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XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
The XMM-Newton survey of the SMC:The Be/X-ray binary population
Richard Sturmon behalf of the SMC XMM-Newton large project collaboration
Max-Planck-Institut fur extraterrestrische Physik
The X-ray Universe 2011Berlin, 27.06.2011
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Neutron Star X-ray Binaries – Classification
X-ray binaries
High Mass X-ray Binary
early type OB companion starM∗ > 8M�
trace recent star formation
Low Mass X-ray Binary
late type companionM∗ < 2M�
number ∝ galaxy massnone known in the SMC
Supergiant systems
Supergiant I-II
Be/X-ray Binaries
V–III emission line stardecretion disk of Be star
Disk fed
1038 erg s−1Wind fed
1037 erg s−1Persistent
1034−35 erg s−1
small long term variabilitylong puls periods
low or no Fe Kα emission
Transient
Type I outburst: 1036−37 erg s−1
Type II outburst: >1037 erg s−1
quiescence: ∼1033 erg s−1
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Be/X-ray Binaries – Phenomenology
X-rays powered by accretion of matter from companion staronto a compact object:
high variability possiblepowerlaw like (Γ ∼ 0.8) spectrumsoft excesspulsations
optical & infrared emission dominated by Be star:spectral types O9e–B4evariable emission lines (e.g. Hα)variable IR excess
Credit: Walt Feimer, NASA/Goddard Space Flight Center
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
HMXBs in the Milky Way and nearby galaxies
227 HMXBs and candidates – 130 pulsars
MW: Liu et al. (2006)
SMC: Haberl & Pietsch (2004); Coe et al. (2005) + new discoveries
LMC: Negueruela & Coe (2002); Shtykovskiy & Gilfanov (2005) + new discoveries
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The Be/X-ray binary population in the SMC
Galaxy
1%
25%
74%
SG HMXB diskSG HMXB windBe/X-ray binary
SMC
1%
25%
99%
Over-abundance of HMXBsNo wind accretion poweredsupergiant system
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Why observe HMXB in the SMC?
Galaxy – Physics ofindividual systems
high-resolutionspectroscopy andtimingaccretion processwind structure
SMC – Statisticalstudies
Observations ofmany systemssimultaneously atsimilar distancelow foregroundabsorptionglobal propertiespopulation studies
5.1×104 5.2×104 5.3×104 5.4×104
340
342
344
346
348
puls
e pe
riod
(s)
time (modified JD)
SAX J0103.2−7209
5.1×104 5.2×104 5.3×104 5.4×104
0.1
110
lum
inos
ity (
1035
erg
s−1)
time (modified JD)
SAX J0103.2−7209
Eger & Haberl (2008)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
HMXBs and Star Formation History
N
E
20’
HI map Stanimirovic et al. (1999)
HMXBs in regions with starformation bursts 25-60 Myrago
number of HMXBs correlateswith SFR at 42 Myr
Antoniou et al. (2010)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The SMC in HI
HI (Stanimirovic et al. 1999)
20’
N
E
-1s 22.07s
0.72s
31.03s
-1s
65.78s
-1s
726s
3.34s
11.48s
-1s
1323s
-1s
-1s
345.2s
6.85s
-1s
967s
-1s
7.92s
-1s
455s
304.5s
8.02s-1s
-1s
202.52s
201.9s
2.76s
291.33s
152.34s
280.4s
565s
101.16s
-1s
-1s
140.1s
644.6s
701.6s
59.07s
499.2s
2.37s
-1s
341.9s46.63s
-1s
-1s
138s
169.3s
-1s
325.4s
-1s
-1s15.3s
82.4s
-1s
7.78s
8.9s
172s
91.12s
323.2s
214.03s
755.5s
-1s
894s9.13s-1s
18.37s74.67s
-1s
-1s
25.55s
11.87s
263s
-1s
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The SMC in X-ray
(2.0-4.5) keV
(1.0-2.0) keV
(0.2-1.0) keV
N
E
20’
-1s 22.07s
0.72s
31.03s
-1s
65.78s
-1s
726s
3.34s
11.48s
-1s
1323s
-1s
-1s
345.2s
6.85s
-1s
967s
-1s
7.92s
-1s
455s
304.5s
8.02s-1s
-1s
202.52s
201.9s
2.76s
291.33s
152.34s
280.4s
565s
101.16s
-1s
-1s
140.1s
644.6s
701.6s
59.07s
499.2s
2.37s
-1s
341.9s46.63s
-1s
-1s
138s
169.3s
-1s
325.4s
-1s
-1s15.3s
82.4s
-1s
7.78s
8.9s
172s
91.12s
323.2s
214.03s
755.5s
-1s
894s9.13s-1s
18.37s74.67s
-1s
-1s
25.55s
11.87s
263s
-1s
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Discovery of the 11.866 s Be/X-ray binary pulsar
New X-ray transientLX = 3.97 ×1036 erg s−1
variability of >560
Spectrum:absorbed power-lawΓ = 0.53± 0.08indication of soft excess
Spin period:(11.86642± 0.00017) s
Be counterpart
Hα emissionEW = (−3.5± 0.6) A
NIR excess and variability
Sturm et al. (2011)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Discovery of the 11.866 s Be/X-ray binary pulsar
New X-ray transientLX = 3.97 ×1036 erg s−1
variability of >560
Spectrum:absorbed power-lawΓ = 0.53± 0.08indication of soft excess
Spin period:(11.86642± 0.00017) s
Be counterpart
Hα emissionEW = (−3.5± 0.6) A
NIR excess and variability
Sturm et al. (2011)
10−3
0.01
0.1
Cou
nts
s−1
keV
−1
−4
−2
0
2
χ
1 100.5 2 5−4
−2
0
2
4χ
Channel energy (keV)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Discovery of the 11.866 s Be/X-ray binary pulsar
New X-ray transientLX = 3.97 ×1036 erg s−1
variability of >560
Spectrum:absorbed power-lawΓ = 0.53± 0.08indication of soft excess
Spin period:(11.86642± 0.00017) s
Be counterpart
Hα emissionEW = (−3.5± 0.6) A
NIR excess and variability
Sturm et al. (2011)
0 0.05 0.1 0.15 0.2 0.25
020
4060
Pow
er
Frequency (Hz)
0.95
1.00
1.05
1.10
1.15
0.2-
1.0
keV
0.9
1.0
1.1
1.2
1.0-
2.0
keV
0.9
1.0
1.1
1.22.
0-4.
5 ke
V
0.900.95
1.00
1.05
1.10
4.5-
10.0
keV
0.0 0.5 1.0 1.5 2.0Phase (11.86642 s)
0.900.951.001.051.101.15
0.2-
10.0
keV
0.500.550.600.650.70
HR
1
0.35
0.40
0.45
0.50
HR
2
-0.020.000.020.040.060.080.100.12
HR
3
0.0 0.5 1.0 1.5 2.0Phase (11.86642 s)
-0.15
-0.10
-0.05
HR
4
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Discovery of the 11.866 s Be/X-ray binary pulsar
New X-ray transientLX = 3.97 ×1036 erg s−1
variability of >560
Spectrum:absorbed power-lawΓ = 0.53± 0.08indication of soft excess
Spin period:(11.86642± 0.00017) s
Be counterpart
Hα emissionEW = (−3.5± 0.6) A
NIR excess and variability
Sturm et al. (2011)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Discovery of the 11.866 s Be/X-ray binary pulsar
New X-ray transientLX = 3.97 ×1036 erg s−1
variability of >560
Spectrum:absorbed power-lawΓ = 0.53± 0.08indication of soft excess
Spin period:(11.86642± 0.00017) s
Be counterpart
Hα emissionEW = (−3.5± 0.6) A
NIR excess and variability
Sturm et al. (2011)
5000-17
-16
-15
-14
6200 6400 6600 6800
0.8
1
1.2
1.4
1.6
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Discovery of the 11.866 s Be/X-ray binary pulsar
New X-ray transientLX = 3.97 ×1036 erg s−1
variability of >560
Spectrum:absorbed power-lawΓ = 0.53± 0.08indication of soft excess
Spin period:(11.86642± 0.00017) s
Be counterpart
Hα emissionEW = (−3.5± 0.6) A
NIR excess and variability
Sturm et al. (2011)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Discovery of the 214 s Be/X-ray binary pulsar
40.0 20.0 0:50:00.0 49:40.0
-72:58:00
59:00
-73:00:00
01:00
02:00
03:00
Right Ascension
De
cli
na
tio
n
BG
MOS2
MOS1
pn
0.0
0.5
1.0
1.5
2.0
0.2-
1.0
keV
0.5
1.0
1.5
2.0
2.5
1.0-
2.0
keV
0.6
0.8
1.0
1.2
1.4
2.0-
4.5
keV
0.40.60.81.01.21.41.6
4.5-
10.0
keV
0.0 0.5 1.0 1.5 2.0Phase (214.045 s)
0.8
1.0
1.2
1.4
1.6
0.2-
10.0
keV
10−3
0.01
2×10−4
5×10−4
2×10−3
5×10−3
Cou
nts
s−1
keV
−1
1 100.5 2 5
−4
−2
0
2
4
χ
Channel energy (keV)
10−4 10−3 0.01 0.1
020
4060
Pow
er
Frequency (Hz)
TS_0601211401merged_sc4_200_10000.fits
Start Time 15139 22:01:52:914 Stop Time 15140 7:13:30:677
Bin time: 2.840 s
?
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Detection of the 11.48 s Be/X-ray binary pulsar
0.0 0.3 0.8 1.8 3.9 8.0 16.2 32.4 65.3 130.3 259.7
EPIC MOS1
0601212601
0.0 0.3 0.8 1.9 4.1 8.5 17.3 34.7 69.8 139.3 277.7
EPIC MOS1
0301170501
10−3
0.01
0.1
1
Cou
nts
s−1
keV
−1
1 100.5 2 5 20
−2
0
2
χ
Channel Energy (keV)
0.70.80.91.01.11.21.3
0.2-
1.0
keV
0.6
0.8
1.0
1.2
1.41.
0-2.
0 ke
V
0.8
1.0
1.2
1.4
2.0-
4.5
keV
0.6
0.8
1.0
1.2
1.4
4.5-
10.0
keV
0.0 0.5 1.0 1.5 2.0Phase (11.49 s)
0.80.91.01.11.21.3
0.2-
10.0
keV
Townsend et al. (2011)
Discovered by INTEGRAL(IGR J01054-7253)
Swift follow up
RXTE found spin period
XMM-Newton confirmedposition and spin
Orbital solution
55000 55020 55040 55060DATE (MJD)
3.823
3.824
3.825
3.826
3.827
3.828
3.829
Obs
erve
d pe
riod
of H
arm
onic
(s)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
2 further transients in the survey data
2’
Γ = 0.79− 1.16NH = (8± 2)×1022 cm−2
LX = 5.6×1035 erg s−1
double peaked Hα lineEW = −(33± 3) A
10−3
5×10−4
2×10−3
5×10−3
Cou
nts
s−1
keV
−1
1 100.5 2 5
−1
0
1
χ
Channel Energy (keV)
2’
Γ = 0.66− 0.83NH < 7×1020 cm−2
LX = 1.1×1035 erg s−1
correlating with early typeemission line star
10−3
2×10−4
5×10−4
2×10−3
5×10−3
Cou
nts
s−1
keV
−1
1 100.5 2 5
0
2
χ
Channel Energy (keV)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The search for new candidates
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The search for new candidates
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The search for new candidates
The XMM-Newton point sourcecatalog of the SMC:(Sturm et al., in preperation)
3053 X-ray sources
5.7 deg2 total area
95 individual observations
astrometric improved positionsaccuracy ∼1.42′′
complete to 10−14 erg s−1 cm−2
in the (0.2–4.5) keV band4.3 ×1033 erg s−1 (for the SMC).
exposure: 10-30 ks (average),∼600 ks (maximum)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The search for new candidates
X-ray selection using hardness ratios:
−1 −0.5 0 0.5 1−1
−0.
50
0.5
1
HR
3
HR2
SXP8.02 (AXP?)SMC pulsars
−1 −0.5 0 0.5 1−1
−0.
50
0.5
1
HR
3
HR2
AGN
−1 −0.5 0 0.5 1−1
−0.
50
0.5
1
HR
3
HR2
stars
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The search for new candidates
Optical counterpart:
Magellanic Cloud PhotometricSurvey (Zaritsky et al. 2002)
16605 sources in theXMM-Newton field
position accuracy ∼0.3′′
−1 −0.5 0 0.5 1 1.5 2
2015
V (
mag
)
B−V (mag)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The search for new candidates
Result:
93 X-ray sources
51 known HMXB10 candidates from previousstudies32 new candidates
further investigation necessary...
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Be/white dwarf systems
Population synthesis models predict for Be companions(Pols et al. 1991; Raguzova 2001)
10% neutron stars20% helium stars70% white dwarfs
expected X-ray properties:
Hard X-ray emission during accretion at 1029−33 erg s−1
Supersoft X-ray emission during thermonuclear surface burningBut: absorption and disc truncation
possible candidates:
γ Cas and γ Cas like objects (Haberl 1995; Lopes de Oliveira et al. 2006)
one SSS in the LMC (Kahabka et al. 2006)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Be/white dwarf systems
Population synthesis models predict for Be companions(Pols et al. 1991; Raguzova 2001)
10% neutron stars20% helium stars70% white dwarfs
expected X-ray properties:
Hard X-ray emission during accretion at 1029−33 erg s−1
Supersoft X-ray emission during thermonuclear surface burningBut: absorption and disc truncation
possible candidates:
γ Cas and γ Cas like objects (Haberl 1995; Lopes de Oliveira et al. 2006)
one SSS in the LMC (Kahabka et al. 2006)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Be/white dwarf systems
Population synthesis models predict for Be companions(Pols et al. 1991; Raguzova 2001)
10% neutron stars20% helium stars70% white dwarfs
expected X-ray properties:
Hard X-ray emission during accretion at 1029−33 erg s−1
Supersoft X-ray emission during thermonuclear surface burningBut: absorption and disc truncation
possible candidates:
γ Cas and γ Cas like objects (Haberl 1995; Lopes de Oliveira et al. 2006)
one SSS in the LMC (Kahabka et al. 2006)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
A new candidate in the SMC?
New Discovery of a faint supersoft X-ray source(kT = 76+3
−6 eV, F(0.2−1.0)keV = 9.4×1033 erg s−1)
O7IIIe–B0Ie companion star in the SMC
(Sturm et al., in preperation)
10.2 0.5 2 5
02×
10−
34×
10−
36×
10−
3
Cou
nts
s−1
keV
−1
Channel Energy (keV)
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Spectral distributionof Be/X-ray binaries in the SMC
average photon index Γ = (0.79± 0.20)spectral confirmation of 3 HMXB candidates
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Absorption of Be/X-ray binaries in the SMC
0 2×1021 4×1021 6×1021 8×1021 1022 1.2×1022
02×
1022
4×10
226×
1022
8×10
2210
23
NH (
cm−
2 )
HI (cm−2)
HMXB
0 2×1021 4×1021 6×1021 8×1021 1022 1.2×1022
02×
1022
4×10
226×
1022
8×10
2210
23
NH (
cm−
2 )
HI (cm−2)
AGN
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Spin Period distribution
Bimodal distribution in the SMC?Comparing SMC and MW: KS-Test probability: 46%
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
The Corbet relation
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
Summary
4 new HMXB in the SMC found during the survey(SXP11.87, SXP214 and two transients)
XMM-Newton confirmed position and pulsation of SXP11.5
∼ 29 bright detections of known HMXBs in the survey data(144 in total)
Spectra of bright sources ⇒ confirmation of 3 HMXB candidates
Hardness ratio selection and correlation with optical catalogsresults in ∼ 30 new candidates
One candidate for a Be/white dwarf system found
to be continued...
XMM-NewtonSMC survey:
The Be/X-raybinary population
Richard Sturm
Introduction
Classification
Phenomenology
HMXBs in theSMC
SF History
Discoveries
SXP11.87
SXP214
SXP11.5
Furthertransients
New candidates
Be/WD systems
Population
Bibliography
References
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