Deciphering the JWST spectrum of a ‘little red dot’ at z ∼ 4.53: An obscured AGN and its star-forming host

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Volume 691 (November 2024)

A&A, 691 (2024) A52

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Table 1.

Line wavelengths and fluxes from our best-fit model.

Line	Wavelength	Flux	Flux
	(Å)	(uncorrected)	(corrected)
Lyα^⋆	1215.40	96 ± 5	3 $_{- 3}^{+ 41} \times 10^{4}$ $^{+41}_{-3} \times 10^{4}$
C IV^⋆	1549.48	16 ± 4	1 $_{- 1}^{+ 4} \times 10^{3}$ $^{+4}_{-1} \times 10^{3}$
He II^⋆	1640.40	20 ± 5	1 $_{- 1}^{+ 4} \times 10^{3}$ $^{+4}_{-1} \times 10^{3}$
C III] ^⋆	1907.71	38 $_{- 4}^{+ 5}$ $^{+5}_{-4}$	1 $_{- 1}^{+ 3} \times 10^{3}$ $^{+3}_{-1} \times 10^{3}$
Mg II^⋆	2799.12	16 ± 3	100 $_{- 57}^{+ 149}$ $^{+149}_{-57}$
[O II] ^⋆	3728.50	32 $_{- 10}^{+ 16}$ $^{+16}_{-10}$	134 $_{- 71}^{+ 163}$ $^{+163}_{-71}$
[Ne III] ^⋆	3869.87	25 $_{- 13}^{+ 15}$ $^{+15}_{-13}$	94 $_{- 57}^{+ 125}$ $^{+125}_{-57}$
[Ne III] ^⋆	3968.59	21 $_{- 12}^{+ 26}$ $^{+26}_{-12}$	82 $_{- 54}^{+ 151}$ $^{+151}_{-54}$
Hδ^⋆	4102.94	7 ± 1	27 $_{- 12}^{+ 24}$ $^{+24}_{-12}$
Hγ^⋆	4341.73	19 ± 2	63 $_{- 26}^{+ 50}$ $^{+50}_{-26}$
[O III] ^⋆	4364.44	17 ± 2	57 $_{- 24}^{+ 46}$ $^{+46}_{-24}$
Hβ^⋆	4862.74	64 ± 10	179 $_{- 47}^{+ 71}$ $^{+71}_{-47}$
[O III] ^⋆	4960.30	109 ± 3	297 $_{- 104}^{+ 179}$ $^{+179}_{-104}$
[O III] ^⋆	5008.24	325 ± 9	872 $_{- 302}^{+ 515}$ $^{+515}_{-302}$
He I^†	5877.25	11 ± 1	1 ± 0.1 × 10³
Hα (narrow) ^⋆	6564.70	259 ± 8	512 $_{- 136}^{+ 202}$ $^{+202}_{-136}$
[S II] ^⋆	6718.29	2 ± 0.3	4 $_{- 1}^{+ 2}$ $^{+2}_{-1}$
[S II] ^⋆	6732.67	3 ± 0.3	6 ± 2
He I^†	7067.10	14 ± 1	534 ± 29
He I^†	8446.70	12 ± 1	188 ± 11
Hα (broad) ^†	6564.70	160 ± 6	9 ± 0.5 × 10³

Notes. Fluxes are given in units of 10⁻¹⁹ erg s⁻¹ cm⁻². He I and broad Hα line fluxes are corrected by A_V = 5.61 ± 0.04 (indicated with a † symbol) from the optical-NIR power-law fit, while the rest of the lines are corrected by A_V = 0.9 ± 0.4 (indicated with a ⋆ symbol) from the Balmer decrement. The SMC attenuation correction is quite large at the Lyα wavelength.

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