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TheThe BroadBroad--BandBand XX--rayray SpectrumSpectrumofof CygnusCygnus XX--1 1 MeasuredMeasured by by
INTEGRALINTEGRAL
Marion Cadolle BelService d’Astrophysique, CEA-Saclay, France
Internal INTEGRAL Workshop, Noordwijk, 18 - 21 January 2005
P. Sizun, A. Goldwurm, P. Laurent, A. Zdziarski, J. Malzac, E. Jourdain, J-P. Roques, P. Goldoni, J. Rodriguez, C. Gouiffès & L. Foschini
CygnusCygnus XX--11Bright Bright XX--rayray emissionemission (1964)(1964)
High mass XHigh mass X--ray binaryray binary-- 2 2 kpckpc-- orbital period: 5.6 days orbital period: 5.6 days -- wind accretionwind accretion10 M¤ black hole18 M¤ giant (09.7 I) companion
Complex spectral-timing behaviour- incoherent fast X-ray variability- hard spectrum above 100 keV- persistent X-ray emission
First black hole prototypeFirst black hole prototype
Two Main Spectral StatesTwo Main Spectral States
High/SoftDominant soft X-ray thermal component; photon spectral index = 2.2
Low/Hard (90% time)Low flux for soft X-rays, strong flux for hard photons (keV)Photon spectral index 1.5-2, cut-off at E = 100 keV: comptonization
Low/Hard
High/Soft
McConnell et al. 2002
0,1
0,5
Spec
tral
inde
x
Truncated Julian Days (TJD)Flux
-1,5
-4
8500 10000 11500
Cts
s-1
20
100
BATSE index (20-100 keV)BATSE flux
RXTE counts (1.5-12 keV)
High/Soft Low/Hard
Observation LogObservation Log
PVPV--PhasePhase ((27th November - 15th December, 2002)
GPS (GPS (betweenbetween 2003, March 2003, March andand 2004, 2004, SeptemberSeptember))
Open Open TimeTime ((7 - 11th June, 2003)
Calibration in 2004, Calibration in 2004, NovemberNovember 2222ndnd
ASM Light ASM Light CurveCurve
Spectral transitions Spectral transitions probablyprobably occurringoccurring
1: 1: PVPV--phasephase2: Open 2: Open TimeTime3: GPS3: GPS4: 4: calibratcalibrat..
52600
ASM
Cou
nt R
ate
(cts
s-1)
1.5-
12 k
eV
50
0
100
150
52800 53000 53200 53400Universal Time (MJD)
SimultaneousSimultaneous ASM ASM andand IBIS/ISGRI IBIS/ISGRI LightLight CurvesCurves
Changes in IBIS/ISGRIChanges in IBIS/ISGRI CorrespondingCorresponding hardnesshardness ratio ?ratio ?
52600
ASM
Cou
nt R
ate
(cts
s-1) 1.
5-12
keV
50
0
100
100
52800 53000
200
53200 53400Universal Time (MJD)
ISGR
I Co
unt
Rate
(cts
s-1) 20
-200
keV
This work
52610
200
0
100
300
IBIS
/ISG
RI C
ount
Ra
te (ct
s s-
1 )20
-200
keV
52615 52620
Har
dnes
s ra
tio
20-3
0/30
-40
keV 0.64
0.620.600.580.56
Universal Time (MJD)
Bazzano et al. 03
Time bins ~ 0.15 d
100
050
150
IBIS
/ISG
RI C
ount
Ra
te (ct
s s-
1 )20
-300
keV
Har
dnes
s ra
tio
20-3
0/30
-40
keV
0.60
0.55
0.50
0.45
200
52798 52799 52800Universal Time (MJD)
52801
Zooms on IBIS/ISGRI Light Zooms on IBIS/ISGRI Light CurvesCurvesandand HardnessHardness RatioRatio
CorrespondingCorresponding HardnessHardness RatioRatioHar
dnes
s Ra
tio
40-1
00/2
0-30
keV
1
0.8
0.6
Universal Time (MJD)
1.2
1.4
1.6
52600 52800 53000 53200 53400
1.91.9
2.32.2
1.9
2.32.2
Hard state
Soft state
Photon index
DecemberDecember 02 02 SpectraSpectra
IBIS/ISGRI (128 ks)3% systematics
JEMX (31 ks)3% systematics
SPI (156 ks)3% systematics
kT = 93 +18 keV weak disc component ~ 0.2 Ltot
t = 1.5 ± 0.2 L 0.5-10 keV: 3.8 1036 ergs s-1
Fe line 6.4 ± 0.4 keV not well constrained?2
réd = 1.70 (dof = 219) EW = 223 eV; reflection 0.38 ± 0.05
-12Model = absorbed black body disc + comptonizationAdding then reflection + gaussian components
JuneJune 03 03 SpectraSpectra
kT = 104 ± 16 keV disc: kTin = 1.22 keV, comp. ~ 0.4 Ltott = 0.3 ± 0.1 L 0.5-10 keV: 6.6 1036 ergs s-1
Fe line 7.1 ± 0.1 keV well defined?2
réd = 1.88 (dof = 230) EW = 190 eV; reflection 0.58 ± 0.05
JEMX (200 ks)1% systematics
IBIS/ISGRI (219 ks)3% systematics
SPI (306 ks)3% systematics
IBIS/PICsIT (200 ks)no systematics
GPS 03GPS 03--04 04 SpectraSpectraHar
dnes
s Ra
tio
40-1
00/2
0-30
keV
1
0.8
0.6
Universal Time (MJD)
1.2
1.4
1.6
52800 53000 53200
1.9
1.9
2.3 2.2
1.9
2.3
2.2
Hard state
Soft state
PreliminaryPreliminary Spectral Spectral ParametersParametersin GPS 03in GPS 03--0404
1.451.450.780.781.021.021.081.081.021.02?2réd
(dof=185)
0.4±0.20.3±0.10.3±0.10.8±0.20.4±0.1ReflectionReflectionangleangle
7±2(bad)469
6.0±0.5(bad)721
7.1±0.1(good)
89
6.7±0.8(bad)297
6.3±0.3(bad)557
FeFe lineline(keV)(keV)
EW (EW (eVeV))
1.4 keV0.5 Ltot
weak0.4 Ltot
1.1 keV0.4 Ltot
1.5 keV0.4 Ltot
weak0.2 Ltot
DiscDisc ((kTkTinin))LL0.5-10 keV
113±720.2±0.1
57±102.5±0.1
61±200.6±0.3
106±490.3±0.2
59±202.5±0.5
kT (keV)kT (keV)t
Gr. 5Gr. 5Gr. 4Gr. 4Gr. 3Gr. 3Gr. 2Gr. 2Gr. 1Gr. 1GroupGroupParametersParameters
HARD HARDSOFT SOFT SOFT
NovemberNovember 04 04 SpectraSpectra
kT = 94 ± 44 keV disc: kTin = 1.27 keV, comp. ~ 0.4 Ltott = 0,4 ± 0.2 L 0.5-10 keV: 6.8 1036 ergs s-1
Fe line 7.8 ± 0.6 keV well defined?2
réd = 1,05 (dof = 209) reflection 0.35 ± 0.15
JEMX (6 ks) no systematics
IBIS/ISGRI (8 ks)3% systematics
SPI (8 ks)no systematics
Spectra comparisons in ESpectra comparisons in E22 f(Ef(E))December 02 and June 03December 02 and June 03
SOFTHARD
ConclusionsConclusionsEvolutions from hard (December 02, GPS) to soft states (June 03,Evolutions from hard (December 02, GPS) to soft states (June 03,GPS) thanks to combined JEMX, IBIS and SPI spectraGPS) thanks to combined JEMX, IBIS and SPI spectra
Probably intermediate states instead of real soft statesProbably intermediate states instead of real soft states(conclusion also supported by radio observations, see Malzac(conclusion also supported by radio observations, see Malzac et al.et al. 04)04)
ComptonizationComptonization models work well (typical for such a black hole)models work well (typical for such a black hole)
Fe lines and reflection values consistent with precedent studiesFe lines and reflection values consistent with precedent studies
Future work: Future work: -- Other models (Other models (eqpaireqpair, , comppscompps, , ……) to be tested on all available data) to be tested on all available data-- SPI highSPI high--energy data significance requires investigationenergy data significance requires investigation-- Study of fast variability (QPOs)Study of fast variability (QPOs)
Spectra comparisons in ESpectra comparisons in E22 f(Ef(E))December 02 and June 03December 02 and June 03
LHS
E2f(
E) k
eV c
m-2
s-1
Energy (keV)20 50 100 200 500
1
10-1
10
HSS
McConnellet al. 02(CGRO,
BeppoSAX)
Har
dnes
s ra
tio
40-1
00/2
0-30
keV
1
0.8
0.6
Universal Time (MJD)
1.2
1.4
1.6
52800 53000 53200
1.9
1.9
2.3 2.2
1.9
2.3
2.2
Hard state
Soft state
TheThe INTEGRAL SatelliteINTEGRAL Satellite
INTERnational Gamma Ray Astrophysical Laboratory (ESA)Imager IBIS (2 detectors ISGRI, PICsIT): 13 keV to 10 MeVSpectrometer (SPI): 20 keV to 8 MeVLarge energy coverage
Spectral Spectral ParametersParametersGr. 1Gr. 1 ?2
réd = 1.02 (dof = 185) HARDkT = 59 ± 20 keV, t = 2.5 ± 0.5, weak disc component ~ 0.3 LtotFe line 6.3 ± 0.3 keV not well defined, reflection ~ 0.35 ± 0.07
Gr. 2Gr. 2 ?2réd = 1.08 (dof = 185) SOFT
kT = 106 ± 49 keV, t = 0.3 ± 0.2, kTin = 1.46 keV, comp. ~ 0.5 LtotFe line 6 ± 2 keV not well defined, reflection ~ 0.8 ± 0.2
Gr. 3Gr. 3 ?2réd = 1.02 (dof = 185) SOFT
kT = 61 ± 20 keV, t = 0.6 ± 0.3, kTin = 1.11 keV, comp. ~ 0.5 LtotFe line 7.1 ± 0.1 keV well constrained, reflection ~ 0.3 ± 0.1
Gr. 4Gr. 4 ?2réd = 0.78 (dof = 185) HARD
kT = 57 ± 10 keV, t = 2.5 ± 0.05, weak disc component ~ 0.3 LtotFe line 6.0 ± 0.5 keV not well defined, reflection ~ 0.28 ± 0.04
Gr. 5Gr. 5 ?2réd = 1.45 (dof = 185) SOFT
kT = 113 ± 72 keV, t = 0.2 ± 0.1, kTin = 1.41 keV, comp. ~ 0.6 LtotFe line 6 ± 2 keV not well defined, reflection ~ 0.36 ± 0.21