EUCLID Euclid On behalf of Isobel Hook Thanks to Euclid team (especially Bruno and Stephen in the audience) Euclid background • Part of the ESA cosmic visions M‐class (~450Meuros) selecHon process with launch in 2018 • Only truly extragalacHc mission in process (except SPICA which is joint JAXA mission) • SubmiRed yellow book late last year and await final decision in February • ~3 missions go into a 18 month definiHon phase with 2M‐class missions being selected Euclid in a nutshell • Euclid is a cosmology mission using BAO and WL as its primary probes. • Wide‐field imaging over 20000 sq degs to R+I+Z=24 and J,H,K photometry. • Slitless spectroscopy over same area to H~19.5 with 70M galaxies and sample 19Gpc3 • ~1% precision in cosmological parameters, test GR on large scales to 2% • Awesome legacy value including possible galacHc surveys and planet searches (hRp://arxiv.org/abs/ 1001.3349) • 122 page YB at hRp://arxiv.org/abs/0912.0914 JDEM • Presently part of the Decadal Review process in the USA (~summer reporHng). Includes detailed cost and schedule informaHon • Three mission concepts (SNAP, ADEPT and DESTINY). Some discussions of merging these • A year ago, embryonic discussions of IDECS – those are frozen because of CV and Decadal • JDEM could be a stronger mission for transients Supernovae with Euclid Isobel Hook University of Oxford and INAF (Obs. Roma) Thanks to R. Nichol, M. Della Valle, F. Mannucci, A. Goobar, P. AsHer, B. Leibundgut, A. Ealet Euclid Conference 17‐18 Nov 2009 Finding & Using Supernovae • Need to know for each SN – Type – Redshin – For cosmology: distance (from corrected peak magnitude) • in turn requires colours and good sampling of the lightcurve Example images from the High-z team (Schmidt et al) Example spectrum and mulH‐colour light‐curve from SNLS Parameters of a Euclid SN survey (i) Imaging • Deep survey (repeat observaHons) – Lightcurves in J, H, K, (R+I+Z) – photo‐zs for most host galaxies – spaHal locaHon of the SN within its host • Details TBD (matched to primary science requirements) – FOV > 40 sq deg in at least two patches of > 10 sq deg – ~40 visits : Cadence TBD J, H, K (5σ point source) R+I+Z (10σ extended source) Depth Each Visit (AB mag) Final Depth (AB mag) 24 26 24.5 26.5 Above: Euclid deep survey parameters: imaging Parameters of a Euclid SN survey (ii) Spectroscopy • Deep survey – spectroscopic z for brighter host galaxies – some spectroscopic SN types. Photo typing needs to be invesHgated • Details TBD Depth Each Visit (AB mag) Final Depth (AB mag) Slitless spectroscopy (conHnuum) H~19.5 H~21.5 DMD spectroscopy (conHnuum) H~22 H~24 Above: Euclid deep survey parameters: spectroscopy PotenHal for valuable SN survey: Deep (esp NIR), wide area, stable Expected Euclid SN counts in J band Counts for a 5 year survey assuming 10 sq deg monitored at any Hme. Produces 1000‐2000 SNeIa to z<0.7 Plus a further 1000‐2000 to z<1 (detecHons only) Comparable number of CC SNe N(z) for SNe detected 1 mag fainter than peak, esHmated by A. Goobar based on assumpHons in Goobar et al arXiv:0810.4932 (SN Ia rates from Dahlen et al 2004). “DetecHon‐only” curve is an esHmate (IH) of total number of detectable SNeIa (no lightcurves) IdenHfied systemaHcs in SNLS3 (preliminary) Systematic • Brightness‐colour relaHon is complex • Different RV cf our Galaxy? • SN show intrinsic colour‐L relaHon (β) • Possible z variaHon of β • Euclid NIR photometry will disentangle these effects % <w> Extra error Statistical only 4.3 … SNLS zero points 4.5 1.3 SNLS filters 4.4 0.6 External zero points 4.7 1.9 External filters 4.5 0.8 SN colour relation 5.0 2.5 BD+17 colours 5.1 2.6 BD+17 SED 4.4 0.4 Peculiar velocities 4.4 0.5 Malmquist bias 4.4 0.7 Nicmos non-linearity 4.4 0.7 Non-Ia contamination 4.4 0.7 All systematics 6.8 5.0 Conley et al. in prep Euclid’s role in SN cosmology • Large sample – 1000 ‐ 2000 SNeIa z<0.7 • Deep, stable IR photometry – Control of dust exHncHon – Smaller scaRer in Hubble diagram at longer rest‐frame wavelengths • Benefit of coordinated ground‐based opHcal campaign – measure standard rest‐frame B‐band and I‐band distances to the same supernovae SN Ia mix vs redshin RelaHve mix of young+old evolves strongly with redshin Euclid rate measurement accurate to ~ 5% in Δz=0.1 bins Less affected by dust (Sullivan et al 2006) SNe with Euclid : Summary • Euclid deep surveys can provide (“for free”) • SNIa cosmology – much‐improved exHncHon correcHons – Rest‐frame I‐band Hubble diagram with thousands of objects to z ~ 0.7 – Benefit of coordinated ground‐based opHcal campaign measure standard rest‐frame B‐band and I‐band distances to the same supernovae • Accurate SN rates – Including exHncted SNe – Use to constrain progenitor models, models of feedback processes, SFH, beRer understanding of SNeIa for cosmology