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Table 2:

Overview of the sources included in the LRIS mask.
ID $\alpha$ (J2000.0) $\delta$ (J2000.0) $z_{\rm spec}$ $z_{\rm phot}$ F775W $\mu$ (mags) $z_{\rm class}$ Features

1.1
198.77725 51.81934 $0.8889\pm0.0003$ $\rm0.965^{+0.075}_{-0.240}$ $22.19\pm0.01$ $4.78\pm0.22$ 4 $[{\rm OII}]$, $[{\rm NeIII}]$, H$\delta$, H$\gamma$
3.1 198.76696 51.83205 3.277 $\pm$0.002 $\rm 3.35^{+0.052}_{-0.134}$ $22.69\pm0.02$ $3.40\pm0.47$ 4 $Ly_\alpha$(em), SiIV, SiII
3.3 198.75824 51.82982 $3.277 \pm0.002$ $\rm 3.35^{+0.024}_{-0.036}$ $25.34\pm0.05$ $1.66\pm0.22$ 4 $Ly_\alpha$(em), SiIV, SiII
4.2/5.2 198.76075 51.82487 $1.9082 \pm0.004$ $\rm 2.25^{+0.216}_{-0.222}$ $23.72\pm0.02$ $2.54\pm0.03$ 3 ${\rm CIV}$, SiII, ZnII
6.1 198.77984 51.82640 $2.360 \pm0.002$ $\rm 2.59^{+0.144}_{-0.159}$ $23.56\pm0.02$ $1.96\pm0.04$ 4 $Ly_\alpha$(em), SiIV, CIV, SiII
7.3 198.75869 51.82814 $2.983 \pm 0.002$ $\rm 3.20^{+0.210}_{-0.675}$ $26.81\pm0.10$ $1.87\pm0.02$ 9 $Ly_\alpha$(em)
10.1 198.78708 51.81424 $2.627 \pm 0.004$ $\rm 3.10^{+0.324}_{-0.162}$ $21.40\pm0.01$ $2.69\pm0.65$ 3 $Ly_\alpha$(abs), SiIV
11.3 198.76242 51.80954 $2.627 \pm 0.004$ $\rm 2.70^{+0.189}_{-0.261}$ $23.55\pm0.02$ $1.73\pm0.02$ 3 $Ly_\alpha$(abs), SiIV, SiII
15.1 198.76284 51.81246 $2.355 \pm 0.002$ $\rm 2.44^{+0.171}_{-0.231}$ $24.89\pm0.05$ $2.26\pm0.10$ 4 $Ly_\alpha$(em), CIV
15.3 198.78825 51.82173 $2.355 \pm 0.002$ $\rm 2.60^{+0.150}_{-0.363}$ $25.44\pm0.05$ $1.56\pm0.05$ 4 $Ly_\alpha$(em), SiIV, CIV
16.1/16.3 198.78851 51.82096 $2.810 \pm0.004$ $\rm 2.75^{+0.171}_{-0.165}$ $25.52\pm0.06$ $1.61\pm0.02$ 3 $Ly_\alpha$(abs), FeII
20 198.76659 51.83626 $1.279 \pm0.0005$ $\rm 1.10^{+0.125}_{-0.126}$ $21.86\pm0.01$ $1.51\pm0.03$ 4 $[{\rm OII}]$
21 198.76000 51.83451 $1.279 \pm0.0005$ $\rm 1.13^{+0.137}_{-0.103}$ $22.57\pm0.02$ $1.75\pm0.02$ 4 $[{\rm OII}]$
23 198.75612 51.80736 $5.827 \pm 0.0015$ 6.0+0.42-0.38 $27.20\pm0.30$ $1.20\pm0.03$ 9 $Ly_\alpha$(em)
gal2 198.78811 51.84276 $0.5632 \pm 0.0004$ $\rm0.550^{+0.123}_{-0.140}$ $20.49\pm0.01$ $0.29\pm0.01$ 4 $[{\rm OII}]$, K, H, MgI, MgII
gal4 198.76596 51.85902 $3.2269 \pm 0.002$ $\rm 3.44^{+0.09}_{-0.07}$ $24.16\pm0.03$ $0.40\pm 0.02$ 3 $Ly_\alpha$(abs), SiII, SiIV
gal11-a 198.76772 51.79678 $2.2864 \pm0.002$ $\rm 2.56^{+0.235}_{-0.252}$ $22.86\pm0.01$ $0.85\pm0.02$ 4 $Ly_\alpha$(em), SiII, CIV
gal12 198.77770 51.79462 $2.290 \pm0.002$ $\rm 2.32^{+0.255}_{-0.698}$ $25.32\pm0.08$ $0.83\pm0.03$ 4 $Ly_\alpha$(em), CIV, AlIII
gal13-b 198.77518 51.78871 $1.035 \pm0.001$ $\rm 1.05^{+0.108}_{-0.112}$ $23.45\pm0.03$ $0.48\pm0.01$ 4 $[{\rm OII}]$
gal16 198.79701 51.77606 $0.3906 \pm0.0005$ -   $0.10\pm0.01$ 4 K, H
gal17 198.79065 51.77097 $1.236 \pm0.0005$ -   $0.27\pm0.02$ 4 $[{\rm OII}]$
gal18-b 198.78816 51.77364 $0.5860 \pm0.0005$ -   $0.19\pm0.01$ 4 $[{\rm OII}]$, MgII, K, H
gal19-a 198.77100 51.76841 $0.2909 \pm0.0005$ -   $0.01\pm0.01$ 4 K, H
gal19-b 198.77063 51.76935 $0.3622 \pm0.0005$ -   $0.06\pm0.01$ 4 $[{\rm OII}]$, K, H
gal1 198.78155 51.83971 $0.1432 \pm0.0005$       4 $[{\rm OII}]$, H$\beta$, $[{\rm OIII}]$
gal3 198.77735 51.85023 $0.087 \pm0.0005$       4 $[{\rm OII}]$, K, H, H$\beta$, $[{\rm OIII}]$
gal11-b 198.76774 51.79744 $0.280\pm0.001$       4 $[{\rm OII}]$, H$\beta$, $[{\rm OIII}]$
gal13-a 198.77540 51.78808 $0.1762 \pm0.0005$       4 K, H
gal14 198.78653 51.78574 $0.1011 \pm0.0003$       4 $[{\rm OII}]$, H$\beta$, $[{\rm OIII}]$
gal18-a 198.78753 51.77299 $0.2705 \pm0.0005$       4 K, H
gal20 198.79633 51.76602 $0.2766 \pm0.0005$       4 K, H
gal21 198.78704 51.76265 $0.2781 \pm0.0005$       4 K, H
gal22-a 198.77246 51.75876 $0.2410 \pm0.0005$       4 $[{\rm OII}]$, K, H
gal22-b 198.77236 51.76022 $0.2766 \pm0.0005$       4 K, H
gal23 198.75441 51.86258 $0.1765 \pm0.0004$       4 $[{\rm OII}]$, K, H, H$\beta$, $[{\rm OIII}]$
gal24 198.75110 51.86508 $0.2683 \pm0.0005$       4 K, H
From left to right: identification, astrometric position, spectroscopic redshift, photometric redshift estimate, ACS-F775W band photometry when available, magnification in magnitudes, redshift quality class (see Sect. 2.3), main spectroscopic features. The mentions (abs) and (em) refer to an Ly$_\alpha$ line in absorption or in emission, respectively. The first part of the table corresponds to multiply-imaged systems, the second part to background sources, the third part to cluster members and foreground sources.

Source LaTeX | All tables | In the text

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