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X-ray Observations of New Gamma-ray Pulsars Discovered by Fermi LAT

X-ray Observations of New Gamma-ray Pulsars Discovered by Fermi LAT. Nobuyuki Kawai and Yoshikazu Kanai (Tokyo Tech) On behalf of Fermi/LAT Collaboration. Suzaku. Motivation. Fermi LAT detected 55 pulsars including 24 new ones X-ray observations are essential for those newcomers.

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X-ray Observations of New Gamma-ray Pulsars Discovered by Fermi LAT

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  1. X-ray Observations ofNew Gamma-ray PulsarsDiscovered by Fermi LAT Nobuyuki Kawaiand Yoshikazu Kanai (Tokyo Tech) On behalf ofFermi/LAT Collaboration Suzaku

  2. Motivation • Fermi LAT detected 55 pulsars including 24 new ones • X-ray observations are essential for those newcomers (1) X-ray counterparts can give unique information ofprecise positions in the sky if the sources cannot be found in the radio survey (2) Gamma-ray studies cannot find any differences between radio-loud and radio-quiet pulsars but how about X-ray properties?

  3. XIS0+3 images 0.5 – 10 keV Preliminary Suzaku Observations • - 12 pulsars, 280 ks in total for AO4 • XIS nominal position • No window/burst/timing option- Detecting pulsation is NOT aimed • 9 pulsars observed as of today

  4. J0357+32 J0633+0632 J1413-6205 J1459-60 and J1028-5819 …discovered in radio but no X-ray observations J1907+06 J1954+2836 J1958+2846 J2238+59 • Right: Position in the P – P plot • E = 5.8 x 1033 – 2.8 x 1036 erg/s • tc = 20 – 547 kyr . . ATNF Pulsars Observed Pulsars Observed Pulsars

  5. Pulsars observedby Suzaku Observed Pulsars - Position in the all-sky map

  6. . • - tc = 59 kyr, E = 1.2 x 1035 erg s-1 • 24 ks exposure • Soft point source + Extended emission PSR J0633+0632 - Images XIS0+3 0.5 – 2 keV 2 – 10 keV 3s error fromtiming analysis Preliminary 95% error inour latest catalog

  7. . • - tc = 59 kyr, E = 1.2 x 1035 erg s-1 • 24 ks exposure • Soft point source + Extended emission PSR J0633+0632 - Images XIS0+3 0.5 – 2 keV 2 – 10 keV Background Source Preliminary

  8. PSR J0633+0632– Spectrum - Absorbed power-law model is the best Preliminary NH < 4 x 1020 cm-2 G = 1.52 cn2 = 74.73 / 77 + 0.09 – 0.08

  9. . • - tc = 547 kyr, E = 5.8 x 1033 erg s-1 • 21 ks exposure • Point source + Extended emission? PSR J0357+32 - Images XIS0+3 3s error fromtemporal analysis 0.5 – 2 keV 2 – 10 keV Preliminary 95% error inour latest catalog

  10. . • - tc = 547 kyr, E = 5.8 x 1033 erg s-1 • 21 ks exposure • Point source + Extended emission? PSR J0357+32 - Images XIS0+3 0.5 – 2 keV 2 – 10 keV Background Source Preliminary

  11. PSR J0357+32 - Spectrum - Absorbed power-law model is the best Preliminary NH < 6 x 1021 cm-2 G = 1.87 cn2 = 22.23 / 19 + 0.53 – 0.41

  12. Results Overview • X-ray counterparts are found for most of the targets • Only one target lacks obvious counterpart... Nearby source is analyzed • PL or PL + BB model is preferred Preliminary • “Known radio pulsars” • are radio pulsars • Detected by Fermi LAT • and • Studied in X-ray band. • Including 5 EGRET PSRs Distribution of photon index similar to known pulsars. “Fermi LAT pulsars”include pulsars Suzakuobserved, Geminga andthe new pulsar in CTA 1(meaning no radiodetection or radio quiet)

  13. - Distance can be estimated with Lg and Fg for new pulsars - Assuming a relation Lgµ E0.5 . Distance Estimation to Calculate X-ray Luminosity Pulsar Catalog paper(Abdo et al., ApJ submitted)

  14. . ( ) Ögelman 1995,Kawai et al. 1997 • New pulsars follow the relation Lxµ E, too • No differences were found in this study . Lxµ E Spin-down Luminosity vs X-ray Luminosity Lx distribution Preliminary Crab Preliminary Fermi LAT can find fainter PSRs More complete population studies

  15. Summary • We are observing Fermi LAT pulsars with Suzaku • Faint X-ray counterparts are found for most of targets • Power-law component found for all sources • Properties similar to those of gamma-ray pulsars with radio emission Further X-ray observations are ongoingwith Chandra and XMM-Newton

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