Large Area Survey of Lyman Alpha Emitters Zheng

Large Area Survey of Lyman Alpha Emitters Zheng Yale Center for Astronomy and Astrophysics Yale/WIYN One Degree Imager Survey Workshop Oct 3 rd, 2009

ODI Survey

Adding an Hα narrow-band filter a lot of Hα related sciences

Searching for z~4. 5 galaxies with prominent Lyα emission Lyman Alpha Emitters (LAEs) Ouchi et al. 2008 Broad bands + narrow-band efficient in selecting LAEs Ouchi et. 2003

ODI survey of LAEs: ~10 x volume of existing narrow-band surveys If Survey Area: 36 sq. deg. Text Hα filter width: 60Å (33 comoving Mpc) Expect to find 4500± 1500 LAEs with LLyα>1042. 5 erg/s (~0. 5 L*) at z~4. 5 LALA Large Area Lyman Alpha survey (Rhoads et al. 2000) SXDS Subaru/XMM-Newton Deep Survey (Ouchi et al. 2008) SDF Subaru Deep Field (Kashikawa et al. 2004) MUSYC Multiwavelength Survey by Yale-Chile (Gawiser et al. 2007)

A LARGE sample of z~4. 5 LAEs • Early galaxy formation • LAE-LBG connection • AGN fraction • Accurate Lyα LF and UV LF • Lyα EW distribution UV luminosity dependence • Clustering of LAEs luminosity dependence, 3 D • A large number of Lyman Alpha Blobs • . . .

A LARGE sample of z~4. 5 LAEs • Early galaxy formation Wang et al. 2009 LALA • LAE-LBG connection • AGN fraction • Accurate Lyα LF and UV LF • Lyα EW distribution UV luminosity dependence • Clustering of LAEs luminosity dependence, 3 D • A large number of Lyman Alpha Blobs • . . . Lyα LF and UV LF, test LAE models

A LARGE sample of z~4. 5 LAEs • Early galaxy formation • LAE-LBG connection deficit of UV bright, high Lyα EW sources • AGN fraction • Accurate Lyα LF and UV LF • Lyα EW distribution Ando et al. 2006 Dust? Age? Observational effect of small volume? UV luminosity dependence • Clustering of LAEs luminosity dependence, 3 D • A large number of Lyman Alpha Blobs • . . . ZZ et al. 2009 Model

A LARGE sample of z~4. 5 LAEs Shimasaku et al. 2004 Subaru Deep Field z=4. 86 sample variance • Early galaxy formation z=4. 79 • LAE-LBG connection • AGN fraction Kavac et al. 2007 • Accurate Lyα LF and UV LF Gawiser et al. 2007 MUSYC z~3. 1 LALA z~4. 5 • Lyα EW distribution UV luminosity dependence • Clustering of LAEs Model luminosity dependence, 3 D • A large number of Lyman Alpha Blobs • . . . Luminosity dependence: LAE-halo connection, environment Anisotropic 3 D correlation function: environment, strong test for LAE models ZZ et al. 2009

ODI survey of LAEs: Observation requirements Use non-optimal observing conditions (e. g. , 1” seeing). [~250 hours] with 2” aperture ~6 hr per field for 5σ detection (LLyα=1042. 5 erg/s) 36 fields, ~100 -200 hours of narrow-band observation, depending on the luminosity threshold we choose.

ODI - Large Area Survey of Redshift Four and Half Lyman Alpha Emitters LA-So-Re-Fa. H-LA ✴ It can be done under non-optimal observing conditions, making a good use of the time. (~200 hrs) ✴ It will have one order of magnitude increase in survey volume. ✴ We expect to detect ~5000 z~4. 5 LAEs and many LABs. ✴ A large sample of LAEs would help answer a lot of questions, r ty! greatly u iyoung galaxies, and provide n enhance our understanding. O of these u t r strong tests of models. po p O