Table 1
Rest wavelengths in vacuum of lines detected in the CRIRES spectra.
| λ (nm) | Stellar or IS | Abs. or EmL | Notes | Lines from the NIST database within ±0.2 nm |
|---|---|---|---|---|
| 1315.4 | S | Abs. | (1) | Zn I (1315.42 nm), Al I (1315.43 nm), Th I (1315.45 nm), Fe I (1315.52 nm) Fe I (1315.52 nm), Cs II (1315.53 nm) |
| 1316.5 | S | EmL | (2) | C I (1316.42 nm), Fe II (1316.60 nm), Fe II (1316.65 nm), Cs II (1316.68 nm) |
| 1316.8 | S? | Abs. | O I (1316.75, 1316.85, 1316.87 nm), Fe II (1316.82 nm) | |
| 1317.3 | S | EmL | (3) | Th I (1317.14, 1317.19 nm), Fe I (1317.39, 1317.42 nm), V I (1317.43 nm), Th II (1317.52 nm) |
| 1318.1 | IS | Abs. | DIB | Th I (1317.97, 1318.20 nm), Si I (1318.05 nm), Fe I (1318.06 nm) Kr I (1318.10 nm), Ti I 1318.20 nm), Th II (1318.29 nm), V I 1318.29 nm) |
| 1527.0 | IS | Abs. | DIB | Cr II (1526.97 nm), Fe I (1526.84, 1527.12 nm), Kr I 1527.01 nm), Fe II (1527.10 nm) |
| 1529.9 | S | Abs. | (4) | Th II (1529.72 nm), Fe II (1529.73, 1529.87, 1529.90, 1529.98 nm), Cs II (1529.80 nm), V I (1529.82 nm), Th I (1529.93, 1529.98, 1530.04 nm), Fe II (1529.98 nm), Hg I (1530.00 nm), Fe I (1530.00, 1530.03, 1530.06, 1530.10 nm) |
| 1555.7 | S | Abs. & EmL | Br line | Fe I (1555.64, 1555.78, 1555.88 nm), Th I (1555.59, 1555.74 nm), Ti II (1555.63 nm), Fe II (1555.81 nm) |
| 1561.1 | IS | Abs. | DIB | Ti I (1560.91, 1560.94 nm), Fe II (1560.96 nm), Cr II (1561.14 nm), Al II (1561.14 nm) Th I (1561.24 nm) |
| 1562.4 | S | Abs. | (4) | Se I (1562.27 nm), Ti II (1562.38 nm), Th I (1562.44 nm), Fe II (1562.54, 1562.59 nm) |
| 1563.0 | S | Abs. | (4) | Fe II (1562.84 nm), Th II (1562.89 nm), B I (1562.90 nm) |
| 1563.5 | S | Abs. | (4) | B I (1563.33 nm), Fe I (1563.36, 1563.39, 1563.53 nm, Th II (1563.58 nm) |
| 1564.4 | ??? | Abs. | Weak | Fe I (1564.32, 1564.38 nm), Th II (1564.47, 1564.56, 1564.61 nm), V I (1564.47 nm), Fe II (1564.52 nm) |
| 1565.1 | IS | Abs. | DIB | Fe I (1564.92, 1565.28 nm) Fe II (1564.96, 1565.21 nm) Ar II (1565.21 nm) |
| 1566.1 | S | EmL | (5) | V I (1566.1 nm), Fe I (1566.2 nm) |
| 1567.0 | IS | Abs. | DIB | Ti I (1566.05 nm), V I (1566.07 nm) |
| 1610.9 | S | Abs. & EmL | Br. line | Ti I (1619.73, 1610.99, 1611.03 nm), Th I (1610.84, 1610.98 nm), Ar II (1610.94 nm) |
| 1616.4 | S | Abs. | Ti I (1616.21, 1616.47, 1616.56), Be I (1616.21) Fe I (1616.21, 1616.34 nm), Fe II (1616.31, 1616.39 nm) | |
| 1616.7 | S | Abs. & EmL | (6) | Ti I (1616.56, 1616.84 nm), Fe I (1616.72 nm), Th II (1616.78 nm), Si I (1616.81 nm) |
| 1625.3 | S | EmL | Al II (1625.11, 1625.23 nm), Fe I (1625.14, 1625.33 nm) | |
| 1626.1 | S | EmL | – | Fe I (1625.91 nm), P I (1625.92 nm), Fe I (1625.34 nm), Ti I (1626.37 nm) |
| 1633.8 | S? | Abs. | Fe II (1633.74 nm), Fe I (1633.76 nm), C I (1633.84 nm) | |
| 1634.2 | S | EmL | – | Fe I (1634.16 nm) |
Notes. We also show lines taken from the NIST database within ±0.2 nm in vacuum wavelength. (1) Only observed in magnetic stars. (2) Only observed in blue supergiants. (3) Observed in B2 and earlier spectral types. Contaminates 1318.1 nm DIB. (4) Only observed in one magnetically peculiar star. (5) Only observed in blue supergiant and emission-line stars. (6) Only observed in blue supergiant and Wolf-Rayet stars.
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