A dataset provided by the European Space Agency

Name: The orbital light curve of the galactic supersoft X-ray source QR And
Published: 2003-02-09T00:00:00Z

Proposal ID	004794
Title	The orbital light curve of the galactic supersoft X-ray source QR And
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0047940101 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0047940201
DOI	https://doi.org/10.5270/esa-t1ohpqx
Principal Investigator, PI	Dr Klaus Reinsch
Abstract	QR And is the brightest binary supersoft X-ray source visible in the whole sky.Despite intense optical/UV follow-up observations, its nature is still largelyuncertain. With XMM we will for the first time be able to continuously monitorthe soft X-ray flux over a complete binary orbital cycle of 15.85 hr. The EPICpn and MOS will be used to firmly derive the orbital light curve of this uniqueobject and, therewith, to provide information about the orbital inclination, the suggested existence of an accretion disk rim, and the origin of short-termfluctuations. In addition, we will obtain high-quality phase-averaged spectrawith the EPIC pn, EPIC MOS, and RGS providing diagnostical information on the
Publications	The XMM Cluster Survey: optical analysis methodology and the first data release \|Mehrtens Nicola Romer A. Kathy et al. \| MNRAS \| 423-1024 \| 2012 \| 2012MNRAS.423.1024M \| http://ui.adsabs.harvard.edu/#abs/2012MNRAS.423.1024M The XMM Cluster Survey: X-ray analysis methodology \|Lloyd-Davies E. J. Romer A. Kathy et al. \| MNRAS \| 418-14 \| 2011 \| 2011MNRAS.418...14L \| http://ui.adsabs.harvard.edu/#abs/2011MNRAS.418...14L The XMM-Newton serendipitous ultraviolet source survey catalogue \|Page M. J. Brindle C. et al. \| MNRAS \| 426-903 \| 2012 \| 2012MNRAS.426..903P \| http://ui.adsabs.harvard.edu/#abs/2012MNRAS.426..903P Obscuration effects in super-soft-source X-ray spectra \|Ness J.-U. Osborne J. P. et al. \| A&A \| 559-50 \| 2013 \| 2013A&A...559A..50N \| http://ui.adsabs.harvard.edu/#abs/2013A&A...559A..50N Serendipitous UV source catalogues for 10 years of XMM and 5 years of Swift \|Yershov V. N. \| Ap&SS \| 354-97 \| 2014 \| 2014Ap&SS.354...97Y \| http://ui.adsabs.harvard.edu/#abs/2014Ap&SS.354...97Y Short-period X-ray oscillations in super-soft novae and persistent super-soft sources \|Ness J.-U. Beardmore A. P. et al. \| A&A \| 578-39 \| 2015 \| 2015A&A...578A..39N \| http://ui.adsabs.harvard.edu/#abs/2015A&A...578A..39N Sunyaev-Zeldovich effect or not? Detecting the main foreground effect of most galaxy clusters \|Xiao Weike Chen Chen et al. \| MNRAS \| 432-41 \| 2013 \| 2013MNRAS.432L..41X \| http://ui.adsabs.harvard.edu/#abs/2013MNRAS.432L..41X FUV and X-ray grating spectra of novae and supersoft X-ray sources \|Orio M. \| AdSpR \| 38-1469 \| 2006 \| 2006AdSpR..38.1469O \| http://ui.adsabs.harvard.edu/#abs/2006AdSpR..38.1469O The Million Optical - Radio/X-ray Associations (MORX) Catalogue \|Flesch Eric W. \| PASA \| 33-52 \| 2016 \| 2016PASA...33...52F \| http://ui.adsabs.harvard.edu/#abs/2016PASA...33...52F Anisotropy of the galaxy cluster X-ray luminosity-temperature relation \|Migkas Konstantinos Reiprich Thomas H. \| A&A \| 611-50 \| 2018 \| 2018A&A...611A..50M \| http://ui.adsabs.harvard.edu/#abs/2018A&A...611A..50M The XMM Cluster Survey: Present status and latest results \|Viana P. T. P. Mehrtens N. et al. \| AN \| 334-462 \| 2013 \| 2013AN....334..462V \| http://ui.adsabs.harvard.edu/#abs/2013AN....334..462V Testing emergent gravity on galaxy cluster scales \|Tamosiunas Andrius Bacon David et al. \| JCAP \| 5-53 \| 2019 \| 2019JCAP...05..053T \| http://ui.adsabs.harvard.edu/#abs/2019JCAP...05..053T Chandra Follow-up of the SDSS DR8 Redmapper Catalog Using the MATCha Pipeline \|Hollowood Devon L. Jeltema Tesla et al. \| ApJS \| 244-22 \| 2019 \| 2019ApJS..244...22H \| http://ui.adsabs.harvard.edu/#abs/2019ApJS..244...22H Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters \|Palmese A. Annis J. et al. \| MNRAS \| 493-4591 \| 2020 \| 2020MNRAS.493.4591P \| http://ui.adsabs.harvard.edu/#abs/2020MNRAS.493.4591P Classification of 4XMM-DR9 sources by machine learning \|Zhang Yanxia Zhao Yongheng \| MNRAS \| 503-5263 \| 2021 \| 2021MNRAS.503.5263Z \| http://ui.adsabs.harvard.edu/#abs/2021MNRAS.503.5263Z Selection of Compton-thick AGN from a hard photometric sample using XMM-Newton observations \|Mostafa Reham Guainazzi Matteo \| MNRAS \| 525-5080 \| 2023 \| 2023MNRAS.525.5080M \| http://ui.adsabs.harvard.edu/#abs/2023MNRAS.525.5080M The XMM-Newton Line Emission Analysis Program (X-LEAP). I. Emission-line Survey of O VII O VIII and Fe L-shell Transitions \|Pan Zeyang Qu Zhijie et al. \| ApJS \| 271-62 \| 2024 \| 2024ApJS..271...62P \| http://ui.adsabs.harvard.edu/#abs/2024ApJS..271...62P From Active Stars to Black Holes: A Discovery Tool for Galactic X-Ray Sources \|Rodriguez Antonio C. \| PASP \| 136-054201 \| 2024 \| 2024PASP..136e4201R \| http://ui.adsabs.harvard.edu/#abs/2024PASP..136e4201R 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	2001-12-31T17:10:12Z/2002-01-01T10:39:02Z
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.
Creator Contact	https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
Date Published	2003-02-09T00:00:00Z
Last Update	2025-01-27
Keywords	"diagnostical information", "EPIC", "orbital inclination", "intense optical", "epic pn", "epic mos", "short term fluctuations", "soft xray flux", "orbital light curve", "85 hr", "XMM", "accretion disk rim"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Dr Klaus Reinsch, 2003, 'The orbital light curve of the galactic supersoft X-ray source QR And', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-t1ohpqx