Introduction Phase-Averaged Phase-Resolved Outlook PSR B Monitoring with RXTE from 1996 to Katja Pottschmidt (UCSD) May 2007
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1 Monitoring with RXTE from 1996 to 2005 May 2007 S. Suchy (UCSD), J. Wilms (FAU), S. Haney (UCSB) R.E. Rothschild (UCSD)
2 Source current RXTE-PCA PCU 2 rate, 3 20 kev top layer: 14.5 counts/s (Crab 1800 counts/s) D 4.2 kpc P 150 ms unusually high Ṗ characteristic age 1600 yr Ginga (Kawai 93) CGRO (Ulmer 93, Matz 94, Kuiper 99) RXTE (Marsden 97, Rots 98) BeppoSax (Cusumano 01) Chandra (Yatsu 05, DeLaney 05) INTEGRAL (Forot 06)
3 RXTE Monitoring about 1 ObsID/month here: AO1 AO PCA calibration epochs 3 5 average exposure 2.7 ks 4.1 ks in 2001, for less PCUs HEXTE not rocking in epoch : 6 ObsIDs offset : no GoodXenon : enhanced bkg : short Exposure [ks] JD
4 RXTE: Timing & Early Spectra Phase-Coherent Timing Livingstone et al., 2005 radio & RXTE-PCA residuals wrt Taylor expansion in Φ (3rd-5th derivative in ν) Early Spectra Marsden et al. (1997) Rots et al. (1998) monitoring aspect not explored
5 Spectroscopy Outline Pulse-phase-averaged monitoring (PCA) time-averaged (PCA+HEXTE) Pulse-phase-resolved (work in progress) monitoring (PCA on-pulse) time-averaged (PCA+HEXTE) determine source stability Goals identify possible calibration effects most detailed phase-resolved analysis
6 Rates 3-20 kev, top layer faint bkg subtracted version emv all available PCUs <1999: 5 PCUs on >1999: <5 PCUs on >2001: sub-obsids, different # of PCUs PCU 2 on during all ObsIDs best calibrated gradual decrease, modeled in response Rate [cps] JD
7 Rates 3-20 kev, top layer faint bkg subtracted version emv all available PCUs <1999: 5 PCUs on >1999: <5 PCUs on >2001: sub-obsids, different # of PCUs Rate [cps] JD PCU 2 on during all ObsIDs best calibrated gradual decrease, modeled in response
8 Spectral Model phabs*(power+gauss) 3-20 kev, faint bkg background as correction files no systematics, typical χ 2 red = Standard2f Data Mode all available PCUs 1 all parameters free (E Fe, σ Fe restricted), top layer 2 the same for all layers PCU 2, top layer 1 all parameters free (E Fe, σ Fe restricted) 2 E Fe =6.4 kev, σ Fe =0.1 3 N H = 0.6
9 Spectral Fit Parameters N H a Typical Monitoring Observation = Γ = A Γ b = E Fe [kev] = σ Fe [kev] = A Fe c = EW [ev] = 133 = 9.6 A bkgcorr [%] = 5.4 F 4 10 kev d a /cm 2, b 10 2 ph kevcm 2 c 10 4 ph cm 2 s, d erg cm 2 s Norm. Counts s 1 kev 1 χ χ χ Power Law ObsID Date 10/09/2003 Exposure 4.9 ks Power Law + Gauss Power Law + Gauss, Fe Norm=0 10 Energy [kev] PCU 2 Top Layer χ 2 red=1.4 χ 2 red=0.9 χ 2 red=2.0
10 (Absorbed) Flux Evolution all available PCUs 7% down since 2000 clear drop at epoch 4/5 boundary calibration effect PCU 2 no drop at epoch 4/5 boundary maybe gradual decline of 2% since 2000 calibration? use PCU 2 data for time-averaged and phase-resolved 4 10 kev Flux [10 11 erg s 1 cm 2 ] JD
11 (Absorbed) Flux Evolution all available PCUs 7% down since 2000 clear drop at epoch 4/5 boundary calibration effect PCU 2 no drop at epoch 4/5 boundary maybe gradual decline of 2% since 2000 calibration? use PCU 2 data for time-averaged and phase-resolved 4 10 kev Flux [10 11 erg s 1 cm 2 ] JD
12 Power Law Norm & N H Calibration effect visible in other parameters? all available PCUs 10% drop in power law normalization N H increasingly difficult to determine PCU 2 no drop in power law normalization why 2% flux drop? N H constrained to < cm 2 only Γ Norm [10 2 ph kev 1 cm 2 s 1 kev] JD
13 Power Law Norm & N H Calibration effect visible in other parameters? all available PCUs 10% drop in power law normalization N H increasingly difficult to determine PCU 2 no drop in power law normalization why 2% flux drop? N H constrained to < cm 2 only N H [10 22 cm 2 ] JD
14 Power Law Norm & N H Calibration effect visible in other parameters? all available PCUs 10% drop in power law normalization N H increasingly difficult to determine PCU 2 no drop in power law normalization why 2% flux drop? N H constrained to < cm 2 only Γ Norm [10 2 ph kev 1 cm 2 s 1 kev] JD
15 Power Law Index PCU kev flux drop marginally softer 1 kev) Gaussian distribution with Γ=2.03, σ Γ = JD all available PCUs no trend in Γ Γ 2.00 Gaussian distribution with Γ=2.02, σ Γ =
16 Power Law Index PCU kev flux drop marginally softer 1 kev) Gaussian distribution with Γ=2.03, σ Γ =0.05 all available PCUs no trend in Γ Gaussian distribution with Γ=2.02, σ Γ =0.03 Number of Observations Γ
17 Power Law Index PCU kev flux drop marginally softer 1 kev) Gaussian distribution with Γ=2.03, σ Γ =0.05 all available PCUs no trend in Γ Gaussian distribution with Γ=2.02, σ Γ =0.03 Number of Observations Γ
18 Iron Line PCU 2 E Fe constrainable to 6 7 kev (uncertainties often peg) σ Fe consistent with 0 norm not consistent with 0 norm stable and, especially for frozen E Fe and σ Fe, well constrained Fe Line Norm [10 4 ph cm 2 s 1 ] JD
19 Iron Line PCU 2 E Fe constrainable to 6 7 kev (uncertainties often peg) σ Fe consistent with 0 norm not consistent with 0 norm stable and, especially for frozen E Fe and σ Fe, well constrained Fe Line Norm [10 4 ph cm 2 s 1 ] JD
20 Long-Term Stability, PCU 2 Avg. Parameter exposure [ks] 2.8± ± kev rate [cps] 15.82± ± kev flux [10 11 erg ] 9.92± ±0.02 cm 2 s A Γ [10 2 N H [10 22 cm 2 ] 0.54± ±0.07 Γ 2.02± ±0.01 1keV] 0.071± ±0.001 kevcm 2 s bkg correction [%] 2±1 0.3±3 χ 2 red 0.68± ±0.05
21 Epoch-Averaged Spectra PCU 2 Top: 3 25 kev 0.5% systematics epoch 5: Xe L edge HEXTE: epoch 3: no bkg epoch 4: kev epoch 5: kev Previous background model, fits will be redone. normalized counts/s/kev χ χ Epoch 4 PCU2 Top Layer HEXTE without Fe with Fe Energy [kev]
22 Epoch-Averaged Spectra PCU 2 Top: 3 25 kev 0.5% systematics epoch 5: Xe L edge HEXTE: epoch 3: no bkg epoch 4: kev epoch 5: kev Previous background model, fits will be redone. normalized counts/s/kev χ χ Epoch 5 PCU2 Top Layer HEXTE without Fe with Fe Energy [kev]
23 Epoch-Averaged Parameters Parameter Epoch 3 Epoch 4 Epoch 5 exp. PCA/HEXTE [ks] 81.2/ 37.6/ /179.7 N H [10 22 /cm 2 ] Γ EW F 4 10 kev [10 11 erg ] cm 2 s flux constant (HEXTE) χ 2 red/dof 0.83/ / /89
24 Monitoring Pulse Profiles Extraction filter GoodXenon rsp, bkg: seextract pha2 (Φ- & E-bins): (ik)fasebin 5 ephemrides from Φ: -0.05, 0., 0., 0.02, 0. offset from radio by 0.27 (Kawai et al., 1991) Examples 1/ephemeris, random 3 40 kev, 0.05 Φ-bins normalized to off-pulse Norm. Count Rate [cps] Peak Off PCU 2 Top Layer Pulse Phase
25 Monitoring Pulse Profiles Extraction filter GoodXenon rsp, bkg: seextract pha2 (Φ- & E-bins): (ik)fasebin 5 ephemrides from Φ: -0.05, 0., 0., 0.02, 0. offset from radio by 0.27 (Kawai et al., 1991) Examples 1/ephemeris, random 3 40 kev, 0.05 Φ-bins normalized to off-pulse Norm. Count Rate [cps] Peak Off PCU 2 Top Layer Pulse Phase
26 Monitoring Pulse Profiles Extraction filter GoodXenon rsp, bkg: seextract pha2 (Φ- & E-bins): (ik)fasebin 5 ephemrides from Φ: -0.05, 0., 0., 0.02, 0. offset from radio by 0.27 (Kawai et al., 1991) Examples 1/ephemeris, random 3 40 kev, 0.05 Φ-bins normalized to off-pulse Norm. Count Rate [cps] Peak Off PCU 2 Top Layer Pulse Phase
27 Monitoring Pulse Profiles Extraction filter GoodXenon rsp, bkg: seextract pha2 (Φ- & E-bins): (ik)fasebin 5 ephemrides from Φ: -0.05, 0., 0., 0.02, 0. offset from radio by 0.27 (Kawai et al., 1991) Examples 1/ephemeris, random 3 40 kev, 0.05 Φ-bins normalized to off-pulse Norm. Count Rate [cps] Peak Off PCU 2 Top Layer Pulse Phase
28 Monitoring Pulse Profiles Extraction filter GoodXenon rsp, bkg: seextract pha2 (Φ- & E-bins): (ik)fasebin 5 ephemrides from Φ: -0.05, 0., 0., 0.02, 0. offset from radio by 0.27 (Kawai et al., 1991) Examples 1/ephemeris, random 3 40 kev, 0.05 Φ-bins normalized to off-pulse Norm. Count Rate [cps] Peak Off PCU 2 Top Layer Pulse Phase
29 Pulse Off-Pulse Fit add sub-obsids Φ= peak.pha Φ= off.pha (Rots et al., 1998) data 1:1 peak.pha back 1:1 off.pha phabs power Typical Parameters N H [10 22 cm 2 ] = Γ = a A Γ = b F 4 10 kev = 4.4 a 10 2 ph kevcm 2 1keV, b erg cm 2 s Norm. Counts s 1 kev Off ObsID Date 10/09/ Energy [kev] PCU 2 Top Layer Peak
30 Pulse Off-Pulse Fit add sub-obsids Φ= peak.pha Φ= off.pha (Rots et al., 1998) 1.0 PCU 2 Top Layer data 1:1 peak.pha back 1:1 off.pha phabs power Typical Parameters Norm. Counts s 1 kev ObsID Date 10/09/2003 Peak Off N H [10 22 cm 2 ] = Γ = a A Γ b F 4 10 kev a 10 2 ph kevcm 2 1keV, b erg cm 2 s = = 4.4 χ Power Law χ 2 red= Energy [kev]
31 Pulsed Rate & Flux Evolution rates less constrained, still overall declining F 4 10 kev : no trend F kev : decline? (pulsed flux harder) 1996/ /2005 flux comparison: 3 5% decline Rate [cps] JD Average General Parameters χ 2 red =1.00 ± 0.05 exposures: 1.02(4) ks 1.52(7) ks
32 Pulsed Rate & Flux Evolution rates less constrained, still overall declining F 4 10 kev : no trend F kev : decline? (pulsed flux harder) 1996/ /2005 flux comparison: 3 5% decline Average General Parameters χ 2 red =1.00 ± 0.05 exposures: 1.02(4) ks 1.52(7) ks 4 10 kev Flux [10 11 erg s 1 cm 2 ] JD
33 Pulsed Rate & Flux Evolution rates less constrained, still overall declining F 4 10 kev : no trend F kev : decline? (pulsed flux harder) 1996/ /2005 flux comparison: 3 5% decline Average General Parameters χ 2 red =1.00 ± 0.05 exposures: 1.02(4) ks 1.52(7) ks kev Flux [10 11 erg s 1 cm 2 ] JD
34 Pulsed Component N H & Γ Comparison to phase-averaged average N H : (2 3) cm 2 (mostly consist. with 0) harder, Gaussian distribution: Γ=1.36, σ Γ =0.11 Consistent with previous time-averaged results: Kawai et al., 93: N H, Γ 1.30(5) Γ JD phase averaged Γ Rots et al., 98: N H, Γ 1.35(1)
35 Pulsed Component N H & Γ Comparison to phase-averaged average N H : (2 3) cm 2 (mostly consist. with 0) harder, Gaussian distribution: Γ=1.36, σ Γ =0.11 Consistent with previous time-averaged results: Kawai et al., 93: N H, Γ 1.30(5) Rots et al., 98: N H, Γ 1.35(1) Number of Observations Γ
36 Epoch-Averaged Pulse Profiles 25 Epoch 3 Epoch 4 Epoch ks 37.6 ks ks 20 Next Step phase-resolved spectroscopy for Φ 0.03 bins highest resolution so far (?) Count Rate [cps] Epoch kev PCU 2 Top Layer Pulse Phase
37 Epoch-Averaged Pulse Profiles 25 Epoch 3 Epoch 4 Epoch ks 37.6 ks ks 20 Next Step phase-resolved spectroscopy for Φ 0.03 bins highest resolution so far (?) Count Rate [cps] Epoch kev PCU 2 Top Layer Pulse Phase
38 Epoch-Averaged Pulse Profiles 25 Epoch 3 Epoch 4 Epoch ks 37.6 ks ks 20 Next Step phase-resolved spectroscopy for Φ 0.03 bins highest resolution so far (?) Count Rate [cps] Epoch kev PCU 2 Top Layer Pulse Phase
39 To Do revise PCA+HEXTE epoch averaged & phase-averaged spectra create HEXTE epoch averaged pulse profiles check energy dependence of the pulse profiles model PCA+HEXTE epoch averaged & phase-resolved spectra are the (calibration) trends F, Γ, N H also visible in: other PCUs individually? other 0.01 Crab sources?
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1 SUMMARY 1 G21.5-0.9 1 Summary Distance: 5 kpc ( Safi-Harb et al., 2001 ) Position of Central Source (J2000): ( 18 33 34.0, -10 34 15.3 ) X-ray size: 4.7 x4.6 Description: 1.1 Summary of Chandra Observations
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1 SUMMARY 1 SNR 0505-67.9 1 Summary Common Name: DEM L71 Distance: 50 kpc (distance to LMC, Westerlund(1990) ) Center of X-ray emission (J2000): ( 05 05 42.0, -67 52 39.8 ) X-ray size: 86 x 74 Description:
Sequence Obs ID Instrument Exposure uf Exposure f Date Observed Aimpoint (J2000) (ks) (ks) (α, δ)
1 SUMMARY 1 G120.1+01.4 1 Summary Common Name: Tycho s Distance: 2.4 kpc ( Chevalier et al., 1980 ) Center of X-ray emission (J2000): ( 00 25 19.9, 64 08 18.2 ) X-ray size: 8.7 x8.6 Description: 1.1 Summary
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1 SUMMARY 1 SNR 0525-66.1 1 Summary Common Name: N 49 Distance: 50 kpc (distance to LMC, Westerlund(1990) ) Position of Central Source (J2000): ( 05 25 59.9, -66 04 50.8 ) X-ray size: 85 x 65 Description:??
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