Table 2.
Zeeman-splitting analysis results obtained from fitting the Stokes I and V spectra of OH megamasers in IRAS 02524+2046 with the method described in Sect. 4.2.1.
| Gaussian | S | ν | Δν | B// |  |
 |
Heliocentric velocity |
|---|---|---|---|---|---|---|---|
| (mJy) | (MHz) | (MHz) | (mG) | (mG) | (mG) | (km s−1) | |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
| 1 | 1.65 ± 0.08 | 1408.3385 ± 0.0016 | 0.0299 ± 0.0016 | 54720.96 ± 0.40† | |||
| 2 | 4.88 ± 0.12 | 1409.9954 ± 0.0007 | 0.0436 ± 0.0011 | 54304.36 ± 0.18† | |||
| 3 | 3.14 ± 0.16 | 1410.0873 ± 0.0101 | 0.1700 ± 0.0077 | 54281.29 ± 2.55† | |||
| 4 | 4.35 ± 0.18 | 1410.4488 ± 0.0032 | 0.1058 ± 0.0055 | 3.6 ± 0.9* | 1.8 ± 1.0* | 5.5 ± 1.1* | 54190.54 ± 0.81† |
| 5 | 1.65 ± 0.16 | 1410.6081 ± 0.0024 | 0.0400 ± 0.0035 | 6.5 ± 1.3* | 5.8 ± 1.7* | 7.5 ± 1.6* | 54150.56 ± 0.60† |
| 6 | 2.02 ± 0.04 | 1410.7831 ± 0.0299 | 0.3664 ± 0.0243 | 54106.66 ± 7.51† | |||
| 7 | 3.97 ± 0.19 | 1411.5623 ± 0.0003 | 0.0054 ± 0.0003 | 54326.98 ± 0.07 | |||
| 8 | 3.12 ± 0.20 | 1411.6399 ± 0.0010 | 0.0299 ± 0.0016 | 54307.52 ± 0.24 | |||
| 9 | 4.65 ± 0.18 | 1411.6620 ± 0.0035 | 0.1107 ± 0.0047 | 54301.97 ± 0.89 | |||
| 10 | 2.81 ± 0.44 | 1411.8626 ± 0.0037 | 0.0424 ± 0.0039 | 54251.67 ± 0.92 | |||
| 11 | 1.55 ± 0.30 | 1411.9924 ± 0.0018 | 0.0168 ± 0.0027 | 54219.12 ± 0.45 | |||
| 12 | 11.84 ± 3.51 | 1412.0781 ± 0.0063 | 0.0659 ± 0.0099 | 11.4 ± 0.5 | 11.7 ± 0.6 | 10.3 ± 0.6 | 54197.62 ± 1.59 |
| 13 | 1.36 ± 0.29 | 1412.0935 ± 0.0017 | 0.0094 ± 0.0023 | 16.0 ± 1.3 | 13.0 ± 1.2 | 26.8 ± 2.5 | 54193.76 ± 0.44 |
| 14 | 0.79 ± 0.39 | 1412.1386 ± 0.0033 | 0.0105 ± 0.0049 | 17.6 ± 2.4 | 7.4 ± 8.0 | 14.7 ± 2.8 | 54182.46 ± 0.84 |
| 15 | 14.99 ± 2.56 | 1412.1953 ± 0.0378 | 0.1349 ± 0.0181 | −11.5 ± 0.5 | −11.1 ± 0.8 | −11.5 ± 0.6 | 54168.24 ± 9.47 |
| 16 | 6.81 ± 1.40 | 1412.1989 ± 0.0026 | 0.0335 ± 0.0032 | 9.2 ± 0.6 | 10.4 ± 0.9 | 8.0 ± 0.7 | 54167.35 ± 0.64 |
| 17 | 3.95 ± 0.29 | 1412.3056 ± 0.0004 | 0.0091 ± 0.0007 | 54140.62 ± 0.10 | |||
| 18 | 16.52 ± 1.51 | 1412.3329 ± 0.0013 | 0.0354 ± 0.0015 | 6.8 ± 0.2 | 6.3 ± 0.3 | 7.0 ± 0.3 | 54133.77 ± 0.32 |
| 19 | 5.30 ± 1.59 | 1412.4760 ± 0.0155 | 0.0733 ± 0.0078 | −13.4 ± 1.1 | −11.5 ± 1.3 | −14.6 ± 1.3 | 54097.91 ± 3.89 |
| 20 | 1.01 ± 0.12 | 1412.7497 ± 0.0017 | 0.0130 ± 0.0019 | 7.7 ± 2.0 | 9.5 ± 2.4 | 5.6 ± 2.4 | 54029.34 ± 0.43 |
| 21 | 7.97 ± 0.08 | 1412.9354 ± 0.0004 | 0.0358 ± 0.0005 | 2.1 ± 0.4 | 1.9 ± 0.5 | 2.2 ± 0.5 | 53982.86 ± 0.10 |
| 22 | 3.73 ± 0.05 | 1413.0107 ± 0.0024 | 0.1782 ± 0.0022 | 53964.01 ± 0.61 | |||
| 23 | 0.98 ± 0.08 | 1414.5672 ± 0.0026 | 0.0277 ± 0.0026 | 53574.74 ± 0.64 |
Notes. Column (1) numbers the Gaussian components. Columns (2)−(4) present the fit parameters (peak flux density, line center, and line width) with their 1σ uncertainties. Column (5) shows the derived magnetic field strength and its uncertainty, where values annotated with an asterisk designate components attributed to the 1665 MHz OH transition (using a splitting coefficient of 3.270 Hz μG−1). When these emissions are instead assumed to be dominated by 1667 MHz OH transition using a splitting coefficient of 1.964 Hz μG−1, the derived values are 6.1 ± 1.5 mG and 10.9 ± 2.2 mG for Gaussian components 4 and 5, respectively. Columns (6) and (7) separately list magnetic field values obtained from fitting the first- and second-epoch observations independently. Column (8) gives the heliocentric velocities, and the dagger denotes values corresponding to the assumed 1665 MHz OH maser components.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.