A dataset provided by the European Space Agency

Name 077019
Title Probing the Dark Matter Nature of the 3.5 keV Line with Draco
URL

http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190101
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190201
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190301
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190401
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190501
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190601
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190701
http://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0770190801

DOI 10.5270/esa-9ev2byd
Author Prof Alexey Boyarsky
Description In recent months, much excitement has been generated in the scientific community by the detection of an X-ray line at 3.5keV in galaxy clusters, M31, and the Galactic Center that is consistent with a decay product of light dark matter. It is very difficult to explain the properties of this line across all of these targets consistently with any known atomic transition line or instrumental anomaly. An important check on the nature of this signal may be obtained by observing classical dwarf spheroidals, which are strongly dark matter dominated and contain very little, if any, hot gas. We thus propose a 1.3Msec observation of the Draco dwarf galaxy, which we show to be a sufficient exposure to either detect a dark matter decay line or robustly exclude the dark matter hypothesis.
Publication Deep XMM observations of Draco rule out at the 99 per cent confidence level a dark matter decay origin for the 3.5 keV line . Jeltema, Tesla, Profumo, Stefano, . MNRAS . 458-3592 . 2016 . 2016MNRAS.458.3592J ,
Searching for decaying dark matter in deep XMM-Newton observation of the Draco dwarf spheroidal . Ruchayskiy, Oleg, Boyarsky, Alexey, et all. . MNRAS . 460-1390 . 2016 . 2016MNRAS.460.1390R ,
Probing the nature of dark matter with deep XMM-Newton observations of the dwarf spheroidal galaxies . Boyarsky, A., Ruchayskiy, O., . AN . 338-287 . 2017 . 2017AN....338..287B ,
XMM-Newton study of the supersoft symbiotic system Draco C1 . Saeedi, Sara, Sasaki, Manami, . MNRAS . 473-440 . 2018 . 2018MNRAS.473..440S ,
Scalar field dark matter with spontaneous symmetry breaking and the 3.5 keV line . Cosme, Catarina, Rosa, Joao G., . PhLB . 781-639 . 2018 . 2018PhLB..781..639C ,
Classification of low-luminosity stellar X-ray sources in the field of the Draco dwarf spheroidal galaxy . Saeedi, Sara, Sasaki, Manami, et all. . A&A . 627-128 . 2019 . 2019A&A...627A.128S ,
Geometry of the Draco C1 Symbiotic Binary . Lewis, Hannah M., Anguiano, Borja, et all. . ApJ . 900-43 . 2020 . 2020ApJ...900L..43L ,
Instrument EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage 2015-09-11T16:43:09Z/2015-10-20T07:25:09Z
Version 17.56_20190403_1200
Mission Description The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's 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 Earth's 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 2015-10-26T23:00:00Z
Publisher And Registrant European Space Agency
Credit Guidelines European Space Agency, 2015-10-26T23:00:00Z, 077019, 17.56_20190403_1200. https://doi.org/10.5270/esa-9ev2byd