06/02/2009Diego Götz - The SVOM Mission1 La Thuile Italy 06/ th Rencontres de Moriond SVOM A new mission for Gamma-Ray Bursts Studies Diego Götz Irfu-SAp, CEA Saclay on behalf of the SVOM Collaboration

06/02/2009Diego Götz - The SVOM Mission2 GRB physics Acceleration and nature of the relativistic jet Radiation processes The early afterglow and the reverse shock The GRB-supernova connection Short GRB progenitors GRB progenitors Fundamental Origin of high-energy cosmic rays Probing Lorentz invariance Short GRBs and gravitational waves physics Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies Scientific rationale of the SVOM mission GRB phenomenon Diversity and unity of GRBs GRB phenomenon Diversity and unity of GRBs

06/02/2009Diego Götz - The SVOM Mission3 GRB physics Acceleration and nature of the relativistic jet Radiation processes The early afterglow and the reverse shock The GRB-supernova connection Short GRB progenitors GRB progenitors Fundamental Origin of high-energy cosmic rays Probing Lorentz invariance Short GRBs and gravitational waves physics Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies Scientific rationale of a new GRB mission GRB phenomenon Diversity and unity of GRBs GRB physics Acceleration and nature of the relativistic jet Radiation processes The early afterglow and the reverse shock

06/02/2009Diego Götz - The SVOM Mission4 GRB physics Acceleration and nature of the relativistic jet Radiation processes The early afterglow and the reverse shock The GRB-supernova connection Short GRB progenitors GRB progenitors Fundamental Origin of high-energy cosmic rays Probing Lorentz invariance Short GRBs and gravitational waves physics Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies Scientific rationale of a new GRB mission GRB phenomenon Diversity and unity of GRBs The GRB-supernova connection Short GRB progenitors GRB progenitors

06/02/2009Diego Götz - The SVOM Mission5 Elliptical host galaxy at z = Gehrels et al., Nat 437, 851, 2005 GRB B Short GRBs from NS merging?

06/02/2009Diego Götz - The SVOM Mission6 GRB physics Acceleration and nature of the relativistic jet Radiation processes The early afterglow and the reverse shock The GRB-supernova connection Short GRB progenitors GRB progenitors Fundamental Origin of high-energy cosmic rays Probing Lorentz invariance Short GRBs and gravitational waves physics Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies Scientific rationale of a new GRB mission GRB phenomenon Diversity and unity of GRBs Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies

06/02/2009Diego Götz - The SVOM Mission7 On 13/09/08 at 06:46:54 Swift/BAT triggers on GRB T + 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 The farthest ever GRB The farthest ever GRB z = 6.7 Greiner et al., GCN 8223, 2008 T + 2 h: VLT records a NIR spectrum VISIBLENIR

06/02/2009Diego Götz - The SVOM Mission8 z 0,010,1110 D L (cm) GRBs SNIa (SCP) SNIa (Calàn-Tololo) Ω M =0.0, Ω Λ =1.0 Ω M =0.3, Ω Λ =0.7 Ω M =1.0, Ω Λ =0.0 E peak –E iso correction applied to GRB data GRB Ghirlanda et al., ApJ 613, L13, 2004 GRBs as standard candle ?

06/02/2009Diego Götz - The SVOM Mission9 GRB physics Acceleration and nature of the relativistic jet Radiation processes The early afterglow and the reverse shock The GRB-supernova connection Short GRB progenitors GRB progenitors Fundamental Origin of high-energy cosmic rays Probing Lorentz invariance Short GRBs and gravitational waves physics Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies Scientific rationale of a new GRB mission GRB phenomenon Diversity and unity of GRBs Fundamental Origin of high-energy cosmic rays Probing Lorentz invariance Short GRBs and gravitational waves physics

06/02/2009Diego Götz - The SVOM Mission10 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 KM3 VIRGO LIGO

06/02/2009Diego Götz - The SVOM Mission11 What we require for the SVOM mission

06/02/2009Diego Götz - The SVOM Mission12 Permit the detection of all know types of GRBs, with a special care on high-z GRBs and low-z sub-luminous GRBs Scientific requirements on SVOM Scientific requirements on SVOM Provide fast, reliable and accurate GRB positions Measure the broadband spectral shape of the prompt emission (from visible to MeV) Measure the temporal properties of the prompt emission Quickly identify the afterglows of detected GRBs, including those which are highly redshifted (z>6) Quickly provide (sub-) arcsec positions of detected afterglows Quickly provide redshift indicators of detected GRBs

06/02/2009Diego Götz - The SVOM Mission13 A wide field-of-view camera to trigger on GRBs present within its field- of-view in the X-ray and soft gamma-ray band A spectro-photometer to observe simultaneously in the gamma-ray band the trigger camera field-of-view A narrow field-of-view telescope to quickly observe (after an autonomous satellite repointing) in the soft X-ray band the error box provided by the trigger camera A narrow field-of-view telescope to quickly observe in the visible band the error box provided by the trigger camera A set of ground-based wide field-of-view cameras to observe simultaneously in the visible band the trigger camera field-of-view Two ground-based narrow field-of-view telescopes to quickly observe in the visible and near infrared bands the error box provided by the trigger camera Scientific instruments Scientific instruments

06/02/2009Diego Götz - The SVOM Mission14 Selected scientific instruments Selected scientific instruments ECLAIRs coded mask telescope 2 sr FOV; keV XIAO soft X-ray telescope 23x23 arcmin FOV; keV VT optical telescope nm GRM gamma-ray monitor 2 sr FOV; 50 keV - 5 MeV GWACS F-GFT C-GFT

06/02/2009Diego Götz - The SVOM Mission15 What we expect from the SVOM instruments

06/02/2009Diego Götz - The SVOM Mission16 ECLAIRs: the trigger camera Main design objective A low energy threshold in the X-ray domain Simulated sensitivity 3.5 keV Energy (keV) Counts Peak energy (keV) 1 Sensitivity (ph cm -2 s -1 ) ECLAIRs BAT IBIS BATSE ECLAIRs expected to be more sensitive than SWIFT (BAT) for GRBs whose peak energy is < 20 keV

06/02/2009Diego Götz - The SVOM Mission17 ECLAIRs – Anticipated performances Simulated redshift distribution of long GRBs to be detected by ECLAIRs Nearly 20% of ECLAIRs GRBs could be situated at high redshift (z > 6) Redshift z Fraction > z (%) ECLAIRs SWIFT (bright)SWIFT DATA (SWIFT)

06/02/2009Diego Götz - The SVOM Mission Energy (keV) Photon cm -2 s -1 keV ECLAIRs GRM T=1s Average GRB spectrum with a keV flux of 1 photon cm -2 s -1 GRM: the gamma-ray spectrometer Enable E peak measurement up to ~ 500 keV

06/02/2009Diego Götz - The SVOM Mission Seconds from trigger Flux (counts s -1 ) σ detection time (s) Expected XIAO light curves for a sample of representative afterglows XIAO: the soft X-ray telescope XIAO is sensitive enough to provide precise localizations for most GRBs

06/02/2009Diego Götz - The SVOM Mission Magnitude at 1000 seconds 0.2 Cumulative probability VT: the visible telescope The 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-SWIFT VT-SVOM

06/02/2009Diego Götz - The SVOM Mission21 Spectral band Field of View Localization Accuracy GRBs/yr GRM50keV-5MeV 2 sr Not applicable ~80 ECLAIRs keV 2 sr 10 arcmin ~80 XIAO keV diameter 25 arcmin 10 arcsec ~72 VT nm nm 21  21 arcsec 1 arcsec ~64 Space instruments expected performances Space instruments expected performances

06/02/2009Diego Götz - The SVOM Mission22 Ground instruments GWAC Wavelength coverage: Limiting magnitude: Overall field-of-view: ~ nm ~ 15 (5 σ, 10s) ~ 90 deg. × 90 deg. C-GFTDiameter: Field-of-view: Wavelength coverage: ~ 100 cm ~ 23 arcmin × 23 arcmin ~ nm F-GFTDiameter: Field-of-view: Photometric band: ~ 100 cm ~ 30 arcmin × 30 arcmin B V R I J H Photometric redshift of high z GRBs

06/02/2009Diego Götz - The SVOM Mission23 SVOM multi-wavelength capabilities Space and ground instruments join to enable a unique coverage Time (s) Log. scale Time (m) Lin. scale Frequency (Hz) Space Ground Slew GRM ECLAIRs XIAO VT GWAC F-GFT C-GFT

06/02/2009Diego Götz - The SVOM Mission24 Orbit Altitude:Inclination: ~ km < 30 deg Longitude Latitude SAA

06/02/2009Diego Götz - The SVOM Mission25 Pointing strategy Anti-solar Avoid the Milky Way Avoid the strongest sources (Sco X-1) Requirement: adjust the observing program to allow follow-up observations with the largest ground telescopes (8 m class) in > 75% of the cases

06/02/2009Diego Götz - The SVOM Mission26 Space-ground link Prompt delivery of the basic GRB data Dedicated VHF Network

06/02/2009Diego Götz - The SVOM Mission27 Schedule Developed by CNES, CNSA, & CAS: end of phase A successfully reached; Launch in 2013 Life-time: 3 years (goal: 5 years) Links with the astronomical community Prompt delivery of the basic GRB data to the GCN will enable the whole GRB community to react upon SVOM GRBs Join the SVOM project through the SVOM VHF Collaboration! To install our VHF receivers we are looking for sites with unocculted horizons unocculted horizons permanent internet connection permanent internet connection -30°< latitude < 30° -30°< latitude < 30° Contact me:

06/02/2009Diego Götz - The SVOM Mission28 SVOM compared to SWIFT Prompt emission measurement More sensitive below keV E peak measurement capability Multi-wavelength capabilities from visible band to MeV gamma rays Afterglow emission measurement > 10 more sensitive in the visible Sensitive in the nm band Follow-up observations Dedicated follow-up robotic telescopes GRBs much easily scrutinized by the largest telescopes SVOM: the successor of SWIFT

06/02/2009Diego Götz - The SVOM Mission29 SVOM measurement requirements (1) SVOM measurement requirements (1) Localize during the nominal duration of the mission ≥ 200 GRBs of all kinds, including short GRBs ( s), long GRBs (up to 1000s) and GRBs particularly rich in X-rays In all cases, observe the GRB field in the X-ray and gamma-ray band (4 keV to 5 MeV) from 5 min before and 10 min after T 0 In > 70% of the cases, observe the GRB direction in the soft X-ray and visible bands from 70% of the cases, observe the GRB direction in the soft X-ray and visible bands from < 5 min after T 0 and up to T 0 +1 day (down to a limit magnitude M V = 23) Measure the GRB celestial coordinates with an accuracy better than 12 arc min (for 7 sigma sources) in J2000 reference frame In > 20% of the cases, observe simultaneously 5min before and 15 min after T 0 inband down to a limit magnitude M V = 15 In > 20% of the cases, observe simultaneously 5min before and 15 min after T 0 in visible band down to a limit magnitude M V = 15 Trigger on GRBs present within the field of view during part of their duration

06/02/2009Diego Götz - The SVOM Mission30 In all cases where a candidate counterpart is detected by the soft X-ray telescope, measure on-board its celestial coordinates with an accuracy in J2000 better than 40 arc sec, with a goal of 20 arc sec after ground processing within 8 min after T 0 in 80% of the cases In all cases where a candidate is detected by the on-board visible telescope, deliver the GRB celestial coordinates with an accuracy better than 1 arc sec J2000 frame within 1 hour after T 0 In > 40% of the cases, in 40% of the cases, in < 5 min after T 0, measure the error box of 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 0.5 arc sec in the J2000 frame, and its flux in at least 3 photometric bands Adjust the observing program to allow follow-up observations with the largest ground telescopes (8 m class) in > 75% of the cases Make available the best measurement of the GRB celestial coordinates to ground based telescopes in less than 1 min after T 0 in 85% of the cases and in less than 2 min after T 0 in less than 90% the cases (TBC) SVOM measurement requirements (2) SVOM measurement requirements (2)