Table 2
Longitudinal magnetic fields of three stars obtained with different algorithms.
| HD 94660 | HD 96441 | HD 171184 | |
| Method | ⟨Bz⟩ (G) | ⟨Bz⟩ (G) | ⟨Bz⟩ (G) |
| (a) | −2506 ± 68 | −74 ± 39 | 125 ± 41 |
| (b) | −2622 ± 63 | −65 ± 39 | 139 ± 41 |
| (c) | −2549 ± 69 | −32 ± 47 | 150 ± 45 |
| (d) | −2512 ± 68 | −71 ± 39 | 166 ± 40 |
| (e) | −2452 ± 69 | −78 ± 39 | 127 ± 42 |
| (f) | −2496 ± 68 | −79 ± 39 | 148 ± 40 |
| (g) | −2508 ± 69 | −77 ± 39 | 127 ± 41 |
| (h) | −2453 ± 71 | −74 ± 40 | 110 ± 62 |
| (j) | −2499 ± 67 | −75 ± 39 | 117 ± 40 |
| (k) | −2811 ± 101 | −168 ± 47 | 171 ± 56 |
| (l) | −2406 ± 99 | 123 ± 77 | 53 ± 62 |
| (m) | −3005 ± 146 | −185 ± 57 | 126 ± 71 |
Notes. Keys to the methods. (a): as described at the end of Sect. 3.5; (b): same as (a), but with flat-fielding correction; (c): same as (a), but with optimal extraction; (d): same as (a), but using a 6 pixel aperture; (e): same as (a), but using a 18 pixel aperture; (f): same as (a), but without clipping; (g): same as (a), but without rectifying; (h): same as (a), with a 250 pixel wide filter; (j): same as (a), trimming only the first and the last 10 spectral points; (k): same as (a), but using Balmer lines only; (l): same as (a), but using metal lines. (m): same as (k) (i.e., using Balmer lines only), but applying a 2 pixel rebinning. For all cases, we have computed error bars using Eq. (11). All observations were obtained with grism 600B and a 0.5′′ slit width. Observing dates were 2003-02-08, 2004-04-17 and 2003-08-29 for HD 94660, HD 96441, and HD 171184, respectively.
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