DISCOVERY OF AN UNIDENTIFIED
                    <i>FERMI</i>
                    OBJECT AS A BLACK WIDOW-LIKE MILLISECOND PULSAR

Kong, Albert; Huang, R. H. H.; Cheng, K. S.; Takata, Jumpei; Yatsu, Yoichi; Cheung, C. C.; Donato, D.; Lin, L.; Kataoka, J.; Takahashi, Y.; Maeda, K.; Hui, C. Y.; Tam, P. H. T.

doi:10.1088/2041-8205/747/1/l3

Cited by 56 publications

(35 citation statements)

References 39 publications

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“…The number of MSP binaries detected in gamma-rays by Fermi-LAT has rapidly increased in the last year with the newly discovered systems PSR J1231-1411, PSR J0614-3329, and PSR J2214+3000 (Ransom et al 2011), PSR J1816+4510 (Kaplan et al 2012), PSR J0101-6422, PSR J1514-4946, and PSR J1902-5105 (Kerr et al 2012). A few are found to host so-called black widow pulsars such as PSR J2051-0827 (Wu et al 2012) and J 2339+0533 (Romani & Shaw 2011;Kong et al 2012). A number of them are detected as faint X-ray sources with X-ray luminosities typical of radio MSPs (e.g.…”

Section: Introductionmentioning

confidence: 99%

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

Martino

Belloni

Falanga

et al. 2013

A&A

129

137

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Context. XSS J1227.0-4859 is a peculiar, hard X-ray source recently positionally associated to the Fermi-LAT source 1FGL J1227.9-4852/2FGL J1227.7-4853. Multi-wavelength observations have added information on this source, indicating a low-luminosity lowmass X-ray binary (LMXB), but its nature is still unclear. Aims. To progress in our understanding, we present new X-ray data from a monitoring campaign performed in 2011 with the XMM-Newton, RXTE, and Swift satellites and combine them with new gamma-ray data from the Fermi and AGILE satellites. We complement the study with simultaneous near-UV photometry from XMM-Newton and with previous UV/optical and near-IR data. Methods. We analysed the temporal characteristics in the X-rays, near-UV, and gamma rays and studied the broad-band spectral energy distribution from radio to gamma rays. Results. The X-ray history of XSS J1227 over 7 yr shows a persistent and rather stable low-luminosity (6 × 10 33 d 2 1 kpc erg s −1 ) source, with flares and dips being peculiar and permanent characteristics. The associated Fermi-LAT source 2FGL J1227.7-4853 is also stable over an overlapping period of 4.7 yr. Searches for X-ray fast pulsations down to msec give upper limits to pulse fractional amplitudes of 15 − 25% that do not rule out a fast spinning pulsar. The combined UV/optical/near-IR spectrum reveals a hot component at ∼13 kK and a cool one at ∼4.6 kK. The latter would suggest a late-type K2−K5 companion star, a distance range of 1.4−3.6 kpc, and an orbital period of 7-9 h. A near-UV variability ( 6 h) also suggests a longer orbital period than previously estimated. Conclusions. The analysis shows that the X-ray and UV/optical/near-IR emissions are more compatible with an accretion-powered compact object than with a rotational powered pulsar. The X-ray to UV bolometric luminosity ratio could be consistent with a binary hosting a neutron star, but the uncertainties in the radio data may also allow an LMXB black hole with a compact jet. In this case, it would be the first associated with a high-energy gamma-ray source.

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Section: Introductionmentioning

confidence: 99%

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

Martino

Belloni

Falanga

et al. 2013

A&A

129

137

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“…For example, Cheung et al (2012) used Chandra to obtain X-ray images over the error ellipses of several Fermi-LAT sources out of the Galactic plane. With the refined X-ray positions in hand, variable optical counterparts were found for two sources that were then proposed to be elusive "radio-quiet" millisecond pulsars (Kong et al 2012;Romani & Shaw 2011;Romani 2012;Kataoka et al 2012). Both systems were subsequently confirmed as pulsars at radio wavelengths (Pletsch et al 2012;Belfiore 2013;Ray et al 2013); time-variable mass loss may sometimes obscure the radio emission.…”

Section: Introductionmentioning

confidence: 99%

1fgl J0523.5–2529: A New Probable Gamma-Ray Pulsar Binary

Strader¹,

Chomiuk²,

Сонбас³

et al. 2014

ApJ

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We report optical photometric and Southern Astrophysical Research spectroscopic observations of an X-ray source found within the localization error of the Fermi Large Area Telescope unidentified γ -ray source 1FGL J0523.5−2529. The optical data show periodic flux modulation and radial velocity variations indicative of a binary with a 16.5 hr period. The data suggest a massive non-degenerate secondary ( 0.8 M ), and we argue the source is likely a pulsar binary. The radial velocities have good phase coverage and show evidence for a measurable eccentricity (e = 0.04). There is no clear sign of irradiation of the secondary in either photometry or spectroscopy. The spatial location out of the Galactic plane and γ -ray luminosity of the source are more consistent with classification as a recycled millisecond pulsar than as a young pulsar. Future radio timing observations can confirm the identity of the primary and further characterize this interesting system.

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“…They furthermore challenge the existence of transitional MSP binaries to be identified yet. In particular radio MSPs systems have greatly increased in number with many associated with Fermi sources (Ransom et al 2011;Kaplan et al 2012;Kerr et al 2012;Kong et al 2012;Roberts 2013) among which PSR J1023+0038 (Tam et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Unveiling the redback nature of the low-mass X-ray binary XSS J1227.0−4859 through optical observations★

Martino

Casares

Mason

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The peculiar low mass X-ray binary XSS J12270-4859, associated with the Fermi/LAT source 2FGL J1227.7-4853, was in a X-ray, gamma-ray and optical low-luminosity persistent state for about a decade until the end of 2012, when it has entered into the dimmest state ever observed. The nature of the compact object has been controversial until the detection of a 1.69ms radio pulsar early 2014. We present optical spectroscopy and optical/near-IR photometry during the previous brighter and in the recent faint states. We determine the first spectroscopic orbital ephemeris and an accurate orbital period of 6.91246(5) h. We infer a mid G-type donor star and a distance d= 1.8-2.0 kpc. The donor spectral type changes from G5 V to F5 V between inferior and superior conjunction, a signature of strong irradiation effects. We infer a binary inclination 45 o i 65 o and a highly undermassive donor, M 2 ∼ 0.06 − 0.12 M ⊙ for a neutron star mass in the range 1.4-3 M ⊙ . Thus this binary joins as the seventh member the group of "redbacks". In the high state, the emission lines reveal the presence of an accretion disc. They tend to vanish at the donor star superior conjunction, where also flares are preferentially observed together with the occurrence of random dips. This behaviour could be related to the propeller mechanism of the neutron star recently proposed to be acting in this system during the high state. In the low state, the emission lines are absent at all orbital phases indicating that accretion has completely switched-off and that XSS J12270-4859 has transited from an accretion-powered to a rotation-powered phase.

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DISCOVERY OF AN UNIDENTIFIED FERMI OBJECT AS A BLACK WIDOW-LIKE MILLISECOND PULSAR

Cited by 56 publications

References 39 publications

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

1fgl J0523.5–2529: A New Probable Gamma-Ray Pulsar Binary

Unveiling the redback nature of the low-mass X-ray binary XSS J1227.0−4859 through optical observations★

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