A high-multiplex and high-definition MOS for the E-ELT
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1 A high-multiplex and high-definition MOS for the E-ELT Lex Kaper (University of Amsterdam, NOVA, co-pi E-ELT/MOSAIC) NL team: R. Navarro (NOVA), B. Lemasle (UvA), R. Roelfsema (NOVA)
2 MOSAIC: E-ELT/MOS Multi-Object Spectrograph for Astrophysics, Intergalactic medium studies and Cosmology OPTIMOS/EVE (2010) + EAGLE (2010) = MOSAIC (2015) PI F. Hammer (Paris Obs, F), co-pi s: B. Barbuy (Sao Paulo, Br), J.-G. Cuby (Marseille, F), L. Kaper (NOVA, NL), S. Morris (Durham, UK), PM P. Jagourel (Paris Obs) PS C. Evans (UK-ATC) IS G. Dalton (RAL, Oxford) More than 50% of VLT time devoted to MOS observations First-light MOS(s) for TMT and GMT Letter of Intent MOS/HIRES, deadline April 10 th, 2015 Start of (competitive?) phase A study Q MOS will become the workhorse instrument of the E-ELT Builds on expertise: VLT/FLAMES, VLT/X-shooter, VLT/KMOS, VLT/MOONS (phase A), WHT/WEAVE
3
4 E-ELT/MOS science cases: White Paper Evans, Puech, et al. (2015arXiv: ) SC1: First light spectroscopy of the most distant galaxies (z ~ 6-13) SC2: Evolution of large-scale structure (IGM tomography) SC3: Mass assembly of galaxies through cosmic time SC4: AGN/galaxy co-evolution and AGN feedback SC5: Resolved stellar populations beyond the Local Group SC6: Galaxy archaeology with metal-poor stars SC7: Galactic center science SC8: Planet formation in different environments MOSAIC Science Team: Chris Evans et al. (73 members) NL science team members: Soeren Larsen, Paul Groot (RU), Ivo Labbe (UL), Eline Tolstoy, Karina Caputi (RUG), Alex de Koter, Lex Kaper, Bertrand Lemasle (UvA)
5 Science requirements MOSAIC
6 Top-level requirements E-ELT/MOS (ESO , March 2 nd, 2015) high definition high multiplex Multiplex few tens ~400 Field of view (7 x7 ) 1 x1 6 x6 0.9 x0.9 Spatial sampling mas GLAO Wavelength coverage (2.5) μm Resolving power 5,000 20,000 Common focal plane approach, possibly fibre-link to HIRES for brightest targets in the field Targets: HST (HUDF), JWST, Euclid, WISH, E-ELT/MICADO,
7
8 Fiber-only option Mixed Architecture Design MOSAIC FOO MAD Fiber-fed spectrograph: sky background subtraction see also ESO Messenger March 2013
9 High multiplex science channels FOO 6x LGS 6x NGS 12x science (high def.) 120x science (high mult.)
10
11 40 Telescope development Diameter mirror (m) E-ELT 10 5 VLT
12 Massive stars in the Local Group and beyond (with Lucas Ellerbroek, Olga Hartoog, Bram Ochsendorf, Frank Tramper)
13
14 VLT/X-shooter The most powerful optical/near-ir spectrograph
15 VLT/X-shooter spectrum nm VLT/X-shooter: Vernet et al. 2011, A&A 536, A105
16 IC1613
17 Tramper et al. 2011, ApJ 741, L8; Tramper et al. 2014, A&A 572, A36
18 He II 4686 Halpha M Ý Z 0.69 Vink et al. (2001, A&A 369, 574) Predicted mass-loss rates as a function of decreasing metallicity are too low Tramper et al. (2011, 2014) Lucy (2012, A&A 543, A18): Additional mass-loss mechanism?
19 First VLT/X-shooter spectrum of massive stars outside Local Group: NGC 55
20 Hartoog et al. 2012, MNRAS 422, 367
21 Extremely Large Telescope
22 Obtaining spectra of O stars in Local Group (and beyond) M V ~ -6 Resolving power R ~ 10, λ/D Limiting mag m V ~ 21 VLT/X-shooter 0.03 ~ 25 E-ELT/MOS Distance (kpc) m V Separation 0.3 pc (arcsec) SMC IC Cen A Virgo cluster
23 RSG J-band spectra in Virgo with S/N ~ 200 in 1 night E-ELT
24 Evolved red giants in galaxies out to 4Mpc number of observable targets ~100 Ben Davies
25 E-ELT: Red supergiants in galaxies out to 35 Mpc number of observable targets increased to ~1500!! Ben Davies
26 ELT-MOS pointings Sculptor group
27 E-ELT/MOS example: NGC 55 Evans et al. Proc. SPIE 2012arXiv:
28 Conclusions A common focal plane has been a very fruitful approach to investigate the synergies and complementarities between different MOS concepts MOSAIC A fibre-link to HIRES seems to be a logical next step in this approach. Late arrival of a MOS in the E-ELT instrument suite is a great risk for the scientific success of the E-ELT. With the E-ELT it will become possible to study massive star populations in a representative sample of galaxies (up to the Virgo cluster). Extra-galactic astronomy and astrophysics will merge. It is obvious that at distances in and beyond the Local Group multi-object spectroscopy is the way forward (certainly if the amount of telescope time is limited).
29 NL workpackages MOSAIC (NOVA-4 proposal) Project science (Kaper, Lemasle, (NL) science team) Project management (Navarro, NOVA) Workpackage Spectrographs (optomechanical design) NOVA Opt/IR group Workpackage Data reduction software (postdoc) Travel budget Budget Staff FTE Cost (k ) NOVA Opt/IR group Travel, hardware, PD Total NOVA 4 request UvA in kind NOVA ESFRI PD Total MOSAIC NL WP
30
31 Gantt chart MOSAIC Call for proposals delta phase A PDR FDR MAIT Commissioning
32 Hans Lipperhey ( ) Delft (May 2014) telescope ~1625 Hollandsche kijker (1608)
33 Embassies of the King of Siam (10 Sep 1608) Newsletter (Zoomers 2008): First visit of a Siamese diplomatic mission to Europe Peace negotiations with Spain (de Spinola) Demonstration telescope by Hans Lipperhey Prins Maurits ( ) A few days before the departure of Spinola from The Hague, an optician from Middelburg offered a few glasses to His Excellence... with which it is possible to see the windows of the church in Leiden. [...] the mentioned glasses are very useful to inspect objects at a distance of a mile and further, as if they are very nearby. Even the stars that are usually invisible due to their small size and our poor sight, can be seen with this instrument."
34 Very Large Telescope, Cerro Paranal, Chile
35 Cerro Armazones, site E-ELT
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