h2020 opticon (730890) · h2020 opticon (730890) jörg-uwe pott max-planck-institut for astronomy,...

H2020 OPTICON (730890)

Jörg-Uwe Pott Max-Planck-Institut for Astronomy, Heidelberg, GER

Mid-term Review Brussels 17th October 2018

Theme Interferometry # WP’s 08, 11

Overview: 5min each on 5 topics

• Network NA.2 • WP11.1: European interferometry initiative networking –

introduction of the network, lead by bureau and science council • WP11.2..5: VLTI-training: summer schools, Fizeau program, VLTI

expertise centers – lead Univ. Porto, POR, all • JRA.Hardware: explore the next generation

instrumentation for the VLT interferometer • WP8.1: P-Rex: predictive piston control based on adaptive

optics real-time data – lead MPIA, GER • WP8.2: Hi-5: a high-contrast integrated optics imager, lead by

Univ. Liege, B • WP8.3: iVis: concept delevopment for enabling visible

interferometry with the VLTI – lead Univ./Obs. Nice, FR

NA2: VLTI Expertise Centres Network OPTICON WP11

Paulo J.V. Garcia – Porto University

OPTICON Mid Term Review, 17th Oct 2018

Background on optical interferometry

• Combines the light from telescopes separated by a baseline B, obtaining information with an angular resolution λ/B.

• Typically a factor of 15 above current 8m class telescopes equipped with AO and still an unique parameter space in the ELT era.

• Comparatively short wavelength (x10-3) with respect to radio/sub-millimetre translates in significant technical challenges and youth of the technique (first common user facility was the VLTI circa 2001).

Monnier et al. Kraus et al. Kloppenborg et al. Benisty et al.

Goal for the WP11: Establish a network of VLTI expertise centres | Motivation

• Scientific growth with PIONIER 1.5 gen instrument • 4 interferometry related ERC grants in the last 3 years • VLTI infrastructure refurbishing stable system

• 2nd gen instrument GRAVITY behaving with outstanding stability and sensitivity (beating specs) workhorse K-band interferometric spectrograph

• 2nd gen instrument MATISSE successful sky commissioning on-going

• Builds on and expands successful OPTICON Fizeau programme, VLTI schools, VLTI Community Days, JMMC example and in coordination with ESO.

• Builds on the community-building work by the European Interferometry Initiative (http://www.european-interferometry.eu) involving 15 countries, ESO and ESO.

http://www.european-interferometry.eu/


Objectives a) Coordinate the creation of an European-wide network of VLTI

Expertise Centres; b) Organize schools that will train the VLTI users; c) Support observing proposal preparation and data reduction; d) Co-organize with ESO the VLTI community days and the

European Interferometry Initiative meetings; e) Focus the highly successful Fizeau staff exchange grant

scheme towards young researchers and VLTI outreach in communities without much optical-infrared interferometry know-how;

f) Exchange experience and coordinate with the radio-mm interferometry community;

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Sub-work packages

• WP11.1. Coordination • Day-to-day network activities including reporting. • Monthly teleconferences of EII Bureau.

• WP11.2 VLTI Expertise Centres Network • Backbone of dissemination activities to new VLTI users. • Network includes the three partners from this networking activity

(JMMC/France, Porto/Portugal, Exeter/UK), as well as the three interferometry JRA (WP8) lead partners (Nice/France, Liège/Belgium, Heidelberg/Germany).

• WP11.3 Fizeau Programme Staff Exchange

• WP11.4 VLTI Schools

• WP11.5 VLTI Community days and European Interferometric Initiative meetings

• Transparent real-time reporting at http://www.european-interferometry.eu

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Deliverables

• D.11.1 VLTI School in Porto report [M12] • This deliverable was moved to M19 (ie summer 2018; cf.

report and justification)

• D.11.2 VLTI Expertise Centres Network Website Report [M12]

• Successfully delivered. • Individuals responsible for support identified and active. • Supported by ESO Users Committee Poll 2018.

• D.11.3 VLTI School in Nice report [M36] • Planning started

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Fizeau Programme

• Selection committee members from non-funded (WP8/11) OPTICON countries

• Josef Hron (AU, Chair), Péter Ábrahám (HU, deputy), Jose C. Guirado (ES), Alessandro Marconi (IT), Sofia Ramstedt (SE).

• Calls issued: 2017A, 2017B, 2018A and 2018A-VLTI School.

• Total funding for 27 exchanges was awarded. • Details @ http://www.european-

interferometry.eu/fizeau-program/funding-results

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http://www.european-interferometry.eu/fizeau-program/funding-results

http://www.european-interferometry.eu/fizeau-program/funding-results

VLTI Community days

• March, 2017, 56 participants.

• The days presented a) current status of the VLTI; b) presentation of prospective for the infrastructure by ESO and the community; c) discussion on ideas and science cases for future instruments

• Face-to-face meeting of the Science Council European Interferometric Initiative

a) a report and discussion on the OPTICON-FP7 activities; b) the foreseen activities for H2020; c) perspective activities for the VLTI infrastructure and others; d) internal EII organization aspects.

• Following the meeting an electronic procedure for the election of the EII bureau took place. The transition took place in August 2017.

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VLTI School in Portugal, 2018

• Lisbon, 9th to the 14th of July. • The school had 37 students, 28 of

which were MSc or PhD students, 38% female.

• The students originated from 15 different countries

• Brasil, Bulgaria, China, Denmark, France, Germany, Greece, Hungary, Ireland, Italy, Latvia, Norway, Poland, The Netherlands, United Kingdom and ESO.

• Full funding (flight, lodging, subsistence) awarded to most students, including Fizeau Programme complement.

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WP8.1: P-REx: The AO fed Piston Reconstruction Experiment

Jörg-Uwe Pott, Saavi Perera (MPIA) Felix Widmann (MPIA, MPE)

Martin Glück (Univ. Stuttgart)

P-REx - The Idea

- Reconstruct the piston drift over a single

telescope in real-time using the AO-WFS data - Differential Piston = Tip/Tilt * wind speed

- Use differential piston drift several telescopes

to stabilize interferometric fringe position

(coherence time)

- Ease requirements on an existing fringe tracker - Increasing number of science targets / sky coverage

- No additional hardware needed SPIE: Astronomical Telescopes + Instrumentation - 13.06.2018 - Felix Widmann

The Concept

ΔP = [tip · vx + tilt ᐧ vy] · t

Differential Piston

= Tip/Tilt * wind speed

Directly from the AO system Cross correlation of 2D-POL WFS data

Other approaches: Atmospheric modeling (Sivo 2018)

SPIE: Astronomical Telescopes + Instrumentation - 13.06.2018 - Felix Widmann

The Assumptions to test during WP8

- Tip/Tilt are dominant modes of the atmospheric

turbulence

- Main turbulence in one main layer (ground layer)

- Layer driven by wind speed (Taylors Frozen Flow

Hypothesis)

- Temporal decorrelation (boiling) timescale

?

?

✔

✔


P-REx Simulations results


P-REx Simulation results

MIR

NIR

optical

What requirements have to be fulfilled?


First Conclusions

- 8m telescopes with a good WFS sampling are needed - Synergies with next generation IF instrumentation requiring

higher Strehls for improved coupling efficiency

- Multilayer turbulence: - Strong ground layer needed (~ 50%)

- Majority of layers should move within 40 degrees

- Alternative route: a simpler GLAO system


On-Sky data - LBT FLAO

Wind measurement:



3.5 m



RMSE below 2 μm for 2/3 of the test cases


Combination with other systems:

- Internal OPD: Metrology system (e.g. GRAVITY: Lippa 2016)

- Vibrations: Accelerometer based control (Böhm 2017)

Other interesting applications possible

- ELTs: Piston control for large individual mirrors

-

Further thoughts for a VLTI implementation


WP8.1: Opticon mid-term status

- P-REx algorithm developed, showing promising results from simulations and first on-sky tests

- Published in Widmann et al. 2018MNRAS.475.1224 and SPIE

- Next test level for 2019: LBTI, and VLTI/Gravity

- Other interesting applications possible in the ELT phasing context

- Central deliverable (on-sky performance tests, and implementaion plan) is on track

- Use of Opticon-resources

- FTE hired, and working (Saavi Perera), complemented by MPIA personell

- Powerful server funded for computation intensive tasks SPIE: Astronomical Telescopes + Instrumentation - 13.06.2018 - Felix Widmann

LBT-I VLT-I

P-REx on large interferometers

https://ui.adsabs.harvard.edu/abs/2018MNRAS.475.1224W/abstract

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Hi-5

WP8.2: Hi-5 project

• L/M-band high-contrast interferometry on the VLTI (Defrère et al. 2018)

• Leverage the angular resolution of the VLTI and nulling interferometry

• Leverage new developments in L/M-band integrated optics

VLTI (Cerro Paranal, Chile) 24

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Hi-5

High-contrast interferometry status: landscape Defrère et al. 2018

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Hi-5

Science case 1: exozodiacal disks

• Thermal near-IR = missing link in current exozodiacal disk models (interactions between hot dust and asteroid belts)

• Measuring the faint end of the exozodi luminosity function

(complementary with LBTI in northern hemisphere)

Kral et al. 2018

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Hi-5

Science case 2: exoplanets

• L/M-band = sweet spot for direct exoplanet imaging o Favorable star/planet contrast o Access to planet radius and temperature o Molecular bands / nonequilibrium chemistry

Skemer et al. 2014

(Jupiter)

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Hi-5

Science case 3: planet formation • Imaging young stars in nearby star forming regions

o Search for young, forming planets (e.g., explore the cavities of transitions disks)

o Need good imaging capabilities in addition to high contrast o Prepare for PFI science

Wallace (in prep)

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Hi-5

Project timeline

• Oct. 2017: kickoff meeting

• Nov. 2017: hiring of PhD student (T. Boulet) • June 2018: project update presented at SPIE (Austin, US)

• July 2018: project science case presented at COSPAR (Pasadena, US)

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Hi-5

Hi-5 kickoff meeting

• Hi-5 kickoff meeting held in Liège in October 2017;

• Meeting website with presentations: http://www.biosignatures.ulg.ac.be/hi-5/index.html

• Meeting summary and outcome published in peer-reviewed journal (Defrère et al. 2018)

http://www.biosignatures.ulg.ac.be/hi-5/index.html

http://www.biosignatures.ulg.ac.be/hi-5/index.html

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Hi-5

Current project outcomes

1. Peer-reviewed paper on the project published in Experimental Astronomy (Defrère et al. 2018a)

2. Project update published in the SPIE proceedings (Defrère et al. 2018b)

3. PhD student developed a software to compute the exoplanet yield of Hi-5 https://github.com/AmiralVespasien3/Exoplanets_Interferometer_Simulator

Related content • Kernel nulling (Martinache and Ireland, 2018, accepted for publication in A&A,

https://arxiv.org/abs/1802.06252)

https://github.com/AmiralVespasien3/Exoplanets_Interferometer_Simulator

https://arxiv.org/abs/1802.06252



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Hi-5

Project status

• OPTICON funding status: • Full time PhD student (one year, used ~35kEUR); • Achievements: exoplanet science case definition (mainly target list) and

corresponding high-level technical constraints (i.e. need for the longest VLTI baselines);

• External resources allocated to the project • Local PI (Denis Defrère): 10% of his time in 2016-2018; • Grant from University of Liège to organize kickoff meeting (~5k); • Achievements: organization of kickoff meeting, publications and

presentation of project, networking activities, supervision of PhD student.

• Future plan • PhD student will leave in November 2018 (for personal reasons) • Hiring of postdoc under progress

• If good candidate is found, OPTICON funding will be divided between the postdoc (full time, 75% of remaining funding) and the local PI (part time, 25% of remaining funding).

• If no good candidate, local PI will dedicate 100% of his time to the project (February 2019 to February 2020)

WP8.3: iVis bringing interferometry in the visible to

the VLTI: why and how

SPICA 33

HRA & PLATO R. Ligi, N. Nardetto, A. Crida, D. Mourard

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Direct measurement of the angular diameter + Gaia parallaxe Bias on the diameter: limb-darkening, rotation, pulsation, environment, spots..... characterization of the surface and of the environment. To do that we need for precise estimation of diameters of reference star • Surface brightness color relations

should be improved • SED fitting is also important but

stellar models are not at the required precision

relations not arrurate (7%) and incoherent (8%)

relations accurate (1-2%) but incoherent (6%)

2% of precision

Surface Brightness Color Relations

Important for early type eclipsing binaries (M31/M33)

Important for late type eclipsing binaries (LMC/SMC)

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SPICA 36

WP8.3 first term: Develop SPICA as test program

SPICA: Stellar Parameters and Images with a Cophased Array a testbed for modern visible interferometry at CHARA Performing a survey of stellar parameters for ~1000 stars (>0.2mas, R<8) with homogeneous measurements and in parallel precise infrared photometry. Identification of departure to the simple LD model and further analysis (rotation, circumstellar environment…) For a subsample of bright and larger stars (>0.7mas, R<5), surface imaging for limb darkening. Seems feasible in 3 years, 70n/year with optimized observing strategy

Optical design of SPICA

SPICA

Dimension=(3’x5’)

The two main difficulties are: - Injection in SM fibres in partial AO correction - Phase tracker for long exposure capabilities

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SPICA

Uncorrected

Visib

le

H Ba

nd

TelAO ON

Qualitative behaviour under partial correction by AO Based on the code by M. Ireland, ANU ~r0=10cm, t0=6ms

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Fibre coupling efficiency in the lab

SPICA 39

OPTICON Support + Collaboration ONERA

R=140 R=3000 V²=0.25 8.7 5.4 V²=0.01 5.5 2.3

Table 1: Limiting magnitude with a group delay tracking

R=140 R=3000 V²=0.25, DIT=0.2s

10.1 6.7

V²=0.01, DIT=0.2s

6.7 3.5

V²=0.25, DIT=30s

10.4 7.1

V²=0.01, DIT=30s

7.0 4.0

Limiting magnitude defined as S/N=10 per spectral channel in 10mn of integration

These estimations use a sky-validated S/N calculator SPICA

SNR consideration … long exposures Fringe Tracker

Table 2: Limiting magnitude with a phase delay tracking

Degraded transfer function

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Development of intergrated optics component for 6T-ABCD fringe sensor

SPICA

The specifications are the following: • Operation wavelength range: 1.5-1.8 μm (i.e., H

astronomical band) • Single-mode waveguides over the H band • Operation with both linear polarizations

simultaneously • Number of telescopes to be combined: 6 • Number of baselines to be coded: 15 • Type of fringe coding: ABCD coding • Phase shift between 4 ABCD outputs: 90° +/-

10° over the whole spectral band. • Throughput: larger than 60% over the H

band (goal: 65%) • Contrast level: larger than 95% in polarized

light • Flux balancing: all the outputs corresponding to

one input waveguide should have the same flux over the H band. Tolerance: +/- 15%

• Flux cross-talk: below 0.5% (an input beam that is not supposed to contribute to a fringe pattern contribute to less than 0.5% of the flux)

Pre-study made by VLC photonics • Technology is mature (2 or 3

different platforms) • T between 35% and 50% (+?) • Cost: 13k€ + 30k€ - 3-4m delay

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Estimation of performance for a H-band CHARA FT

VLTI-GRAVITY FT performance

H band FT, 5 SpCh, 6T ABCD, Selex detector. T0=10ms , Texp=5..10min

SPICA 43

SPICA

WP8.3: working towards the deliverable

• Design phase of the IO component (Summer 2018) + construction (this fall)

• Design of the MIRCx interface • Photometric characterization at IPAG

(winter 2018) • Development of the control system, phase

sensor, state machine in 2019 (based on the Gravity software)

• Integration fall 2019 at CHARA

• 2-year postdoc funded by OPTICON (Fabien Patru, this fall)

• Support from Lagrange Lab in Nice for opto-mechanical interface to MIRCx

• Funding from CNRS, UCA and OPTICON

• CESAR to CHARA in June & Octobre 2018. Final validation of the optical design (including or not TT mirror, sensor for TT)

• Funding application (ANR) in Nov. 2018 • Start of the detailed design by the Nice

technical group (after the final delivery of MATISSE): end of 2018.

• Construction in Nice from Summer 2019 to Summer 2020. Tests in Nice winter 2020

• Integration at Mount Wilson around Summer 2021

Fringe Tracker SPICA

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In parallel, we have published a recent paper in Exp. Astronomy developing the science case of visible Interferometry at the VLTI and discussing the main issues and how to overcome them. Millour, 2018+

WP8.3: Project status at mid-term review OPTICON funding status • Start of post-doc (Fabien Patru) in Jan 2019 for 1+1yr until

the end of the program. • Achievements: preliminary optical design of SPICA done,

refereed paper resubmitted to experimental astronomy describing the iVis concept (Millour+ 2018). Based on complementary funding

External ressources allocated to the project • PI and PM of SPICA (D. Mourard and P. Berio) also involved

in iVis. • Funding to buy the camera and produce the fringe tracker

of SPICA obtained locally (IDEX JEDI UCA). Future plan for the second half of the project • Make F. Patru work out the detailed concept for iVis on

the VLTI, which is the deliverable, and will be based on the SPICA testbed presented here

h2020 opticon (730890) · h2020 opticon (730890) jörg-uwe pott max-planck-institut for astronomy,...

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