Constraints on the presence of a 3.5 keV dark matter emission line from Chandra observations of the Galactic centre

Home

All issues

Volume 590 (June 2016)

A&A, 590 (2016) A71

Full HTML

Highlight

Free Access

Table 3

Emission lines included in the base model.


Emission lines						Additional lines
Energy	Line	Energy	Line	Energy	Line	Energy	Width	Normalisation
[ keV ]		[keV]		[keV]		[keV]	[keV]	[photons cm^-2 s^-1]


2.01	Si xiv	3.47	K xviii	6.39^a	Fe K-α	4.84^a	unresolved	1.04 × 10^-6
2.05^a	Al xiii	3.51	K xviii	6.70^a	Fe xxv	9.01^a	unresolved	5.88 × 10^-6
2.18^a	Si xii	3.62	Ar xvii	6.62^a	Fe xxiv
2.29^a	Si xii	3.68	Ar xvii	6.95^a	Fe xxiv
2.34^a	Si xii	3.71	K xix	7.29^a^b	Fe xxv
2.45^a	Si xv	3.86	Ca xix	7.79^a	Ni xxvii
2.51^a	Si xiv	3.90	Ca xix	7.81^a	Fe xxv
2.62^a	Si xiv	3.93	Ar xviii	7.88^a	Fe xxv
2.88	Si xv	4.10	Ca xx	8.29^a	Fe xxv
3.12	Ar xvii	4.58	Ca xix	8.30^a	Fe xxvi
3.31	Ar xviii	5.69^a^b	Cr xxiii	8.70^a^b	Fe xxvi

Notes. Known astrophysical emission lines included in the model together with additional unknown unresolved lines. Notice none of the additional lines lies in the vicinity of 3.5 keV.

^(a)

Removed in narrow interval model due to no influence on χ².

^(b)

Removed in broad interval model.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.