Optical-Infrared Instrumentation

Transcription

1 Optical-Infrared Instrumentation NWO-FAPESP meeting 16 March 2015 Wilfried Boland NOVA Executive Director

2 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

3 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

4 Coherent national program National strategic plan sets priorities Long-range planning: 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

5 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

6 Contributions to largest facilities

7 Our instrumentation teams Op-IR Group NOVA-ALMA team

8 Instrumentation overview 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

9 Origin funding instrumentation ; total = 24.5 M

10 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

11 Op-IR instrumentation group Core Competences Opto-mechanical cryogenic systems engineering Spectroscopy Polarimetry Interferometry JWST-MIRI Sphere-ZIMPOL MATISSE Cryogenic Precision Optics & Mechanisms Improvement loop: Design Manufacture Test

12 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 : participation in Phase-A studies for four instruments For JWST 2009 MIRI cold optical bench for mid-ir spectrometer

13 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. IRAS :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 H2 18 O in emission toward source A1, in absorption to B. glycoaldehyde H2 18 O CO 6 5 H2CO contours: mm dust van der Marel et al. 2013, 2014; Bruderer et al Publications ALMA: 98 publ; 30% NL Band-9: 11 publ; 55% NL Jørgensen et al. 2012; Kristensen et al. 2013; Persson et al. 2013

14 Multi Unit Spectroscopic Explorer Integral field spectrometer for the VLT: (Instantaneous) band width: nm 1 x1 FoV, 0.2 pixels Resolving power (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 1 st 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

15 VLT/X-shooter (2009) The most powerful spectrograph in the world 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 1 st 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,

16 Four key-science projects Epoch reionization Surveys Transients Cosmic rays LOFAR DCLA 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

17 Instrumentation program Focus on E-ELT instrumentation PI role in mid-ir imager/spectrometer METIS Partner role in 1 st 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 ( GHz) receiver: final design and series production together with GARD (Sweden)

18 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

19 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 3 rd instrument, imager-spectrometer METIS mid-infrared wavelengths on telescope in 2027 Technology development for METIS in collaboration with industry

20 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

21 ALMA related projects ALMA receiver cartridges Band-9: GHz Band-5: 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 In red: dust in SN 1987A 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)

22 BlackGEM Optical array for gravitational wave counterparts Aim Timeline Phase 1 Per telescope Location To detect and characterize the population of GW counterparts 2016, 5-year project 4 telescopes (3 M ); Phase 2; 15 telescopes (10 M ) 2.7 square degrees, 0.56 /pix, 65cm aperture ESO La Silla GPO/ Marly

23 -NL Goals of the NOVA CTA project 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 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

24 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

25 polarimetric instrumentation development for direct exoplanet characterization WHT/ExPo VLT/SPHERE-ZIMPOL E-ELT/EPICS-EPOL circumstellar disks exo-jupiters rocky exoplanets spin-off: polarimetric instrumentation development for atmospheric aerosol measurements

26 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