Insights from Radio Wavelengths into Supernova Progenitors
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Transcript of Insights from Radio Wavelengths into Supernova Progenitors
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Insights from Radio Wavelengths into Supernova Progenitors
Laura ChomiukJansky Fellow, Michigan State University
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Supernova Types: I vs. II
Type I:No Hydrogen
Thermonuclear WD explosions (Ia)
and Core collapse of massive stars stripped of H envelopes (Ib/c)
Type II:Show Hydrogen
Core collapse of massive stars with H envelope
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Supernova Types: A Continuum of H-richness
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(Smartt 2009)
A diverse, complicated zoo of massive stars and core-collapse SNe
+ SNe Ia
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Searching for SN progenitors directly with optical imaging
SN 2005gl
Before During After
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Or, constraining SN progenitors indirectly-- in the radio
Soderberg et al (2008)
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SN 1970G: The first SN detected in the radio
(Gottesman et al. 1972, Goss et al. 1973)
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shell
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SN 1994I @ 20 cm Weiler et al. (2011)
absorbed (either free-free or synchrotron)
synchrotron τ ≈ 1
fading because
blast decelerates
and CSM decreases in
density
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vw ≈ 30 km/svsn ≈ 10,000 km/s
SN blast probes ~1 year of mass loss in one day!
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What makes a SN bright at radio wavelengths?
A fast blastwave Expansion into dense surroundings
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Radio bolsters a division in Type I SNe:
Type Ib/c: Show radio emission, core collapse
Type Ia: No radio emission, thermonuclear
(Panagia et al. 1986)
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Relativistic SN 1998bw associated with GRB 980425
(Kulkarni et al. 1998, Wieringa et al. 1999)(Galama et al. 1998)
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A diversity of mass loss histories
SN 2003bg (Soderberg et al. 2006)
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Shells, Spirals, and Shelves
SN 1993J (Weiler et al. 2007)
SN 2007bg (Salas et al. 2012)(Ryd
er et
al. 20
04)
SN 2001ig
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SNe Ib/c: WR stars or interacting binaries?
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Mdot/vwind = 10-10 10-9 10-8 10-7 10-6
M yr-1 / km s-1
SNe Ib/c show mass loss rates consistent with WR stars.
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Still no radio emission from SNe Ia
(Panagia et al. 2006)
Time Since Explosion (Days)
Radio Luminosity (erg/s/Hz)
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WD + Giant
WD + Sub-giant or Main Sequence WD + WD
(NASA/Swift/ Aurore Simonnet, Sonoma State Univ.)
Different progenitor models predict different circumbinary environments.
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...And still no radio emission from SNe Ia!
Assumes vw = 50 km/s
VLA
JVLA
nISM = 1 cm-3
M = 10
-8 M yr
-1
.
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Strong limits on the environment of SN 2011fe from EVLA
(Chomiuk et al. 2012, Horesh et al. 2011)
SN 2011fe
assumes vw = 50 km/s
nISM = 1 cm-3
M = 10
-8 M yr
-1
.
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Chomiuk et al. (2012), Margutti et al. (2012)
Strong limits on the environment of SN 2011fe from EVLA
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SN 2009ip: Watching an LBV explode
(Mauerhan et al. 2012)
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(Mauerha
n et a
l. 201
2)
SN 2009ip: No longer an impostor since ~Sept 15
No radio detection yet; VLA monitoring ongoing
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SN 1970G revisited
33.7 ± 4.3 μJy @ 5 GHz (Dittman et al. in prep)
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SN 1970G consistently challenges our radio facilities
(Stockdale et al. 2001, Dittman et al. in prep)
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SN 1970G: Decline in Radio + Rise in X-rays = Compact Object?
(Dittman et al. in prep)
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Radio light curves of SNe trace mass loss histories of progenitors.
Discovery of first radio SN
Theory of radio SN
Type I SNe split into Ia and Ib/c
Long GRB associated with a relat-ivistic SN
Diversity of mass loss histories• Ib/c mass loss consistent with WR• No Ia radio detections
Jansky VLA Era:• Sensitivity Bonanza!• Relativistic SNe w/o GRBs• Still no Ia radio detections
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end
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A continuum in blast wave velocities between normal SNe Ib/c and GRBs
(Soderberg et al. 2010, more in prep)