On the gamma-ray emission from the core of the Sagittarius dwarf galaxy
Abstract
We use Fermi-LAT data to analyse the faint gamma-ray source located at the centre of the Sagittarius (Sgr) dwarf spheroidal galaxy. In the 4FGL-DR3 catalogue, this source is associated with the globular cluster, M54. We investigate the spectral energy distribution and spatial extension of this source, with the goal of testing two hypotheses: (1) the emission is due to millisecond pulsars within M54, or (2) the emission is due to annihilating dark matter from the Sgr halo. For the pulsar interpretation, we consider a two-component model which describes both the lower-energy magnetospheric emission and possible high-energy emission arising from inverse Compton scattering. We find that this source has a point-like morphology at low energies, consistent with magnetospheric emission, and find no evidence for a higher-energy component. For the dark matter interpretation, we find the signal favours a dark matter mass of mχ = 29.6 ± 5.8 GeV and an annihilation cross section of σv = (21. ± 0.59) x 10-26 cm3 s-1 for the $$b\bar{b}$$ channel (or mχ = 8.3 ± 3.8 GeV and σv = (0.90 ± 0.25) x 10-26 cm3 s-1 for the τ+τ- channel), when adopting a J-factor of J = 1019.6 GeV2 cm-5. This parameter space is consistent with gamma-ray constraints from other dwarf galaxies and with dark matter interpretations of the Galactic Centre Gamma-Ray Excess.
- Publication Date:
- Research Org.:
- Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP); National Aeronautics and Space Administration (NASA); European Research Council (ERC); Swedish Research Council (SRC); Swedish National Space Agency; National Science Foundation (NSF); USDOE Laboratory Directed Research and Development (LDRD) Program
- OSTI Identifier:
- 1992933
- Alternate Identifier(s):
- OSTI ID: 1909869
- Report Number(s):
- FERMILAB-PUB-22-890-T; arXiv:2212.08194
Journal ID: ISSN 0035-8711
- Grant/Contract Number:
- de-sc0010813; AC02-07CH11359; SC0010813; 80NSSC22K1577; 742104; 2019–05135; 117/19; AST-1813881
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 524 Journal Issue: 3; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
- Subject:
- 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; 79 ASTRONOMY AND ASTROPHYSICS; astroparticle physics; globular clusters; galaxies; dwarf; dark matter; gamma-rays; general
Citation Formats
Evans, Addy J., Strigari, Louis E., Svenborn, Oskar, Albert, Andrea, Harding, J. Patrick, Hooper, Dan, Linden, Tim, and Pace, Andrew B. On the gamma-ray emission from the core of the Sagittarius dwarf galaxy. United Kingdom: N. p., 2023.
Web. doi:10.1093/mnras/stad2074.
Evans, Addy J., Strigari, Louis E., Svenborn, Oskar, Albert, Andrea, Harding, J. Patrick, Hooper, Dan, Linden, Tim, & Pace, Andrew B. On the gamma-ray emission from the core of the Sagittarius dwarf galaxy. United Kingdom. https://doi.org/10.1093/mnras/stad2074
Evans, Addy J., Strigari, Louis E., Svenborn, Oskar, Albert, Andrea, Harding, J. Patrick, Hooper, Dan, Linden, Tim, and Pace, Andrew B. Thu .
"On the gamma-ray emission from the core of the Sagittarius dwarf galaxy". United Kingdom. https://doi.org/10.1093/mnras/stad2074.
@article{osti_1992933,
title = {On the gamma-ray emission from the core of the Sagittarius dwarf galaxy},
author = {Evans, Addy J. and Strigari, Louis E. and Svenborn, Oskar and Albert, Andrea and Harding, J. Patrick and Hooper, Dan and Linden, Tim and Pace, Andrew B.},
abstractNote = {We use Fermi-LAT data to analyse the faint gamma-ray source located at the centre of the Sagittarius (Sgr) dwarf spheroidal galaxy. In the 4FGL-DR3 catalogue, this source is associated with the globular cluster, M54. We investigate the spectral energy distribution and spatial extension of this source, with the goal of testing two hypotheses: (1) the emission is due to millisecond pulsars within M54, or (2) the emission is due to annihilating dark matter from the Sgr halo. For the pulsar interpretation, we consider a two-component model which describes both the lower-energy magnetospheric emission and possible high-energy emission arising from inverse Compton scattering. We find that this source has a point-like morphology at low energies, consistent with magnetospheric emission, and find no evidence for a higher-energy component. For the dark matter interpretation, we find the signal favours a dark matter mass of mχ = 29.6 ± 5.8 GeV and an annihilation cross section of σv = (21. ± 0.59) x 10-26 cm3 s-1 for the $b\bar{b}$ channel (or mχ = 8.3 ± 3.8 GeV and σv = (0.90 ± 0.25) x 10-26 cm3 s-1 for the τ+τ- channel), when adopting a J-factor of J = 1019.6 GeV2 cm-5. This parameter space is consistent with gamma-ray constraints from other dwarf galaxies and with dark matter interpretations of the Galactic Centre Gamma-Ray Excess.},
doi = {10.1093/mnras/stad2074},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 524,
place = {United Kingdom},
year = {Thu Jul 13 00:00:00 EDT 2023},
month = {Thu Jul 13 00:00:00 EDT 2023}
}
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