Observations and Inferences from Lyman-α Emitters
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1 Observations and Inferences from Lyman-α Emitters Christopher J. White 6 March 2013
2 Outline 1 What Are Lyα Emitters? 2 How Are They Observed? 3 Results and Inferences 4 HSC 5 Conclusion
3 The Lyα Line n = 2 1 transition of H λ = 1216 Å Strongly scattered by neutral H Red-skewed in distant sources
4 Relation to Early Galaxies Lyman Alpha Emitters (LAEs) observed Need hot stars star forming Blocked by dust low-metallicity Seen for z 2 7 Primordial?
5 Narrowband Photometry Use narrowband filter Tune to Lyα at chosen z Contamination? [O II] [O III] Hα Ouchi 2008
6 Narrowband Photometry Use narrowband filter Tune to Lyα at chosen z Contamination? [O II] [O III] Hα Gronwall 2007
7 Spectroscopic Followup Ouchi 2008
8 Spectroscopic Followup AGN?: high-ionization lines 10% AGN No He II: not primordial
9 Spectroscopic Followup Ouchi 2008
10 Blank-Field Spectroscopy Multiple slits on instrument Smaller samples Good for faint objects Faintness problem for followup/confirmation Martin 2008
11 Blank-Field Spectroscopy Multiple slits on instrument Smaller samples Good for faint objects Faintness problem for followup/confirmation Martin 2008
12 The Data So Far 1 2 thousand observed Specific redshift windows, 2 z 7 Small studies: statistics Changing fraction of population z = 5: outnumber LBGs 4 : 1 Disappearing by z = 2
13 LALA Large Area Lyman Alpha survey 0.72 deg < z < 4.57 Too many large EWs Zero metallicity? Top-heavy IMF? Episodic star formation? Malhotra 2002
14 ECDF-S Extended Chandra Deep Field 0.28 deg 2 z = 3.1 EWs not too large Signs of dust Gronwall 2007
15 SXDS Subaru, XMM-Newton, etc. z = 3.1, 3.7, 5.7 Lyα LFs of LAEs do not evolve by more than a factor of 2 3 in either luminosity or number density May co-evolve with IGM Ouchi 2008
16 SXDS Subaru, XMM-Newton, etc. z = 3.1, 3.7, 5.7 Lyα LFs of LAEs do not evolve by more than a factor of 2 3 in either luminosity or number density May co-evolve with IGM Ouchi 2008
17 SXDS Subaru, XMM-Newton, etc. z = 3.1, 3.7, 5.7 Lyα LFs of LAEs do not evolve by more than a factor of 2 3 in either luminosity or number density May co-evolve with IGM Ouchi 2008
18 Probing Reionization Neutral IGM attenuation of Lyα Gunn-Peterson trough in QSOs for z > 6 No significant attenuation for LAEs Malhotra 2004
19 Low Redshift Study of z = 2.3 LAEs More massive Dusty Diverse Second burst of star formation Nilsson 2011
20 Clumpy Dust Suppose dust isolated in cold clumps Lyα not likely to penetrate clumps Enhance EW without destroying photons Explains 1 of 4 z = 4 LAEs Finkelstein 2008
21 Going Further with HSC Large field of view (1.77 deg 2 ) Capable of seeing galaxies and blobs Multiple narrow-band filters
22 Going Further with HSC
23 Conclusions LAEs common at large redshifts, but hard to observe Represent particular epoch of galaxy evolution Not the same as today Not the beginning of the story Narrowband photometry Better surveys to come
24 References I Steven L. Finkelstein et al. Effects of Dust Geometry in Lyα Galaxies at z = 4.4. The Astrophysical Journal, 678: , May Eric Gawiser et al. The Physical Nature of Lyα-Emitting Galaxies at z = 3.1. The Astrophysical Journal, 642:L13 L16, May Caryl Gronwall et al. Lyα Emission-Line Galaxies at z = 3.1 in the Extended Chandra Deep Field-South. The Astrophysical Journal, 667:79 91, September Takashi Hamana et al. Properties of host haloes of Lyman-break galaxies and Lyman α emitters from their number densities and angular clustering. Monthly Notices of the Royal Astronomical Society, 347: , January Sangeeta Malhotra and James E. Rhoads. Large Equivalent Width Lyα Line Emission at z = 4.5: Youg Galaxies in a Young Universe? The Astrophysical Journal, 565:L71 L74, February 2002.
25 References II Sangeeta Malhotra and James E. Rhoads. Luminosity Functions of Lyα Emitters at Redshifts z = 6.5 and z = 5.7: Evidence against Reionization at Z 6.5. The Astrophysical Journal, 617:L5 L8, December Crystal L. Martin et al. A Magellan IMACS Spectroscopic Search for Lyα-Emitting Galaxies at Redshift 5.7. The Astrophysical Journal, 679: , June K. K. Nilsson et al. The nature of z 2.3 Lyman-α emitters. Astronomy and Astrophysics, 529:A9, May Masami Ouchi et al. The Subaru/XMM-Newton Deep Survey (SXDS). IV. Evolution of Lyα Emitters From z = 3.1 to 5.7 in the 1 deg 2 Field: Luminosity Functions and AGN. The Astrophysical Journal Supplement Series, 176: , June 2008.
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