In the Forward Shock (FS) model, the GRB afterglow is produced in thecircumburst medium when the ejecta interacts with it. However, a few GRBs havean X-ray lightcurve with a very large change of decay slope, that is hard toexplain by a FS, while their optical behaviour is different and more consistentwith it. One proposed solution is that X-ray emission is produced within theejecta, and ends in a few ks. We propose to test this scenario by observing atlate epochs 2 GRBs with a large break in the X-ray lightcurve and detectedoptical afterglow with XMM-Newton. In this model, the X-ray flux at late epochsshould return to a shallower decay, similar to the optical, when the emissionfrom the FS prevails. XMM-Newton high sensitivity is required to constrain the X-ray flux at late times.
The 80 Ms follow-up of the X-ray afterglow of GRB 130427A challenges the standard forward shock model |De Pasquale, M., Page, M. J., et al. | MNRAS | 462-1111 | 2016 | 2016MNRAS.462.1111D | http://ui.adsabs.harvard.edu/#abs/2016MNRAS.462.1111D
X\\u2011HESS: A large sample of highly accreting serendipitous AGN under the XMM\\u2011Newton microscope |Laurenti, M., Tombesi, F., et al. | AN | 344-20230053 | 2023 | 2023AN....34430053L | http://ui.adsabs.harvard.edu/#abs/2023AN....34430053L
The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O VII, O VIII, and Fe L-shell Transitions |Pan, Zeyang, Qu, Zhijie, et al. | ApJS | 271-62 | 2024 | 2024ApJS..271...62P | http://ui.adsabs.harvard.edu/#abs/2024ApJS..271...62P
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
2013-05-13T03:12:55Z/2013-06-20T09:14:15Z
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, Dr Massimiliano De Pasquale, 2014, 'Non-forward shock components in X-ray afterglows', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-vh51ryu
