SLIDE 1
Kari Helgason
- Max Planck Institute for Astrophysics
From the Resolved to the Unresolved: The Role of Cosmic Backgrounds in Future Surveys
Max Planck Institut für Astrophysik
Kari Helgason Max Planck Institute for Astrophysics Max Planck - - PowerPoint PPT Presentation
Kari Helgason Max Planck Institute for Astrophysics Max Planck - - PowerPoint PPT Presentation
From the Resolved to the Unresolved: The Role of Cosmic Backgrounds in Future Surveys Kari Helgason Max Planck Institute for Astrophysics Max Planck Institut fr Astrophysik Cosmic Backgrounds ? ? -ray Near-IR X-ray Mid-IR UV
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SLIDE 3
Galaxy Counts Resolved galaxies Direct measurements IR Fluctuations
Extragalactic Background Light
TeV blazars
UV Optical NIR mid-IR
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F(θ) = hFi + δFθ
NIR background fluctuations probe populations that are inaccessible to direct detection
NIRB Fluctuations
SLIDE 5
NIRB Fluctuations
Kashlinsky et al. 2012
clustering excess!
l = 1000
HST/NICMOS Spitzer/IRAC Akari/IRC
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Millennium
1.4 deg
Guo et al. 2011 Henriques et al. 2012
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Cosmic X-ray background
Chandra Spitzer
Cappelluti et al. 2013
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What could it be?
- Zodiacal Light
- Galactic Cirrus
- Instrumental effects
- Unknown systematics
- Known galaxy populations (Helgason et al. 2012)
- First Stars and Black Holes? (Kashlinsky 2005,2012)
- Intrahalo Light? (Cooray et al. 2012, Zemcov et al. 2014)
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Helgason+2014
η? & 5% ✓ FCIB 1 nW m−2sr−1 ◆ ✓1 + z 10 ◆
ρBH & 105MMpc3 ✓ FCIB 1 nW m2sr1 ◆ ✓1 + z 10 ◆
Stars at high-z:
Black Holes at high-z:
SLIDE 10
Intrahalo Light?
- No correlation with Hubble ACS sources <28 mag
- No correlation with mask or extended wings of removed galaxies
- How to produce correlation with X-rays?
- Requires half of all stars to live outside galaxies
- L/M ratio is extrapolated from 1014Mo down to 1010Mo, creating light where
there is none.
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Helgason & Kashlinsky 2012
HST/WFC3 Spitzer CIBER Akari Fermi
JWST 2018-20
CIB fluctuations probe populations that are inaccessible to direct detection
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High-z tomography with JWST
P(z2) = ✓ P22 − (P12)2 P11 ◆
DATA
+ contam
NIRCAM
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- Wide band VIS & NISP instruments covering 0.5-2μm
- Wide survey:
- 20,000 deg2, 24 mag (5σ)
- Deep survey:
- 40 deg2, 26 mag (5σ)
LIBRAE
Looking at the near-Infrared Background Radiation Anisotropies with Euclid
Euclid
- A. Kashlinsky (PI), R. Arendt, J. Mather, H. Moseley, K. Helgason, G. Fazio, M. Ashby,
- N. Cappelluti, A. Ferrara, G. Hasinger, V. Bromm, F. Atrio-Barandela, J. Staguhn
SLIDE 14
LIBRAE
Looking at the near-Infrared Background Radiation Anisotropies with Euclid
Spectral Signatures Spatial Signatures
- A. Kashlinsky (PI), R. Arendt, J. Mather, H. Moseley, K. Helgason, G. Fazio, M. Ashby,
- N. Cappelluti, A. Ferrara, G. Hasinger, V. Bromm, F. Atrio-Barandela, J. Staguhn
SLIDE 15
LIBRAE
Looking at the near-Infrared Background Radiation Anisotropies with Euclid
- A. Kashlinsky (PI), R. Arendt, J. Mather, H. Moseley, K. Helgason, G. Fazio, M. Ashby,
- N. Cappelluti, A. Ferrara, G. Hasinger, V. Bromm, F. Atrio-Barandela, J. Staguhn
CIB vs CXB: Chandra, eROSITA 21 cm signal: LOFAR, SKA Secondary CMB?
Cross Correlations
See Fernandez et al. 2013
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