Science Case Fiber/Slit Wavelength Cov ResolutionWav.Cal. Stability

Typical Mag

Throughput FOV AO Multiplex

metals in the IGM fiber/slit 0.32-1.5 >100.000 15-21

few arcsec in the IR?

tomography fibers 0.35-0.70 10.000 19-21 (24) >10% 5 arcmin no ~10x

molecules fiber/slit 0.32-0.7 >100.000 15-20 >10%few arcsec no

galaxiesfiber/slit/IFU 0.35-2.4 10.000 K=24 >20% 30" not really ~10x

primordial Gals red-2.4

>4000-10000 J=26 >20% 3 arcmin not really ~10x

GRBs fiber/slit 0.32-2.4 >5000 15-24 >20%few arcsec in the IR

constants fibers 0.32-0.70 >150.000comb < 1m/s 15-18few arcsec no

expansion fiber 0.35-0.70 >100.000comb2 cm/s (20yr) 15-17 >20%

few arcsec no

HIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY

RESOLUTION

>100.000-150.000 (IGM metals, molecules, constants)(300.000 would be fine too – turbulence? See Evoli 2011)

~10.000 (galaxies, GRBs)

- “Linearly goeth Spectral Range, with the volume scaleth Resolution”

- “Only above R ~ 150.000 Astronomy becomes Astrophysics”

log NHI = 14.7 δ=7

log NHI = 13.5 δ=0

log NCIV = 12

20h

z=3

SPECTRAL RANGE

310-320 nm (constants, IGM metals, molecules, expans.?)350-370 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: J0818+1722 (zem= 6.00, Jvega = 18.5)

Si II 1260z=5.79

C II 1334O I 1302

Si II 1260z=5.87

O I 1302C II 1334

Si II 1526z=5.06

VIS

NIR

R=8800

R=5600

V.D’Odorico + 2010

Metal pollution in the Universe

13.8< log N(CIV) <15

Adelberger 05

D’Odorico, Cupani, Cristiani + 2012

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

0.64

0.86

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~20000. 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 1.450 2.450 2.500 3900

I+z+J 0.800 1.360 1.400 3857

V+R 0.470 0.810 0.850 3765

K 1.950 2.450 1.250 8800

H 1.460 1.830 0.925 8892

J 1.080 1.360 0.700 8714

I+z 0.820 1.030 0.525 8809

R 0.630 0.790 0.400 8875

V 0.500 0.630 0.325 8692

K high 2.090 2.320 0.575 19174

H high 1.545 1.715 0.425 19176

J high 1.170 1.290 0.300 20500

z 0.820 0.910 0.225 19222

R high 0.610 0.680 0.175 18428

V high 0.530 0.590 0.150 18666

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 FGS/NIRISS @ Goddard

NIRCAM and NIRSPEC in 2013]

HIRESHIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY

Fiber spectrograph2 res. Modes (15.000 – 150.000) 3 arms covering (0.32) 0.35-1.7 (2.4) micronHigh-throughput (>20%)3-5’ FOV10x multiplex for the low-res mode High-fidelity (few cm/s, S/N~200 in one exposure)

HIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY

Fiber spectrograph2 res. Modes (15.000 – 150.000) 3 arms covering (0.32) 0.35-1.7 (2.4) micronHigh-throughput (>20%)10x multiplex for the low-res modeHigh-fidelity (1 cm/s, S/N~200 in one exposure)

HIR

ESESO

HIRESHIGH REDSHIFT GALAXIES and COSMOLOGY SUMMARY

Fiber spectrograph2 res. Modes (15.000 – 150.000) 3 arms covering (0.32) 0.35-1.7 (2.4) micronHigh-throughput (>20%)3-5’ FOV10x multiplex for the low-res mode High-fidelity (1 cm/s, S/N~200 in one exposure)