Cosmology with Supernovae
description
Transcript of Cosmology with Supernovae
![Page 1: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/1.jpg)
Cosmology with Supernovae
Bruno LeibundgutEuropean Southern Observatory
![Page 2: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/2.jpg)
Outline
Supernova types• core-collapse supernovae• thermonuclear supernovae
Cosmology with supernovae• Hubble constant, H0 lecture I• mapping of the cosmological expansion
history, H(z) lecture II
![Page 3: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/3.jpg)
Supernova observing
![Page 4: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/4.jpg)
Supernovae
Extremely bright stellar explosions
![Page 5: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/5.jpg)
Supernovae
Walter Baade (1893-1960) Fritz Zwicky (1898-1974)
![Page 6: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/6.jpg)
Supernovae
Extremely bright stellar explosionsImportant for the production of the heavy
elements
Big Bang
Stars
Supernovae
![Page 7: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/7.jpg)
Supernovae
Extremely bright stellar explosionsImportant for the production of the heavy elementsBest distance indicators in the universe
The only reliable way of determining extragalactic distances is through supernova investigations.
F. Zwicky
![Page 8: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/8.jpg)
SN 1994D
![Page 9: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/9.jpg)
Supernova classification
Based on spectroscopy
core collapse in massive stars
SN II (H)SN Ib/c (no H/He)Hypernovae/GRBs thermonuclear
explosions
SN Ia (no H)
![Page 10: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/10.jpg)
SupernovaSpectroscopy
Type Ia
![Page 11: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/11.jpg)
Supernova Spectroscopy
Type II
![Page 12: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/12.jpg)
Supernova types
thermonuclear SNe• from low-mass stars
(<8M)• highly evolved stars
(white dwarfs)• explosive C and O
burning• binary systems
required• complete disruption
core-collapse SNe• high mass stars
(>8M)• large envelopes
(still burning)• burning due to
compression• single stars (binaries
for SNe Ib/c)• neutron star
![Page 13: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/13.jpg)
Shaping supernova emission
Light curves as signatures of the energy release in supernovae• energy sources• photon escape• modulations• external effects
ColoursLuminosity
![Page 14: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/14.jpg)
Energy sourcesshock
• breakout• kinetic energy
cooling• due to expansion of the ejecta
radioactivity• nucleosynthesis
recombination• of the shock-ionised material
![Page 15: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/15.jpg)
Importance of light curves
explosion mechanismsenergy sourcesenvironmental effectsprogenitor systemsremnantsdistance determinations and cosmology
![Page 16: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/16.jpg)
Core-collapse supernovae
Suntzeff (2003)
Core collapse
light curve
![Page 17: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/17.jpg)
Expansion
Brightness increase• increased surface area• slow temperature decrease
![Page 18: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/18.jpg)
Recombination
Balance of the recombination wave and the expansion of the ejecta• leads to an extended plateau phase
Hamuy et al. (2001)Hamuy et al. (2001)
![Page 19: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/19.jpg)
![Page 20: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/20.jpg)
Isotopes of Ni and other elements• conversion of -
rays and positrons into heat and optical photons
Diehl and Timmes (1998)
Radioactivity
Contardo (2001)
![Page 21: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/21.jpg)
The variety of SN light curves
Patat et al. (2001)
![Page 22: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/22.jpg)
Distances in the local universeAssume a linear expansion
Hubble law
v=cz=H0·D
![Page 23: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/23.jpg)
A modern Hubble diagram
![Page 24: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/24.jpg)
Universal expansion
![Page 25: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/25.jpg)
Distances in the local universe
Assume a linear expansionHubble law
v=cz=H0·D
Use the distance modulusm-M=5log(D/10pc)-5
Distances of a ‘standard candle’ (M=const.)m=5log(z)+b
b = M+25+5log(c)-5log(H0)
![Page 26: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/26.jpg)
The Hubble constant
Sets the absolute scale of cosmology• replaces these annoying h’s in all the theorists
talksMeasure redshifts and distances in the
nearby universe• Supernovae can do this in two ways:
– Expanding photosphere method of core-collapse SNe– accurate (relative) distances from SN Ia
![Page 27: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/27.jpg)
Expanding Photosphere MethodBaade (1942)Schmidt et al. (1993), Eastman et al. (1996), Hamuy et al. (2001)
Assume homologous expansionR(t)=R0+v(t-t0)
Photometric angular diameter
)(4.02 10)(
ATBf
DR
![Page 28: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/28.jpg)
Distances from EPM
Dtt
vi
i
i 0
Slope gives the distance
Intercept the size of the progenitor and/or time of explosion
![Page 29: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/29.jpg)
Distances from EPMNote that this distance measurement is
completely independent of any other astronomical object!• no distance ladder
Assumption:• massive envelope that creates a photosphere• spherical symmetry
not true for many core collapse supernovae• correction factors for deviation from black
body spectrum model dependent
![Page 30: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/30.jpg)
EPM so far
Limitations• needs large and extensive data sets• difficulties to get into the Hubble flow• distances only to galaxies with supernovae
– difficult to build large sample
Promise• completely independent distance
measurements– checks on the Cepheid distance scale
![Page 31: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/31.jpg)
Distances with Type Ia Supernovae
Use the Hubble diagram (m-M vs. log z)m-M=5log(z)+25+5log(c)-5log(H0)
Note that the slope is given here.
Hubble constant can be derived when the absolute luminosity M is known
logH0=log(z)+5+log(c)-0.2(m-M)
![Page 32: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/32.jpg)
Nearby SNe IaPhillips et al. (1999)
![Page 33: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/33.jpg)
Hubble constant from SNe Ia
Calibrate the absolute luminosity• through Cepheids
– ‘classical distance ladder’– depends on the accuracy of the previous rungs on the ladder– LMC distance, P-L(-C) relation, metalicities
– HST program (Sandage, Tammann)– HST Key Programme (Freedman, Kennicutt, Mould)
• through models– extremely difficult
![Page 34: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/34.jpg)
Testing the SNe Ia as distance indicators
Hubble diagram of SNe Ia in the local, linear expansion, Hubble flow
Calibration through “primary” distance indicators
Theoretical models
![Page 35: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/35.jpg)
Absolute Magnitudes of SNe Ia
SN Galaxy m-M MB MV MI Dm15
1937C IC 4182 28.36 (12) -19.56 (15) -19.54 (17) - 0.87 (10)1960F NGC 4496A31.03 (10) -19.56 (18) -19.62 (22) - 1.06 (12)1972E NGC 5253 28.00 (07) -19.64 (16) -19.61 (17) -19.27 (20) 0.87 (10)1974G NGC 4414 31.46 (17) -19.67 (34) -19.69 (27) - 1.11 (06)1981B NGC 4536 31.10 (12) -19.50 (18) -19.50 (16) - 1.10 (07)1989B NGC 3627 30.22 (12) -19.47 (18) -19.42 (16) -19.21 (14) 1.31 (07)1990N NGC 4639 32.03 (22) -19.39 (26) -19.41 (24) -19.14 (23) 1.05 (05)1998bu NGC 3368 30.37 (16) -19.76 (31) -19.69 (26) -19.43 (21) 1.08 (05)1998aq NGC 3982 31.72 (14) -19.56 (21) -19.48 (20) - 1.12 (03)Straight mean -19.57 (04) -19.55 (04) -19.26 (0 6)Weighted mean -19.56 (07) -19.53 (06) -19.25 (0 9)
Saha et al. 1999
![Page 36: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/36.jpg)
Dm15 relation Phillips (1993), Hamuy et al. (1996), Phillips et al. (1999)
MLCSRiess et al. (1996, 1998), Jha et al. (2003)
stretchPerlmutter et al. (1997, 1999), Goldhaber et al. (2001)
MAGICWang et al. (2003)
Light curve shape – luminosity
![Page 37: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/37.jpg)
Altavilla, Thesis
![Page 38: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/38.jpg)
The magic of the light curve shapes
Goldhaber et al. 2001
![Page 39: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/39.jpg)
B
V
I
The SN Ia luminosity can be normalised
Bright = slow Dim = fast
Riess et al. 1996
![Page 40: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/40.jpg)
Phillips et al. 1999
Correlations
![Page 41: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/41.jpg)
Normalisation of the peak luminosity
Phillips et al. 1999
Using the luminosity-decline rate relation one can normalise the peak luminosity of SNe Ia
![Page 42: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/42.jpg)
SN Ia CorrelationsLuminosity vs. decline rate
• Phillips 1993, Hamuy et al. 1996, Riess et al. 1996, 1998, Perlmutter et al. 1997, Goldhaber et al. 2001
Luminosity vs. rise time• Riess et al. 1999
Luminosity vs. color at maximum• Riess et al. 1996, Tripp 1998, Phillips et al. 1999
Luminosity vs. line strengths and line widths• Nugent et al. 1995, Riess et al. 1998, Mazzali et al. 1998
Luminosity vs. host galaxy morphology• Filippenko 1989, Hamuy et al. 1995, 1996, Schmidt et al. 1998, Branch et al.
1996
![Page 43: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/43.jpg)
SN Ia Correlations
Drell et al. 2000
Riess et al. 1998
Phillips et al. 1999
Perlmutter et al. 1997
![Page 44: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/44.jpg)
SN Ia Correlations
Leibundgut 2000
![Page 45: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/45.jpg)
The nearby SN Ia sample
Evidence for gooddistances
![Page 46: Cosmology with Supernovae](https://reader036.fdocuments.us/reader036/viewer/2022062502/56814c2b550346895db930b0/html5/thumbnails/46.jpg)
Hubble constant from SNe Ia
Extremely good (relative) distance indicators• distance accuracy around 10%
Uncertainty in H0 mostly on the LMC and the Cepheid P-L relation