Please use this identifier to cite or link to this item:
|Title:||XMM-Newton and INTEGRAL view of the hard state of EXO 1745-248 during its 2015 outburst||Authors:||Matranga, M.
Di Salvo, T.
Torres, D. F.
DE MARTINO, Domitilla
Gambino, A. F.
|Issue Date:||2017||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||603||First Page:||A39||Abstract:||Context. Transient low-mass X-ray binaries (LMXBs) often show outbursts that typically last a few weeks and are characterized by a high X-ray luminosity (L<SUB>x</SUB> ≈ 10<SUP>36</SUP>-10<SUP>38</SUP> erg s<SUP>-1</SUP>), while most of the time they are found in X-ray quiescence (L<SUB>X</SUB> ≈ 10<SUP>31</SUP>-10<SUP>33</SUP> erg s<SUP>-1</SUP>). The source EXO 1745-248 is one of them. <BR /> Aims: The broad-band coverage and sensitivity of the instrument on board XMM-Newton and INTEGRAL offers the opportunity of characterizing the hard X-ray spectrum during the outburst of EXO 1745-248. <BR /> Methods: We report on quasi-simultaneous XMM-Newton and INTEGRAL observations of the X-ray transient EXO 1745-248 located in the globular cluster Terzan 5, performed ten days after the beginning of the outburst (on 2015 March 16) of the source between March and June 2015. The source was caught in a hard state, emitting a 0.8-100 keV luminosity of ≃ 10<SUP>37</SUP> erg s<SUP>-1</SUP>. <BR /> Results: The spectral continuum was dominated by thermal Comptonization of seed photons with temperature kT<SUB>in</SUB> ≃ 1.3 keV, by a cloud with a moderate optical depth τ ≃ 2, and with an electron temperature of kT<SUB>e</SUB> ≃ 40 keV. A weaker soft thermal component at temperature kT<SUB>th</SUB> ≃ 0.6-0.7 keV and compatible with a fraction of the neutron star radius was also detected. A rich emission line spectrum was observed by the EPIC-pn on board XMM-Newton; features at energies compatible with K-α transitions of ionized sulfur, argon, calcium, and iron were detected, with a broadness compatible with either thermal Compton broadening or Doppler broadening in the inner parts of an accretion disk truncated at 20 ± 6 gravitational radii from the neutron star. Strikingly, at least one narrow emission line ascribed to neutral or mildly ionized iron is needed to model the prominent emission complex detected between 5.5 and 7.5 keV. The different ionization state and broadness suggest an origin in a region located farther from the neutron star than where the other emission lines are produced. Seven consecutive type I bursts were detected during the XMM-Newton observation, none of which showed hints of photospheric radius expansion. A thorough search for coherent pulsations from the EPIC-pn light curve did not result in any significant detection. Upper limits ranging from a few to 15% on the signal amplitude were set, depending on the unknown spin and orbital parameters of the system.||URI:||http://hdl.handle.net/20.500.12386/27288||URL:||http://arxiv.org/abs/1703.07389v1
|Appears in Collections:||1.01 Articoli in rivista|
Show full item record
Files in This Item:
|Matranga_2017.pdf||Pdf editoriale||1.15 MB||Adobe PDF||View/Open|
checked on Sep 23, 2020
checked on Sep 23, 2020
Items in DSpace are published in Open Access, unless otherwise indicated.