IXPE and XMM-Newton Observations of the Soft Gamma Repeater SGR 1806–20

Medientyp: E-Artikel
Titel: IXPE and XMM-Newton Observations of the Soft Gamma Repeater SGR 1806–20
Beteiligte: Turolla, Roberto; Taverna, Roberto; Israel, Gian Luca; Muleri, Fabio; Zane, Silvia; Bachetti, Matteo; Heyl, Jeremy; Di Marco, Alessandro; Gau, Ephraim; Krawczynski, Henric; Ng, Mason; Possenti, Andrea; Poutanen, Juri; Baldini, Luca; Matt, Giorgio; Negro, Michela; Agudo, Iván; Antonelli, Lucio A.; Baumgartner, Wayne H.; Bellazzini, Ronaldo; Bianchi, Stefano; Bongiorno, Stephen D.; Bonino, Raffaella; Brez, Alessandro; [...]
Erschienen: American Astronomical Society, 2023
Erschienen in: The Astrophysical Journal
Sprache: Nicht zu entscheiden
DOI: 10.3847/1538-4357/aced05
ISSN: 0004-637X; 1538-4357
Schlagwörter: Space and Planetary Science ; Astronomy and Astrophysics
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Beschreibung: <jats:title>Abstract</jats:title> <jats:p>Recent observations with the Imaging X-ray Polarimetry Explorer (IXPE) of two anomalous X-ray pulsars provided evidence that X-ray emission from magnetar sources is strongly polarized. Here we report on the joint IXPE and XMM-Newton observations of the soft <jats:italic>γ</jats:italic>-repeater SGR 1806–20. The spectral and timing properties of SGR 1806–20 derived from XMM-Newton data are in broad agreement with previous measurements; however, we found the source at an all-time low persistent flux level. No significant polarization was measured apart from the 4–5 keV energy range, where a probable detection with PD = 31.6% ± 10.5% and <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{PA}=-17\buildrel{\circ}\over{.} {6}_{-15\buildrel{\circ}\over{.} 0}^{+15\buildrel{\circ}\over{.} 5}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>PA</mml:mi> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>17</mml:mn> <mml:mrow> <mml:mo>.°</mml:mo> </mml:mrow> <mml:msubsup> <mml:mrow> <mml:mn>6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>15</mml:mn> <mml:mrow> <mml:mo>.°</mml:mo> </mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>15</mml:mn> <mml:mrow> <mml:mo>.°</mml:mo> </mml:mrow> <mml:mn>5</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaced05ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> was obtained. The resulting polarization signal, together with the upper limits we derive at lower and higher energies (2–4 and 5–8 keV, respectively), is compatible with a picture in which thermal radiation from the condensed star surface is reprocessed by resonant Compton scattering in the magnetosphere, similar to what was proposed for the bright magnetar 4U 0142+61.</jats:p>
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