MOSAIC for the ESO-ELT François Hammer (see http://www.mosaic-elt.eu)
Also: Heidelberg/Göttingen, Stockholm/Lund/Uppsala, Helsinki/Turku, Madrid Complutense/IAA, Roma/Arcetri, Vienna, Lisboa/Porto è Last newcomers: Geneva and Univ. of Michigan
Xavier Barcons; EWASS; Liverpool; 12 Avril 2018
Pre-Phase B activities 1. Finalize trade-offs Prof François Hammer Dr Adrian Russell Observatoire Paris-Site de Meudon Director of Programmes • Comparison with other instruments: to GEPI Phone +49 89 320 06955 5 Pl Jules Janssen arussell@eso.org be complimentary with Harmoni 92195 Meudon Cedex France 25 May 2018 • Multiplex depends on mass/volume/budget Dear Francois I am writing to confirm that the MOSAIC project has held the Phase A review and the Review Board congratulated the team for the excellent work. As you know there are a number of actions which need to be completed in order to fully define which version of MOSAIC will be 2. Interfaces with the telescope implemented. These pre-phase B activities are necessary in order to close out on the science trade-offs and set the final top-level requirements of the instrument. Mass/volume finalized by ESO • This has been driven by a number of factors, not least is the fact that ESO no longer has the budget to pay for the MOSAIC hardware. We are taking a proposal to the June 2018 Council to allow MOSAIC to be funded externally in return for GTO. Assuming this proposal is met positively then we hope to move rapidly to confirm the top-level requirements and the target budget for fundraising (the two are related of course). 3. Proposal to ESO Council Further (joint) work will also be required to define fully the interface to the telescope and help define the requirements of the PFS for Nasmyth B. • To exchange GTO against FTE & ESO is still working on the assumption that these pre-Phase B activities will continue smoothly into a GTO funded Phase BCD to completion starting in early 2019 and keep the MOSAIC team hardware budget fully engaged without any major hiatus. I therefore encourage you to plan the effort availability of the team accordingly. • Possibility of Public Surveys Best wishes Dr Adrian Russell ESO Director of Programmes Cc: Dr Mark Casali
MOS ‘Principle’ 1. exploits the telescope collecting surface 1. a moderately good image quality è To perform exceptional & unique science advances in 2020s
16 existing ten meter class telescopes: Total surface area = that of the E- ELT! François Hammer, MOSAIC for ELT, Comité de Suivi
Telescope coating severely limits performance in B, and in the VIS; optimized for METIS. Contract for coating M1 has been cancelled. This justifies limiting VIS to l > 450 nm
Science and final TLRs for MOSAIC Finalize Trade-offs after comparison with other facilities in the 2020s: • We have already limited the MOS capabilities mostly because of (1)Telescope performances (background: no K band, < 1.8 micron, mirror coating: l > 450nm) and (2) Other instruments (comparison with Harmoni shows MOS better for galaxies; fine-tuning of the HDM pixel size) • Mass/budget imposes us to limit to: 4 NIR Spectrographs + 2 VIS Spectrographs
4 prioritized Science Cases First-light galaxies Inventory of matter (incl. mass assembly) Extragalactic stellar populations Evolution of dwarf galaxies Essential to vs. Benefitial to Cf Phase A Science Description
WEBSIM-COMPASS simulator HMM=High Multiplex Mode (mono- aperture fibers) HDM=High Definition Mode (IFUs) http://websim-compass.obspm.fr/ Puech, SPIE, 2016
Instrument parameter space Physical parameter space Observational parameter space Exploring all the parameter space(s) (N>>10 parameters) for all SCs would be prohibitive in (calculation & human) time
The reionisation of the Universe: first objects E-ELT & JWST VLT & HST
Example: z~9 LAEs/LBGs z=9 mJ=28 10 hr
Most distant galaxies: MOSAIC, follow-up of JWST imagery: Higher spectral resolution, search for popIII? z ~ 9 J AB =28 10 hrs z ~ 7 20 hrs Simulations: Disseau et al. J AB =26 IFUs: unbeatable for the best sky subtraction
Collecting surface ensures MOSAIC without competitors for faintest sources in NIR From Vanzella et al. 2014
INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE ILLUSTRIS-TNG
INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE IGM TOMOGRAPHY
Lyman forest: targets at z=3.5, AB=24.5-25.5 (2-10 hrs) Simulations: Japelj et al. AND Metallic lines (missing baryons): targets at z= 3.5, AB=24.5-25.5 Simulations: Rahmani et al. (in prep.) 19 March 2018 François Hammer, MOSAIC for ELT, Comité de Suivi
z ~ 0.1 Werk et al. 2014 COS-HALO with HST 19 March 2018 François Hammer, MOSAIC for ELT, Comité de Suivi
Distant background galaxy z~ 3.5 Circumgalactic medium (CGM) ~ 200-300 kpc Distant background galaxy z~3.5 4500 9000 MOSAIC@E-ELT can z ≥ 3 provide a full understanding of the evolution of the warm/cold gas surrounding galaxies Distant background galaxy Adapted from
INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE ILLUSTRIS-TNG
INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE DARK MATTER FROM ROTATION CURVES GENZEL+17
High definition mode: dark matter evolution from well-sampled rotation curves up to z=4 MOAO is required to provide at least 5 to 7 resolution elements per rotation curve side François Hammer, MOSAIC for ELT, Comité 19 March 2018 de Suivi
IFU ~ 2hrs Simulations of a z=3.6 L* galaxy with EW=50, 200A, pixel scale =80 to 160 microns Simulations: Wang, Puech et al.
Survey speed: MOSAIC will be 8 times faster than HARMONI in doing rotation curves Puech, Evans et al. SPIE, 2018
Local Universe: the Universal rotation curve had required tens of galaxies in each mass bin (e.g. Salucci et al. 2007) A more stringent requirement on multiplex is necessary in the early Universe where galaxies are mostly peculiar, meaning that for 10 galaxies we may expect only 1-4 rotating disks, depending on mass/redshift
in the distant Universe (%) % Fraction of matter in the local Universe z=3-3.5 100 83% 17 4500 9000 Redshifted lines (A, z=3.5) Stars Cool gas Warm-hot Hot Total baryons
Bright emissions: “dithering” may improve spatial resolution by ~ 2 VLT, KECK At z > 6: witnessing the elaboration of ELT the first super massive black holes 19 March 2018 François Hammer, MOSAIC for ELT, Comité de Suivi
MOSAIC performance NGC 55 S/N ~25 S/N ~65 S/N ~140 S/N ~240 S/N >400
MOSAIC performance
Mass, volume & cost issues
MOSAIC multiplex depends first on mass/vol./cost Full MOSAIC (5 NIR + 5 VIS spectrographs): • Too heavy (42 tons instead of 40 tons available) • Too expensive, 32M€ without contingencies! • Could the Consortium be enlarged? • ESO limits on GTO would imply 25M€ as a limit for hardware cost • Would it be better to keep maximal the space of discovery?
MOSAIC multiplex depends first on mass/vol./cost Full MOSAIC (5 NIR + 5 VIS spectrographs): • Too heavy (42 tons w/o contingencies, instead of 40 tons available) • Too expensive, 32M€ without contingencies! • Could the Consortium be further enlarged? • ESO limits on GTO would imply 25M€ as a limit for hardware cost • Would it be better to keep maximal the space of discovery?
Science and final TLRs for MOSAIC Finalize Trade-offs and comparison with other facilities in the 2020s: • Mass/budget imposes us to limit to: 4 NIR Spectrographs + 2 VIS Spectrographs • Very simplified modes (3) for a very powerful instrument: • Keep High Definition Mode: 8 IFUs in NIR (10 as a goal) + High multiplex in both VIS: 80 & NIR: 80+80 (goal: 80 è 100)
IFUs & high multiplex modes • 80 point like objects in VIS, 160 in NIR (or 80 with 80 sky fibers) • 8 IFUs with MOAO in NIR (High Definition Mode) • VIS could be observed simultaneously with HMM-NIR or HDM
Distribution & Operation of observing modes
Fibre link & system complexity Complexity/risk vs GIRAFFE: + : Adaptive Optics, number of spectrographs, more demanding in sky subtraction -: less functions in spectrographs (same slit), larger plate scale
Conclusions • This year 2019: finalize TLRs and prepare the Phase B design • Budget for hardware almost closed, still few new partners in contact • Prepare the Consortium: up to 15 countries, 40 Institutes!!! • Negotiations necessary with ESO for acceding to the telescope • Both MOS/HIRES are classified as Phase 2 instruments (lower priorities) • Also 2019: starting of the survey preparation (130 to 150 GTO nights) • Requires (young) scientists willing to simulate science of the 2020-30
Recommend
More recommend
