CIBER: Launched!

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CIBER Launched! February 25, 2009 at 345 am
The First Galaxies, Quasars, and Gamma-Ray
Bursts Ian Sullivan June 10, 2010
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CIBER Collaboration
James Bock Viktor Hristov Andrew Lange Louis
Levenson Peter Mason Ian Sullivan Michael Zemcov
Asantha Cooray
Brian Keating Tom Renbarger
Toshio Matsumoto Shuji Matsuura Kohji
Tsumura Takehiko Wada
Dae Hee Lee Uk Won Nam
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Formation of structure and galaxies
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Numerical Simulation of Reionization
Around z10, UV radiation from the first stars
and proto-galaxies caused the intergalactic
medium of neutral Hydrogen to become
ionized. Current predictions are that these stars
had mass M30-300Msun
z9
z8
Trac Cen 2007
z7
z6
Orange regions are ionized
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How can you detect the first stars?
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Has the light from the first stars been detected?
The diffuse background (yellow) appears much
brighter than the sum of resolved galaxies (blue)
TeV blazar absorption spectra set an upper limit
on the EGB, but estimates of this limit vary
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CIBER The Cosmic Infrared Background Experiment
Dual wide-field Imagers ? 1.0, 1.6 µm ?/??2 2o
x 2o FOV 7 pixels.
Low-Resolution Spectrometer ? 0.7 - 1.8
µm. ?/??20 6o x 6o FOV 80 pixels
Narrow-Band Spectrometer ? 0.8542 µm (Ca II)
?/??1000 8o x 8o FOV 120 pixels
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Focal Plane Assemblies
Bi-stable cold shutter
The shutter is actuated by two electromagnets
Detector
Plunger
Active thermal control stage
Each assembly is thermally isolated from the
optics, and strapped to the LN2 tank with copper
braid
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Nose cone with parachute
Guidance system and gas reservoir
Telemetry
Star tracker
Experiment cryostat
Payload shutter door
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CIBERs flight

• Apogee is strongly sensitive to payload mass
  CIBER achieved 335km with a 1060lb payload.
• Total flight time was 15 minutes, including 6
  minutes of observations

• We observed 4 cosmological fields, 2
  foreground assessment fields, and the star Vega
  for calibration of the NBS
• The cosmological fields are chosen to enjoy
  exceptional ancillary coverage to minimize point
  source contamination.

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Imagers
Measuring fluctuations in the near-Infrared
Background
Quantity 2009 Flight Units
I-band Imager (1.0 mm) I-band Imager (1.0 mm) I-band Imager (1.0 mm)
Responsivity 11.5 e- / mJ/m2sr
Read noise CDS 17 e-
Dark Current 0.24 e-/s
dnIn (1s)/pixel 43 nW/m2sr, 50 s
Array 1024x1024 HAWAII-1 (HgCdTe)
H-band Imager (1.6 mm) H-band Imager (1.6 mm) H-band Imager (1.6 mm)
Responsivity 18.7 e- / mJ/m2sr
Read noise CDS 14 e-
Dark Current 0.28 e-/s
dnIn (1s)/pixel 128 nW/m2sr, 50 s
Array 1024x1024 Hawaii-1 (HgCdTe)
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Imagers Fluctuations in the Near-Infrared
Background
Sources from reionization should have a distinct
spatial power spectrum However, local galaxies
dominate until they are removed to a low level
Science window
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Low-Resolution Spectrometer (LRS)
Measuring the absolute brightness of the
near-Infrared Background
Quantity 2009 Flight Units
Low-Resolution Spectrometer Low-Resolution Spectrometer Low-Resolution Spectrometer
Responsivity 10-65 e- / mJ/m2sr
Read noise CDS 25 e-
Dark Current 0.5 e-/s
dnIn (1s)/pixel 10-30 nW/m2sr, 50 s
Number of slits 5
Array 256x256 PICNIC (HgCdTe)
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LRS The absolute brightness of the Near Infrared
Background
The LRS will be the first instrument to span the
entire 0.7 1.8 µm range
Low-Resolution Spectrometer sensitivity after 50s
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Zodiacal Light spectrum with the LRS

• By itself, the LRS measures the shape of the
  spectrum of the Zodiacal Light
• Absolute calibration can be further improved in
  the future with the NBS

Tsumura et al 2010
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Narrow-Band Spectrometer (NBS)
Measuring the absolute brightness of the Zodiacal
Light
Quantity 2009 Flight Units
Narrow-Band Spectrometer Narrow-Band Spectrometer Narrow-Band Spectrometer
Responsivity 2.3 e- / mJ/m2sr
Read noise CDS 28 e-
Dark Current lt0.6 e-/s
dnIn (1s)/pixel 87 nW/m2sr, 50 s
Resolution 1220 l/Dl
Array 256x256 PICNIC (HgCdTe)
?
2
?
Narrow-band filter
1
?
0
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NBS Absolute brightness of the Zodiacal Light
l8532-8536nm
l8536-8540nm

• NBS design uses a narrow band filter tuned to a
  reflected CaII solar line to measure absolute
  intensity of ZL in each field.
• The wavelength across the array varies as ?o
  ?i cos ?

l8540-8544nm
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Modifications

• All hardware modifications are complete for the
  second flight. These include
• New fixed baffles with Laser Black
• Extended radiation shield above
• front plate
• New shutter door black liner
• All instruments moved inboard ¼
• Pop-up baffles for all instruments
• New calibration lamp for the NBS
• Strengthened suspension

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Five more flights to come

• July 2010
• February 2011
• July 2011 four-stage non-recoverable flight
• Summer 2013 first flight of CIBER2
• Spring 2014

CIBER2