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CIBER: Launched! February 25, 2009 at 3:45 am The First Galaxies, Quasars, and Gamma-Ray Bursts Ian Sullivan June 10, 2010.

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Presentation on theme: "CIBER: Launched! February 25, 2009 at 3:45 am The First Galaxies, Quasars, and Gamma-Ray Bursts Ian Sullivan June 10, 2010."— Presentation transcript:

1 CIBER: Launched! February 25, 2009 at 3:45 am The First Galaxies, Quasars, and Gamma-Ray Bursts Ian Sullivan June 10, 2010

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

3 Formation of structure and galaxies

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

5 How can you detect the first stars?

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)

7 Dual wide-field Imagers λ= 1.0, 1.6 μm λ  Δλ=2 2 o x 2 o FOV 7” pixels. CIBER: The Cosmic Infrared Background Experiment Narrow-Band Spectrometer λ= μm (Ca II) λ/Δλ= o x 8 o FOV 120” pixels Low-Resolution Spectrometer λ= μm. λ/Δλ=20 6 o x 6 o FOV 80” pixels

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

9 Nose cone with parachute Star tracker Guidance system and gas reservoir Telemetry Experiment cryostat Payload shutter door

10

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. CIBER’s 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

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

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

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

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 µm range

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

17 Narrow-Band Spectrometer (NBS) Measuring the absolute brightness of the Zodiacal Light Narrow-band filter λ λ λ Quantity2009 Flight Units Narrow-Band Spectrometer Responsivity2.3 e- /  J/m 2 sr Read noise CDS28e- Dark Current<0.6e-/s  I (1  )/pixel 87nW/m 2 sr, 50 s Resolution1220  Array256x256 PICNIC (HgCdTe)

18 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  = nm = nm = nm NBS: Absolute brightness of the Zodiacal Light

19 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

20 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


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