supernovae: lighthouses of the cosmos
TRANSCRIPT
Supernovae:Lighthouses of the Cosmos
Supernovae:Lighthouses of the Cosmos
Space Telescope Science Institute8 January 2008
Nino Panagia
Space Telescope Science InstituteItalian National Institute of Astrophysics - Catania Obs.
Supernova Ltd
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Chichen-Itzà (Yucatan)A Mayan Observatory
Chichen-Itzà (Yucatan)A Mayan Observatory
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Mount Palomar Observatory (5m)Mount Palomar Observatory (5m)
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European Southern Observatory:Very Large Telescope: VLT1 (8m)European Southern Observatory:Very Large Telescope: VLT1 (8m)
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ESO-VLT (4 telescopes, 8m each)ESO-VLT (4 telescopes, 8m each)
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Keck Telescopes (2×10m) at Mauna Kea (HI)Keck Telescopes (2×10m) at Mauna Kea (HI)
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Arecibo (PR) Radiotelescope (300m)Arecibo (PR) Radiotelescope (300m)
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Kuiper Airborne Observatory (KAO)Kuiper Airborne Observatory (KAO)
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International Ultraviolet Explorer (IUE)International Ultraviolet Explorer (IUE)
Hubble Space Telescope (HST; 2.4m)Hubble Space Telescope (HST; 2.4m)
Edwin Hubble,
the astronomer
Edwin Hubble,
the astronomer
Hubble, the space telescope…Hubble, the space telescope…
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15Launch on 24 April 1990
HST launch on 24 April 1990, [Space Shuttle Discovery]
HST launch on 24 April 1990, [Space Shuttle Discovery]
The Glorious Endof Massive Stars
The Glorious Endof Massive Stars
Supernovae
You can’t live with them…You can’t live without them…
You can’t live with them…You can’t live without them…
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Supernovae?Supernovae?
SUPERNOVA = super - nova
very newbright star
(Baade & Zwicky 1934)
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Supernova ExplosionsSupernova Explosions
Supernovae represent the violent demiseof stars much bigger (3-40 times) than our Sun
• Very bright, 100 – 10000 millionbrighter than the Sun
• They produce large amounts of heavy elements (O, Mg, Si… Fe)
• The explosions supply the entire parent galaxy of kinetic energy
• Very bright, 100 – 10000 millionbrighter than the Sun
• They produce large amounts of heavy elements (O, Mg, Si… Fe)
• The explosions supply the entire parent galaxy of kinetic energy
How are they studied…How are they studied…
With optical and ultraviolet observations….With optical and ultraviolet observations….
and infrared and radio…and infrared and radio…
in X-rays…in X-rays…and in Gamma-raysand in Gamma-rays
5m Mt Palomar5m Mt Palomar Hubble Space TelescopeHubble Space Telescope International Ultraviolet ExplorerInternational Ultraviolet Explorer
Very Large ArrayVery Large Array
IntegralIntegralChandraChandra
Spitzer Space TelescopeSpitzer Space Telescope
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Why do we care about Supernovae?Why do we care about Supernovae?
• Explosive death of stars• Heavy element enrichment • Energy injection
• Distance indicators• Tracers of stellar populations
• Bright background sources Studies of the ISM
• Bright light echoes 3-D structure of the ISM
Evolution of stellar systems and galaxies
Cosmology
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Historical SupernovaeHistorical SupernovaeYear Type mmax Discovery SN Remnant185? I? -8 Chinese RCW86
393 ? -1 Chinese
837 ? -8? Chinese IC 443
1006 I -10 Chinese /Arab SN 1006
1054 II -6 China/Japan/Chaco Canyon
Crab Nebula
1181 II? -1 China/Japan 3C58
1572 I -4 Tycho Brahe Tycho
1604 I -3 Kepler* Kepler
ca. 1680 II 5? Flamsteed Cas A
1987 II +2.9 Ian Shelton SN1987A
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SN 1604: the “Kepler” Supernova
It appeared in the sky near an expected planetary conjunction :
First noticed in Padua,It was studied in detail by Kepler
(De Stella nova in pede Serpetarii)
Padua, 9 October 1604
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Anasazi petrograph in Chaco Canyon (NM) shows the Crab Nebula explosion (5 July 1054)
Anasazi petrograph in Chaco Canyon (NM) shows the Crab Nebula explosion (5 July 1054)
Supernova
Moon crescent at ~3ºfrom the SN
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Crab Nebula: a recent SN explosionCrab Nebula: a recent SN explosion
Crab Nebula: a recentSN explosion (~July 1054)
A typicalPLERION
(from ancient Greek πληρεs = full
Weiler & Panagia 1978)
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The Cygnus Loop:an old supernova
The Cygnus Loop:an old supernova
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Supernovae in numbersSupernovae in numbers
Supernova (SN) type Ia Ib/c-II
Peak Luminosity 4 billion L 1 billion L
Ejected Mass about 1.4 M 1-10 M
Fraction of Ni/Co/Fe about 50% few %
Stellar Remnant none neutron star/black hole
As bright as the Moon at… 750 ly 300 ly
As bright as Venus at… 9000 ly 6000 ly
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SN 1979C: my FIRST supernovaSN 1979C: my FIRST supernova
SN 1979C in NGC 4321 = M100
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SN1979C in the optical and in the radioSN1979C in the optical and in the radio
• Optical • Radio
April 1979 April 2000April 1979 April 2000
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SN 1979C: TEN years of radio observations detect the presence of a companion
SN 1979C: TEN years of radio observations detect the presence of a companion
Spiraling circumstellar material as predicted for a binary system made of 10 e 15 M stars that orbit around each other with a 5000 year period
A detached spiral system!
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SN 1994D in NGC 4526SN 1994D in NGC 4526
HST-WFPC2
A supernova as bright as the nucleus of its parent galaxyA supernova as bright as the nucleus of its parent galaxy
Energetics of SN ExplosionsEnergetics of SN Explosions
Nuclear Explosion
Core Collapse
Involved Mass ~1 M several M
Progenitors Stars of moderate mass (3-8M ) in binary systems
Massive Stars (above 8M )
SN Types Type Ia Types II, Ib/c
Neutrinos 1051 erg 1053 erg
Kinetic Energy 1051 erg 1051 erg
Radiation 1049 erg 1049 erg
Energetics of Supernova Esplosions
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How does a type Ia supernova (SNIa) explode?How does a type Ia supernova (SNIa) explode?
A possible scenario for a SNIa explosion:the “single-degenerate” case
Companion Star
Red Dwarf
Companion Star
Red Dwarf
Accretion discAccretion disc
Stream of matterStream of matter
White DwarfWhite Dwarf
The white dwarf accretes matter from its companion, thus increasing its mass and shrinking its size.
The white dwarf accretes matter from its companion, thus increasing its mass and shrinking its size.
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How does a type Ia supernova (SNIa) explode?How does a type Ia supernova (SNIa) explode?
The “double degenerate”scenario
After both stars in a binary system become white dwarfs, they may start spiraling in to merge and form a more massive compact star
After both stars in a binary system become white dwarfs, they may start spiraling in to merge and form a more massive compact star
When the mass of the white dwarf reaches a critical value (about1.44M , also called the Chandrasekhar limit), the star collapses.
The collapse triggers a series of nuclear reactions that transform the Carbon-Oxygen core into radioactive Nickel (which decays quickly into radioactive Cobalt, to become stable Iron) and produce the powerful SNIa explosion that we see.
When the mass of the white dwarf reaches a critical value (about1.44M , also called the Chandrasekhar limit), the star collapses.
The collapse triggers a series of nuclear reactions that transform the Carbon-Oxygen core into radioactive Nickel (which decays quickly into radioactive Cobalt, to become stable Iron) and produce the powerful SNIa explosion that we see.
Explosion of a
type Ia supernova
Explosion of a
type Ia supernova
from both channels…from both channels…
Gravitational Energy released ≅ 3 x 1053 ergs
The core, about 1.5M of Fe, collapses to become a Neutron Starwhose radius is RNS ~ 10 km
Onion-skin structure Collapse (implosion)
Type II Supernova: It is the end of a MASSIVE star (greater than 8M ) whose nucleus collapses because of its own gravity after exhausting all possible nuclear reactionsH → Fe.
Type II Supernova: It is the end of a MASSIVE star (greater than 8M ) whose nucleus collapses because of its own gravity after exhausting all possible nuclear reactionsH → Fe.
Onion-skin structure Collapse (implosion)
Iron Degenerate CoreIron Degenerate Core
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Core collapse Supernova ExplosionCore collapse Supernova Explosion
Kinetic Energy of the explosion ≈ 1% x Etot
Energy of electromagnetic radiation ≈ 0.01% x Etot
Neutrinos ≈ 99% x Etot
Newborn Neutron Star ExplosionNewborn Neutron Star Explosion
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Future Supernovae in our GalaxyFuture Supernovae in our Galaxy
Star Distance Degrees fromequator
Betelgeuse ( α Orionis) 540 lyr +7º
Antares (α Scorpii) 400 lyr -26º
η Carinae 6000 lyr -60º
Eta Carinae: about 150 solar massesand ready to explode…
Eta Carinae: about 150 solar massesand ready to explode…
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The Large Magellanic Cloud [LMC]The Large Magellanic Cloud [LMC]
Large Magellanic Cloud
30 DoradusMilky Way
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SN 1987A in the LMC:A “nearby” supernova (only 170,000 lyrs)
SN 1987A in the LMC:A “nearby” supernova (only 170,000 lyrs)
The 30 Dor Nebula beforeSN 1987A explosion
The 30 Dor Nebula afterSN 1987A explosion
23 February 1987
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The explosion of SN 1987AThe explosion of SN 1987A
Kabooooom!!!
23 February 1987
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First observation with the HST-FOC(Jakobsen et al. 1991)
First observation with the HST-FOC(Jakobsen et al. 1991)
An historical imageof SN 1987A
24 April 1990 24 August 1990
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SN 1987A:its neighborhoodSN 1987A:its neighborhood
HST-WFPC2, Panagia et al 2002
A star cluster 14 million years old
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A family portrait of Supernova 1987A A family portrait of Supernova 1987A
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Supernova 1987Ain the Large Magellanic Cloud(at about 170,000 light years from us: next door!)
Supernova 1987Ain the Large Magellanic Cloud(at about 170,000 light years from us: next door!)
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SN 1987A: 4 years of light curvesSN 1987A: 4 years of light curves
Decay time 111.3 days → Lifetime of 56Co
Total
Ultraviolet
1988 1990 1991 1992
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10 years later the ring started lighting up…
10 years later the ring started lighting up…
More than 20 spotsnow seen to brighten, due to the collision of the ejecta with the central ring.
Over the next decades, as the entire ring will light up, the Evolutionary history of the star’s mass loss will be revealed
1996
2006
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Optical, X-ray, & Radio light curves of SN1987A ring
Optical, X-ray, & Radio light curves of SN1987A ring
optical
radio
X-ray
The fireworks have started! 1990 1995 2000 2005
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What did we learn from SN 1987A?What did we learn from SN 1987A?
• Explosion of a massive star (~18 M )
• The hypothesis of a core collapse with an enormous production of neutrinos is verified
• The production of Ni and the decay into Co and Fe:56Ni→56Co →56Fe, ~0.08M is verified
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Another lesson from SN 1987A…Another lesson from SN 1987A…
• The star was a blue supergiant at the time of the explosion
• The star had been a red supergiant about 10,000 years before exploding
• We haven’t detected yet the stellar remnant, a neutron star
There are quite a number of points thatwe still have to clarify in stellar evolution There are quite a number of points that
we still have to clarify in stellar evolution
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From our neighborhood… to VERY FAR away…
From our neighborhood… to VERY FAR away…
Moving toward supernovae
at the frontiers of the Universe
Moving toward supernovae
at the frontiers of the Universe
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Observing StrategyObserving StrategyGround Based Searches: Observing Strategy
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High Redshift SupernovaeHigh Redshift Supernovae
SN97cj
The CfA SN team: Schmidt, Riess, Kirshner, Garnavich et al.
z = 0.50
SN97cj
Epoch 2 - Epoch 1 = Difference
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High Redshift SupernovaeHigh Redshift Supernovae
By 1999 more than 100 SNIa had been discovered and studied at redshifts higher than 0.3 by two independent groups (Perlmutter et al 1998, 1999; Riess et al 1998)
• SNIa at redshifts 0.3-0.8 appeared to be systematically 0.3 mags dimmer than expected for an empty Universe
• SNIa at redshifts 0.3-0.8 appeared to be systematically 0.3 mags dimmer than expected for an empty Universe
The first results were announced by both teams at the 191st AAS meeting in Washington DC, January 9, 1998The first results were announced by both teams at the 191st AAS meeting in Washington DC, January 9, 1998
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Both teams find that the supernovae at redshift ~0.5 are ~0.3 magnitudes fainter than expectedBoth teams find that the supernovae at redshift ~0.5 are ~0.3 magnitudes fainter than expected
• This suggests that the expansion of the Universe be accelerated, pushed by a “dark energy”, corresponding to ΩΛ ~ 0.7.
• This conclusion is consistent with the measurements of Cosmic Microwave Background
ΩM
Most recent results: Knop et al. 2003
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The Expansion of the UniverseThe Expansion of the Universe
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SN 1997ff : Discovery and SerendipitySN 1997ff : Discovery and Serendipity
• SN 1997ff was discovered by a re-observation of the Hubble Deep Field North (Gilliland, Nugent & Phillips 1999).
• Serendipitously the same field was observed by the NICMOS GTO team, within hours of the SN discovery, and again 25 days later (Thompson et al. 1999).
• The field was observed again six months later (Dickinson et al.)
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An Accelerating Universe?(Riess et al 2001)
An Accelerating Universe?(Riess et al 2001)
• SN 1997ff, at z ~ 1.7, appears to be brighter than expected for an empty Universe!
• Its luminosity is consistent with predictions for a model with ΩΜ ~ 0.3, ΩΛ ~ 0.7 in the deceleration phase.
• The observations are not consistent with models that assume a systematic weakening of SNIa due to either intergalactic dust absorption or to evolution of the intrinsic luminosity,
SN 1997ff suggests an expanding Universe…
←B
right
er |
Fain
ter →
←B
right
er |
Fain
ter →
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Another Supernova in the Hubble Deep Field… and more to come…
Another Supernova in the Hubble Deep Field… and more to come…
“The final answer will be provided by many more high-z SNIa observations, which will confirm, revise or reject the current conclusions.”Freely adapted from the consultation of the doctors at Pinocchio’s sickbed[Collodi: “Le Avventure diPinocchio”]
“The final answer will be provided by many more high-z SNIa observations, which will confirm, revise or reject the current conclusions.”Freely adapted from the consultation of the doctors at Pinocchio’s sickbed[Collodi: “Le Avventure diPinocchio”]
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The Universe is ACCELERATING!The Universe is ACCELERATING!←
Brig
hter
|Fa
inte
r →←
Brig
hter
|Fa
inte
r →
(Riess et al. 2004)(Riess et al. 2004)
g
Universe now expanding ~20% faster than 5 billion years ago THE ACCELERATING UNIVERSE – NOW!
Universe now expanding ~20% faster than 5 billion years ago
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New Cosmological FrameworkNew Cosmological Framework
Geometry & Kinematics:Flat, Ω0=1, accelerating UniverseGeometry & Kinematics:Flat, Ω0=1, accelerating Universe
δρ/ρ produced from Quantum Fluctuations during Inflationδρ/ρ produced from Quantum Fluctuations during Inflation
Composition of our Universe:Dark Energy ΩΛ~ 0.7Dark Matter Ωm~ 0.3Atoms Ωb ~ 1/25
Composition of our Universe:Dark Energy ΩΛ~ 0.7Dark Matter Ωm~ 0.3Atoms Ωb ~ 1/25
Microphysics:Inflation workingMicrophysics:Inflation working
KT 001.0725.20 ±=
Gyrt 2.07.130 ±=11
0 371 −−±= MpckmsH
t0 = 14.5 ±1.5 Gyrs
H0 = 63±6 km s-1 Mpc-1
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The Big Rip puzzle
If the Universe keeps accelerating it will end up breaking into pieces…
The Big Rip puzzle
If the Universe keeps accelerating it will end up breaking into pieces…
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What is going to happen? We are in the dark....
What is going to happen? We are in the dark....
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Meanwhile let’s enjoy the glory…
Gruber Cosmology Prize 2007
Meanwhile let’s enjoy the glory…
Gruber Cosmology Prize 2007