XMM-Newton's view of the multiple uorescence lines of GX 301 2

Transcription

1 XMM-Newton's view of the multiple uorescence lines of GX 31 2 Felix Fürst Dr. Karl Remeis-Sternwarte Bamberg Erlangen Centre for Astroparticle Physics (ECAP) Friedrich-Alexander-University Erlangen-Nuremberg Slawo Suchy, ngo Kreykenbohm, Laura Barragán, Jörn Wilms, Katja Pottschmidt, sabel Caballero, Peter Kretschmar, José Miguel Torrejón, Sebastian Müller, Matthias Kühnel, Carlo Ferrigno, Richard E. Rothschild June 28th 211 The X-ray Universe 211 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 1 / 18

2 The system HMXB with 4 M, B1 a+ companion (Kaper et al., 26) very bright pre-periastron are accretion stream (Leahy & Kostka, 28) highly structured, dense medium [lt-sec] [cts sec 1 ] Wray eccentric orbit e = XMM 47ksec Obs To Earth -2 [lt-sec] 2 4 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 2 / 18

3 The overall spectrum 1 1 Cts sec 1 kev χ Energy [kev] 8 1 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 3 / 18

4 The overall spectrum Cts sec 1 kev S Kα Ar Kα Ca Kα Cr Kα Fe Kα Fe Kβ Ni Kα Ni Kβ N H,1 = 141(3) 1 22 cm 2 N H,2 = 54(1) 1 22 cm 2 Γ =.9(2).1 First evidence for χ f) 2 Cr Kα at 5.41 kev Ni Kβ at 8.26 kev Energy [kev] 8 1 best t χ 2 red = 1.2 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 4 / 18

5 The lightcurve and the pulse prole 2 Counts/sec Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 5 / 18

6 The lightcurve and the pulse prole 2 Counts/sec Strong aring activity and pulse period of 685 sec evident using orbital ephemeris by Doroshenko et al. (21) Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 5 / 18

7 The lightcurve and the pulse prole 2 Counts/sec 15 1 cts/sec Phase Strong aring activity and pulse period of 685 sec evident using orbital ephemeris by Doroshenko et al. (21) Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 5 / 18

8 The lightcurve and the pulse prole 2 Counts/sec Strong aring activity and pulse period of 685 sec evident using orbital ephemeris by Doroshenko et al. (21) Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 5 / 18

9 The lightcurve and the pulse prole 2 Counts/sec Strong aring activity and pulse period of 685 sec evident using orbital ephemeris by Doroshenko et al. (21) Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 5 / 18

10 An O-state 8 6 cts/sec Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 6 / 18

11 An O-state 8 6 cts/sec pulses are missing similar to the o-state seen by Gö ü³ et al. (211) similar to Vela X-1 (Kreykenbohm et al., 28) 26 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 6 / 18

12 An O-state 8 6 cts/sec source is still visible no pulsed ux no accretion larger region (> 2 lt-sec) visible in X-rays Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 6 / 18

13 Divide data by states 2 Counts/sec Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 7 / 18

14 Divide data by states 2 a) Counts/sec Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 7 / 18

15 Time resolved spectroscopy Counts/sec cts sec 1 kev med. cont., med abs. 1 : : : : 4 soft cont., high abs. 2 3 hard cont., low abs. 4 Γ =.93(4), N H,1 = 147(6), N H,2 = 59(4) Γ = 1.1(4), N H,1 = 175(5), N H,2 = 47(2) Γ =.78(3), N H,1 = 114(5), N H,2 = 53(4) Γ = 1.5(6), N H,1 = 13(8), N H,2 = 42(9) 6 Energy [kev] 8 1 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 8 / 18

16 Time resolved spectroscopy Counts/sec cts sec 1 kev med. cont., med abs. 1 : : : : 4 soft cont., high abs. 2 3 hard cont., low abs. 4 Γ =.93(4), N H,1 = 147(6), N H,2 = 59(4) Γ = 1.1(4), N H,1 = 175(5), N H,2 = 47(2) Γ =.78(3), N H,1 = 114(5), N H,2 = 53(4) Γ = 1.5(6), N H,1 = 13(8), N H,2 = 42(9) 6 Energy [kev] 8 1 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 8 / 18

17 Time resolved spectroscopy Counts/sec cts sec 1 kev med. cont., med abs. 1 soft cont., high abs. 2 3 : F(Fe Kα) = (8.2 ±.5) 1 3 : F(Fe Kα) = (11. ±.4) 1 3 : F(Fe Kα) = (12.7 ±.7) 1 3 : F(Fe Kα) = (7.8 ±.9) Energy [kev] hard cont., low abs Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 8 / 18

18 Time resolved spectroscopy Counts/sec med. cont., med abs. 1 soft cont., high abs. 2 3 hard cont., low abs. 4 cts sec 1 kev Energy [kev] Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 8 / 18

19 Time resolved spectroscopy Counts/sec 2 med. cont., 1 med abs. Eqw. of Fe Kα highest during part 1 2 soft cont., high abs. 2 3 hard cont., low abs. 4 cts sec 1 kev Energy [kev] Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 8 / 18

20 Time resolved spectroscopy Counts/sec 2 med. cont., 1 med abs. Eqw. of Fe Kα highest during part 1 Spectra change 2 strongly with time. 1 cts sec 1 kev soft cont., high abs. 2 3 hard cont., low abs Energy [kev] Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 8 / 18

21 Pulse-to-pulse spectroscopy 2 cts/sec Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 9 / 18

22 Pulse-to-pulse spectroscopy 2 cts/sec same model as for overall spectrum, but frozen Γ =.9 and N H,2 = cm 2. ncluded only the Fe Kα, Fe Kβ, and Ni Kα line. Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 9 / 18

23 Pulse-to-pulse spectroscopy cts/sec NH,1 15 Cov. Fract Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 1 / 18

24 Pulse-to-pulse spectroscopy cts/sec NH,1 N H strongly variable, indicates structure 15in the accretion material. Cov. Fract Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 1 / 18

25 Pulse-to-pulse spectroscopy cts/sec NH,1 N H strongly variable, indicates structure 15in the accretion material. Cov. Fract. Drop in.9 Covering Fraction can be due to a hole in the material Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 1 / 18

26 Pulse-to-pulse spectroscopy cts/sec 1 5 Eqw. Fe Kα F(Fe Kα) Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 11 / 18

27 Pulse-to-pulse spectroscopy cts/sec 1 5 Eqw. Fe Kα F(Fe Kα) ron line2 ux varies mostly with continuum Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 11 / 18

28 Pulse-to-pulse spectroscopy cts/sec 1 5 Eqw. Fe Kα 15 Eqw. should be proportional to N H 1 in a spherically symmetric absorber model. (noue, 1985) 5 F(Fe Kα) ron line2 ux varies mostly with continuum Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 11 / 18

29 ron line behavior Equivalent width [kev] N H,1 [1 22 H-atoms cm 2 ] 2 22 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 12 / 18

30 ron line behavior 1.8 Corr Equivalent width [kev] Corr N H,1 [1 22 H-atoms cm 2 ] 2 22 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 12 / 18

31 ron line behavior 1.8 Corr.66 O-state shows indication for 1.6 a dierent behavior! Equivalent width [kev] 1.4 X-rays from a dierent region become dominant 1.2 dierent behavior expected Corr N H,1 [1 22 H-atoms cm 2 ] 2 22 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 12 / 18

32 Summary partially covered spectrum with 1 24 cm 2 and expected uorescence lines (including Cr Kα) highly variable ux and N H o-state due to cessation of accretion (residual ux is not pulsed) accreted material must be strongly structured Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 13 / 18

33 O-state and absorber geometry two absorbers with two uorescence regions: main component very close to the neutron star, following the continuum secondary component farther away and more independent of the momentary continuum ux measured N H not necessarily a good tracer for amount of uorescence material as it is highly structured see also Fürst et al., 211, A&A, Suchy et al., 211, ApJ, to be submitted Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 14 / 18

34 Bibliography Doroshenko V., Santangelo A., Suleimanov V., et al., 21, A&A 515, 1 Gö ü³ E., Kreykenbohm., Belloni T.M., 211, A&A 525, L6 noue H., 1985, Space Sci. Rev. 4, 317 Kaper L., van der Meer A., Najarro F., 26, A&A 457, 595 Kreykenbohm., Wilms J., Kretschmar P., et al., 28, A&A 492, 511 Leahy D.A., Kostka M., 28, MNRAS 384, 747 Makino F., Leahy D.A., Kawai N., 1985, Space Sci. Rev. 4, 421 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 15 / 18

35 Pulse-to-pulse spectra cts/sec Norm 2 1 PF (RMS) Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 16 / 18

36 Pulsed fraction behavior.55 Corr pulsed fraction (RMS) N H,1 [1 22 H-atoms cm 2 ] 2 22 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 17 / 18

37 Pulsed fraction behavior.55 Corr..2 No correlation visible,.5 contradicting results by Makino et al..45 (1985)..4 pulsed fraction (RMS) N H,1 [1 22 H-atoms cm 2 ] 2 22 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 17 / 18

38 Pulsed fraction behavior.55 Corr..2 No correlation visible,.5 contradicting results by Makino et al..45 (1985)..4 pulsed fraction (RMS) O-state not due.35 to increased N H N H,1 [1 22 H-atoms cm 2 ] 2 22 Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 17 / 18

39 Pulse-to-pulse spectra cts/sec Norm 2 1 Gainshift Felix Fürst (Dr. Remeis-Sternwarte) XMM-Newton's view of GX /6/28 18 / 18