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near-IR science at high spectral resolution

2 nd Generation Science with the LBT Ringberg Castle, July 13-19, 2008. near-IR science at high spectral resolution. Livia Origlia. INAF - Osservatorio Astronomico di Bologna, Italy. livia.origlia@oabo.inaf.it. near IR science at high spectral resolution.

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near-IR science at high spectral resolution

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  1. 2nd Generation Science with the LBT Ringberg Castle, July 13-19, 2008 near-IR science at high spectral resolution Livia Origlia INAF - Osservatorio Astronomico di Bologna, Italy livia.origlia@oabo.inaf.it

  2. near IR science at high spectral resolution • chemical abundances & abundance patterns SF history, timescales, rates, etc., primordial vsself-enrichment etc. • radial velocities, velocity dispersions, Zeeman splitting distances, masses, m.f, etc. • near IR range crucial to study • red, reddened, redshifted objects: • earth-like planets • cool SPs • galaxy bulges and centers • extra-galactic star clusters & SPs • young SSCs & star forming regions/galaxies • host galaxies of both type I & II AGNs • high z (>4) Lya absorbers & GRBs ............

  3. neutral atomic lines Fe, Si, Ca, Mg, Ti, Al, Na cool stars: near - IR spectra

  4. OH, CO, CN molecular bands  very sensitive to C, O & N abundances cool stars: near - IR spectra

  5. chemical abundances the SF history of a stellar system is imprinted in its chemical abundance patterns a elements: O, Si, Ca, Mg,Ti type II SNewithmassive progenitors released in the ISM from the very beginning of the SF onset Fe - group elements type Ia SNewith intermediate mass progenitors C, N, s-process elements AGBwithlow-intermediate mass progenitors released in the ISM after@1 Gyr from the SF onset

  6. a-elements: O, Si, Ca, Mg, Ti 0.5 Galactic Bulge, E gal halo – like but at higher SFR [a/Fe] Galactic Halo from a gas enriched by SNII on a short (< 1 Gyr) timescale 0.3 SFR Galactic Disk from a gas also enriched by SNIa on a longer timescale 0.0 -2.0 -1.0 0.0 [Fe/H] our Galaxy

  7. SURVEY of cluster & field M giants H band (1.5-1.8 micron) echelle spectra with NIRSPEC at Keck II Rich, Origlia & Valenti 2007, ApJ 665, 119 abundance patterns in the Galactic Bulge

  8. integrated spectra VISUAL NEAR IR old SPs RGB + HB + MS @TipRGB young SPs MS+BSG+nebularRSG spec+pop synthesis model (IMF) dependent@ RGB/RSG SB/AGN nebular + host RSG / host

  9. SSC - NIRSPEC@Keck R=25,000 Larsen et al. 2006 NGC 6946 WPC2@HST F555W D=5.9 Mpc, age=10-15 Myr s=10.4 km/s, M=1.7 x 106 Mo L/M  Salpeter IMF Larsen et al. 2001 extra-galactic stellar clusters s = 9.1 km/s [Fe/H] = -0.45 +/- 0.1 [Ca,Mg,Al/Fe] = +0.25 +/- 0.15 [O,Ti/Fe] = +0.29 +/- 0.10 [Si/Fe] = +0.08 +/- 0.18 [C/Fe] = -0.25 +/-0 .11 12C/13C = 8 +/- 2

  10. chemistry kinematics Dv @30 km/s sint @13 km/s Mdyn>106 Mo small galaxies molecular blends few atomic lines global metallicity,a/Fe R£10,000 Dv@10 km/s sint@4 km/s Mdyn@105 Mo massive GCs R@30,000 OH lines,CO blends several atomic lines accurate (<0.2dex) Fe,C,O,a -1.0 mag Dv @ 3 km/s sint @1.3 km/s Mdyn@104 Mo Magellanic-like GCs m.f., RVs (1m/s) OH,CO,CN lines many atomic lines detailed (<0.1dex) Fe,CNO+isotopes,a R³100,000 -2.0 mag near IR science at high spectral resolution

  11. K H OH H J R=10,000 R=30,000 R=100,000

  12. UKIDSS: 2MASS: H,K£14 H,K£18 >8mELT 4-8m MCs R@104 M31 R@104 inner MW TO R@105 few Mpc R@104 R@104 few-tens Mpc R@104 R@104105 R@104105 brightest tens pc hundreds pc R@105 atmospheres during a transit R>104 near IR science at high spectral resolution sensitivity res SPs integ SPs DLAs Lya abs planets

  13. N 1.8 : R @ 5,000 q=0.5” SR @ l/5 LS + MOS N 3.75 : R @ 10,000 q=0.25” SR @ l/10 LS + MOS N 3.75 : R @ 10,000 q=0.25” SR @ l/10 LS + MOS N 30 : R @ 30,000 q=0.10” SR @ l/30 LS N 30 : R @ 30,000 q=0.10” SR @ l/30 LS near IR science at high spectral resolution

  14. near IR science at high spectral resolution LUCIFER@LBT R=10-30,000 s/n=30 texp=2hr H@15-16  2MASS [& beyond] RGB Tip: H@-5  (m-M)0=20-21  @100 kpc RSG,AGB: H@-9  M31 GC: Hint@-11;-13  (m-M)0=27-29  @10 Mpc

  15. LUCIFER@LBT today: N 3.75 : R @ 10,000 q=0.25” SR @ l/10 LS + MOS N 30 : R @ 30,000 q=0.10” SR @ l/30 LS existing R@30,000 @ 4-8m telescopes: CSHELL@IRTF R=30,000 q=0.5”x30” l/240 GIANO*@TNG R=50,000 q=0.5”x6” l/1.3 PHOENIX@Gemini R=50,000 q=0.3”x14” l/200 CRIRES@VLT R=50,000 q=0.5”x15” l/100 NIRSPEC@ KeckII R=37,000 q=0.3”x24” l/10 SDSS3-APOGEE: MW H-band survey at R=20,000 (2011-14) MOS at med/high res  unique capability

  16. possible competitive upgrades ? R>10,000  complementary capability to JWST today: R=10,000+MOS kinematics of resolved SPs [1] R=30,000 + MOS  N3.75 + immersion grating? [nSi=3.4  RIG@3 RNG] chem & kin of both resolved & integrated SPs today: R=30,000 + LS  chem & kin of massive GCs [2] R=30,000 + larger SR  N30 + cross disperser? higher efficiency for multi-line science [3] R=30,000 + larger FoV  N30 + IFU? >some MOS at @twice the spatial res of [1] > higher sensitivity

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