Unusually BrightSupernovae
Robert Quimby

Absolute Magnitude Distributions of Supernovae
C9444$-G-A,.$H*ï9$I%3ïJ$KJL9E
C9444$-G-A,.$H*ï9$I%3ïJ$KJL9E

D+,-$%-*$FBA/<M<?+,BG-$D+,-

Data from LOSS (Li et al. 2011)
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123
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95 $

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ï54:-+;$%.-<=>ï&2.>?<,-$'+@AB,<=-$CDï2+A=E-- Robert Quimby (Kavli IPMU) --ï55
2

SLSN Spectra• SLSN-I (like 2005ap)• SLSN-II (like 2006gy)• Type Ia• Type II

Hundreds of times brighter than SNIa in the UV!
-- Robert Quimby (Kavli IPMU) --3

SLSN Light Curves

unfiltered ROTSE-IIIb (optical) magnitudes-- Robert Quimby (Kavli IPMU) --4

What are SLSNe Physically?
Three possibilities under consideration:
1) Pair Instability supernovae?
2) Supernovae powered by ejecta/windinteraction?
3) Supernovae powered by a compact
remnant?
-- Robert Quimby (Kavli IPMU) --5

Are SLSNe: 1) Pair-Instability SNe?
• First Proposed it the 1960’s (Rakavyet al. 1967; Barkat et al. 1967)• Massive stars are supported byradiation pressure• At high temperatures, photons are
created with E > e+e-

• Losses to pair production soften theEOS, and lead to instability• Expected fate of the first (lowmetal, high mass) stars
Waldman 2008-- Robert Quimby (Kavli IPMU) --6

SN 2007bi: A Slowly Fading SLSN-I

Gal-Yam et al. 2009
• Optical light curve decay rate consistent with ~7 M of 56Ni
• Iron abundance in nebular spectra also consistent with ~4-7 M of 56Ni

See however Dessart et al. 2012-- Robert Quimby (Kavli IPMU) --7

Some SLSN Fade Fast
No. 6, 2010

NEW OBSERVATIONS OF THE VERY LUMINOUS

Bolometric Luminosity (LO• )1011

SN2006gy
1010

Total Luminosity
NIR Luminosity
Late-time photometry
limits the
Optical Luminosity

56Ni production to <2.5 Msun
(not enough to explain the peak)

109

108
2.5 MO• 56Ni

107
0200

400
600
Days since explosion

800

Figure 5. Evolution of the bolometric luminosity of SN 2006gy during the firstet al.
2010as black circles, and NIR data
800 days after explosion. OpticalMiller
data areshown
are red squares. Early-time data (< 250 days) are from Smith et al. (2010).
-- Robert
QuimbyIPMU)
The optical detection nearday 400
is from(KavliKawabataet --al. (2009). All other>400 days. Tfrom Smith e
400 comes fr(2009), while
direct integra
The three labased on theThe decay rathan the obs∼0.2 mag (1a rate that is t
The PISN
good agreem
after an artifi
evolutionaryNIR luminos
required lessrays (from rameans that th8 . Th(100 d)−1Are SLSNe: 2) Powered by Interactions?
Narrow emission lines indicate
ejecta/wind interaction

Ejecta run into surrounding
material (progenitor wind,shells, etc.) and convert
kinetic energy into luminosity

Smith et al. 2008see also Smith & McCray 2007,
Chevalier & Irwin 2011-- Robert Quimby (Kavli IPMU) --9

Initial Plateau in SLSN-I?
SN 2006oz (SLSN-I)“SN 2009ip” (LBV turned SN)

Leloudas et al. (2012)see also Moriya et al. 2012-- Robert Quimby (Kavli IPMU) --Mauerhan et al. (2012)10-12-13

temperatur

log10 density (sn e d= 2 ×B10field
Pthof ergs,(1)
Ep =a minimum
tp !large
td requires
amount ofadiabatic
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that has occurred
21sh1
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injection
the interior
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α = time1/2),
injectingmost ofresets
the energy
into 2.0 (JIns Ω
50 −2iFig=2×10Pergs,
(1)
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scale toremnant
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the initial 1.5(top)the expanding
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sn thep ).
3p >where P10 = Pi /10
ms
weset
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c
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anrole. (2)The 0.5andcoE
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ertia toenergies
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tional energy
at B
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fixedatsin
α=1/2),
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5×10BκMEergs,L∼
es of 551
Fig. 1.—
entp !peaktd expanding
requiresminimum
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imone month(4)−3/8 1/8
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cula
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10andinitial
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bilit
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field ofd requiresspins
Pi =time−entropy
20 ms Brange.
range.
Thislate
injection resets the interiorshell (Junnear−3/8 1/8
14−1/4energy scaletoE∼
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theinitial
B > 1.8 ×int10 P10p κesM5
E51 G,(3)Th
sity interi
3.
HYDRODYNAMICALIMPACT
thermal energy when 2Ep−1> Esn (te /tp ). Thus even low ical calcul
coorTh
where κenergies
cm< gE , M
Mejimportant/5 M" and role.
E51 =Thees = κ/0.2
5 = anmagnetarEplayculationspsnOur simple
estimateignores
the details of how the decom
51−1
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are in the magnetar
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throughout
theinteriorofejectrange. This late time entropy injection resets the interioris(Jun1998
the energy
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mechscale
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evenlowespsnep
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551
ener
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dmagnetar
Ep <Esn play magnetar
an importantenergy
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we assume
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is thercomparabbu(4) ejecta.impl
resultingpeak luminosity
malizedsphericallyat theis base of the supernova ejecta.
Th
beco
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is primarily
a functionof inthehomologous
magnetic field.
This (8/7)ρ vdo
2
The
to −2
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Eis0 sp tpassumed43
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43−1−1veloth∼∼
5 ×1010 B
κes Merg
showsLpeak
that∼ Lpeak−1410
sE51 erg
SNes canbe energized
5witha shallow
structurein the ,interior
t2dpower law density
achieved from magnetars with B14 = 1 − 10 and initial implyingvea(4)! ms range.
"# $−δ
spins
intheP=2−
20
becomesw
iv
3--− δof the
Mejmagneticv
is primarily
a function
field. This-- Robertwhich
Quimby(Kavli IPMU)
11Are SLSNe: 3) Powered by Magnetars?

temperature (104 K)

by the time t ∼ td leads
to low−1/4
luminosities.
−3/8
1/8
14
whereNow
PB=P/10msand
weset
NS(tE
momentof in-(3) -14
10 >i × the1.8
10 impact
P10 κofes latetheMconsidertime"t)
eneG,
551
ertiaergy
to injection
be Ins =from
1045a young
g cm2magnetar. This magnetarrota- -15
with radiusloses
Rns =
2 −1
where
κes and= κ/0.2
gset
Mmagnetic
Mejmagnetar/5M" radiationand10 energykminitialspin
Ω
2π/P
. The
rota-E51 = -16
tionalatthecmrate
dipole5 i=i =,by51 energy−1istional(withtheangle,α,betweenrotation
dipole 3.0Eergs. The
requiredfieldsand
aremagnetic
in the magnetar
sn /10SLSN-I Host Galaxies• Prefer less luminous hosts that CCSN
• May be similar to LGRB hosts

Lunnan et al. 2014-- Robert Quimby (Kavli IPMU) --12

Discovery of PS1-10afx(Pan-STARRS1 Team)Sky Position
RA = 22:11:24.162
Dec. = +00:09:43.49(Aquarius)

Explosion

First Detected:
August 31, 2010

(short exposure)(long exposure)

Chornock et al. (2013)

Peak Brightness:~22 mag (i-band)~24 mag (r-band)

Unusually red color!
-- Robert Quimby (Kavli IPMU) --Difference
Chornock et al. (2013)

Chornock et al. (2013)

Before Explosion

Chornock et al. (2013)

Relative Brightness at Each Wavelength

near peak brightness

a few days after peak

Photometry

Redshift z=1.388 from narrow
host lines and supernova
features. Color is relatively red
for superlumious supernovae

Observed brightnesscombined with luminosity
distance (from redshift)
implies high luminosity, butevolution is much faster thantypical superluminous
supernovae

Chornock et al. (2013)

SpectraPS1-10afx Has Spectra Similar
to Type Ia Supernovae
Relative Brightness at Each Wavelength

5 days before peak

2 days beforepeak

1 days after peak

2 days afterpeak

Type Ia
comparisonspectraPS1-10afx Spectra: good match to SNIa,
but not SNIc

Riess et al. (2007)-- Robert Quimby (Kavli IPMU) --16

PS1-10afx
Photometry

Compared to SNIa TemplatesCompared to a Normal SNIa
PS1-10afx

2011fe(normal SNIa)-- Robert Quimby (Kavli IPMU) --17

PS1-10afx is a Type Ia Supernova
Magnified by a Gravitational Lens

A. Tsuboi/Kavli IPMUFirst strongly lensed Type Ia supernova!
-- Robert Quimby (Kavli IPMU) --So Where is the Lens?

-- Robert Quimby (Kavli IPMU) --19

New Spectra Show...Two Galaxies!

Lens MgII• Host OII (and MgII) at z=1.39• Lens OII (and MgII) at z=1.12-- Robert Quimby (Kavli IPMU) --20

Smaller Image Separations areEasier to Find-- Robert Quimby (Kavli IPMU) --21

How to Identify Lensed SN-- Robert Quimby (Kavli IPMU) --22

Direct H0 Measurement with Lensed SNeIa• Each lensed image traverses a different path
• Path length differences lead to time delays• Delays are inversely proportional to H0

Oguri & Marshall 201010?
• Use color selection to find more lensed SNIa
• Use HST or AO to confirm and follow-up-- Robert Quimby (Kavli IPMU) --23