Table 1.

XMMNewton observations used in this paper.

OBS_IDDateStateFluxtRGS1, 2tpntMOS1tMOS2NotesStacking
(⁠|$\rm {photons \, m}^{-2}\, \rm {s}^{-1}$|⁠)(ks)(ks)(ks)(ks)group
04050901012006-10-15Low–Int7.897819999OLD L–I
06938505012012-12-16Low–Int10.111290114113OLD L–I
06938512012012-12-22Low–Int11.011785122121OLD L–I
07425903012014-07-05Int–Bright18.162546161(*)
07945806012017-03-29Low–Int11.041263937(*)
08039901012017-06-14Int–Bright15.5131109128128NEW I–B
08039902012017-06-20Int–Bright13.5130111129128NEW I–B
08039903012017-08-31Low–Int8.6109427064(**)NEW L–I
08039904012017-09-02Low–Int8.5115535046(**)NEW L–I
08039907012017-09-24Low–Int9.1121111010(***)NEW L–I
08039905012017-12-07Int–Bright12.090608986(**)NEW I–B
08039906012017-12-09Int–Bright14.710971117116(**)NEW I–B
OBS_IDDateStateFluxtRGS1, 2tpntMOS1tMOS2NotesStacking
(⁠|$\rm {photons \, m}^{-2}\, \rm {s}^{-1}$|⁠)(ks)(ks)(ks)(ks)group
04050901012006-10-15Low–Int7.897819999OLD L–I
06938505012012-12-16Low–Int10.111290114113OLD L–I
06938512012012-12-22Low–Int11.011785122121OLD L–I
07425903012014-07-05Int–Bright18.162546161(*)
07945806012017-03-29Low–Int11.041263937(*)
08039901012017-06-14Int–Bright15.5131109128128NEW I–B
08039902012017-06-20Int–Bright13.5130111129128NEW I–B
08039903012017-08-31Low–Int8.6109427064(**)NEW L–I
08039904012017-09-02Low–Int8.5115535046(**)NEW L–I
08039907012017-09-24Low–Int9.1121111010(***)NEW L–I
08039905012017-12-07Int–Bright12.090608986(**)NEW I–B
08039906012017-12-09Int–Bright14.710971117116(**)NEW I–B

Notes. The ULX state refers to the low-to-intermediate and intermediate-to-bright flux levels, primarily chosen from the total flux and shape of the X-ray spectra (see Figs 2 and A1). Absorbed 0.3–10 keV fluxes are computed with a multicomponent model consisting of two modified blackbody components plus comptonization corrected for Galactic absorption (see Section 3.1). Exposure times account for background flaring removal. (*) RGS spectra contaminated by either X-2 or SNR (only EPIC-pn is used for PCA); (**) EPIC cameras affected by solar flares; (***) Additional calibration exposure (only RGS is operating for the full orbit).The acronyms OLD L–I, NEW L–I, and NEW I–B stay for old low–intermediate, new low–intermediate, and new intermediate–bright states.

Table 1.

XMMNewton observations used in this paper.

OBS_IDDateStateFluxtRGS1, 2tpntMOS1tMOS2NotesStacking
(⁠|$\rm {photons \, m}^{-2}\, \rm {s}^{-1}$|⁠)(ks)(ks)(ks)(ks)group
04050901012006-10-15Low–Int7.897819999OLD L–I
06938505012012-12-16Low–Int10.111290114113OLD L–I
06938512012012-12-22Low–Int11.011785122121OLD L–I
07425903012014-07-05Int–Bright18.162546161(*)
07945806012017-03-29Low–Int11.041263937(*)
08039901012017-06-14Int–Bright15.5131109128128NEW I–B
08039902012017-06-20Int–Bright13.5130111129128NEW I–B
08039903012017-08-31Low–Int8.6109427064(**)NEW L–I
08039904012017-09-02Low–Int8.5115535046(**)NEW L–I
08039907012017-09-24Low–Int9.1121111010(***)NEW L–I
08039905012017-12-07Int–Bright12.090608986(**)NEW I–B
08039906012017-12-09Int–Bright14.710971117116(**)NEW I–B
OBS_IDDateStateFluxtRGS1, 2tpntMOS1tMOS2NotesStacking
(⁠|$\rm {photons \, m}^{-2}\, \rm {s}^{-1}$|⁠)(ks)(ks)(ks)(ks)group
04050901012006-10-15Low–Int7.897819999OLD L–I
06938505012012-12-16Low–Int10.111290114113OLD L–I
06938512012012-12-22Low–Int11.011785122121OLD L–I
07425903012014-07-05Int–Bright18.162546161(*)
07945806012017-03-29Low–Int11.041263937(*)
08039901012017-06-14Int–Bright15.5131109128128NEW I–B
08039902012017-06-20Int–Bright13.5130111129128NEW I–B
08039903012017-08-31Low–Int8.6109427064(**)NEW L–I
08039904012017-09-02Low–Int8.5115535046(**)NEW L–I
08039907012017-09-24Low–Int9.1121111010(***)NEW L–I
08039905012017-12-07Int–Bright12.090608986(**)NEW I–B
08039906012017-12-09Int–Bright14.710971117116(**)NEW I–B

Notes. The ULX state refers to the low-to-intermediate and intermediate-to-bright flux levels, primarily chosen from the total flux and shape of the X-ray spectra (see Figs 2 and A1). Absorbed 0.3–10 keV fluxes are computed with a multicomponent model consisting of two modified blackbody components plus comptonization corrected for Galactic absorption (see Section 3.1). Exposure times account for background flaring removal. (*) RGS spectra contaminated by either X-2 or SNR (only EPIC-pn is used for PCA); (**) EPIC cameras affected by solar flares; (***) Additional calibration exposure (only RGS is operating for the full orbit).The acronyms OLD L–I, NEW L–I, and NEW I–B stay for old low–intermediate, new low–intermediate, and new intermediate–bright states.

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