CEA-Saclay, IRFU-Service d’Astrophysique The SVOM Mission for GRB Studies Bertrand Cordier CEA-Saclay, IRFU-Service d’Astrophysique

Prominent questions for the present decade Astrophysics How black holes form relativistic outflows? What was the first stellar population? How the Universe has been re-ionized? ....… Physics Where UHE cosmic-rays are accelerated? When a source of gravitational waves will be identified? Can we better constrain the nature of the dark energy? ....… Advanced GRB studies to provide unique answers

What we want to learn from the SVOM mission

Scientific rationale of the SVOM 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 The GRB-supernova connection Short GRB progenitors GRB progenitors Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies Cosmology Tracing star formation Re-ionization of the universe Cosmological parameters Cosmological lighthouses (absorption systems) Host galaxies Fundamental Origin of high-energy cosmic rays Probing Lorentz invariance Short GRBs and gravitational waves physics

Scientific rationale of the SVOM GRB mission CEA-Irfu, IRAP, APC, IAP, Paris, LAM, Obs Strasbourg, LPAG, LUPM, LAL, GEPI, LPC2E, University of Leicester, MPE

What we require for the SVOM mission

SVOM scientific instrument arrangement October 2013 MXT VT ECLAIRs GRM GFT-2 GWAC GFT-1

What we expect from the SVOM instruments

ECLAIRs: the trigger camera Main characteristics Coded mask telescope Wide FOV 2 Sr 6400 CdTe – 1024 cm2 4 keV – 250 keV Anticipated performances Loc. accuracy < 10arcmin 80 GRBs / year

GRM – The Gamma Ray Monitor Main characteristics NaI detectors FOV : 6 Sr 50 keV – 5 MeV Anticipated performances Loc. accuracy ~ 2° 110 GRBs / year

MXT – The Multi-channel X-ray Telescope Main characteristics Wolter-I X-ray lens FOV 1 deg2 PN CCD 256x256 75µ 0.3 keV – 10 keV Anticipated performances Loc. accuracy < 1 arcmin 20 arcsec for bright GRB 80 GRBs / year

VT – The Visible Telescope Main characteristics Ф=40cm FOV 1 : 26 x26 arcmin2 2 X 2048x2048 CCD 400 nm – 950 nm Anticipated performances Loc. accuracy < 2 arcsec Mv = 22.5 in 300s

Photometric redshift of high z GRBs Ground instruments GWAC Wavelength coverage: ~ 400-900 nm Limiting magnitude: ~ 15 (5σ, 10s) Overall field-of-view: ~ 90 deg. × 90 deg. GFT-1 Diameter: ~ 100 cm Field-of-view: ~ 23 arcmin × 23 arcmin Wavelength coverage: ~ 400-950 nm GFT-2 Diameter: ~ 100 cm Field-of-view: ~ 30 arcmin × 30 arcmin Photometric band: B V R I J H Photometric redshift of high z GRBs

A gold plated example from SWIFT satellite On 04/23/09 (07:55:19 UT): Swift/BAT triggers on a long GRB (GRB 090423) σPosition ≈ 3 arcmin SWIFT XRT SWIFT BAT T + 72 sec: Swift/XRT start observations σPosition ≈ 2.3 arcsec T + 16h: photometric indication of a very high redshift by 2.2m MPE telescope σPosition < 1 arcsec & z ≈ 8.1±0.4 T + 17.5h: spectroscopic confirmation of the redshift by ESO/VLT z ≈ 8.26±0.07 → ECLAIRs → MXT → VT & GFTs → Suivi

SVOM multi-wavelength capabilities 102 103 104 105 10 1 -5 1022 1020 1016 1018 1014 1015 Time (s) Log. scale Time (m) Lin. scale Frequency (Hz) Space Ground Slew GRM ECLAIRs MXT VT GWAC GFT-1 GFT-2 Space and ground instruments join to enable a unique coverage

Mission requirements

SVOM Pointing Strategy Sun Night side SVOM orbit (i ~ 30°) Most of the GRBs detected by SVOM to be well above the horizon of large ground based telescopes all located at tropical latitudes

SVOM- attitude law anti solar ECLAIRs FOV roque de los muchachos maunea kea SCO X1 anti solar GALACTIC PLANE Cerro Paranal ECLAIRs FOV

Prompt Dissemination of GRB Parameters

SVOM Observation Strategy Space ECLAIRs and GRM observe the prompt X/gamma emission GRB trigger provided by ECLAIRs at timeT0 multi messenger follow-up Robotic telescopes T0 + 1 min GFTs (B, V, R, I, J, H band) VT (V and R bands) MXT (soft X-rays) T0 + 2-5 min Ground GWAC (prompt in the V band)

SVOM and the GW The coalescence of compact binary system is supposed to be an effective source of gravitational waves detectable by the advanced version of the ground based gravitational-wave detectors LIRGO and Virgo. 2017 2019 2022 The ground based detectors LIGO and Virgo are rapidly improving in sensitivity and localization. In 2020+ the network should be able to detect the likely binary neutron collapse up to 450Mpc within an error box of few deg2. Expected NS-NS mergers detection rate: about 40/year within 445 Mpc (z~0.1) Expected BH-NS mergers detection rate: about 10/year within 927 Mpc (z~0.2) (Abadie et al. 2010) Thanks to MXT, SVOM has a good probability to detect and localise a GW event associated to a short GRB

SVOM Science Management Plan The scientific exploitation of the SVOM mission is organized as follows: Three main categories: 1- The Core Program : GRB science 1.1- The Burst Advocates 1.2- Key programs 1.3-Exceptional GRBs 2- The General Program : Non-GRB science 2.1- Pointed narrow-field observations 2.2- Wide-field surveys 3- Targets of Opportunity Chinese and French scientists have a complete access to the data provided by all SVOM instruments. The publications involving SVOM data are submitted to a rule respecting a ratio China/France

Road MAP - 2014 Mars 2014 dégel de la mission SVOM –> lancement 2020 Juin 2014 signature du MOU entre le CNES et la CNSA le statut du télescope X nos droits sur les données Eté 2014 kick-off phase B mission SVOM Fin été 2014 réunion scientifique SVOM France Fédérer la communauté SVOM France Présentation du Science Management Plan Préparer le suivi des alertes Préparer la science hors-sursaut

University of Leicester NAOC, Beijing IHEP, Beijing XIOPM, Xi’an SECM, Shanghai CEA-Irfu, Saclay IRAP, Toulouse APC, Paris IAP, Paris LAM, Marseille Obs Strasbourg LPAG Grenoble LUPM Montpellier LAL Orsay GEPI Meudon LPC2E Orléans University of Leicester MPE, Garching CNES, Toulouse GO SVOM ! Expected launch 2020 Phase B kick-off 2014

谢谢 Thank you