From Avi Loeb reionization. Quest to the Highest Redshift.
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Transcript of From Avi Loeb reionization. Quest to the Highest Redshift.
![Page 1: From Avi Loeb reionization. Quest to the Highest Redshift.](https://reader034.fdocuments.net/reader034/viewer/2022051417/5697bfeb1a28abf838cb8272/html5/thumbnails/1.jpg)
From Avi Loeb
reionization
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Quest to the Highest Redshift
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Difficulties in finding high-z galaxies and quasars
• Faint: m-M ~ 47, even the brightest galaxies need Keck/HST; only the brightest quasars can be detected with large surveys
• Rare: e.g. z~6 quasar surface density is one per 500 sq. deg
• Red: all spectral features shifted to the red part of the spectrum, Ly alpha at 1216x7 = 8500 A, where:– sky is very bright– CCD is very insensitive
• Low surface brightness: SB ~ (1+z)-4 = 1/2400
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High-redshift Galaxies/Quasars Searching Technique
• Lyman break technique– Broad-band optical colors– Quasars – 80’s; galaxies – 90’s
• Narrow-band imaging (Lyman alpha emitter)– Galaxies – 80’s
• Slitless Spectroscopy – Wide-area spectroscopy – Looking for strong emission line– Quasars – 70’s; galaxies – now
• Cross-identification with other wavelength– Radio: quasars – 60’s; galaxies – 60’s– X-ray: quasars – 80’s– Submillimeter: galaxies – 90’s
• Serendipity (a.k.s. luck…)– If you are Hy Spinrad (Berkeley) or his student, then it will work…
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So how far could each of these techniques go?
• Lyman break:– Quasars: 6.4– Galaxies: 6.6; maybe 10?
• Narrow band imaging – Galaxies: 7.0
• Slitless spectroscopy– Quasars: 4.7– Galaxies: 6.5
• Cross-identification– Quasars: 6.1 (radio)– Galaxies: 5.2 (radio)
• Luck:– Quasars: 4.3– Galaxies: 5.5
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Lyman Break Galaxies I:Spectrum of high-z galaxies
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Lyman break galaxies II:Colors of LBG
Key: The presence of absorption at lambda < 1216A in the rest-frame UV of the galaxy produces a BREAK in the observed high-z galaxy spectrum: LYMAN BREAKby looking for “drop-out” objects in broad-band colors as a result of the Lyman break, we can find high-redshift galaxies!
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Lyman break galaxies III:color selection
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Narrow-band Imaging
• Idea:– Young galaxies are dominated by young stars and star
forming regions
– With strong HII regions and strong Ly alpha emission lines
– Looking for Lyman alpha line by looking for enhancement in the flux within narrow filters
– High success rate, but still needs follow-up spectroscopy to eliminate contaminants: strong emission lines other than Ly-alpha
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Matching towards high-z
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The most distant galaxy known to date z=6.98
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Even higher redshifts
Z~10?
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The new highest redshift record?
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Lyman Emitter at z~10?
• Keck blind spectroscopic survey along critical lines of high-z clusters
– Six promising Ly emitter candidates at z=8.7 - 10.2
– Limit of ground-based search; extremely difficult to confirm spectroscopically
Stark, Ellis et al.
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The history of star formation in the universe
• Estimating star formation in a galaxy– Roughly proportional to the UV flux UV flux comes
from young, hot stars
– Roughly proportional to the Lyman alpha flux Lyman alpha emission comes from HII regions around young, hot stars
• Madau plot:– Star formation volume density (including all galaxies)
as a function of redshift
– Rapid increase from z=0 to 1.5
– Slow decline at z>2
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46,420 Quasars from the SDSS Data Release Three
wavelength4000 A 9000 A
reds
hift
0
1
2
3
5
Ly
CIV
CIIIMgII
HOIII
FeII
FeII
Ly forest
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30 at z>660 at z>5.5>100 at z>5
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Quasar Evolution at z~6
• Strong density evolution
– Density declines by a factor of ~40 from between z~2.5 and z~6
• Black hole mass measurements
– MBH~109-10 Msun
– Mhalo ~ 1012-13 Msun
– rare, 5-6 sigma peaks at z~6 (density of 1 per Gpc3)
• Quasars accreting at maximum rate
– Quasar luminosity consistent with Eddington limit
Fan et al. 2006, 2010
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Quest to the Highest Redshift
080913
050904
090423
000131
970228
GRBs
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z=8.2 GRB
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A brief cosmic historyBig Bang: the universe filled
with hot gas
Cosmic Dark Age: no light no star, no quasar
First light: the first galaxies and quasars in the universeCosmic Renaissance: universe lit up
by young galaxies and quasars “reionization” completed, the universe is transpartent and the dark ages ended
today
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A brief cosmic historyBig Bang: the universe filled
with hot gas
Cosmic Dark Age: no light no star, no quasar
First light: the first galaxies and quasars in the universeCosmic Renaissance: universe lit up
by young galaxies and quasars “reionization” completed, the universe is transpartent and the dark ages ended
today
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When did 1-sigma peak collapse
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Cooling Rate of Primordial Gas
n=0.045 cm^-3
Atomic cooling
H_2 cooling
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1-sigma
2-sigma
3-sigma
Atomic cooling
H_2 cooling
2-sigma
Collapse Redshift of Halos
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Binding Energy of Dark Matter Halos
1-sigma 2-sigma
3-sigma
Supernova
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Emergence of the First Star Clusters
molecular hydrogen
Yoshida et al. 2003
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Z=30
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First star simulation
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Fate of first stars
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Massive Accretion by Metal-Free Proto-StarsMassive Accretion by Metal-Free Proto-Stars
25pc 0.5pc
Bromm & Loeb
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Simulation of a Hypernova Explosion
100 pc
Heavy elements
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The end of dark ages: Movie
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Reionization
• After recombination, the universe was neutral• At z~20 – 30, the first generation galaxies and
mini quasars formed• At z~6 – 15, the UV radiation from the first
generation objects ionized most of the HI in the universe– The neutral fraction of the universe changed from 1 to
10^-5 (phase transition in ionization state)– The temperature of the IGM electrons changed from
CMB temperature to 10^4 (phase transition accompanied by temperature change)
– IGM becomes transparent to UV radiation, the universe is like a giant HII region (temperature change accompanied by opacity change)
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Gnedin 2000
Neutral fraction Light background
Gas density
Gas temperature
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Three stages
Pre-overlap
Overlap
Post-overlap
From Haiman & Loeb