1. Sino-French collaboration on the Dark Universe Charling Tao CPPM/IN2P3/CNRS Visiting professor, Director Tsinghua Center for Astrophysics + Zhang Xinmin (IHEP) April 2011 Jinan, FCPPL workshop

2. A mysterious Dark Universe CMB(WMAP) SNe Ia LSS Universe is mainly dark ~70% DE and ~25% DM. Definition:  c (  c =10 -29 g/cm 3 ) We measure with percent precision the extent of our ignorance

3. A quick history of S-F collaborations on DU 1991: First sino-french workshop on Dark Matter in IHEP and collaboration on DM Beijing- Paris-Roma-Saclay  infamous DAMA! 2011: New Sino-french collaboration on underground laboratories 2004 and 2005: Workshops on galaxy formation and evolution 2005 and 2006: Sino-French workshop on the Dark Universe in Marseilles and Beijing  SVOM, POLAR, projects + phenomenology collaboration + SN seeds After 2006 : FCPPL meetings (mainly IN2P3/IHEP + Univ) After 2008: LIA Origins (mainly INSU/NAOC + Univ) 4 years of FCPPL

4. Dark Universe Projects 2006-2010 SVOM/ECLAIRS : (Many partners) cf B. Cordier POLAR: JP Vialle (LAPP) + IHEP/Tsinghua (Zhang ShuangNan) (AMS: LAPP + IHEP + …) SN -Participation of young Chinese in SNLS and SNFactory +Wang Xiao-Feng(Tsinghua) /Reynald Pain (LPNHE)/CT(CPPM) + Zhang TianMeng thesis finished 2010 Zhou Shu (NAOC)/S. Basa(LAM) +Wu Chao post doc LPNHE, now NAOC /SVOM + visits CPPM + Deng Jinsong visits to CPPM, now SVOM DM phenomenology : -Bi Xiaojun (IHEP) et al + D.Maurin (LPNHE/LPSC) + J. Lavalle (CPPM) + Salati (LAPP) 1 paper

5. Full Calculation of Clumpiness Boost factors for Antimatter Cosmic Rays in the light of Lambda-CDM N-body simulation results. Abandoning hope in clumpiness enhancement? J. Lavalle, Q. Yuan, D. Maurin, X.J. Bi, Astron.Astrophys.479:427-452,2008 (citation 95 today) DM subhalos in galaxy are predicted by N-body simulation. DM annihilation rate is increased by the subhalos We calculate the enhancement based on the simulation results.

6. Dark Universe Projects 2006-2010 SVOM/ECLAIRS GRB : cf B. Cordier (IRFU)/ Wei JianYan (NAOC) POLAR: JP Vialle (LAPP) + IHEP/Tsinghua (Zhang ShuangNan) (AMS: LAPP + IHEP + …) SN -Participation of young Chinese in SNLS and SNFactory +Wang Xiao-Feng(Tsinghua) /Reynald Pain (LPNHE)/CT(CPPM) + Zhang TianMeng thesis finished 2010 Zhou Shu (NAOC)/S. Basa(LAM) +Wu Chao post doc LPNHE, now NAOC /SVOM + visits CPPM + Deng Jinsong visits to CPPM, now SVOM DM phenomenology : -Bi Xiaojun (IHEP) et al + D.Maurin (LPNHE/LPSC) + J. Lavalle (CPPM) + Salati (LAPP) 1 paper -Qin Bo et al (NAOC) + Tilquin + CT (CPPM) 2 papers, collaboration ongoing without special request to FCPPL, now mainly LIA Origins Multiprobe determination of cosmological parameters: 3 papers + 1 in prep Sun Lei thesis finished 2009 : Zuhui Fan (PKU)/ C. T (CPPM) French + Chinese Jury together (first? Only?)

7. What is Dark Energy? Cosmological Constant??? New form of « field/matter? » Quintessence? Unified Dark Matter? Modified Gravity/GR ? - Non minimal Couplings? - Extra-Dimensions? - Anisotropy/ inhomogeneity effects? - Negative energy? How to distinguish them? - w(z) = p/  w=cte= -1 w(z) Effective w(z) Particle physicist bias

8. Only w(z) Probably too naive ! LSS formation and evolution are probes of initial perturbations and DE! Need not only w(z), but also growth rate, and understanding of non-linear features.

9. Measuring dw/dz = a challenge ! Motivation= separate the different theoretical interpretations A difficult estimate (  w’ < 10 %) Hypothesis to control w=p/  parametrisation –Other cosmoogical parameters  m … –Sensitivity to systematics to % A necessity.. Compare and combine probes Identify, evaluate and reduce systematical effects

10. 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)

11. Power of Combinations astro-ph 0609591 DE Task force

12. Current constraint on the equation of state of dark energy WMAP7+SDSS(DR7)+SN Ia (Union2) Li Hong et al

13. Constraints on other cosmological parameters: Li Hong et al (WMAP7+SDSS+SN Ia –Union2)

14. DARK ENERGY: MULTIPROBE Global Analysis using EGEE and EUCHINA data grids Sino French collaboration CPPM/CPT/IHEP/PKU/NAOC/ Beijing Normal U. + collaborators A.Tilquin, Sun Lei, Fan Zuhui, Li Hong, Zhang XinMing + CT+ … Sun Lei’s Thesis

15. 2 by 2 combinations (  T =1) At the moment, SNIa are best

16. 3 by 3 combinations (  T =1) BAOSN WL WMAP Best 3 probe combination today!

17. Beware of error determinations! eg, Plot from Spergel et al astro-ph/0603449, WMAP3: Tension: WMAP3, & Weak Lensing CFHTLS first results Beware when central values do not coincide! - Systematics - Theoretical bias - Analysis bias - Or indication for new physics? The game is not always to have the smallest error bars… NB: Tension disappeared with more recent CFHTLS data: Fu Liping et al, …

18. SN Union sample (Kowalski et al.2008) vs “WMAP+BAO+WL fit” Colours correspond to different error estimates on combined fit Probes are compatible within large error bars High z : statistics not sufficient! galaxy subtraction? contamination SN a little bit too bright at high z ? (<5%)

19. (CMB+BAO+WL)%SN-CONSTITUTION More nearby and selected sub-sample of the Union SNIa at z>1 Better agreement at z>1 Indicates problems with Union high z sample 1  prediction Best SN fit  CDM SN best fit:  m =0.29+/-0.02 CONSTITUTION

20. (CMB+BAO+WL)%SN2009 Use SDSS SN sample at intermediate z More restricted selection of SNIa at high z Perfect agreement between CMB+BAO+WL prediction and SNIa +/-1  prediction Best SN fit  CDM SN best fit:  m =0.29  0.02

21. Measure dw/dz = a challenge ! Motivation= separate the different theoretical interpretations A difficult estimate (  w’ < 10 %) Hypothesis to control w=p/  parametrisation –Other cosmoogical parameters  m … –Sensitivity to systematics to % A necessity.. Compare and combine probes Identify, evaluate and reduce systematical effects in as many complementary probes as possible

22. CMB: Planck But do not expect much improvement on w(z). Check WMAP anomaly (cf Li Ti Pei’s presentation)? Type Ia Supernovae: d L (z) to z  1.5 Key issue is physics/evolution: do we understand SNe Ia? Weak lensing: G(t) to z  1.5 Promising; requires photo-z’s Key issues are fidelity, stability of psf, calibration Cluster counts: d A (z), H(z) - accuracy/non-linearities? Baryon “wiggles”: d A (z), H(z) to z=3 Late developer: cleanest but requires huge surveys AP test ISW effect Pairs of galaxies : Christian Marinoni + Adeline Buzzi (CPT+CPPM ) How can w(z) be better measured?

23. 2015 CMBWMAP 2/3WMAP 7 Planck ClustersAMI SZA APEX AMIBA SPT ACT DES Supernovae Pan-STARRS DESLSSTSNLS-ESSENCE Spectroscopy SKA FMOS SDSS ImagingCFHTLS ATLASKIDSJDEM LSSTSKA SDSS SUBARU 2005 2015 SDSS XCS EUCLID 2010 Subaru DLS LAMOST DES, VISTA Pan-STARRS Hypersuprime Surveys to measure Dark Energy KDUST BigBoss KDUST BOSS + SNF

24. DE: future Need large full sky surveys New/improved probes testing basic cosmology assumptions AND studies of systematics

25. WMAP - 7 years Jarosik et al. arxiv 1001.4744 Better measurements of 3rd peak.

26. WMAP7 vs WMAP5  CDM parameters Larson et al. arxiv:1001.4635 Not much has changed on cosmological parameters!

27. Inconsistency with WMAP quadrupole determination? Due to quaternion interpolation offset: Liu and Li arXiv 1003.1073 Liu and Li arXiv 0907.2731 Consequences on cosmological parameters!

28. New project requesting funding from FCPPL Supernovae Factory II Cf Wang Xiaofeng’s presentation Zhang Tianmeng, Wu Chao, Deng Jinsong, André Tilquin, Dominique Fouchez, Stéphane Blondin, Gerard Smadja, Yannick Copin, Rui Pereira, Nicolas Chotard, Emmanuel Gangler Support for SN workshop end 2011 requested from FCPPL, LIA Origins + Tsinghua +… In LIA structure: how to support thematic workshops ? generate participation from astro/cosmo community

29. DM/ Underground laboratory collaboration project supported by FCPPL Tsinghua, IHEP, Sichuan, LSM, IRFU Cf presentations by Yue Qian and Ioannis Giomataris Mostly Particle Physicists interest What about a DM project collaboration? Edelweiss is open to Chinese collaborators, CDEX or Panda-X (Ni Kai Xuan) welcome French participants R&D for future : Directional low pressure TPC’s for DM signature Cf MIMAC with Micromegas (Daniel Santos)

30. New projects approved by LIA Origins Antarctica : Dome A/Dome C collaboration Chinese Center for Astrophysics in Antarctica (many Chinese institutions, including IHEP, Tsinghua…) + Nice/CPPM + … Astrophysical and cosmological constraints on DM Zhang XinMin, Bi XiaoJun, Fan Zuhui, Shan HuanYuan, Qin Bo, Jean Paul Kneib + Zhan Hu + Fu Liping + CT + … Analysis of weak lensing data and comparison with N-body simulations (support requested to NSFC + Tsinghua+ LIA Origins) Initial contacts have been supported by FCPPL/CPPM/LAM

31. Other DU Projects under discussion between Chinese and French scientists -DM detectors: Panda-X, Low pressure TPCs, … -CMB analysis? (cf Prof. Li Ti Pei’s talk and Planck) -LSST -AST3/KDUST Antarctica optical and IR surveys -New ideas for mini-multiobjects Spectrographs

32. Conclusions Many requests for support: strong interest in collaboration from French scientists. French level of support from CNRS Luckily Chinese support for science has increased Good news : Physics will be included in ANR-NSFC agreement! Support for thematic workshops missing in FCPPL

33. Physics department Engineering Physics department Computer Science Department THCA 高能功物说 IHEP CPPM ( 法国 ) + NAOC + …. Li Tipei and Shang Renchen 2001 http://cfa.tsinghua.edu.cn/

34. THCA Research topics Broad range of data analysis efforts Projects: –HXMT –80 cms TNT (Tsinghua National observatory of China Telescope ） Xinglong –LIGO gravitational wave –Dark Universe 暗宇宙 Jinping CDEX DM direct detection 暗物质直接检测 SNFactory LSST ， EUCLID DomeA Antarctica Center - 南极天文中心 ~ 50% of THCA faculty attended FCPPL Jinan! Record?

35. 谢谢！ Participants for listening to me Shandong U. Organizers for their patience and hospitality. Apologies for being a single day participant! Jin Shan and Lydia for their efforts for FCPPL Chen Gang and Olivier for accepting the burden