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|Title:||A Very Young Radio-loud Magnetar||Authors:||Esposito, P.
Zelati, F. Coti
ISRAEL, Gian Luca
Castillo, G. A. Rodríguez
|Issue Date:||2020||Journal:||THE ASTROPHYSICAL JOURNAL LETTERS||Number:||896||Issue:||2||First Page:||L30||Abstract:||The magnetar Swift J1818.0-1607 was discovered in 2020 March when Swift detected a 9 ms hard X-ray burst and a long-lived outburst. Prompt X-ray observations revealed a spin period of 1.36 s, soon confirmed by the discovery of radio pulsations. We report here on the analysis of the Swift burst and follow-up X-ray and radio observations. The burst average luminosity was Lburst ∼ 2 × 1039 erg s-1 (at 4.8 kpc). Simultaneous observations with XMM-Newton and NuSTAR three days after the burst provided a source spectrum well fit by an absorbed blackbody ( NH = (1.13 ± 0.03) × 1023 cm-2 and kT = 1.16 ± 0.03 keV) plus a power law (Γ = 0.0 ± 1.3) in the 1-20 keV band, with a luminosity of ∼8 × 1034 erg s-1, dominated by the blackbody emission. From our timing analysis, we derive a dipolar magnetic field B ∼ 7 × 1014 G, spin-down luminosity E˙rot∼1.4×1036 erg s-1, and characteristic age of 240 yr, the shortest currently known. Archival observations led to an upper limit on the quiescent luminosity <5.5 × 1033 erg s-1, lower than the value expected from magnetar cooling models at the source characteristic age. A 1 hr radio observation with the Sardinia Radio Telescope taken about 1 week after the X-ray burst detected a number of strong and short radio pulses at 1.5 GHz, in addition to regular pulsed emission; they were emitted at an average rate 0.9 min-1 and accounted for ∼50% of the total pulsed radio fluence. We conclude that Swift J1818.0-1607 is a peculiar magnetar belonging to the small, diverse group of young neutron stars with properties straddling those of rotationally and magnetically powered pulsars. Future observations will make a better estimation of the age possible by measuring the spin-down rate in quiescence.||URI:||http://hdl.handle.net/20.500.12386/29845||URL:||https://iopscience.iop.org/article/10.3847/2041-8213/ab9742||ISSN:||2041-8205||DOI:||10.3847/2041-8213/ab9742||Bibcode ADS:||2020ApJ...896L..30E||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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