Table 1
Summary of the most recent studies (along with the original work of Iwasawa & Taniguchi 1993) of the X-ray Baldwin effect.
| (1) | (2) | (3) | (4) | (5) |
| Reference | A | B | Sample | Observatory/instrument |
|
|
||||
| Fits per observation | ||||
|
|
||||
| Shu et al. (2012) | 1.58 ± 0.03 ∗ | −0.18 ± 0.03 | 32 (RQ) | Chandra/HEG |
| Shu et al. (2010) | 1.58 ± 0.03 ∗ | −0.22 ± 0.03 | 33 (RQ+RL) | Chandra/HEG |
| Bianchi et al. (2007) | 1.73 ± 0.03 | −0.17 ± 0.03 | 157 (RQ) | XMM-Newton/EPIC |
| Jiang et al. (2006) | – | −0.20 ± 0.04 | 101 (RL+RQ) | XMM-Newton/EPIC + Chandra/HEG |
| Jiang et al. (2006) | – | −0.10 ± 0.05 | 75 (RQ) | XMM-Newton/EPIC + Chandra/HEG |
| Jiménez-Bailón et al. (2005) | – | −0.06 ± 0.20 | 38 (RQ) | XMM-Newton/EPIC |
| Zhou & Wang (2005) | – | −0.19 ± 0.04 | 66 (RQ+RL) | XMM-Newton/EPIC |
| Page et al. (2004) | – | −0.17 ± 0.08 | 53 (RQ+RL) | XMM-Newton/EPIC |
| Iwasawa & Taniguchi (1993) | – | −0.20 ± 0.03 | 37 (RQ+RL) | Ginga |
|
|
||||
| Fits per source | ||||
|
|
||||
| Shu et al. (2012) | 1.64 ± 0.03* | −0.11 ± 0.03 | 32 (RQ) | Chandra/HEG |
| Shu et al. (2010) | 1.63 ± 0.04* | −0.13 ± 0.04 | 33 (RQ+RL) | Chandra/HEG |
Notes. The model commonly used to fit the data is log EW = A + Blog LX,44, where LX,44 is the 2–10 keV luminosity in units of 1044 erg s. The table is divided into works for which the fit was done per observation (i.e., using all the available observations for every source of the sample) and per source (i.e., averaging the values of EW and L X of different observations of the same source). The table lists (1) the reference; (2) the value of the intercept; (3) the value of the slope; (4) the number and type of objects in the sample; (5) the observatory and instrument used. Dashes are given when the value is not available.
These values of the intercepts were corrected in order to be consistent with Eq. (5), because those reported in Shu et al. (2010, 2012) are relative to the 2–10 keV luminosity in units of 1043 erg s (LX,43).
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