the first billion years of history - seeing galaxies close to the dawn of time andrew bunker, andrew...
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The First Billion Years of The First Billion Years of
History - seeing Galaxies History - seeing Galaxies
Close to the Dawn of TimeClose to the Dawn of Time
Andrew Bunker,Andrew Bunker,
Anglo-Australian Anglo-Australian
ObservatoryObservatory
& University of Oxford& University of Oxford
KIAA/PKU WorkshopKIAA/PKU Workshop
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"Lyman break technique" - sharp drop in flux at
below Ly-. Steidel et al. have >1000 z~3
objects, "drop" in U-band.
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HUBBLE SPACE HUBBLE SPACE
TELESCOPETELESCOPE
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"Lyman break
technique" - sharp
drop in flux at
below Ly-.
Steidel et al. have
>1000 z~3 objects,
"drop" in U-band.
Pushing to higher
redshift- Finding
Lyman break
galaxies at z~6 :
using i-drops.
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Using HST/ACS GOODS data - CDFS &
HDFN, 5 epochs B,v,i',z'
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By selecting on rest-
frame UV, get
inventory of ionizing
photons from star
formation. Stanway,
Bunker & McMahon
(2003 MNRAS)
selected z-drops
5.6<z<7 - but large
luminosity bias to
lower z.
Contamination by
stars and low-z
ellipticals.
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10-m Kecks10-m Kecks
8-m Gemini8-m Gemini
ESO VLTsESO VLTs
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The Star Formation
History of the Univese Bunker, Stanway, z=5.8
Ellis, McMahon
& McCarthy (2003)
Keck/DEIMOS
spectral follow-up
& confirmation
I-drops in the Chandra Deep
Field South with HST/ACS
Elizabeth Stanway, Andrew
Bunker, Richard McMahon
2003 (MNRAS)
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GLARE I: Stanway, Glazebrook, Bunker et al.
2004 ApJ 604, L13
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GLARE II: Stanway, Bunker, Glazebrook et al.
2007 MNRAS 376, 272
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For I-drops (z~6) would only get ~1 per NIRSpec field bright enough for S/N~3-10 in continuum in 1000sec for
abs line studies
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Looking at the UDF (going 10x deeper, z'=26 28.5 mag)
Bunker, Stanway, Ellis
&McMahon 2004
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After era probed
by CMBR the
Universe enters
the so-called
“dark ages” prior
to formation of
first stars
Hydrogen is then
re-ionized by the
newly-formed
stars
When did this
happen?
What did it?
DARK AGES
Redshift z
5
10
1100
2
0
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Implications for Reionization
From Madau, Haardt & Rees (1999) -amount
of star formation required to ionize Universe
(C30
is a clumping factor).
This assumes escape fraction=1 (i.e. all ionzing photons make
it out of the galaxies)
Our UDF data has star formation at z=6 which is 3x less than
that required! AGN cannot do the job.
We go down to 1M_sun/yr - but might be steep (lots of low
luminosity sources - forming globulars?)
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Ways out of the Puzzle
- Cosmic variance
- Star formation at even earlier epochs to reionize
Universe (z>>6)?
- Change the physics: different recipe for star
formation (Initial mass function)?
- Even fainter galaxies than we can reach with the
UDF?
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Spitzer – IRAC (3.6-8.0 microns)
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- z=5.83 galaxy
#1 from
Stanway, Bunker
& McMahon
2003 (spec conf
from Stanway et
al. 2004,
Dickinson et al.
2004). Detected
in GOODS
IRAC 3-4m:
Eyles, Bunker,
Stanway et al.
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Other Population Synthesis Models
Maraston vs. Bruzual & Charlot
B&C =500Myr,
0.7Gyr, 2.4x1010MsunMaraston =500Myr,
0.6Gyr, 1.9x1010Msun
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●30Myr const SFR
with E(B-V)=0.1
●No reddening
●0.2solar
metallicity
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-Have shown that some z=6 I-drops have old stars and
large masses (subsequently confirmed by H. Yan et al)
-Hints that there may be z>6 galaxies similar (Egami
lens). Mobasher source - z=6.5??? (probably lower-z) -Turn now to larger samples, to provide stellar mass
density in first Gyr with Spitzer-- In Stark, Bunker, Ellis et al. (2006) we look at v-
drops (z~5) in the GOODS-South-21 have spectroscopic redshifts, 2/3rds unconfused at
Spitzer resolution-- Also use 200 photometric redshifts (going fainter),
>50 unconfused
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Eyles, Bunker, Ellis et al. astro-ph/0607306
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Eyles, Bunker, Ellis et al. astro-ph/0607306
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Eyles, Bunker, Ellis et al. astro-ph/0607306
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Eyles, Bunker, Ellis et al. astro-ph/0607306
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DAZLE - Dark Ages 'z' Lyman-alpha Explorer
IoA - Richard McMahon, Ian Parry; AAO - Joss Bland-Hawthorne
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JAMES WEBB SPACE TELESCOPE – JAMES WEBB SPACE TELESCOPE –
successor to Hubble (2013+)successor to Hubble (2013+)
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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 L2 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
● 2014 launch
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
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ESA Contributions to JWST● NIRSpec
– ESA Provided– Detector & MEMS Arrays from NASA
● MIRI Optics Module– ESA Member State Consortium– Detector & Cooler/Cryostat from NASA
● Ariane V Launcher (ECA)
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
(closely similar to HST model…)
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NIRSpec IST
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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 1000sec NIRSpec