Table 7.
Probabilities related to the local sample.
| FXRT | doffset | Pch | Pdist.FXRT(†) | N | P(X = 1|M < Mhost |
|---|---|---|---|---|---|
| (arcmin) | (M < Mhost) | ∧d ≤ doffset) (††) | |||
| (1) | (2) | (3) | (4) | (5) | (6) |
| 1 | 12.2 | 3.5e × 10−4 | 3.0 × 10−3 | 134 | 0.27 |
| 2 | 0.4 | 8.4 × 10−7 | 3.3 × 10−6 | 216 | 7.0 × 10−4 |
| 3 | 5.5 | 1.3 × 10−5 | 6.2 × 10−4 | 29 | 1.7 × 10−2 |
| 4 | 0.4 | 1.9 × 10−6 | 3.3 × 10−6 | 303 | 9.9 × 10−4 |
| 5 | 1.3 | 2.8 × 10−6 | 3.5 × 10−5 | 114 | 3.9 × 10−3 |
| 6 | 1.2 | 1.5 × 10−4 | 2.9 × 10−5 | 508 | 1.5 × 10−2 |
| 11 | 2.7 | 0.15 | 1.5 × 10−4 | 571 | 7.8 × 10−2 |
Notes. Column 1: FXRT candidate number. Column 2: Angular offset of the local FXRT, in arcmin, from its associated host galaxy center. Column 3: Probability of a random chance alignment between an FXRT and a nearby galaxy at least as bright as the associated host galaxy. Column 4: Probability of finding a distant FXRT at an angular offset doffset. Column 5: Number of Chandra observations that include a nearby galaxy at least as bright as the associated host galaxy. Column 6: Probability of finding one (X = 1) distant FXRT given a cut distant offset (d < doffset) and host galaxy magnitude (M < Mhost).
Using Poisson statistic, P(k; λ), for one source, k = 1, and λ is equal to the density of distant FXRTs, ≈6.5 × 10−6 arcmin−2, multiplied by the circular area defined with a radius equal to the angular offset.
Using Binomial statistic, P(k; N; Pdis.FXRT), for number of trials, N(M < Mhost), number of success events (in this case X = 1), and success probability of Pdist.FXRT (see Sect. 3.5).
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