Tsinghua Center for Astrophysics and the Dark

Universe:Science, People, Projects

Charling TaoTHCA / CPPM

LIA Origins 2012 –La Londe les Maures

Centre de Physique des Particules de

Marseille CPPM

Unité Mixte de Recherche 6550CNRS/IN2P3-Université de la MéditerranéeMarseille, France

2500m

300mactive

Ground Station- La Seyne sur Mer

~60m

~100m

Local electro

nic

Optical

Module

triplet

Hydrophone

Time calibrati

onLED

Beacon

Câble électro-optiquesous marin de

~ 40km

Balises acoustiques

Câbles de raccordement

Conteneur électronique

Boite de jonctionlest

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 …

2001http://www.thca.tsinghua.edu.cn/

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)

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(20-250 keV NaI/CsI 5100 cm2)

LE (1 － 15 keV SCD 400 cm2)

ME

(5-30 keV SiPIN 1000 cm2)

Collimator 1°× 6°

The hard X-ray modulation telescope HXMTHXMT

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=10-29 g/cm3)

What we know is only 4%

of the energy density of the Universe

We now measure with precision the amount of our ignorance !

A concordanceCDM 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 Cosmology1998 SURPRISE:

Indication for

negative deceleration parameter q0

Acceleration!!!

= (t)/c(t) =

k

/3H02

q0= 1/2< 0Redshift z

But only

2effect!

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 MO

Red giant

White dwarf

Chandrasekhar mass 1.4 MO

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 = 1.6 10-10 Joules

obs ~ (10-12 GeV)4 ~ (meV)4 Coincidence

with Neutrino scale?

XX• General Relativity scale

• Cosmological measurements

obs ~ (10-12 GeV)4 = 2 x 10-17 J/cm3

• Particle physics ~ vacuum energy

vacuum = perfect fluid p= -G

EW ~ (200 GeV)4 = 3 x 1040 J/cm3

QCD ~ (0.3 GeV)4 = 1.6 x 1029 J/cm3

Pl ~ (1018 GeV)4 = 2 x 10103 J/cm3

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

astro-ph 0609591

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

• 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

Dark Energy phenomenology: some milestones

Gigi Guzzo

Cluster counts

Supernovae

Baryon Wiggles

Cosmic Shear Angular diameter distanceGrowth rate of structure

Evolution of dark matter perturbations

Standard ruler

Angular diameter distance

Standard candleLuminosity distance

Evolution of dark matter perturbationsAngular diameter distanceGrowth rate of structure

The concordance model stands quite strong!

CMBSnapshot 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: 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, ….

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 SNFactoryNational 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

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

0.03 < 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 SurveyTop ranked ground-based project in 2010 Decadal Survey

Optimized for time domainOptimized for time domain

scan modescan mode

deep modedeep mode

10 square degree field10 square degree field

6.5m effective aperture6.5m effective aperture

24th mag in 20 sec24th mag in 20 sec

>20 Tbyte/night>20 Tbyte/night

Real-time analysisReal-time analysis

Engineered to minimize systematics for Dark EnergyEngineered to minimize systematics for Dark Energy

38

The Telescope

Artist’s rendition of LSST site,El Penon Peak,Cerro Pachon, Chile

1.5 m atmospheremonitoring telescope

Altitude over azimuth

Carousel Dome

The high curvature mirrors allow a shorter, lighter & more stable telescope

LSST is sited inan NSF compoundnear 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

CosmologyZhan Hu et al.

EuclidA 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: 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

zspec zspec

zphoto

• 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

zphoto

OPT OPT+IR

Predictions for theexpansion 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 AKunlun 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

• 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 ASummer 2011 in Xuyu

The Kunlun Dark Universe Survey Telescope

5000 sq deg down to mag 29

Astrophysical and Astrophysical and Cosmological Cosmological

Determinations of Determinations of Dark Matter 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, Sichuanfor 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 DMHot or Cold, or Warm?

CDM is non-relativistic

at decoupling, forms

structures in a hierarchical,

bottom-up scenario.

HDM is tightly bound byobservations and LSS formation

WDM?

Nature of DMHot or Cold?

CDM is non-relativistic

at decoupling, forms

structures in a hierarchical,

bottom-up scenario.

HDM is tightly bound byobservations and LSS formation

Numerical Simulations prefer CDM

Collaboration VIRGO 1996http://www.mpa-garching.mpg.de/~virgo/virgo/

CDM

SCDM

CDM

OCDM

Z=3 Z=1 Z=0

OMEGA = 1LAMBDA = 0H0 = 50 km/(Mpc sec)Sigma8 = 0.51

OMEGA = 0.3LAMBDA = 0 H0 = 70 km/(Mpc sec)Sigma8 = 0.85

OMEGA = 0.3LAMBDA = 0H0 = 50 km/(Mpc sec)Sigma8 = 0.51

(not hot DM)Cf CT review, arXiv:1110.0298

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 countersG. Gerbier, J. Rich, M. Spiro, C. TaoNuclear Physics B - Proceedings Supplements

Volume 13, February 1990, Pages 207-208

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 ?

˜ ˜ Z ˜ H 10 ˜ H 2

0

Look everywhere possibleLook 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

MMN

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

dRdE R

=Ro

Eore -ER/Eor

recoil energy

incident energy

kinematic factor = 4MMN/(M+ MN)2

event rate per unit mass

total event rate (point like nucleus)

1 2 3 4 5 6 7 8 9 100E/(E0r)

0123456789

10• 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)• …• XmassDesign and competitionLow 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 1001.4643

Due to quaternion interpolation offset: Liu and Li arXiv 1003.1073

Liu and Li arXiv 0907.2731