Evolved stellar populations & E-ELT

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1 Evolved stellar populations & E-ELT G. BONO Outline of the talk E-ELT in a nutshell First light + 3,4,5 EHB stars/agb manque Conclusions GalagbIII, Vienna, 1 st August 2014

Novel 5 mirror design to include adaptive optics in the

8 m Classical 3-mirror anastigmat + 2 flat fold mirrors

3 m Multiple laser guide stars, launched from the side.

2 The Telescope M2: 4.2 m Nasmyth telescope with a segmented primary mirror. Novel 5 mirror design to include adaptive optics in the telescope. M4 (AO): 2.4 m M5 (TT): 2.6 x 2.1 m M3: 3.8 m Classical 3-mirror anastigmat + 2 flat fold mirrors (M4, M5). Nasmyth focus M1 (seg): 39.3 m Multiple laser guide stars, launched from the side. Two instrument platforms nearly the size of tennis courts can host 3 instruments each + Coudé lab. Nearly 3000 tonnes of moving structure.

3 The Mirrors M1: 39.3 m, 798 hexagonal segments of 1.45 m tip-to-tip: 978 m 2 collecting area M4: 2.4 m, flat, adaptive 6000 to 8000 actuators M5: 2.6 x 2.1 m, flat, provides tip-tilt correction

4 The Dome Classical design. Diameter = 86 m, height = 74 m. ~3000 tonnes of steel. Fully air-conditioned and wind shielded.

Instrument Roadmap Following recommendations by the SWG and STC, 2 first-light instruments have been identified, kick-off: 2012. Next group (ELT-3, 4 and 5) broadly identified.

5 Instrument Roadmap Following recommendations by the SWG and STC, 2 first-light instruments have been identified, kick-off: Next group (ELT-3, 4 and 5) broadly identified. Scientifically equal and so sequence is determined by technical readiness. Kick-off: every two years. Planet camera and spectrograph on separate track. Flexibility is maintained by including an as yet unspecified instrument (ELT-6). All phase A studies remain in the pool of possible instruments.

6 First Generation E-ELT Instruments First Light: E-ELT -- CAM (MICADO): R. Davies E-ELT -- IFS (HARMONI): N. Thatte 3) E-ELT MIR: L, M, N 4) E-ELT HIRES (Optical NIR) 5) E-ELT MOS: Fibers + IFUs (optical, NIR) 6) E-ELT Not defined yet

7 E-ELT Project Science Team TLRs for the first light instruments released in 2013: 1-- E-ELT CAM 2-- E-ELT IFU TLRs for 3,4 & 5 instruments released early this year 3 E-ELT MIR 4 E-ELT HIRES 5 E-ELT MOS Formal approval of the TLRs by STC +STC sub-com for E-ELT Next meeting in September in Rome Science operations and calibrations

8 E-ELT CAM: MICADO Plus SCAO + MAO

9 Metallicity gradients in Virgo s ellipticals MAORY PSF Schreiber et al Greggio et al AGB/RSGs in Coma s ellipticals (plausible)!

NIR images & SCAO at 8m telescopes FLAO@LBT M15 core FWHM of 0.05 (J) & 0.06 (Ks) arcsec.

10 NIR images & SCAO at 8m telescopes M15 core FWHM of 0.05 (J) & 0.06 (Ks) arcsec. Strehl ratio 13 30% (J), 50 65% (Ks) J-band image Limiting magnitudes: J~22.5 mag Ks~23 mag Drift of the PSF shape at larger Distances from the NGS

11 Symmetric vs asymmetric PSF Increase in the number of unknowns (8 vs 4), but AO images are oversampled (ROMAFOT environment) Fiorentino et al. (2014)

12 NIR CMDs of M15

13 The absolute age of M15: NIR LUCI (4x4arcmin): 19J sec 20K 20 sec PISCES (26X26arcsec): 30J 30 sec 30K 15 sec WFC3: F160W(H) 3X200+6X250sec Monelli et al. (2014)

14 E-ELT Integral Field Spectrograph: HARMONI

15 E-ELT Integral Field Spectrograph: HARMONI Plus SCAO 33,000 spaxels per exposure!

16 DETECTION OF THREE CEPHEIDS IN THE NUCLEAR BULGE!!! Matsunaga et al. (2011)

17 Three classical Cepheids in the NB Periods from ~20 to 23.5 days True distance modulus = 14.50±0.07 mag (7.9±0.2±0.3 Kpc) Spitzer single epoch magnitude support this distance projected distance from the central black hole Δl = -6.9, -7.8, 33.9 (pc) Δb = 0.4, 0.7, 6.5 (pc) located in the thin disk-like structure of the NB Mean J magnitude ~ 15.5 Mean K magnitude ~10.2 Ak (selective absorption) Av~25-30 mag!! Obscured AGBs and RSGs in the Bulge and in the NB

18 E-ELT: HIRES

19 HIRES: possible observing modes MR-MOS for all modules/wavelengths with full spec coverage HR 2 MOS/IFU only in IR where AO works patrol field of MOS depends on where the fibers positioner is located parallel modes, e.g. MR-MOS in optical while HR in IR on a single object

HIRES: stellar science stellar atmospheres (3D structure,

yields etc.) stellar evolution (critical stage

pre-main & WD-cooling sequences, star/disk/planet formation) stellar

spectral resolution critical to fully de-blend lines of any chemical

e. to resolve [sub]structures E-ELT critical to get high SNR with

chemical abundances) for quantitative spectroscopy of faint stellar

20 HIRES: stellar science stellar atmospheres (3D structure, asteroseismology,surface parameters & activity, mixing, diffusion, yields etc.) stellar evolution (critical stages, e.g. pre-main & WD-cooling sequences, star/disk/planet formation) stellar pop (chemical evolution, environment effects, LG and beyond) high spectral resolution critical to fully de-blend lines of any chemical specie (including isotopes) to kinematically resolve line profiles, i.e. to resolve [sub]structures E-ELT critical to get high SNR with impact on accuracy (e.g. chemical abundances) for quantitative spectroscopy of faint stellar pop (TO stars, W/B dwarfs) IR critical to study cool & metal rich stellar populations star forming regions and proto-planetary disks for specific line diagnostics (e.g. O isotopes in the K band, O from many OH lines in the H band)

21 Is the Spite plateau an universal relation?

22 Extremely MP Halo Stars SMSS J Five objects: [Christlieb+2002; Frebel+2005; Norris+2007; Caffau+2011 Keller+2013 skymapper Carbon enhanced Extremely Iron poor A few & probably a single low-energy SN Extremely massive SN (pair-instability) should Rapidly increase Fe content UPPER LIMIT 10^{-7.1} 3σ c.l.

23 Extremely Metal-Poor Halo Stars Preliminary evidence indicates that for [Fe/H] <-4.5 the assumption of instantaneous mixing of star-forming gas might not be appropriate

24 Carbon-enhanced M.P. stars Only MSTO & dwarves blue- dashed line [C/Fe]=+1 Caffau+ (2013) + X-SHOOTER LP pending! Spite+ (2013) Identification of a few C enhanced & α-poor SMSSJ A(C)~9~solar!!

25 Requirements for in J,H,K-band Large FoV High multiplex Spatial res. > a few arcsec > intrinsic < arcsec Abundances (Iron, α-, s-, r-elements) High-res R~20,000 Limiting mag. K~23 mag CRIRES (+GIANO) update crucial step, atmosphere models, line identifications, molecules (NIR regime)

26 E-ELT: MOS (Fiber Only Option)

27 E-ELT: MOS

28 E-ELT: MOS (Mixed Architecture design)

EHB stars in ω Cen HB morphology a) Increase in He b) Increase in mass loss Rotation, binarity Two different paths: He enhancement from super AGB (Alvio, Doherty,

29 EHB stars in ω Cen HB morphology a) Increase in He b) Increase in mass loss Rotation, binarity Two different paths: He enhancement from super AGB (Alvio, Doherty, Karakas, Oscar) Hot helium flashers Castellani + (1993, 2006), Pier-Oscar RG truncation (Eric, Kamath) (Castellani ; Monelli ; Calamida ) Cassisi

30 Spectra CI Latour , submitted CI CIV CIII CII Hδ Hγ HeI HeI HeI HeI HeI HeI HeII HeII HeII

31 NLTE analysis: H, He, C, N, O

32 NLTE analysis: Carbon

33 Log N(He)/N(H) Log N(He)/N(H) Three different groups Teff (K) Log g

34 LogY Log N(He)/N(H) He & C Strongly correlated Similar evidence for field SdO/SdB stars Preliminary evidence (Moehler et al. 2002, 2007, 2011) Log N(C)/N(H) Detection of N in He & C enhanced objects Deeper and more accurate Spectra. Log C

35 Evolutionary links Miller-Bertolami et al. (2008) Brown + (2001) Early hot He Flashers shallow mixing Late hot He Flashers Deep mixing Gravitational settling moves the tracks at lower Teff and g (Michaud et al. 2011) Competing mechanism to slow down diffusion processes: [radiative levitation] Convective mixing Mass loss

36 Cocnclusions I The 8-10m class telescopes are paving the road for ELTs: Relevant impact on seeing limited (GLAO): optical spectroscopy (HARMONI, HIRES, MOSAIC) Adaptive optics (MAO, SCAO): Imaging: MICADO Spectroscopy: HARMONI, [HIRES], MOSAIC (IFUs) The transitions to ELTs is not trivial at all. A new spin on theoretical modeling: atmospheres (nir lines), envelopes, interiors Opening new approaches to handle data from IFS & NIR images

37 Conclusions II Stellar Astrophysics is in good shape We are facing a substantial change in the approach for doing astrophysics: User Oriented Experiment Oriented ESTOTE PARATI!!!

38 NEAR FUTURE

39 NEAR FUTURE

40 13-17 October 2014 Resolved And Unresolved Stellar PopUlaTIoNs

41 The difference between normal persons and insane ones is precisely that the normal persons have all the diseases of the mind, while the madmen have only one! R. Musil, The Man Without Qualities

42 The End Image credit : Swinburne Astronomy Productions/ESO

43 Credits To young & senior researchers with whom I have the pleasure to share this wonderful adventure THANKS!

44 riserve

45 Caffau et al. (2012) EMP stars when the Spectral resolution IS a crucial issue.

46 ESPRESSO

47 Approaching H-burning limit & beyond Transition between VLMS & BDs MS-Knee Mk~5.5 Transition from late-m to L-type Diatomic metal species (TiO, VO, FeH) incorporated in grains Formation of Fe & Si grains produce optically thick clouds that veil gaseous absorption bands L-type Redder NIR colors 1.5k-2.0k K At lower Teff the clouds start to sink and CH4 supplant CO as the dominat C-bearing molecule T-type Bluer NIR colors (Te~1.0k K ) Saumon et al. (2008) For types later than T5 CIA by H2 enhances bluer NIR colors

Transition between BDs & Free Floating Giant Planets Mk Late T-type Mk~16 For Teff ~600K the NH3 join Water and CH4 absorption N2 vertical mixing the NIR Flux COLLAPSE Y

48 Transition between BDs & Free Floating Giant Planets Mk Late T-type Mk~16 For Teff ~600K the NH3 join Water and CH4 absorption N2 vertical mixing the NIR Flux COLLAPSE Y spectral type For ages older than 1 Gyr the Decrease is mag!!! J-K Burrows et al. (2003) NIRCAM@JWST & E-ELT CAM Will constrain the change in the IMF in the transition VLMs-BDs-GPs

49 Spectroscopy in the MIR region HR spectroscopy in L, M bands Line list for NH3 and N2 are incomplete in NIR!

50 A global cloud map of brown dwarfs CRIRES spectra by Crossfield et al. (2014, Nature)

51 A global cloud map of brown dwarfs

Direction - Conférence. The European Extremely Large Telescope

Direction - Conférence. The European Extremely Large Telescope Direction - Conférence The European Extremely Large Telescope The E-ELT 40-m class telescope: largest opticalinfrared telescope in the world. Segmented primary mirror. Active optics to maintain collimation