Having discovered the pulsar in Puppis A and ruled out a magnetar, we willdetermine if it is a weakly magnetized neutron star like the other CCO pulsarsby obtaining a phase-coherent timing solution, the only practical way ofmeasuring its spin-down rate. Our sensitivity to P-dot will correspond to asurface dipole B-field as small as 3.e10 G, comparable to to our measured valuefor the CCO pulsar PSR J1852+0040 in Kes 79. New spectra will also allow us tofurther localize its apparent 0.8 keV emission line in rotation phase, and tomodel the emission and viewing geometry of this unique system. This will provideimportant support for the anti-magnetar model of CCOs, while exploringpossible reasons for their unexplained surface hot spots.
Publications
The Spin-down of PSR J0821-4300 and PSR J1210-5226: Confirmation of Central Compact Objects as Anti-magnetars |Gotthelf, E. V., Halpern, J. P., | ApJ | 765-58 | 2013 | 2013ApJ...765...58G | http://ui.adsabs.harvard.edu/#abs/2013ApJ...765...58G
The XMM-Newton serendipitous survey. VIII. The first XMM-Newton serendipitous source catalogue from overlapping observations |Traulsen, I., Schwope, A. D., et al. | A&A | 624-77 | 2019 | 2019A&A...624A..77T | http://ui.adsabs.harvard.edu/#abs/2019A&A...624A..77T
Measuring the Nonaxially Symmetric Surface Temperature Distribution of the Central Compact Object in Puppis A |Alford, J. A. J., Gotthelf, E. V., et al. | ApJ | 927-233 | 2022 | 2022ApJ...927..233A | http://ui.adsabs.harvard.edu/#abs/2022ApJ...927..233A
Rectangular core-collapse supernova remnants: application to Puppis A |Meyer, D. M. -A., Vel\\u00e1zquez, P. F., et al. | MNRAS | 515-594 | 2022 | 2022MNRAS.515..594M | http://ui.adsabs.harvard.edu/#abs/2022MNRAS.515..594M
Robust constraints on feebly interacting particles using XMM-Newton |Luque, Pedro De la Torre, Balaji, Shyam, | PhRvD | 109-L101305 | 2024 | 2024PhRvD.109j1305L | http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j1305L
Multimessenger search for electrophilic feebly interacting particles from supernovae |Luque, Pedro De la Torre, Balaji, Shyam, | PhRvD | 109-103028 | 2024 | 2024PhRvD.109j3028L | http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j3028L
Importance of Cosmic-Ray Propagation on Sub-GeV Dark Matter Constraints |De la Torre Luque, Pedro, Balaji, Shyam, | ApJ | 968-46 | 2024 | 2024ApJ...968...46D | http://ui.adsabs.harvard.edu/#abs/2024ApJ...968...46D
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2010-05-02T18:38:01Z/2011-04-13T04:51:35Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations. Since Earths atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
European Space Agency, Prof Jules Halpern, 2012, 'Measuring the Magnetic Field of the CCO Pulsar in Puppis A', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-yreicsy
