GA-NIFS: The highly overdense system BR1202-0725 at z ∼ 4.7 - A double active galactic nucleus with fast outflows plus eight companion galaxies

Home

All issues

Volume 702 (October 2025)

A&A, 702 (2025) A102

Full HTML

Open Access

Table 5.

Emission line observed fluxes (in units of 10⁻¹⁷ erg s⁻¹ cm⁻²), emission line ratios, and main properties (ionization parameter U, and gas phase metallicity, in terms of oxygen abundance and relative to solar) of the LAEs and confirmed companions, from their integrated spectra reported in Figs. 9 and 11.

	LAE1a	LAE1b	LAE2	C1	C2	C3	C4
Hα	15.8 ± 1.3	27.0 ± 0.9	4.9 ± 0.5	12.0 ± 1.1	2.1 ± 0.2	12.3 ± 0.7	1.35 ± 0.10
Hβ	16.4 ± 1.9^a	21 ± 3^a	< 0.9	4 ± 2	< 0.4	5.7 ± 1.3	< 0.3
[Ne III] λ3869 Å	7.5 ± 1.4	7.7 ± 1.6	< 0.8	3.2 ± 1.9	< 1.1	< 2	< 0.5
[N II] λ6584 Å	< 0.4	4.14 ± 0.15	2.54 ± 0.11	< 0.7	0.78 ± 0.14	9.4 ± 0.6	0.51 ± 0.06
[O II] λ3727,29 Å	36 ± 2	44 ± 2	< 1.6	11 ± 2	3.6 ± 0.7	19 ± 2	< 1.0
[O III] λ5007 Å	79 ± 4	70 ± 2	< 0.9	40 ± 3	6.8 ± 0.6	12.5 ± 1.2	4.2 ± 0.3

Hα/Hβ	–	–	–	3.0 ± 1.6	–	2.2 ± 0.5	–
log([N II]/Hα)	< − 1.6	−0.82 ± 0.02	−0.29 ± 0.05	< −1.2	−0.43 ± 0.09	–0.12 ± 0.04	–0.42 ± 0.06
log([O III]/Hβ)	0.68 ± 0.06	0.53 ± 0.07	–	1.0 ± 0.2	> 1.3	0.34 ± 0.11	> 1.2
log([O III]/[O II])	0.34 ± 0.04	0.21 ± 0.03	–	0.57 ± 0.11	0.28 ± 0.10	−0.18 ± 0.07	–

log(U)	−2.75 ± 0.03	−2.86 ± 0.02	–	–2.56 ± 0.09	−2.80 ± 0.08	−3.16 ± 0.05	–
12+log(O/H)	8.19 $_{- 0.22}^{+ 0.17}$ $_{-0.22}^{+0.17}$	8.35 $_{- 0.14}^{+ 0.12}$ $_{-0.14}^{+0.12}$	8.77 $_{- 0.19}^{+ 0.17}$ $_{-0.19}^{+0.17}$	8.08 $_{- 0.25}^{+ 0.19}$ $_{-0.25}^{+0.19}$	8.47 $_{- 0.16}^{+ 0.13}$ $_{-0.16}^{+0.13}$	8.58 $_{- 0.07}^{+ 0.06}$ $_{-0.07}^{+0.06}$	8.77 $_{- 0.22}^{+ 0.17}$ $_{-0.22}^{+0.17}$
Z/Z_⊙ ^b	0.31 $_{- 0.12}^{+ 0.15}$ $_{-0.12}^{+0.15}$	0.45 $_{- 0.12}^{+ 0.15}$ $_{-0.12}^{+0.15}$	1.2 $_{- 0.4}^{+ 0.6}$ $_{-0.4}^{+0.6}$	0.25 $_{- 0.11}^{+ 0.14}$ $_{-0.11}^{+0.14}$	0.60 $_{- 0.18}^{+ 0.21}$ $_{-0.18}^{+0.21}$	0.77 $_{- 0.11}^{+ 0.12}$ $_{-0.11}^{+0.12}$	1.2 $_{- 0.5}^{+ 0.6}$ $_{-0.5}^{+0.6}$

Notes. ^aThese measurements should be taken with caution due to the presence of spikes at the wavelengths of Hβin the spectrum of LAE1 (see Fig. 9); for this reason, we have not used the ratios involving this line to estimate the metallicity of LAE1a and LAE1b. ^bAssuming a solar photospheric value of 12+log(O/H)_⊙ = 8.69 (Asplund et al. 2009).

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.