Large field of view and ELTs: an impossible marriage?

1. www.bo.astro.it/maory Large field of view and ELTs: an impossible marriage? Paolo Ciliegi (INAF -OABO) on behalf of the MAORY team Multi conjugate Adaptive Optics RelaY for the E-ELT INAF (OA-Bologna, OA-Padova, IASF-Bologna, OA-Arcetri) Università di Bologna Office National d’Etudes et des RecherchesAerospatiales European Organisation for Astronomical Research in the Southern Emisphere Tomelleris.r.l.

2. OUTLINE • MAORY OVERVIEW : the multi conjugate adaptive optics module for ELT • THE LARGEST POSSIBLE FIELD OF VIEW @ ELT from GLAO to DIFFRACTION LIMIT • SYNERGIES BETWEEN SURVEY FACILITIES AND ELT.

3. What is MAORY? • Multi conjugate Adaptive Optics RelaY for the E-ELT • Corrected field of view • Central unvignetted 53"x53" • Maximum requested field Ø=120" • Technical field Ø=160" for Natural Guide Star search • Wavefront sensing • 6 Sodium LGS WFSLGS projected from M1 edge • 3 NGS WFS • Wavefront correction • Telescope M4 + M5 • 2 post-focal deformable mirrors (4km, 12.7km) • Output ports for science instruments • Gravity invariant with mechanical derotation for MICADO • Lateral port for detached instrument (no mechanical derotation)

4. What is MAORY? • Client instruments • MICADO • High angular resolution camera (and slit spectrograph) • Precision astrometry and photometry • Required AO correction: uniform with high sky coverage • Wavelength range 0.8-2.4µm. Field of view: 53"53" • MAORY thermal background < 50% (telescope + sky) @Ks • SIMPLE • High spectral resolution IR spectrograph • Required AO correction: on-axis with high sky coverage • Others

5. Overall layout Pre-focal station Nasmyth platform MAORY MICADO Gravity invariant port Area fordetachedinstrument Lateralport

6. Post-focal relay

7. Performance – Strehl Ratio Seeing 0.8 arcsec Seeing 0.6 arcsec MAORY vs. ATLAS ATLAS performance courtesyof T. Fusco Ks 2.16µm H 1.65µm J 1.215µm I 0.9µm

8. Performance – Sky coverage Although we have 6 LGS projected from M1 edge, we still need Natural Guide Stars (NGS) for Tip Tilt correction Sodium layer effects

9. Sky coverage…. where to search NGS NGS WFS MICADO MAX FOV 160arcsec 53” 20”

10. Performance – Sky coverage • Sky coverage evaluated at North Galactic Pole • Reference conditions: Seeing 0.8", L0 = 25m • Random star counts generated by TRILEGAL code • 3-NGS asterisms formed for each trial down to H ~ 21 • “Best” asterism chosen. Figure of merit for each NGS asterism • Measurement noise • Temporal error • Anisoplanatic errors (NGS positions and uneven brightness) • Each star is assigned the Strehl Ratio value corresponding to its position in the NGS seach field Ø = 160" • Strehl Ratio comes from MCAO correction (1.5-1.8µm)

11. Performance – Sky coverage

12. THE LARGEST POSSIBLE FIELD OF VIEW @ ELT LARGE FIELD OF VIEW AND ELT : AN IMPOSSIBLE MARRIAGE ?

13. THE LARGEST POSSIBLE FIELD OF VIEW @ ELT LARGE FIELD OF VIEW AND ELT : AN IMPOSSIBLE MARRIAGE ? The actual imaging camera designed for E-ELT is MICADO characterized by superb capabilities in terms of sensitivity (K ~ 30 mag AB, 5 sigma , 1-2 ours) resolution (3 mas pix scale) and astrometric precision.

14. THE LARGEST POSSIBLE FIELD OF VIEW @ ELT LARGE FIELD OF VIEW AND ELT : AN IMPOSSIBLE MARRIAGE ? The actual imaging camera designed for E-ELT is MICADO characterized by superb capabilities in terms of sensitivity (K ~ 30 mag AB, 5 sigma , 1-2 ours) resolution (3 mas pix scale) and astrometric precision. The Micado Field of view is 53 x 53 arcsec.

15. 53 x 53 arcsec field with a spatial resolution at the diffraction limit level and a 3 mas pixels size is an impressive, huge field of view that will open new frontiers in may astronomical fields (see Greggio and Fiorentino talks) MICADO 53’’x53’’

16. 53 x 53 arcsec field with a spatial resolution at the diffraction limit level and a 3 mas pixels size is an impressive, huge field of view that will open new frontiers in may astronomical fields ….but of course is not a survey facility…. MICADO 53’’x53’’

17. WFI ESO 2.2m 2040’’ x 2040’’ (34’ x 34’) MICADO 53 x 53 arcsec WIRCAM CFHT near infrared 0.3’’/pixel 20’ x 20’ 2 MASS 8.5’ x 8.5’ ACS HST 202’’x202’’

18. WFI at the ELT Large deep imaging surveys have formed the backbone of extra-galactic survey for the last 15-20 years and there is no reason to expect this to change dramatically in the coming years. LSST VISTA VST SASIR Can we image a Wide Field Imager for ELT that can play a direct role as survey facility? Network Program “ Wide Field Imaging at the E-ELT : from GLAO to diffraction limit” PI . M. Arnaboldi (ESO) (E-TRE-ESO-508-0755)

19. We investigate the possibility for a Wide Field Imager exploiting the full MCAO corrected field Balance between NGS search field Number of detectors NGS WFS 90 x 90 arcsec Pixel scale : 8-10mas MICADO MAX FOV 160arcsec 53”

20. ELT and Large Field of view Maximum field of view at a resolution slightly worse than diffraction limit (8-10 mas pixel scale) is about 90 x 90 arcsec. We can reach bigger field of view (tens of squared arcmin, 5’x5’) but we must accept moderate resolution at the level of the GLAO correction. These numbers confirm the difficulty of the giant telescopes to work alone as survey facilities, highlighting the absolute need for synergies among different facilities.

21. SYNERGY --- MAORY and NEAR INFRARED SURVEY Which is the fundamental “food” for MAORY ?

22. SYNERGY --- MAORY and NEAR INFRARED SURVEY Which is the fundamental “food” for MAORY ? In our sky coverage calculation, we simulated the availability of a deep (down to H=21) infrared catalogue For real observations we need real deep catalogues with: Reliable stars/galaxies separation. Accurate position (NGS probe have a FoV of 3’’) These catalogue must be already available at the time of the proposal in order to check the NGS asterism. Deep near infrared catalogues will be a fundamental input that forthcoming survey facilities like VISTA and SASIR must provide to ELT.

23. CONCLUSION THE COUPLED MAORY + MICADO IS A FANTASTIC TOOL IN TERMS OF STREHL RATIO, EE, SENSIBILITY RESOLUTION AND ASTROMETRIC PRECISION …HOWEVER WITH A FOV OF 53 X 53 arcsec is not an instrument for surveys

24. CONCLUSION THE COUPLED MAORY + MICADO IS A FANTASTIC TOOL IN TERMS OF STREHL RATIO, EE, SENSIBILITY RESOLUTION AND ASTROMETRIC PRECISION …HOWEVER WITH A FOV OF 53 X 53 arcsec is not an instrument for surveys We investigate the possibility for a Wide Filed imager @ ELT. At resolution slightly worse than diffraction limit the maximum FoV is ~ 90 x 90 arcsec, while at GLAO resolution is 5 x 5 arcmin. …. So Large Field of views and ELT seems to be an impossible marriage !!!

25. CONCLUSION THE COUPLED MAORY + MICADO IS A FANTASTIC TOOL IN TERMS OF STREHL RATIO, EE, SENSIBILITY RESOLUTION AND ASTROMETRIC PRECISION …HOWEVER WITH A FOV OF 53 X 53 arcsec is not an instrument for surveys We investigate the possibility for a Wide Filed imager @ ELT. At resolution slightly worse than diffraction limit the maximum FoV is ~ 90 x 90 arcsec, while at GLAO resolution is 5 x 5 arcmin. …. So Large Field of views and ELT seems to be an impossible marriage !!! …. This impossible marriage implies that the synergies between survey facilities and giant telescopes are fundamental. As an example we show that large (possible all sky) deep (H~ 21) near infrared catalogues are a fundamental input that forthcoming survey facilities must provide to ELT