Table 3.
Parameters of RX J1605.3+3249, as extracted from the EPIC images in the AO14 and 2012 observations.
| Parameter/obsid | 0764460201 | 0764460301 | 0764460401 | 0764460501 | 0671620101⋆ |
|---|---|---|---|---|---|
| Detection likelihood | 2.5 × 106 | 1.4 × 106 | 1.2 × 106 | 1.2 × 106 | 0.9 × 106 |
| Counts | 4.360(7) × 105 | 2.458(5) × 105 | 2.185(5) × 105 | 2.262(5) × 105 | 1.669(5) × 105 |
| ...0.2–0.5 keV | 2.579(5) × 105 | 1.456(4) × 105 | 1.305(4) × 105 | 1.331(4) × 105 | 0.987(3) × 105 |
| ...0.5–1.0 keV | 1.669(4) × 105 | 0.939(3) × 105 | 0.823(3) × 105 | 0.872(3) × 105 | 0.6356(27) × 105 |
| ...1.0–2.0 keV | 1.11(12) × 104 | 0.625(9) × 104 | 0.566(8) × 104 | 0.586(9) × 104 | 0.462(8) × 104 |
| Rate (s−1) | 4.278(7) | 4.326(9) | 4.226(10) | 4.351(10) | 4.379(12) |
| Rate (frame−1 camera−1) | |||||
| ...pn | 0.2832(4) | 0.2861(6) | 0.2804(6) | 0.2861(6) | 0.2842(7) |
| ...MOS1 | 0.5601(21) | 0.5992(28) | 0.5283(27) | 0.5921(29) | 1.589(10)† |
| ...MOS2 | 0.6338(22) | 0.6328(9) | 0.639(3) | 0.641(3) | 1.889(11)† |
| ‡HR1 | −0.2142(15) | −0.2160(21) | −0.2262(23) | −0.2082(22) | −0.2164(26) |
| ‡HR2 | −0.8757(13) | −0.8753(17) | −0.8714(18) | −0.8740(18) | −0.8644(21) |
| ‡HR3 | −0.9975(13) | −0.9958(21) | −0.9993(16) | −0.9994(12) | −0.9955(26) |
| RA (h min sec) | 16 05 18.5(6) | 16 05 18.5(6) | 16 05 18.5(7) | 16 05 18.5(8) | 16 05 18.4(9) |
| Dec (d m s) | +32 49 19.3(5) | +32 49 19.2(5) | +32 49 19.7(6) | +32 49 19.6(7) | +32 49 18.7(8) |
| RA offset (″) | −0.6 ± 0.4 | +0.2 ± 0.3 | −0.7 ± 0.4 | −0.2 ± 0.5 | −1.2 ± 0.3 |
| Dec offset (″) | +1.1 ± 0.3 | +1.0 ± 0.3 | +0.5 ± 0.4 | +0.9 ± 0.5 | −0.3 ± 0.5 |
| Reference sources | 56 | 53 | 50 | 49 | 38 |
Notes. Counts and rates are given in the total XMM-Newton energy band (0.2–12 keV), unless otherwise specified. The EPIC source coordinates RA and Dec are astrometrically corrected, using as reference the GSC 2.3.2 catalogue (see text). The corresponding 1σ errors take into account the astrometric errors in each coordinate. ( ⋆ )The source parameters, as extracted from the 2012 observation (obsid 0671620101), are shown for comparison. ( † )The 2012 MOS observations were operated in full-frame mode, yielding higher counts per frame in comparison with the AO14 MOS exposures. ( ‡ )Hardness ratios (HR) are ratios of the difference to total counts in two contiguous of the first four XMM-Newton energy bands.
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