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Astroparticle and Cosmology session

Charling Tao 1st FCPPL Workshop, January 2008. Astroparticle and Cosmology session. 2 hours session : Not a summary of all Astroparticle and Cosmology projects in France, nor Sino-French projects

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Astroparticle and Cosmology session

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  1. Charling Tao 1st FCPPL Workshop, January 2008 Astroparticle and Cosmology session • 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

  2. 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

  3. 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 (ZHOUXu – presently in South Pole) • - Tsinghua University (WANG Xiaofeng –expecting father)

  4. 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

  5. From observations to the Concordance Model SNe Ia CMB(WMAP) Universe is mainly dark LSS ~70% DE and ~25% DM. Definition:W=r/rc (rc=10-29 g/cm3)

  6. SNLS French 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

  7. 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

  8. SNLS first year Hubble diagram 45 nearby SN from literature +71 SNLS SNIa C2/d.o.f=1 with an additional intrinsic dispersion sint=0.13 mag (errors take into account covariance matrix of fitted parameters mB,s,c)

  9. SN Ia use as standard candle? Mag at peak in B filter light curve Light Curve in local reference frame – corrections Galactic extinction correction But SN Ia are not exact standard candles:

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

  11. BUT ARE standardisable to some level before:mB after, eg, stretch : correction mBcor = mB – a (s-1) Different methods of standardisation : stretch (SCP), MLC2k2 (HiZ), Dm15, .DC12..

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

  13. Constraints on cosmological parameters Dm= 0.2 - 0.3 effect! Riess 04

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

  15. 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) • DC12 WANG Xiaofeng , Tsinghua U (2005) Phenomenological observations!

  16. 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!

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

  18. Applications to high-redshift SNLS-1 data

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

  20. SN Ia distances from C12 calibration

  21. DC12 vs SALT standardisation SNLS-1 subsample Strong prior WM=0.27 +/- 0.04 DC12 Compatible with SALT - smaller dispersion (< 0.1) But Indication (>2s) for non LCDM behaviour? Preliminary Contours 95% CL with Kosmoshow (A. Tilquin) Subsample SNLS + nearby (86) Wang Xiaofeng Subsample SNLS + nearby/premax (67)

  22. 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)

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

  24. 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

  25. 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

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