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

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lyman emitters with no hst counterpart

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

Oct 07, 2023 144 likes •336 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)

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Lyman-⍺ Emitters with no HST Counterpart

Michael Maseda (Leiden), Roland Bacon, Marijn Franx, and the MUSE GTO Team

F606W F775W F850LP

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HOW WE GOT HERE

➤ MUSE is fantastic, because before we had to do things like

this:

Rauch+08 (92h FORS2)

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HOW WE GOT HERE

➤ Bacon+15:

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HOW WE GOT HERE

➤ Bacon+17: 72 “HST-undetected” LAEs in the UDF

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HOW WE GOT HERE

➤ Maseda+18: 155 “high-EW” LAEs in the UDF

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HOW WE GOT HERE

➤ Maseda+18: 155 “high-EW” LAEs in the UDF

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➤ Plausibly high-EW LAEs (> 200 Å) ➤ Can only occur with young ages (< 10 Myr), very low

metallicities, and/or top-heavy IMFs

WHY ARE THESE SOURCES POTENTIALLY INTERESTING?

Hashimoto+17a

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SPECTRAL STACKS

➤ Using correction from zLyα to zsys using FWHMLyα (Verhamme+

submitted)

(Preliminary)

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PHOTOMETRIC STACKS

➤ Blue continuum slopes ➤ MUV ~ -15 ➤ Effect of Ly-⍺ visible

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PHOTOMETRIC STACKS

➤ Blue continuum slopes ➤ MUV ~ -15 ➤ Effect of Ly-⍺ visible

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PHOTOMETRIC STACKS

➤ Blue continuum slopes ➤ MUV ~ -15 ➤ Effect of Ly-⍺ visible

β λrest (Å)

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DETERMINATION OF EW

➤ mUV from stacks for a given object (otherwise limit) ➤ 휷 from stacks in redshift bin

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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

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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

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SLIDE 15

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

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SLIDE 16

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

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SLIDE 17

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

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IS THIS EXPECTED?

It’s hard to distinguish between these models, but undetected sources are expected

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CONCLUSION AND OUTLOOK

➤ More than 150 high-EW LAEs in the UDF ➤ MUV 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

!!