old massive galaxies in the early universe tell better stories about reionization
DESCRIPTION
Old Massive Galaxies in the Early Universe tell better Stories about Reionization. Nino Panagia (STScI, INAF, SN Ltd). Mostly based on work done in collaboration with: (in inverse alphabetical order ) Tommy Wiklind Massimo Stiavelli Bahram Mobasher Mike Fall Et Al. - PowerPoint PPT PresentationTRANSCRIPT
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15 March 2006 The End of the Dark Ages 1
Old Massive Galaxies
in the Early Universe
tell better Stories
about Reionization
Nino Panagia (STScI, INAF, SN Ltd)
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15 March 2006 The End of the Dark Ages 2
Mostly based on work done
in collaboration with: (in inverse alphabetical order)
Tommy Wiklind
Massimo Stiavelli
Bahram Mobasher
Mike Fall
Et Al.
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15 March 2006 The End of the Dark Ages 3
We know that the Universe is not quite ionized
at redshift z=6.28
Becker et al. (2001)
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15 March 2006 The End of the Dark Ages 4
Becker et al (2001):The full story
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The Principles of Reionization (RI)
• Reionization requires sources of Lyman continuum photons
• Reionization depends primarily on the UV output of the RI sources integrated over time
• Reionization is a function of the UV photon escape fraction, f, from the RI sources and the clumpiness of the IGM
<Q> = <MHI> × f –1 × B(z1,z2,C) Ly-c photons HI mass =
HI×Volumeescapefraction
photons neededper ionization
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The effect of the IGM clumping on Reionization
[Stiavelli, Fall & Panagia 2004a]
Clumping factor C = <n2H>/<nH>2
Eff
ecti
ve n
umbe
r of
pho
tons
to io
nize
an
atom
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15 March 2006 The End of the Dark Ages 7
Recognizing the Reionization Agents
• (Young Bright) Galaxies at z>6.5 are doing it
• (Evolved Massive) Galaxies at z<6.5 have done it
• Together they define the process of Reionization
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32 30 28 26 24 32 30 28 26 24 mAB(rest=1400Å)
Reionization constraints from HUDF observationsStiavelli, Fall & Panagia (2004b)
T=100,000K (Z=0) T=50,000K (Z=Z/100)
The blue line refers to UDF objects selected by i-z>2, the red one to i-z>1.3.
The galaxies that may be ionizing NOW…
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z=2.5-3.4
HUDF-JD2, a Balmer Break Galaxy prototypeA galaxy that did it in the past?
[Mobasher et al. 2005]
z = 6.5M = 61011 M
Observed [m] 0.5 1 2 5 10
Rest-frame [m] 0.1 0.2 0.4 0.8
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Properties of HUDF-JD2[Mobasher et al 2005, Panagia et al 2005]
Massive M/M = 6 × 1011
Bright L/L = 1012
Evolved Age > 350-650 Myr zform > 9
Ionizing Q ~ 4 × 1072 Ly-c photons
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HUDF-JD2:An Old Galaxy
that did a LOT
eff: Ratio of the time averaged Lyman continuum
photon flux to the present UV flux
Age
Model includingchemical evolution
[Panagia et al 2005]
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HUDF-JD2
dereddenedcompanions
Enough to re-ionizeits region of Universe?
By itself only if high escape fractionand low clumping
Easily if invisible companions with a reasonable LF are present
Panagia et al. 2005
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HUDF-JD2: A summary
• Massive, luminous, protypical Balmer-break galaxy
• It has had an important impact (>20%) on the reionization of the IGM starting a z~15
• With the “help” of fainter companions distributed according to an =1.6 Schechter LF it may account for the whole effect
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Is HUDF-JD2 unique?
• Tommy Wiklind answered this question: “not quite”
• Actually, combining deep HST and Spitzer multi-band photometry one finds about one bright BBG per 10 square-arcmin field
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Re-Ionization Balance - I
• UV output from BBGs in the Chandra Deep Field South Qtot = 4.2 × 1073 f Lyman-continuum photons
• H-atoms in a volume in the redshift interval 7-15
NH = 1.2 × 1073 atoms
• If the detected BBGs are the only UV sources in the field
B/f = 3.5
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15 March 2006 The End of the Dark Ages 17
The effect of the IGM clumping on Reionization
[Stiavelli, Fall & Panagia 2004a]
Clumping factor C = <n2H>/<nH>2
Eff
ecti
ve n
umbe
r of
pho
tons
to io
nize
an
atom
![Page 17: Old Massive Galaxies in the Early Universe tell better Stories about Reionization](https://reader036.vdocument.in/reader036/viewer/2022062519/568150f7550346895dbf12e0/html5/thumbnails/17.jpg)
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Re-Ionization Balance - II• With a clumping C > 10 B > 2 f > 0.6 unlikely!?
• The IMF may be top-heavy too easy!!!
• Additional, fainter, undetected galaxies contribute to the reionization possible
• In this case, with C>10 and f<0.2, the fainter companions should provide an additional ~200% of ionizing radiation.
• This corresponds to a Schechter luminosity function steeper than =1.3 quite reasonable
• Detecting and studying the fainter companions is not easy with current telescopes but it will feasible with JWST.
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Conclusions
Big
Ban
g
H II
z ~
6-1
0
“Dark Ages”
TIGM ~ 4z K
z ~
10
3 z ~
∞ re
com
bin
ati
on
t z
H I
TIGM ~ 104 K
normal galaxy
S1Here Now
primordial galaxy
Hubble Deep Field
Hubble Ultra Deep Field
end of reionization
JWSTHST
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15 March 2006 The End of the Dark Ages 20
Conclusions
• Balmer-Break Galaxies (BBG) are important for the reionization of the IGM starting at z~15 or higher
• With the help of fainter companions they have the potential of ionizing the IGM entirely
• JWST is needed to detect and study the population of “reionizers”
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THE END