astroparticle and cosmology session charling tao 1st fcppl workshop, january 2008 - 2 hours session...
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Astroparticle and Cosmology session
Charling Tao
1st FCPPL Workshop, January 2008
- 2 hours session :
Not a summary of all Astroparticle and Cosmology projects in France, nor Sino-French projects
Refer to recent Sino French Conference on Origins 15-20 October 2007 http://origins.obspm.fr
A dedicated new LIA with
INSU/NAOC + Universities +APC and CPPM
- Projects for FCPPL: (history?), SCIENCE, People involved, what support expected from FCPPL
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1st workshop: Astroparticle and
cosmology
- SVOM: the present status Stéphane BASA (LAM)
- The POLAR Project Jean-Pierre VIALLE (LAPP)
- DARK Matter Phenomenology Julien Lavalle (U.Torino, CPPM)
- AMS and related topics Chen GuoMing (IHEP)
- Cosmic rays with radiotelescopes in China Olivier MARTINEAU-HUYNH
(LPNHE- Paris 6)
- Determination of cosmological parameters André Tilquin (CPPM)
- Astrophysics with particle physics detectors - Particle physics issues with astrophysics tools
Thanks to Prof. Chen Hesheng for his support in his Tuesday presentation: Non Accelerator physics is an important part of Particle Physics
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Marseille cosmology group CPPM/LAM/CPT
- active in with many other collaborators
+ Dark Energy Phenomenology (cf André Tilquin CPPM)
+ SVOM (cf Stéphane Basa LAM)
+ Supernovae projects :
SNLS, SNF, SNAP, Dome C/A in South Pole + …
- NAOC (ZHOU Xu – presently in South Pole)
- Tsinghua University (WANG Xiaofeng –expecting father)
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Young people involved in our SF observational cosmology cooperations
* Postdoc in LPHNE/ SNF WU Chao
* Cotutored PhD Students from French Ministry of Foreign Affairs
- ZHANG TianMeng (LAM Stéphane Basa /NAOC Zhou Xu) / SNLS
- SUN Lei (PKU FAN Zuhui/ CPPM C. TAO) / Systematics of Weak Lensing, Baryon Oscillations, SN and their impact on the determination of dark energy parameters
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From observations to the Concordance Model
CMB(WMAP)
SNe Ia
LSS
Universe is mainly dark
~70% DE
and
~25% DM.
Definition: c (c=10-29
g/cm3)
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SNLSFrench Canadian (+ others) collaboration with CFHT Megacam telescope
has already collected >350 (spectro id /VLT+Gemini) SN Ia in ~3 yr.
When combined with BAO, 1st year results on w favor a Cosmological constant as the source of acceleration
2 more years to go: expect many more SNe!
improvement expected in both stat. and systematics
What we learnt:
The power of (multicolor & rolling) imaging : SN identification, control of systematics.
Calibration is delicate
Environment matters (also at high-z)
Need improved LC modeling (using SNLS data -> SALT2)
Need unbiased NEARBY sample
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Low Red Shift (Z < 0.1) Supernova factory (SNF)
• Berkeley/Paris/Lyon/Lyon/Yale + LAM+CPPM +… Collab• Purpose
–Discover a large number (500 or more) nearby TypeIa Supernovae–Redshift range 0.03 to 0.08–Take spectrum of each Sne every 4 days or so
• Scientific Goals–Anchor Hubble Diagram for large Hi-z Surveys–Systematic study of TypeIa Supernovae Spectroscopic Follow-up– Spectroscopy Hawaii 2.2 m (Supernova Factory)
Todate, more than 100 well followed up SNIa
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2/d.o.f=1 with an additional intrinsic dispersion
int=0.13 mag
(errors take into account covariance matrix of fitted parameters m
B,s,c)
45 nearby SN from literature+71 SNLS SNIa
SNLS first year Hubble diagram
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Mag at peak in B filter
SN Ia use as standard candle?
light curve
Light Curve in local reference frame – corrections
Galactic extinction correction
But SN Ia are not exact standard candles:
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SNIa are not standard candles
SNIa light can be followed-up for many weeks with telescopes
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BUT ARE standardisable to some level
before: mB after, eg, stretch : correction mBcor = mB – (s-1)
Different methods of standardisation :
stretch (SCP), MLC2k2 (HiZ), m15, .C12..
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Precision on the magnitude dominated by intrinsic dispersion:
mint 0.15Not a big problem Statistical reduction by number of SN observed
Stretch uncorrected
Stretch corrected
Precision on the magnitude at the maximum
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Constraints on cosmological parameters
m= 0.2 - 0.3 effect!Riess 04
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Systematic differences between standardisation methods (Riess et al. 2004)
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SNe Ia correlations standardisation methods
m15 relation BATM
Phillips (1993), Hamuy et al. (1996), Phillips et al. (1999), Prieto et al. (2006)
•MLCS MLCS2k2
Riess et al. (1996, 1998), Jha et al. (2002, 2006)
•Stretch SALT
Perlmutter et al. (1997), Goldhaber et al. (2001), Guy et al. (2005)
• C12 WANG Xiaofeng , Tsinghua U (2005)
Phenomenological observations!
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The distances from standardised SNe Ia
distance accuracy around 10%
Tonry et al. 2003
Evidence for good distances,
but not good enough for precise cosmology!
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The color parameter C12 as a new luminosity indicator
Wang Xiaofen (Tsinghua U) et al. 2005, ApJ, 620, L87
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Applications to high-redshift SNLS-1 data
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Wang et al. 2005a, ApJ, 620, L87
distance accuracy around 4-5%
SN Peak luminosity vs C12
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SN Ia distances from C12 calibration
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C12 vs SALT standardisation SNLS-1 subsample
C12 Compatible with SALT
- smaller dispersion (< 0.1)
But
Indication (>2) for non CDM behaviour?
Contours 95% CL with Kosmoshow (A. Tilquin)
Subsample SNLS + nearby (86) Wang Xiaofeng
Subsample SNLS + nearby/premax (67)
Strong prior M=0.27 +/- 0.04
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Questions raised from this comparison analysis
Systematic checks
-Need More statistics !!!! from both hi z AND Nearby SN
Involvement in SNF
(1 Chinese postdoc Chao WU in LPNHE)
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Cluster counts
Supernovae
Baryon Wiggles
Cosmic Shear Angular diameter distanceGrowth rate of structure
Evolution of dark matter perturbations
Standard ruler
Angular diameter distance
Standard candleLuminosity distance
Evolution of dark matter perturbationsAngular diameter distanceGrowth rate of structure
The concordance model stands quite strong!
CMBSnapshot at ~400,000 yr, viewed from z=0
Angular diameter distance to z~1000
Growth rate of structure (from ISW)
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Other Apologies for absences
- Dark Energy phenomenology partners:
- ZHANG XinMin, (IHEP) : health problems
- FAN Zuhui (PKU) and ZHU Zong-Hong (Beijing Normal U.) Teaching duties exam week
- 21CMA: light of first stars + CR with radioantennas
WU XiangPing Passport problem , future codirector of NAOC/INSU LIA
- SVOM (ZHANG ShuangNan + WU Bobing, IHEP) : Very important funding review for SVOM decided Jan. 4 for this week
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1st workshop:Astroparticle and
cosmology
- SVOM: the present status Stéphane BASA (LAM)
- The POLAR Project Jean-Pierre VIALLE (LAPP)
- DARK Matter Phenomenology Julien Lavalle (U.Torino, CPPM)
- AMS and related topics Chen GuoMing (IHEP)
- Cosmic rays with radiotelescopes in China Olivier MARTINEAU-HUYNH
(LPNHE- Paris 6)
- Determination of cosmological parameters André Tilquin (CPPM)- Astrophysics with particle physics detectors
- Particle physics issues with astrophysics tools