すざく衛星による高銀緯フェルミ
未同定天体の系統探査	
(Takahashi	  et	  al.	  in	  prep.)	

第11回高宇連研究会＠早稲田	
高橋洋輔 (早稲田)	  片岡淳,	  中森健之,	  前田洸登 (早稲田),	  L.	  Stawarz,	  	  佐藤理江,	  高橋忠幸,	  田中康之 (ISAS/JAXA),真喜屋龍,	  	  戸谷友則 (京都),金井義和,	  河合誠之 (東工大),	  	  C.C.	  Cheung	  (NASA/GSFC),	  L.	  Guillemot,	  P.	  C.	  C.	  Freire	  (MPIfR),	  I.	  Cognard	  (LPCE/CNRS)	
1	

Outline	  1. IntroducHon	  1. What	  is	  unassociated	  sources?	  
2. About	  our	  study	  2. ObservaHon	  results	  3. Discussion	  	  4. Conclusion	  	  Fermi	  gamma-­‐ray	  space	  telescope	

hWp://fermi.gsfc.nasa.gov/	

•約3時間で一回全天を走査	•2年間で約1800個のガンマ線天体を発見	
•そのうち約30％は未同定天体	

2FGL	  catalog:	  Abdo	  et	  al.	  2011	

3	

Fermi/LAT	  unassociated	  sources	
Unassociated	  sources	  are	  sources	  that	  have	  no	  associaHons	  in	  other	  wavelength.	
• The	  number	  of	  unassociated	  sources	
2FGL	  catalog	  –	  572	  out	  of	  1873	
Many	  sources	  are	  sHll	  remained	  unassociated!	

MoHvaHon	  of	  Suzaku	  observaHon	
• To	  survey	  a	  new-­‐type	  gamma-­‐ray	  source	
4	Fermi	  gamma-­‐ray	  space	  telescope	

2FGL	  catalog:	  Abdo	  et	  al.	  2011	

5	IntroducHon	
• This	  study	  is	  a	  second	  year	  campaign	  of	  X-­‐ray	  follow-­‐up	  observaHons	  with	  Suzaku.	
In	  the	  ﬁrst	  year	  of	  this	  campaign,	  we	  observed	  four	  unassociated	  sources	  with	  Suzaku.	  
-­‐1FGL	  J1231.1-­‐1410	  	  -­‐1FGL	  J1311.7-­‐3429	  -­‐1FGL	  J1333.2+5056	  	  -­‐1FGL	  J2017.3+0603	  hWp://www.astro.isas.ac.jp/suzaku/overview/	 6	First	  Year	  Campaign	  J1333.2+5056	 

J1231.1-­‐1410	 
J1311.7-­‐3429	 

J2017.3+0603	 

Selec<on	  Criteria	  |b|=10 deg	Gamma-ray all-sky image of two year observation by Fermi•Unassociated	  Objects	  •More	  than	  10	  degrees	  away	  from	  the	  galacHc	  plane	  •TS	  value	  >	  200	  First	  Year	  Results
1FGL J1231.1-1410

MSP	  
1FGL J1333.2+5056

1FGL J1311.7-3429

X-­‐ray	  ﬂare	  1FGL J2017.3+0603

MSP	  

Maeda, K., et al., 2011, Apj, 729,8	103	Second	  Year	  Campaign	  1FGL J1312.6+0048

1FGL J1739.4+8717|b|=10 deg	
1FGL J1743.8-7620
1FGL J0106.7+4859

1FGL J2043.2+1709

1FGL J2302.8+4443

1FGL J1902.0-5110
Gamma-ray all-sky image of two year observation by Fermi

9	  1FGL J2302.8+4443

10	  Results:	  1FGL	  J2302.8+4443	
• One X-ray point source wasdiscovered	Black:xis0+3
Gray:xis1
Model: bbody
kT=0.31 keV

Χ2/d.o.f = 2.98/11
Preliminary	Suzaku/XIS0+3	  (0.5-­‐2keV)	  (Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

11	

Results:	  1FGL	  J2302.8+4443	
Millisecond pulsar
PSR J2302+4442(P=5.20ms, d=1.2kpc)
Cognard et al. 2011

• LAT	  pulsa<ons	  are	  detected	  • This	  source	  is	  iden<ﬁed	  as	  a	  millisecond	  pulsar	  PSR	  J2302+4442	  reported	  by	  Cognard	  et	  al.	  2011	  • XMM-­‐Newton	  detected	  X-­‐ray	  counterpart	  of	  MSP	  PSR	  J2302+4442	

Preliminary	Suzaku/XIS0+3	  (0.5-­‐2keV)	  (Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

12	DetecHon	  of	  X-­‐ray	  counterpart	• Position of X-ray point sourceis consistent with a radio
position of PSR J2302+44• Thermal X-ray emission

Suzaku detected X-ray emission froma millisecond pulsar	
Preliminary	
13	

1FGL J1312.6+0048

1FGL J2043.2+1709

14	

•

1FGL	  J2043.2+1709	 •Preliminary	

1FGL	  J1312.6+0048	
Preliminary	Suzaku/XIS0+3	  (0.5-­‐10keV)	  (Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

•Two X-ray point sources
inside the 2FGL error ellipse	

• One	  X-­‐ray	  point	  source	  was	   discovered	   inside	  the	  2FGL	  error	  ellipse	
15	•

1FGL	  J2043.2+1709	 •Millisecond	  pulsar	  PSR	  J2043+1710	  (P=2.38ms,	  d=1.8kpc)	  (Guillemot	  et	  al.	  in	  prep.)	  Preliminary	

1FGL	  J1312.6+0048	
Millisecond	  pulsar	  	  	  PSR	  J1312+00	  	  	  	  	  	  	  	  	  (2FGL	  catalog)	  Suzaku/XIS0+3	  (0.5-­‐10keV)	  (Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)		  	  	  Preliminary	•90%	  conﬁdence	  upper	  limit	  for	   •90%	  conﬁdence	  upper	  limit	  for	  PSR	  J2043+1710	  PSR	  J1312+00	  F2-­‐10keV	  <	  3.63×10-­‐14	  erg	  cm-­‐2	  s-­‐1	  F2-10keV < 1.08×10-13 erg cm-2 s-1
16	

1FGL J1739.4+8717

17	• 1FGL	  J1739.4+8717	
• One	  X-­‐ray	  source	  was	  discovered	  in	  the	  2FGL	  error	  ellipse	

Model:	  power-­‐law	Preliminary	Suzaku/XIS0+3	  (0.5-­‐10keV)	  (Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

X-­‐ray	  spectrum	  created	  assuming	  a	  point	  source	

18	Gamma-­‐ray	  ﬂare	  of	  J1739.4	
ﬂaring	• Suzaku	  observaHon	  was	  conducted	  under	  the	  low	  gamma-­‐ray	  state	  • One	  NVSS	  source	  is	  located	  inside	  the	  error	  ellipse		?
razal
B
Suzaku observation

hWp://heasarc.gsfc.nasa.gov/FTP/fermi/data/lat/catalogs/
source/lightcurves/2FGLJ1738.9+8716.png	

NVSS	  source	Preliminary	

19	

1FGL J1743.8-7620
1FGL J0106.7+4859

1FGL J1902.0-5110

20	

Other three sources• 1FGL	  J0106.7+4853	  Flux(2-10keV)<1.04×10-13
Preliminary	• 1FGL	  J1902.0-­‐5110	  PSR J1902-5105•PSR J1902-5105
Flux(2-10keV)<1.68×10-14
Preliminary	• 1FGL	  J1743.8-­‐7620	  Flux(2-10keV)<8.95×10-14
Preliminary	• X-­‐ray	   upper	   limits	   were	   calculated	  for	   these	   three	   sources	   which	  Suzaku	   could	   not	   detect	   any	   X-­‐ray	  counterparts	  • 1FGL	   J1902.0-­‐5110	   is	   idenHﬁed	   as	  millisecond	   pulsar	   PSR	   J1902-­‐5105	  and	  X-­‐ray	  upper	  limit	  for	  the	  pulsar	  is	   presented	   (Ransom	   &	   Fermi	   Pulsar	   Search	  21	ConsorHum.	  2010)

Source	  List	
• Some	  of	  our	  targets	  have	  associaHons	  in	  2FGL	  catalog	
1FGL name

Association

LAT pulsation

X-ray
counterpart(This work)

J0106.7+4853

No		-­‐

No	

J1312.6+0048	

MSP	  PSR	  J1312+00		
-­‐Yes	  (not	  PSR)	

J1739.4+8717	

No		-­‐

Yes?	

J1743.8-7620	

No		-­‐

No	

J1902.0-5110	

MSP	  PSR	  J1902-­‐5105	

Yes	  No	

J2043.2+1709	

MSP	  PSR	  J2043+1710	

Yes	  No	J2302.8+4443	

MSP	  PSR	  J2302+4442	

Yes	  Yes	

22	  10-­‐14	10-­‐12	Spectral	  Energy	  DistribuHon	

10-­‐17	10-­‐18	

Maeda	  et	  al.	  2011	Spectral	  energy	  distribuHons	  of	  a	  millisecond	  pulsar	  PSR	  J1231-­‐1411	  •Gamma-­‐ray	  emission	  is	  far	  stronger	  compared	  to	  radio	  emission	Abdo	  et	  al.	  2010	

Spectral	  energy	  distribuHons	  of	  a	  blazar	  PKS	  0528+134	  •A	  radio	  ﬂux	  is	  only	  two	  orders	  of	  magnitude	  less	  than	  a	  gamma-­‐ray	  ﬂux	23	  Discussion	

F1.4	  GHz/F0.1-­‐100	  GeV	

 :	  Our	  targets	  × :	  Blazars	   :	  Millisecond	  pulsars	

F2-­‐10	  keV/F0.1-­‐100	  GeV	• Clear	  separa<on	  between	  blazars	  and	  millisecond	  pulsars	  can	  be	  seen	  • Most	   of	   our	   targets	  are	   predicted	   to	   be	  millisecond	  pulsars	  • Only	  J1739.4	  is	  located	  at	  the	  blazars	  region	  (assuming	  NVSS	  source	  as	  a	  radio	  counterpart)	  24	F1.4	  GHz/F0.1-­‐100	  GeV	

Discussion	 :	  Our	  targets	  × :	  Blazars	   :	  Millisecond	  pulsars	
☆:	  First	  year	  targets	  •1FGL	  J1311.7	  is	  ploWed	  on	  the	  millisecond	  pulsars	  region,	  while	  the	  X-­‐ray	  counterpart	  is	  a	  variable	  source	  •AGN	  candidate	  1FGL	  J1333.2+5056	  certainly	  ploWed	  on	  the	  leo	  edge	  of	  blazars	  region	  F2-­‐10	  keV/F0.1-­‐100	  GeV	25	Conclusions	• DetecHon	  of	  X-­‐ray	  counterpart	  to	  MSP	  PSR	  J2302+4442	  • Millisecond	  pulsars	  are	  dominant	  objects	  among	  Fermi	  unassociated	  sources,	  but	  truly	  mysterious	  unassociated	  sources	  are	  sHll	  remained	

Future	  Work	• More	  X-­‐ray	  follow-­‐up	  observaHons	  with	  Suzaku	  – Four	  observaHons	  are	  planned	  in	  AO-­‐6	  cycle,	  	  	  	  	  1FGL	  J0103.1+4840,	  1FGL	  J1311.7-­‐3429,	  	  	  	  	  	  	  	  	  	  	  	  	  1FGL	  J1946.7-­‐5404,	  1FGL	  J2339.7-­‐0531	  (PI:	  Kong,	  A.,	  co-­‐PI:	  Kataoka,	  J.)	Finished	  	  • Further	  invesHgaHon	  based	  on	  mulHwavelength	  26	observaHons	Second	  Year	  Campaign	  We	  observed	  seven	  unassociated	  sources	  based	  on	  the	  eleven	  month	  of	  analysis.	  

Selec<on	  Criteria	  •Source	  name	  – 1FGL	  J0106.7+4853,	  J1312.6+0048,	  J1739.4+8717,	  J1743.8-­‐7620,	  J1902.0-­‐5110,	  J2043.2+1709,	  J2302.8+4443	  •Unassociated	  Objects	  •More	  than	  10	  degrees	  away	  from	  the	  galacHc	  plane	  •TS	  value	  >	  200	  27	Summary	  Counterpart

F(2-10keV)
erg cm-2 s-1

Gamma-ray
F(100 MeV- 200 GeV)erg cm-2 s-1

J0106.7+4853

No<	  1.43×10-­‐13	

2.42×10-­‐12	No	

J1312.6+0048	

Yes

8.01×10-­‐13	

1.04×10-­‐12	No	

J1739.4+8717	

No<	  1.11×10-­‐13	  	2.62×10-­‐12	No	

J1743.8-7620	

No<	  8.41×10-­‐14	

6.47×10-­‐12	No	

J1902.0-5110	

No<	  8.13×10-­‐15	  (for	  PSR)	

5.08×10-­‐12	Yes	J2043.2+1709	

No5.78×10-­‐12	Yes	J2302.8+4443	

Yes

5.62×10-­‐12	Yes	

X-ray
Name

kT	  =	  0.31	  keV	Radiopulsation

28	

Appendix	  1	  -­‐	  nH	  contour	

J2043.2 source A	

J2043.2 source B	

J2302.8	29

Appendix	  2	  –	  X-­‐ray	  light	  curve	  (XIS0+1+3)	  	J2043.2 source B	

J2043.2 source A	

J2302.8	30

Appendix	  3	  –	  J2043.2	  source	  B	Spectrum of source B with background	Black:xis0+3
Red:background	

Src B
backgroundA peak around 5 keV is not seen on the background spectrum.	

31

Appendix	  5	  –	  Radial	  proﬁle	  for	  source	  A	  of	  J2043.2	
• Photon counts vs r (Distance from the center of the source)	

Line: PSF
Plot: data	

Src A

32

Appendix	  6	  –	  Suzaku	  images	

(Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

1FGL J0106.7+4853	

xis0+3 (0.4-2keV)	

xis0+3 (2-10keV)	

xis1 (0.4-2keV)	

xis1 (2-10keV)	

33

Appendix	  6	  –	  Suzaku	  images	
(Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

1FGL J1739.4+8717	

xis0+3 (0.4-2keV)	

xis0+3 (2-10keV)	

xis1 (0.4-2keV)	

xis1 (2-10keV)	

34

Appendix	  6	  –	  Suzaku	  images	
(Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

1FGL J1743.8-7620	

xis0+3 (0.4-2keV)	

xis0+3 (2-10keV)	

xis1 (0.4-2keV)	

xis1 (2-10keV)	

35

Appendix	  6	  –	  Suzaku	  images	
(Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

1FGL J1902.0-5110	xis0+3 (0.4-2keV)	

xis0+3 (2-10keV)	

xis1 (0.4-2keV)	

xis1 (2-10keV)	

36

Appendix	  6	  –	  Suzaku	  images	
(Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

1FGL J2043.2+1709	

xis0+3 (0.4-2keV)	

xis0+3 (2-10keV)	

xis1 (0.4-2keV)	

xis1 (2-10keV)	

37

Appendix	  6	  –	  Suzaku	  images	
(Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

1FGL J2302.8+4443	

xis0+3 (0.4-2keV)	

xis0+3 (2-10keV)	

xis1 (0.4-2keV)	

xis1 (2-10keV)	

38

1FGL	  J1311.7-­‐3429	  Maeda	  et	  al.	  2011	  1FGL	  J1231.1-­‐1410	
Bright	  γ-­‐ray	  ﬂux	  &	  blackbody	  +	  PL	  is	  similar	  to	  the	  spectral	  structure	  of	  Geminga	  pulsar	  

1FGL	  J1311.7-­‐3429	
No	  pulse	  detecHon	  (γ-­‐ray,	  radio)	  Remain	  uncertain	  (not	  typical	  blazar)	  ?	  
QHB	  (QSO	  Hosted	  Blazar)	  ?!	  • 1FGL	  J1312.6+0048	
• One	  X-­‐ray	  point	  source	  was	   discovered	   inside	  the	  2FGL	  error	  ellipse	
Black:xis0+3
Gray:xis1
Model:	  power-­‐law	Preliminary	Suzaku/XIS0+3	  (0.5-­‐10keV)	  (Subtracted	  NXB,	  corrected	  Exposure	  and	  VignePng)	

42