Table 1.
Relevant information for the objects in our sample.
| ID | RA | Dec | z | Instrument | Configuration | S/N | Ref. |
|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
| GS_3073 | 57.078 | −27.884 | 5.555 | NIRSpec/IFS | G395M/F290LP – 0.25″ | 83 | Übler et al. (2023) |
| COS-ZS7 | 150.099 | 2.3436 | 7.145 | NIRSpec/IFS | G395M/F290LP – 0.50″ | 6 | Übler et al. (2024) |
| CEERS-01019 | 215.035 | 52.890 | 8.681 | NIRSpec/MSA | G395M/F290LP | ≲1 | Larson et al. (2023) |
| JADES-000954 | 189.152 | 62.260 | 6.762 | NIRSpec/MSA | G395M/F290LP | 6 | Maiolino et al. (2024a) |
| JADES-028074 | 189.065 | 62.234 | 2.261 | NIRSpec/MSA | G395M/F290LP | 10 | Juodžbalis et al. (2024b) |
| JADES-209777 | 53.156 | 27.776 | 3.711 | NIRSpec/MSA | 235M/F170LP | 132 | Juodžbalis et al. (2025) |
| RUBIES-CEERS-49140 | 214.892 | 52.878 | 6.687 | NIRSpec/MSA | G395M/F290LP | 11 | Kocevski et al. (2024) |
| RUBIES-CEERS-55604 | 214.982 | 52.956 | 6.985 | NIRSpec/MSA | G395M/F290LP | 15 | Kocevski et al. (2024) |
| UNCOVER-20466 | 3.640 | −30.386 | 8.502 | NIRSpec/MSA | PRISM/CLEAR | 9 | Kokorev et al. (2023) |
| Abell2744-QSO1 | 3.604 | −30.382 | 7.045 | NIRSpec/MSA | PRISM/CLEAR | 37 | Furtak et al. (2024) |
| XID2028 | 150.547 | 1.619 | 1.593 | NIRSpec/IFS | G140H/F100LP – 0.25″ | 38 | Cresci et al. (2023) |
| DELS J0411–0907 | 62.869 | −9.130 | 6.820 | NIRSpec/IFS | G395M/F290LP – 0.35″–0.45″ | 50 | Marshall et al. (2023) |
| VDES J0020–3653 | 5.131 | −36.895 | 6.855 | NIRSpec/IFS | G395M/F290LP – 0.35″–0.45″ | 80 | Marshall et al. (2023) |
| PJ308-21 | 308.042 | −21.234 | 6.234 | NIRSpec/IFS | G395M/F290LP – 0.30″ | 50 | Loiacono et al. (2024) |
| J0100+2802 | 15.054 | 28.041 | 6.327 | NIRCam/WFSS | F356W | 132 | Yue et al. (2024b) |
| JJ0148+0600 | 27.157 | 6.006 | 5.977 | NIRCam/WFSS | F356W | 92 | Yue et al. (2024b) |
| J159-02 | 159.226 | −2.544 | 6.381 | NIRCam/WFSS | F356W | 23 | Yue et al. (2024b) |
| J1030+0524 | 157.613 | 5.415 | 6.304 | NIRCam/WFSS | F356W | 59 | Yue et al. (2024b) |
| J1120+0641 | 170.006 | 6.690 | 7.085 | NIRCam/WFSS | F356W | 34 | Yue et al. (2024b) |
| J1148+5251 | 177.069 | 52.864 | 6.422 | NIRCam/WFSS | F356W | 38 | Yue et al. (2024b) |
| J010953.13-304726.30 | 17.471 | −30.791 | 6.790 | NIRCam/WFSS | F356W | 80 | Yang et al. (2023b) |
| J021847.04+000715.20 | 34.696 | 0.121 | 6.770 | NIRCam/WFSS | F356W | 42 | Yang et al. (2023b) |
| J022426.54-471129.40 | 36.111 | −47.192 | 6.522 | NIRCam/WFSS | F356W | 324 | Yang et al. (2023b) |
| J022601.87+030259.28 | 36.508 | 3.050 | 6.541 | NIRCam/WFSS | F356W | 192 | Yang et al. (2023b) |
| J024401.02-500853.70 | 41.004 | −50.148 | 6.731 | NIRCam/WFSS | F356W | 116 | Yang et al. (2023b) |
| J030516.92-315056.00 | 46.320 | −30.791 | 6.614 | NIRCam/WFSS | F356W | 116 | Yang et al. (2023b) |
| J200241.59-301321.69 | 300.673 | −30.223 | 6.688 | NIRCam/WFSS | F356W | 137 | Yang et al. (2023b) |
| J223255.15+293032.04 | 338.230 | 29.509 | 6.666 | NIRCam/WFSS | F356W | 42 | Yang et al. (2023b) |
| RUBIES-EGS-8488 | 215.035 | 52.891 | 6.68 | NIRSpec/MSA | G395M/F290LP | ≲1 | This work |
| RUBIES-EGS-948917 | 214.893 | 52.857 | 6.73 | NIRSpec/MSA | G395M/F290LP | 5 | This work |
| RUBIES-CEERS-966623‡ | 214.876 | 52.881 | 8.35 | NIRSpec/MSA | G395M/F290LP | 3 | This work |
| SBS_0335-052E | 54.434 | −5.044 | 0.014 | FORS1 | 600B, 600R | 60 | Izotov et al. (2009) |
| J102530.29+140207.3 | 156.376 | 14.035 | 0.101 | SDSS | – | 5 | Izotov & Thuan (2008) |
| J104755.92+073951.2 | 161.983 | 7.664 | 0.168 | SDSS | – | 5 | Izotov & Thuan (2008) |
Notes. Identifier (1), coordinates (2,3) and redshift (4). Column 5 reports the instrument employed for these observations. Column 6 describes the configuration adopted for each observation. In the case of NIRSpec multi-shutter array (MSA) we report the disperser/filter coupling. In the case of integral field spectroscopy (IFS) we also report the radius of the circular extraction region in arcseconds. In the case of Wide Field Slitless Spectroscopy (WFSS) we report the filter employed for the observations analysed here. In Column 7 we report the average signal to noise (S/N) estimated in a continumm window centered at rest-frame 5100 Å. Column 8 highlights the reference papers for the spectral data employed in this work for each source. We also report the instrument and configuration for the spectra of AGNs in dwarf galaxies. ‡: Already reported in Kocevski et al. (2024), but without the broad component in Hβ.
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