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Tsinghua Center for Astrophysics and the Dark Universe: Science, People, Projects Charling Tao THCA / CPPM LIA Origins 2012 –La Londe les Maures Centre de Physique des Particules de Marseille CPPM Unité Mixte de Recherche 6550 CNRS/IN2P3-Université de la Méditerranée Marseille, France ANTARES detector KM3 10 lines with 30 floors: 900 Optical Modules Optical Module triplet DM, n astrophysics Ground Station- La Seyne sur Mer Time calibratio n LED Beacon Local electroni c ~60m Bouée 2500m Câble électro-optique sous marin de ~ 40km Hydrophone 300m active Conteneur électronique Câbles de raccordement ~100m Boite de jonction lest Balises acoustiques THCA http://www.thca.tsinghua.edu.cn/ 2001 Li Tipei • IHEP Shang Rencheng Zhang ShuangNan, Lou Yuqing Feng Hua, Zhang Youhong, Zhou Jianfeng … • Physics dept • Eng.Phys dept Since 2010, CT Wang Xiaofeng, Hu Jian +… Postdocs, students,.. Benefit from Tsinghua U. environment • Physics Department: Particle theory, fundamental physics, atomic/molecular physics, new technology,… • Engineering Physics department + since 2010 • Computing department • Precision Instruments department: TMT+ spectrographs +… • (School of space and aviation: ?) Emphasis on R&D and new technologies? My mission for Tsinghua University: Evaluate the possibilities for THCA development into an international level astrophysics center Understanding the Dark Universe: astroparticle, Cosmology and gravity physics – – – – – Multiwavelength astroparticle physics :X-ray, gamma-ray, FAST,… SN astrophysics Multiprobe Cosmology: CMB, SN, WL, Clusters, BAO,… DM: JinPing collaboration on low background environment, R&D TPC Gravitational wave research :LIGO Collaborations… + IHEP + MOUs signed since 2011 with: • NAOC • China Antarctica Astrophysics Center • SNFactory + Collaborations with France: • France China Particle Physics Lab • Official participation to LIA Origins Academic issues • Teaching: “Astrophysics path” within Faculty of Sciences – Need more faculty to offer a complete undergraduate and graduate school programme… – Need more students! Tsinghua Undergraduates are among best in the world,eg 2012 Hubble fellows : 3(/17) were undergraduates in Tsinghua U. Goal in the longer term: (Astrophysics Department?) • 20 undergraduate students/year • 20 graduate students/year • Search for faculty (non-chinese are welcome) Broad range of data analysis efforts – Sources of data: • • • • Chandra, XMM-Newton, XTE, ASCA, BATSE, EGRET, WMAP, Planck, SDSS, 2dF, NVSS, CFHTLS, SNFactory,Lick Observatory TNT – Astrophysical objects and cosmological probes • The Sun, X-ray binaries, gamma-ray bursts, galaxies, AGNs/QSOs, • clusters of galaxies, large scale structures, CMB, SN, weak lensing,… – Phenomenology • Dark Matter and Dark Energy • Gravitational wave THCA Research projects - HXMT – 80 cms TNT (Tsinghua National observatory of China Telescope)Xinglong – LIGO gravitational wave (French visitor: E.Lebigot) – FAST – Dark Universe . SNFactory + … French postdoc in NAOC/THCA: N. Chotard . EUCLID . DomeA Antarctica with AST3 and KDUST (Wang Xiaofeng) . Jinping DM direct detection (Yue Qian et al…): CDEX +…? – IFU Spectrographs for TMT,+ other? The hard X-ray modulation telescope HXMT • HXMT is a wide band (1-250 keV) X-ray observatory, all-sky survey with high angular LE (1-15 keV SCD 400 cm2) resolution and sensitivity Collimator 1°× 6° Launch in 2015 HE (20-250 keV NaI/CsI 5100 cm2) ME Official administrative launch 2 days ago! (5-30 keV SiPIN 1000 cm2) Xinlong 80 cms TNT 2003 SN Ia Light curve • Transient research:SN, GRB afterglow,AGN • Very useful pedagogical training tool for students A mysterious Dark Universe ! What we know is only 4% of the energy density of the Universe We now measure with precision the amount of our ignorance ! Graph source: Wikipedia Definition: W=r/rc (rc=10-29 g/cm3) A concordance LCDM model Multi-probe concordance : CMB, + SN, clusters, galaxies redshift surveys, Weak Lensing, … Concordance LCDM model with Cold Dark Matter and Cosmological constant (or DE) 2/3 Dark Energy 1/3 Dark Matter SNIa and Cosmology 1998 SURPRISE: Indication for negative deceleration parameter q0 Acceleration!!! But only 2s effect! At the time B magnitude at maximum W = r(t)/rc(t) = WM+ WL = 1- Wk WL = L/3H02 q0= 1/2 WM- WL < 0 Hubble diagram Redshift z Supernovae type Ia Best known « standard » candles Red giant White dwarf Chandrasekhar mass 1.4 MO SNIa : 2 stars accretion (a white dwarf +…) Chandrasekhar mass 1.4 MO What is this Dark Energy? New form of « field/matter? » Modified Gravity/GR ? Unified Dark Matter? - Non minimal Couplings? Quintessence? Cosmological Constant??? w =-1 How to distinguish them? - equation of state w(z) = p/r - Extra-Dimensions? - Anisotropy/ inhomogeneity effects? - Negative energy? - …. A problem for field theorists Value of cosmological constant L ! • General Relativity X L scale X • Cosmological measurements 1 GeV = 1.6 10-10 Joules rLobs ~ (10-12 GeV)4 = 2 x 10-17 J/cm3 • Particle physics L ~ vacuum energy vacuum = perfect fluid p= -rL= - L/(8pG) rLEW ~ (200 GeV)4 = 3 x 1040 J/cm3 rLQCD ~ (0.3 GeV)4 = 1.6 x 1029 J/cm3 rLPl ~ (1018 GeV)4 = 2 x 10103 J/cm3 Difference ~ 120 orders of magnitude ! rLobs ~ (10-12 GeV)4 ~ (meV)4 Coincidence with Neutrino scale? Latest results SNLS3 + other SNIa Conley et al. Jan 2011 Flat Universe and Constant w SNIa: best single probe constraint on EoS todate Power of Combinations DE Task force astro-ph 0609591 Dark Energy phenomenology: some milestones • 2006, DETF Report (Albrecht et al.): use multiple probes to control systematics. Identified 4 “best” probes: • Sn-Ia (as standard candles) • BAO (as standard ruler) • Clusters (H(z) + growth) • Weak Lensing (H(z)+ growth) • w(z) is main goal • 2005-2007: DE could be a mirage of modified gravity: need to measure w(z) and f(z) independently • 2009, FoMSWG Report (Albrecht et al.): importance of multiple probes, independent w(z) and f(z) and broad discovery space use of single FoM discouraged • 2011 EUCLID chosen by ESA Gigi Guzzo 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 Cosmic Shear Standard candle Luminosity distance Evolution of dark matter perturbations 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 How can w(z) be better measured? • CMB: Planck • Type Ia Supernovae: dL(z) to z 2 • Ongoing with various ground-based/HST surveys • Key issue is physics/evoln: do we understand SNe Ia? • Weak lensing: G(t) to z 1.5 • Promising; requires photo-z’s • Key issues are fidelity, calibration • Cluster counts: dA(z), H(z) - accuracy/non-linearities? • Baryon “wiggles”: dA(z), H(z) to z=3 • Late developer: cleanest but requires huge surveys • AP test • ISW effect • Galaxy pairs, …. Combined constraints Latest results SNLS3 years + WMAP +BAO equation of state parameter w around 5% statistical and systematic accuracy. The statistical uncertainty on w from SNe Ia is now reduced to the level where systematic effects are comparable. Today systematics are dominated by calibrations, dust corrections, and SNIa diversity Best studied with nearby SN spectroscopy Nearby Supernova Factory - Goals: addressing SNIa systematics for cosmology Anchoring the Hubble diagram at low z Fix the low SNIa magnitude to Dm=0.02!!! -Tools: precise spectro-photometry -SNIa, SNIb,c, SNII studies Nearby SNFactory National Energy Research Scientific Computing Center Discovery: Two cameras (one wide field) 1.2 m ground based telescopes: NEAT/QUEST Lightcurve follow-up with YALO Photo-spectro follow-up with Field Integral Spectrometre (SNIFS) at UH 2.2m telescope (Hawaii) SNFactory: THE nearby SN spectrophotometric database 0.03 < z < 0.08 Status 2010 SNF Others Total All typed SN 624 71 695 SNIa 396 50 446 Follow up >5 147 38 190 Processed 62 12 74 (101) Spec < max 49 9 58 SNFactory II/PTF Still need more and better measured nearby SNIa for calibration understanding of SNIa subclasses need more SNIa detected before maximum for better maximum determination • New Collaboration : US (Berkeley, Yale) + France+ Germany + Tsinghua using the now well running SNIFS spectrograph in UH 2.2m • MOU with Yale telescope in Chile and Palomar Transient Factory (PTF) group for SN detection Use of Chinese telescopes for trigger? under study (Xuyu, Xinlong,Lijiang ) THE spectrophotometric nearby SN reference! Tsinghua THCA and SNFactory • MOU signed April 16, 2011 • THCA contributes 1/3 for UH data SNIa cosmology Future • Nearby SN in the near future • Waiting for SNI thousand SNIa scale programs EUCLID (CT co-coordinator SN WG ) and LSST Large Synoptic Survey Telescope LSST Top ranked ground-based project in 2010 Decadal Survey Optimized for time domain scan mode deep mode 10 square degree field 6.5m effective aperture 24th mag in 20 sec >20 Tbyte/night Real-time analysis Engineered to minimize systematics for Dark Energy The Telescope 1.5 m atmosphere monitoring telescope Artist’s rendition of LSST site,El Penon Peak, Cerro Pachon, Chile The high curvature mirrors allow a shorter, lighter & LSST is sited in an NSF compound more stable telescope near SOAR & Altitude over azimuth Gemini Carousel Dome 38 LSST Science Collaborations LSST data has no proprietary period allows both the astronomical and particle physics communities to carry out the science. - Supernovae - Strong Lensing - Weak lensing - Large-scale structure/baryon oscillations - Galaxies - Active Galactic Nuclei - Milky Way and Local Volume Structure - Transients/variable stars - Stellar Populations - Solar System - Informatics and Statistics LSST Science Book Cosmology Zhan Hu et al. Euclid A geometrical probe of the universe proposed for Cosmic Vision All-sky optical imaging for gravitational lensing = + All-sky near-IR spectra to H=22 for BAO The Euclid Concept • Named in honour of the pioneer of geometry • Euclid will survey the entire extra-galactic sky (15000 deg2) to simultaneously measure its two principal dark energy probes: – Weak lensing: • Diffraction limited galaxy shape measurements in one broad visible R/I/Z band. • Redshift determination by Photo-z measurements in 3 YJH NIR bands to H(AB)=24 mag, 5σ point source – Baryonic Acoustic Oscillations: • Spectroscopic redshifts for 33% of all galaxies brighter than H(AB)=22 mag, σz<0.006 • With constraints: – Aperture: max 1.2 m diameter – Mission duration: max ~5 years Decision : October 4, 2011 EUCLID selected over PLATO Shear Data: Ground vs Space space weak lensing shear ground Space: small and stable PSF: larger number of resolved galaxies reduced systematics Typical cosmic shear is ~ 1%, and must be measured with high accuracy + Ground data: Photometric redshifts OPT+IR OPT zphoto zphoto zspec zspec • Will need redshifts for 109 galaxies − possible to 5% with ground-based Pan-Starrs survey etc. • But need 1-2 micron IR for z >1 − impossible from ground (sky brightness) • Need >105 spectroscopic redshifts for calibration Predictions for the expansion history and growth rate The current measurement of H(z) is from Wang & Mukherjee (2007). The error forecast for Euclid measurement of H(z) is obtained using a fisher matrix code (from Y. Wang) Growth Rate f_g(z) Errors from direct measurement of redshiftspace distortions on two-point correlation function (from L. Guzzo). SNIa cosmology Future • Nearby SN in the near future • Waiting for SNI thousand SNIa scale programs EUCLID (CT co-coordinator SN WG ) and LSST • Or … Antarctica projects Antarctica Dome A Kunlun Telescope will answer fundamental questions about the structure of the Universe. Wang Lifan Advantage: great seeing! Expect: 0.3 arc sec, eg space Major Relevant Features • • • • • Continuous observing time for more than 3 months Low temperature, low sky background in thermo IR Low turbulence boundary layers, good seeing Dry air, high transmission in IR Large Isoplanatic Angle • Aurora • High relative humidity • Difficult to access Towards a large Antarctica Dome A Kunlun Dark Universe Survey Telescope (KDUST) First stage 2011-2013: 3 x 75 cms telescopes (AST3) - Already designed, one AST3 installed in Dome A, THCA contributes to one AST3 and take responsibility for SN search KDUST-2.5 m : 2012-2016 - Starting discussions with US, Australian, French Larger (> 4m) KDUST: Timescale too early to define! Astronomy of the Next Decade in Antarctica • Time-Domain • Large Sky Area • Beyond Optical Wavelength: UV, IR, Sub-mm, … • • • • • • • • • Planets Stellar Variability AGN Gravitational Lensing Gravitational Waves Extra-dimension Supernovae The Dark Universe … Multiprobe measurements (SNIa, BAO, Clusters, Weak Lensing, …) for cosmology and ancillary science THCA and Antarctica research • MOU signed March 16, 2011 • THCA joins Chinese Center for Antarctic Astronomy (NAOC, Nanjing Purple Mountain Observatory, NIAOT…) • THCA contributes to 1 AST3 • THCA coordinates SN research • Other DE contributions in the future … Antarctica Schmidt Telescopes (AST3) • • • • • • Aperture:75cm; FOV:4.2°; Wave Band:400nm-900nm ( i,g, r, or IR? filter for 3 telescopes ); Scale:1 arcsec/pixel; Image quality:80%energy encircled in one pixel; CCD: 9micron /pixel, 10580x10560 (95.22mm x 95.05mm image area); • Type: STA1600; Working mode: frame transfer readout Focal length: 1867mm Distorsion in the whole field: 0.012% (less than 1 pixel) Total optical length: 2.2m First AST3 in Dome A, commissioning data taken since darkness Summer 2011 in Xuyu Dec 2011 in Dome A The Kunlun Dark Universe Survey Telescope 5000 sq deg down to mag 29 Astrophysical and Cosmological Determinations of Dark Matter THCA Charling Tao and Shan Huan Yuan • Analyze existing CFHT data: first identification of clusters with WL on CFHT data Shan et al., ApJ 2012 • Prepare for Large surveys. LSST, EUCLID, KDUST Opportunity in Jinping, Sichuan for direct detection DM detectors • After Mentougou in IHEP > 20 years ago… • Great mountain coverage Tsinghua Physical Engineering Dpt Leadership VP Cheng Jian Ping 程建平 CJPL Many « Underground » physics topics: DM, Proton Decay, neutrinos physics, … Possible size of cavity ? Yue Qian 岳骞 Nature of DM Hot or Cold, or Warm? CDM is non-relativistic at decoupling, forms structures in a hierarchical, bottom-up scenario. HDM is tightly bound by observations and LSS formation WDM? Nature of DM Hot or Cold? CDM is non-relativistic at decoupling, forms structures in a hierarchical, bottom-up scenario. HDM is tightly bound by observations and LSS formation Cf CT review, arXiv:1110.0298 Numerical Simulations prefer CDM (not hot DM) Z=3 Z=1 Z=0 LCDM OMEGA = 1 LAMBDA = 0 H0 = 50 km/(Mpc sec) Sigma8 = 0.51 SCDM OMEGA = 0.3 LAMBDA = 0 H0 = 70 km/(Mpc sec) Sigma8 = 0.85 tCDM OMEGA = 0.3 LAMBDA = 0 H0 = 50 km/(Mpc sec) Sigma8 = 0.51 OCDM Collaboration VIRGO 1996 http://www.mpa-garching.mpg.de/~virgo/virgo/ DM Detection • Not one single experiment can convince of discovery of DM • Need for signature of galactic origin • If > 100 GeV Neutralinos, DD need directional detectors! DM Directional Detector: the future Personal interest for > 20 years • • 1975-1979 Cylindrical Drift chamber in PhD thesis back for Fermilab DIS muon CHIO in Smithsonian (Washington DC) 1979-1982: UA1 Central Detector 1st W event in UA1 CD • 1995-1998 The HELLAZ solar pp neutrino project Tom Ypsilantis, Jacques Séguinot et al… , with a Micromegas Dark matter detection with hydrogen proportional counters G. Gerbier, J. Rich, M. Spiro, C. Tao Nuclear Physics B - Proceedings Supplements Volume 13, February 1990, Pages 207-208 Developping THCA Attract more people students, postdocs, faculty, visitors – Internal Tsinghua - Stronger involvement in teaching - Develop collaborations with Engineering departments – Develop collaboration with NAOC, PMO and IHEP – International collaborations for research (and teaching) • Access to existing data • Future Chinese projects, eg Antarctica • Visiting scientists – Next step: Official participation of THCA to LIA Origins? 谢谢 Merci DM: SUSY Neutralinos ? • A natural particle physics solution • Stable linear combination gauginos and higgsinos (LSP) 0 0 ˜ ˜ ˜ ˜ = + Z + H1 + H2 • SUSY > 7 parameters MSSM no predictive power • Experimental Constraints LEP, pp, b-->s, + ... Look everywhere possible ! Direct and Indirect Detections WIMP searches: Direct detection • Principle : (Goodman and Witten,1985, Drukier and Stodolsky 1984) Elastic scattering of galactic DM off detector nuclei M Nuclear recoils of a few keV • Exponential recoil energy distribution event rate per unit mass recoil energy total event rate (point like nucleus) dR = Ro e -ER/Eor dE R Eor incident energy kinematic factor = 4MMN/(M+ MN)2 • Rates: Weak interactions or smaller 10 Ge, Si, NaI, LXe, … 9 8 7 6 5 4 3 2 1 0 0 1 2 3 4 5 6 7 8 9 10 E/(E0r) • Need of signatures for identifying galactic origin –Annual modulation with MASSIVE detectors –Directionality : low pressure TPC? –Dependence on nucleus MN Science with an underground directional detector • DM detection and direction of Cygnus X1 (low pressure TPC) • HELLAZ large volume (2000 m3!) pp solar neutrino energy spectrum • Dirac vs Majorana neutrinos • Neutrino magnetic moment (MUNU, SuperMUNU) • … • Xmass Design and competition Low pressure vs high pressure 3rd International conference on Directional Detection of Dark Matter (CYGNUS 2011), Aussois, France, 8-10 June 2011 •Progress with DRIFT II and DRIFT III, •Status of the DMTPC Experiment, •NEWAGE , •The Directional Dark Matter Detector (D^3) •R&D Status of Nuclear Emulsion for Directional Dark Matter Search MIMAC (cf Daniel Santos) •Most progress •Most convincing Discuss concrete collaboration with Chinese for 1m3 project?! Mini workshop November 2011 Tsinghua with French + Chinese community: Tsinghua, Jiaotong, IHEP, USTC, … MOU for MIMAC? 发现了美国宇宙微波背景探测卫星WMAP公 布的微波背景温度图存在严重系统误差 质疑WMAP宇宙学 — 2010年10 月英国皇家天文学会刊物 《News and Reviews on Astronomy & Geophysics》 载 文详细评介了对于WMAP结果的 质疑,图为该期封面. 李惕碚 + Liu Hao (IHEP) Inconsistency with WMAP quadrupole calculation? Liu and Li arXiv 0907.2731 Liu and Li arXiv 1001.4643 Due to quaternion interpolation offset: Liu and Li arXiv 1003.1073