SHARK-NIR@LBT SYSTEM FOR CORONAGRAPHY WITH HIGH … · HW 380 570 60 --- 1010 Prototypes 20 20...

The SHARK-NIR Team: J.Farinato1, F.Pedichini2, E.Pinna3, C.Baffa3,

A.Baruffolo1, M.Bergomi1, L.Carbonaro3, A.Carlotti4, M.Centrone2,

L.Close5, J.Codona5, M.Dima1, S.Esposito3, D.Fantinel1, G.Farisato1,

W.Gaessler6, E.Giallongo2, D.Greggio1, J.C.Guerra5, O.Guyon5,

P.Hinz5, F.Lisi3, D.Magrin1, L.Marafatto1,7, A.Puglisi3,

R.Ragazzoni1, B.Salasnich1, C.Verinaud4, V.Viotto1

SHARK-NIR@LBT

SYSTEM FOR CORONAGRAPHY WITH HIGH

ORDER ADAPTIVE OPTICS FROM R TO K BAND

THE NIR CHANNEL

1) INAF PADOVA 2) INAF ROMA 3) INAF-ARCETRI 4) IPAG

5) STEWARD OBSERVATORY – ARIZONA (USA) 6) MPIA 7) UNIVERSITY OF PADOVA

Jacopo Farinato

11/11/2014 3:06 PM SHARK-NIR@LBT - Pianeti Extrasolari - Roma 1

2 11/11/2014 3:06 PM SHARK-NIR@LBT - Pianeti Extrasolari - Roma

Extreme AO correction in the NIR region with SR > 95% best PSF subtraction with or without coronagraph increasing target S/N.

Very good SR > 40% in the optical R-I bands new window for high angular resolution (~17 mas) at a single telescope, comparable to what achievable at LBT by NIR interferometry.

Contrast < 10-4

H band w/o coronograph

Why SHARK

SHARK is the VIS & NIR coronographic imager that will make use of the LBT excellent AO performances!


Direct imaging of close giant planets investigating the main evolutionary stages:

Young planets, from early phases of growth (the first few million years) when these are hot, surrounded by disks, and can be revealed thermally at T> 300 K in NIR and in Halpha (VIS channel)

Old giant planets, very close (< 5-10 pc ) and bright, whose reflected light could be detected for separations of the order of 100-200 mas in the visible, where greater is their emission, and also in the NIR if very cloudy.

Disks around Young Stars and their Jets

High-contrast images of circumstellar disks with optical/near-IR coronagraphy and polarimetric differential imaging

Coronagraphic imaging of stellar jets

2D maps of Jets

AGNs and QSOs

SHARK CORO science


What is SHARK?

• Initial idea:

• Essentially a Coronagraphic camera, working from R to K bands (designed

for high contrast imaging)

• The basic idea is to make it simple as possible (compact, light, close to the

WFS) and cheap

• The baseline coronagraphic technique is classical Lyot

• Several designs initially considered (in the SHARK proposal submitted for

the call for ideas for 2nd generation LBT instrumentation - October 2012)


Even if it is a 2nd generation instrument, it can coexist with the 1st generation, with an impact as soft as possible (simplicity, small dimension, only partially overlapping wavelength range).

In fact, SHARK basic features are:

NIR Coro-Camera (J,H,K)

VIS Coro-Camera (R,I)

VIS Spectrograph

Call for LBT instruments (Feb 2014)

LMIRCam L; M

Pyramid

WFS

Pyramid

WFS

SHARK

NIR J; H; K

SHARK

VIS R; I

Vis

IFU

R; I

SHARK-VIS

PI Fernando Pedichini

SHARK-NIR

PI Jacopo Farinato


SHARK location: at the entrance of LBTI (preliminary agreement with Phil Hinz)

SHARK-VIS SHARK-NIR

Talk of Fernando Pedichini


The NIR Channel

The Chriostat

Bearing


SHARK NIR Optical Design


SHARK NIR Optical design performance


SHARK NIR characteristics summary SHARK NIR main characteristics

Large FoV design

Observing Modes Imaging/Coronagraphy

Detector format [px] 2048x2048

FoV x ["] 30.67

FoV y ["] 30.67

FoV along the diagonal ["] 43.37

scale ["/px] 0.015

Airy Radius @ 1 micron [px] 2

Airy Radius @ 1.25 micron [px] 2.501

Number of mirrors in the camera 5 (3 flat and 2 off-axis parabolas)

Cold Stop Yes, in the intermediate pupil plane

ADC Yes, deployable

Max circular FoV diameter 30.67"

Max FoV along the diagonal 43.37"

Strehl at 10" FoV diameter

(in all Bands) >99%

Strehl at 30" FoV diameter

(J Band) >95%

Strehl within whole FoV (43.37" in diagonal) (J Band) >81%

Optical bench dimension along the input optical axis [mm] ~220

Optical bench dimension in the direction perpendicular to the

input optical axis [mm] ~350

Max diameter off-axis parabolas [mm] 52

Max diameter folding mirrors [mm] 55


Coronagraphy

• There is a baseline design for the coronagraph (Classical

Lyot), but we do have a flexible design with filter wheels

on both the focal and the pupil planes, where different

techniques might be implemented

Lyot technique


The SHARK-NIR Team INAF Padova (Project Responsible, NIR Channel Opto-Mechanics and IC Software)

INAF-Arcetri (AO Interaction and CRYO and NIR detector support)

Steward Observatory (LBTI interfaces, NIR detector, alternative CORO design)

MPIA for SW design (Wolfgang Gaessler) (and motors electronics? TBD)

IPAG (alternative CORO design)

ESO (alternative CORO design)

INAF-Rome (Coordination with VIS Channel)

Science team (INAF Padova, INAF Roma, INAF Arcetri, INAF Catania, IPAG, Steward Observatory , MPIA, University of Padova, University of Catania, INAFTorino, INAF Palermo, Aix Marseille Université (LAM), ESO)

Instrument Scientist soon in the SHARK-NIR Team

A Board of supervisor (both from Science group and from Instrument experts) to ensure that the sinergy between the two channels is preserved

Well identified and shared responsibilities, with reasonable required manpower

A total of ~18 FTEs (including science) for the project completion


SHARK-NIR Schedule Milestones

On request of LBT Board, SHARK-NIR is a fast track project with a very aggressive (success oriented!) schedule (which supposes a certain cash flow), the main milestones of which are:

Estimated T0 in January 2015

Conceptual Design Review in T0 + 5m (May 2015)

Final Design Review in T0 + 14m (February 2016)

NIR Camera for Direct Imaging on SKY in about 2.5-3 years from T0 (Fall 2017)

NIR CORO mode on Sky in about 3.5 years from T0 (Mid 2018)


SHARK-NIR Cost Estimate

ITEM Cost (K€)

Hardware (NO VAT) 1060

Travels 200

Contracts 320

TOTAL 1580

TOTAL + CONT. (10%) 1740

NIR Channel

CASH FLOW (K€) 1st year 2nd year 3rd year 4th year Total

Travels 30 40 50 80 200

Contracts 122 66 66 66 320

Design studies 30 --- --- --- 30

HW 380 570 60 --- 1010

Prototypes 20 20

TOTAL 582 676 176 146 1580

Cash Flow fundamental to accomplish the aggressive schedule


Statement on Open Use

We intend SHARK to be a facility instrument, and

thus to offer it to the whole LBTO community,

beyond the partners involved in our proposal.


Conclusions We do have an outstanding main science case, plus several others very interesting

cases which require binocularity and coronagraphy (we did not touch the NON-Coro and the single eye science)




We will make use of the XAO LBT capability (with SOUL even better!)

LBT (PWFS, on sky data, good seeing 0.6”)

LBT (PWFS-L3CCD, simulation, good seeing

Palomar (SH, on sky data, average seeing 0.6”-1.0”)

VLT-Sphere (SH, Lab test, average seeing, 0.85”)

Sphere

(lab SH)




We will make use of the XAO LBT capability

The NIR Arm is unique in the LBT scenario in its CORO fashion






International scenario favourable: North Sky 2 competitors, Palm3000 and SCExAO, and with the latter we can work in sinergy







SHARK-NIR is very simple, small and close to the WFS (NCP and flexure minimization)








SHARK-NIR is a 2nd generation instrument which can coexist with the 1st generation








SHARK-NIR is a 2nd generation instrument which can coexist with the 1st generation

SHARK-NIR is “cheap” and potentially “fast” (depending on the cash flow)







SHARK is very simple, small and close to the WFS (NCP and flexure minimization)

SHARK is a 2nd generation instrument which can coexist with the 1st generation

SHARK is “cheap” and potentially “fast” (depending on the cash flow)

October 20 2014, the Board endorsed SHARK NIR for the conceptual study phase (CDR in May 2015)

SHARK-NIR@LBT SYSTEM FOR CORONAGRAPHY WITH HIGH … · HW 380 570 60 --- 1010 Prototypes 20 20...

Documents

Transcript of SHARK-NIR@LBT SYSTEM FOR CORONAGRAPHY WITH HIGH … · HW 380 570 60 --- 1010 Prototypes 20 20...