Seeing the Distant Universe in 3 D 3

Seeing the Distant Universe in 3 D 3 D Integral Field Spectroscopy at high redshift Andrew Bunker, AAO & Oxford

Redshift z After era probed by WMAP the Universe enters the so-called “dark ages” prior to formation of first stars Hydrogen is then re-ionized by the newlyformed stars When did this happen? 1100 DARK AGES 10 5 2 What did it? 0

z~1 HDF spiral H (1. 6 m) J (1. 2 m) I (0. 8 m) V (0. 6 m) B (0. 45 m) U (0. 3 m) Near Infrared Camera NICMOS HUBBLE SPACE TELESCOPE

H (1. 6 m) J (1. 2 m) I (0. 8 m) V (0. 6 m) B (0. 45 m) U (0. 3 m)

"3 D" Spectroscopy Previously used a "long slit" in spectroscopy - cut down background light, become more sensitive Relatively new technique - integral field spectroscopy - arrange elements to survey a 2 D area (rather than a 1 D line) The spectra gives a 3 rd dimension (wavelength, or velocity)

Cambridge IR Panoramic Survey Spectrograph Integral Field Spectroscopy

What is CIRPASS? 500 fibres IFU · Near-infrared integral field unit (spectra over a 2 D area) · Built by the Io. A with support of Sackler foundation & PPARC · Wavelengths 0. 9 -1. 8 mm (z, J, H): doubles range of Gemini IFU science · 490 spatial samples & variable image scales 0. 05"-0. 33" up to 5"x 12" field · Large wavelength coverage Instrument cryostat (Dl=2200Å) at R~4000: great sensitivity between OH sky lines · Limiting line flux on an 8 m ~2 x 10 -18 ergs/sec/cm^2 (5 3 hours) On dome floor

Sky "glow" in the near-IR

Exquisitely sensitive to line emission redshifted between OH ● Star formation at z>1 (H , [OIII]5007Å, H , [OII]3727Å) ● Robust star formation rate measures down to 1 M⊙/yr ● Rotation curves, kinematics ● Masses, extinction, metallicity ● Nature of damped Lyman- systems at high-z ● Lensed galaxies/dark matter sub -clumping ● Ages of young star clusters ● IFU Science

Gemini Integral Field Spectroscopy · Institute of Astronomy, Cambridge: Andy Bunker(AAO/Oxf), Joanna Smith (Ph. D student), Rachel Johnson (Oxf), Gerry Gilmore & Ian Parry, Rob Sharp, Andrew Dean etc CIRPASS team · Gemini: Matt Mountain, Kathy Roth, Marianne Takamiya, Inger Jørgensen, Jean-Rene Roy, Phil Puxley, Bryan Miller, etc. (Director's discretionary time) · Durham: Richard Bower, Roger Davies (Oxf), Simon Morris, Mark Swinbank etc. & GMOS team – Program with Gemini Observatory to demonstrate the power of IFUs (5 nights GMOS+8 nights CIRPASS) · Large interntational team (CIRPASS observations involve ~50 scientists) lead by Cambridge/Gemini/Durham · First demonstration of near-IR IFU science

GEMINI-NORTH GMOS-IFU Andrew Bunker, Gerry Gilmore (Io. A, Cambridge) & Roger Davies (Durham/Oxford) optical: Gemini Multi-Object Spectrograph Hawaii June 02 Chile Aug '02, Mar/Jun 03 GEMINI-SOUTH

Q 2237+03 Einstein cross Search for dark matter substructure - Ben Metcalf, Lexi Moustakas, Bunker z=1. 7 QSO, z=0. 04 lens

Substructure at 104 M⊙<M<108 M⊙ is 4%-7% of surface mass density - high compared to some CDM predictions (but poss. variability/microlensing)

Q 2237+03 Einstein cross Ben Metcalf, Lexi Moustakas, Andy Bunker & Ian Parry (2004, accepted by Ap. J, astro-ph/0309738)

A z=1. 2 radio galaxy 3 C 324 (Joanna Smith Ph. D) · Extended blue light over >5", aligned with radio · 3 C radio galaxy z=1. 2 deep HST im. · studied by Spinrad & Dickinson · evidence of a cluster · size well-suited to GMOS/CIRPASS · study emission lines [OII] & [OIII]/H (kinematics)

[OIII] map in 3 D of a z=1. 2 galaxy (Smith, Bunker et al. ) Sky (xy) (xz) Semi-raw frame (yz)

CIRPASS [OIII]5007 HST R-band GMOS-IFU [OII]3727 HST B-band (rest-UV) 3 C 324 alignment effect, with Joanna Smith (Ph. D student)

GMOS IFU Spectroscopy Gemini-N · 3 C 324 z=1. 21 radio galaxy - "reduced" 2 D (still has sky & cosmics, but extracted fibres) 8000Å 8300Å [OII]3727Å @z=1. 2

Wavelength/velocity 3 C 324 3 -D data cube [OII]3727 structure has two velocity components at +/-400 km/s

CIRPASS [OIII]5007 HST R-band GMOS-IFU [OII]3727 HST B-band (rest-UV) 3 C 324 - Smith, Bunker, et al. : alignment effect

Galaxy kinematics redshift 1! H map of a CFRS disk galaxy with CIRPASS (Smith, Bunker et al. , submitted)

Wavelength/velocity [OII]3727Å doublet, ~300 km/s velocity shift z=1 arc 3 D data cube

z=1 arc de-lensed Mark Swinbank, Joanna Smith, Richard Bower, Andrew Bunker et al sky (lensed) de-lensed HST/WFPC (B, R, I) F 450 W, F 606 W, F 814 W [OII]3727Å velocity map

Galaxy Kinematics at High Redshift: Why do we care? - For disk galaxies, velocity at flat part of rotation curve correlates with the stellar mass of the galaxy (I- or K-band) - the Tully Fisher relation -How does this scaling relation evolve with time? - In "classical" model, dark halo forms first, and disk forms later: M/L decreases with time. -So circular velocity at a fixed stellar mass less in the past - BUT in hierarchical assembly, make galaxies through mergers, so stellar mass vs. circular velocity follows same relation over a wide range of redshifts - Can test this through rotation curves of z~1 galaxies - Use rest-optical lines redshifted into near-infrared - IFUs ideal - no uncertainty of slit axis vs. galaxy axis

Emission lines ⇒ Star formation rates, metallicity, dust extinction, kinematics

Damped Ly- QSO Absorption Systems Bunker, Warren et al.

Star formation in damped Ly- systems (Joanna Smith Ph. D)

CIRPASS refereed Publications · "Spectroscopic Gravitational Lensing and Limits on the Dark Matter Substructure in Q 2237+0305" R. B. Metcalf, L. A. Moustakas, A. J. Bunker & I. R. Parry Ap. J (astro-ph/0309738) · "Extragalactic integral field spectroscopy on Gemini" A. Bunker, J. Smith, I. Parry, R. Sharp, A. Dean, G. Gilmore, R. Bower, A. M. Swinbank, R. Davies, R. B. Metcalf & R. de Grijs (astro-ph/0401002) · "CIRPASS near-IR integral field spectroscopy of massive star clusters in the starburst galaxy NGC 1140" R. de Grijs, L. J. Smith, A. Bunker, R. Sharp, J. Gallagher, P. Anders, A. Lancon, R. O'Connell & I. Parry; MNRAS (astro-ph/0404422) · "The Tully-Fisher Relation at z~1 from CIRPASS near-IR IFU H -alpha spectroscopy" J. Smith, A. Bunker, N. Vogt et al. MNRAS 2004

Seeing fluorescence from neutral hydrogen 20" z=4. 5 QSO illuminating its protogalaxy 200Å zem=4. 487 5" Spatially Extended Ly- Emission

Extended Ly- , narrow (FWHM~1000 km/s) Recombination line probably powered by reprocessed QSO UV flux rather than by local star formation. Central QSO (solid line) broad Ly- Extended narrow Ly- (dashed line), no continuum The HI cloud of the host galaxy is ~>35 kpc/h 70 ( =0. 3)

SPH simulations, distribution of neutral gas at z~3 (from Katz et al. and Rauch, Haehnelt & Steinmetz). Left box is 22 Mpc comoving, 15 arcmin; right zoomed x 10

The catch: very faint low surface brightness Wavelength/Å The deepest spectrum in the Universe?

Rauch, Haehnelt, Bunker, Becker et al. (2007) Win with IFUs rather than long-slit: MUSE?

DAZLE - Dark Ages 'z' Lyman-alpha Explorer (Io. A - Richard Mc. Mahon, Ian Parry; AAO - Joss Bland-Hawthorne

"Lyman break technique" - sharp drop in flux at below Ly-. Steidel et al. have >1000 z~3 objects, "drop" in Uband. Pushing to higher redshift- Finding Lyman break galaxies at z~6 : using i-drops.

The Star Formation History of the Univese Bunker, Stanway, Ellis, Mc. Mahon & Mc. Carthy (2003) Keck/DEIMOS spectral follow-up & confirmation I-drops in the Chandra Deep Field South with HST/ACS Elizabeth Stanway, Andrew Bunker, Richard Mc. Mahon 2003 (MNRAS) z=5. 8

Galaxies at z~6 are small - barely resolved by HST. E-ELT diffraction limit ~0. 01” (~50 -100 pc). See individual HII regions?

What is JWST? ● 6. 55 m deployable primary ● Diffraction-limited at 2 µm ● Wavelength range 0. 6 -28 µm ● Passively cooled to <50 K ● Zodiacal-limited below 10 µm ● Sun-Earth L 2 orbit ● 4 instruments ● – 0. 6 -5 µm wide field camera (NIRCam) – 1 -5 µm multiobject spectrometer (NIRSpec) – 5 -28 µm camera/spectrometer (MIRI) – 0. 8 -5 µm guider camera (FGS/TF) 5 year lifetime, 10 year goal

NASA/ESA/CSA - JWST ● NIRSpec – ESA near-IR MOS to 5 um, 3’x 3’ ● NIRCAM - 3’x 3’ imager <5 um ● FGS (Canada) - has tunable 1% narrow-band NIR filters in ● MIRI - mid-infrared Europe/US (closely similar to HST model…)

NIRSpec IST

Absorption lines at z>5 - a single v. bright Lyman break z=5. 5 galaxy, Dow. Hygelund et al (2005), AB=23 -24, VLT spectrum (22 hours), R~3000; S/N=3 -10 at R=1000, 2700 in 1000 sec NIRSpec

E-ELT

For I-drops (z~6) would only get ~1 per NIRSpec field bright enough for S/N~3 -10 in continuum in 1000 sec for abs line studies

- Does AO Help you? If Ly-alpha is compact, AO will boost point-source sensitivity -- Unclear if this will be the case - extended Ly-alpha haloes known, and expected through resonant scattering (see the far edge of the ionized bubble) -For morphological analysis, unclear that high-tech ELT AO is better than a poorer but better-quantified PSF (e. g. from space) --If you can’t quantify where 10 -20% of the light goes from a centrally-condensed core, that’s the difference between a disk and bulge morphology when fitting Sersic index -

Conclusions - 3 D IFU spectroscopy at high redshift is (finally) realising its potential, but still small sample sizes --Important as a probe of galaxy kinematics, and spatiallyresolved maps of stellar populations, metallicity -- Trace the evolution of the assembly of stellar mass --Explore the nature of gravitational lenses (dark matter) -- Explore the nature of the galaxies responsible for QSO absorption lines --In future might see fluorescence of the HI gas --Compact galaxies at high-z: need AO on ELTs to get real IFU benefit -

GMOS-IFU (Swinbank et al. 2003)

! H G LT IN EA N H AR W CFRS 22. 1313 CIRPASS H Lensed arc z=1 GMOS [OII] Tully-Fisher a redshift 1! Swinbank, Smith, Bower, Bunker et al.