Table 1.
Detectable metal lines in JWST/NIRSpec mock spectra at 26 AB mag for different effective temperatures and redshifts.
| Teff [K] | log(g) [cgs] | z = 1 | z = 3 | z = 6 | z = 10 |
|---|---|---|---|---|---|
| 4000 | 0.0 | No detectable lines | No detectable lines | No detectable lines | No detectable lines |
| 6000 | 0.0 | No detectable lines | Ca IIλ3934 Å | Ca IIλ3934 Å (a) | Ca IIλ3934 Å (a) |
| Ca IIλ3969 Å | Ca IIλ3969 Å (a) | Ca IIλ3969 Å (a) | |||
| 8000 | 1.0 | No detectable lines | No detectable lines | No detectable lines | No detectable lines |
| 10 000 | 2.0 | No detectable lines | No detectable lines | No detectable lines | No detectable lines |
| Si IIλ1265 Å | |||||
| Si IIIλ1295 Å | |||||
| Si IVλ1393 Å | C IIλ1335 Å | ||||
| C IVλ1550 Å (b) | Si IVλ1393 Å | ||||
| 15 000 | 2.0 | No detectable lines | No detectable lines | N IVλ1719 Å (b) | Si IVλ1403 Å |
| Al IIIλ1854 Å | C IVλ1550 Å (b) | ||||
| Mg IVλ1894 Å (b) | N IVλ1719 Å (b) | ||||
| Al IIIλ1854 Å | |||||
| Mg IVλ1894 Å (b) | |||||
| Si IIIλ1295 Å | |||||
| Si IVλ1393 Å | C IIλ1335 Å | ||||
| Si IVλ1403 Å | Si IVλ1393 Å | ||||
| 20 000 | 2.4 | No detectable lines | No detectable lines | C IVλ1550 Å (b) | Si IVλ1403 Å |
| N IVλ1719 Å (b) | C IVλ1550 Å (b) | ||||
| Al IIIλ1854 Å | Al IIIλ1854 Å | ||||
| Mg IVλ1894 Å (b) | Mg IVλ1894 Å (b) | ||||
| Si IVλ1403 Å | |||||
| 30 000 | 3.2 | No detectable lines | No detectable lines | C IVλ1550 Å (a,b) | Si IVλ1393 Å (a) |
| Fe IVλ1631 Å (b) | Si IVλ1403 Å | ||||
| N IVλ1719 Å (b) | C IVλ1550 Å (a,b) | ||||
| N Vλ1239 Å (a) | |||||
| 50 000 | 4.2 | No detectable lines | No detectable lines | No detectable lines | O Vλ1371 Å (a) |
| N IVλ1488 Å | N Vλ1239 Å (a) | ||||
| 50 000 (WR star) | 4.0 | No detectable lines | No detectable lines | C IVλ1550 Å (a) | N IVλ1488 Å |
| N IVλ1720 Å | C IVλ1550 Å (a) | ||||
Notes. A few examples of mock spectra for particular Teff and redshifts are displayed in Figs. 1, 2, and 3. The stellar atmosphere spectra based on models with Teff ≤ 10 000 K use [M/H]= − 1, while the hotter stars use [M/H]= − 0.845. (a)Also detectable at 27 AB mag. (b)Part of a broader continuum feature.
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