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Day 8550: 23.41 years since outburst
NASA/ADS: 2435 (~2 /week) refereed papers, 24875 c. (since 1987)
Crab : 2511 (23658 c.) since 1892
Cass A: 239 (2596 c.) since 1948
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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Supernova SN 1987A
- The birth of a Remnant –
P. Bouchet & J. Danziger
Collaborators:
• mid-IR: Eli Dwek, Rick Arendt, James de Buizer
• X-rays : Sangwook Park
• HST : SAINTS Team (R. Kirshner, PI)
• CSM : Ben Sugerman, Arlin Crotts, Steve Lawrence
• Five Years of Mid-Infrared Evolution of the Remnant of SN 1987A: The Encounter Between the Blast Wave and the
Dusty Equatorial Ring: Dwek, E. et al., 2010, ApJ in press
• Observing Supernova 1987A with the Refurbished Hubble Space Telescope, France, K., et al., 2010, Science, in
press
• Infrared and X-Ray Evidence for Circumstellar Grain Destruction by the Blast Wave of Supernova 1987A: Dwek, E.,
et al., 2008, ApJ, 676, 1029
• SN 1987A after 18 Years: Mid-Infrared Gemini and Spitzer Observations of the Remnant: Bouchet, P., et al., 2006,
ApJ, 650, 212
• High-Resolution Mid-infrared Imaging of SN 1987A: Bouchet, P., et al., 2004, ApJ, 611, 394
• Evolution and Geometry of Hot Spots in Supernova Remnant 1987A: Sugerman, B., et al., 2002, ApJ, 572, 209
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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Imaging with
the Hubble Space Telescope (HST)
SAINTS
Collaboration
CSM : EQ ring 1.34 lt-yr; i = 45°, produced by a mass loss event that
occurred ~ 20,000 before explosion
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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X-ray Imaging
ROSAT/HRI
(5” pixels)
HEASARC/SkyView
N
E
ACIS (1999-10): Burrows et al. 2000
Green-Blue: ACIS
Red: HST
Contour: ATCA
1 arcsecond
Park, 2007
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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mid-IR Imaging
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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Radio Imaging
ATNF, Gaensler, 2007
• Limb brightened
• Bright lobes to
east and west
• Eastern lobe
brighter than
western lobe,
& brightening
faster
 Same as X-rays
ATCA 9 GHz diffraction
limited
arcsec)
super-resolved
(0.5(0.9
arcsec)
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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X-ray and Radio Light Curves
Park et al., 2006; Zhekov et al., 2009  2-shocks model
ROSAT
(Hasinger et al. 1996)
X-ray (2005-7) vs. Optical (2005-4)
Chandra
(0.5 – 2 keV)
Density and
Temperature of
ATCA
the soft X-ray
emitting gas have
ROSAT
Chandra
not significantly
(3 – 10 keV)
changed during
the > 5 years
Similar rates of hard X-ray and radio
period.
X-ray Flux (10-13 ergs/cm2/s)
0.5-2 keV fractional flux
“Fast” shock
d ~ 6200
X-ray Flux (10-13 ergs/cm2/s)
keV
1.0.5-2
Soft
X-Ray = Decelerated, slow (300-1700 kms-1); kT= 0.3 – 0.6 keV
keV
2.3-10
Hard
X-Ray = High-speed (3700±900 kms-1); kT= 2 – 5 keV
Radio: Gaensler & Staveley-Smith, 2007
ACIS 3-8 keV
ACIS 0.4-0.5 keV
ACIS 0.5-2 keV: Park et al., 2008
Contours:
ATCA 9GHz
Contours: HST (Peter Challis)Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay
– COSPAR
2010Contours: ATCA 9GHz
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11.7μm (Bouchet et al., 2006) and HST (Challis,
2006)
EQUATORIAL RING
McCray, 2007
HOT « FINGERS »
Optical/Soft X-rays
IR??
SHOCK WAVE
NS/BH
HOT GAS
REVERSE SW
?
Radio
Hard X-rays
COOL EJECTA
Low speed oblique radiative
shock: optical/UV
Cf. Michael et al. 1998
Slower shock in high-density
soft X-rays – COSPAR 2010
Patrice Bouchet – DSM/IRFU/Sapknot:
CEA-Saclay
High speed shock: radio,
hard X-ray
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Mid-IR observations of the
Circumstellar Dust
T-ReCS, Gemini T-ReCS, Gemini T-ReCS, Gemini
6526
VISIR, VLT
7241
7569
6067
~
~
6526, Qa
7241/6067, N
The silicate emission increased as t0.87, consistent with X-ray observations, suggesting
the blast wave has transitioned from a free expansion to the Sedov phase (now
expanding
into the main
body of–the
ER).2010
Patrice
Bouchet – DSM/IRFU/Sap
CEA-Saclay
COSPAR
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HST vs VISIR (VLT)
Overlay of HST (Dec2006)
(black) with VISIR (red-yellow)
shows correlation far from
100 percent!
Other comparisons show
dust annulus possibly (?) thicker
than visual HST annulus.
Where is the dust?
What heats the dust?
1. In the X-ray emitting gas?
2. In the denser UVO emitting knots?
1. Collisional heating?
2. Radiative heating?
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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Origin of the mid-IR emission?
T-ReCS/HST
ACIS/11.7 mm
ATNF/11.7 mm
ACIS/18.3 mm
ATNF/18.3 mm
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
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Observations with SPITZER
Silicates
Silicates + Black body
ne (cm-3)
Grain absorption coeffs.
 ne = (2 – 4) x 104 cm-3
Dwek et al., 2010
Mystery contributor: much higher T, grain radii or IR emissivity smaller, significantly
shorter sputtering time, distinct evolution: No temporal change of spectral shape
Patrice
Bouchet
– DSM/IRFU/Sap
CEA-Saclay –of
COSPAR
2010
and in the mass ratio?:

A clue
to binarity
progenitor
?
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IRX: the IR to X-ray Flux ratio
 Dust cooling dominates the cooling via atomic transitions at T ≥ 106 K
L(Te) erg cm3 s-1
L(Te): Equilibrium atomic cooling rate
for a plasma with ER abundances
Ld(T): Gas
cooling rate
via dust –gas
collisions
Dwek et al., 2010
IRX =
L(T)
Ld(T)
Te (K)
=
SN 1987A
1987, ApJ 320
Cooling rate via atomic processes
≈ 2.5  a ≥ 0.30 mm
Cooling rate via dust-gas collisions
The cooling of the shocked gas is dominated by IR emission from the
collisionally-heated dust with radii > 0.3 mm, and a significant fraction of the
refractory elements
in the
ER is depleted
onto
dust (Dwek
et al., 2010)
Patrice Bouchet
– DSM/IRFU/Sap
CEA-Saclay
– COSPAR
2010
IRFU/ Service
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IRX vs. Dust Destruction
IRX
No obvious dust destruction yet
IRX Constant  No cooling of the shocked gas yet
 t(Si grains) = 4 – 15 yr, t(C dust) = 0.4 – 1 yr
 Gas cooling time for the shocked gas = 12 – 20 yr
 grain destruction may become important
only at day ≈ 9200
 the X-ray emission may not be affected until
t ≈ 30 yr
IRX  a ≥ 0.30 mm
Dwek et al., 2008 Te
(K)
Mass of radiating
dust in ring = ~10-6 MSun
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
d’Astrophysiqu
e
Observations with the
Hubble Space Telescope
The SAINTS team (PI: R.P. Kirshner) monitors SN 1987A with HST since it
was launched. The recent repair of STIS allows us to compare observations
in 2004, just before its demise, with those in 2010.
The young remnant of supernova 1987A (SN 1987A)
offers an unprecedented glimpse into the hydrodynamics
and kinetics of fast astrophysical shocks
Last Results (January 31st., 2010): France et al., 2010
• Ly and H lines from shock emission continue to brighten,
while their maximum velocities continue to decrease.
• Evidence for resonant scattering (within the source) of
Ly photons from hotspots on the equatorial ring (to
blueshifts ∼ −12,000 km s−1) .
• Emission to the red of Ly attributed to N V 1239,1243Å
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
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Central part (debris) shows blue (approaching) extends to ~4000
– 6000 km/s. Red extension not apparent because dust in ejecta
blocks far side receding (France et al., 2010).
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
d’Astrophysiqu
e
Lya 2010 – 2004 difference image (black
indicates similar intensities):
1. Lya emission has increased in
brightness by factor 1.6 – 2.4 
increased flux of H atoms into the
shock region
2. The maximum Doppler shift in the
northern blueshifted emission is
decreasing as a function of time
(France et al., 2010)
Lya:Ha ~ 80 (5:1
for a Balmerdominated shock)
If the Lya photons produced by the same mechanism as the Ha photons  Lya:Ha should be
the same for all velocities  a sufficient number of Lya photons are emitted by the hotspots and
the neutral H layer in the expanding envelope scatters Lya photons by ~ 6000 kms-1
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
d’Astrophysiqu
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Slit in geocoronal Lya
 N V lines are detectable because, unlike
hydrogen atoms, N4+ ions emit hundreds of
photons before they are ionized.
 The profiles of the N V lines differ
markedly from that of H  scattering of
N4+ ions by magnetic fields in the ionized
plasma(?)
 N V emission provides a
unique probe of the
isotropization zone of the
collisionless shock
(France et al., 2010)
 H atoms are excited by collisions without
significant deflection
 N atoms become ionized and gyrate about a
magnetic field that is parallel to the shock and
moving with the fluid velocity of the shocked
plasma. CEA-Saclay – COSPAR 2010
Patrice Bouchet – DSM/IRFU/Sap
IRFU/ Service
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G54.1+0.3
IR shell – gas and dust condensed from
SN debris and then heated by stars in
cluster. Expanding pulsar wind also heats
dust.
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010
IRFU/ Service
d’Astrophysiqu
e
THE END….. (Thank you!)
Patrice Bouchet – DSM/IRFU/Sap CEA-Saclay – COSPAR 2010