The investigators request a 130 ks stare. of 3C 111 in order to measure thehigh-frequency end of the power spectral density (PSD) of the X-ray fluxvariations. Combined with long-term monitoring with RXTE that is sampling theintermediate and low frequencies, the data will define the break in the PSD.This will add an FR II radio galaxy to the relationship between break frequency,black-hole mass, and accretion rate of both AGNs and XRBs. The long-term lightcurves display dips in X-ray flux that precede the appearance of superluminalknots in the radio jet. The lag between the start of an X-ray event and thefirst appearance of a knot in the jet core. will determine the length scale ofthe jet, which we can relate to the black hole.s gravitational radius.
Discussing the physical meaning of the absorption feature at 2.1 keV in 4U 1538-52 |Rodes-Roca, J. J., Torrejon, J. M., et al. | AN | 335-804 | 2014 | 2014AN....335..804R | http://ui.adsabs.harvard.edu/#abs/2014AN....335..804R
Comparison of ejection events in the jet and accretion disc outflows in 3C 111 |Tombesi, F., Sambruna, R. M., et al. | MNRAS | 424-754 | 2012 | 2012MNRAS.424..754T | http://ui.adsabs.harvard.edu/#abs/2012MNRAS.424..754T
A comprehensive analysis of the hard X-ray spectra of bright Seyfert galaxies |Lubinski, P., Beckmann, V., et al. | MNRAS | 458-2454 | 2016 | 2016MNRAS.458.2454L | http://ui.adsabs.harvard.edu/#abs/2016MNRAS.458.2454L
The 3CR Chandra Snapshot Survey: Extragalactic Radio Sources with Redshifts between 1 and 1.5 |Stuardi, C., Missaglia, V., et al. | ApJS | 235-32 | 2018 | 2018ApJS..235...32S | http://ui.adsabs.harvard.edu/#abs/2018ApJS..235...32S
X-ray occultations in active galactic nuclei: distribution in size of orbiting clouds and total mass content in the cloud ensemble |Pietrini, P., Torricelli-Ciamponi, G., | A&A | 628-26 | 2019 | 2019A&A...628A..26P | http://ui.adsabs.harvard.edu/#abs/2019A&A...628A..26P
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
2009-02-15T14:44:57Z/2009-02-17T04:01:23Z
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 ALAN MARSCHER, 2010, 'PSD BREAK comma JET SCALE comma AND BLACK-HOLE MASS OF THE FR II RADIO GALAXY 3C 111', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-u9uboix
