Table 2.
Parameters of the best-fit spectral models to the observed XMM-Newton EPIC PN spectrum of Ho II X-1 (ObsID:0864550501).
| Tbabs×(bbody+diskpbb) | Tbabs×(diskbb+diskbb) | ||||||
|---|---|---|---|---|---|---|---|
| Component | Parameter | Unit | Value | Component | Parameter | Unit | Value |
| Tbabs | NH | 1021 cm−2 | 1.02 ± 0.05 | Tbabs | NH | 1021 cm−2 | 0.68 ± 0.04 |
| bbody | kT | keV | 0.182 ± 0.005 | diskbb | Tin | keV | 0.31 ± 0.01 |
| bbody | Norm | (3.0 ± 0.2)×10−5 | diskbb | Norm | 29 ± 4 | ||
| diskpbb | Tin | keV | 1.95 ± 0.07 | diskbb | Tin | keV | 1.46 ± 0.04 |
| diskpbb | p | 0.5 | diskbb | Norm | (4.2 ± 0.5)×10−2 | ||
| diskpbb | Norm | (3.9 ± 0.6)×10−3 | |||||
| LX = (1.18 ± 0.02)×1040 erg s−1 | LX = (1.02 ± 0.01)×1040 erg s−1 | ||||||
| χ2/d.o.f. 131/144 | χ2/d.o.f. 175/144 | ||||||
| Tbabs×(diskbb+comptt) | Tbabs×redden×diskir | ||||||
| Component | Parameter | Unit | Value | Component | Parameter | Unit | Value |
| Tbabs | NH | 1021 cm−2 | 1.21 ± 0.01 | Tbabs | NH | 1021 cm−2 | 0.13 ± 0.01 |
| diskbb | Tin | keV | 0.17 ± 0.01 | redden | E(B − V) | 0.05 | |
| diskbb | norm | 329 ± 104 | diskir | kTdisk | keV | 0.18 ± 0.01 | |
| compTT | redshift | 0 | diskir | Γ | 2.16 ± 0.04 | ||
| compTT | T0 | keV | 0.17 ± 0.01 | diskir | kTe | keV | 2 |
| compTT | kT | keV | 2.8 ± 0.8 | diskir | Lc/Ld | 0.83 ± 0.05 | |
| compTT | τp | 4.5 ± 0.9 | diskir | fin | 0.1 | ||
| compTT | Approx | 1 | diskir | rirr | 1.1 | ||
| compTT | Norm | (1.6 ± 0.3)×10−3 | diskir | fout | 5 × 10−4 | ||
| diskir | log rout | 7 | |||||
| diskir | Norm | 324 ± 88 | |||||
| LX = (1.3 ± 0.8)×1040 erg s−1 | LX = (1.3 ± 0.7)×1040 erg s−1 | ||||||
| χ2/d.o.f. 109/144 | χ2/d.o.f. 128/141 | ||||||
Notes. The spectral fitting was done using the XSPEC X-ray spectral fitting software (Arnaud 1996, see detailed description of the models in the XSPEC manual). The ISM absorption towards Ho II X-1 is included using the Tbabs model (Wilms et al. 2000). Four models, previously discussed in the literature to model the X-ray spectra of Ho II X-1 are fitted as is shown in the four quadrants in the table. In each quadrant, the first column gives the name of the spectral component of the corresponding model in XSPEC, the second column gives the model parameter, the third column gives units, and the fourth column gives the value and the error of the corresponding parameter. Those values that do not have an associated error in the table were fixed during the fitting process. In the Tbabs×(bbody+diskpbb) model, p is fixed at 0.5 (Kajava et al. 2012). In the Tbabs×(diskbb+comptt) model the seed temperature for the comptt model is fixed as being the same as the Tin in the diskbb model (Pintore et al. 2014). In the Tbabs×redden×diskir model, Te, fin and rirr are fixed during the fitting (Tao et al. 2011). LX is calculated for a distance of 3.05 Mpc.
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