| Título: | A strongly magnetized pulsar within the grasp of the milky way’s supermassive black hole |
| Autores: |
Rea, Nanda Esposito, Paolo Pons Botella, José Antonio Turolla, Roberto Torres, Diego F. Israel, Gian Luca Possenti, Andrea Burgay, Marta Viganò, Daniele Papitto, Alessandro Perna, Rosalba Stella, Luigi Ponti, Gabriele Baganoff, Frederick K. Haggard, Daryl Camero-Arranz, Ascensión Zane, Silvia Minter, Anthony Mereghetti, Sandro Tiengo, Andrea Schödel, Rainer Feroci, Marco Mignani, Roberto P. Götz, Diego |
| Fecha: |
2013-11-12 2013-11-12 2013-09-11 |
| Publicador: | RUA Docencia |
| Fuente: |
 |
| Tipo: | info:eu-repo/semantics/article |
| Tema: |
Galaxy: center Stars: neutron X-rays: individual (SGR J1745–2900) Astronomía y Astrofísica |
| Descripción: |
The center of our Galaxy hosts a supermassive black hole, Sagittarius (Sgr) A∗. Young, massive stars within 0.5 pc of Sgr A∗ are evidence of an episode of intense star formation near the black hole a few million years ago, which might have left behind a young neutron star traveling deep into Sgr A∗’s gravitational potential. On 2013 April 25, a short X-ray burst was observed from the direction of the Galactic center. With a series of observations with the Chandra and the Swift satellites, we pinpoint the associated magnetar at an angular distance of 2.4±0.3 arcsec from Sgr A∗, and refine the source spin period and its derivative (P = 3.7635537(2) s and ˙ P = 6.61(4) × 10−12 s s−1), confirmed by quasi simultaneous radio observations performed with the Green Bank Telescope and Parkes Radio Telescope, which also constrain a dispersion measure of DM = 1750 ± 50 pc cm−3, the highest ever observed for a radio pulsar. We have found that this X-ray source is a young magnetar at ≈0.07–2 pc from Sgr A∗. Simulations of its possible motion around Sgr A∗ show that it is likely (∼90% probability) in a bound orbit around the black hole. The radiation front produced by the past activity from the magnetar passing through the molecular clouds surrounding the Galactic center region might be responsible for a large fraction of the light echoes observed in the Fe fluorescence features. We acknowledge support by grants AYA 2012-39303, SGR2009-811, iLINK 2011-0303, AYA 2010-21097-C03-02, Prometeo 2009/103, AYA2010-17631, P08-TIC-4075, INAF 2010 PRIN grant, Chandra Awards GO2-13076X, G03-14060X, GO3-14099X and G03-14121X, and an EU Marie Curie IEF (FP7-PEOPLE-2012-IEF-331095). |
| Idioma: | Inglés |
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