The AWM 7 cluster is a nearby bright cluster (z=0.017; kT=3.7 keV), which formsa part of the Perseus- Pisces filament. We propose to map the AWM 7 cluster tocover 0.3-1 r500 with 8 pointings with a 200 ks total exposure. One objective isto derive Si abundance out to r500. With Suzaku data out to the virial radius,we will be able to constrain the ratio of the Si mass in the ICM and totalstellar luminosity of galaxies out to the virial radius. Another objective is toderive two-dimensional maps of temperature and entropy, and with the Suzaku dataout to the virial radius, and to study history of accretion along the filamentand gas heating.
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
Blasts from the Past: Supernova Shock Breakouts among X-Ray Transients in the XMM-Newton Archive |Alp, Dennis, Larsson, Josefin, | ApJ | 896-39 | 2020 | 2020ApJ...896...39A | http://ui.adsabs.harvard.edu/#abs/2020ApJ...896...39A
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
Luminosity Function and Event Rate Density of XMM-Newton-selected Supernova Shock Breakout Candidates |Sun, Hui, Liu, He-Yang, et al. | ApJ | 927-224 | 2022 | 2022ApJ...927..224S | http://ui.adsabs.harvard.edu/#abs/2022ApJ...927..224S
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
XMM-Newton-discovered Fast X-ray Transients: host galaxies and limits on contemporaneous detections of optical counterparts |Eappachen, D., Jonker, P. G., et al. | MNRAS | 527-11823 | 2024 | 2024MNRAS.52711823E | http://ui.adsabs.harvard.edu/#abs/2024MNRAS.52711823E
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
2014-08-11T08:07:38Z/2014-08-12T00:39:18Z
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 Kyoko Matsushita, 2015, 'Si mass and the entropy distribution of the AWM7 cluster out to r500', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-e1axu5b
