Lyman- Emitters with no HST Counterpart Michael Maseda (Leiden), - PowerPoint PPT Presentation

Oct 07, 2023 •144 likes •335 views

F606W F775W F850LP Lyman- Emitters with no HST Counterpart Michael Maseda (Leiden), Roland Bacon, Marijn Franx, and the MUSE GTO Team HOW WE GOT HERE MUSE is fantastic, because before we had to do things like this: Rauch+08 (92h FORS2)

F606W F775W F850LP Lyman- ⍺ Emitters with no HST Counterpart Michael Maseda (Leiden), Roland Bacon, Marijn Franx, and the MUSE GTO Team
HOW WE GOT HERE ➤ MUSE is fantastic, because before we had to do things like this: Rauch+08 (92h FORS2)
HOW WE GOT HERE ➤ Bacon+15:
HOW WE GOT HERE ➤ Bacon+17: 72 “HST-undetected” LAEs in the UDF
HOW WE GOT HERE ➤ Maseda+18: 155 “high-EW” LAEs in the UDF
HOW WE GOT HERE ➤ Maseda+18: 155 “high-EW” LAEs in the UDF
WHY ARE THESE SOURCES POTENTIALLY INTERESTING? ➤ Plausibly high-EW LAEs (> 200 Å) ➤ Can only occur with young ages (< 10 Myr), very low metallicities, and/or top-heavy IMFs Hashimoto+17a
SPECTRAL STACKS ➤ Using correction from z Ly α to z sys using FWHM Ly α (Verhamme+ submitted) (Preliminary)
PHOTOMETRIC STACKS ➤ Blue continuum slopes ➤ M UV ~ -15 ➤ Effect of Ly- ⍺ visible
PHOTOMETRIC STACKS ➤ Blue continuum slopes ➤ M UV ~ -15 ➤ Effect of Ly- ⍺ visible
PHOTOMETRIC STACKS ➤ Blue continuum slopes ➤ M UV ~ -15 ➤ Effect of Ly- ⍺ visible β λ rest (Å)
DETERMINATION OF EW ➤ m UV from stacks for a given object (otherwise limit) ➤ 휷 from stacks in redshift bin
IS THIS EXPECTED? ➤ Based on an EW distribution (Hashimoto+17b) and a UV luminosity function (Bouwens+15), can predict fraction of LAEs that are below a detection limit
IS THIS EXPECTED? ➤ Based on an EW distribution (Hashimoto+17b) and a UV luminosity function (Bouwens+15), can predict fraction of LAEs that are below a detection limit
IS THIS EXPECTED? ➤ Based on an EW distribution (Hashimoto+17b) and a UV luminosity function (Bouwens+15), can predict fraction of LAEs that are below a detection limit
IS THIS EXPECTED? ➤ Based on an EW distribution (Hashimoto+17b) and a UV luminosity function (Bouwens+15), can predict fraction of LAEs that are below a detection limit Force EW < 240 Å
IS THIS EXPECTED? ➤ Based on an EW distribution (Hashimoto+17b) and a UV luminosity function (Bouwens+15), can predict fraction of LAEs that are below a detection limit
IS THIS EXPECTED? It’s hard to distinguish between these models, but undetected sources are expected
CONCLUSION AND OUTLOOK ➤ More than 150 high-EW LAEs in the UDF ➤ M UV as faint as -15 ➤ Blue ( β ~ -2) UV continuum slopes ➤ They appear to be an extension of the known LAE population ➤ More work (JWST?) will be required to fully characterize them ! �� !

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