on the doorstep of reionization judd d. bowman california institute of technology august 27, 2009
DESCRIPTION
On the Doorstep of Reionization Judd D. Bowman California Institute of Technology August 27, 2009. Redshifted 21 cm global signal E xperiment to D etect the G lobal E poch of Reionization S ignature (EDGES) EDGES latest results. The History of Hydrogen Gas. Image: Scientific American 2006. - PowerPoint PPT PresentationTRANSCRIPT
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On the Doorstep of ReionizationOn the Doorstep of Reionization
Judd D. BowmanJudd D. BowmanCalifornia Institute of TechnologyCalifornia Institute of Technology
August 27, 2009August 27, 2009
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1.1. Redshifted 21 cm global signalRedshifted 21 cm global signal
2.2. EExperiment to xperiment to DDetect the etect the GGlobal lobal EEpoch poch of Reionization of Reionization SSignature (EDGES)ignature (EDGES)
3.3. EDGES latest resultsEDGES latest results
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The History of Hydrogen Gas
Image: Scientific American 2006
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When did reionization occur? How long did it last?
Furlanetto, Oh, & Briggs 2006
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21 cm Overview
• Spin-flip hyperfine transition of neutral hydrogen=21 cm (rest-frame), =1420 MHzAt z = 6: =1.5 m, = 203 MHzAt z = 15: =3.4 m, = 89 MHz5’9” = 1.75 m z=7.3
• Use CMB as a “backlight”, then brightness temperature is:
mKTTxzzT
S
CMBHIb
1119, 2/1
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KineticCMB
Ionized fraction xi = 1 - xHI
Mean brightness temperature
Spin, TS
Pritchard & Loeb 2008
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Localized bubbles
Mesinger & FurlanettoMesinger & Furlanetto
100 Mpc
z = 10xHI=0.89Ionizing photons escape…
Mesinger & FurlanettoMesinger & Furlanetto
100 Mpc
z = 9xHI=0.74Bubbles grow and merge…
Mesinger & FurlanettoMesinger & Furlanetto
100 Mpc
z = 8.25xHI=0.53
Mesinger & Furlanetto
100 Mpc
z = 7.25xHI=0.18On local scales,a more complex picture
•Reionization fronts•X-ray background•UV backgrounds
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Local patchy evolution… MWA’s objective
Primarily density fluctuations
Early timesEarly times(z > 15)(z > 15)
Late timesLate times (z < 6)(z < 6)
Ionized regions
Furlanetto et al. 2004
5 ar
cmin
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Big
Ban
g! Today
Pritchard & Loeb 2008
100 10 z [redshift]
50
0
-50
-100
T b [m
K]
21 cm global brightness temperature
5001005010 [MHz]
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Modeling reionization history
The main astrophysical parameters are: N_ion
f_esc
f_star
f_lya
f_xray
- Number of ionizing photons per baryon in star formation
- Escape fraction of ionizing photons from galaxies(probably between 0.02 and 0.2)
- Star forming efficiency by mass(uncertain to order of magnitude)
- Number of Ly- photons per baryon in stars (popII)(uncertain to a factor of few)
- X-ray luminosity relative to value extrapolated from Glover and Brand (uncertain to more than order of magnitude)
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Modeling reionization history
Code from J. Pritchard
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Key reionization-era science questions:• When did reionization occur?• What sources were responsible for reionization?
– Properties of ionizing sources; connect galaxy-scale physics to large-scale events by e.g. anti-correlation of 21 cm maps with galaxy formation (near-IR surveys)
• How did the cosmic web evolve?– Topological transition from ionized bubbles into the filamentary web seen in Ly-alpha
forest• How did first quasars form? What were their properties?
– Large HII regions, even after quasars dormant, able to image and constrain emission mechanisms, lifetimes, luminosity function, evolution
• When did first black holes form? What were their properties?– X-ray heating of IGM near galaxies hosting first black holes and supernovae produces
distinctive features in power spectrum (troughs, large amplitudes), z~15• How does radiative feedback affect high-z galaxy formation?
– Directly probe UV and X-ray backgrounds in IGM that regulate star formation and its end products, structure formation, clumping. Soft-UV background z>15 decouples 21 cm spin temperature from CMB
See decadal science review: “Astrophysics from the Highly-Redshifted 21 cm Line”, Furlanetto et al. (2009)
21 cm global vs. local science
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Why global 21 cm?
• Straightforward probe of mean neutral fraction and HI gas temperatures (spin + kinetic)• Star formation history, galaxy evolution, early feedback mechanisms, etc.• Direct constraint on redshift and duration of reionization
• In principle, a simple experiment: No imaging required!– Signal fills aperture of any antenna – a single dipole is sufficient– Ignore ionospheric distortions– Ignore polarized foregrounds
• The only feasible 21 cm probe of the Dark Ages (z>15) IGM for the next decade
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2.Experiment to Detect the
Global Epoch of Reionization Signature(EDGES)
with Alan E. E. Rogers (MIT/Haystack)
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All-sky spectrum
21 cm global signal
All-sky radio spectrum (100-200 MHz)
RFI
Instrument bandpassTotal spectrum components:• Diffuse Galactic (200K to >1000K)
- Synchrotron (99%)- Free-free (1%)
• Sun (variable)• Extragalactic sources (~50K)• CMB (2.7K)• Galactic RRLs (< 1 K)• 21 cm (10 mK)
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EDGES approach• Trade-off: Compared to MWA, we’ve lost extreme difference in spectral
coherence between foreground and signal
• Constrain the derivative of the 21 cm brightness temperature contribution to <1 mK/MHz between 50 and 200 MHz
Furlanetto 2006
Frequency derivative
Mean brightness temperature
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AEER
EDGES block diagram
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“Four-point” antenna
Ground screen
balun
Analog electronics enclosures
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in from antenna
to 2nd stage
calibration source
2nd stage amp
dithering noise source
to digitizer
LNA
switch
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Acqiris DP310: 12-bit, 420 MS/s
bandpass filter/analog electronics
voltage supplyin from
frontend
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RFI trailer
MWA fiber
CSIRO “hut”
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antennaRFI trailer
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Murchison Radio-Astronomy Observatory, Boolardy Station, Western Australia
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Radio Frequency Interference (RFI)
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US radio “pollution”
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West Forks, Maine (Jan 2009)
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Orbcom LEO satellite constellation
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Site selection: Local environment
(< 1 mK)
Antenna beam pattern: CasA (1400 Jy) ~50 K
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Comparison Switch Scheme
• 3-position switch to measure (cycle every 10s):
• Solve for antenna temperature:
(Tcal > TL 300 K, TA 250 K, TR 20 K)
• Limitations: – Total power differences between TL and TA produce residuals– Temporal variations: comparing measurements distinct different times
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Antenna (p2)Internal load (p0)
Noise source (p1)
p1– p0
p2 – p0“Calibrated” sky spectrum
T_A ~ (p2 – p0) / (p1 – p0)
“Calibrated” sky spectrumw/ RFI filtering and integration
The Joy of Calibration
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EDGES: Antenna Impedance Match
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EDGES: Absolute Calibration
Fully calibrated, western Australia
= 2.5 0.1 (3 sigma)Tgal = 237 10 K (3 sigma) @ 150 MHz
Long cable between antenna & LNAsto measure reflection coefficient in situ
Rogers & Bowman 2008
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EDGES: Drift Scans
Rogers & Bowman 2008
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3. EDGES Latest Results
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Measured spectrum
Murchison Radio-Astronomy Observatory (MRO)
Jan 25 – Feb 14, 2009
10 days:- 50 wall-clock hours on sky- ~7 integrated hours
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Integration… rms vs. time w/ baseband removal
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19 mK rms – thermally limited
Green = 100 kHzBlack = 2 MHz
Characterizing progress
Jan/Feb 2009 Bowman et al. 2008
75 mK rms – systematic limited
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Model fitting
• Polynomial term:
• Simple step model of reionization:
2 science parameters: T21 and 0 12 nuisance parameters: an (ACKK!!)
11
0n
nnap
021 HTm
“instantaneous” reionizationT21
to account for impedance mismatch + galactic spectrum
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Model fitting
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Confidence intervals on T21 (as of February 2009)
• Constraints scale linearly with thermal noise• Low-level RFI contamination apparent?
68%
99%
z=13 z=6
< 90 mK
reionization barrier
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Confidence intervals on T21 (as of last night!)
reionization barrier
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21 cm derivative: constraints and forecasts
Current
worst-case anticipated systematic limit
Integrate +improve bandpass
fastest plausible reionization
z=13z=6 z=25
NOT reionization…
absorption
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EDGES status & future work
• Current: – 19 mK rms in measured spectrum– 21 cm step constrained to <90 mK between 7<z<10– 21 cm derivative <40 mK / MHz between 7<z<10 (w/ caveats)
• Aug-Dec 2009: unattended deployment– Cross 30 mK reionization “barrier” to rule out rapid reionization
• The next 3 years (funded by NSF!):– Replace digital backend with Berkeley CASPER open architecture
boards for high throughput, but performance– Redesign antenna to improve impedance match (use lower order
polynomial for continuum removal)– Attempt detection of z>15-25 absorption feature to “set clock” for
interpreting reionization
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HI“Observation of a Line in the
Galactic Radio Spectrum: Radiation from Galactic
Hydrogen at 1,420 Mc./sec”
“Doc” Ewen & Purcell 1951
CMB“A Measurement of Excess Antenna Temperature at
4080 Megacycles per Second”
Penzias & Wilson 1965
EoRFirst detection of reionization?…
Bowman & Rogers????
A final thought…
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The end
This scientific work uses data obtained from the Murchison Radio-astronomy Observatory. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site.
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EDGES: Site Selection
Variations on the Radar Equation…
Scattered sky noise:
Scattered receiver noise:
4G
PP
RG
PP
24
Couple spectral structure in scattering coefficient, , to spectrum
Structure + ripple
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EDGES: Combined xHI Limits
Furlanetto, Oh, & Briggs 2006 Dunkley et al. 2008
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21 cm landscape - scienceInflationary physics and cosmology 30 < z < 200 46 > > 7 MHz• Probe of the matter power spectrum at very small scales ℓ > 104 to 106
• Perturbations to primordial power spectrum and spatial curvature: ns ,
• Neutrino masses, non-Gaussianity, etc.• Baryon collapse
Reionization and the Dark Ages 6 < z < 30 203 > > 46 MHz • Spin and kinetic temperature history of the IGM• Reionization history, Stromgren spheres (quasar proximity zones)• Star formation history / models for ionizing sources• Abundance of mini-halos• Magnetic fields in IGM• Cosmology
Large scale structure/galaxy evolution z < 6 1420 > > 203 MHz • Dark Energy through BAOs, cosmology, neutrino masses, etc.• HI in galaxies/halos, masses of DLAs at z = 3• Indirectly see helium reionization