The XMM-Newton serendipitous survey

Watson, M. G.; Schröder, A. C.; Fyfe, D.; Page, C. G.; Lamer, G.; Mateos, S.; Pye, J. P.; Sakano, M.; Rosen, S. R.; Ballet, J.; Barcons, X.; Barret, D.; Böller, Thomas; Brunner, H.; Brusa, M.; Caccianiga, A.; Carrera, Francisco J.; Ceballos, M. T.; Ceca, R. Della; Denby, M.; Denkinson, G.; Dupuy, S.; Farrell, Sean; Fraschetti, Federico; Freyberg, M. J.; Guillout, P.; Hambaryan, V.; Maccacaro, T.; Mathiesen, Benjamin F.; McMahon, R. G.; Michel, Laurent; Motch, C.; Osborne, J. P.; Page, M. J.; Pakull, M. W.; Pietsch, W.; Saxton, R. D.; Schwope, A. D.; Severgnini, P.; Simpson, Moira; Sironi, G.; Stewart, G. C.; Stewart, I. M.; Stobbart, A. M.; Tedds, J. A.; Warwick, R. S.; Webb, N. A.; West, R. G.; Worrall, D. M.; Yuan, Weimin

doi:10.1051/0004-6361:200810534

Cited by 454 publications

(505 citation statements)

References 58 publications

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“…1). 5C 7.245 has been detected in X-rays with a flux of 7.1±2.5×10 −14 erg s −1 cm −2 in the 0.2-12 keV band, taken from the XMM-Newton Serendipitous Source Catalogue (2XMM hereafter; Watson et al 2009). However, the relatively low signal to noise (∼3) of this 2XMM detection results in a positional uncertainty large enough for the X-ray position to coincide with either the g or K-band sources.…”

Section: Agn Locationmentioning

confidence: 99%

Witnessing the transformation of a quasar host galaxy at z = 1.6

Humphrey

Roche

Gomes

et al. 2015

Monthly Notices of the Royal Astronomical Society

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A significant minority of high redshift radio galaxy (HzRG) candidates show extremely red broad band colours and remain undetected in emission lines after optical 'discovery' spectroscopy. In this paper we present deep GTC optical imaging and spectroscopy of one such radio galaxy, 5C 7.245, with the aim of better understanding the nature of these enigmatic objects. Our g-band image shows no significant emission coincident with the stellar emission of the host galaxy, but does reveal faint emission offset by ∼3 ′′ (26 kpc) therefrom along a similar position angle to that of the radio jets, reminiscent of the 'alignment effect' often seen in the optically luminous HzRGs. This offset g-band source is also detected in several UV emission lines, giving it a redshift of 1.609, with emission line flux ratios inconsistent with photoionization by young stars or an AGN, but consistent with ionization by fast shocks. Based on its unusual gas geometry, we argue that in 5C 7.245 we are witnessing a rare (or rarely observed) phase in the evolution of quasar hosts when stellar mass assembly, accretion onto the back hole, and powerful feedback activity has eradicated its cold gas from the central ∼20 kpc, but is still in the process of cleansing cold gas from its extended halo.

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Section: Agn Locationmentioning

confidence: 99%

Witnessing the transformation of a quasar host galaxy at z = 1.6

Humphrey

Roche

Gomes

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…A medium aluminum filter was used in front of the cameras to reject visible light from the stars. Seventy-one X-ray sources were detected that are listed in the XMM-Newton Serendipitous Source Catalog (Watson et al 2009). …”

Section: Introductionmentioning

confidence: 99%

“…X-ray fluxes are normally derived from source count rates using energy conversion factors (ECF). In the XMM-Newton catalog, these factors are calculated from a broadband source spectrum caracterised by a power law with a photon index Γ = 1.7 and an absorption column density N H = 3 × 10 20 cm −2 (Watson et al 2009). …”

Section: Introductionmentioning

confidence: 99%

X-ray emission regimes and rotation sequences in M 35

Gondoin

2013

A&A

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Context. Late-type stars in young open clusters show two kinds of dependence of their X-ray emission on rotation. They also tend to group into two main sub-populations that lie on narrow sequences in diagrams where their rotation periods are plotted against their (B − V) colour indices. A correlation between these two regimes of X-ray emission and the rotation sequences has been recently observed in the M 34 open cluster. Sun-like M 34 stars also show a drop of their X-ray to bolometric luminosity ratio by about one order of magnitude at a Rossby number of about 0.3. Aims. The present study looks for similar connections between X-ray activity and rotation in an other open cluster. The aim is to consolidate a model of X-ray activity evolution on the main sequence and to provide observational constraints on dynamo processes in the interiors of late-type stars. Methods. The paper compares XMM-Newton measurements of X-ray stellar emission in M 35 with X-ray luminosity distributions derived from rotation period measurements assuming either an X-ray regime transition at a critical Rossby number or a correlation between X-ray emission regimes and rotation sequences. Results. This second hypothesis could account for the low number of M 35 stars detected in X-rays. A model of X-ray activity evolution is proposed based on the correlation. One major output is that the transition from saturated to non-saturated X-ray emission occurs at Rossby numbers between about 0.13 and 0.4 for each star depending on its mass and initial period of rotation on the ZAMS. This prediction agrees with observations of stellar X-ray emission in M 34. It explains the large range of X-ray luminosities observed among Sun-like stars in young open clusters. Conclusions. I conclude that the correlation between X-ray emission regimes and rotation sequences could be a fundamental property of the early evolution of stellar magnetic activity on the main sequence. I argue that the angular momentum redistribution mechanism(s) responsible for the transition between rotation sequences could result in a changing mixture of dynamo processes occurring side by side, possibly including a turbulent dynamo at high rotation rate and an interface-type dynamo whose efficiency decreases progressively at later stage of stellar evolution when rotation dies away.

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“…This fact, coupled with the large field of view (FOV) of 30 , means that a single pointing on average detects 50 to 100 serendipitous X-ray sources (Watson et al 2009). …”

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confidence: 99%

TheXMM-Newtonserendipitous survey

Rosen

Webb

Watson

et al. 2016

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Context. Thanks to the large collecting area (3 × ∼1500 cm 2 at 1.5 keV) and wide field of view (30 across in full field mode) of the X-ray cameras on board the European Space Agency X-ray observatory XMM-Newton, each individual pointing can result in the detection of up to several hundred X-ray sources, most of which are newly discovered objects. Since XMM-Newton has now been in orbit for more than 15 yr, hundreds of thousands of sources have been detected. Aims. Recently, many improvements in the XMM-Newton data reduction algorithms have been made. These include enhanced source characterisation and reduced spurious source detections, refined astrometric precision of sources, greater net sensitivity for source detection, and the extraction of spectra and time series for fainter sources, both with better signal-to-noise. Thanks to these enhancements, the quality of the catalogue products has been much improved over earlier catalogues. Furthermore, almost 50% more observations are in the public domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science Centre to produce a much larger and better quality X-ray source catalogue. Methods. The XMM-Newton Survey Science Centre has developed a pipeline to reduce the XMM-Newton data automatically. Using the latest version of this pipeline, along with better calibration, a new version of the catalogue has been produced, using XMM-Newton X-ray observations made public on or before 2013 December 31. Manual screening of all of the X-ray detections ensures the highest data quality. This catalogue is known as 3XMM. Results. In the latest release of the 3XMM catalogue, 3XMM-DR5, there are 565 962 X-ray detections comprising 396 910 unique X-ray sources. Spectra and lightcurves are provided for the 133 000 brightest sources. For all detections, the positions on the sky, a measure of the quality of the detection, and an evaluation of the X-ray variability is provided, along with the fluxes and count rates in 7 X-ray energy bands, the total 0.2-12 keV band counts, and four hardness ratios. With the aim of identifying the detections, a cross correlation with 228 catalogues of sources detected in all wavebands is also provided for each X-ray detection. Conclusions. 3XMM-DR5 is the largest X-ray source catalogue ever produced. Thanks to the large array of data products associated with each detection and each source, it is an excellent resource for finding new and extreme objects.Key words. catalogs -astronomical databases: miscellaneous -surveys -X-rays: general Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.The catalogue is available at http://cdsarc.u-strasbg.fr/ viz-bin/VizieR?-meta.foot&-source=IX/46

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The XMM-Newton serendipitous survey

Cited by 454 publications

References 58 publications

Witnessing the transformation of a quasar host galaxy at z = 1.6

Witnessing the transformation of a quasar host galaxy at z = 1.6

X-ray emission regimes and rotation sequences in M 35

TheXMM-Newtonserendipitous survey

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