06/02/2009diego götz - the svom mission1 la thuile italy 06/02 2009 44 th rencontres de moriond...

06/02/2009 Diego Götz - The SVOM Mission 1

La ThuileItaly

06/022009 44th Rencontres de Moriond

SVOMSVOMA new mission forA new mission for

Gamma-Ray Bursts StudiesGamma-Ray Bursts Studies

DiegoDiego G GötzötzIrfu-SAp, CEA SaclayIrfu-SAp, CEA Saclay

on behalf of the SVOM Collaborationon behalf of the SVOM Collaboration


GRB physicsGRB physics Acceleration and nature of the relativistic jetAcceleration and nature of the relativistic jetRadiation processesRadiation processesThe early afterglow and the reverse shockThe early afterglow and the reverse shock

The GRB-supernova connectionThe GRB-supernova connectionShort GRB progenitorsShort GRB progenitors

GRB progenitorsGRB progenitors

FundamentalFundamental Origin of high-energy cosmic raysOrigin of high-energy cosmic raysProbing Lorentz invarianceProbing Lorentz invarianceShort GRBs and gravitational wavesShort GRBs and gravitational waves

physicsphysics

CosmologyCosmology

Tracing star formationTracing star formationRe-ionization of the universeRe-ionization of the universeCosmological parametersCosmological parameters

Cosmological lighthouses (absorption systems)Cosmological lighthouses (absorption systems)Host galaxiesHost galaxies

Scientific rationale of the SVOM mission Scientific rationale of the SVOM mission

GRB phenomenonGRB phenomenon Diversity and unity of GRBsDiversity and unity of GRBsGRB phenomenonGRB phenomenon Diversity and unity of GRBsDiversity and unity of GRBs






physicsphysics

CosmologyCosmology



Scientific rationale of a new GRB mission Scientific rationale of a new GRB mission

GRB phenomenonGRB phenomenon Diversity and unity of GRBsDiversity and unity of GRBs







physicsphysics

CosmologyCosmology








Elliptical host galaxy at z = 0.225

Gehrels et al., Nat 437, 851, 2005 Gehrels et al., Nat 437, 851, 2005

GRB 050509B

Short GRBs from NS merging?Short GRBs from NS merging?






physicsphysics

CosmologyCosmology





CosmologyCosmology




On 13/09/08 at 06:46:54 Swift/BAT triggers on GRB 080913T + 2 m: Swift/XRT and Swift/UVOT observe the GRB (X-ray & visible)T + 3 m: GROND observes the GRB field in the visible and NIR band

Shady et al., GCN 8217, 2008 Shady et al., GCN 8217, 2008

The farthest ever GRB The farthest ever GRB

z = 6.7z = 6.7

Greiner et al., GCN 8223, 2008 Greiner et al., GCN 8223, 2008

T + 2 h: VLT records a NIR spectrum

VISIBLE

NIR


z 0,01 0,1 1 10

DL

(cm

)

1028

1029

1027

GRBs

SNIa (SCP)

SNIa (Calàn-Tololo)

ΩM=0.0, ΩΛ=1.0ΩM=0.3, ΩΛ=0.7ΩM=1.0, ΩΛ=0.0

Epeak–Eiso correction applied to GRB data

GRB GRB 080913080913

Ghirlanda et al., ApJ 613, L13, 2004 Ghirlanda et al., ApJ 613, L13, 2004

GRBs as standard candle ?GRBs as standard candle ?






physicsphysics

CosmologyCosmology






physicsphysics


anticipate that GRBs could be sources of:

Ultra high energy cosmic rays

High energy neutrinos

Gravitational waves

In the framework of the “standard” model of GRBs, many theoreticians

AUGER SOUTH

AUGER NORTH

ANTARES

AMANDA

ICECUBE

KM3VIRGO

LIGO


What we What we requirerequirefforor the SVOM mission the SVOM mission


Permit the detection of all know types of GRBs, with a special care on Permit the detection of all know types of GRBs, with a special care on high-z GRBs and low-z sub-luminous GRBshigh-z GRBs and low-z sub-luminous GRBs

Scientific requirements on SVOMScientific requirements on SVOM

Provide fast, reliable and accurate GRB positionsProvide fast, reliable and accurate GRB positions

Measure the broadband spectral shape of the prompt emissionMeasure the broadband spectral shape of the prompt emission(from visible to MeV)(from visible to MeV)

Measure the temporal properties of the prompt emissionMeasure the temporal properties of the prompt emission

Quickly identify the afterglows of detected GRBs, including those Quickly identify the afterglows of detected GRBs, including those which are highly redshifted (z>6)which are highly redshifted (z>6)

Quickly provide (sub-) arcsec positions of detected afterglowsQuickly provide (sub-) arcsec positions of detected afterglows

Quickly provide redshift indicators of detected GRBsQuickly provide redshift indicators of detected GRBs


A wide field-of-view cameraA wide field-of-view camera to trigger on GRBs present within its field- to trigger on GRBs present within its field-of-view in the of-view in the X-rayX-ray and and soft gamma-raysoft gamma-ray band band

A spectro-photometerA spectro-photometer to observe simultaneously to observe simultaneously in the gamma-ray in the gamma-ray bandband the trigger camera field-of-view the trigger camera field-of-view

A narrow field-of-view telescopeA narrow field-of-view telescope to quickly observe ( to quickly observe (after an after an autonomous satellite repointing)autonomous satellite repointing) in the in the soft X-ray bandsoft X-ray band the error box the error box provided by the trigger camera provided by the trigger camera A narrow field-of-view telescopeA narrow field-of-view telescope to quickly observe in the to quickly observe in the visible band visible band the error box provided by the trigger camera the error box provided by the trigger camera

A set of ground-based wide field-of-view camerasA set of ground-based wide field-of-view cameras to observe to observe simultaneously in the simultaneously in the visiblevisible band the trigger camera field-of-view band the trigger camera field-of-view

Two ground-based narrow field-of-view telescopesTwo ground-based narrow field-of-view telescopes to quickly observe to quickly observe in the in the visiblevisible and and near infrarednear infrared bands the error box provided by the bands the error box provided by the trigger camera trigger camera

Scientific instrumentsScientific instruments


Selected scientific instrumentsSelected scientific instruments

ECLAIRs coded mask telescope2 sr FOV; 4-250 keV

XIAO soft X-ray telescope23x23 arcmin FOV; 0.5-2 keV

VT optical telescope400-1000 nm

GRM gamma-ray monitor2 sr FOV; 50 keV - 5 MeV

GWACS F-GFT QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.C-GFT


What we expect fromWhat we expect fromthe SVOM instrumentsthe SVOM instruments


ECLAIRs: the trigger cameraECLAIRs: the trigger camera

Main design objectiveMain design objective

A low energy threshold in the X-ray domain

Simulated sensitivitySimulated sensitivity

3.5 keV

Energy (keV)10 40 605020 30

Cou

nts

100

200

300

0

10010 103

Peak energy (keV)

1

Sen

sitiv

ity (

ph c

m-2 s

-1)

ECLAIRs

BAT

IBIS

BATSE

ECLAIRs expected to be more sensitive than SWIFT

(BAT) for GRBs whose peak energy is < 20 keV


ECLAIRs – Anticipated performancesECLAIRs – Anticipated performances

Simulated redshift distribution of long GRBs to be detected by ECLAIRsSimulated redshift distribution of long GRBs to be detected by ECLAIRs

Nearly 20% of ECLAIRs GRBs could be situated at high redshift (z > 6)Nearly 20% of ECLAIRs GRBs could be situated at high redshift (z > 6)

0 6 1082 40

Redshift z

20

40

60

80

100

Fra

ctio

n >

z (

%)

ECLAIRs

SWIFT (bright) SWIFT

DATA (SWIFT)


100 1031 10 104

Energy (keV)

10-5

Pho

ton

cm-2 s

-1 k

eV-1

10-4

10-6

10-3

10-2

10-1

1

10

ECLAIRs

GRM

T=1s

Average GRB spectrum with a 50-300 keV flux of 1 photon cmAverage GRB spectrum with a 50-300 keV flux of 1 photon cm-2-2 s s-1-1

GRM: the gamma-ray spectrometer GRM: the gamma-ray spectrometer

Enable EEnable Epeakpeak measurement up to measurement up to ~ 500 keV~ 500 keV


103 104100Seconds from trigger

10-3

Flu

x (c

ount

s s-1

)

10-1

1

1000.1

0.51.0

10

100

1000

50002000

100002000050000 5σ

det

ectio

n tim

e (s

)

Expected XIAO light curves for a sample of representative afterglowsExpected XIAO light curves for a sample of representative afterglows

XIAO: the soft X-ray telescope XIAO: the soft X-ray telescope

XIAO is sensitive enough to provide precise localizations for most GRBs


12 14 16 18 20 22 24Magnitude at 1000 seconds

0.2Cum

ulat

ive

prob

abili

ty

0.0

0.4

0.6

0.8

1.0

VT: the visible telescope VT: the visible telescope

The intrinsic cumulative GRB apparent optical afterglow distributionThe intrinsic cumulative GRB apparent optical afterglow distribution

VT is sensitive enough to detect ~ 80% of the SVOM GRBs

Akerlof & Swan, ApJ 671, 1868, 2007

UVOT-UVOT-SWIFTSWIFT

VT-SVOMVT-SVOM


Spectral bandSpectral band Field of Field of ViewView

Localization Localization AccuracyAccuracy GRBs/yrGRBs/yr

GRMGRM 50keV-5MeV50keV-5MeV 2 sr2 sr Not applicableNot applicable ~80~80

ECLAIRsECLAIRs 4-250 keV4-250 keV 2 sr2 sr 10 arcmin10 arcmin ~80~80

XIAOXIAO 0.3-2 keV0.3-2 keVdiameterdiameter

25 arcmin25 arcmin10 arcsec10 arcsec ~72~72

VTVT400-650 nm400-650 nm

650-950 nm650-950 nm

21 21 21 21

arcsecarcsec1 arcsec1 arcsec ~64~64

Space instruments expected performancesSpace instruments expected performances


Ground instrumentsGround instrumentsGWACGWAC

Wavelength coverage:Wavelength coverage:

Limiting magnitude:Limiting magnitude:

Overall field-of-view:Overall field-of-view:

~ ~ 400-900 nm400-900 nm

~ ~ 15 (515 (5σσ, 10s), 10s)

~ ~ 90 deg. 90 deg. × 90× 90 deg. deg.

C-GFTC-GFTDiameter:Diameter:

Field-of-view:Field-of-view:

Wavelength coverage:Wavelength coverage:

~ 100 c~ 100 cmm

~ ~ 23 arcmin 23 arcmin × 23 arcmin× 23 arcmin

~ 400-950 nm~ 400-950 nm

F-GFTF-GFTDiameter:Diameter:

Field-of-view:Field-of-view:

Photometric band:Photometric band:

~ 100 c~ 100 cmm~ ~ 30 arcmin 30 arcmin × 30 arcmin× 30 arcmin

B V R I J HB V R I J HPhotometric redshift of high z GRBs


SVOM multi-wavelength capabilitiesSVOM multi-wavelength capabilities

Space and ground instruments join to enable a unique coverageSpace and ground instruments join to enable a unique coverage

102 103 104 105101-5 0

1022

1020

1016

1018

1014

1015

1014

Time (s)Log. scale

Time (m)Lin. scale

Fre

quen

cy (

Hz)

Fre

quen

cy (

Hz) Space

Ground

Slew

GRM

ECLAIRs XIAO

VT

GWAC

F-GFT

C-GFT


OrbitOrbit

Altitude:Altitude: Inclination:Inclination:~ ~ 600-650 km600-650 km < 30 deg.< 30 deg.

-60 0-180 -120 60 120 180Longitude

Latit

ude

-60

-90

-30

0

30

60

90

SAA


Pointing strategyPointing strategy

Anti-solarAnti-solar

Avoid the Milky WayAvoid the Milky Way

Avoid the strongest sources (Sco X-1)Avoid the strongest sources (Sco X-1)

QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.

Requirement: aRequirement: adjust the observing program to allow djust the observing program to allow follow-up observationsfollow-up observations with the with the largest ground telescopeslargest ground telescopes (8 m class) in (8 m class) in > 75% of the cases> 75% of the cases


Space-ground linkSpace-ground link

Prompt delivery of the basic GRB dataPrompt delivery of the basic GRB data

Dedicated VHF NetworkDedicated VHF Network


ScheduleScheduleDeveloped by CNES, CNSA, & CAS: end of phase A successfully Developed by CNES, CNSA, & CAS: end of phase A successfully reached; Launch in 2013reached; Launch in 2013

Life-time: 3 years (goal: 5 years)Life-time: 3 years (goal: 5 years)

Links with the astronomical communityLinks with the astronomical communityPrompt delivery of the basic GRB data to the GCN will enable the Prompt delivery of the basic GRB data to the GCN will enable the whole GRB community to react upon SVOM GRBswhole GRB community to react upon SVOM GRBs

Join the SVOM project through the SVOM VHF Collaboration!Join the SVOM project through the SVOM VHF Collaboration!

To install our VHF receivers we are looking for sites withTo install our VHF receivers we are looking for sites with unocculted horizonsunocculted horizons permanent internet connectionpermanent internet connection -30°< latitude < 30°-30°< latitude < 30°

Contact me: Contact me: [email protected]@cea.fr


SVOM compared to SWIFTSVOM compared to SWIFT

Prompt emission measurementMore sensitive below 20-30 keVMore sensitive below 20-30 keV

EEpeakpeak measurement capability measurement capability

Multi-wavelength capabilities from visible band to MeV gamma rays Multi-wavelength capabilities from visible band to MeV gamma rays

Afterglow emission measurement > 10 more sensitive in the visible> 10 more sensitive in the visible

Sensitive in the 650-950 nm bandSensitive in the 650-950 nm band

Follow-up observationsDedicated follow-up robotic telescopesDedicated follow-up robotic telescopes

GRBs much easily scrutinized by the largest telescopesGRBs much easily scrutinized by the largest telescopes

SVOM: the successor of SWIFT


SVOM measurement requirements (1)SVOM measurement requirements (1)LocalizeLocalize during the nominal duration of the mission during the nominal duration of the mission ≥≥ 200 GRBs of all kinds200 GRBs of all kinds, , including including shortshort GRBs (0.005-2 s), GRBs (0.005-2 s), long long GRBs (up to 1000s) and GRBs GRBs (up to 1000s) and GRBs particularly particularly rich in X-raysrich in X-rays

In all cases, observe the GRB field in the In all cases, observe the GRB field in the X-ray and gamma-ray band X-ray and gamma-ray band (4 keV to 5 MeV)(4 keV to 5 MeV) from from 5 min before 5 min before andand 10 min after T 10 min after T00

In In > 70%> 70% of the cases, observe the GRB direction in the of the cases, observe the GRB direction in the soft X-raysoft X-ray and and visiblevisible bands frombands from < 5 min< 5 min after T after T00 and up to and up to TT00+1 day+1 day (down to a limit (down to a limit

magnitude Mmagnitude MVV = 23) = 23)

Measure the Measure the GRB celestial coordinatesGRB celestial coordinates with an accuracy better than with an accuracy better than 1122 arc arc minmin (for 7 sigma sources) in J2000 reference frame (for 7 sigma sources) in J2000 reference frame

In In > > 220%0% of the cases, observe simultaneously of the cases, observe simultaneously 5min before 5min before and and 115 min 5 min afterafter TT00 inin visible bandband down to a limit magnitude down to a limit magnitude MMVV = = 1515

Trigger on GRBs Trigger on GRBs present withinpresent within the field of view during the field of view during part of their durationpart of their duration


In In all all casescases where a candidate counterpart is detected by the soft X-ray where a candidate counterpart is detected by the soft X-ray telescope, measure on-board its telescope, measure on-board its celestial coordinatescelestial coordinates with an accuracy with an accuracy in in J2000 J2000 better than better than 40 arc sec40 arc sec, with a goal of , with a goal of 220 arc sec0 arc sec after ground after ground processing within processing within 8 min8 min after Tafter T00 in 80% of the cases in 80% of the cases

In all casesIn all cases where a candidate is detected by the on-board visible where a candidate is detected by the on-board visible telescopetelescope, , deliver deliver the GRB the GRB celestial celestial coordinatescoordinates with an accuracy better with an accuracy better than than 1 arc sec1 arc sec J2000 frame J2000 frame within within 1 1 hourhour after T after T00

In In > 40%> 40% of the cases, in of the cases, in < 5 min< 5 min after T after T00, measure the error box of the , measure the error box of the

GRB with F-GFT or C-GFT. When the afterglow is detected, to measure the GRB with F-GFT or C-GFT. When the afterglow is detected, to measure the celestial coordinates of the GRB with a relative accuracy better than celestial coordinates of the GRB with a relative accuracy better than 0.5 arc 0.5 arc sec sec in the J2000 frame,in the J2000 frame, and its flux in at least 3 photometric bandsand its flux in at least 3 photometric bands

AAdjust the observing program to allow djust the observing program to allow follow-up observationsfollow-up observations with the with the largest ground telescopeslargest ground telescopes (8 m class) in (8 m class) in > 75% of the cases> 75% of the cases

Make available the best measurement of the GRB Make available the best measurement of the GRB celestial coordinatescelestial coordinates to to ground based telescopes in ground based telescopes in less than 1 minless than 1 min after Tafter T00 in 85% of the cases in 85% of the cases

and in less than 2 min and in less than 2 min after Tafter T00 in less than 90% the cases (TBC) in less than 90% the cases (TBC)

SVOM measurement requirements (2)SVOM measurement requirements (2)

06/02/2009diego götz - the svom mission1 la thuile italy 06/02 2009 44 th rencontres de moriond...

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