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

2500m 300m active Ground Station- La Seyne sur Mer ~60m ~100m Local electroni c Optical Module triplet Hydrophone Time calibratio n LED Beacon Câble électro-optique sous marin de ~ 40km Balises acoustiques Câbles de raccordement Conteneur électronique Boite de jonction lest Bouée 10 lines with 30 floors: 900 Optical Modules ANTARES detector  KM3 DM,  astrophysics

THCA Physics dept Eng.Phys dept IHEP Since 2010, CT Wang Xiaofeng, Hu Jian +… Postdocs, students,.. Li Tipei Shang Rencheng Zhang ShuangNan, Lou Yuqing Feng Hua, Zhang Youhong, Zhou Jianfeng …

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

– 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 Understanding the Dark Universe: astroparticle, Cosmology and gravity physics

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)

Computing at THCA LIGO-China group : Cao Junwei et al. Future: HXMT, Antarctica, Euclid, LSST, 2m space,… Very Large amount of data, eg, LSST 40 Tb/night= SDSS Issues: storage, database, processing, fast access, transfers, data selection,…  initiate discussions at national level (NAOC+Univ.) Astrocomputing? Google partnership with LSST… Chinese: Baidu?,…

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?

HXMT is a wide band (1-250 keV) X-ray observatory, all-sky survey with high angular resolution and sensitivity HE ( keV NaI/CsI 5100 cm 2 ) LE (1 － 15 keV SCD 400 cm 2 ) ME ( 5-30 keV SiPIN 1000 cm 2 ) Collimator 1°× 6° HXMT The hard X-ray modulation telescope HXMT Launch in 2015 Official administrative launch 2 days ago!

Xinlong 80 cms TNT Very useful pedagogical training tool for students 2003 Transient research ： SN, GRB afterglow,AGN SN Ia Light curve

A mysterious Dark Universe ! Graph source: Wikipedia Definition:  c (  c = g/cm 3 ) What we know is only 4% of the energy density of the Universe We now measure with precision the amount of our ignorance !

A concordance  CDM model Multi-probe concordance : CMB, + SN, clusters, galaxies redshift surveys, Weak Lensing, …  Concordance  CDM 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 q 0 Acceleration!!!   =  (t)/  c (t) =       k    /3H 0 2 q 0 = 1/2     < 0 Redshift z But only 2  effect! At the time Hubble diagram B magnitude at maximum

Supernovae type Ia Best known « standard » candles SNIa : 2 stars accretion (a white dwarf +…)  Chandrasekhar mass 1.4 M O Red giant White dwarf Chandrasekhar mass 1.4 M O

magnitude SN Ia are not exact standard candles! The light of SNIa explosions can be followed up for several weeks with telescopes SNIa Light curves

Different standardisation methods Before: m B After, eg, stretch correction: m Bcor = m B – a (s-1) stretch (SCP), MLC2k2 (HiZ),  m 15,.. Wang Xiaofeng :  C12 + different classes of SNIa (HV?) Standardisation to  m =0.2

What is this 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? - equation of state w(z) = p/  w =-1

A problem for field theorists Value of cosmological constant  ! Difference ~ 120 orders of magnitude ! 1 GeV = Joules   obs ~ ( GeV) 4 ~ (meV) 4 Coincidence with Neutrino scale? X X General Relativity   scale Cosmological measurements   obs ~ ( GeV) 4 = 2 x J/cm 3 Particle physics   ~ vacuum energy vacuum = perfect fluid p= -    G    EW ~ (200 GeV) 4 = 3 x J/cm 3   QCD ~ (0.3 GeV) 4 = 1.6 x J/cm 3   Pl ~ (10 18 GeV) 4 = 2 x J/cm 3

Latest results SNLS3 + other SNIa Conley et al. Jan 2011 Flat Universe and Constant w SNIa: best single probe constraint on EoS todate

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 systematic effects Any way

Power of Combinations astro-ph DE Task force

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 : 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 Dark Energy phenomenology: some milestones Gigi Guzzo

Beware of error determinations! eg, Plot from Spergel et al astro-ph/ , WMAP3: Tension: WMAP3, & Weak Lensing CFHTLS 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, …

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)

CMB: Planck Type Ia Supernovae: d L (z) to z  2 Ongoing with various ground-based/HST surveys Key issue is physics/evol n : 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: 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 Galaxy pairs, …. How can w(z) be better measured?

Combined constraints  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 Latest results SNLS3 years + WMAP +BAO

Nearby Supernova Factory - Goals: addressing SNIa systematics for cosmology -Tools: precise spectro-photometry -SNIa, SNIb,c, SNII studies Anchoring the Hubble diagram at low z  Fix the low SNIa magnitude to  m=0.02!!!

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 spectro- photometric database Status 2010 SNFOthersTotal All typed SN SNIa Follow up > Processed (101) Spec < max < z < 0.08

SNFactory II/PTF 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  THE spectrophotometric nearby SN reference! Still need more and better measured nearby SNIa for  calibration  understanding of SNIa subclasses  need more SNIa detected before maximum for better maximum determination Use of Chinese telescopes for trigger? under study (Xuyu ， Xinlong ， Lijiang ）

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

38 The Telescope Artist’s rendition of LSST site,El Penon Peak, Cerro Pachon, Chile 1.5 m atmosphere monitoring telescope Altitude over azimuth Carousel Dome The high curvature mirrors allow a shorter, lighter & more stable telescope LSST is sited in an NSF compound near SOAR & Gemini

LSST Science Collaborations - 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 data has no proprietary period allows both the astronomical and particle physics communities to carry out the science.

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 deg 2 ) 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, σ z <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: small and stable PSF:  larger number of resolved galaxies  reduced systematics weak lensing shear space ground Typical cosmic shear is ~ 1%, and must be measured with high accuracy

+ Ground data: Photometric redshifts z spec z photo Will need redshifts for 10 9 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 >10 5 spectroscopic redshifts for calibration z photo OPT OPT+IR

Predictions for the expansion history and growth rate Growth Rate f_g(z) Errors from direct measurement of redshift- space distortions on two-point correlation function (from L. Guzzo). 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)

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

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 Major Relevant Features

Towards a large Antarctica Dome A Kunlun Dark Universe Survey Telescope (KDUST)  First stage : 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 : Starting discussions with US, Australian, French  Larger (> 4m) KDUST: Timescale too early to define !

Astronomy of the Next Decade in Antarctica 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 Time-Domain Large Sky Area Beyond Optical Wavelength: UV, IR, Sub-mm, …

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 Dec 2011 in Dome A Summer 2011 in Xuyu

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 Yue Qian 岳骞 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 ?

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

Numerical Simulations prefer CDM Collaboration VIRGO  CDM SCDM  CDM OCDM Z=3Z=1Z=0 OMEGA = 1 LAMBDA = 0 H0 = 50 km/(Mpc sec) Sigma8 = 0.51 OMEGA = 0.3 LAMBDA = 0 H0 = 70 km/(Mpc sec) Sigma8 = 0.85 OMEGA = 0.3 LAMBDA = 0 H0 = 50 km/(Mpc sec) Sigma8 = 0.51 (not hot DM) Cf CT review, arXiv:

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 Cylindrical Drift chamber in PhD thesis back for Fermilab DIS muon CHIO in Smithsonian (Washington DC) : UA1 Central Detector 1 st W event in UA1 CD 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

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? Developping THCA

谢谢 Merci

DM: SUSY Neutralinos ? Look everywhere possible Look everywhere possible ! Direct and Indirect Detections A natural particle physics solution Stable linear combination gauginos and higgsinos (LSP) SUSY > 7 parameters MSSM  no predictive power Experimental Constraints LEP, pp, b-->s ...

WIMP searches: Direct detection MM MNMN Ge, Si, NaI, LXe, … Principle : (Goodman and Witten,1985, Drukier and Stodolsky 1984) Elastic scattering of galactic DM off detector nuclei Nuclear recoils of a few keV Need of signatures for identifying galactic origin –Annual modulation with MASSIVE detectors –Directionality : low pressure TPC? –Dependence on nucleus Rates: Weak interactions or smaller dR dE R = RoRo EorEor e -E R /E o r recoil energy incident energy kinematic factor = 4M  M N /(M  + M N ) 2 event rate per unit mass total event rate (point like nucleus) E/(E 0 r) Exponential recoil energy distribution

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 1m 3 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 Due to quaternion interpolation offset: Liu and Li arXiv Liu and Li arXiv