News from SN 1987A The end of a Teenager

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News from SN 1987A The end of a Teenager

• Bruno Leibundgut,Karina Kjær, Rubina Kotak, Per
  Gröningsson, Claes Fransson, Jason Spyromilio
• and the SAINTS team

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The excitement is back
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The complex SN 1987A
SAINTS
Reminder Today is day 7053 of SN 1987A
Suntzeff
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Origin of the ring(s)

• Equatorial (inner) ringR 1018 cm, Vexp 10
  km/s, tdyn 2104 years
• Origin (?) Merger inducing the equatorial mass
  loss and outer rings (Podsiadlowski
  1992, Morris Podsiadlowski 2005)
• Explains geometry as well as large N/C

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The ring

• Dominating at all wavelengths
• emission increasing for the past six years

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Optical, X-rays and Radio
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The ring collision

• Dominating at all wavelengths
• emission increasing for the past six years
• Emission from the stationary ring
• narrow lines (FWHM 10 km/s)
• known since 1987
• Shocked ring region (forward shock)
• intermediate lines (300 km/s)
• Reverse shock
• ejecta (15000 km/s)

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High-resolution spectroscopy

• VLT/UVES
• 310-1000nm, ?v6 km/s
• 170 intermediate (300 km/s) velocity lines
• (half of these are Fe II)
• ring lines easily detected
• broad lines from the reverse shock (Ha)

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Reverse shock
Gröningsson et al. VLT/UVES Smith et al.
Magellan/LDSS3 Henk et al. HST/STIS
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Reverse shock (II)

• Forward shock is ionizing the ejecta
• at some point all H atoms will be ionized before
  they reach the reverse shock and the emission
  will turn off
• X-rays give the amountof ionizing photons
• Monitoring the Ha emission will tell

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Intermediate lines shocked material in the ring

• HI, He I, N II, O I-III, Fe II, Ne III-V..
  Cooling, photoionized gas behind radiative shock
  into ring protrusions

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Coronal lines

• O III, Ne III-V, Ar V, Fe VII, Fe X-XI, Fe XIV
• velocity also 300 km/s
• shocked ring gas
• provides information on shock temperature
• X-ray lines found by Zhekov et al.

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Coronal line diagnostics

• Line flux depends on the shock velocity
• vshock300 to 400 km/s

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A prediction come true
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Time evolution
optical Gröningsson et al. X-rays Park et al.

• Coronal lines and soft X-ray emission have the
  same temporal behavior
• soft X-rays are from the hot spots
• hard X-rays are from the reverse shock and the
  blast wave

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Spatially resolved infrared spectroscopy - SINFONI

• Details in Karina Kjærs talk
• separate ring from ejecta
• trace the ring in individual lines
• get spectra from separate regions
• photometry of selected regions

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Spectral evolution
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Images at different wavelengths
Fe II 1.64µm
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IR light curve

• Average decline of ejecta luminosity very slow
  for the past 9 years (roughly 0.16 mag/year in K)
• Ring about 10 times brighter than the ejecta

JHK
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Spectral evolution in K
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Summary

• SN 1987A is as interesting as ever
• ring collision is in full swing
• shocked material can be analyzed through the
  X-rays and the coronal lines
• reverse shock observed with HST and from the
  ground
• dust formation can be observed in the thermal
  infrared ? see John Danzigers talk
• detailed analysis of the ring emission in
  progress ? see Karina Kjærs talk