A bottom-up search for Lyman-continuum leakage in the Hubble Ultra Deep Field

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Volume 666 (October 2022)

A&A, 666 (2022) A145

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Table 5.

Escape fractions and IGM correction.

Object	^(a)	^(b)	T_IGM		^(c)
F275W-314	51 ± 33%	57%	72 ± 9%	82 ± 12%	77 ± 9%
F275W-2055	57 ± 19%	105%	66 ± 8%	153 ± 14%	76 ± 9%
F336W-189	3 ± 0.8%	23%	7 ± 5%	325 ± 200%	36 ± 22%
F336W-554	28 ± 7%	203%	49 ± 11%	441 ± 110%	67 ± 15%
F336W-606	40 ± 17%	67%	42 ± 3%	146 ± 12%	91 ± 6%
F336W-1013	4 ± 0.6%	103%	24 ± 15%	442 ± 295%	15 ± 10%
F336W-1041	108 ± 30%	397%	100 ± −%	397 ± −%	100 ± −%

Notes.

^(a)

Bold as in Table 1. The quoted uncertainties here are an estimate based on the assumption that the true S/N of the large-aperture photometry is the same as the corrected S/N in the segmentation map photometry (see Sect. 3.4), and assuming no uncertainties due to the stellar population modeling. They are not propagated further.

^(b)

No uncertainties are quoted here, as the relative and absolute escape fraction only differ by a dust correction term adopted from the BAGPIPES best-fit galaxy model.

^(c)

Uncertainties quoted here are based solely on the simulated IGM transmission distribution. Uncertainties in this quantity and in f_esc are highly degenerate.

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