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 für Astrophysik

Cosmic Backgrounds ? ? ữ -ray Near-IR X-ray Mid-IR UV Far-IR Optical CMB ? Radio Cross-correlations

Galaxy Counts Extragalactic Background Light Direct measurements TeV blazars IR Fluctuations Resolved galaxies UV Optical NIR mid-IR

NIRB Fluctuations F ( θ ) = h F i + δ F θ NIR background fluctuations probe populations that are inaccessible to direct detection

NIRB Fluctuations l = 1000 Kashlinsky et al. 2012 clustering excess! HST/NICMOS Spitzer/IRAC Akari/IRC

Millennium 1.4 deg Guo et al. 2011 Henriques et al. 2012

Cosmic X-ray background Chandra Spitzer Cappelluti et al. 2013

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)

Helgason+2014 Stars at high-z: ✓ ◆ ✓ 1 + z ◆ F CIB η ? & 5% 1 nW m − 2 sr − 1 10 Black Holes at high-z: ✓ ◆ ✓ 1 + z ◆ F CIB ρ BH & 10 5 M � Mpc � 3 1 nW m � 2 sr � 1 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 10 14 M o down to 10 10 M o , creating light where there is none.

Helgason & Kashlinsky 2012 HST/WFC3 Spitzer CIBER Akari Fermi JWST 2018-20 CIB fluctuations probe populations that are inaccessible to direct detection

High-z tomography with JWST NIRCAM P 22 − ( P 12 ) 2 ✓ ◆ P ( z 2 ) = + contam P 11 DATA

LIBRAE Looking at the near-Infrared Background Radiation Anisotropies with Euclid • Wide band VIS & NISP instruments covering 0.5-2 μ m • Wide survey: • 20,000 deg 2 , 24 mag (5 σ ) • Deep survey: • 40 deg 2 , 26 mag (5 σ ) 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

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

LIBRAE Looking at the near-Infrared Background Radiation Anisotropies with Euclid Cross Correlations Secondary CMB? 21 cm signal: LOFAR, SKA CIB vs CXB: Chandra, eROSITA See Fernandez et al. 2013 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

Near-IR Background Workshop 2015 MPA, June 1-3