We propose a re-observation of NGC 499 which, with NGC 507, forms one of thebest examples of a group-group merger in the local universe. Excellent archivalXMM data for NGC 507 is available, but virgul80% of our 55 ks AO5 observation of NGC499 was lost to background flaring. With this re-observation we will be able toproduce high resolution spectral maps of both groups and the gas between them,providing a wealth of data on the effects of the merger on the two systems. Wewill search for signs of tidal stripping and gas compression, and produce modelsof the temperature, abundance and mass distribution out to virgul600 kpc, providingdetailed information on the structure of the two systems and shedding light onthis important stage in the evolution of groups.
Publications
Constraints on turbulent velocity broadening for a sample of clusters, groups and elliptical galaxies using XMM-Newton |Sanders, J. S., Fabian, A. C., | MNRAS | 410-1797 | 2011 | 2011MNRAS.410.1797S | http://ui.adsabs.harvard.edu/#abs/2011MNRAS.410.1797S
Revealing O VII from stacked X-ray grating spectra of clusters, groups and elliptical galaxies |Sanders, J. S., Fabian, A. C., | MNRAS | 412-35 | 2011 | 2011MNRAS.412L..35S | http://ui.adsabs.harvard.edu/#abs/2011MNRAS.412L..35S
The cosmological analysis of X-ray cluster surveys - II. Application of the CR-HR method to the XMM archive |Clerc, N., Sadibekova, T., et al. | MNRAS | 423-3561 | 2012 | 2012MNRAS.423.3561C | http://ui.adsabs.harvard.edu/#abs/2012MNRAS.423.3561C
Velocity width measurements of the coolest X-ray emitting material in the cores of clusters, groups and elliptical galaxies |Sanders, J. S., Fabian, A. C., | MNRAS | 429-2727 | 2013 | 2013MNRAS.429.2727S | http://ui.adsabs.harvard.edu/#abs/2013MNRAS.429.2727S
SPIDERS: the spectroscopic follow-up of X-ray selected clusters of galaxies in SDSS-IV |Clerc, N., Merloni, A., et al. | MNRAS | 463-4490 | 2016 | 2016MNRAS.463.4490C | http://ui.adsabs.harvard.edu/#abs/2016MNRAS.463.4490C
X-ray properties of the X-CLASS-redMaPPer galaxy cluster sample: the luminosity-temperature relation |Molham, Mona, Clerc, Nicolas, et al. | MNRAS | 494-161 | 2020 | 2020MNRAS.494..161M | http://ui.adsabs.harvard.edu/#abs/2020MNRAS.494..161M
Multiwavelength classification of X-ray selected galaxy cluster candidates using convolutional neural networks |Kosiba, Matej, Lieu, Maggie, et al. | MNRAS | 496-4141 | 2020 | 2020MNRAS.496.4141K | http://ui.adsabs.harvard.edu/#abs/2020MNRAS.496.4141K
SPIDERS: overview of the X-ray galaxy cluster follow-up and the final spectroscopic data release |Clerc, N., Kirkpatrick, C. C., et al. | MNRAS | 497-3976 | 2020 | 2020MNRAS.497.3976C | http://ui.adsabs.harvard.edu/#abs/2020MNRAS.497.3976C
The Cosmic Large-Scale Structure in X-rays (CLASSIX) Cluster Survey. III. The Perseus-Pisces supercluster and the Southern Great Wall as traced by X-ray luminous galaxy clusters |B\\u00f6hringer, Hans, Chon, Gayoung, | A&A | 651-16 | 2021 | 2021A&A...651A..16B | http://ui.adsabs.harvard.edu/#abs/2021A&A...651A..16B
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 Ewan O.Sullivan, 2008, 'NGC 499 - Mapping the merger of two X-ray luminous galaxy groups', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-77drc5x
