| ID♯ . | UDF ♯ . | F775W mag (a) . | z BPZ (a) . | z EAZY (a) . | Emission line detected by MUSE (b) . | z MUSE (b) . | CONF.† (b) . | Identification . |
|---|---|---|---|---|---|---|---|---|
| 1 | 9397 | 21.031|$\, \pm \,$|0.001 | 1.30–1.42–1.52 | 0.12–0.17–1.33 | Hδ, O|$\,$| ii1 | 1.2185 | 2 | Quasar (c) |
| 2 | 7025 | 25.276|$\, \pm \,$|0.006 | 3.21–3.40–3.59 | 2.89–2.96–3.04 | Lyα | 3.326 | 2 | Galaxy (d) |
| 3 | 6732 | 24.587|$\, \pm \,$|0.006 | 2.90–3.09–3.27 | 3.13–3.19–3.25 | C|$\,$| iii1, Lyα | 3.1882 | 2 | Quasar (e) |
| 4 | 4070 | 25.959|$\, \pm \,$|0.01 | 2.44–2.60–2.75 | 1.76–1.84–1.91 | C|$\,$| iii1, C|$\,$| iii2 | 2.4908 | 3 | Galaxy (d,f) |
| 5 | 8230 | 25.531|$\, \pm \,$|0.013 | 3.34–3.54–3.73 | 3.14–3.22–3.29 | Lyα | 3.6716 | 3 | Galaxy (d,f) |
| 6 | 5711 | 27.353|$\, \pm \,$|0.016 | 0.51–0.59–0.77 | 0.09–0.12–0.17 | Hβ, Hγ, O|$\,$| ii1, O|$\,$| ii2, O|$\,$| iii1, O|$\,$| iii2 | 0.6206 | 3 | Galaxy (g,h) |
| 7 | 8942 | 27.662|$\, \pm \,$|0.033 | 0.70–0.78–0.85 | 0.01–0.03–0.05 | O|$\,$| iii2 | 1.4469 | 2 | |
| 8 | 2087 | 26.597|$\, \pm \,$|0.014 | 3.50–3.72–3.94 | 3.33–3.42–3.51 | Lyα | 3.7282 | 2 | Galaxy (d) |
| 12 | 5550 | 28.781|$\, \pm \,$|0.0533 | 2.60–2.78–2.95 | 2.48–2.61–2.80 | ||||
| 14 | 2047 | 29.103|$\, \pm \,$|0.0708 | 1.50–1.96–2.35 | 1.66–2.04–2.42 | ||||
| 16 | 8858 | 28.856|$\, \pm \,$|0.078 | 1.54–1.69–1.84 | 1.59–1.70–1.80 | ||||
| 20 | 5019 | 29.155|$\, \pm \,$|0.0886 | 1.27–1.52–2.12 | 1.37–1.57–1.89 |
| ID♯ . | UDF ♯ . | F775W mag (a) . | z BPZ (a) . | z EAZY (a) . | Emission line detected by MUSE (b) . | z MUSE (b) . | CONF.† (b) . | Identification . |
|---|---|---|---|---|---|---|---|---|
| 1 | 9397 | 21.031|$\, \pm \,$|0.001 | 1.30–1.42–1.52 | 0.12–0.17–1.33 | Hδ, O|$\,$| ii1 | 1.2185 | 2 | Quasar (c) |
| 2 | 7025 | 25.276|$\, \pm \,$|0.006 | 3.21–3.40–3.59 | 2.89–2.96–3.04 | Lyα | 3.326 | 2 | Galaxy (d) |
| 3 | 6732 | 24.587|$\, \pm \,$|0.006 | 2.90–3.09–3.27 | 3.13–3.19–3.25 | C|$\,$| iii1, Lyα | 3.1882 | 2 | Quasar (e) |
| 4 | 4070 | 25.959|$\, \pm \,$|0.01 | 2.44–2.60–2.75 | 1.76–1.84–1.91 | C|$\,$| iii1, C|$\,$| iii2 | 2.4908 | 3 | Galaxy (d,f) |
| 5 | 8230 | 25.531|$\, \pm \,$|0.013 | 3.34–3.54–3.73 | 3.14–3.22–3.29 | Lyα | 3.6716 | 3 | Galaxy (d,f) |
| 6 | 5711 | 27.353|$\, \pm \,$|0.016 | 0.51–0.59–0.77 | 0.09–0.12–0.17 | Hβ, Hγ, O|$\,$| ii1, O|$\,$| ii2, O|$\,$| iii1, O|$\,$| iii2 | 0.6206 | 3 | Galaxy (g,h) |
| 7 | 8942 | 27.662|$\, \pm \,$|0.033 | 0.70–0.78–0.85 | 0.01–0.03–0.05 | O|$\,$| iii2 | 1.4469 | 2 | |
| 8 | 2087 | 26.597|$\, \pm \,$|0.014 | 3.50–3.72–3.94 | 3.33–3.42–3.51 | Lyα | 3.7282 | 2 | Galaxy (d) |
| 12 | 5550 | 28.781|$\, \pm \,$|0.0533 | 2.60–2.78–2.95 | 2.48–2.61–2.80 | ||||
| 14 | 2047 | 29.103|$\, \pm \,$|0.0708 | 1.50–1.96–2.35 | 1.66–2.04–2.42 | ||||
| 16 | 8858 | 28.856|$\, \pm \,$|0.078 | 1.54–1.69–1.84 | 1.59–1.70–1.80 | ||||
| 20 | 5019 | 29.155|$\, \pm \,$|0.0886 | 1.27–1.52–2.12 | 1.37–1.57–1.89 |
*References are follows. (a): Rafelski et al. (2015), (b): Inami et al. (2017), (c): Véron-Cetty and Véron (2010), (d): Straatman et al. (2016), (e): Fiore et al. (2012), (f): Cameron et al. (2011), (g): Thompson et al. (2005), (h): Coe et al. (2006).
†“CONF.” is a confidence level of the MUSE detection in which “1” corresponds to the best case.
| ID♯ . | UDF ♯ . | F775W mag (a) . | z BPZ (a) . | z EAZY (a) . | Emission line detected by MUSE (b) . | z MUSE (b) . | CONF.† (b) . | Identification . |
|---|---|---|---|---|---|---|---|---|
| 1 | 9397 | 21.031|$\, \pm \,$|0.001 | 1.30–1.42–1.52 | 0.12–0.17–1.33 | Hδ, O|$\,$| ii1 | 1.2185 | 2 | Quasar (c) |
| 2 | 7025 | 25.276|$\, \pm \,$|0.006 | 3.21–3.40–3.59 | 2.89–2.96–3.04 | Lyα | 3.326 | 2 | Galaxy (d) |
| 3 | 6732 | 24.587|$\, \pm \,$|0.006 | 2.90–3.09–3.27 | 3.13–3.19–3.25 | C|$\,$| iii1, Lyα | 3.1882 | 2 | Quasar (e) |
| 4 | 4070 | 25.959|$\, \pm \,$|0.01 | 2.44–2.60–2.75 | 1.76–1.84–1.91 | C|$\,$| iii1, C|$\,$| iii2 | 2.4908 | 3 | Galaxy (d,f) |
| 5 | 8230 | 25.531|$\, \pm \,$|0.013 | 3.34–3.54–3.73 | 3.14–3.22–3.29 | Lyα | 3.6716 | 3 | Galaxy (d,f) |
| 6 | 5711 | 27.353|$\, \pm \,$|0.016 | 0.51–0.59–0.77 | 0.09–0.12–0.17 | Hβ, Hγ, O|$\,$| ii1, O|$\,$| ii2, O|$\,$| iii1, O|$\,$| iii2 | 0.6206 | 3 | Galaxy (g,h) |
| 7 | 8942 | 27.662|$\, \pm \,$|0.033 | 0.70–0.78–0.85 | 0.01–0.03–0.05 | O|$\,$| iii2 | 1.4469 | 2 | |
| 8 | 2087 | 26.597|$\, \pm \,$|0.014 | 3.50–3.72–3.94 | 3.33–3.42–3.51 | Lyα | 3.7282 | 2 | Galaxy (d) |
| 12 | 5550 | 28.781|$\, \pm \,$|0.0533 | 2.60–2.78–2.95 | 2.48–2.61–2.80 | ||||
| 14 | 2047 | 29.103|$\, \pm \,$|0.0708 | 1.50–1.96–2.35 | 1.66–2.04–2.42 | ||||
| 16 | 8858 | 28.856|$\, \pm \,$|0.078 | 1.54–1.69–1.84 | 1.59–1.70–1.80 | ||||
| 20 | 5019 | 29.155|$\, \pm \,$|0.0886 | 1.27–1.52–2.12 | 1.37–1.57–1.89 |
| ID♯ . | UDF ♯ . | F775W mag (a) . | z BPZ (a) . | z EAZY (a) . | Emission line detected by MUSE (b) . | z MUSE (b) . | CONF.† (b) . | Identification . |
|---|---|---|---|---|---|---|---|---|
| 1 | 9397 | 21.031|$\, \pm \,$|0.001 | 1.30–1.42–1.52 | 0.12–0.17–1.33 | Hδ, O|$\,$| ii1 | 1.2185 | 2 | Quasar (c) |
| 2 | 7025 | 25.276|$\, \pm \,$|0.006 | 3.21–3.40–3.59 | 2.89–2.96–3.04 | Lyα | 3.326 | 2 | Galaxy (d) |
| 3 | 6732 | 24.587|$\, \pm \,$|0.006 | 2.90–3.09–3.27 | 3.13–3.19–3.25 | C|$\,$| iii1, Lyα | 3.1882 | 2 | Quasar (e) |
| 4 | 4070 | 25.959|$\, \pm \,$|0.01 | 2.44–2.60–2.75 | 1.76–1.84–1.91 | C|$\,$| iii1, C|$\,$| iii2 | 2.4908 | 3 | Galaxy (d,f) |
| 5 | 8230 | 25.531|$\, \pm \,$|0.013 | 3.34–3.54–3.73 | 3.14–3.22–3.29 | Lyα | 3.6716 | 3 | Galaxy (d,f) |
| 6 | 5711 | 27.353|$\, \pm \,$|0.016 | 0.51–0.59–0.77 | 0.09–0.12–0.17 | Hβ, Hγ, O|$\,$| ii1, O|$\,$| ii2, O|$\,$| iii1, O|$\,$| iii2 | 0.6206 | 3 | Galaxy (g,h) |
| 7 | 8942 | 27.662|$\, \pm \,$|0.033 | 0.70–0.78–0.85 | 0.01–0.03–0.05 | O|$\,$| iii2 | 1.4469 | 2 | |
| 8 | 2087 | 26.597|$\, \pm \,$|0.014 | 3.50–3.72–3.94 | 3.33–3.42–3.51 | Lyα | 3.7282 | 2 | Galaxy (d) |
| 12 | 5550 | 28.781|$\, \pm \,$|0.0533 | 2.60–2.78–2.95 | 2.48–2.61–2.80 | ||||
| 14 | 2047 | 29.103|$\, \pm \,$|0.0708 | 1.50–1.96–2.35 | 1.66–2.04–2.42 | ||||
| 16 | 8858 | 28.856|$\, \pm \,$|0.078 | 1.54–1.69–1.84 | 1.59–1.70–1.80 | ||||
| 20 | 5019 | 29.155|$\, \pm \,$|0.0886 | 1.27–1.52–2.12 | 1.37–1.57–1.89 |
*References are follows. (a): Rafelski et al. (2015), (b): Inami et al. (2017), (c): Véron-Cetty and Véron (2010), (d): Straatman et al. (2016), (e): Fiore et al. (2012), (f): Cameron et al. (2011), (g): Thompson et al. (2005), (h): Coe et al. (2006).
†“CONF.” is a confidence level of the MUSE detection in which “1” corresponds to the best case.
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