Starbursts from z~3 to 7- Starbursts from z~3 to 7- 10 10 Daniel Schaerer (Geneva Observatory, OMP Toulouse) • Stellar populations: ages, star formation histories, masses, (IMF, metallicities, …) • Reddening: amount (attenuation law, …) • StarFormationRate and SFR density in z ~ 3 to 7-10 galaxies (LBG and Lyman-α emitters)
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Starbursts from z~3 to 7-10 Starbursts from z~3 to 7-10 Daniel Schaerer (Geneva Observatory, OMP Toulouse) Stellar populations: ages, star formation histories,
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Starbursts from z~3 to 7-10Starbursts from z~3 to 7-10Daniel Schaerer (Geneva Observatory, OMP Toulouse)
• Stellar populations:
ages, star formation histories,
masses, (IMF, metallicities, …)• Reddening:
amount
(attenuation law, …)• StarFormationRate and SFR density
– Stellar populations, SF histories, reddening ...• LBG at z ~4 – 6
– Comparing their properties with z~3 – …including UDF
• Lyman-α emitters (LAE)• Distant galaxies seen through the Gravitational Telescope
– Properties of two lensed z ~6-7 galaxies– Searches for z ~ 7 – 10 galaxies and first results
Not discussed: ERO, sub-mm galaxies, red galaxies at z>3, …
Main observables:• Detailed spectroscopy -- rarely available at z>~3
age, SF history, IMF (from line fits) cf. talk Leitherer attenuation (from UV slope or Balmer decrement) cf. poster Noll+ abundances (eg. from R23, or from UV lines) cf. talks Rix, Mehlert,
de Mello
kinematics, masses cf. talk Erb
• Narrowband flux, « poor » spectroscopy z, emission line flux, EW
• Broad-band flux SED, zphot
– Detailed SED fits…– Beta-slope attenuation
• Average SED(z), luminosity functions, …
Observables & methods
this review
Observables & methods – SED degeneracies
1) age – reddening degeneracy (UV restframe):UV slope depends on age, SF history, reddening (+law)
Can be « broken » in some special cases! E.g.:- Presence of emission line (EL) ongoing SF (young burst or continuous SF)- Flat/rising slope + EL Strong extinction- Very steep (blue) slope young + no/little extinctionOr by adding: * restframe optical data (near-IR, SPITZER)* UV lines (cf. Leitherer talk)
2) A priori UV slope NOT metallicity indicator! For « normal » metallicities (Z>~1/50 Zsun) little dependent on Z. Very metal-poor populations: FLATTER slope due to nebular continuum !
Only possible if statistical correlations hold (e.g. Heckman et al. 1998)
But: none of these studies includes information from
presence of Lyman-α
Main results:* mass estimates* typical ages: ~30 Myr to 1 Gyr now confirmed by SPITZER/IRAC mid-IR obs. (Barmby et al. 2004) * no young AND dust free object* From Δt of sample and relative absence of quiescent objects recurrent SF
Papovich et al. (2001)
Age – e-folding timeprob.distribution
Age – stellar mass probability distribution
Age – dust attenuation probability distribution
LBG at z > 3: from 3 to 4
• No detailed SED analysis of galaxies with z >>3
(cf. Schaerer & Pello 2004: 3 lensed galaxies with z>~6)
• UV luminosity density @ z=4 ~ identical to z=3:
Papovich et al. (2004) -- GOODSOuchi et al. (2004) -- SUBARU
Deep Fields global average SFR ~const if same reddening
• Reddening ~constant between z~3 and 4 (from UV colors: i-z’; Ouchi et al. 2004) But: Papovich et al. (2004): possible « blueing » (decrease of mean age, reddening, decrease of M/L)
Ouchi et al. (2004)
0 1 2 3 4 5
LBG at z > 3: from 3 to 5Ouchi et al. (2004) -- SUBARU Deep Fields (BVRiz’): ~2600 LBG at z~4-5
Possible decrease of UV luminosity density from z~3 to 5 – also Iwata et al. (2003) – HDF-N/SUBARU (Viz’) Lehnert & Bremer (2003) – Riz + spectroscopy
z~5: basically no information on reddening since i band affected by Lyman-α forest but: colors consistent with little reddening (L&B03+)• Important uncertainty at z>~5: integration
of LF ! No difference in observed LF from z ~3 to 5
(Ouchi et al.) 0 1 2 3 4 5
afterbeforeLF integration
z~5 spectroscopic follow-ups:* Iwata et al. poster* Douglas,Bremer+ (talk, poster)
LBG at z ~ 5 (cont.)Samples & follow-ups:
1) Iwata et al. (2003) – HDF-N/SUBARU (Viz’) Deep spectroscopy of 17 objects with FOCAS/SUBARU: Ando et al. (2004)
8 confirmed at z~4.5 – 5.2 7 with no or weak Ly-α emission, but relatively strong IS abs.lines In contrast with z~3 LBG ! Due to selection of brightest objects (>L*) ?
2) Lehnert & Bremer (2003) – Riz + spectroscopy cf. poster+talk Bremer+ Bremer et al. (2004) – Viz (Chandra Deep Field S)
6 of 13 galaxies confirmed by Ly-α emission (flux ~(0.2-2.5)*e-17) + break « high » EW(Ly-α) indicative of young age and/or ongoing SF X-ray non-detections: SB or < weak AGN
UV luminosity density from these and brighter objects insufficient to maintain ionisation Sources of reionisation fainter than MAB(1700Ang) > - 21
3) Ouchi et al. (2004) -- SUBARU Deep Fields (BVRiz’)no spectroscopic follow-up yet ?!
i-dropouts: LBG at z~6HST -- UDF: (ACS i’z’+ NICMOS JH)
* Bunker et al. (2004): 54 candidates i’-dropouts over 11 arcmin2 part of UDF (ACS only).
Determine LF, SFR density, …
* Stanway et al. (2004): ~27 candidates with i’z’JH
(z-J) color ~flat spectral slope – SB!
possibly bluer than LBGs at lower z
(lower reddening?, young populations?)
Stanway et al.z_phot z_photextinction
i-dropouts: LBG at z~6
HDF-N (i’z’/ACS + JH/NICMOS) and RDCS field (i’z’/ACS + JKs/ISAAC):
Bouwens et al. (2003 , 2004)
* 11+1 objects with optical + near-IR,
total 21+2 candidates with z>~6
* (z-J) color ~flat spectral slope – SB
* H or K: large uncertainties
no information on stellar populations
* detailed derivations of UV luminosity
density (SFR density) using different
methods and accounting for surface
brightness dimming => SFRD ~14x Stanway
small decrease (39±21 %) of SFRD
from z ~3 to 6
Going beyond z ~ 6-6.5 …
Requires:
* HST: UDF -- ACS+NICMOS (JH): some z dropouts with blue J-H ?!
cf. talk Thompson, poster Bouwens et al.
* HST: ACS grism spectroscopy (Ly-α break up to z ~7; cf. Rhoads et al.04)
* deep JH AND K photometry (J: 7-10 dropout)
present: combined with gravitational lensing !! Future: 30m tel.,JWST
* other selection technique: emission line search
(Lyman-α emitters (LAE))
with narrowband filters, tunable filters, « blind » searches (long-slit spectroscopy, IFU)… in optical or near-IR
So far: successfully applied to from z~2-4 to 6.58
Lyman-α emitters (LAE)
• Numerous LAE searches: see e.g. reviews by Spinrad (2003), Taniguchi et al. (2003)
• Currently used to trace SFR(z) out to
z~6.6 (also clustering properties…)
But: Lyman-α gives only lower limit on
SFR, since affected by several
« destruction » processes (dust,
ISM geometry + kinematics)
• Most LAE are detected in very few (1!)
or no broad-band filter
Little known about their properties,
stellar populations, nature, relation with LBG …Taniguchi et al. (2004)
High median EW(Ly-a) ! AGN ? Very-metal poor objects or Pop III ? Extreme/”massive” IMFs ?
Nature puzzling !BUT: Many metal free objects at z < 6 expected ?? High EW real? Uncertainties in EW from NB ?
* Keck Follow-up spectroscopy of z=5.7 candidates: 3 of 4 confirmed (Rhoads et al. 2002) * no other UV lines detected (but deep enough?) (Wang et al., Dawson et al. 2004)* overall SED ? Nature of LALA sources puzzling !
Similar programs: Hu et al. (2004): SUBARU deep imaging, similar selection criteria 26 z=5.7 candidates, 19 confirmed (DEIMOS/Keck) less than 25% have EW(Ly-a) > 240 Ang! Difference due to deeper imaging !? Ajiki et al. (2002, 2004): several LAE, none with EW(Ly-a) > 200 Ang!
Lyman-α emitters (LAE) at z~ 4.5 – 5.7
Hu et al. 2002, ApJ, 568, L75Hu et al. 2002, ApJ, 568, L75
Abell 370 HCM 6A, z=6.56
• NB excessNB excess•asymetric emission line (Lya)asymetric emission line (Lya)• no secondary imageno secondary image• magnification 4.5 (1.6 mag)magnification 4.5 (1.6 mag)
z >~6-7 galaxies seen through the “Gravitational Telescope”
Prediction:IRAC/SPITZER (non detection) could
confirm strong extinction
SPITZER/IRAC sensitivity
Abell 370 HCM 6A, z=6.56
Main results from spectral fitting:
* Good fits with burst models: age ~ 100-200 Myr, ~no extinction -- BUT no Lyα emission expected then !!
* Good fits with SFR=const + non negligible extinction (AV~1.)
SFR ~ 80-300 Msun/yr (cf. Hu et al.: 9 Msun/yr)
Also mass, luminosity estimateObserved/predicted Lyα flux ~ 9-66%
(Hu+Haiman 2002: ~1/5) No indication on age, metallicity
Schaerer & Pelló (2004)
Abell 2218 KESR, z undetermined (~6-7)
Observations: VIZJHK (HST: WFPC2, ACS, NICMOS), spectroscopic UL on continuum flux (9000-9300 Ang), no emission line – Kneib et al. (2004)
Main results from spectral fitting:* Photometric redshift well behaved z~5.8—6.8* Age: 5-90 Myr (up to 200 Myr)* Best fits: generally little / no extinction* Absence of Lyα NOT SURPRISING ! Intrinsic: too old population Emission present but destroyed (…)
* Quite strong degeneracies in age, SF histories, extinction law !
Object detected with IRAC/SPITZER !(Egami et al. 2004)
Above results compatible with SPITZER observations
Schaerer & Pelló (2004)
Searching for z ~7-10 galaxies with the “Gravitational Telescope”
Abell 1689 - ACS / HST
* Target clusters: “lensing” galaxy clusters with well-defined mass models existing deep optical imaging (ground/HST)
typically 1—3 mag amplification* Ultra-deep NIR (JHK) exposures in cluster corePrime targets: z ~ 7 to 10 galaxies
J-H
H-K
Search for lensed distant/primeval/PopIII galaxies at z > 7
Step 1) Ultra-deep JHK (ISAAC/VLT) + existing optical imaging (HST,…): Traditional drop-out technique + blue rest-frame UV spectrum photometric redshift estimate + selection of starbursts
Step 2) Follow-up near-IR « high-res » spectroscopy (ISAAC): emission line (Ly-a, HeII?) search redshift + other properties !?
Pelló, Schaerer (2001-2003), Barton et al.(2004)
Z~9 critical line
Optical dropouts
H-K
J-H
First spectroscopic confirmation of a possible z=10 lensed source (Abell 1835-IR1916)
Pelló, Schaerer, Richard, Pelló, Schaerer, Richard, Le Borgne, Kneib, 2004, Le Borgne, Kneib, 2004, A&A 415, L19 A&A 415, L19
First spectroscopic confirmation of a possible z=10 lensed source (Abell 1835-IR1916)
Redshift indicators:1) photometric-z ~ 9-112) emission line with z=10.0 if Ly-α3) galaxy on top of critical line for z>~9
* Intrinsic flux: >~ 28.5 – 29. magAB in H and Ks * Magnification factor ~25-100 (3.5 to 5 magnitudes)* Ly-alpha line flux ~ (4.1±0.5)x10-18 erg/s/cm2
Derived properties: (z=10. 460 Myr after Big Bang)* SFR(UV) ~ 2-3 Msun yr-1, SFR(Ly-a) >~ 0.03-0.09
Difference due to: loss of Ly-a photons (ISM geometry,…) partial IGM transmission as source z >> 6!* UV slope no extinction & young population
* Mass estimate (Salpeter IMF 1-100 Msun): M* ~ (9-50).106 Msun (young bursts or const SFR) heavier than massive GC, typical for super star cluster
…properties as expected for young z~10 proto-galaxy…
News from Abell 1835-IR1916
z=2.52Metal-poor HII galaxy (SBS 0335-052)
AV=3.6 !!easy to verify…
* H-band spectroscopy: low z (~2.5) solution excluded* additional photometry (Z, SZ bands):non-detections - compatible with A&A results Schaerer et al. (2004)-- also other attempts to detect IR1916 in optical
* re-analysis of ISAAC spectroscopy (Weatherley et al., astro-ph): non-standard technique not suited to complex observational setup
* GEMINI/NIRI H-band imaging (Bremer et al. 2004): not detected in H spurious? transient source ? Probability = ?
upcoming HST ACS+NICMOS observations of Abell1835 & AC114 fields other z ~7-9 candidates
A1835-2582 A1835-2582 (Richard et al. 2003): z=1.67, [OIII]5007, 4959, H_beta (Richard et al. 2003): z=1.67, [OIII]5007, 4959, H_beta detecteddetected
A1835-775:A1835-775: z=1.888 double line 10760A /10765.5A; likely [OII]3727 z=1.888 double line 10760A /10765.5A; likely [OII]3727
A1835-1055:A1835-1055: z=7.89z=7.89 if Ly if Ly ; unlikely [OII]3727 z=1.9; ; unlikely [OII]3727 z=1.9; or z= 1.16 if [OIII]5007 (no [OIII]4959)or z= 1.16 if [OIII]5007 (no [OIII]4959) or z= 1.2238 if H_beta (no [OIII]5007)or z= 1.2238 if H_beta (no [OIII]5007)
A1835-1143: faint line to be confirmed Data reduction ongoingA1835-1736: no detection within the J bandA1835-1916: z=10.0 Ly emitter Also: AC114:AC114: 1 observing run/ 2 nights/ 2 1rst priority candidates 1 observing run/ 2 nights/ 2 1rst priority candidates