Charling Tao
THCA / CPPM
LIA Origins 2012 –La Londe les Maures

Unité Mixte de Recherche 6550
CNRS/IN2P3Université de la Méditerranée
Marseille, France

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

2001
Li Tipei
Shang Rencheng
Zhang ShuangNan, Lou Yuqing
Feng Hua, Zhang Youhong,
Zhou Jianfeng …
• Physics dept
• Eng.Phys dept http://www.thca.tsinghua.edu.cn/
• IHEP
Since 2010, CT
Wang Xiaofeng,
Hu Jian
+…
Postdocs, students,..

• 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

+ 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

• 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)

– 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

- 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 LE (1
－
15 keV SCD 400 cm 2 ) resolution and sensitivity
Collimator 1 °× 6 °
Launch in 2015
HE
(20-250 keV NaI/CsI 5100 cm 2 )
Official administrative launch 2 days ago!
ME
(
5-30 keV SiPIN 1000 cm 2 )

2003
SN Ia
Light curve
• Transient research ： SN, GRB afterglow,AGN
• Very useful pedagogical training tool for students

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/r c
( r c
=10 -29 g/cm 3 )

A concordance L CDM model
Multi-probe concordance : CMB, + SN, clusters, galaxies redshift surveys, Weak
Lensing, …

Concordance L CDM model with
Cold Dark Matter and Cosmological constant (or DE)
2/3
Dark
Energy
1/3
Dark
Matter

W
= r
(t)/ r c
(t) =
W
M
W
L
= 1- W k
= L
/3H
0
2
+ W q
0
= 1/2
W
M
- W
L
< 0
L
1998 SURPRISE:
Indication for But only
2 s effect!
negative deceleration parameter q
0
Acceleration!!!
At the time
B magnitude at maximum
Hubble diagram
Redshift z

Red giant
White dwarf
Chandrasekhar mass 1.4
M
O
SNIa : 2 stars accretion (a white dwarf +…)
 Chandrasekhar mass 1.4 M
O

New form of
« field/matter? »
Quintessence?
Unified Dark Matter?
Cosmological Constant???
w =-1
How to distinguish them?
- equation of state w(z) = p/ r
Modified
Gravity/GR ?
- Non minimal
Couplings?
- Extra-Dimensions?
- Anisotropy/ inhomogeneity effects?
- Negative energy?
- ….

A problem for field theorists
Value of cosmological constant L !
•
• General Relativity
X
X
L scale
Cosmological measurements r
L obs ~ (10 -12 GeV) 4 = 2 x 10 -17 J/cm 3
• Particle physics  L
~ vacuum energy vacuum = perfect fluid p= r
L
= - L/(8p
G
) r
L
EW ~ (200 GeV) 4 = 3 x 10 40 J/cm 3 r
L
QCD ~ (0.3 GeV) 4 = 1.6 x 10 29 J/cm 3 r
L
Pl ~ (10 18 GeV) 4 = 2 x 10 103 J/cm 3
1 GeV = 1.6 10 -10 Joules r
L obs ~ (10
Difference ~ 120 orders of magnitude !
-12 GeV) 4 ~ (meV) 4
Coincidence with
Neutrino scale?

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

DE Task force astro-ph 0609591

• 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!
CMB
Snapshot at ~400,000 yr, viewed from z=0
Angular diameter distance to z~1000
Growth rate of structure (from ISW)
Supernovae Standard candle
Luminosity distance
Cosmic Shear
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

• 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, ….

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

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

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)

0.03 < z < 0.08
Status
2010
SNF
All typed SN 624
SNIa 396
Follow up >5
Processed
Spec < max
147
62
49
Others
71
50
38
12
9
Total
695
446
190
74 (101)
58

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!

• MOU signed
April 16, 2011
• THCA contributes
1/3 for UH data

• Nearby SN in the near future
• Waiting for SNI thousand SNIa scale programs
EUCLID (CT co-coordinator SN WG ) and 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

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

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

Cosmology
Zhan Hu et al.

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

• 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

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

OPT OPT+IR z photo z photo z spec z spec
• 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

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).

• 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

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 !

• 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

• 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 …

• 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

Summer 2011 in Xuyu
Dec 2011 in Dome A

5000 sq deg down to mag 29

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

Cold
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?

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
Z=3 Z=1 Z=0
L CDM
SCDM t CDM
OCDM
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
Collaboration VIRGO 1996 http://www.mpa-garching.mpg.de/~virgo/virgo/

• Not one single experiment can convince of discovery of DM
• Need for signature of galactic origin
• If > 100 GeV Neutralinos, DD need directional detectors!

• 1975-1979 Cylindrical Drift chamber in PhD thesis back for Fermilab
DIS muon CHIO in Smithsonian (Washington DC)
• 1979-1982: UA1 Central Detector 1 st 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


• A natural particle physics solution
•
Stable linear combination gauginos and higgsinos (LSP)
 =  ˜ +  ˜ +  H
1
0 +  H
2
0
• SUSY > 7 parameters MSSM  no predictive power
• Experimental Constraints LEP, pp, b-->s
, +
...
Look everywhere possible !
Direct and Indirect
Detections

• Principle : (Goodman and Witten,1985, Drukier and Stodolsky 1984)
Elastic scattering of galactic DM off detector nuclei
M

M
N Nuclear recoils of a few keV
• Exponential recoil energy distribution event rate per unit mass total event rate
(point like nucleus) recoil energy dR dE
R
=
R
E o r o e
-E
R
/E o r incident energy kinematic factor
= 4M

M
N
/(M

+ M
N
) 2
• Rates : Weak interactions or smaller
4
3
2
1
0
7
6
5
Ge, Si, NaI, LXe, …
8
0 1 2 3 4 5 6 7 8 9 10
E/(E
0 r)
• Need of signatures for identifying galactic origin
–Annual modulation with MASSIVE detectors
–Directionality : low pressure TPC?
–Dependence on nucleus

• 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?

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)

Liu and Li arXiv 1001.4643
Due to quaternion interpolation offset: Liu and Li arXiv 1003.1073