MULTI-WAVELENGTH OBSERVATIONS OF THE BLACK WIDOW PULSAR 2FGL J2339.6-0532 WITH OISTER AND SUZAKU
ABSTRACT Multi-wavelength observations of the black widow binary system 2FGL J2339.6-0532 are reported. The Fermi gamma-ray source 2FGL J2339.6-0532 was recently categorized as a black widow in which a recycled millisecond pulsar (MSP) is evaporating the companion star with its powerful pulsar wind....
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| creator | Yatsu, Yoichi Kataoka, Jun Takahashi, Yosuke Tachibana, Yutaro Kawai, Nobuyuki Shibata, Shimpei Pike, Sean Yoshii, Taketoshi Arimoto, Makoto Saito, Yoshihiko Nakamori, Takeshi Sekiguchi, Kazuhiro Kuroda, Daisuke Yanagisawa, Kenshi Hanayama, Hidekazu Watanabe, Makoto Hamamoto, Ko Nakao, Hikaru Ozaki, Akihito Motohara, Kentaro Konishi, Masahiro Tateuchi, Ken Matsunaga, Noriyuki Morokuma, Tomoki Nagayama, Takahiro Murata, Katsuhiro Akitaya, Hiroshi Yoshida, Michitoshi Ali, Gamal B. Mohamed, A. Essam Isogai, Mizuki Arai, Akira Takahashi, Hidenori Hashimoto, Osamu Miyanoshita, Ryo Omodaka, Toshihiro Takahashi, Jun Tokimasa, Noritaka Matsuda, Kentaro Okumura, Shin-ichiro Nishiyama, Kota Urakawa, Seitaro Nogami, Daisaku Oasa, Yumiko |
| description | ABSTRACT Multi-wavelength observations of the black widow binary system 2FGL J2339.6-0532 are reported. The Fermi gamma-ray source 2FGL J2339.6-0532 was recently categorized as a black widow in which a recycled millisecond pulsar (MSP) is evaporating the companion star with its powerful pulsar wind. Our optical observations show clear sinusoidal light curves due to the asymmetric temperature distribution of the companion star. Assuming a simple geometry, we constrained the range of the inclination angle of the binary system to , which enables us to discuss the interaction between the pulsar wind and the companion in detail. The X-ray spectrum consists of two components: a soft, steady component that seems to originate from the surface of the MSP, and a hard, variable component from the wind-termination shock near the companion star. The measured X-ray luminosity is comparable to the bolometric luminosity of the companion, meaning that the heating efficiency is less than 0.5. In the companion orbit, 1011 cm from the pulsar, the pulsar wind is already in the particle-dominant stage with a magnetization parameter of . In addition, we precisely investigated the time variations of the X-ray periodograms and detected a weakening of the orbital modulation. The observed phenomenon may be related to unstable pulsar wind activity or weak mass accretion, both of which can result in the temporal extinction of the radio pulse. |
| doi_str_mv | 10.1088/0004-637X/802/2/84 |
| format | Article |
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Essam ; Isogai, Mizuki ; Arai, Akira ; Takahashi, Hidenori ; Hashimoto, Osamu ; Miyanoshita, Ryo ; Omodaka, Toshihiro ; Takahashi, Jun ; Tokimasa, Noritaka ; Matsuda, Kentaro ; Okumura, Shin-ichiro ; Nishiyama, Kota ; Urakawa, Seitaro ; Nogami, Daisaku ; Oasa, Yumiko</creator><creatorcontrib>Yatsu, Yoichi ; Kataoka, Jun ; Takahashi, Yosuke ; Tachibana, Yutaro ; Kawai, Nobuyuki ; Shibata, Shimpei ; Pike, Sean ; Yoshii, Taketoshi ; Arimoto, Makoto ; Saito, Yoshihiko ; Nakamori, Takeshi ; Sekiguchi, Kazuhiro ; Kuroda, Daisuke ; Yanagisawa, Kenshi ; Hanayama, Hidekazu ; Watanabe, Makoto ; Hamamoto, Ko ; Nakao, Hikaru ; Ozaki, Akihito ; Motohara, Kentaro ; Konishi, Masahiro ; Tateuchi, Ken ; Matsunaga, Noriyuki ; Morokuma, Tomoki ; Nagayama, Takahiro ; Murata, Katsuhiro ; Akitaya, Hiroshi ; Yoshida, Michitoshi ; Ali, Gamal B. ; Mohamed, A. Essam ; Isogai, Mizuki ; Arai, Akira ; Takahashi, Hidenori ; Hashimoto, Osamu ; Miyanoshita, Ryo ; Omodaka, Toshihiro ; Takahashi, Jun ; Tokimasa, Noritaka ; Matsuda, Kentaro ; Okumura, Shin-ichiro ; Nishiyama, Kota ; Urakawa, Seitaro ; Nogami, Daisaku ; Oasa, Yumiko ; on behalf of OISTER team</creatorcontrib><description>ABSTRACT Multi-wavelength observations of the black widow binary system 2FGL J2339.6-0532 are reported. The Fermi gamma-ray source 2FGL J2339.6-0532 was recently categorized as a black widow in which a recycled millisecond pulsar (MSP) is evaporating the companion star with its powerful pulsar wind. Our optical observations show clear sinusoidal light curves due to the asymmetric temperature distribution of the companion star. Assuming a simple geometry, we constrained the range of the inclination angle of the binary system to , which enables us to discuss the interaction between the pulsar wind and the companion in detail. The X-ray spectrum consists of two components: a soft, steady component that seems to originate from the surface of the MSP, and a hard, variable component from the wind-termination shock near the companion star. The measured X-ray luminosity is comparable to the bolometric luminosity of the companion, meaning that the heating efficiency is less than 0.5. In the companion orbit, 1011 cm from the pulsar, the pulsar wind is already in the particle-dominant stage with a magnetization parameter of . In addition, we precisely investigated the time variations of the X-ray periodograms and detected a weakening of the orbital modulation. The observed phenomenon may be related to unstable pulsar wind activity or weak mass accretion, both of which can result in the temporal extinction of the radio pulse.</description><identifier>ISSN: 0004-637X</identifier><identifier>ISSN: 1538-4357</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/802/2/84</identifier><language>eng</language><publisher>United Kingdom: The American Astronomical Society</publisher><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; Binary systems ; BOLOMETERS ; Companion stars ; COMPARATIVE EVALUATIONS ; DIAGRAMS ; GAMMA RADIATION ; gamma rays: stars ; INCLINATION ; LUMINOSITY ; MAGNETIZATION ; MASS ; Orbitals ; ORBITS ; PULSARS ; pulsars: general ; pulsars: individual (2FGL J2339.6-0532) ; STARS ; STELLAR WINDS ; TEMPERATURE DISTRIBUTION ; X-RAY SPECTRA ; X-rays ; X-rays: binaries</subject><ispartof>The Astrophysical journal, 2015-04, Vol.802 (2), p.1-11</ispartof><rights>2015. The American Astronomical Society. All rights reserved.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c424t-5059366075bdeb1efe222170fa8ccb685c316bfbaad88019be0b011c9946d5103</citedby><cites>FETCH-LOGICAL-c424t-5059366075bdeb1efe222170fa8ccb685c316bfbaad88019be0b011c9946d5103</cites><orcidid>0000-0003-4433-3600 ; 0000-0003-1890-3913</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.1088/0004-637X/802/2/84/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.1088/0004-637X/802/2/84$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://www.osti.gov/biblio/22882585$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Yatsu, Yoichi</creatorcontrib><creatorcontrib>Kataoka, Jun</creatorcontrib><creatorcontrib>Takahashi, Yosuke</creatorcontrib><creatorcontrib>Tachibana, Yutaro</creatorcontrib><creatorcontrib>Kawai, Nobuyuki</creatorcontrib><creatorcontrib>Shibata, Shimpei</creatorcontrib><creatorcontrib>Pike, Sean</creatorcontrib><creatorcontrib>Yoshii, Taketoshi</creatorcontrib><creatorcontrib>Arimoto, Makoto</creatorcontrib><creatorcontrib>Saito, Yoshihiko</creatorcontrib><creatorcontrib>Nakamori, Takeshi</creatorcontrib><creatorcontrib>Sekiguchi, Kazuhiro</creatorcontrib><creatorcontrib>Kuroda, Daisuke</creatorcontrib><creatorcontrib>Yanagisawa, Kenshi</creatorcontrib><creatorcontrib>Hanayama, Hidekazu</creatorcontrib><creatorcontrib>Watanabe, Makoto</creatorcontrib><creatorcontrib>Hamamoto, Ko</creatorcontrib><creatorcontrib>Nakao, Hikaru</creatorcontrib><creatorcontrib>Ozaki, Akihito</creatorcontrib><creatorcontrib>Motohara, Kentaro</creatorcontrib><creatorcontrib>Konishi, Masahiro</creatorcontrib><creatorcontrib>Tateuchi, Ken</creatorcontrib><creatorcontrib>Matsunaga, Noriyuki</creatorcontrib><creatorcontrib>Morokuma, Tomoki</creatorcontrib><creatorcontrib>Nagayama, Takahiro</creatorcontrib><creatorcontrib>Murata, Katsuhiro</creatorcontrib><creatorcontrib>Akitaya, Hiroshi</creatorcontrib><creatorcontrib>Yoshida, Michitoshi</creatorcontrib><creatorcontrib>Ali, Gamal B.</creatorcontrib><creatorcontrib>Mohamed, A. Essam</creatorcontrib><creatorcontrib>Isogai, Mizuki</creatorcontrib><creatorcontrib>Arai, Akira</creatorcontrib><creatorcontrib>Takahashi, Hidenori</creatorcontrib><creatorcontrib>Hashimoto, Osamu</creatorcontrib><creatorcontrib>Miyanoshita, Ryo</creatorcontrib><creatorcontrib>Omodaka, Toshihiro</creatorcontrib><creatorcontrib>Takahashi, Jun</creatorcontrib><creatorcontrib>Tokimasa, Noritaka</creatorcontrib><creatorcontrib>Matsuda, Kentaro</creatorcontrib><creatorcontrib>Okumura, Shin-ichiro</creatorcontrib><creatorcontrib>Nishiyama, Kota</creatorcontrib><creatorcontrib>Urakawa, Seitaro</creatorcontrib><creatorcontrib>Nogami, Daisaku</creatorcontrib><creatorcontrib>Oasa, Yumiko</creatorcontrib><creatorcontrib>on behalf of OISTER team</creatorcontrib><title>MULTI-WAVELENGTH OBSERVATIONS OF THE BLACK WIDOW PULSAR 2FGL J2339.6-0532 WITH OISTER AND SUZAKU</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>ABSTRACT Multi-wavelength observations of the black widow binary system 2FGL J2339.6-0532 are reported. The Fermi gamma-ray source 2FGL J2339.6-0532 was recently categorized as a black widow in which a recycled millisecond pulsar (MSP) is evaporating the companion star with its powerful pulsar wind. Our optical observations show clear sinusoidal light curves due to the asymmetric temperature distribution of the companion star. Assuming a simple geometry, we constrained the range of the inclination angle of the binary system to , which enables us to discuss the interaction between the pulsar wind and the companion in detail. The X-ray spectrum consists of two components: a soft, steady component that seems to originate from the surface of the MSP, and a hard, variable component from the wind-termination shock near the companion star. The measured X-ray luminosity is comparable to the bolometric luminosity of the companion, meaning that the heating efficiency is less than 0.5. In the companion orbit, 1011 cm from the pulsar, the pulsar wind is already in the particle-dominant stage with a magnetization parameter of . In addition, we precisely investigated the time variations of the X-ray periodograms and detected a weakening of the orbital modulation. The observed phenomenon may be related to unstable pulsar wind activity or weak mass accretion, both of which can result in the temporal extinction of the radio pulse.</description><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>Binary systems</subject><subject>BOLOMETERS</subject><subject>Companion stars</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>DIAGRAMS</subject><subject>GAMMA RADIATION</subject><subject>gamma rays: stars</subject><subject>INCLINATION</subject><subject>LUMINOSITY</subject><subject>MAGNETIZATION</subject><subject>MASS</subject><subject>Orbitals</subject><subject>ORBITS</subject><subject>PULSARS</subject><subject>pulsars: general</subject><subject>pulsars: individual (2FGL J2339.6-0532)</subject><subject>STARS</subject><subject>STELLAR WINDS</subject><subject>TEMPERATURE DISTRIBUTION</subject><subject>X-RAY SPECTRA</subject><subject>X-rays</subject><subject>X-rays: binaries</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqNkUFvm0AQhVdRK8V18gdyWqmXXrB3Z1nYPRIH29TURAbsqpctrBeVyDYOiw_994U66rHKaTSa782M3kPogZIJJUJMCSGu4zH_-1QQmMJUuDdoRDkTjsu4_wGN_gG36JO1L0MLUo7Qz295nEXOLtiGcbheZEucPKbhZhtkUbJOcTLH2TLEj3EwW-Fd9JTs8HMep8EGw3wR46_AmJx4DuEM-vGgjtIs3OBg_YTT_Eewyu_Qx6o4WHP_Vscon4fZbOnEySKaBbGjXXA7hxMumecRn5d7U1JTGQCgPqkKoXXpCa4Z9cqqLIq9EITK0pCSUKqldL09p4SN0efr3sZ2tbK67oz-pZvTyehOAQgBXPCe-nKlzm3zejG2U8faanM4FCfTXKyivmTAweP-O9D-K1_6f2_DFdVtY21rKnVu62PR_laUqCEfNfitBvtVn48CJdxeNLmK6uasXppLe-rt-Z_gDwePhhU</recordid><startdate>20150401</startdate><enddate>20150401</enddate><creator>Yatsu, Yoichi</creator><creator>Kataoka, Jun</creator><creator>Takahashi, Yosuke</creator><creator>Tachibana, Yutaro</creator><creator>Kawai, Nobuyuki</creator><creator>Shibata, Shimpei</creator><creator>Pike, Sean</creator><creator>Yoshii, Taketoshi</creator><creator>Arimoto, Makoto</creator><creator>Saito, Yoshihiko</creator><creator>Nakamori, Takeshi</creator><creator>Sekiguchi, Kazuhiro</creator><creator>Kuroda, Daisuke</creator><creator>Yanagisawa, Kenshi</creator><creator>Hanayama, Hidekazu</creator><creator>Watanabe, Makoto</creator><creator>Hamamoto, Ko</creator><creator>Nakao, Hikaru</creator><creator>Ozaki, Akihito</creator><creator>Motohara, Kentaro</creator><creator>Konishi, Masahiro</creator><creator>Tateuchi, Ken</creator><creator>Matsunaga, Noriyuki</creator><creator>Morokuma, Tomoki</creator><creator>Nagayama, Takahiro</creator><creator>Murata, Katsuhiro</creator><creator>Akitaya, Hiroshi</creator><creator>Yoshida, Michitoshi</creator><creator>Ali, Gamal B.</creator><creator>Mohamed, A. Essam</creator><creator>Isogai, Mizuki</creator><creator>Arai, Akira</creator><creator>Takahashi, Hidenori</creator><creator>Hashimoto, Osamu</creator><creator>Miyanoshita, Ryo</creator><creator>Omodaka, Toshihiro</creator><creator>Takahashi, Jun</creator><creator>Tokimasa, Noritaka</creator><creator>Matsuda, Kentaro</creator><creator>Okumura, Shin-ichiro</creator><creator>Nishiyama, Kota</creator><creator>Urakawa, Seitaro</creator><creator>Nogami, Daisaku</creator><creator>Oasa, Yumiko</creator><general>The American Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0003-4433-3600</orcidid><orcidid>https://orcid.org/0000-0003-1890-3913</orcidid></search><sort><creationdate>20150401</creationdate><title>MULTI-WAVELENGTH OBSERVATIONS OF THE BLACK WIDOW PULSAR 2FGL J2339.6-0532 WITH OISTER AND SUZAKU</title><author>Yatsu, Yoichi ; Kataoka, Jun ; Takahashi, Yosuke ; Tachibana, Yutaro ; Kawai, Nobuyuki ; Shibata, Shimpei ; Pike, Sean ; Yoshii, Taketoshi ; Arimoto, Makoto ; Saito, Yoshihiko ; Nakamori, Takeshi ; Sekiguchi, Kazuhiro ; Kuroda, Daisuke ; Yanagisawa, Kenshi ; Hanayama, Hidekazu ; Watanabe, Makoto ; Hamamoto, Ko ; Nakao, Hikaru ; Ozaki, Akihito ; Motohara, Kentaro ; Konishi, Masahiro ; Tateuchi, Ken ; Matsunaga, Noriyuki ; Morokuma, Tomoki ; Nagayama, Takahiro ; Murata, Katsuhiro ; Akitaya, Hiroshi ; Yoshida, Michitoshi ; Ali, Gamal B. ; Mohamed, A. 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Essam</creatorcontrib><creatorcontrib>Isogai, Mizuki</creatorcontrib><creatorcontrib>Arai, Akira</creatorcontrib><creatorcontrib>Takahashi, Hidenori</creatorcontrib><creatorcontrib>Hashimoto, Osamu</creatorcontrib><creatorcontrib>Miyanoshita, Ryo</creatorcontrib><creatorcontrib>Omodaka, Toshihiro</creatorcontrib><creatorcontrib>Takahashi, Jun</creatorcontrib><creatorcontrib>Tokimasa, Noritaka</creatorcontrib><creatorcontrib>Matsuda, Kentaro</creatorcontrib><creatorcontrib>Okumura, Shin-ichiro</creatorcontrib><creatorcontrib>Nishiyama, Kota</creatorcontrib><creatorcontrib>Urakawa, Seitaro</creatorcontrib><creatorcontrib>Nogami, Daisaku</creatorcontrib><creatorcontrib>Oasa, Yumiko</creatorcontrib><creatorcontrib>on behalf of OISTER team</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Yatsu, Yoichi</au><au>Kataoka, Jun</au><au>Takahashi, Yosuke</au><au>Tachibana, Yutaro</au><au>Kawai, Nobuyuki</au><au>Shibata, Shimpei</au><au>Pike, Sean</au><au>Yoshii, Taketoshi</au><au>Arimoto, Makoto</au><au>Saito, Yoshihiko</au><au>Nakamori, Takeshi</au><au>Sekiguchi, Kazuhiro</au><au>Kuroda, Daisuke</au><au>Yanagisawa, Kenshi</au><au>Hanayama, Hidekazu</au><au>Watanabe, Makoto</au><au>Hamamoto, Ko</au><au>Nakao, Hikaru</au><au>Ozaki, Akihito</au><au>Motohara, Kentaro</au><au>Konishi, Masahiro</au><au>Tateuchi, Ken</au><au>Matsunaga, Noriyuki</au><au>Morokuma, Tomoki</au><au>Nagayama, Takahiro</au><au>Murata, Katsuhiro</au><au>Akitaya, Hiroshi</au><au>Yoshida, Michitoshi</au><au>Ali, Gamal B.</au><au>Mohamed, A. Essam</au><au>Isogai, Mizuki</au><au>Arai, Akira</au><au>Takahashi, Hidenori</au><au>Hashimoto, Osamu</au><au>Miyanoshita, Ryo</au><au>Omodaka, Toshihiro</au><au>Takahashi, Jun</au><au>Tokimasa, Noritaka</au><au>Matsuda, Kentaro</au><au>Okumura, Shin-ichiro</au><au>Nishiyama, Kota</au><au>Urakawa, Seitaro</au><au>Nogami, Daisaku</au><au>Oasa, Yumiko</au><aucorp>on behalf of OISTER team</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>MULTI-WAVELENGTH OBSERVATIONS OF THE BLACK WIDOW PULSAR 2FGL J2339.6-0532 WITH OISTER AND SUZAKU</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2015-04-01</date><risdate>2015</risdate><volume>802</volume><issue>2</issue><spage>1</spage><epage>11</epage><pages>1-11</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><abstract>ABSTRACT Multi-wavelength observations of the black widow binary system 2FGL J2339.6-0532 are reported. The Fermi gamma-ray source 2FGL J2339.6-0532 was recently categorized as a black widow in which a recycled millisecond pulsar (MSP) is evaporating the companion star with its powerful pulsar wind. Our optical observations show clear sinusoidal light curves due to the asymmetric temperature distribution of the companion star. Assuming a simple geometry, we constrained the range of the inclination angle of the binary system to , which enables us to discuss the interaction between the pulsar wind and the companion in detail. The X-ray spectrum consists of two components: a soft, steady component that seems to originate from the surface of the MSP, and a hard, variable component from the wind-termination shock near the companion star. The measured X-ray luminosity is comparable to the bolometric luminosity of the companion, meaning that the heating efficiency is less than 0.5. In the companion orbit, 1011 cm from the pulsar, the pulsar wind is already in the particle-dominant stage with a magnetization parameter of . In addition, we precisely investigated the time variations of the X-ray periodograms and detected a weakening of the orbital modulation. The observed phenomenon may be related to unstable pulsar wind activity or weak mass accretion, both of which can result in the temporal extinction of the radio pulse.</abstract><cop>United Kingdom</cop><pub>The American Astronomical Society</pub><doi>10.1088/0004-637X/802/2/84</doi><tpages>11</tpages><orcidid>https://orcid.org/0000-0003-4433-3600</orcidid><orcidid>https://orcid.org/0000-0003-1890-3913</orcidid></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2015-04, Vol.802 (2), p.1-11 |
| issn | 0004-637X 1538-4357 1538-4357 |
| language | eng |
| recordid | cdi_osti_scitechconnect_22882585 |
| source | Open Access: IOP Publishing Free Content |
| subjects | ASTROPHYSICS, COSMOLOGY AND ASTRONOMY Binary systems BOLOMETERS Companion stars COMPARATIVE EVALUATIONS DIAGRAMS GAMMA RADIATION gamma rays: stars INCLINATION LUMINOSITY MAGNETIZATION MASS Orbitals ORBITS PULSARS pulsars: general pulsars: individual (2FGL J2339.6-0532) STARS STELLAR WINDS TEMPERATURE DISTRIBUTION X-RAY SPECTRA X-rays X-rays: binaries |
| title | MULTI-WAVELENGTH OBSERVATIONS OF THE BLACK WIDOW PULSAR 2FGL J2339.6-0532 WITH OISTER AND SUZAKU |
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