A telescope for an ANtarctica Imaging & Survey Extragalactic Studies on Galaxy Evolution with a Wide Field Optical/IR telescope on Dome C A telescope for an ANtarctica Imaging & Survey denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Outline Interesting characteristics of Dome C from an astronomer working in the topic of galaxies Definition of the science project and how to carry it out Conclusions denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Atmospheric Emission (Burton et al. 2005) Bands @ ~200 m Bands @ 350, 450 m ? denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Thermal Emission at South Pole and Mauna Kea  for the same S/N: DDome C ≥ 3  Delsewhere (ground-based) Band l m) South Pole (1) Mauna Kea Ks 2.15 0.15 16.5 3 13.4 Kd 2.4 0.3 15.6 6 12.4 L’ 3.8 100 8.6 2000 5.3 M’ 4.8 1000 5.4 2.104 2.1 SB +3.2 +3.3 in mJy/arsec2 and magnitudes/arcsec2 (approx.) (1) from : Ashley et al. 1996, Nguyen et al. 1996, Phillips et al. 1999, Burton et al., 2001 denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Exceptional Natural seeing: ~ 300 mas above an altitude of ~ 30 - 50m Lawrence et al. (2004) Exceptional Natural seeing: ~ 300 mas above an altitude of ~ 30 - 50m Wide Isoplanetic Angle: ~ 6 arcsecs in visible denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Agabi et al. (2006) Balloon @ 30m 2.0’’ 1.5’’ 1.0’’ 0.5‘’ 0.0’’ denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Characteristics of Dome C Very cold (average -50°C down to -90°C) Very far away Dry atmosphere (250 m) Superb natural seeing (above ~30m) Wide isoplanetic angles (up to arcmin-sized in NIR) Long coherence times (+ isoplanetic angles   # NGS) Long « nights »  continuous observations High stability (clear skies for 74% of the time in winter) GOOD / BAD Very cold (average -50°C down to -90°C) Very far away Boreal aurorae (but close to geomagnetic South Pole) Tough conditions Human psychology denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

What path for Extragalactic Antarctica Astronomy ? Given the known characteristics of Dome C Given the known characteristics of galaxies Given the (ground-based or space) facilities already in use or in (already funded) project Assuming that any type of project must be (relatively) cheap Is there a « niche » that would provide Original Data to (at least) galaxy people ? denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Parameter Space for Galaxy Studies Range Related Science (not exhaustive) Field of View ≤ 1 arcmin (down to few arcsecs) Individual high-z galaxies Few (2-4) arcmins Deep Fields Several (10-20) arcmins Local galaxies, small surveys  1 sq. degree Surveys Spectral Resolution Imaging (R < 5) Morphology SEDs (R ~ few 10) SFR, SFH, … Low resolution (R ~ few 100) Redshifts Intermediate resolution (R ~ few 1000) Line ratios (Balmer decrement, abundances, …) High resolution ( R > 5000) Dynamics, line profiles Angular Resolution (in visible) Diffraction limited Stellar populations,  ~ 200 mas Morphology at high z ~ 1 arcsec Multi-wavelength analysis low-z Wavelength Range Optical (0.3 - 1.0 um) SFR, SFH, line diagnotiscs NIR (1.0 - 2.5 um) Mass, high-z MIR (2.5 - 15 um) PAH, AGN / starburst diagnostics FIR (15 - 200 um) SFR, dust, AGN/ starburst diagnostics Sub-mm (< 1 mm) SFR, dust Others : cost, PSF stability, temporal resiolution, Strehl ratio / EE, interferometry, coronography, … denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

What are we left* with ? *color coding can be further discussed… Wide field of view (Ø ~1 deg) Optical / NIR High angular resolution (but not diffraction-limited in visible) Imaging / SED (/ Spectroscopy) Operations : the simpler the better denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

What do we need ? Telescope M1: Ø ~ 3m An optical design for a wide field telescope providing < ~1/4’’ PSF ? Can we build a telescope on top of a 30-50m tower ? What if we can’t ? Some kind of AO ? denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

For instance : Optical Design from Gérard Lemaître Dprimary = 2 - 3m Wide FOV ~ 1 deg2 0.3 <  (m) < 1 Size of spot: 0.25’’ RMS Room for AO ? Behavior at  > 1m ? denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

How to get rid of the turbulent ground layer ? Build some sort of light and stiff 30 to 50m high tower ? h=30-50m denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

I recommend not using palm-trees ! If that proves possible, it is probably the simple way to reach the specifications but … I recommend not using palm-trees ! denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Wider isoplanetic angles From Aristidi et al. (2006): 0 (Dome C) ~6 arcsec  3 x 0 (Other sites)  x 10 probability of finding NGS in visible denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Even wider in NIR 0 (Dome C): ~ 6 arcsecs @ 0.5m 0 (Dome C): ~ 1/2 arcmin @ 2.2m denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

GLAO Simulations are being carried out by ONERA (Thierry Fusco) Adaptive optics enable large telescopes to provide diffraction limited images, but their corrected field is restrained by the angular decorrelation of the turbulent wave-fronts. However many scientific goals would benefit a wide and uniformly corrected field, even with a partial correction. Ground Layer Adaptive Optics (GLAO) systems are supposed to provide such a correction by compensating the lower part of the atmosphere only. Indeed, this layer is in the same time highly turbulent and isoplanatic on a rather wide field. denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Point source sensitivity of a WF survey (borrowed to Nicolas) Aperture: 3 m pixel scale = 0.24’’ Throughput = 30% Deep ‘standard’ Survey 30 sec per field 1000 deg2 in 133h or « 5 days » Very deep survey (Kd et L’) 30 min per field 100 deg2 in 35 « days » Diff (arc sec) 3m « standard » Survey (?000 sq deg) S/B = 5 « deep» Survey (?00 sq deg.) Kd 0.35 21.8 (17.9) 25.8 (20.1) L’ 0.65 16.5 (13.7) 18.7 (15.8) Passively cooled 200K and Low background telescope (e = 1%) Diffraction limited, AO Green italics: same telescope at best tropical site NICMOS HDF-N Limiting magnitudes: denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Complementary to SWIRE (7 fields 65 deg2) & WISE (All-sky survey) Antarctica « standard » Survey « deep» Survey SPITZER (IRAC) (SWIRE) WISE VISTA 3 m space 80 cm space 40 cm Paranal 4 m Int.time 30s 30 mn 1 sec Spatial resolution 0.4’’ (Limited by diffraction at 2 microns) 1.4’’ 5’’ per pixel ~ 0.7 ’’ Kd 21.8 (17.9) 1.3Jy 25.8 (20.1) 0.03Jy n.a. 19, 21, 22 At K short L’ 16.5 (13.7) 62.5Jy 18.7 (15.8) 8Jy 19.0 7.3Jy 15.3 (140Jy) Green: same telescope at best tropical site NICMOS HDF-N Limiting magnitudes: denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

OH suppressors studied at OAMP/LAM (jean-luc.gach@oamp.fr for details) Sky brightness at 650 nm << 2.2 μm dominated by OH emission will be essentially identical at Dome C to that at all other observatory sites, including Mauna Kea (Kenyon & Storey 2006) Decreasing OH airglow -> increasing SNR (by a factor of 2) but also increasing maximum exposure times before saturation -> better efficiency denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Multiband filters studied at OAMP/LAM (jean-luc. gach@oamp Multiband filters studied at OAMP/LAM (jean-luc.gach@oamp.fr for details) Lebrun et al. (1998) designed to detect LBGs at z ~ 3 Can be also be done in NIR Gain in exposure times -> better efficiency No need to frequently change filters denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

What would be the « killer » science case of the Antarctica Imaging Survey (ANIS) ? SDSS/VISTA-like survey (several thousands deg2) with JWST-like angular resolution (about 0.2’’) from visible to near-infrared wavelengths Galaxy Formation & Evolution (morphology, SEDs, photometric redshifts, …) Cosmology (cosmic shear, large scale structures, …) Galactic plane (stellar evolution and star formation) (Extra-)Solar system bodies denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

FIR/sub-mm prospective must not be forgotten IRAS discovered Ultra Luminous IR Galaxies (ULIRG) Are there any Ultra Luminous Sub-mm Galaxies (ULSG) ? First All-Sky survey in the sub-mm range denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Conclusions We propose a 2-3m visible - NIR (MIR) telescope that includes GLAO, a OH suppressor device and multi-band filters to carry out a SDSS/VISTA-like survey with JWST angular resolution : ANIS Must start soon to be useful for JWST, SPICA, ALMA More to come before Roscoff (hopefully) Think about a funding strategy (especially in Europe) denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

Dome C Let’s dream … Dome C / visible Dome C / near-IR Dome C / sub-mm denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16

M e r c i Dome C denis.burgarella@oamp.fr Optical and Infrared Wide-Field Astronomy in Antarctica 09/12/2018 01:16