Introduction. Chris Evans UK Astronomy Technology Centre (STFC)

Transcription

1 Introduction Chris Evans UK Astronomy Technology Centre (STFC) São Paulo Nov 2015

2 Introduction From the VLT to the E-ELT: Building a Brazilian-UK partnership on astronomical instrumentation for the world s largest telescopes Activities: Evans, Barbuy, Sharples, Cunha, Castilho Stellar populations workshop (Nov 2015) Instrumentation workshop (Feb 2016) Visits of early-stage researchers to the UK 1 complete, 3 booked, ~3 more planned

3 Background

4 E-ELT Science Case Planets & Stars Stars & Galaxies Galaxies & Cosmology

5 Instrumentation

6 E-ELT Instrumentation BIG Nasmyth platforms! Big enough for a VLT!

7 E-ELT Instrumentation Phase A studies Completed early instrument studies 2 studies of AO modules Two selected for first light Full instrument suite to be built-up over first decade

8 E-ELT Instrumentation: ESO Roadmap Two 1 st -light instruments: HARMONI & MICADO Future decision points mapped out 2015/16 HARMONI MICADO METIS MOS HIRES EPICS

9 Previous MOS Phase A Studies EAGLE EVE Multi-IFU, AO-corrected, near-ir Multi-fibre/IFU, opt/ir

10 MOSAIC: Background MOS workshop in A dam (Oct 12) Meetings in UK, Ita, Fra, Bra, NL The Science Case for Multi-Object Spectroscopy on the European ELT January 2015 New Science Simulations ELT-MOS White Paper arxiv: Updates to White Paper White Paper v2; Phase A call arxiv: arxiv: Proposal submission: tomorrow! 1

11 MOSAIC requirements Evans et al. Proc. SPIE arxiv: Multi-Object Spectroscopy with the European ELT: Scientific synergies between EAGLE & EVE C. J. Evans 1, B. Barbuy 2, P. Bonifacio 3, F. Chemla 3, J.-G. Cuby 4, G. B. Dalton 5,6, B. Davies 7, K. Disseau 3, K. Dohlen 4, H. Flores 3, E. Gendron 8, I. Guinouard 3, F. Hammer 3, P. Hastings 1, D. Horville 3, P. Jagourel 3, L. Kaper 9, P. Laporte 3, D. Lee 1, S. L. Morris 10, T. Morris 10, R. Myers 10, R. Navarro 11, P. Parr-Burman 1, P. Petitjean 12, M. Puech 3, E. Rollinde 12, G. Rousset 8, H. Schnetler 1, N. Welikala 13, M. Wells 1, Y. Yang 3,14 1 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 2 Universidade de São Paulo, IAG, Rua do Matão 1226, Cidade Universitária, São Paulo, GEPI, Observatoire de Paris, CNRS, Univ. Paris Diderot, Place Jules Janssen, Meudon, France 4 Aix Marseille Université, CNRS, LAM UMR 7326, 13388, Marseille, France High definition : 10s of objects at fine spatial resolution provided by multi-object AO 5 Astrophysics, Department of Physics, Keble Road, Oxford OX1 3RH 6 Space Science and Technology, Rutherford Appleton Laboratory, HSIC, Didcot OX11 0QX 7 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 8 LESIA, Observatoire de Paris, CNRS, Univ. Paris Diderot, Univ. P. & M. Curie, Place J. Janssen, Meudon, France 9 Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH, Amsterdam, The Netherlands 10 Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK 11 NOVA ASTRON, PO Box 2, 7990 AA Dwingeloo, The Netherlands 12 Institut d'astrophysique de Paris, 98bis Blvd. Arago, Paris, France High multiplex : >100 objects observed at seeing limit/with ground-layer AO 13 Institut d'astrophysique Spatiale, CNRS & Univ. Paris Sud XI, Orsay Cedex, France 14 National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China ABSTRACT The EAGLE and EVE Phase A studies for instruments for the European Extremely Large Telescope (E-ELT) originated from related top-level scientific questions, but employed different (yet complementary) methods to deliver the required observations. We re-examine the motivations for a multi-object spectrograph (MOS) on the E-ELT and present a unified set of requirements for a versatile instrument. Such a MOS would exploit the excellent spatial resolution in the nearinfrared envisaged for EAGLE, combined with aspects of the spectral coverage and large multiplex of EVE. We briefly discuss the top-level systems which could satisfy these requirements in a single instrument at one of the Nasmyth foci of the E-ELT. Keywords: instrumentation: adaptive optics; ELTs; spectrographs galaxies: evolution; stellar content

12 MOSAIC Requirements SC3: Galaxy evolution SC5: Resolved stellar pops beyond the Local Group SC6: Galaxy archaeology > 1 Mpc < 1 Mpc

13 MOSAIC: High-definition mode HST-ACS NGC55 Effective multiplex of >>100

14 MOSAIC: High-multiplex mode HST-ACS NGC55 FLAMES LR08 MOSAIC

15 MOSAIC Phase A Core partners in Phase A: Brazil, France, Germany, Netherlands, UK Phase A to start in Feb/Mar 2016, lasting 20 months. Science workpackage/simulations to include: Revisit science requirements Trade-off studies - wavelength coverage, field-of-view, AO requirements, etc Develop a set of MOSAIC Reference Surveys

16 Other developments KMOS E-ELT

17 VLT-MOONS UK-led consortium to build 3 rd -generation instrument for the VLT KMOS MOONS ~40 sq. arcmin; 24 targets ~500 sq. arcmin 1,000 fibres sim. λ-coverage LR & HR modes 1000 stars/galaxies simultaneously 1000 fiber positioners Optical to near-ir light (0.6µm-1.8µm simultaneously) dispersed in cryogenic spectrographs

18 Galaxy Evolution from peak SFR to present day Quantitative spectroscopy of large (10 5 ) samples of high-z galaxies Disentangling structures of the inner MW with 10 5 stars

19 APOGEE 2 Six-year survey, started in 2014B (Apache Point) Southern survey starts in 2016B (Las Campanas) APOGEE limiting mag: H~12.2 Substantially further/deeper with MOONS Image credit: Ricardo Schiavon

20 VLT-MOONS: Wavelength coverage RI R= 4,000 YJ R= 4,000 H R= 6,000

21 Tests of different diagnostics underway I-band R=9,000 YJ-band R=4,500 H-band R=20,000 FLAMES (multiplex = 130) KMOS (multiplex = 24) PI: Oscar Gonzalez (ESO/Edinburgh) APOGEE (multiplex = 300) Also need to learn lessons from Gaia-ESO & APOGEE analysis: Calibration (data), calibration (models), quality control, survey management, higher-level data products, archiving

22 MOONS Legacy Stellar Survey(s) Stellar GTO: ~ nights Inner MW Origlia & Gonzalez Dwarfs/tails Bonifacio Magellanic Clouds Cioni & Mucciarelli MW clusters Randich First plans now under development (numbers of fields, nights etc) I-band: MOONS cf. FLAMES? Throughput by >3 Multiplex by 7.5

23 MOONS PDR in October, operation in 2019 Field of view 500 sq. arcmin Multiplex Low resolution mode High resolution mode 1000 fibres Throughput > 30 % R = 4, λ = 0.64μm 1.8μm simultaneously R>9,000 for CaT + R=4,000 in YJ-band + R=20,000 in H band Unique contribution to studies of Milky Way Archaeology Formidable SDSS-like survey at z>1 Vital follow-up machine for Euclid, WFIRST, LSST, et al. Last bit of MOS parameter space for Paranal, for now

24 Aims for this workshop Learn about each other s current research, incl: - Ideas for ELT science, and their requirements - New APOGEE results/lessons Identify areas of common interest for future collaboration - Observing proposals - PhD projects (& funding) - Other funding schemes (e.g. toward MOSAIC) Other potential areas for scientific/engineering collaboration? - CUBES - Other MOS instruments (PFS/MS-DESI)? - LSST? SOAR? Gemini? - Need for a (blue) optical MOS on VLT after FLAMES?

25 Thanks!