The effect of kick velocities on the spatial distribution of millisecond pulsars and implications for the Galactic center excess

Observations of the Milky Way by the SPI/INTEGRAL satellite have confirmed the presence of a strong 511 keV gamma ray line emission from the bulge, which requires an intense source of positrons in the galactic center. These observations are hard to account for by conventional astrophysical scenarios, whereas other proposals, such as light DM, face stringent constraints from the diffuse gamma ray background. Here we suggest that light superconducting strings could be the source of the observed 511 keV emission. The associated particle physics, at the ~ 1 TeV scale, is within the reach of planned accelerator experiments, while the distinguishing spatial distribution, proportional to the galactic magnetic field, could be mapped by SPI or by future, more sensitive satellite missions.

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Connecting the new H.E.S.S. diffuse emission at the Galactic Center with the Fermi GeV excess: A combination of millisecond pulsars and heavy dark matter?

Physical Review D ◽

10.1103/physrevd.94.123008 ◽

2016 ◽

Vol 94 (12) ◽

Cited By ~ 4

Author(s):

Thomas Lacroix ◽

Joseph Silk ◽

Emmanuel Moulin ◽

Céline Bœhm

Keyword(s):

Dark Matter ◽

Galactic Center ◽

Diffuse Emission ◽

Millisecond Pulsars

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The 6.4 keV Fe Line and the SiO Emission in the GC

Symposium - International Astronomical Union ◽

10.1017/s0074180900220354 ◽

2001 ◽

Vol 205 ◽

pp. 36-37

Author(s):

J. Martín-Pintado ◽

P. de Vicente ◽

N. Rodríguez-Fernández ◽

A. Fuente ◽

P. Planesas

Keyword(s):

Spatial Distribution ◽

Gas Phase ◽

Molecular Clouds ◽

Galactic Center ◽

X Rays ◽

Refractory Elements

We present a map of the Galactic center in the J=l-0 line of SiO covering the region mapped with the ASCA satellite in the 6.4 keV Fe line. We find a correlation between the spatial distribution of the Fe 6.4 keV line and the SiO emission. The SiO abundance increases by more than a factor of 20 in the regions with strong Fe 6.4 keV line. This indicates that the Fe 6.4 keV line mainly arises from molecular clouds with large gas phase abundance of refractory elements. We discuss the implications of the correlation on the origin of the hard X-rays, and the heating and the chemistry of the molecular clouds in the GC.

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Pulsar Searches at Effelsberg

Symposium - International Astronomical Union ◽

10.1017/s0074180900180799 ◽

2004 ◽

Vol 218 ◽

pp. 133-134 ◽

Cited By ~ 1

Author(s):

B. Klein ◽

M. Kramer ◽

P. Müller ◽

R. Wielebinski

Keyword(s):

Radio Telescope ◽

Galactic Center ◽

Millisecond Pulsars ◽

Highly Dispersed ◽

L Band ◽

Under Construction ◽

5 Ghz ◽

Key Aspects ◽

Pulsar Searches

We report on the progress of our search for highly dispersed pulsars near the Galactic Center at 5 GHz using the 100-m radio telescope in Effelsberg. We also present key aspects of our new survey for millisecond pulsars at 21 cm in parts of the northern sky. This survey will greatly benefit from the L-band multibeam receiver and a new FFT-based backend which are currently under construction at the MPIfR.

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ON DETECTING MILLISECOND PULSARS AT THE GALACTIC CENTER

The Astrophysical Journal ◽

10.1088/0004-637x/805/2/172 ◽

2015 ◽

Vol 805 (2) ◽

pp. 172 ◽

Cited By ~ 27

Author(s):

Jean-Pierre Macquart ◽

Nissim Kanekar

Keyword(s):

Galactic Center ◽

Millisecond Pulsars

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Bulge Globular Clusters

Symposium - International Astronomical Union ◽

10.1017/s0074180900223322 ◽

2002 ◽

Vol 207 ◽

pp. 15-23

Author(s):

B. Barbuy ◽

S. Ortolani ◽

E. Bica

Keyword(s):

Spatial Distribution ◽

Globular Clusters ◽

Galactic Center ◽

Bulge Formation

The properties of the globular clusters located within 20° × 20° of the Galactic Center are discussed. In particular their spatial distribution, metallicities and ages are presented and discussed in the context of different scenarios of bulge formation.

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