Spectral and timing properties of IGR J00291+5934 during its 2015 outburst

Tiziana Di Salvo, Rosario Iaria, D'Aì, Riggio, Bozzo, Pintore, Egron, Sanna, Burderi, Papitto, Ferrigno, Di Salvo

Risultato della ricerca: Article

14 Citazioni (Scopus)

Abstract

We report on the spectral and timing properties of the accreting millisecond X-ray pulsar IGR J00291+5934 observed by XMM-Newton and NuSTAR during its 2015 outburst. The source is in a hard state dominated at high energies by a Comptonization of soft photons (~0.9 keV) by an electron population with kTe ~30 keV, and at lower energies by a blackbody component with kT ~ 0.5 keV. A moderately broad, neutral Fe emission line and four narrow absorption lines are also found. By investigating the pulse phase evolution, we derived the best-fitting orbital solution for the 2015 outburst. Comparing the updated ephemeris with those of the previous outbursts, we set a 3σ confidence level interval -6.6 × 10-13 s s-1 < P˙ orb < 6.5 × 10-13 s s-1 on the orbital period derivative. Moreover, we investigated the pulse profile dependence on energy finding a peculiar behaviour of the pulse fractional amplitude and lags as a function of energy.We performed a phase-resolved spectroscopy showing that the blackbody component tracks remarkably well the pulse profile, indicating that this component resides at the neutron star surface (hotspot).
Lingua originaleEnglish
pagine (da-a)2910-2917
Numero di pagine8
RivistaMonthly Notices of the Royal Astronomical Society
Volume466
Stato di pubblicazionePublished - 2017

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outburst
time measurement
energy
pulses
orbitals
pulse amplitude
XMM-Newton telescope
profiles
pulsars
newton
neutron stars
confidence
time lag
spectroscopy
intervals
electron
photons
electrons
x rays

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

Spectral and timing properties of IGR J00291+5934 during its 2015 outburst. / Di Salvo, Tiziana; Iaria, Rosario; D'Aì; Riggio; Bozzo; Pintore; Egron; Sanna; Burderi; Papitto; Ferrigno; Di Salvo.

In: Monthly Notices of the Royal Astronomical Society, Vol. 466, 2017, pag. 2910-2917.

Risultato della ricerca: Article

Di Salvo, T, Iaria, R, D'Aì, Riggio, Bozzo, Pintore, Egron, Sanna, Burderi, Papitto, Ferrigno & Di Salvo 2017, 'Spectral and timing properties of IGR J00291+5934 during its 2015 outburst', Monthly Notices of the Royal Astronomical Society, vol. 466, pagg. 2910-2917.
Di Salvo, Tiziana ; Iaria, Rosario ; D'Aì ; Riggio ; Bozzo ; Pintore ; Egron ; Sanna ; Burderi ; Papitto ; Ferrigno ; Di Salvo. / Spectral and timing properties of IGR J00291+5934 during its 2015 outburst. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 466. pagg. 2910-2917.
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abstract = "We report on the spectral and timing properties of the accreting millisecond X-ray pulsar IGR J00291+5934 observed by XMM-Newton and NuSTAR during its 2015 outburst. The source is in a hard state dominated at high energies by a Comptonization of soft photons (~0.9 keV) by an electron population with kTe ~30 keV, and at lower energies by a blackbody component with kT ~ 0.5 keV. A moderately broad, neutral Fe emission line and four narrow absorption lines are also found. By investigating the pulse phase evolution, we derived the best-fitting orbital solution for the 2015 outburst. Comparing the updated ephemeris with those of the previous outbursts, we set a 3σ confidence level interval -6.6 × 10-13 s s-1 < P˙ orb < 6.5 × 10-13 s s-1 on the orbital period derivative. Moreover, we investigated the pulse profile dependence on energy finding a peculiar behaviour of the pulse fractional amplitude and lags as a function of energy.We performed a phase-resolved spectroscopy showing that the blackbody component tracks remarkably well the pulse profile, indicating that this component resides at the neutron star surface (hotspot).",
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TY - JOUR

T1 - Spectral and timing properties of IGR J00291+5934 during its 2015 outburst

AU - Di Salvo, Tiziana

AU - Iaria, Rosario

AU - D'Aì, null

AU - Riggio, null

AU - Bozzo, null

AU - Pintore, null

AU - Egron, null

AU - Sanna, null

AU - Burderi, null

AU - Papitto, null

AU - Ferrigno, null

AU - Di Salvo, null

PY - 2017

Y1 - 2017

N2 - We report on the spectral and timing properties of the accreting millisecond X-ray pulsar IGR J00291+5934 observed by XMM-Newton and NuSTAR during its 2015 outburst. The source is in a hard state dominated at high energies by a Comptonization of soft photons (~0.9 keV) by an electron population with kTe ~30 keV, and at lower energies by a blackbody component with kT ~ 0.5 keV. A moderately broad, neutral Fe emission line and four narrow absorption lines are also found. By investigating the pulse phase evolution, we derived the best-fitting orbital solution for the 2015 outburst. Comparing the updated ephemeris with those of the previous outbursts, we set a 3σ confidence level interval -6.6 × 10-13 s s-1 < P˙ orb < 6.5 × 10-13 s s-1 on the orbital period derivative. Moreover, we investigated the pulse profile dependence on energy finding a peculiar behaviour of the pulse fractional amplitude and lags as a function of energy.We performed a phase-resolved spectroscopy showing that the blackbody component tracks remarkably well the pulse profile, indicating that this component resides at the neutron star surface (hotspot).

AB - We report on the spectral and timing properties of the accreting millisecond X-ray pulsar IGR J00291+5934 observed by XMM-Newton and NuSTAR during its 2015 outburst. The source is in a hard state dominated at high energies by a Comptonization of soft photons (~0.9 keV) by an electron population with kTe ~30 keV, and at lower energies by a blackbody component with kT ~ 0.5 keV. A moderately broad, neutral Fe emission line and four narrow absorption lines are also found. By investigating the pulse phase evolution, we derived the best-fitting orbital solution for the 2015 outburst. Comparing the updated ephemeris with those of the previous outbursts, we set a 3σ confidence level interval -6.6 × 10-13 s s-1 < P˙ orb < 6.5 × 10-13 s s-1 on the orbital period derivative. Moreover, we investigated the pulse profile dependence on energy finding a peculiar behaviour of the pulse fractional amplitude and lags as a function of energy.We performed a phase-resolved spectroscopy showing that the blackbody component tracks remarkably well the pulse profile, indicating that this component resides at the neutron star surface (hotspot).

KW - Accretion

KW - Accretion discs

KW - Astronomy and Astrophysics

KW - Space and Planetary Science

KW - Stars: neutron

KW - X-rays: binaries

UR - http://hdl.handle.net/10447/228375

UR - http://mnras.oxfordjournals.org/

M3 - Article

VL - 466

SP - 2910

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JO - Monthly Notices of the Royal Astronomical Society

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