Modeling of Dark Matter Prompt and Secondary Signatures in Dwarf Galaxies
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866914052949671936 |
|---|---|
| author | Aravinthan, Athithya Dörner, Julien Tjus, Julia Becker Basu, Aritra Bomans, Dominik Das, Samata Taziaux, Sam Elsässer, Dominik Catena, Riccardo |
| author_facet | Aravinthan, Athithya Dörner, Julien Tjus, Julia Becker Basu, Aritra Bomans, Dominik Das, Samata Taziaux, Sam Elsässer, Dominik Catena, Riccardo |
| contents | Dwarf Spheroidal (dSph) galaxies are very promising laboratories for the indirect search for dark matter (DM), due to their low astrophysical background in radio and gamma-ray frequencies. This is convenient when considering Weakly Interacting Dark Matter (WIMP) that can annihilate and produce radio continuum emission. Radio detections of dSph galaxies, however, prove to be difficult and motivate the consideration of transient galaxies that have just recently become quiescent.
For the past several decades, the prompt emission from DM annihilation signatures has been explored through modeling and the setting of limits. In addition to the prompt annihilation signatures from neutrinos, gamma-rays, electrons, positrons, and antimatter, the secondary emission from charged annihilation products undergoing radiative loss processes also contributes to the picture. For instance, synchrotron radiation and inverse Compton scattering of charged products such as electrons and positrons can provide a significant signal. The quantitative modeling of this secondary emission with the astrophysical background is necessary to place stringent constraints on the nature of DM.
In this work, the multi-wavelength secondary spectrum of DM annihilation for a dwarf galaxy is calculated using the open-source code CRPropa 3.2, which enables the self-consistent treatment of the astrophysical background and secondary emissions. We present a systematic comparison of signatures from conventional astrophysical processes to those expected from DM annihilation. The morphological differences between the two scenarios are investigated. Tests of the impact of different magnetic fields, DM masses, and DM profiles will be performed in the next steps. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_19458 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Modeling of Dark Matter Prompt and Secondary Signatures in Dwarf Galaxies Aravinthan, Athithya Dörner, Julien Tjus, Julia Becker Basu, Aritra Bomans, Dominik Das, Samata Taziaux, Sam Elsässer, Dominik Catena, Riccardo High Energy Astrophysical Phenomena High Energy Physics - Theory Dwarf Spheroidal (dSph) galaxies are very promising laboratories for the indirect search for dark matter (DM), due to their low astrophysical background in radio and gamma-ray frequencies. This is convenient when considering Weakly Interacting Dark Matter (WIMP) that can annihilate and produce radio continuum emission. Radio detections of dSph galaxies, however, prove to be difficult and motivate the consideration of transient galaxies that have just recently become quiescent. For the past several decades, the prompt emission from DM annihilation signatures has been explored through modeling and the setting of limits. In addition to the prompt annihilation signatures from neutrinos, gamma-rays, electrons, positrons, and antimatter, the secondary emission from charged annihilation products undergoing radiative loss processes also contributes to the picture. For instance, synchrotron radiation and inverse Compton scattering of charged products such as electrons and positrons can provide a significant signal. The quantitative modeling of this secondary emission with the astrophysical background is necessary to place stringent constraints on the nature of DM. In this work, the multi-wavelength secondary spectrum of DM annihilation for a dwarf galaxy is calculated using the open-source code CRPropa 3.2, which enables the self-consistent treatment of the astrophysical background and secondary emissions. We present a systematic comparison of signatures from conventional astrophysical processes to those expected from DM annihilation. The morphological differences between the two scenarios are investigated. Tests of the impact of different magnetic fields, DM masses, and DM profiles will be performed in the next steps. |
| title | Modeling of Dark Matter Prompt and Secondary Signatures in Dwarf Galaxies |
| topic | High Energy Astrophysical Phenomena High Energy Physics - Theory |
| url | https://arxiv.org/abs/2509.19458 |