Abell 3667 is the archetype of a merging cluster with radio relics. The NW relicis the brightest cluster relic or halo known. This region was imaged with XMM inAO-7. We detected a X-ray brightness and hardness jump at the edge of the NWrelic. This could be due to a merger shock, or to inverse Compton (IC) emissionfrom the relic; both are consistent within the errors. We propose a longobservation to determine the contributions of shock and IC emission. Comparisonof the shock properties and the radio relic will be a critical test of the shockacceleration model for relics. The relic IC emission will give the magneticfield and cosmic ray energy of the relic. We will determine the efficiency ofparticle acceleration, and provide the first data on the physics of cosmic shock fronts.
X-Ray Scaling Relations for a Representative Sample of Planck-selected Clusters Observed with XMM-Newton |Lovisari, Lorenzo, Schellenberger, Gerrit, et al. | ApJ | 892-102 | 2020 | 2020ApJ...892..102L | http://ui.adsabs.harvard.edu/#abs/2020ApJ...892..102L
Comparing different mass estimators for a large subsample of the Planck-ESZ clusters |Lovisari, L., Ettori, S., et al. | A&A | 644-78 | 2020 | 2020A&A...644A..78L | http://ui.adsabs.harvard.edu/#abs/2020A&A...644A..78L
MeerKAT view of the diffuse radio sources in Abell 3667 and their interactions with the thermal plasma |de Gasperin, F., Rudnick, L., et al. | A&A | 659-146 | 2022 | 2022A&A...659A.146D | http://ui.adsabs.harvard.edu/#abs/2022A&A...659A.146D
Constraining the mass and redshift evolution of the hydrostatic mass bias using the gas mass fraction in galaxy clusters |Wicker, R., Douspis, M., et al. | A&A | 674-48 | 2023 | 2023A&A...674A..48W | http://ui.adsabs.harvard.edu/#abs/2023A&A...674A..48W
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
2010-09-21T13:29:42Z/2010-11-03T09:22:37Z
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 Craig Sarazin, 2011, 'The Physics of Cosmic Shocks: The NW Merger Shock and Radio Relic in Abell 3667', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-af6n2kd
