J/ApJ/698/1398 H1743-322 2003 outburst (McClintock+, 2009)
The 2003 outburst of the X-ray transient H1743-322: comparisons with the black
hole microquasar XTE J1550-564.
McClintock J.E., Remillard R.A., Rupen M.P., Torres M.A.P., Steeghs D.,
Levine A.M., Orosz J.A.
<Astrophys. J., 698, 1398-1421 (2009)>
=2009ApJ...698.1398M 2009ApJ...698.1398M
ADC_Keywords: X-ray sources ; Radio lines
Keywords: accretion, accretion disks - binaries: close - black hole physics -
stars: individual (H1743-322, XTE J1550-564) - X-rays: stars
Abstract:
The bright X-ray transient H1743-322 was observed daily by the Rossi
X-ray Timing Explorer during most of its eight-month outburst in 2003.
We present a detailed spectral analysis and a supporting timing
analysis of all of these data, and we discuss the behavior and
evolution of the source in terms of the three principal X-ray states
defined by Remillard and McClintock (2006ARA&A..44...49R 2006ARA&A..44...49R). These X-ray
results are complemented by Very Large Array data obtained at six
frequencies that provide quite complete coverage of the entire
outburst cycle at 4.860GHz and 8.460GHz. We also present photometric
data and finding charts for the optical counterpart in both outburst
and quiescence.
Description:
We obtained the X-ray light curve of H1743 for the complete 2003
outburst cycle of the source. These are data obtained during 170
pointed RXTE observations using the Proportional Counter Array (PCA).
We observed H1743 a total of about 50 times throughout the course of
the outburst at 8.460GHz and 4.860GHz and about half that many times
at 1.425GHz.
Optical images were obtained using the MagIC CCD camera mounted on the
Magellan-Clay telescope at Las Campanas Observatory. This imager
provides a 2.35' field of view sampled at 0.069"/pix. On 2003 April
5.4 UT (Day 15.4 of the outburst), 300s Johnson R- and I-band images
were obtained under seeing conditions of 0.48". We also secured 5x300s
i'-band exposures of the quiescent state on 2006 June 23.1 UT under
photometric conditions and with a seeing of 0.43".
Objects:
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RA (2000) DE Designation(s)
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17 46 15.6 -32 14 01 H1743-322 = NAME XTE J17464-3213
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 118 170 Spectral parameters for H1743-322
tablea2.dat 160 170 Unabsorbed flux data, quasi-periodic oscillations
(QPO) Data, and state classifications for H1743-322
tablea3.dat 103 73 VLA radio flux densities for H1743-322:
ν≤8.640GHz
tablea4.dat 100 17 VLA radio flux densities for H1743-322:
ν≥14.940GHz
tablea5.dat 37 25 Radio spectral index
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Table 1: Outburst States of Black Holes: Nomenclature and Definitions
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New State Name Definition of X-ray Statea
(Old State Name)
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Thermal Disk fractionb > 75%
(High/Soft) QPOs absent or very weak: ac < 0.005
Weak power continuum: rd < 0.075e
Hard Disk fractionb < 20% (i.e., Power-law fraction^b^ > 80%
(Low/Hard) 1.4f < Gamma < 2.1
Strong power continuum: rd > 0.1
Steep Power Law (SPL) Presence of power-law component with Gamma>2.4
(Very high) Power continuum: rd < 0.15
Either disk fractionb <80% and 0.1-30Hz QPOs present
with ac >0.01 or disk fractionb <50% with no QPOs
present
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Notes :
a: 2-20keV band
b: Fraction of the total 2-20keV unabsorbed flux
c: QPO amplitude (rms)
d: Total rms power integrated over 0.1-10Hz
e: Formerly r<0.06 in McClintock & Remillard (2006, Compact Stellar X-ray
Sources, ed. W. Lewin & M. van der Klis (Cambridge: Cambridge Univ.
Press), 157)
f: Formerly 1.5<Gamma in McClintock & Remillard (2006, Compact Stellar X-ray
Sources, ed. W. Lewin & M. van der Klis (Cambridge: Cambridge Univ.
Press), 157)
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Obs Observation sequential number
5- 9 F5.1 d Day Number of days since discovery on
2003 March 21 = MJD 52719 (G1) (1)
11- 19 F9.3 d MJD Start time of observation in MJD (G2) (1)
21- 25 F5.3 keV Tin ?=- Color temperature of the accretion
disk
27- 31 F5.3 keV e_Tin ? rms uncertainty on Tin
33- 37 F5.2 km R*in ?=- Innner diks radius,
R*in=Rin(cosi)1/2/(D/10kpc) (3)
39- 43 F5.2 km e_R*in ? rms uncertainty on R*in
45- 48 F4.2 --- Gamma ?=- Photon index Γ (for energy band
3keV to Ebreak for broken power-law fits)
50- 53 F4.2 --- e_Gamma ? rms uncertainty on Gamma
55- 58 F4.2 --- Gam.H ?=- Photon index for energy band Ebreak to
200keV (for broken power-law fits only)
60- 63 F4.2 --- e_Gam.H ? rms uncertainty on Gam.H
65- 68 F4.1 keV Ebr ?=- Break energy
70- 72 F3.1 keV e_Ebr ? rms uncertainty on Ebr
74- 78 F5.2 ph/s/cm2/keV F1k Spectral flux at 1keV in power law fit
80- 83 F4.2 ph/s/cm2/keV e_F1k rms uncertainty on F1k
85- 87 F3.1 keV Ek ?=- Central line energy Gaussian line
parameter (5)
89- 91 F3.1 keV e_Ek ? rms uncertainty on Ek
93- 95 F3.1 keV FWHM ?=- Full width at half-maximum intensity
Gaussian line parameter (5)
97- 99 F3.1 keV e_FWHM ? rms uncertainty on FWHM
101-104 F4.2 ph/s/cm2 Flux ?=- Fe-K flux Gaussian line parameter (5)
106-109 F4.2 ph/s/cm2 e_Flux ? rms uncertainty on Flux
111-114 F4.2 --- chi2 Reduced chi2
116-117 I2 --- DOF Degrees Of Freedom
118 A1 --- n_DOF [ijk] Fitting problems (4)
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Note (1): for calendar dates, see Table A3.
Note (3): R*in = Rin(cosi)1/2/(D/10kpc), where i is the inclination angle
and D is the distance to the source in kpc.
Note (4): Notes as follows:
i = Fitted using data from HEXTE Cluster B because data from
Cluster A saturated the telemetry
j = HEXTE fitting range restricted to E=32-200keV
(includes HEXTE-A channels 17-56)
k = PCA background appears to be overestimated in standard
processing, which probably contributes to poor fit
Note (5): Parameters of the Fe-K spectral fitting, see section 2.2
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Obs Observation sequential number
5- 9 F5.1 d Day Number of days since discovery on
2003 March 21 = MJD 52719 (G1)
11- 20 A10 "YYYY/MM/DD" Date UT observation date
22- 26 I5 s Time [0/86400] Observation time
28- 32 F5.3 10-11W/m2 Ftot Total 2-20keV flux
34- 38 F5.3 10-11W/m2 E_Ftot Error on Ftot (upper value)
40- 44 F5.3 10-11W/m2 e_Ftot Error on Ftot (lower value)
46- 50 F5.3 10-11W/m2 Fdisk ?=- Disk 2-20keV flux
52- 56 F5.3 10-11W/m2 E_Fdisk ? Error on Fdisk (upper value)
58- 62 F5.3 10-11W/m2 e_Fdisk ? Error on Fdisk (lower value)
64- 68 F5.3 10-11W/m2 Fpl1 Power Law 2-20keV flux
70- 74 F5.3 10-11W/m2 E_Fpl1 Error on Fpl1 (upper value)
76- 80 F5.3 10-11W/m2 e_Fpl1 Error on Fpl1 (lower value)
82- 86 F5.3 --- Fd/Ft ?=- 2-20keV Disk/Total flux ratio
88- 92 F5.3 --- E_Fd/Ft ? Error on Fd/Ft (upper value)
94- 98 F5.3 --- e_Fd/Ft ? Error on Fd/Ft (lower value)
100-104 F5.3 10-12W/m2 Fpl2 Power Law 20-100keV flux
106-110 F5.3 10-12W/m2 E_Fpl2 Error on Fpl2 (upper value)
112-116 F5.3 10-12W/m2 e_Fpl2 Error on Fpl2 (lower value)
118-123 F6.3 Hz nu ?=- Centroid frequency of the primary ν
quasi-periodic oscillation (QPO) peak (6)
124 A1 --- n_nu Note on nu (10)
126-130 F5.2 --- Amp ?=- QPO amplitude (in %rms) (7)
132-135 F4.2 --- e_Amp ? rms uncertainty on QPOA
137-141 F5.2 --- Q ?=- Ratio Q, Q=(QPO frequency)/FWHM
143-147 F5.2 --- e_Q ? rms uncertainty on Q
149-153 F5.3 --- Cont.r Total rms power (r) integrated over
0.1-10 Hz in the PDS (2-30keV) (8)
155-159 A5 --- State Black hole state, among TD, H, SPL (9)
160 A1 --- n_State Note on State (10)
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Note (6): The uncertainty (1sigma) is <or∼1% for observations 1-85, and 2%
there after. Exceptions are observations 1(3%), 12(2%), 22(2%), 68(8%),
70(3%), 72(2%), 74(2%), 75(2%), 80(3%), 154(3%), and 160(3%).
Note (7): The QPO amplitude is the fractional rms fluctuation, calculated
as the square root of the integrated power in the QPO feature and
expressed as a fraction of the mean count rate. Errors are 1sigma,
with a lower limit of 0.1% for systematic uncertainty in the continuum
model, except for especially narrow QPOs (Q>10).
Note (8): The uncertainty (1sigma) is 1% (observations 1-85), 2%(86-93),
4%(94-102), 6%(103-118), 10%(119-150), 5%(151-168), and
10%(169-170).
Note (9): See Table 1 and Section 2.4 for definitions of states. We note
that some Galactic ridge emission in the PCA field of view or
inaccuracies in the PCA background model may affect the state
classifications for the faintest observations considered in this study.
The 3 principal states are:
TD = thermal dominant (high soft);
H = hard (low hard);
SPL = steep power law (very high)
Note (10): Notes as follows:
h = Harmonic present at 2ν.
i = Fitted using data from HEXTE Cluster B because data from Cluster A
saturated the telemetry
j = Pair of harmonics present at 0.5ν and 2ν
k = HEXTE fitting range restricted to E=32-200keV
(includes HEXTE-A channels 17-56)
l = Weak harmonic present at 2ν
m = Additional weak QPO at 3.9Hz
n = Broad harmonic possibly present at 0.5ν
o = Additional QPO at 4.54Hz
p = Additional narrow QPO at 5.14Hz
q = Additional weak QPO at 4.3Hz
r = Weak and broad harmonic at frequency 2ν
s = Additional QPO at 9.0Hz
t = Weak and broad harmonic possibly present at 2ν
u = Additional QPO at 4.6Hz
v = Strong harmonic present at 2ν
w = Harmonic present at 0.5ν
x = PCA background appears to be overestimated in standard processing
(see footnote "k" in Table A2).
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "YYYY/MM/DD" Date UT observation date
12- 21 F10.4 d MJD1 ?=- Modified Julian Day of observation (G2)
23- 27 F5.1 d Day1 ?=- Number of days since discovery on
2003 March 21 = MJD 52719 (G1).
29- 31 A3 --- VLA Configuration of the VLA antennas
33 A1 --- l_F1.425 Limit flag on F1.425
34- 38 F5.2 mJy F1.425 ?=- VLA flux density at 1.425GHz
40- 43 F4.2 mJy e_F1.425 ? rms uncertainty on F1.425
45- 54 F10.4 d MJD2 ?=- Modified Julian Day of observation (G2)
56- 60 F5.1 d Day2 ?=- Number of days since discovery on
2003 March 21 = MJD 52719 (G1)
62 A1 --- l_F4.86 Limit flag on F4.860
63- 67 F5.2 mJy F4.86 ?=- VLA flux density at 4.860GHz
69- 72 F4.2 mJy e_F4.86 ? rms uncertainty on F4.860
73 A1 --- n_F4.86 [d] Note on upper limit (G3)
75- 84 F10.4 d MJD3 ?=- Modified Julian Day of observation (G2)
86- 90 F5.1 d Day3 ?=- Number of days since discovery on
2003 March 21 = MJD 52719 (G1)
92 A1 --- l_F8.46 Limit flag on F8.460
93- 97 F5.2 mJy F8.46 ?=- VLA flux density at 8.460GHz
99-102 F4.2 mJy e_F8.46 ? rms uncertainty on F8.460
103 A1 --- n_F8.46 [d] Note on upper limit (G3)
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "YYYY/MM/DD" Date UT observation date
12- 21 F10.4 d MJD1 ?=- Modified Julian Day of observation (G2)
23- 27 F5.1 d Day1 ?=- Number of days since discovery on
2003 March 21 = MJD 52719 (G1)
31- 35 F5.2 mJy F14.94 ?=- VLA flux density at 14.940GHz
37- 40 F4.2 mJy e_F14.94 ? rms uncertainty on F14.940
42- 51 F10.4 d MJD2 ?=- Modified Julian Day of observation (G2)
53- 56 F4.1 d Day2 ?=- Number of days since discovery on
2003 March 21 = MJD 52719 (G1)
60- 64 F5.2 mJy F22.46 ?=- VLA flux density at 22.460GHz
66- 69 F4.2 mJy e_F22.46 ? rms uncertainty on F22.460
71- 80 F10.4 d MJD3 ?=- Modified Julian Day of observation (G2)
82- 86 F5.1 d Day3 ?=- Number of days since discovery on
2003 March 21 = MJD 52719 (G1)
89 A1 --- l_F43.34 Limit flag on F43.340
90- 94 F5.2 mJy F43.34 ?=- VLA flux density at 43.340GHz
96- 99 F4.2 mJy e_F43.34 ? rms uncertainty on F43.340
100 A1 --- n_F43.34 [d] Note on upper limit (G3)
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "YYYY/MM/DD" Date UT observation date
12- 21 F10.4 d MJD1 ?=- Modified Julian Day of observation (G2)
22- 26 F5.1 d Day1 ?=- Number of days since discovery on
2003 March 21 = MJD 52719 (G1)
28- 32 F5.2 --- alpha Radio spectral index α (4)
34- 37 F4.2 --- e_alpha rms uncertainty on alpha
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Note (4): Radio spectral index alpha (Sν∝να), which
is based on the 4.860GHz and 8.460GHz data.
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Global notes:
Note (G1): Revnivtsev et al. 2000MNRAS.312..151R 2000MNRAS.312..151R
Note (G2): MJD=JD-2400000.5
Note (G3): Upper limits correspond to the flux density measured at the nominal
position of the center of the beam plus three times the rms noise.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 01-Dec-2011