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Connections between Lyman Break Galaxies and Lyman Alpha Emitters at High Redshift

Connections between Lyman Break Galaxies and Lyman Alpha Emitters at High Redshift. Naveen Reddy (Hubble Fellow, NOAO). C. Steidel ( Caltech ), Arjun Dey (NOAO), Moire Prescott (Steward). Understanding Lyman Alpha Emitters at High Redshift, Heidelberg, Germany, 08 September 2008.

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Connections between Lyman Break Galaxies and Lyman Alpha Emitters at High Redshift

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  1. Connections between Lyman Break Galaxies and Lyman Alpha Emitters at High Redshift Naveen Reddy (Hubble Fellow, NOAO) C. Steidel ( Caltech), Arjun Dey (NOAO), Moire Prescott (Steward) Understanding Lyman Alpha Emitters at High Redshift, Heidelberg, Germany, 08 September 2008

  2. Lyman Alpha Emitters in Continuum-Selected Samples • Number density of LAEs as a function of UV magnitude to compute the LF • Inferring the Modulation of W(Ly) by the selection criteria

  3. Simulations to Quantify the Modulation of W(Ly) by Selection Criteria Reddy et al 2008a

  4. Simulations to Quantify the Modulation of W(Ly) by Selection Criteria Reddy et al 2008a

  5. Simulations to Quantify the Modulation of W(Ly) by Selection Criteria Reddy et al 2008a

  6. Simulations to Quantify the Modulation of W(Ly) by Selection Criteria Reddy et al 2008a

  7. Excess at z~3 relative to z~2 Evolution in the High W(Ly) Tail from z~3 to z~2 Reddy & Steidel 2008

  8. z=2: N(0.07L*<L<L*)~0.98N(>0.07L*) (0.07L*<L<L*)~0.84(>0.07L*) z=3: N(0.1L*<L<L*)~0.97N(>0.1L*) (0.1L*<L<L*)~0.82(>0.1L*) 0.1L* Advantages of our analysis • > 2000 spectroscopic redshifts at the bright-end • modeling of systematic effects (Ly; reddening) • maximum-likelihood constraints on LF that are robust to non-uniform sources of scatter • - 31000 LBGs in 31 independent fields Results on the UV LF at z~2-3 0.07L* Steep faint-end slope of  ~ -1.73, similar to that measured at z~4-6 Reddy & Steidel 2008

  9. LAEs at Low Redshift (z~1.9) Followup Spectroscopy with Keck No Contamination from OII Emitters

  10. LAEs at Low Redshift (z~1.9) • comparisons with continuum-selected samples • larger dynamic range in galaxy properties at lower redshift • accessibility of objects to multi-wavelength analysis LAEs likely trace the population of faint LBGs  fair comparisons should be restricted to *SAME* magnitude range

  11. Evolution in the Number Density of LAEs

  12. Conclusions Constraints on the UV LF at z~2-3: • simulations imply redshift evolution in number density of LAEs (larger at z~3 than z~2), robust to selection effects induced by continuum selection • UV LF evolves strongly between z~6 and z~2 • very steep faint-end slope of theUV LF of  ~ -1.73 at z~2 and z~3, similar to those derived at higher redshifts (z~4-6) • New Survey of z~1.9 LAEs: • preliminary result: strong evolution in the number density of L(Ly) > 1e42 ergs/s between z>3 and z~1.9

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