ガンマ線連星 LS5039からの硬X線パルスの検出
Univ. of Tokyo / Kavli IPMU

米田 浩基

牧島 一夫, 榎戸 輝揚, Dmitry Khangulyan, 松元 崇弘, 高橋忠幸
第2回MeVガンマ線天文学研究会@東京大学
2019 September 26-27

Gamma-ray Binary System

2 / 18・Binary System & The spectral peak in SED is above ~10 MeV→ By definition, the important objects in MeV astronomy
A&A 565, A38 (2014)

PSR B1259-53

LS 5039

Fig. 9. X-ray to TeV
The COMPTEL sofdata) for the INFC a
combined with simi
(Suzaku, Takahashi(Fermi/LAT, Hadascband (HESS, Aharoa high-energy SED
shows that 1) the eergies above 1 keVation dominance isgies. The lines – s
X-ray spectra repres
of Takahashi et al. (tern of LS 5039. T
their measured X-raStar
LS 5039O

FGL J1018.6-5856

O

LMC P-3O

LS I +61 303

Be

HESS J0632+057

Be

4FGL J1405.1-6119 (Corbet+19)O

PSR J2032+4127

Be

PSR B1259-53

Be

Compact
objectall available COMPTEL data of this sky
the INFC
period. For
INFC the SED suggests a strong spectralPorb
break between the two bands with a drop in flux by a factor of 5 the known but unidentified COMPTEL
3.9 theday
counterpart of LS 5039.
between 30 MeV?and 100 MeV.
In general, the COMPTEL measurements shed light on an inAs in previous analyses (e.g., Coll
16.6significant
day MeV source that is consisteteresting region ?
of the LS 5039 SED where the maximum of thehigh-energy emission of LS 5039 occurs and where significant of LS 5039, which in the COMPTEL 1
spectral changes? are happening. Therefore these COMPTEL
kind of stable and steady flux level. B
10.2a dayresults add important information on the emission pattern of sured Fermi/LAT spectra of Fermi-detec
LS 5039, and so?provide additional constraints for modeling the
26.5COMPTEL
day error box into the COMPTE
to be the most likely counterpart. This id
microquasar.
by dayextrapolating the measured Suzaku
?
315.5
MeV
band. Assuming no spectral breaks
6. Discussion
gies,
the
extrapolations reach similar flu
?
13.7
day
In recent years, after new γ-ray instruments became opera- COMPTEL fluxes, for the orbit-averagetional – in particular the ground-based Cherenkov telescopes orbit-resolved, analyses.
143 ms pulsar
50 yearOrbit-resolved analyses provide th
HESS, MAGIC, and VERITAS and the γ-ray space telescopeFermi – , a new class of γ-ray emitting objects emerged: the dence that GRO J1823-12 is the coun
ms pulsar
3.4 subdivision
yearof the COMPTEL data in“γ-ray 43
binaries”.
Many binary systems, even of diﬀerent types
like microquasars, colliding wind binaries, millisecond pulsars and SUPC parts of the binary orbit r

n), ASCA (red), and Chandra (magenta). The black filled andpresent the Suzaku observation. Fitting parameters are shown insince the spectral parameters, particularly photon indices, are
2 / 18significantly changed during the observation, we converted theobserved counting rate assuming the power-law parameters
obtained for each phase interval of ∆ = 0.1. The left panel
A&A energy
565, A38 (2014)of Figure 2 shows the resulting light curves in therange of 1–10 keV. Also, a magnified plot of the light curveis shown in the right panel of Figure 2. The phase-folded
Collmar+14

Gamma-ray binary LS 5039

tained from the phase-averaged Suzaku spectrum.
-resolved ASCA spectra were fit using NH frozen atveraged value. As seen in Figure 1, the photon indices(a)Brightest gamma-ray binary
・Luminosity ~ 1 × 1036 erg s-1
・Spectral peak is 10-100 MeV

COMPTEL(b)

Collmar+14

・Orbital modulation of flux is seenfrom X-ray to TeV

Takahashi+09, Collmar+14,
Fermi+18, Mariaud+15

Fig.
The
data
com
(Suz
(Fer
ban
a h
show
ergi
atio
gies
X-ra
of T
tern
thei

Effective/Stable
Particle Accelerator
the INFC period. For INFC the SED suggests a strong spectral all available COMPTEL d・X-ray flux is very stable in ten year scale

break between the two bands with a drop in flux by a factor of 5 the known but unidentifie
the counterpart of LS 503
between 30 MeV and 100 MeV.
In general, the COMPTEL measurements shed light on an inAs in previous analy
Kishishita+09
teresting region of the LS 5039 SED where the maximum of the significant MeV source t
high-energy emission of LS 5039 occurs and where significant of LS 5039, which in theaccspectral changes are happening. Therefore these COMPTEL
a kind of stable and stead
Takahashi+09
results add important information on the emission pattern of sured Fermi/LAT spectra
LS 5039, and so provide additional constraints for modeling the COMPTEL error box into
to be the most likely coun
microquasar.
Kishishita+09
by extrapolating the me
MeV band. Assuming no
Orbital light curves in the energy range of 1–10 keV. Top: Suzaku XIS data with a timeof 2 ks. Overlaid in the range of φ = 0.0–2.0 is the same
6. binDiscussiongies, the extrapolations reshifted by one orbital period (open circles). Bottom: comparison with the past observations. Each color corresponds to XMM-Newton (blue, cyan withCOMPTEL fluxes, for th
In
recentyears,
after
new
γ-ray
instruments
becameoperas, and green with each bin of 2 ks), ASCA (red with each bin of 5 ks), and Chandra (magenta with each bin of 2 ks). Fluxes correspond to unabsorbed
tional – in particular the ground-based Cherenkov telescopes orbit-resolved, analyses.
ue solid lines show periastron and apastron phase and the red dashed lines show superior
conjunction and inferior conjunction of the compact object. Orbit-resolved analy
HESS, MAGIC, and VERITAS and the γ-ray space telescope
1.2 ! φ < 1.8.
Fermi – , a new class of γ-ray emitting objects emerged: the dence that GRO J1823“γ-ray binaries”. Many binary systems, even of diﬀerent types subdivision of the COM
like microquasars, colliding wind binaries, millisecond pulsars and SUPC parts of the・T~ few seconds @20 TeVWhat is the mechanism of particle acceleration?
What makes this source so unusual?

3 / 18

What is the compact object in LS 5039
PERSPECTIVES

A key information to understanding the system
Electron/proton-proton interactions

Microquasar

Pulsar with Be star

If it is a Black Hole…

Electron-photon interactions

Pulsar with massive star

Cometary radio emmission
PulsarRelativistic jet from
BH
γ-rays/υRelativistic jets

PulsarCompact objectof center

If it is a Neutron Star…
PulsarMirabel+12

Massive star

Disk outflow

Be starO star
Shock between Pulsar andA

Ultraviolet emission

Accretion disk
Ultraviolet emission
and massive
clumpy wind

Massive star

γ-rays/υ

γ-rays/υB

C

ObserverHowever, whether it is a BH or a NS is still unknown…
Gamma-ray binaries. Pulsar winds are powered by the rapid rotation of magnetized neutron stars. Gamma rays can be produced either by the interaction of
the relativistic particles of the pulsar wind with the outflowing protons in the disk
or envelope of a Be star (A) (e.g., PSR B1259–63 and LSI +61° 303), or by theirinteraction with UV photons from a very massive main-sequence star (C) (e.g.,

LS 5039 and 1FGL J1018.6–5856). (B) Microquasars are powered by compact
objects (neutron stars or stellar-mass black holes) via mass accretion from a companion star. When the donor star is a massive star with a high-density UV flux andwind, gamma rays can be produced by electron-proton and/or electron-photon
interactions. ν, neutrinos.

Previous Worksvariation of flux at different wave- what different orbital modulation may oper- 5039), but it is not clear whether 1FGL
McSwain+11:time
Upper
band
µJy)
lengths was usedlimit
to identify below
Cygnus X-3 as1 KHz
ate when theinstar radioin the compact
binary is(4.1-14.5
J1018.6–5856 is alsoa TeV source. Its posia gamma-ray binary (3), a microquasar (4) of Be type. These stars are characterized tion is consistent with the TeV source HESS
sourcelimitof collimatedrelativistic
jets, which by a massive
outflsoftow with disk
and/or flatJ1018–589(12), but duekeV)
to possible confuRea+11: Upperfrom
0.005-175
Hz
in
X-ray
band
(0.3-10
was also observed at gamma rays with the tened envelope geometry, in fast rotation. sion with other objects in this complex starAgile satellite (5).
1FGL J1018.6–5856 is a compact object
orbiting with a period of 16.6 days arounda star of more than 20 solar masses. On thebasis of phenomenological similarities withother gamma-ray binaries, it is most likely
a pulsar that produces strong bipolar winds

Here, the gamma rays may be produced by
the interaction of the pulsar wind particles
with the ions in the massive outflow. This
could be the case in the Be compact binaries
PSR B1259–63 and LSI +61° 303, where
the phasing of gamma-ray maximum at GeV
energies is delayed relative to periastron (2).

forming region, it is unclear whether the
Fermi source and a component of the HESS
source are the same object. Resolving thisquestion by using time modulation and/or
more accurate positions of TeV sources will
require improving the sensitivity and angular resolution of ground-based Cherenkov

We focus on hard X-ray band (> 10 keV) for pulsation search

low stellar wind absorption, long data of Suzaku (500ks), NuSTAR (350ks)

5 / 18

1st Step: Timing Analysis by diving data
Effect of orbital motion

0.001 c・Orbital velocity of NS is ~ 0.001 c➔ smears the pulse signal
・Large parameter space,➔ difficult to search pulse with correcting theorbital moduration

Casares+05

Simple and Best Way (no orbital correction)
1. Divide the data into subsets with a time interval of Tsub.
Resolution of timing analysis (1/Tsub) > Orbital modulation (0.001/P)➔ Tsub < 1000 × Pulse Period
2. Apply Fourier analysis to each subset, and merge the result incoherently※ To get enough photons in subsets (>10 events), we focus on pulse signal < 1 Hz.
sin(2*pi*x)

sin(2*pi*x)
1

1

1

0.5

0.5

0.5

0

0

0

-0.5

-0.5

-0.5

-1

-1

0

2

4

6

8

sin(2*pi*x)

-1

0

10

2

4

6

0

2

8

4

6

10
8

10

6 / 18

Fourier Analysis with Suzakusin(2*pi*x)

sin(2*pi*x)
1

1

1

0.5

0.5

0.5

0

0

0

-0.5

-0.5

-0.5

-1

-1

0

2

4

6

8

sin(2*pi*x)

-1

0

10

2

4

6

0

2

8

4

6

10
8

10

ΔT

prob. = 1e-3

Δ T = 4096 s
Δ T = 8192 s↑ Strong Peak at 8.96 s

Δ T = 16384 s

7 / 18

2
Z analysis

To check the peak at 8.96 s, we analyzed the Suzaku data with Z2 statistics.
Z2 statistics (De Jager+89)
A common technique to search a weak periodic signal
Unbinned likelihood analysis (better than ordinary chi-square evaluation)
2
2
Zm =
N
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l=m
X
l=1

0
@

X
i

ti
cos 2⇡l
P

!2

+

X
i

ti
sin 2⇡lP!2 1

A ' log L

1. Make a folded light curve assuming a period.
2. Calculate Fourier component of the obtained profile
3. Sum up the power of the component upto m-th harmonics.

➔

+

+

+

+ …

8 / 18

Conﬁrmation of peak with Z2 statistics
To confirm the peak at 8.96 s, we analyzed the Suzaku data with Z2
statistics.
300

prob. = 1e-3

Σ Z2 (m=1)

250

200

150

Δ T = 5000 s

100
7

8

9

10

11

Period (s)P = 8.960 ± 0.009 s with a chance probability < 1.4 × 10−4
※ Period of peak does not depends on ΔT

9 / 18

Timing Analysis with NuSTAR

We analysis archived NuSTAR data (10-30 keV, gross exp. = 350 ks)
9 year after the Suzaku observation, the number of source event is ~ 11000
150

prob. = 1e-3
Σ Z2 (m=1)

prob. = 1e-2
10050

Δ T = 10000 s
7

8

9

10

11

Period (s)P = 9.045 ± 0.009 s with a change probability of 3 × 10−3
※ Period of peak does not depends on ΔT※ significance level is lower than that of Suzaku, thus no peak in FFT

10 / 18

Orbital Motion Correction

1. Assume a set of orbital parameters, and calculate the orbit of NS
2. correct the photon arrival time to the time on NS
3. apply Z2 analysis to corrected data. (Here the pulse profile was describedwith four Fourier harmonics.)
Z2 (m=4)
0.35

5200

50

55

60

65

ax sinθ (cs)

35

60

60
0.35

4700
0

0.2

900
900
850

0.25

0.4

0.6
5050
40

0.2

40

40
0.15

35

40
40

ax sin50
θ (cs)

45

50

55

ax sinθ (cs)

60
60

35
65

(d)

8.97

8.96

8.98

8.97

8.98

NuSTAR
0.8

1

1.2

1.4

1.6

1.8

2

Pulse Phase

20
10

750

00

45

0.2

8.96(s)Period

8.95

30

800
800

Counts

50

50

70
60

55

0.30.3

Eccentricity

Counts

2

45

(b)

4800

8.95

2

40

20

0
0 8.948.94(m=4)
Z2Z(m=4)35

CountsEccentricity

40

40

30

10

4900

0.15

30

40

5100

5000
5000

45

Z2 (m=4)

Eccentricity

0.2

30

5050

55

50

0.2

(b)

5400
5300

50

0.25

30

60

60

60

0.30.3(c) 5500

Suzaku

70

5500

(m=4)
Z2Z(m=4)65

Z2 (m=4)

(a)

(a)

700
700
650

00

0.2

0.4

0.6

9.03

9.04

9.03

9.05

9.04 Period (s) 9.05

Period (s)

9.06

9.06

The significance level isimprovedconsiderably
1
2
0.8

1

1.2

Pulse Phase

Pulse Phase

1.4

1.6

1.8

2

11 / 18

Solution of Orbital Parameters

Table 1: Best-fitting values of the orbital parameters obtained from Suzaku/NuSTAR observations. Errors are in 90% confidence.

4)

eccentricity

initial phaseomega (deg.)

Pulse period (s)Z 2 (m = 4)

Suzaku53.05+0.68
0.51

0.278+0.013
0.023

0.067+0.008
0.012

54.6+5.1
4.1

8.95648(4)67.97

NuSTAR

48.1+0.4
0.4

0.306+0.013
0.012

0.7285+0.0066
0.004056.8+2.3
4.7

9.05381(3)

66.87

?

10

5400

55

5200

Counts

5300

50

50

・Orbital parameters are consistent with optical

5100

5000
5000

45

4900

40
Z2 (m=4)60

60Counts

40

35

4800
4700
0

Suzaku0.2

0.4

PF = 68±14%

0.6

900
900

0.8

1

1.2

1.4

1.6

1.8

2

Pulse Phase

Counts

800
800

50

50

solutions・axsinθ, eccentricity are different from eachother slightly
・The compact-object mass has been constrained

850

55

750

45

as 1.23 - 2.35 M◎.

700
700

40

40

35

ok

5500

60

60

?

(c) 5500

Z2 (m=4)65

ax sin ✓ (cs)

(d)

650

0
0

NuSTAR
0.2

0.4

0.6

PF = 13.5±4.3%1
1.2
1
Pulse Phase

0.8

1.4

1.6

1.8

22

Pulse Phase

The similar pulse profiles are obtained

12 / 18

Summery of Observational Result
1. Fourier Analysis with Suzaku (10-30 keV) shows a strong peak at 8.96 s
2. Z2 analysis (7s-11s) with Suzaku & NuSTAR (10-30 keV) shows a peak at
8.96 s, 9.05s with a chance probability of < 1.4 × 10−4 and 3 × 10−3
3. No peak was found from 3 - 10 keV in NuSTAR data
4. The obtained pulse profiles are similar though pulse fractions are different(68% of Suzaku, 13% of NuSTAR)
5. The obtained orbital parameters are consistent with optical solutions, butslightly different from each other
6. The compact-object mass has been constrained as 1.23 - 2.35 M◎.

We conclude that the compact object in LS 5039 isa neutron star with P of 8.96 s and Pdot of 3×10-10 s s-1

What is the energy source of LS 5039 activity (1036 erg s-1 ) ?
spin-down luminosity? accretion?
Kinetic energy of stellar wind? Magnetic field?

What is the Energy Source?

13 / 18

1. Spin-down Luminosity(2⇡)2 I Ṗ
34
1
LLD =
⇠
10
erg
s
P3
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2. Accreting Pulsar
・Pulse period is increasing

・No fast time variability like accreting object
3. Stellar Wind
2
1
⇡R
2
31
1
A
Lw ⇠ Ṁw vw
⇥
<
6
⇥
10
erg
s
2
2
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LBF =<latexit sha1_base64="60kjt8t1wdUJKvNtElqgBO6djBs=">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</latexit>

2
3
BNS
RNS

6⌧

⇠ 10

37

⇥

✓

BNS
1015 G

◆2 ✓

RNS
10 km

◆3 ✓

⌧
500 yr◆ 1

erg s 1This is the only scenario that can sustain the luminosity of 1e36 erg/sMagnetar Hypothesis
1. It can only supply the emission
energy of 1036 erg s-1

14 / 18

Magnetars

2. Period of 9s and its derivative isvery consistent with isolated
magnetars value (2-11 s)
3. Strong magnetic field preventsaccretion naturally
⇣
⌘ 2
2GMNS
v
w
8
RB =
⇠
1
⇥
10
⇥
m
2
1
vw
2000 km s

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3
BNS RNS
Dsep

p

2Ṁw vw

!1/3

⇠

<

2 ⇥ 108 ⇥✓Alfven Radius !

1. Left panel:
1/6 P − Ṗ diagram for radio pu◆FIGURE
1/3⇣⌘ 1/6
BNS RRATs (crosses),
Ṁw
v
w
XDINs (triangles), AXPs/SGRs(m,
1
1011 T from the
10 6ATNF
M yrPulsar
2000 km([11],s 1 http://www
Catalogue

McGill SGR/AXP Online Catalog (http://www.physics
indicates the Ṗ upper limit for SGR 0418+5729 [12].
We conclude that the compact object
in LS 5039 is a magnetar
109 to 1015 G and characteristic ages from 103 to 1

15 / 18

Non-thermal Emission in Strong B?
LS 5039

A&A 565, A38 (2014)

Collmar+14

of Anomalous X-Ray Pulsar 4U 0142+61

Stellar Winds Shock395

Fig. 9. X-ray to TeV γ-ray SED of LS 5039.
The COMPTEL soft γ-ray spectra (sum of alldata) for the INFC and SUPC orbital phases are
combined with similar spectra from the X-ray(Suzaku, Takahashi et al. 2009), the MeV/GeV(Fermi/LAT, Hadasch et al. 2012), and the TeVband (HESS, Aharonian et al. 2006a) to build
a high-energy SED of LS 5039. The SED
shows that 1) the emission maximum at energies above 1 keV and 2) a switch in radiation dominance is occurring at MeV energies. The lines – solid and dashed – in the
X-ray spectra represent the model calculationsof Takahashi et al. (2009) on the emission pattern of LS 5039. They do not present a fit totheir measured X-ray spectra.

1 keV

100 keV 10 MeV

1 GeV

100 GeV

10 TeV

Downloaded from https://academic.oup.com/pasj/article-abstract/6
Downloaded from https://academic.ou

of2]Anomalous X-Ray Pulsar 4U
Suzaku0142+61
Observation of Anomalous X-Ray395
Pulsar 4U 0142+61

EnergyDissipation?

395

all available COMPTEL data of this sky region by assuming that
Isolated Magnetar (4U 0142+61)
the known but unidentified COMPTEL source GRO J1823-12 isthe counterpart of LS 5039.
As in previous analyses (e.g., Collmar 2003), we found asignificant MeV source that is consistent with the sky positionof LS 5039, which in the COMPTEL 10−30 MeV band showsa kind of stable and steady flux level. By extrapolating the measured Fermi/LAT spectra of Fermi-detected γ-ray sources in the
COMPTEL error box into the COMPTEL band, we find LS 5039
to be the most likely counterpart. This identification is supported
by extrapolating the measured Suzaku X-ray spectra into theMeVband. Assuming no spectral breaks from keV to MeV ener6. Discussiongies, the extrapolations reach similar flux levels to the measured
In recent years, after new γ-ray instruments became opera- COMPTEL fluxes, for the orbit-averaged (see Fig. 5), as well as
tional – in particular the ground-based Cherenkov telescopes orbit-resolved, analyses.
Orbit-resolved analyses provide the most convincing eviHESS, 1MAGIC,VERITASandMeVthe γ-ray 1space
keV and100
keV 10
GeVtelescopeFermi – , a new class of γ-ray emitting objects emerged: the dence that GRO J1823-12 is the counterpart of LS 5039. A“γ-ray binaries”. Many binary systems, even of diﬀerent types subdivision of the COMPTEL data into the so-called INFC
like microquasars, colliding wind binaries, millisecond pulsars and SUPC parts of the binary orbit results in a flux change
in binaries and novae, have now become confirmed emitters of of the MeV source. The flux measurements in the 10−30 and
γ-ray radiation above 1 MeV (see e.g., Dubus 2013 for a recent 3−10 MeV bands provide evidence at 2.7σ and at 1.6σ, respectively,
thatfrom
the fluxes for the two orbital phases are diﬀerent.
review).data
Confirmed
VHEin(>100
GeV)keV
emissionis still keVknown
61. The Suzaku
are shownthe 0.8–10
and 12–200
energyrangesfor five binary systems, among them the microquasar candidate The combined evidence is 3.1σ. The analyses of the COMPTEL
onents ofLS
Model
E are represented by dashed lines after corrections for 10−30
the interstellar
MeV data, subdivided into orbital phase bins of 0.2, re5039.
s X-ray results
also
0.1–200
keV bandfrom
XMM-Newton/PN(Rea MeV flux. The light curve is consistent in phase,LS are5039
is shown:
detectedtheat γ-rayenergiesabove
100theMeVby sult in a variable
Fermi/LAT
(Abdo
et
al.
2009;
Hadasch
et
al.
2012)
and
above
shape,
andamplitude with the ones observed at X-ray and TeV
sets (den Hartog et al. 2008). In the gamma-ray energy band, the 2! CGRO/COMPTEL
100 GeV by HESS (Aharonian et al. 2005, 2006a) showing re- γ-ray energies, although the statistical evidence for variability is
Fermi/LAT
upperbehavior
limits (Abdoet al.
2010)theareplotted.
In the infrared
opticalranges,92%.
We note that the errors on the fluxes always resultmarkablein bothbands:
flux
is modulated
along itsandonly
and somebinary
data setsfromGeminiinand
Keck II (Durant
van Kerkwijk
orbit,
however,
anticorrelation
for the&diﬀerent
wave- 2006c;
from Hulleman
the fitting process combining four γ-ray sources and two

Lack of thecomponent
above MeV
Enoto+11

Compression ofmagnetosphere?
Downloaded from https://academic.ou

the INFC period. For INFC the SED suggests a strong spectral
break between the two bands with a drop in flux by a factor of 5
between 30 MeV and 100 MeV.
In general, the COMPTEL measurements shed light on an interesting region of the LS 5039 SED where the maximum of thehigh-energy emission of LS 5039 occurs and where significant
spectral changes are happening. Therefore these COMPTEL
results add important information on the emission pattern of
LS 5039, and so provide additional constraints for modeling the
microquasar.

RAl ⇠ Rlc
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We suggest that interactions between the dense stellar winds and thestrong magnetic fields are responsible for the non-thermal emission(Detail theoretical work is needed)18 / 18

Two Component?

A&A 565, A38 (2014)

Pulsed component?
near NS?
Stable Component?
at shock?

Fig. 9. X-ray t
The COMPTEdata) for the IN
combined with
(Suzaku, Takah(Fermi/LAT, H
band (HESS, A
a high-energy
shows that 1)
ergies above 1
ation dominangies. The line
X-ray spectra rof Takahashi etern of LS 503
their measured

If thisis true,
MeV
canspectral
be a pulsed
component.
all available
COMPTEL data of thi
the pulse
INFC period.
For INFC
the gamma-ray
SED suggests a strong
break between the two bands with a drop in flux by a factor of 5

the known but unidentified COMPTConclusion

18 / 18

1. Using timing analysis, we found a periodic component from Suzaku(8.96 s) and NuSTAR (9.046 s).
2. It tells that the compact object in LS 5039 is a magnetar with amagnetic field of ~1015 G
3. We propose that the non-thermal emission of LS 5039 is generated byinteractions between the dense stellar winds and the strong magnetic
fields.
4. The first magnetar-binary system?
5. If this is true, it may be pulsed also in MeV gamma-ray.
Future Work・Why the pulse fraction is weaker in NuSTAR observation?
・Why there is difference in orbital solutions?

➔New long observation in hard X-rays is needed