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Optical-Infrared Instrumentation
NWO-FAPESP meeting
16 March 2015
Wilfried Boland
NOVA Executive Director
NOVA program
Netherlands Research School for Astronomy
– Federation of university institutes
Amsterdam, Groningen, Leiden, Nijmegen
– 350 fte scientific staff: ~55 fte faculty staff/tenure-track, ~70 fte
postdocs, ~150 fte AIOs, ~45 fte instrumentalists; NOVA funds ~20%
Research and instrumentation are interlinked
parts of the NOVA program
– Many discoveries are the result for new observing
capabilities; NOVA wants to be an active player at
the forefront in key areas
Overview Top astronomy = top talent + top instrumentation
– Opening new wavelength ranges
– Larger collecting area
– Enhanced instrument capabilities
– Upcoming non-electromagnetic ‘messengers’
NOVA program enabled university astronomers
in the Netherlands to
– become leaders in Op-IR and sub-mm instruments and be
among the first users of these instruments
– make an early start with LOFAR key programs
– do early technical R&D and feasibility studies to assure
that project plans are realistic
Coherent national program
National strategic plan sets priorities
– Long-range planning: 10-20 years
Access to observing capabilities is
secured via
– Space: ESA, SRON
– Radio domain: ASTRON
– Op-IR + sub-mm: ESO, NOVA; NWO
Funding for large programs (> 10 M€) now depends on successful proposal
to national Roadmap program
NOVA strategy on Instrumentation
Provide science instruments for world leading telescopes
Focus is on ESO (E-ELT, VLT, ALMA)
Contribute to those instruments that are essential for innovation of research themes in research networks
Be among first users of the instrument
Train young instrument scientists, systems engineers, and designers
NOVA astronomers must “invest” in instrumentation projects as Principal Investigator or Instrument Scientist– Translate research questions into technical requirements
– Fund raising; leading (NL part) project team; participation in international consortium
Contributions to largest facilities
Our instrumentation teams
Op-IR Group NOVA-ALMA team
Instrumentation overview 1999-2013
2000 2005 2010 2014
ALMA Band-9
ALMA Band-5
PUMA-2
VLTI-MIDI
VLT-SINFONI
VST-OmegaCAM
Lab Astrophysics
JWST-MIRI
X-Shooter
MUSE
Sphere-Zimpol
LOFAR-DCLA
AMUSE
Gaia-DPAC
VLTI-MATISSE
E-ELT
Origin funding instrumentation
2009-2013; total = 24.5 M€
PROJECT MONITORING
Twice per year by Instrument Steering Committee
– Written progress report in advance of meeting
– Oral presentation by PI’s of projects that have issues to
report
– ISC reports their findings to NOVA Board and Directorate
– Board takes final decisions
Extra mini-review if there are serious issues
Project contingency is held at Board level
Standard PDR, FDR and MRR practice of ESO/ESA
Informal coaching by NOVA Executive Director
Op-IR instrumentation group Core Competences
Opto-mechanical cryogenic systems engineering
Spectroscopy – Polarimetry – Interferometry
Cryogenic Precision Optics & Mechanisms
Improvement loop: Design – Manufacture – Test
JWST-MIRI Sphere-ZIMPOL MATISSE
Op-IR group – Track record For ESO VLT-VLTI
– 2003 MIDI – two-beam combiner for interferometer
– 2004 VISIR – mid-IR high resolution spectrometer
– 2004 SPIFFI – near IR camera
– 2009 X-Shooter – near-IR spectroscopic arm
– 2014 Sphere-Zimpol – polarimetric module
– 2016 MATISSE – LM + N band four beam combiner
For ESO – E-ELT
– 2009-2010: participation in Phase-A studies for four
instruments
For JWST
– 2009 MIRI – cold optical bench for mid-IR spectrometer
IRAS 16293-2422:CO J=6–5 traces the outflow
driven by source A1+A2 of this proto-triple,
which partially covers source B • confirmation of
glycoaldehyde near source A • warm H218O in
emission toward source A1, in absorption to B.
ALMA Band-9 first NL results
Oph IRS48: transitional protoplanetary disk
with mm-sized grains trapped in a pressure
maximum by companion; warm H2CO at same
location; warm CO points at a low gas mass.
H2CO
CO 6–5
H218O
glycoaldehyde
Jørgensen et al. 2012;
Kristensen et al. 2013;
Persson et al. 2013
van der Marel et al. 2013, 2014;
Bruderer et al. 2014
contours: mm dust
Publications
ALMA: 98 publ; 30% NL
Band-9: 11 publ; 55% NL
Multi Unit Spectroscopic Explorer• Integral field spectrometer for the VLT:
• (Instantaneous) band width: 480-930 nm
• 1’x1’ FoV, 0.2’’ pixels
• Resolving power 1770 – 3590 (blue-red)
• First light and commissioning Feb 2014
• Performance equals or exceeds specs
• Narrow-field mode and AO still to come
What is in it for NOVA?
1. ASSIST – technology to test deformable mirrors
2. NOVA in charge of data management invaluable
experience in handling and serving complex 3D data
255 nights of GTO for joint consortium program
1st year NOVA science focal points:
Deep fields with multi-wavelength coverage (incl. UDF):
detect gas around galaxies in emission, resolved galaxy
properties, census of line emitters, redshift survey Deep
fields centered on bright QSOs: find galaxies corresponding to absorbers gas flows around galaxies, detect
VLT/X-shooter (2009)The most powerful spectrograph in the world
300 – 2500 nm in one shot
R ~ 10,000
Consortium: DK, F, I, NL, ESO
L. Kaper (NL-PI), R. Navarro, P. Groot
• Since commissioning, most demanded (with FORS2) VLT instrument
• So far, 178 refereed publications, of which 33 with NL involvement (17 1st author)
• NL: near-infrared spectrograph arm (NOVA-OptIR), data-reduction software
• NL funding (3.6 M€): NOVA, NWO, UvA, RU, ASTRON 43 GTO nights
• Expertise used in new projects: WHT/WEAVE, E-ELT/MOSAIC, BlackGEM, …
LOFAR DCLA Four key-science projects
– Epoch reionization
– Surveys
– Transients
– Cosmic rays
2.1 M€ NOVA start-up funding +
~ 3 M€ NWO+NSS
! Mpc shock in a z=0.2 galaxy
cluster; thermal noise limited
map at 150 MHz
Transients pipeline 1.0:
discovery of 11 min transient of
unknown origin
Instrumentation program2014-2018
Focus on E-ELT instrumentation
– PI role in mid-IR imager/spectrometer METIS
– Partner role in 1st light instrument MICADO
– Feasibility study on MOS instrument MOSAIC
– Technology studies for EPICS, characterization exoplanets
One of three key players in WEAVE, multi-object
spectrometer for 4.2m WHT on La Palma; NOVA+NWO-EW
– Gaia spectroscopic follow-up
ALMA Band-5 (170-211 GHz) receiver: final design
and series production together with GARD (Sweden)
2014-2018 instrumentation, continuation
Hunter for optical afterglows of gravitational wave
events: BlackGEM
Technology development for Cerenkov Telescope
Array (CTA)
Participation in space missions
– Calibration tools for spectrometer in mid-IR instrument
(MIRI) on JWST; also integration/testing support
– Visualization of Gaia data; science support
– Participation in EUCLID Ground Support
ARTS, new transient capability on WSRT
Laboratory astrophysics
E-ELT Instrumentation
European Extremely Large
Telescope (E-ELT)
– 39 meter diameter - Optical-IR
– Construction approved in Dec 2014
– First light ~2025
NOVA is PI for 3rd instrument,
imager-spectrometer – METIS
– mid-infrared wavelengths
– on telescope in 2027
Technology
development for
METIS in
collaboration with
industry
Project structure
NL work packages are led by NL-PI based at a
university institute
NL-PI is Co-I in international consortium consisting of
4-6 partners (from different countries)
Most of instrumentation work is done at NOVA Op-IR
group; science related work and technical R&D at
universities
Participation of industry where possible
Progress is reviewed by NOVA Instrument Steering
Committee twice per year
ALMA related projects
ALMA receiver cartridges
– Band-9: 602-720 GHz
– Band-5: 161-211 GHz
Motivation: assure that ALMA will be equipped with
best receivers; in particular high-frequency receivers
from start
– Dedicated NOVA ALMA instrumentation at RUG in SRON
Groningen laboratory
– Use of SRON heritage developed for HIFI
– Band-9 work could not be done by industry for this price
(17.5 M€ ESO funding for design, prototyping and
production of 72 receiver cartridges + spares)
In red: dust in SN 1987A
BlackGEMOptical array for gravitational wave counterparts
Aim To detect and characterize the population of GW counterparts
Timeline 2016, 5-year project
Phase 1 4 telescopes (3 M€); Phase 2; 15 telescopes (10 M€)
Per telescope 2.7 square degrees, 0.56 ”/pix, 65cm aperture
Location ESO La Silla
GPO/
Marly
-NL
1. Establish NL role in CTA
2. Optimize CTA for NL science interest
E.g. galactic cosmic rays:
• H.E.S.S. image of supernova remnant (SNR) RX J1713
• SNRs sources of PeV particles in Milky Way?
Instrumentation: co-develop camera for 10 – 300 TeV sub-array of CTA
CHEC – collaboration of Australia, Japan,
Netherlands, UK, US to build a camera for
the small-size telescopes of CTA
Contribution:
• Precision time synchronization of all
individual telescopes (< 1ns
telescope to telescope
• Backend camera electronics
Goals of the NOVA CTA project
Other projects WEAVE – Multi-Object Spectrometer for WHT on La Palma
– ~ 15 M€ project; 4 M€ NL contribution of which 0.5 M€ NOVA
– PI Scott Trager
Long-term archiving + data-mining– 1-2 M€ NL investment of which 322 k€ from NOVA
– PI’s Gijs Verdoes Kleijn and Edwin Valentijn
– Science harvesting on OmegaCAM and MUSE GTO observations
ARTS: application on WSRT-Apertif– 2.8 M€ total, 670 k€ NOVA contribution
– PI: Yoeri van Leeuwen
– Radio transients, their likely origin: supernovae, neutron stars, black
holes; astrophysics under extreme density and/or gravity conditions
Laboratory Astrophysics PI: Harold Linnartz; NOVA 250 k€
polarimetric instrumentation development for direct exoplanet characterization
WHT/ExPo
spin-off: polarimetric instrumentation development for atmospheric aerosol measurements
VLT/SPHERE-ZIMPOL E-ELT/EPICS-EPOL
circumstellar disks exo-Jupiters rocky exoplanets
Summary Instrumentation and research are interlinked parts of
the our program
NOVA provides key (parts for) science instruments for
facilities provided by ESO, ALMA, LOFAR, ESA, ….
– In return NL astronomers get innovative data among the first
users --> exciting new science
– Instruments are delivered on time, on budget and within
specifications
We look forward to a flourishing NWO-FAPESP
collaboration in astronomy
– Technology development and instrumentation for ESO
telescopes and ALMA
– Providing an ALMA-type receiver for LLAMA