SciPost Submission Page
Production and propagation of secondary antideuteron in the Galaxy
by Luis Fernando Galicia Cruztitla and Diego Mauricio Gomez Coral
This is not the latest submitted version.
Submission summary
| Authors (as registered SciPost users): | Luis Fernando Galicia Cruztitla |
| Submission information | |
|---|---|
| Preprint Link: | scipost_202411_00001v1 (pdf) |
| Date submitted: | 2024-11-01 02:15 |
| Submitted by: | Galicia Cruztitla, Luis Fernando |
| Submitted to: | SciPost Physics Proceedings |
| Proceedings issue: | 22nd International Symposium on Very High Energy Cosmic Ray Interactions (ISVHECRI 2024) |
| Ontological classification | |
|---|---|
| Academic field: | Physics |
| Specialties: |
|
| Approach: | Phenomenological |
Abstract
This work reviews the current state of the antideuteron ($\bar{d}$) production cross-sections in cosmic ray interactions and its uncertainties, considering the coalescence model and measurements in accelerator experiments. These cross-sections have been included in a simulation of cosmic rays propagation in the Galaxy using GALPROP v.57, with updated parameters of the diffusive reacceleration model. An estimation of the expected antideuteron flux at Earth is presented.
Current status:
Reports on this Submission
Report
The article reviews the current state of the antideuteron production cross-sections and their uncertainties from the measurements at accelerators. An estimate of the expected cosmic-ray antideuteron flux at Earth using GALPROP modelling is presented by the authors. Though the paper is clear in the assumptions and conclusions, I have two important comments which I suggest that authors address before the publication:
1. The earlier calculations of the antideuteron flux at Earth should be properly acknowledged. For instance, the following articles arrive to very similar conclusions:
K. Blum, K. C. Yu. Ng, R. Sato, and M. Takimoto, Phys. Rev. D 96, 103021 (2017)
M. Korsmeier, F. Donato, and N. Fornengo, Phys. Rev. D 97, 103011 (2018)
…
2. In Figure 2 the authors refer to the AMS-02 sensitivity from Ref. [20], which in turn refers to the ICRC-2008 presentation describing AMS in superconducting magnet configuration with 3 years of data collection time. The AMS-02 Experiment with permanent magnet is collecting data for over 13 years. The current status and life-time projections of the AMS-02 sensitivity to antideuterons were presented at ICRC-2023 (a copy of this presentation with relevant slides is attached for reference - in particular, see p.15):
Z. Weng, presentation at the AMS special session at International Cosmic Ray Conference Jul. 28, 2023, Nagoya, Japan.
Recommendation
Ask for major revision
Author: Luis Fernando Galicia Cruztitla on 2025-01-24 [id 5143]
(in reply to Report 1 on 2024-12-11)Reply to report on Scipost_202411_00001v1 Title: Production and propagation of secondary antideuteron in the Galaxy Authors: Luis Fernando Galicia Cruztitla and Diego Mauricio Gómez Coral
Dear Editor and Referee
We greatly appreciate your valuable suggestions on our paper, which have helped to improve it. Your comments allowed us to clarify our conclusions and to include important works from other authors. Below we present the referee’s comments followed by our answers and modifications to the manuscript. We hope that this revised version is suitable for publication.
The authors.
Comments referee
Answer: The following line was added in section 5 (Conclusions): "Previous calculations are consistent with this result [21, 22]", where references [21] and [22] are those suggested by the referee.
Answer: Considering the presentation provided by the referee, a comparison of the antideuteron flux estimation to the current AMS-02 sensitivity with a permanent magnet for 11 years of operation and also to the projected AMS-02 sensitivity for 2030 was performed. In the first case, the estimated flux remained below the AMS-02 lower limit which does not change our previous conclusion. To clarify these differences in sensitivity limits the following lines were included: In section 4.2: “... AMS-02 \bar{d} sensitivity [19] (green lines), considering the projection with a superconducting-magnet configuration.” In section 5.0: “A similar result is obtained when an AMS-02 sensitivity, with a permanent-magnet configuration for 11 years, is considered [20].”
In the second case, the projected AMS-02 sensitivity for 2030 is mentioned in the text, and an additional observation regarding this value compared to the predicted secondary antideuteron flux was added: “Interestingly, a recent AMS-02 sensitivity projection for 2030 with a planned detector upgrade is close to the maximum of our secondary \bar{d} flux estimation [20] (Fig. 2), suggesting that AMS-02 would be practically background-free for possible antideuteron observation coming from dark matter or new astrophysical production mechanisms.”
As you can see we have refrained from showing these new sensitivities in Fig.2 and we have kept this figure as it was because the AMS collaboration explicitly mentioned in the presentation this information is not for publication.