CIBER: Launched! February 25, 2009 at 3:45 am The First Galaxies, Quasars, and Gamma-Ray Bursts Ian...
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- Slide 1
- CIBER: Launched! February 25, 2009 at 3:45 am The First
Galaxies, Quasars, and Gamma-Ray Bursts Ian Sullivan June 10,
2010
- Slide 2
- CIBER Collaboration James Bock Viktor Hristov Andrew Lange
Louis Levenson Peter Mason Ian Sullivan Michael Zemcov Brian
Keating Tom Renbarger Toshio Matsumoto Shuji Matsuura Kohji Tsumura
Takehiko Wada Dae Hee Lee Uk Won Nam Asantha Cooray
- Slide 3
- Formation of structure and galaxies
- Slide 4
- Trac & Cen 2007 z=9z=8 z=7z=6 Numerical Simulation of
Reionization Orange regions are ionized Around z~10, 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 M=30-300M sun
- Slide 5
- How can you detect the first stars?
- Slide 6
- Has the light from the first stars been detected? TeV blazar
absorption spectra set an upper limit on the EGB, but estimates of
this limit vary The diffuse background (yellow) appears much
brighter than the sum of resolved galaxies (blue)
- Slide 7
- Dual wide-field Imagers = 1.0, 1.6 m =2 2 o x 2 o FOV 7 pixels.
CIBER: The Cosmic Infrared Background Experiment Narrow-Band
Spectrometer = 0.8542 m (Ca II) /=1000 8 o x 8 o FOV 120 pixels
Low-Resolution Spectrometer = 0.7 - 1.8 m. /=20 6 o x 6 o FOV 80
pixels
- Slide 8
- Focal Plane Assemblies Detector Active thermal control stage
Plunger Bi-stable cold shutter The shutter is actuated by two
electromagnets Each assembly is thermally isolated from the optics,
and strapped to the LN2 tank with copper braid
- Slide 9
- Nose cone with parachute Star tracker Guidance system and gas
reservoir Telemetry Experiment cryostat Payload shutter door
- Slide 10
- Slide 11
- 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. 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
- Slide 12
- Imagers Quantity2009 Flight Units I-band Imager (1.0 m)
Responsivity11.5 e- / J/m 2 sr Read noise CDS17e- Dark
Current0.24e-/s I (1 )/pixel 43nW/m 2 sr, 50 s Array1024x1024
HAWAII-1 (HgCdTe) H-band Imager (1.6 m) Responsivity18.7 e- / J/m 2
sr Read noise CDS14e- Dark Current0.28e-/s I (1 )/pixel 128nW/m 2
sr, 50 s Array1024x1024 Hawaii-1 (HgCdTe) Measuring fluctuations in
the near-Infrared Background
- Slide 13
- 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
- Slide 14
- Low-Resolution Spectrometer (LRS) Quantity2009 Flight Units
Low-Resolution Spectrometer Responsivity10-65 e- / J/m 2 sr Read
noise CDS25e- Dark Current0.5e-/s I (1 )/pixel 10-30nW/m 2 sr, 50 s
Number of slits5 Array256x256 PICNIC (HgCdTe) Measuring the
absolute brightness of the near-Infrared Background
- Slide 15
- LRS: The absolute brightness of the Near Infrared Background
Low-Resolution Spectrometer sensitivity after 50s The LRS will be
the first instrument to span the entire 0.7 1.8 m range
- Slide 16
- 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
- Slide 17
- Narrow-Band Spectrometer (NBS) Measuring the absolute
brightness of the Zodiacal Light Narrow-band filter 2 1 0
Quantity2009 Flight Units Narrow-Band Spectrometer Responsivity2.3
e- / J/m 2 sr Read noise CDS28e- Dark Current