA)@bjwilli2
*(plus some LMC stuff, too)
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I. Kinematics of SNRs- More and more papers coming out on proper
motions from SNRs
- As t increases, this gets easier and easier to do in the era of high spatial resolution astronomy (JVLA, Hubble, ground-based optical, Chandra)
- But not just proper motions! Spectral information gives info on line-of-sight velocity as well…
- How does all of this translate into increased knowledge of SNRs and their progenitors?
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Chandra - 2000, 2003, 2007, 2009, 2015
Tycho’s SNR
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Chandra - 2000, 2003, 2007, 2009, 2015
Tycho’s SNR
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Chandra - 2000, 2003, 2007, 2009, 2015
VLA - 1984, 1993, 2002,
2014
Tycho’s SNR
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Williams et al. 2013 measured densities of surrounding ISM, found evidence of density gradient
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Reynoso et al. 1997, 10-yr baselineKatsuda et al. 2010, 7-yr baseline
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Plot from Williams et al. 2016, 15-yr baseline in X-rays, 30-yr in radio!
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“But wait! Tycho is circular…”
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Center, Ruiz-Lapuente et al.
2004
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Center, Ruiz-Lapuente et al.
2004
Explosion site, Williams et al.
2016
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Center, Ruiz-Lapuente et al.
2004
Explosion site, Williams et al.
2016
Explosion site, Xue & Schaefer
2015
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Center, Ruiz-Lapuente et al.
2004
Explosion site, Williams et al.
2016
Explosion site, Xue & Schaefer
2015
“Star G,” Ruiz-Lapuente et al.
2004
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- Just because a remnant is circular, doesn’t mean the explosion site and geometric center are the same
- Effect is “only” ~10% for Tycho, but Tycho is dynamically young! Older remnants will show larger effects…
- See further talks on Tycho kinematics by Frank Winkler and Jack Hughes
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RCW 86- Recent paper by Yamaguchi et al.
2016 derives proper motions for nonthermal (1800-3000 km/s) and thermal filaments (720 km/s)
- thermal velocities comparable to those reported by Helder et al. 2013 for optical Hα filaments
- consistent with predictions of Williams et al. 2011 that RCW 86 exploded in bubble, nonthermal rims are where shock hasn’t yet hit bubble wall; see D. Castro talk for physics of synchrotron emission
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G1.9+0.3
Radio image, 1984
X-ray image, 2007
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G1.9+0.3
Radio image, 1984
X-ray image, 2007
Reynolds et al. 2008
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G1.9+0.3 is by far the youngest remnant in the Milky Way, age ~120 years (but no way it could
have been seen from Earth at that time)
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G1.9+0.3 is by far the youngest remnant in the Milky Way, age ~120 years (but no way it could
have been seen from Earth at that time)
Lots of great science…
- Radio flux is still brightening, (Green et al. 2008)
- Overwhelmingly synchrotron-dominated, but spectral variations from place to place (Reynolds et al. 2009)
- Ejecta detected, asymmetrically-distributed, moving up to 18,000 km/s (Borkowski et al. 2009)
- Detected with NuSTAR up to 30 keV (Zoglauer et al. 2015)
- Expansion is asymmetric; see poster by S. Reynolds
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Kepler's SNR
Figure 1(c) from Sankrit et al. 2015
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- Shock velocities vary by a factor of 2
- Comparing proper motions to shock velocities derived from Hα spectroscopy, we get distance of 5.1 ± 0.8 kpc
- At this distance, mean shock velocity in north rim is 1690 km/s, pre-shock density ~8 cm-3
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Chiotellis+ 2012 find Kepler is consistent with a symbiotic binary progenitor (i.e. single-degenerate) of WD + 4-5 Msun AGB star, favor large (> 6 kpc) distance
A few recent papers on Kepler…
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Chiotellis+ 2012 find Kepler is consistent with a symbiotic binary progenitor (i.e. single-degenerate) of WD + 4-5 Msun AGB star, favor large (> 6 kpc) distance
Tsebrenko & Soker 2015 use an “iron bullet” model to explain the “ears” in Kepler
A few recent papers on Kepler…
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Patnaude+ 2012- Interacting with slow (10-20 km/s) wind, mass loss rate > 4 x 10-6 M⊙ yr-1
- Low-density cavity near SN prior to explosion- Subenergetic explosions, large distances (> 7 kpc) required
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Patnaude+ 2012- Interacting with slow (10-20 km/s) wind, mass loss rate > 4 x 10-6 M⊙ yr-1
- Low-density cavity near SN prior to explosion- Subenergetic explosions, large distances (> 7 kpc) required
- Burkey+ 2013 confirm that Kepler is most consistent with SD scenario
- Spatial morphology explained by dense equatorial wind
- North/south density gradient explained by system's movement in northward direction
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Green spectrum from north rim
Yellow spectrum from south rim
Spectroscopic confirmation of much hotter dust in north than in south, density gradient required to produce this factor of 10-20 (Williams+ 2012)
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- Katsuda et al. 2015 find that Kepler is “An Overluminous Type Ia Event Interacting with a Massive Circumstellar Medium…,” a 91T-like SN
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- Katsuda et al. 2015 find that Kepler is “An Overluminous Type Ia Event Interacting with a Massive Circumstellar Medium…,” a 91T-like SN
Is there a link between Kepler and “Ia-CSM” SNe?
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- Bhalerao et al. 2015 used Chandra HETG spectra of several dozen knots to measure the red/blueshift of lines and get radial velocities
- Ejecta knots vary from -2300 to +1400 km/s
- Dynamics limit ejecta mass to <8 M⊙ and progenitor mass to <35 M⊙
G292.0+1.8
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II. What can SNRs tell us about SN progenitors?
Stars
Supernovae
Supernova Remnants
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II. What can SNRs tell us about SN progenitors?
Stars
Supernovae
Supernova Remnants
?
?
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II. What can SNRs tell us about SN progenitors?
Stars
Supernovae
Supernova Remnants
?
?
Conceptually easy…but practically impossible!
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One approach… reverse the problem
Solvable, though not easy
?
?
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XMM-Newton image
G284.3-1.8
See Williams et al. 2015
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XMM
Chandra image, consistent with point source
1FGL J1018.6-5856
• It’s a binary! 16.6d period confirmed in X-rays and ɣ-rays
• Optical counterpart identified: 30 M⨀ O6V((f)) star
• One of only two high-mass ɣ-ray binaries inside an SNR (SS 433 in W50)
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72 ks Chandra Obs. (ours) 105 ks XMM Obs. (PI: De Luca)
Selected two bright regions for analysis: North & West
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North region spectrum
Chandra, XMM MOS 2
kT = 0.67 keV𝛕 = 4.6 x 1012 cm-3 s
Abundances:
O ≡ 1Ne = 1.19Mg = 1.06Si = 0.19Fe = 0.24
Model: phabs x vpshock
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Chandra, XMM MOS 1, XMM MOS 2
West region spectrum
Abundances:
O ≡ 1Ne = 1.30Mg = 4.53Si = 1.50Fe = 0.97
kT = 0.92 keV𝛕 = 1.0 x 1011 cm-3 s
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West region rich in Mg, spectra and abundances similar to N49B in LMC (Park et al. 2003), another SNR with Mg-rich ejecta
Nucleosynthesis models produce significant amounts of Mg in explosions of massive (> 25 M⊙) (Thielemann+ 1996)
SNR N49B
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West region rich in Mg, spectra and abundances similar to N49B in LMC (Park et al. 2003), another SNR with Mg-rich ejecta
Nucleosynthesis models produce significant amounts of Mg in explosions of massive (> 25 M⊙) (Thielemann+ 1996)
Star 1
Star 2
SNR N49B
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West region rich in Mg, spectra and abundances similar to N49B in LMC (Park et al. 2003), another SNR with Mg-rich ejecta
Nucleosynthesis models produce significant amounts of Mg in explosions of massive (> 25 M⊙) (Thielemann+ 1996)
Star 1
Star 2
SNR N49B
To reproduce observed properties, best fit binary evolution models have Star 2 with 27 M⨀ initial mass
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3C 397
Spitzer (IR) & Suzaku (X-ray)
Yamaguchi et al.2015
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High Mn/Fe and Ni/Fe ratios imply high density in the WD core… which implies near Chandrasekhar mass WD… which implies single-degenerate progenitor
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- Katsuda et al. 2015 find that Kepler is “An Overluminous Type Ia Event Interacting with a Massive Circumstellar Medium…,” a 91T-like SN
Is there a link between Kepler and “Ia-CSM” SNe?
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N103B (0509-68.7)
Chandra Spitzer
N103B appears tobe second memberof class of Type Ia
SNRs with dense CSM,long after explosion
(BJW+ 2014)
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N103B (0509-68.7)
Chandra Spitzer
N103B appears tobe second memberof class of Type Ia
SNRs with dense CSM,long after explosion
(BJW+ 2014)
Stay tuned… approved for 400 ks with Chandra, plus 5
orbits HST