A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP,...
-
Upload
abraham-thompson -
Category
Documents
-
view
228 -
download
0
Transcript of A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP,...
![Page 1: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/1.jpg)
A Step towards Precise Cosmology from Type Ia Supernovae
Wang Xiaofeng
Tsinghua University
IHEP, Beijing, 23/04, 2006
![Page 2: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/2.jpg)
Outlines
• What is Supernova?
• The light curve properties of SNe Ia
• The empirical calibration methods for SNe Ia
• New cosmological distances from SNe Ia and the implications for cosmology
![Page 3: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/3.jpg)
Supernova Explosion!
SN 2005mf
![Page 4: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/4.jpg)
Supernova Search 300-400/year since 1998
A New record: 365 in 2005!
![Page 5: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/5.jpg)
SN classificationsTaxonomy Chart Spectroscopic classifications
![Page 6: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/6.jpg)
Stellar evolution and supernova explosion
![Page 7: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/7.jpg)
Type Iasupernovaewhite dwarf in binary stellar system
high H accretion rates
growing C/ O white dwarf
~Chandrasekhar mass (1.4 Msolar) contraction
high central density C fusion
thermonuclear explosion
![Page 8: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/8.jpg)
Type I a: WD defl agration
Expanding, cooling optically-thick shell: 56Ni 56Co
cooling optically-thin: 56Co 56Fe
57Co, 44Ti, 22Na decay
Supernova Light curves
![Page 9: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/9.jpg)
Riess et al. 1999
![Page 10: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/10.jpg)
Raw Hubble diagram of SNe Ia
![Page 11: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/11.jpg)
Luminosity Function of SNe Ia
(wang et al. 2005b)
![Page 12: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/12.jpg)
The environmental effect on SN luminosity
![Page 13: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/13.jpg)
SN Ia correlations m15 relation BATM
Phillips (1993), Hamuy et al. (1996), Phillips et al. (1999)
• MLCS MLCS2k2
Riess et al. (1996, 1998), Jha et al. (2003)
• Stretch SALT
Perlmutter et al. (1997), Goldhaber et al. (2001), Guy et al. (2005)
• C12 method Wang et al. (2005a, b)
![Page 14: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/14.jpg)
The template method (Phillips 1993, Hamuy et al. 1996)
![Page 15: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/15.jpg)
The light curve fitting by template
![Page 16: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/16.jpg)
Luminosity vs. decline rate Piskovski-Phllips relation
Phillips et al. 1999
![Page 17: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/17.jpg)
The SN Ia luminosity can be normalised
Bright = slow Dim = fast
B
V
I
Riess et al. 1996
MLCS method
![Page 18: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/18.jpg)
Stretch factor method
Goldhaber et al. 2001
stretch
![Page 19: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/19.jpg)
The reasons underlying the light curve correlation
SN MB log(L) M(Ni)
SN1989B -19.37 43.06 0.57SN1991T -19.76 43.23 0.84SN1991bg -16.78 42.32 0.11SN1992A -18.80 42.88 0.39SN1992bc -19.72 43.22 0.84SN1992bo -18.89 42.91 0.41SN1994D -18.91 42.91 0.41SN1994ae -19.24 43.04 0.55SN1995D -19.66 43.19 0.77
Deductions
Slower SNe Ia are more luminous
--more energy radiated
More luminous SNe Ia have slower declines at late phases (Phillips et al. 1999, Contardo et al. 2001)
-- slower release of the energy
Slower SNe Ia have larger expansion velocities (Mazzali et al. 1998)
--less efficient trapping of -rays
Contardo et al. 2000; data for SN 1991 from Strolger et al. 2002
![Page 20: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/20.jpg)
The nearby SNe Ia
distance accuracy around 8-12%
Evidence for good distances, but not good enough for precise cosmology
Tonry et al. 2003
![Page 21: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/21.jpg)
The post-maximum color calibration(Wang et al. 2005)
![Page 22: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/22.jpg)
SN Peak Luminosity vs. C12
distance accuracy around 4-5%
![Page 23: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/23.jpg)
Treatment of the host galaxy reddening
![Page 24: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/24.jpg)
![Page 25: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/25.jpg)
Non-standard dust in other galaxies (Wang et al. 2006a) Smaller than the standard
values of 5.5 in U, 4.3 in B, 3.3 in V, and 1.8 in I in the Milkyway
SN explosion may change the size of the dust grains or the distribution of the dust in CSM
![Page 26: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/26.jpg)
Second parameter correlations
![Page 27: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/27.jpg)
The residual correlations
![Page 28: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/28.jpg)
The Most Precise Hubble diagram from SNe Ia
![Page 29: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/29.jpg)
•Normalising Type Ia Supernovae
–light curve and color curve shape corrections
•what is the determining parameter?–Ni mass trapped energy light curve shape (affected also by opacity?)
–temperature colour
–explosion mechanism?
•What are the subluminous objects? a faint end of normal or distinct type ?
![Page 30: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/30.jpg)
Applications to SNLS data
![Page 31: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/31.jpg)
Comparison between different methods: magnitudes at maximum
(TF Vs. SF)
![Page 32: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/32.jpg)
C12 vs. Stretch factor
![Page 33: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/33.jpg)
distribution of Color parameters and Extinction
Nearby vs. distant
C12: 0.44 vs. 0.33
E(B-V)host: 0.062vs.0.077
![Page 34: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/34.jpg)
Calibration difference
![Page 35: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/35.jpg)
Correcting relations
conditions bB RB bV RV
All(excl. 91bg-like) 1.69(10) , 3.45(11) 1.47(10), 2.43(12)
If E(B – V) < 0.40 mag 1.64(09), 2.84(18) 1.43(10), 1.81(20)
If E(B – V) < 0.30 mag 1.60(10), 2.93(22) 1.42(10), 1.86(22)
If E(B – V) < 0.20 mag 1.65(10), 2.90(27) 1.45(10), 2.06(28)
![Page 36: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/36.jpg)
Hubble diagram from C12 calibration
![Page 37: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/37.jpg)
Cosmological results (for 131 well-sampled SNe Ia)
N Fit parameters(C12) parameters(salt) 84 (m, (m,flat
(m, (m,flat
![Page 38: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/38.jpg)
m- contour
![Page 39: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/39.jpg)
m- w contour
![Page 40: A Step towards Precise Cosmology from Type Ia Supernovae Wang Xiaofeng Tsinghua University IHEP, Beijing, 23/04, 2006.](https://reader031.fdocuments.in/reader031/viewer/2022020106/56649e5d5503460f94b56b10/html5/thumbnails/40.jpg)
New result