HIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY

RESOLUTION > (IGM metals, molecules, constants) ( would be fine too – turbulence? See Evoli 2011) ~ (galaxies, GRBs) -“Linearly goeth Spectral Range, with the volume scaleth Resolution” -“Only above R ~ Astronomy becomes Astrophysics”

log N HI = 14.7 δ=7 log N HI = 13.5 δ=0 log N CIV = 12 20h z=3

SPECTRAL RANGE nm (constants, IGM metals, molecules, expans.?) nm (galaxies, tomography, expansion?) ~red (primordial Gals) ~700 nm, optical (molecules, expansion, tomography) IR-H (metals in the IGM) IR-K (galaxies, primordial galaxies, GRBs)

X-shooter spectrum: J (z em = 6.00, J vega = 18.5) Si II 1260 z=5.79 C II 1334 O I 1302 Si II 1260 z=5.87 O I 1302 C II 1334 Si II 1526 z=5.06 VIS NIR R=8800 R=5600 V.D’Odorico

Metal pollution in the Universe 13.8< log N(CIV) <15 Adelberger 05 D’Odorico, Cupani, Cristiani An archaeological record of past star formation

Reionization: sources of systematics Smaller transmission region due to the presence of associated strong overdensities ! WRONG estimate of the transmission region !!

SED of ionizing spectrum vs. ion.potentials

ADAPTIVE OPTICS ? Most cases do not require adaptive optics (good, HIRES can be used during “bad” weather!) The optical/higher res (constants, expansion, tomography, molecules …) [sky surface brightness] Galaxies [intrinsic dimensions ~0.2”] not extreme AO Would be useful for point-like sources in the IR, when we go faint (GRBs, metals in the IGM at high-z) GLAO?

FOV/Multiplex Most cases do not require multiplex/wide field of view (constants, expansion, GRBs, molecules, IGM metals) FOV: 30” galaxies, 3’ primordial galaxies, 5’ tomography limited multiplex (~10x) MULTIPLEX ANTICORRELATES WITH RESOLUTION (slicer!)

Fibers are OK or required for most of the cases (provided that the sky subtraction in the IR is correct) IFU for galaxies? (see also HARMONI) The whole range UV-optical-IR in one shot is highly desired (e.g. transient phenomena – GRBs, see also economy of ELT time) Throughput MUST be large (faint objects), [cf. HARMONI ~>35%]

CALIBRATIONS Justify stability at a level of few cm/s for ALL high S/N (~>200) cases Need for High-Fidelity spectroscopy (see Dravins 2010) Not only wavelength calibration (Laser Comb) but also (e.g.) flat fielding, relative flux resp., psf (fibers may be an advantage) Telluric lines?

Visible and near-infrared (0.47 to 2.45 µm) integral field spectrograph, over a range of resolving powers from R (≡λ/Δλ) ~ 4000 to R~ The instrument provides simultaneous spectra of ~32000 (8000) spaxels in the near-IR (visible) arranged in a 2:1 aspect ratio contiguous field. HARMONI Arribas, 2011

HARMONI Wavelength Ranges & Resolving Powers Band min [µm] max [µm]  [Å/pixel] R H+K I+z+J V+R K H J I+z R V K high H high J high z R high V high

HARMONI Sensitivity  20 mas spaxels provide best sensitivity for point sources  40 mas spaxels best for extended sources

JWST is not a competitor (complementary resolution) ☺ nor we can expect a synergy [MIRI and Goddard NIRCAM and NIRSPEC in 2013]

HIRES HIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY Fiber spectrograph 2 res. Modes ( – ) 3 arms covering (0.32) (2.4) micron High-throughput (>20%) 3-5’ FOV 10x multiplex for the low-res mode High-fidelity (few cm/s, S/N~200 in one exposure)

HIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY Fiber spectrograph 2 res. Modes ( – ) 3 arms covering (0.32) (2.4) micron High-throughput (>20%) 10x multiplex for the low-res mode High-fidelity (1 cm/s, S/N~200 in one exposure) HIRES ESO

HIRES HIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY Fiber spectrograph 2 res. Modes ( – ) 3 arms covering (0.32) (2.4) micron High-throughput (>20%) 3-5’ FOV 10x multiplex for the low-res mode High-fidelity (1 cm/s, S/N~200 in one exposure)