A5093077062- Astrophysical Phenomena and Observations
- Stellar, planetary, and galactic studies
- Pulsars and Gravitational Waves Research
- Mechanics and Biomechanics Studies
- Astrophysics and Cosmic Phenomena
- Astrophysics and Star Formation Studies
- Astronomical Observations and Instrumentation
- Adaptive optics and wavefront sensing
- High-pressure geophysics and materials
- Gamma-ray bursts and supernovae
University of Palermo
2023-2024
National Institute for Astrophysics
2023-2024
Institut de Recherche en Astrophysique et Planétologie
2024
Université de Toulouse
2024
Centre National de la Recherche Scientifique
2024
Université Toulouse III - Paul Sabatier
2024
Abstract We present the first X-ray polarization measurements of GX 339–4. IXPE observed this source twice during its 2023–2024 outburst, once in soft-intermediate state and again a soft state. The observation taken intermediate shows significant (4 σ ) degree P X = 1.3% ± 0.3% angle θ −74° 7° only 3–8 keV band. FORS2 at Very Large Telescope simultaneously, detecting optical B , V R I bands (between ∼0.1% ∼0.7%), all roughly aligned with polarization. also detect discrete jet knot from radio...
Aims. X 1822-371 is an eclipsing binary system with a period close to 5.57 h and orbital derivative Ṗ orb of 1.42(3) × 10 −10 s −1 . The extremely high value its compatible super-Eddington mass transfer rate from the companion star and, consequently, intrinsic luminosity at Eddington limit. source also X-ray pulsar, it shows spin frequency 1.69 Hz in spin-up phase 7.4 −12 Assuming limit, neutron magnetic field strength B = 8 G estimated. However, direct measure could be obtained observing...
The X-ray dipper MAXI J1305-704 is a dynamically confirmed black hole (BH) binary discovered decade ago. While its only outburst has been studied in detail X-rays, follow-up at other wavelengths scarce. We report here the results from an optical spectroscopy campaign across of J1305-704. analysed two epochs data obtained by Magellan Clay Telescope during consecutive nights, when source was soft spectral state. identified typical emission lines outbursting low-mass binaries, such as hydrogen...
XTE J1710-281 is a transient eclipsing binary system with period close to 3.28 hours, hosting neutron star. The average eclipse duration 420 seconds, and arrival times reported in the literature span from 1999 2017. A previous analysis of using timing technique revealed complex pattern delays, indicating presence three orbital glitches. These glitches correspond sudden variations period, allowing for identification four distinct epochs. We have re-analyzed 78 spanning 18 years utilizing...
X 1822-371 is an eclipsing binary system with a period close to 5.57 hr and orbital derivative $\dot{P}_{\rm orb}$ of 1.42(3)$\times 10^{-10}$ s s$^{-1}$. The extremely high value its compatible super-Eddington mass transfer rate from the companion star and, consequently, intrinsic luminosity at Eddington limit. source also X-ray pulsar, it shows spin frequency 1.69 Hz in spin-up phase $7.4 \times 10^{-12}$ Assuming limit, neutron magnetic field strength $B = 8 10^{10}$ G estimated. However,...
Aims. XTE J1710−281 is a transient eclipsing binary system with period close to 3.28 h that hosts neutron star. The average eclipse duration 420 s, and arrival times reported in the literature span from 1999 2017. A previous analysis of using timing technique revealed complex pattern delays, indicating presence three orbital glitches. These glitches correspond sudden variations allow for identification four distinct epochs, during which derivative was estimated be −1.8 × 10 −12 s −1 , 0.07...
We propose a novel approach for determining the orbital inclination of low-mass X-ray binary systems by modelling H α and β line profiles emitted accretion disc, with Newtonian (i.e. non-relativistic) version DISKLINE . applied model to two sample sources, Swift J1357.2–0933 MAXI J1305–704, which are both transient black hole systems, analyse observations that were collected during quiescent state one observation an outburst. The profile is well described model, although we had add Gaussian...
Swift J1357.2−0933 is a transient low-mass X-ray binary hosting stellar-mass black hole. The source exhibits optical dips and very broad emission lines during both outburst quiescence, which are thought to be the result of high orbital inclination. We present phase-resolved spectroscopy obtained with 10.4 m Gran Telescopio Canarias (GTC). spectra focus on H β spectral region quiescence. line exceptionally (full width at half maximum, FWHM > 4000 Å), in agreement previous studies focused α...
Swift J1357.2-0933 is a transient low-mass X-ray binary hosting stellar-mass black hole. The source exhibits optical dips and very broad emission lines during both outburst quiescence, which are thought to be the result of high orbital inclination. We present phase-resolved spectroscopy obtained with 10.4m Gran Telescopio Canarias (GTC). spectra focus on $\rm{H}\beta$ spectral region quiescence. line exceptionally (full width at half maximum, FWHM > 4000 \AA), in agreement previous studies...