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The Near Infrared Background Excess and Star Formation in the HUDF

The Near Infrared Background Excess and Star Formation in the HUDF. Rodger Thompson Steward Observatory University of Arizona. Blameless Collaborators. Mark Dickinson Daniel Eisenstein Xiaohui Fan Garth Illingworth Rob Kennicutt Marcia Rieke. The near infrared background excess

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The Near Infrared Background Excess and Star Formation in the HUDF

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  1. The Near Infrared Background Excess and Star Formation in the HUDF Rodger Thompson Steward Observatory University of Arizona

  2. Blameless Collaborators • Mark Dickinson • Daniel Eisenstein • Xiaohui Fan • Garth Illingworth • Rob Kennicutt • Marcia Rieke

  3. The near infrared background excess The lack thereof Star formation history of the HUDF Topics

  4. Near Infrared Background Excess • Claims of a Near InfraRed Background (NIRBE) of ~70 nW m-2 sr-1, not due to known galaxies, stars or zodiacal light, that peaks at 1.4-1.6 mm. • Resolved objects in the NUDF and NHDF contribute 6-7 nW m-2 sr-1, a factor of 10 below the claimed background. • Fluctuations in deep 2MASS images claimed as evidence for a population of very high redshift (10-15) Pop. III stars. (Kashlinsky et al. 2006)

  5. Implications of the NIRB • Most popular model for the NIRB is the light from the high redshift Pop. III stars that reionized the universe. • Requires that the total number of baryons turned into stars in the first 3% of the age of the universe be greater than or equal to the total number of baryons converted to stars in the remaining 97%. • The metals produced by this conversion must be hidden in black holes. • There must be no x-ray producing accretion onto the black holes. • The NIRB must not interact with TeV emission from distant blazars.

  6. Fluctuation Analysis of the NICMOS UDF F160W Image

  7. Results of the Fluctuation Analysis • The fluctuations observed in the 2MASS field can be completely accounted for by the redshift 0-7 galaxies such as those observed in the NUDF • There is no need for an excess population of high redshift Pop.III stars to account for the fluctuations • Fluctuations have been removed as evidence for a NIRBE at 1.6 mm

  8. The IRTS NIRBE • Wide field of view spectrometer • Aperture almost 17 times the size of the NUDF • Zodiacal light and contributions from sources determined from models • After subtraction of modeled components, 70 out of 330 nW m-2 sr-1 remain and is attributed to a NIRBE

  9. The NIRBE According to IRTS

  10. IRTS vs NICMOS FLUX ALLOCATIONS All fluxes in nW m-2 Sr-1 Observed Modeled

  11. Differences • The zodiacal component determined by medianed images in the NUDF exceeds the IRTS modeled component by 100 nW m-2 sr-1. • Dwek et al. 2006 point out that the IRTS spectrum is better fit by a zodiacal spectrum than a high z Pop.III spectrum. • The IRTS NIRBE is most likely due to an under estimate of the zodiacal light component by the model.

  12. Caveats • A NIRBE component that is flat on scales of greater than 100” would be mistaken for zodiacal light in our reduction. • At odds with CMB predictions • A NIRBE component that is clumped on the order of several arc minutes could be missed by our two small fields. • Archival proposal to check other fields • However the light in a NIRB can not be distributed in the same manner as the light from baryonic matter at redshifts of 6 and less.

  13. Scattering of UV Light at High Z • Emission from massive Pop. III stars will be primarily shortward of 912 Å and will be degraded into Ly a photons. • In a metal and dust free gas they can scatter to large distances and become smooth on scales of 10-100 arc seconds.

  14. Smoothing on 10 arc second Scales Portion of the NUDF at 1.6 mm Same portion with background in 10” gaussians

  15. Star Formation History in the NICMOS UDF

  16. The F775W Mag. vs Redshift AGN

  17. Star Formation Rates • Star formation rate determined from the rest frame 1500 Å flux via the Madau relation. • The flux is measured from the selected SED without extinction to produce an extinction corrected SFR.

  18. Star Formation Intensity Distribution • The star formation intensity x is the SFR in M per year per proper square kpc. • The distribution function h(x) is the sum of all proper areas in an x interval, divided by that interval and divided by the comoving volume defined by the field and redshift interval.* • Under this definition SFR is the first moment of h(x); SFR = ∫x h(x) dx * Lanzetta et al. 1999, ASP Conf. Ser. 191, 223

  19. Star Formation Density Redshift = 1 95% complete 60% complete Log(h(x)) Starburst Log Star Formation Intensity x in M per year per kpc2 About 80% of the stars are formed in a “starburst region”

  20. Application of the Distribution • The SFR is calculated for every pixel that is part of a galaxy. • Assumes a uniform SED and extinction within a galaxy • Assumes that the rest frame 1500 Å light is distributed in the same way as the observed flux in the ACS F775W band.

  21. The Observed h(x)

  22. Star Formation History of the NUDF

  23. Comparison with the NHDF

  24. Conclusions • Fluctuations have been removed as evidence for a NIRBE at 1.6 mm. • The IRTS NIRBE is probably zodiacal flux. • Any NIRBE must be either maximally flat or maximally clumped. • The star formation history of the universe is roughly constant from z=1-6. • The vast majority of star formation occurs in a minority of galaxies at any one time.

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