X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-ray<i>Fermi</i>-LAT association

Martino, D. de; Belloni, T.; Falanga, M.; Papitto, A.; Motta, S.; Pellizzoni, A.; Evangelista, Y.; Piano, G.; Masetti, N.; Bonnet‐Bidaud, J. M.; Mouchet, M.; Mukai, K.; Possenti, A.

doi:10.1051/0004-6361/201220393

Cited by 122 publications

(155 citation statements)

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“…This confirms the importance of this identification work on catalogued but unidentified high-energy sources, because peculiar objects can be found within the considered samples (see, for instance, Paper IX; Masetti et al 2007Masetti et al , 2008bBassani et al 2012;de Martino et al 2010de Martino et al , 2013. With the present data, we also correct two results given in Paper IX, namely the actual redshift (z = 2.02) of the Type 1 QSO IGR J16388+3557 and the correct counterpart of source IGR J06293−1359.…”

Section: Discussionsupporting

confidence: 88%

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Chavushyan¹

2013

A&A

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Within the framework of our program (running since 2004) of identification of hard X-ray INTEGRAL sources through optical spectroscopy, we present the results concerning the nature of 33 high-energy objects. The data were acquired with the use of six telescopes of different sizes and from one on-line archive. The results indicate that the majority of these objects (23 out of 33) are active galactic nuclei (AGNs), whereas 10 are sources in the local Universe with eight of which in the Galaxy and two in the Small Magellanic Cloud (SMC). Among the identified AGNs, 13 are of Type 1 (i.e., with broad emission lines), eight are of Type 2 (with narrow emissions only), and two are X-ray bright, optically normal galaxies with no apparent nuclear activity in the optical. Six of these AGNs lie at high redshift (z > 0.5). Concerning local objects, we found that five of them are Galactic cataclysmic variables, three are high-mass X-ray binaries (two of which lying in the SMC), one is a low-mass X-ray binary, and one is classified as a flare star that is likely of RS CVn type. The main optical properties and inferred physical characteristics of these sources are presented and discussed.

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Section: Discussionsupporting

confidence: 88%

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Chavushyan¹

2013

A&A

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“…Subsequent independent multi-wavelength studies (Pretorius 2009;Saitou et al 2009;de Martino et al 2010de Martino et al , 2013Hill et al 2011; casted doubts on this classification, suggesting instead an identification as a LMXB showing unusual dipping and flaring behaviour on timescales of few hundreds of seconds. XSS J12270−4859 was subsequently recognised to be spatially coincident with a moderately bright gamma-ray source that was detected by Fermi-LAT emitting up to 10 GeV (de Martino et al 2010;Hill et al 2011), and is now known as 3FGL J1227.9−4854.…”

Section: Xss J12270-4859mentioning

confidence: 99%

Different twins in the millisecond pulsar recycling scenario: Optical polarimetry of PSR J1023+0038 and XSS J12270-4859

Baglio

D’Avanzo

Campana

et al. 2016

A&A

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We present the first optical polarimetric study of the two transitional pulsars PSR J1023+0038 and XSS J12270-4859. This work is focused on the search for intrinsically linearly polarised optical emission from the two systems. To this aim, we carried out multiband optical (BVRi) and near-infrared (NIR; JHK) photo-polarimetric observations of the two systems using the ESO New Technology Telescope (NTT) at La Silla (Chile), equipped with the EFOSC2 and the SOFI instruments. The system XSS J12270-4859 was observed during its radio-pulsar state; we did not detect a significant degree of polarisation in any of the bands, with 3σ upper limits, for example, of 1.4% in the R-band. We built the NIR−optical averaged spectral energy distribution (SED) of the system, which could be described well by an irradiated black body with radius R * = 0.33 ± 0.03 R and albedo η = 0.32 ± 0.05, without the need for further components. Thus, we excluded the visible presence of an extended accretion disc and/or of relativistic jets. The case was different for PSR J1023+0038, which was in its accretion phase during our campaign. We measured a linear polarisation of 1.09 ± 0.27% and 0.90 ± 0.17% in the V and R bands, respectively. The phase-resolved polarimetric curve of the source in the R band reveals a hint of a sinusoidal modulation at the source 4.75 h orbital period, peaked at the same orbital phase as the light curve. The measured optical polarisation of PSR J1023+0038 could, in principle, be interpreted as electron scattering with free electrons, which can be found in the accretion disc of the system or even in the hot corona that sorrounds the disc itself, or as synchrotron emission from a jet of relativistic particles or an outflow. However, the NIR-optical SED of the system built from our dataset did not suggest the presence of a jet. We conclude that the optical linear polarisation observed for PSR J1023+0038 is possibly due to Thomson scattering with electrons in the disc, as is also suggested from the possible modulation of the R-band linear polarisation at the system orbital period.

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“…Some LMXBs show rapid time variability and hard X-ray spectra (c.f., XSS J12270−4859; Saitou et al 2011;de Martino et al 2013). However, they show spectral hardening during flares, whereas 2XMM J185114.3−000004 didn't show any significant spectral change during its flare.…”

Section: Xmm J1851143−000004mentioning

confidence: 99%

Discovery of X-Ray Emission From the Galactic Supernova Remnant G32.8-0.1 With Suzaku

Bamba

Terada

Hewitt

et al. 2016

ApJ

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We present the first dedicated X-ray study of the supernova remnant (SNR) G32.8−0.1 (Kes 78) with Suzaku. X-ray emission from the whole SNR shell has been detected for the first time. The X-ray morphology is well correlated with the emission from the radio shell, while anti-correlated with the molecular cloud found in the SNR field. The X-ray spectrum shows not only conventional low-temperature (kT ∼ 0.6 keV) thermal emission in a non-equilibrium ionization state, but also a very high temperature (kT ∼ 3.4 keV) component with a very low ionization timescale (∼ 2.7 × 10 9 cm −3 s), or a hard non-thermal component with a photon index Γ∼2.3. The average density of the low-temperature plasma is rather low, of the order of 10 −3 -10 −2 cm −3 , implying that this SNR is expanding into a low-density cavity. We discuss the X-ray emission of the SNR, also detected in TeV with H.E.S.S., together with multi-wavelength studies of the remnant and other gamma-ray emitting SNRs, such as W28 and RCW 86. Analysis of a time-variable source, 2XMM J185114.3−000004, found in the northern part of the SNR, is also reported for the first time. Rapid time variability and a heavily absorbed hard X-ray spectrum suggest that this source could be a new supergiant fast X-ray transient.

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

Cited by 122 publications

References 57 publications

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Different twins in the millisecond pulsar recycling scenario: Optical polarimetry of PSR J1023+0038 and XSS J12270-4859

Discovery of X-Ray Emission From the Galactic Supernova Remnant G32.8-0.1 With Suzaku

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