SHARK-VIS: project status F. PEDICHINI &

SHARK-VIS TEAM LBT USER MEETING 2017

SHARK-VIS team: Osservatorio Astronomico di Roma

F. Pedichini (P.I., optics)

S. Antoniucci (science)

G. Li Causi (data reduction)

M. Mattioli (engineering, control SW)

M. Stangalini (AO simulation)

V. Testa (archive, pipeline, science)

Osservatorio Astronomico di Arcetri

E. Pinna (SOUL)

A. Puglisi, G. Agapito (AO simulation)

Osservatorio Astronomico di Padova

J. Farinato (SHARK-NIR P.I.)

SHARK-NIR team

INAF Trieste Archiving facility

Steward Observatory

P. Hinz (LBTI)

M. Montoya (LBTI)

E. Downey (LBTI)

LBTO & LBTO mountain crew

SHARK Science team 70+ researchers , 15+ affiliations

Supervisor board S. Esposito (INAF Arcetri) E. Giallongo (INAF OAR) R. Ragazzoni (INAF OAPD)

SHARK-VIS expected performance are based on “on sky experimental data” at 630nm from the Forerunner experiment with 5e-5 det. contrast

Pedichini+ 2017

SHARK-VIS MISSION: a fast track P.I. instrument to extend LBT AO-SCIENCE

into the visible

FWHM 17.3 mas S=0.5 630nm

Why not to go into the VISIBLE ?

Sky background is low Detectors are cheap and quite Albedo is increasing Bright recombination lines (Hα) λ/D resolution 15mas at 8m (ELT at K)

(L. Close et Al. SPIE 9148 – 2014)

SHARK-VIS project history:

Relevant publication:

2017/01 JATIS M.Stangalini, F. Pedichini et al.: Speckle statistics in adaptive optics images at visible wavelengths.

2016/09 arXiv 16090514P, AJ in press. F. Pedichini et al: High Contrast Imaging in the Visible: First Experimental Results at the Large Binocular Telescope.

2016/08 SPIE.9908E..32P. F.Pedichini, F.Ambrosino et al.: The V-SHARK high contrats imager at LBT.

2015/10 AO4ELT 2x F. Pedichini et al. J. Farinato et al.

2014/08 SPIE.9147E..7JF. J. Farinato, F. Pedichini, E. Pinna et al.: SHARK (System for coronagraphy with High-order adaptive optics from R to K bands): a proposal for the LBT 2nd generation instrumentation.

2014/08 SPIE.9147E..8Fs. M.Stangalini, F. Pedichini et al.: The solar system at 10 parsec: exploiting the ExAO of LBT in the visual wavelengths.

2014/03 ebi..confP4.74F. J. Farinato, C. Baffa et al.: The NIR arm of SHARK (System for coronagraphy with High-order adaptive optics from R to K bands).

2012 – first white paper from R to K

2014 – SHARK bino presented to LBT SAC

2014 – NIR and VIS from R to K with two PIs

2015 – Signature of SHARKS CDP MOUs

2016 - SHARK-VIS Conceptual Design Review

2017 Q1 – SHARK-VIS Final Deisgn Review

2017 Q3 – Delta FDR

SHARK-VIS requirements strongly driven by science cases to extend LBT AO science into the

VISIBLE (next talk by S. Antoniucci)

YOUNG ACCRETING PLANETS

hα PSF contrast at 150mas

<1e-4 (0.6” seeing)

Detection contrast at 150 mas

<5e-5 (after p.p.)

10” ADI optimized FOV

Coronagraphy

MINOR BODIES OF SOLAR SISTEM

Wavelength coverage from

400 to 1000nm

Diffraction limited core PSF

FWHM 10-25mas

Nyquist sampling at 500nm

6.5mas/pixel

DISK AND JET MORPHOLOGY

Detection contrast at 50 mas

<1e-3 (after p.p.) (1.2”seeing)

Fast frame rate (1kHz on 1.3” x 1.3“)

Fast & low RON detector

SDI by pupil splitting

Access to pupil plane

Simultaneous observing with SHARK-NIR and LMIRCAM

CLOSE BINARY STARS PATHFINDER for Coronagraphy and

exoplanets reflected light

SHARK-VIS science driven main requirements:

separation < 50 mas

1. 10 arcsec Field Of View

2. Diffraction limited from 0.4 to 1 micron

3. Active PSF and Pupil Stabilization

4. Fast frame rate (1kHz) for lucky imaging

5. NCPA mitigation

6. Selectable pupil optics (stop, Wollaston, hologram, grism….)

7. Coronagraphy and IFU ready

8. ….

a) Low budget (HW ≈ 400k)

b) Low mass < 100kg

c) Fast Track P.I. instrument < 2y

d) Low impact on LBTO ( < 0.5 FTE est.)

e) Designed to become an LBTO facility

2011 - FLAO COMMISSIONING AT LBT

HIP 76041 AT 750NM THE FORERUNNER (2015) AND CDP LAYOUT(2015-16)

SHARK-VIS the origins:

separation < 50 mas S.Esposito priv. comm.

SHARK-VIS timeline:

separation < 50 mas

FIRST LIGHT 18 MONTHS

≈Q1 2019

HARDWARE 400

FTE 732

TOTAL VALUE 1132

TAXES 22% 249

CONTINGENCY 20% 226

TOTAL 1607

HARDWARE

SHARE

CASH FLOW

BUDGET and CASH-FLOW (by INAF):

SHARK-VIS yesterday: today: Waiting for September 2017 delta FDR to assess: • Science detector selection • Management plan • SW and HW ICDs • Filter list • Science cases Already accepted: Opto-mechanical design Axes and controls Envelope Operation efficiency Timeline Budget

SHARK-VIS where it will be:

separation < 50 mas

SHARK-VIS how does it work:

separation < 50 mas

cal

guide

science

tip/tilt ADC mask f#15 coll.

filter stop f#26 cam.

Split-filters Zoom lens

mirror glass

IFU

fast feedback

slow feedback

active position control

SHARK-VIS filters (#12+): 7 Wb + 2 Mb + 2 split SDI…

RED - NIR 600 - 900

EXP - NIR 700 - 1000

VIS 500 - 600

EXP - BLUE 450 - 400

VIS - NIR 500 - 750

VIS-BLUE 450 - 550

RED - 600 - 700 r 650/30

v 550/30

I - 700 - 800

Hα 2nm + cont (T>90%)

OI 2nm + cont (T>90%)

SHARK-VIS Forerunner Experiment

Target: GLIESE 777

R mag=5.7

NCPA correction

20 min data sequence

1 ms cadence

FLAO correcting 500 modes

Band 610-650 nm

Pedichini+ 2017 Stangalini+ 2016

Short exposure Long exposure

Data quality with seeing 0.8” – 1.5”

Very unstable seeing conditions SR ranging from 0.05 to 0.55 This makes PSF removal difficult

Forerunner on sky results:

separation < 50 mas

o Forerunner PSF core is diffraction limited with 1.2” of unstable seeing

o DIT = 1ms PSF jitter frozen and recovered with post processing

o 630nm with 40nm of bandwidth

o 20 minute total exposure (70° of field rotation)

o Basic ADI processing on 1.2e6 frames (Marois 2005)

o Detection at S/N>6 of fake planets at contrast of 5e-5

o No data selection

o Achieved Detection is 10 times the photon noise

Forerunner 0.8”-1.5”(630nm)

SVS 1.2” (630nm)

SVS 0.6” (500nm)

SVS 0.6” (650nm)

Forerunner 630nmADI, S/N >6

SHARK-VIS Radial Contrast for direct imaging

offset from guide star [mas]

con

tras

t

Del

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agn

itu

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“SOUL updated”

It’s Science Time for SHARK-VIS

Thank you!

• Observe simultaneously in two narrow-band filters: line and adjacent continuum

• Estimate by the continuum image the PSF to subtract at each frame

line

cont

Wollaston prism

filters

• Take images at different field angles (not derotated)

• Estimate by median the PSF to subtract to every the frames

ADI (Marois+ 2005) SDI

SHARK-VIS SDI setup

-

OPTICAL relay performances and tolerances:

0.00E+000 1.40E-004 2.80E-004 4.20E-004 5.60E-004 7.00E-004 8.40E-004 9.80E-004 1.12E-003 1.26E-003 1.40E-003

0

0.01

0.02

0.03

0.04

0.05

0.06

0.07

0.08

0.09

0.1

+Y Field in Degrees

Diffraction Limit

SHARK-VIS_noadc_def.zmxConfiguration 1 of 1

RMS Wavefront Error in Waves

RMS Wavefront Error vs Field

13/02/2017Poly 0.4 0.5 0.6 0.7 0.8 0.9 1

Reference: Centroid

Surface IMA: Detector

65.00

OBJ: 0.0000, 0.0000 (deg)

IMA: 0.000, 0.000 mm

OBJ: 0.0000, -0.0014 (deg)

IMA: -0.000, -5.218 mm

OBJ: 0.0000, 0.0014 (deg)

IMA: 0.000, 5.172 mm

OBJ: 0.0014, 0.0000 (deg)

IMA: 5.188, -0.023 mm

OBJ: -0.0014, 0.0000 (deg)

IMA: -5.188, -0.023 mm

0.4000

0.5000

0.6000

0.7000

0.8000

0.9000

1.0000

SHARK-VIS_noadc_def.zmxConfiguration 1 of 1

Spot Diagram

13/02/2017 Units are µm. Airy Radius: 12.64 µmField : 1 2 3 4 5RMS radius : 0.815 0.702 0.879 0.687 0.690GEO radius : 1.338 1.313 1.641 1.479 1.463Scale bar : 65 Reference : Centroid

Surface IMA: Detector

65.00

OBJ: 0.0000, 0.0000 (deg)

IMA: -0.117, -1.655 mm

OBJ: 0.0000, 0.0010 (deg)

IMA: -0.119, 1.975 mm

OBJ: 0.0000, -0.0010 (deg)

IMA: -0.115, -5.308 mm

OBJ: 0.0000, 0.0014 (deg)

IMA: -0.120, 3.524 mm

OBJ: 0.0000, -0.0014 (deg)

IMA: -0.115, -6.880 mm

OBJ: 0.0010, 0.0000 (deg)

IMA: 3.514, -1.667 mm

OBJ: -0.0010, 0.0000 (deg)

IMA: -3.748, -1.666 mm

OBJ: 0.0014, 0.0000 (deg)

IMA: 5.070, -1.679 mm

OBJ: -0.0014, 0.0000 (deg)

IMA: -5.305, -1.677 mm

0.6000

tolerMC_WORST.ZMXConfiguration 1 of 1

Spot Diagram

13/02/2017 Units are µm. Airy Radius: 18.97 µmField : 1 2 3 4 5 6 7 8 9RMS radius : 2.577 2.507 1.895 2.310 1.603 2.517 2.648 2.761 2.732GEO radius : 4.594 4.048 2.912 3.844 3.024 3.961 4.915 4.673 4.627Scale bar : 65 Reference : Centroid

0.00E+000 1.40E-004 2.80E-004 4.20E-004 5.60E-004 7.00E-004 8.40E-004 9.80E-004 1.12E-003 1.26E-003 1.40E-003

0

0.01

0.02

0.03

0.04

0.05

0.06

0.07

0.08

0.09

0.1

+Y Field in Degrees

Diffraction Limit

tolerMC_WORST.ZMXConfiguration 1 of 1

RMS Wavefront Error in Waves

RMS Wavefront Error vs Field

13/02/2017Poly 0.6

Reference: Centroid

Tries: 1000 Statistic: flat

Radius: ±0.2 mm Shifts: ±0.2 mm

Tilt: ±0.1 degrees

Only camera refocus

To avoid high order aberration λ/100

optical quality required

ABS system

REQUIREMENTS

HARDWARE PI PIEZO S-330

•Mitigates residual PSF jitter (≈ 17mas rms)

•Allows fine subpixel centering of PSF

•Compensates ADC chief ray tilt

•Reduction of Jitter by a factor 6 at least

•0.3 pixel r.m.s.

A.R.M.A.

EXPECTED PERFORMANCE

SHARK-VIS detector: sCMOS+ or EMCCD

READOUT

format

Frame

rate

[kHz]

DIT

[ms]

Data rate

[MB/s-TB/h]

2k x 2k 0.04 25 360 1.30

512 x 512 0.4 2.5 210 0.75

200 x 200 1 1 80 0.29

+RON +CALIBRATION +Q.E. -SHUTTER -DYNAMIC -FOV -BLOOMING

+EFFICIENT +DYNAMIC +FOV -CALIBRATION

ADC performances ADC BANDWIDTH vs WAVE