Supernovae: Lighthouses of the Cosmos

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

8 January 2008 Nino Panagia STScI/INAF-CT/SN Ltd

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Observing the StarsObserving the Stars


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Chichen-Itzà (Yucatan)A Mayan Observatory

Chichen-Itzà (Yucatan)A Mayan Observatory


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Stonehenge (England)Stonehenge (England)


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Galileo ‘600Galileo ‘600


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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)

The Hubble Space Telescope (HST)The Hubble Space Telescope (HST)

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…


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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Supernova 1006…Supernova 1006…


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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


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Supernova 1999gn in NGC 4303

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

The most distant supernova, SN 1997ffThe most distant supernova, SN 1997ff


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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

MODELS OF EXPANDING UNIVERSE - 10 YRS AGO

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

SUMMARY…


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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


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THE ENDTHE END

Supernovae: Lighthouses of the Cosmos

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