Transcript Tsinghua Center for Astrophysics and the Dark - CPPM

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
–
–
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–
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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
= 4MMN/(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