Brief Introduction to China’s Space Astronomy Programs · Brief Introduction to China’s Space...

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Brief Introduction to China’s Space Astronomy Programs Shuang-Nan Zhang [email protected] Center for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 2015-08-05 1/40

Transcript of Brief Introduction to China’s Space Astronomy Programs · Brief Introduction to China’s Space...

Page 1: Brief Introduction to China’s Space Astronomy Programs · Brief Introduction to China’s Space Astronomy Programs Shuang-Nan Zhang zhangsn@ihep.ac.cn Center for Particle Astrophysics

Brief Introduction to China’s

Space Astronomy Programs

Shuang-Nan Zhang

[email protected]

Center for Particle Astrophysics

Institute of High Energy Physics

Chinese Academy of Sciences

2015-08-05 1/40

Page 2: Brief Introduction to China’s Space Astronomy Programs · Brief Introduction to China’s Space Astronomy Programs Shuang-Nan Zhang zhangsn@ihep.ac.cn Center for Particle Astrophysics

2015 2020 2025

China’s Space Astronomy Satellites

2030

radio

IR/O

X-r

ay

γ-r

ay

e/C

R

/GR

W

Cosmic

Web

DAMPE

SVOMHXMT XTP

EP

mmVLBI 21cm

SULFRO

21cm

COME

cLISA

STEP

JEEEDIS

NEarth

2015-08-05

UV

2/40

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Main scientific objectives (1-250 keV energy band)Scan monitoring of the Galactic plane transients watch dog: need

ground follow-up observations.

Pointed observations Black hole and neutron star x-ray binaries:

need coordinated ground observations

Satellite Facts:

Mass: ~2800 kg

Orbit: 550 km, 43° Lifetime: 4 yrs

Officially approved in March 2011

Now in final stages of FM and calibration

Planned launch time: Aug. 2016

Core programs open to many international scientists and

organizations to reward their contributions to HXMT

Hard X-ray Modulation Telescope (HXMT)

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High Energg (HE):

NaI/CsI, 20-250 keV, 5000 cm2

Low Energy (LE):

SCD,1-15 keV, 384 cm2

Star

trackers

Medium (ME):

Si-PIN,5-30 keV, 952 cm2

ME

HELE

HXMT Payloads

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HXMT Sensitivity

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DAMPE: launch in ~Dec. 2015

2015-08-05

+ Switzerland

+ Italy

6/40

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Gamma-ray mapping by 30 days

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Fermi, 195 Weeks ~ 8σDAMPE 3 years

DAMPE for gamma-ray line observations

DAMPE will confirm or deny the “suspicious” dark matter

annihilation line of Fermi with high significance

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SVOM: ~2021 launch (China-France)

VTGRM

Eclairs

GFTsGWAC

MXT

4-250 keV

30 keV-5 MeV

0.3-5 keV

450-900 nm 400-1700 nm

400-650 nm, 650-950 nm

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VHF Network

Prompt dissemination of GRB parameters

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Ground

Space

GWAC

GFTs (g, r, i, J, H)

T0 +1 min

1-2 m robotic telescopes

GRB trigger provided by ECLAIRs at time T0

VT (V & R band photometry)

MXT (Soft X-ray photometry)

T0 + 5 min

Multi messenger follow-up

GRB observation strategy

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X-ray Timing and Polarization (XTP) mission

Singularity?

Neutron or

Quark Star?

Extreme gravity

magnetism

density

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XTP satellite baseline design

Selected for Phase 0/A

in 2011, expected

launch in 2020-2025.

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Enhanced XTP (or eXTP): option 1

LOFT LAD• 2 lines*5 columns*2 panels = 20 LAD

– ~1.5 m2 effective area for collimating

detectors

+ LOFT consortium: Italy, UK, Germany, Switzerland,

Netherland …2015-08-05 14/40

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Effective area of eXTP option 1

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Enhanced XTP (or eXTP): option 2

• 2 lines*5 columns*4 panels+2 = 42 LAD

– ~3 m2 effective area for collimating detectors

– Loss of ~ 0.1 m2 of XTP LFA

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Einstein Probe (EP)

Selected for Phase 0/A

in 2013, proposed for

launch in 2020-2025.

+ UK

Lobster-eye optics

17/40

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Adv. LIGO Adv. Virgo ~2018

VHF

GPS天线

X波段天线

测控天线

星敏感器

星敏感器

龙虾眼X射线

望远镜

EM counterparts of GW explosions

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VHF

GPS天线

X波段天线

测控天线

星敏感器

星敏感器

龙虾眼X射线

望远镜

X-ray binaries

ULX

Active galactic

nuclei

X-ray binaries

Quiet galaxy

Black holes of all scales in the universe

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Capability of Einstein Probe

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China’s Space Station Program

Ph

ase

-I

2003

201110 astronauts in 5 flights space walk

Ph

ase

-II

2016

Space lab:

no living cabin

Ph

ase

-II

2020 Space Station

3 large modules

+ 2 m telescope

~10-year lifetimeHERD

HERD

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2015 2020 2025

China’s Space Station Astronomy Program

2030

IR/O

X-r

ay

γ-r

ay

e/C

R

HERD

POLAR

Chinese Space Station

Optical Survey

Dark Energy

NEATER

ASM ?(a mini XTP but

with low-E pol.)

(EP in scanning

mode without XFT)

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Gamma-ray burst polarization : POLAR

• China- Switzerland

collaboration– Energy range: 50-350 keV;

FOV of POLAR: ~½ sky

• Onboard China’s spacelab

TG-2: launch time Aug. 2016

• Main science: GRB jet &

central engine; tests of

quantum gravity theories

Tian-Gong 天宫

Palace in

Heaven

Plastic scintillator

stacks

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Results agree with Monte-Carlo simulations

POLAR ESRF Calibration

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Effective Area of POLAR

• Monte Carlo based study

• Aeff is dependent on E and

incoming photon angle

• Figure of merit: Aeff x m100

S. Xiong, N. Produit, B. Wu, Expected performance of

a hard X-ray polarimeter (POLAR) by Monte Carlo

simulation, Nucl. Instr. and Meth. A 606 (2009) 552

Energy [keV]

Eff

ecti

ve a

rea

[cm

2]

E. Suarez Garcia, Ph.D. Thesis, Univ. de Genève, 2010

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NEATER Payloads: 2020 launch

Collimated detectors

Si ~400 cm2

Energy: Si ~100 cm2

Polarimetry: GPD 50 cm2

Polarization

E=0.25 keV

~1200 cm2

F~ 1 m Single ref.

MPO or nested

shells?

+ Italy

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Payload Assembly

Weight:146 kg

Power:250 W

Size

<1500*1400*1500mm

Targets

Primary: isolated pulsars

Secondary: accreting pulsars,

microquasars, blazars

Pathfinder of XTP

2015-08-05 27/40

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X-ray All Sky Monitor (XASM): 2020 launch

FOV: 61ox36.9o

+UK

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Wide Field Telescope

WFT

XASM Design: Lobster Eye Optics

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HERD:3D Calo & 5-Side Sensitive

n10X acceptance than most

others, but weight 2.3 T ~1/3 AMS

3D CALO

e/G/CR energy

e/p discriminationSTK(W+SSD)

STK(W+SSD)

Charge

gamma-ray direction

CR back scatter

+ Italy, Switzerland, Sweden2015-08-05 30/40

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HERD

Dark matter particle

protonHe

Gamma-ray

electron

background

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Expected performance of HERD

γ/e energy range (CALO) tens of GeV-10TeV

nucleon energy range (CALO) up to PeV

γ/e angular resol. (Si-strips) 0.1o

nucleon charge resol. (Si-strips) 0.1-0.15 c.u

γ/e energy resolution (CALO) <1%@200GeV

proton energy resolution (CALO) 20%

e/p separation power (CALO) <10-5

electron eff. geometrical factor (CALO) 3.7 m2sr@600 GeV

proton eff. geometrical factor (CALO) 2.6 m2sr@400 TeV

2025 launch?

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PAMELA: 2006-2016 CALET: 2015-2020; AMS: 2011-2021;

DAMPE: 2015-2020; Fermi: 2008-2018; HERD: 2020-2021

HERD sensitivity to gamma-ray line

HERD 1 yr

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000

00

Z

DM annihilation line of HERD

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Expected HERD Proton and He Spectra

Horandel model as HERD input

Only statistical error

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Expected HERD Spectra of C and Fe

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• 25000□°imaging survey: 250-1050nm, ≥6 filters, g, r, & i

≥ AB25 mag (5σ, point source)

• 800□°deep imaging survey: g, r, & i ≥ AB26.5 mag

• 10000□°medium & high galactic latitude slitless

spectroscopy survey: g, r, & i continuum ≥ AB21 mag

Survey ScienceCosmology: dark energy, dark matter, gravity,

large-scale structure, neutrinos, primordial

non-Gaussianity…

AGNs: high-z AGNs, clustering, dual AGNs,

variability, UV excess, host galaxies…

Galaxies: formation & evolution, mergers, high-zs,

dwarfs, LSBs, near field, halos properties…

Milky Way: structure, satellites, dust, extinction…

Stellar science: formation, dwarfs, metal poor…

Solar system (high inclination): TNO、NEA…

Astrometry: reference frame, star clusters…

Ecliptic Coord.

2022?

2015-08-05

World-wide contributions

in science definition

37/40

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Project SiteLaunc

h/Op

FoV REE80

Num

pixel

s

Area Wavelength Num

FilterSpec

deg2 ″ 109 deg2 nm

Space

StationLEO 2022

1.1

0.002

0.15

0.25

2.5

0.002

25000

-

250—1050

900—1700

7

2

yes

yes

Euclid L2 20200.56

0.55

>0.2

0.6

0.6

0.0715000

550—920

1000—2000

1

3

no

yes

WFIRST GEO ≥2024 0.28 >0.2 0.3 2400 927—2000 4 yes

LSST Chile 2022 9.6 >0.7 3.2 20000 320—1050 6 no

Exp NUV u g r i z Y

Imaging 2×150s 25.5 25.5 26.1 25.9 25.7 25.5 24.7

Deep

Imaging7×200s 26.5 26.5 27.1 26.8 26.7 26.5 25.7

Slitless Spec 2×200s 20.3 21.0 21.3 21.4 21.4 21.5 21.0

5σ point source limiting AB mag of Space Station Survey

Comparison with Other Surveys

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The Chinese space station optical survey is very

competitive among its peers, and its capability,

especially high-resolution near-UV imaging and

slitless spectroscopy in the optical, is unique and

highly complementary to other surveys.

Comparison with Other Surveys

Wavelength (μm)

Ang

ula

r re

solu

tion (

“)

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Summary

• Astronomy satellite

– Approved: DArk Matter Particle Exploration (DAMPE,

2015), Hard X-ray Modulation Telescope (HXMT, 2016),

Space Variable Object Monitor (SVOM, 2021)

– Phase 0/A: Einstein Probe (EP: 2020), X-ray Timing and

Polarization (XTP: <2025?)

• Manned Space Flight Program

– Approved: Gamma-ray burst polarization (POLAR, 2016),

NEATER (2020), XASM (2020) , Space Station Optical

Survey (2022?)

– Phase 0/A: HERD (2025?)

Significant international contributions to all missions!

2015-08-05 40/40