Pulsar Powerhouse: The Center of the Crab Nebula

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VLBI of Supernovae and Gamma Ray Bursts
Michael Bietenholz, Hartebeesthoek Radio
Observatory, South Africa
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Dr. Michael Gaylard
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Introduction Why Image Supernovae and GRBs with
VLBI?

• Resolution we can resolve the explosive
  outflows.
• Normal supernova 20000 km/s 0.4 mas/yr at 10
  Mpc, relativistic supernova or GRB, c 0.6
  mas/yr at 100 Mpc
• Determine ejecta speed
• Nature and geometry of the ejecta jets?
  Clumpiness? Bipolar ejections?
• Radio emission is usually due to the interaction
  of the ejecta with the surrounding material from
  interaction we can learn about both ejecta and
  the surrounding material
• Evolution of SN shells, shock acceleration,
  eventual merging with ISM
• Compact remnant of a core-collapse SN?
• Supernova rates, especially in dusty environments
• Direct distances with the expanding shock front
  method out to Virgo cluster

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Supernovae Radio Detection of SNe

• Optical several hundred SNe are detected each
  year
• Radio Only core collapse (Type II, Type I b/c)
  detected to date (limits in Ia next talk). Only
  a few SNe detected each year in radio total
  radio detections to date 60
• Even fewer have been resolved by radio
  observations - so every VLBI observation is of
  great value

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RSNe Detected with VLBI
Name Type Host galaxy Distance (Mpc) Peak (mJy at 8 GHz) References
SN 1978K II NGC 1313 4 gt100? Smith et al 2007.
SN 1979C II M100 16 6 Bartel Bietenholz, Marcaide et al
SN 1980K II NGC6946 6 2 Bartel 1985
SN 1986J II NGC891 10 100 Bietenholz et al 2004
SN 1987A II LMC 0.05 80 Jauncey, Ng, Manchester
SN 1993J II M81 4 100 Bietenholz, Bartel, Marcaide
SN 1994I Ic M51 8 20 Bietenholz Bartel, unpublished
SN 1996cr II Circinus 3.6 100 Bauer et al, Bartel et al in prep
SN 2001em Ib/c NGC 7112 80 4 Bietenholz, Paragi, Schinzel
SN 2001gd II NGC 5033 13 4 Pérez-Torres et al 2008
SN 2003gk Ib NGC 7460 45 2 Bietenholz et al 2013
SN 2003L Ib/c NGC 3506 92 3 Soderberg et al 2005
SN 2004et II NGC 6946 6 2 Martí-Vidal et al
SN 2007gr Ib/c NGC 1058 10 lt 1 Paragi et al 2007
SN 2007uy Ib NGC 2770 27 1 van der Horst 2011
SN 2008D BL Ib/c NGC 2770 27 3 Soderberg, Bietenholz Paragi
SN 2008iz II? M82 3.6 150 Brunthaler et al 2010
SN 2009bb BL Ib/c NGC 3278 40 18 Bietenholz et al 2010
SN 2011dh IIb M51 8.4 7 Bietenholz et al, Martí-Vidal et al
Approximately 30 RSNe with flux densities gt 1 mJy
have been detected in radio, and gt100 have upper
limits.
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RSNe Detected with VLBI
Name Type Host galaxy Distance (Mpc) Peak (mJy at 8 GHz) References
SN 1978K II NGC 1313 4 gt100? Smith et al 2007.
SN 1979C II M100 16 6 Bartel Bietenholz, Marcaide et al
SN 1980K II NGC6946 6 2 Bartel 1985
SN 1986J II NGC891 10 100 Bietenholz et al 2004
SN 1987A II LMC 0.05 80 Jauncey, Ng, Manchester
SN 1993J II M81 4 100 Bietenholz, Bartel, Marcaide
SN 1994I Ic M51 8 20 Bietenholz Bartel, unpublished
SN 1996cr II Circinus 3.6 100 Bauer et al, Bartel et al in prep
SN 2001em Ib/c NGC 7112 80 4 Bietenholz, Paragi, Schinzel
SN 2001gd II NGC 5033 13 4 Pérez-Torres et al 2008
SN 2003gk Ib NGC 7460 45 2 Bietenholz et al 2013
SN 2003L Ib/c NGC 3506 92 3 Soderberg et al 2005
SN 2004et II NGC 6946 6 2 Martí-Vidal et al
SN 2007gr Ib/c NGC 1058 10 lt 1 Paragi et al 2007
SN 2007uy Ib NGC 2770 27 1 van der Horst 2011
SN 2008D BL Ib/c NGC 2770 27 3 Soderberg, Bietenholz Paragi
SN 2008iz II? M82 3.6 150 Brunthaler et al 2010
SN 2009bb BL Ib/c NGC 3278 40 18 Bietenholz et al 2010
SN 2011dh IIb M51 8.4 7 Bietenholz et al, Martí-Vidal et al
Approximately 30 RSNe with flux densities gt 1 mJy
have been detected in radio, and gt100 have upper
limits.
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Radio Lightcurves (SN 1993J)

• Typical pattern seen in SNe with
  frequency-dependent rise and then a power-law
  decay after the supernova has become optically
  thin
• Increase in the steepness of the decay at t
  2500 days (Bartel et al 2002)

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VLBI Movie of SN 1993J

• Global Array VLBI at 8.4 GHz, then 5 GHz and 1.6
  GHz for last epochs
• 35 Epochs of VLBI

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Deceleration
Radius scaled by t0.8 to show deviations from
powerlaw expansion
Bietenholz et al 2010
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µJy/beam
Explosion Center

• Global array 18 antennas (EVN VLBA GBT).
  Used in-beam calibrator technique
• Image background rms 3.7 µJy/beam
• Radius 5.1 1017 cm (34,000 AU 0.16 pc)
• Expanding at 7,500 km/sec
• Limit on a PWN at centre?
• 50 µJy at 1.6 GHz 25 of Crab
  Nebula
• Bietenholz et al 2003 50 µJy at 8.4 GHz (stacked
  3 epochs,1998-2000)
• Marti-Vidal Marcaide 2014 102 µJy at 5.0 GHz
  (stacked images)

1.7 GHz
Bietenholz et al, in prep
6 Mar 2010, day 6187 16 years after the
explosion
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Central Component in SN1986J
Multi-frequency VLBI Image Contours, red 5
GHz Blue ? white 15 GHz

• Central component turned on at age 15 yr
• ? 0.8 milli-arcsec (1017 cm)
• 200 the current radio luminosity of the Crab
  Nebula at 15 GHz

Bietenholz, Bartel Rupen 2004
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Central Component in SN1986J
Multi-frequency VLBI Image Contours, red 5
GHz Blue ? white 15 GHz
Youngest Neutron Star or Black Hole?
Bietenholz, Bartel Rupen 2004
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SN 1987A
Comparison of VLBI image to optical and X-ray
images. Contours VLBI at 1.7 GHz, 0.5, 1.5,
3, and 5 mJy/beam.
Ng et al 2011
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SN 1987A
Comparison of VLBI image to optical and X-ray
images. Contours VLBI at 1.7 GHz, 0.5, 1.5,
3, and 5 mJy/beam.
Ng et al 2011
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ULIRGs Supernova Factories

• Arp 220 (Conway et al), Arp 299 (Bondi, Neff,
  Ulvestad et al.), IRAS 233653604
  (Romero-Cañizales, Pérez-Torres et al.)
• High Sensitivity Array observations at 14 and
  Global VLBI at 8.4 GHz
• 17 sources detected, mostly resolved at 14 GHz
• VLBI crucial to distinguishing starburst and AGN

Conway et al 2010
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Relativistic Expansion SNe and GRBs

• Long Duration GRBs associated with Type Ibc
  supernovae
• Collapse of massive star into a black hole powers
  highly relativistic jet
• GRBs are jets oriented near the line of sight
• The jets not near the line of sight may be
  visible in radio

Image Saxton
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Relativistic Expansion SNe and GRBs

• Long Duration GRBs associated with Type Ibc
  supernovae
• Collapse of massive star into a black hole powers
  highly relativistic jet
• GRBs are jets oriented near the line of sight
• The jets not near the line of sight may be
  visible in radio

Image Saxton
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SN2009bb
SN 2009bb VLBI observations Peak brightness 613
µJy/bm, rms 128 µJy/bm, VLBA, VLA, Hobart,
Tidbinbilla2009 Jun 12 (age 85 days) 40
Mpc Upper limit on angular size 0.64 mas 1.74c
Bietenholz et al 2010
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Limits on Off-Axis Jets
Off-axis jets could be detectable in the
radio However, lower efficiency in par-ticle
acceleration or lower magnetic field could
dras-tically lower model curves Luminosity
limits Bietenholz et al 2014, and Soderberg et
al 2006 (S2006)
SN 2003gk
Bietenholz et al 2014
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SN 2003gk VLBI Observations
8.4 GHz VLBA Ef Arecibo Age7.5 yrs (2011
Apr 11) Contours 20, 30, 50, 70, 90 of peak of
86 µJy/ beam
r 1 light-year
Bietenholz et al 2014
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Limits on Off-Axis Jets
Off-axis jets could be detectable in the
radio However, lower efficiency in par-ticle
acceleration or lower magnetic field could
dras-tically lower model curves Luminosity
limits Bietenholz et al 2014, and Soderberg et
al 2006 (S2006)
Bietenholz et al 2014
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Relativistic Expansion GRB 030329 (SN 2003dh)
22 Apr 2003
Size 1 pc 3 light years
VLBI Expansion Measurements by Taylor et al.
Pihlstrom et al. show clear deceleration, with
transition to non-relativistic regime at t 1yr
Taylor et al, 2004, 2005 Pihlstrom et al. 2007,
Mesler et al 2012
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Relativistic Expansion GRB 030329 (SN 2003dh)
22 Apr 2003
Size 1 pc 3 light years
Speed of light
VLBI Expansion Measurements by Taylor et al.
Pihlstrom et al. show clear deceleration, with
transition to non-relativistic regime at t 1yr
Taylor et al, 2004, 2005 Pihlstrom et al. 2007,
Mesler et al 2012
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The Future of Supernova VLBI

• More sensitivity follow supernova for longer
• Resolve older, more distant supernovae Cas A
  is 1 µJy and 6 mas at 170 Mpc - fill in the gap
  between supernovae and supernova remnants
• Supernova rates ? star formation rates
• Pop III Hypernova
• GRBs and orphan afterglows

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VLBI Supernova Gallery
SN 1987A
SN 1993J
SN 1979C
SN 1986J
SN 1996cr
SN 2008iz
M82
SN 2011dh
SN 1996cr, 1993J, SN1986J, SN1979C Bietenholz,
Bartel et al SN 2008iz Brunthaler et al 2010
M82 supernova/SNR McDonald, Beswick, Argo et al
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(No Transcript)
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Comparison of RSNe SNRs
McDonald et al., 2001