A dataset provided by the European Space Agency

Name: Search for Iron Line Pulsations in Cen X-3
Published: 2009-02-08T00:00:00Z

Proposal ID	040055
Title	Search for Iron Line Pulsations in Cen X-3
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0400550201 https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0400550301
DOI	https://doi.org/10.5270/esa-ha2aegq
Principal Investigator, PI	Dr Timothy Kallman
Abstract	The iron K line provides hints about accretion flows in accreting pulsars viathe line shape, strength and variability behavior. In Cen X-3 line pulsationshave been detected, and the fluorescent line must originate close to the pulsar.But the picture is incomplete owing to the absence of observations which combinesufficient collecting area and spectral resolution. We propose a single 70 ksecobservation at a favorable range of orbital phase in order to confirm the likelysite of the fluorescent line, to better understand the geometry of thereprocessing gas, to better study the gas responsible for absorption at energiesabove the iron line, and to study the average properties of the stellar wind.
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 An All-Sky Atlas of Radio/X-ray Associations \|Flesch, E., \| PASA \| 27-283 \| 2010 \| 2010PASA...27..283F \| http://ui.adsabs.harvard.edu/#abs/2010PASA...27..283F 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 Classification of X-Ray Sources in the XMM-Newton Serendipitous Source Catalog \|Lin, Dacheng, Webb, Natalie A., \| ApJ \| 756-27 \| 2012 \| 2012ApJ...756...27L \| http://ui.adsabs.harvard.edu/#abs/2012ApJ...756...27L The diversity of quasars unified by accretion and orientation \|Shen, Yue, Ho, Luis C., \| Natur \| 513-210 \| 2014 \| 2014Natur.513..210S \| http://ui.adsabs.harvard.edu/#abs/2014Natur.513..210S Sunyaev-Zel.dovich 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 Revealing the broad iron Kalpha line in Cygnus X-1 through simultaneous XMM-Newton, RXTE, and INTEGRAL observations \|Duro, Refiz, Dauser, Thomas, et al. \| A&A \| 589-14 \| 2016 \| 2016A&A...589A..14D \| http://ui.adsabs.harvard.edu/#abs/2016A&A...589A..14D 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 X-ray variability of the HMXB Cen X-3: evidence for inhomogeneous accretion flows \|Sanjurjo-Ferr\\u00edn, G., Torrej\\u00f3n, J. M., et al. \| MNRAS \| 501-5892 \| 2021 \| 2021MNRAS.501.5892S \| http://ui.adsabs.harvard.edu/#abs/2021MNRAS.501.5892S 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 Common patterns in pulse profiles of high-mass X-ray binaries \|Alonso-Hern\\u00e1ndez, J., F\\u00fcrst, F., et al. \| A&A \| 662-62 \| 2022 \| 2022A&A...662A..62A \| http://ui.adsabs.harvard.edu/#abs/2022A&A...662A..62A Energy dependence of quasi-periodic oscillations in accreting X-ray pulsars \|Manikantan, Hemanth, Paul, Biswajit, et al. \| MNRAS \| 531-530 \| 2024 \| 2024MNRAS.531..530M \| http://ui.adsabs.harvard.edu/#abs/2024MNRAS.531..530M 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, RGS1, RGS2
Temporal Coverage	2006-06-12T22:07:40Z/2006-06-13T22:21:24Z
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	2009-02-08T00:00:00Z
Keywords	"accretion flows", "orbital phase", "iron line", "average properties", "stellar wind", "line shape", "incomplete owing", "fluorescent line", "reprocessing gas", "iron line pulsations", "line pulsations", "spectral resolution", "cen x", "favorable range", "accreting pulsars via"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Dr Timothy Kallman, 2009, 'Search for Iron Line Pulsations in Cen X-3', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-ha2aegq