Fundamental Physics at ESA O. Jennrich ESA Science Directorate.

Fundamental Physics at ESA

O. Jennrich

ESA

Science Directorate

SpacePart 06 – Beijing – 19 April 2006

Overview

Two dedicated missions in the Science Directorate LISA Pathfinder LISA

Missions with aspects of FP in the Science Directorate Gaia Planck

Mission concepts under assessment Fundamental Physics Explorer

Minor contributions to nationally led missions Microscope (CNES)

Missions in other Directorates but supported through Science Directorate ACES (led by Human Spaceflight)


ACES


ACES mission

ESA mission conducted by Human Spaceflight To be installed on the ISS (Columbus module) Payload

Cs fountain clock (PHARAO) Hydrogen maser (SHM) Microwave link

Mission goals: Test of a new generation of space clocks Precise and accurate time and frequency transfer Fundamental physics tests

Status: payload development Launch: 2010


Microscope

CNES-led mission to investigate the equivalence principle Target sensitivity 10-15

Room-temperature experiment Measurement principle:

compare the effect of gravity on two masses of different material

2 differential accelerometers in free-fall (PtRh/PtRh and Ti/PtRh)


Microscope

ESA contributes μN thrusters (FEEP) ONERA: inertial sensor development Development status

Satellite PDR February 2006 Launch

May 2010


Planck

Measuring the CMB with unprecedented accuracy T/T = 2 × 10-6 (about 10 times better than WMAP) Angular resolution 5 arcsec (24 μrad) (about 3

times better than WMAP) Wide frequency coverage (30–857 GHz).

Payload Low Frequency Instrument (LFI)

• Intensity and polarization at 33 GHz, 44 GHz and 70 GHz• Cryogenic detectors (20 K)

High Frequency Instrument (HFI)• Bolometric measurements (intensity and polarisation) at 6 frequencies at

100 – 857 GHz• Detector temperature 0.1 K


Planck

Fundamental physics with Planck Nature of Dark Energy and Dark Matter Baryogenesis String theory

Status Payload flight models under test, delivery to ESA

July/August 2006 Launch

Foreseen Q1 2008 (joint launch with Herschel on Ariane 5)


Gaia – Taking a census of the galaxy

Astrometric mission to measure positions, distances, and space motions of stars in our galaxy About a 109 stars up to magnitude 20 median parallax errors: 7 μas at 10 mag; 20-25 μas at

15 mag; 200–300 μas at 20 mag Distance accuracy: between 1% and 10% Velocity accuracy: between 0.5 km/s and 10 km/s

Status Implementation phase

Launch December 2011


Gaia science objectives

Galaxy origin and formation; Physics of stars and their evolution; Galactic dynamics and distance scale; Solar System census; Large-scale detection of all classes of astrophysical objects

including brown dwarfs, white dwarfs, and planetary systems; Fundamental physics


Fundamental Physics with Gaia

Determine PPN parameters |1-| < 5×10-7 |1-|< 3×10-4

Solar quadrupol moment J2 to 10-7–10-8

Variability of the gravitational constant

tG/G to 10-12–10-13 yr-1

Constraints on gravitational wave energy at frequencies between 10-12 Hz and 4×10-9 Hz

Constraints on M and from quasar microlensing


LISA PF

Precursor to LISA Demonstrating critical technologies for LISA

Drag-free Thrusters Interferometry

Single spacecraft in Lissajou type orbit around L1 Mission duration 6 months Mission status:

Mission PDR successful in February 2006 Flight hardware delivery Summer 2006 Launch in Q4 2009


LISA PF

Payload Payload consists of a European contribution

• Two gravitational reference sensors

• Interferometric measurement system

• Drag free control system

• μN thruster

US contribution• Disturbance reduction system – descoped!

• Drag free control system and μN thruster


LISA PF Inertial Sensor


LISA PF IMS


LISA Mission to detect and observe gravitational waves and their

sources Joint ESA/NASA mission

Europe: Payload, Payload integration, propulsion module NASA: Payload, Payload integration, Spacecraft, launcher,

operations Science operations will be conducted jointly

Technological challenges Interferometric measurements to picometer accuracy Drag-free technology Low frequency stability

Definition/Development: 2010 after completion of LISA PF Launch date ~2017 (present planning assumption)


Cluster of 3 spacecraft in a heliocentric orbit

Spacecraft shield the test masses from external forces (solar wind, radiation pressure)

Allows measurement of amplitude and polarisation of GW

LISA mission concept



Trailing the Earth by 20° (50 million kilometers)

Reducing the influence of the Earth-Moon system on the orbits

Keeping the communication requirements (relatively) standard





Equilateral triangle with 5 million kilometers arm length

Results in easily measurable pathlength variations

Orbit is still stable enough to allow for mission duration larger than 5 years





Equilateral triangle with 5 million kilometers arm length

Inclined with respect to the ecliptic by 60°

Required by orbital mechanics



LISA Science Goals Merging supermassive black

holes

Merging intermediate-mass/seed black holes

Gravitational captures

Galactic and verification binaries

Cosmological backgrounds and bursts

NASA/CXC/MPE/S. Komossa et al.

K. Thorne (Caltech) NASA, Beyond Einstein

Determine the role of massive

black holes in galaxy evolution

Make precision tests of Einstein’s

Theory of Relativity

Determine the population of ultra-

compact binaries in the Galaxy

Probe the physics of the early

universe


Call for CV Mission Proposals (1)

First of 3 Calls (TBC) for implementation of CV2015-2025

Available budget for a ~2016 launch: ~320 M€ (1 effective budget year)

The Call will nevertheless be fully open:

No a priori size restriction, but clear cost guidelines

Mission could be

• a small/medium size S/M mission (≤320 M€ cost to ESA)

• a large ESA alone L mission (≤650 M€ cost to ESA)

Selection of L mission will serve for long term technological development for mission launch in 2020

Up to 2 S/M (depending on size) + 1 L missions will eventually be implemented


Schedule of Call for proposals

Call for mission proposals released 22 May 2006

Letters of Intent due 6 June 2006

Briefing to proposers at ESTEC 12 June 2006

Mission proposals due 18 Sep 2006

WG select 3 S-M & 3 L missions for study phaseOctober 2006

All dates to be confirmed!


LISA

Backup slides


ACES Mission Objectives I

ACES Mission Objectives

ACES performances Scientific background and recent results

Test of a new generation of space clocks

Cold atoms in micro-gravity

Study of cold atom physics in microgravity Essential for the development of atomic quantum sensors for space applications (optical clocks, atom interferometers, atom lasers)

Test of the space cold atom clock PHARAO

Frequency instability: < 3∙10-16 at 1 dayInaccuracy: ~ 10-16

Short term frequency instability evaluated by direct comparison to SHM.Long term instability and systematic frequency shifts measured by comparison to ultra-stable ground clocks.

Frequency instability: optical clocks surpass PHARAO by one or more orders of magnitude.Inaccuracy: at present, cesium fountain clocks are the most accurate frequency standards.

Test of the space hydrogen

maser SHM

Frequency instability: < 2.1∙10-15 at 1000 s < 1.5∙10-15 at 10000 sMedium term frequency instability evaluated by direct comparison to ultra-stable ground clocks. Long term instability determined by on-board comparison to PHARAO in FCDP.

Performances of state-of-the-art masers

Maser y (1000 s) y (10000 s)

GALILEO 3.2∙10-14 1.0∙10-14

EFOS C 2.0∙10-15 2.0∙10-15


ACES Mission Objectives II



Precise and accurate time and frequency transfer

Test of the time and frequency

link MWL

Time transfer stability: < 0.3 ps at 300 s < 7 ps at 1day < 23 ps at 10 days

At present, no time and frequency transfer link has performances comparable with MWL.

Time and frequency

comparisons between ground

clocks

Common view comparisons with an uncertainty level below 1 ps per ISS pass.Non common view comparisons at an uncertainty level of

- 2 ps for 1000 s - 5 ps for 10000 s - 20 ps for 1 day

Existing T&F links

Time stability (1day)

Time accuracy

(1day)

Frequency accuracy

(1day)

GPS-DB 2 ns 3-10 ns 4∙10-14

GPS-CV 1 ns 1-5 ns 2∙10-14

GPS-CP 0.1 ns 1-3 ns 2∙10-15

TWSTFT 0.1-0.2 ns 1 ns 2-4∙10-15

Absolute synchronization of ground clocks

Absolute synchronization of ground clock time scales with an uncertainty of 100 ps.

These performances will allow time and frequency transfer at an unprecedented level of stability and accuracy. The development of such links is mandatory for space experiments based on high accuracy frequency standards.

Contribution to atomic time

scales

Comparison of primary frequency standards with accuracy at the 10-16 level.


ACES Mission Objectives III



Fundamental physics tests

Measurement of the gravitational

red shift

Absolute measurement of the gravitational red-shift at an uncertainty level < 50 ∙ 10-6 after 300 s and < 2 ∙ 10-6 after 10 days.

Space-to-ground clock comparison at the 10-16 level, will yield a factor 30 improvement on previous measurements (GPA experiment).

Search for time drifts of

fundamental constants

Time variations of the fine structure constant at a precision level of -1 d/ dt < 110-16 year -1

Crossed comparisons of clocks based on different atomic elements to impose strong constraints on the time drifts of , mee /QCD , and muu /QCD .

Search for violations of

special relativity

Search for anisotropies of the speed of light at the level c / c ~ 10-10.Measurements relying on the time stability of SHM, PHARAO, MWL, and ground clocks over one ISS pass.

ACES results will improve previous measurements (GPS-based measurements, GPA experiment, measurements based on the Mössbauer effect) by at least one order of magnitude.


S-M Missions schedule

Assessment phases Jan 2007 – Dec 2008

Internal assessment phase in 2007

Competitive industrial assessment in 2008

Emphasis on payload, cost and risks

Presentation to Working Groups for prioritisation April 2009

SSAC recommendation for selection April 2009

Selection of 2 missions May 2009

Preparation & release of ITT Jun-Dec 2009

Start of industrial Definition Phase Jan 2010

SPC approval for development phase 1 mission Jun 2011

Launch Mid-end 2016


L Missions schedule

Study and Technology development phase Jan 2007 – Jun 2010

WG review and prioritisation Sep 2010

SSAC recommendation for 1 L mission Oct 2010

Start Technology consolidation Phase Apr 2011

Start Definition Phase Apr 2013

Start Implementation phase Apr 2015

L Mission Launch ≥2020

Fundamental Physics at ESA O. Jennrich ESA Science Directorate.

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