Astroparticle and Cosmology session Charling Tao 1st FCPPL Workshop, January 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 October  A dedicated new LIA with INSU/NAOC + Universities +APC and CPPM - Projects for FCPPL : (history?), SCIENCE, People involved, what support expected from FCPPL

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

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)

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

From observations to the Concordance Model CMB(WMAP) SNe Ia LSS Universe is mainly dark ~70% DE and ~25% DM. Definition:  c (  c = g/cm 3 )

SNLS French Canadian (+ others) collaboration with CFHT Megacam telescope n has already collected >350 (spectro id /VLT+Gemini) SN Ia in ~3 yr. n When combined with BAO, 1st year results on w favor a Cosmological constant as the source of acceleration n 2 more years to go: expect many more SNe! improvement expected in both stat. and systematics What we learnt: n The power of (multicolor & rolling) imaging : SN identification, control of systematics. n Calibration is delicate n Environment matters (also at high-z) n Need improved LC modeling (using SNLS data -> SALT2) n Need unbiased NEARBY sample

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

 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

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:

SNIa are not standard candles SNIa light can be followed-up for many weeks with telescopes

BUT ARE standardisable to some level before: m B after, eg, stretch : correction m Bcor = m B –  (s-1) Different methods of standardisation : stretch (SCP), MLC2k2 (HiZ),  m 15,.  C12..

Precision on the magnitude dominated by intrinsic dispersion:  m int  0.15 Not a big problem  Statistical reduction by number of SN observed Stretch uncorrected Stretch corrected Precision on the magnitude at the maximum

Constraints on cosmological parameters  m= effect! Riess 04

Systematic differences between standardisation methods (Riess et al. 2004)

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!

The distances from standardised SNe Ia distance accuracy around 10% Tonry et al Evidence for good distances, but not good enough for precise cosmology!

The color parameter  C12 as a new luminosity indicator Wang Xiaofen (Tsinghua U) et al. 2005, ApJ, 620, L87

Applications to high-redshift SNLS-1 data

Wang et al. 2005a, ApJ, 620, L87 distance accuracy around 4-5% SN Peak luminosity vs C12

SN Ia distances from  C 12 calibration

 C12 vs SALT standardisation SNLS-1 subsample  C 12 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

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)

Cluster counts Supernovae Baryon Wiggles Cosmic Shear Angular diameter distance Growth rate of structure Evolution of dark matter perturbations Standard ruler Angular diameter distance Standard candle Luminosity distance Evolution of dark matter perturbations Angular diameter distance Growth rate of structure The concordance model stands quite strong! CMB Snapshot at ~400,000 yr, viewed from z=0 Angular diameter distance to z~1000 Growth rate of structure (from ISW)

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

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