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Table D.1.

Main spectroscopic properties of the Cosmic Gems arc and its subregions.

BCDE1,2 A1,2 TAIL CC BCDE1,2+CC ARC2 BC1,2 DE1,2
spectral features
EW([OIII1.2ex]4959) [Å] 47 5 + 6 $ 47^{+6}_{-5} $ < 40 < 20 75 12 + 15 $ 75^{+15}_{-12} $ 51 5 + 6 $ 51^{+6}_{-5} $ < 23 42 7 + 8 $ 42^{+8}_{-7} $ 54 9 + 10 $ 54^{+10}_{-9} $
EW(Hβ) [Å] 18 2 + 3 $ 18^{+3}_{-2} $ 25 7 + 15 $ 25^{+15}_{-7} $ < 52 38 6 + 8 $ 38^{+8}_{-6} $ 21 2 + 3 $ 21^{+3}_{-2} $ < 59 13 3 + 3 $ 13^{+3}_{-3} $ 23 4 + 5 $ 23^{+5}_{-4} $
R3 7.5 ± 1.8 5.9 ± 1.3 7.0 ± 1.4 9.0 ± 3.0 6.5 ± 1.3
βUV 2 . 53 0.03 + 0.03 $ -2.53^{+0.03}_{-0.03} $ 2 . 60 0.06 + 0.06 $ -2.60^{+0.06}_{-0.06} $ 2 . 74 0.06 + 0.06 $ -2.74^{+0.06}_{-0.06} $ 2 . 52 0.06 + 0.06 $ -2.52^{+0.06}_{-0.06} $ 2 . 53 0.02 + 0.02 $ -2.53^{+0.02}_{-0.02} $ 2 . 66 0.05 + 0.05 $ -2.66^{+0.05}_{-0.05} $ 2 . 55 0.03 + 0.03 $ -2.55^{+0.03}_{-0.03} $ 2 . 52 0.03 + 0.04 $ -2.52^{+0.04}_{-0.03} $
Balmer break 1.3 ± 0.1 1.2 ± 0.4 1.0 ± 0.5 1.4 ± 0.4 1.3 ± 0.1 1.2 ± 0.4 1.2 ± 0.2 1.34 ± 0.23

Bagpipes fit
(mw)age [Myr] 12 2 + 3 $ 12^{+3}_{-2} $ (11) 15 2 + 3 $ 15^{+3}_{-2} $ (15) 49 15 + 18 ( 45 ) $ 49^{+18}_{-15}\ (45) $ 95 14 + 14 ( 108 ) $ 95^{+14}_{-14}\ (108) $ 10 1 + 2 $ 10^{+2}_{-1} $ (10) 68 18 + 17 ( 77 ) $ 68^{+17}_{-18}\ (77) $ 14 2 + 2 ( 13 ) $ 14^{+2}_{-2}\ (13) $ 9 1 + 1 ( 8 ) $ 9^{+1}_{-1}\ (8) $
τ [Myr] 3 0 + 1 $ 3^{+1}_{-0} $ (2) 2 1 + 1 $ 2^{+1}_{-1} $ (2) 206 127 + 181 ( 106 ) $ 206^{+181}_{-127}\ (106) $ 306 131 + 121 ( 449 ) $ 306^{+121}_{-131}\ (449) $ 2 0 + 1 $ 2^{+1}_{-0} $ (2) 148 98 + 174 ( 344 ) $ 148^{+174}_{-98}\ (344) $ 3 0 + 0 ( 3 ) $ 3^{+0}_{-0}\ (3) $ 2 0 + 0 ( 1 ) $ 2^{+0}_{-0}\ (1) $
AV [mag] 0 . 23 0.02 + 0.02 $ 0.23^{+0.02}_{-0.02} $ (0.22) 0 . 22 0.08 + 0.07 $ 0.22^{+0.07}_{-0.08} $ (0.24) 0 . 03 0.02 + 0.03 ( 0.01 ) $ 0.03^{+0.03}_{-0.02}\ (0.01) $ 0 . 05 0.03 + 0.04 ( 0.03 ) $ 0.05^{+0.04}_{-0.03}\ (0.03) $ 0 . 21 0.02 + 0.02 $ 0.21^{+0.02}_{-0.02} $ (0.22) 0 . 03 0.02 + 0.03 ( 0.00 ) $ 0.03^{+0.03}_{-0.02}\ (0.00) $ 0 . 24 0.03 + 0.03 ( 0.24 ) $ 0.24^{+0.03}_{-0.03}\ (0.24) $ 0 . 20 0.03 + 0.03 ( 0.19 ) $ 0.20^{+0.03}_{-0.03}\ (0.19) $
Z [Z] 0 . 16 0.01 + 0.01 $ 0.16^{+0.01}_{-0.01} $ (0.16) 0 . 06 0.04 + 0.05 ( 0.04 ) $ 0.06^{+0.05}_{-0.04} (0.04) $ 0 . 06 0.02 + 0.02 ( 0.08 ) $ 0.06^{+0.02}_{-0.02}\ (0.08) $ 0 . 18 0.02 + 0.02 ( 0.19 ) $ 0.18^{+0.02}_{-0.02}\ (0.19) $ 0 . 17 0.01 + 0.01 $ 0.17^{+0.01}_{-0.01} $ (0.17) 0 . 07 0.02 + 0.02 ( 0.08 ) $ 0.07^{+0.02}_{-0.02}\ (0.08) $ 0 . 13 0.02 + 0.02 ( 0.14 ) $ 0.13^{+0.02}_{-0.02}\ (0.14) $ 0 . 17 0.01 + 0.01 ( 0.17 ) $ 0.17^{+0.01}_{-0.01}\ (0.17) $
log ( M / M ) $ \rm log(M_\star/M_\odot)^\dag $ 6 . 72 0.09 + 0.10 ( 6.67 ) $ 6.72^{+0.10}_{-0.09}\ (6.67) $ 6 . 56 0.13 + 0.11 ( 6.56 ) $ 6.56^{+0.11}_{-0.13}\ (6.56) $ 7 . 42 0.12 + 0.10 ( 7.39 ) $ 7.42^{+0.10}_{-0.12}\ (7.39) $ < 5 . 68 0.03 + 0.03 ( 5.70 ) $ < 5.68^{+0.03}_{-0.03}\ (5.70)^\ddag $ 6 . 69 0.08 + 0.10 ( 6.68 ) $ 6.69^{+0.10}_{-0.08}\ (6.68) $ 7 . 68 0.06 + 0.06 ( 7.66 ) $ 7.68^{+0.06}_{-0.06}\ (7.66) $ 6 . 68 0.09 + 0.08 ( 6.63 ) $ 6.68^{+0.08}_{-0.09}\ (6.63) $ 5 . 95 0.14 + 0.11 ( 5.89 ) $ 5.95^{+0.11}_{-0.14}\ (5.89) $
μtot 138 18 + 21 ( 153 ) $ 138^{+21}_{-18}\ (153) $ 50 4 + 4 ( 55 ) $ 50^{+4}_{-4}\ (55) $ 18 2 + 2 ( 21 ) $ 18^{+2}_{-2}\ (21) $ > 500 138 18 + 21 ( 153 ) $ 138^{+21}_{-18}\ (153) $ 107 14 + 15 ( 120 ) $ 107^{+15}_{-14}\ (120) $ 226 45 + 60 ( 259 ) $ 226^{+60}_{-45}\ (259) $

Notes. Main spectral features from the 1D spectra extracted from the regions outlined in Fig. 1 (top lines) and best-fit properties of the same regions, as derived from the Bagpipes fit of the spectra (bottom lines). The equivalent widths represent the rest-frame values. The median values and ±1σ uncertainties are reported for the fit results. The values within the parenthesis refer to the maximum likelihood values. The magnifications reported in the bottom line are estimated from the glafic model, described in Section 3. The masses quoted are intrinsic, i.e., the mass resulting from the fit was delensed (using the magnifications quoted in the last line of the table) and, in the case of BCDE1,2, A1,2, and CC, was divided by half to account for the number of counterimages included in the masks. The lens modeling uncertainty is propagated to the final intrinsic mass. The systematic uncertainty on magnification (i.e., considering different lens models), ranges between 10–40% (see Appendix B). To conservatively estimate the intrinsic mass of the CC region, we considered a lower limit in magnification, as estimated from the MCMC extractions in Appendix B, resulting in an upper limit on the mass estimate.

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