The eROSITA Final Equatorial-Depth Survey (eFEDS): A machine learning approach to inferring galaxy cluster masses from eROSITA X-ray images

We have developed a neural network-based pipeline to estimate masses of galaxy clusters with a known redshift directly from photon information in X-rays. Our neural networks were trained using supervised learning on simulations of eROSITA observations, focusing on the Final Equatorial Depth Survey (...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2024-02, Vol.682, p.A132
Main Authors: Krippendorf, Sven, Baron Perez, Nicolas, Bulbul, Esra, Kara, Melih, Seppi, Riccardo, Comparat, Johan, Artis, Emmanuel, Bahar, Yunus Emre, Garrel, Christian, Ghirardini, Vittorio, Kluge, Matthias, Liu, Ang, Ramos-Ceja, Miriam E., Sanders, Jeremy, Zhang, Xiaoyuan, Brüggen, Marcus, Grandis, Sebastian, Weller, Jochen
Format: Article
Language:English
Subjects:
Artificial neural networks
Galactic clusters
Luminosity
Machine learning
Neural networks
Point sources
Red shift
Simulation
Sky surveys (astronomy)
Supervised learning
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Summary:We have developed a neural network-based pipeline to estimate masses of galaxy clusters with a known redshift directly from photon information in X-rays. Our neural networks were trained using supervised learning on simulations of eROSITA observations, focusing on the Final Equatorial Depth Survey (eFEDS). We used convolutional neural networks that have been modified to include additional information on the cluster, in particular, its redshift. In contrast to existing works, we utilized simulations that include background and point sources to develop a tool that is directly applicable to observational eROSITA data for an extended mass range – from group size halos to massive clusters with masses in between 10 13 M ⊙ < M < 10 15 M ⊙ . Using this method, we are able to provide, for the first time, neural network mass estimations for the observed eFEDS cluster sample from Spectrum-Roentgen-Gamma/eROSITA observations and we find a consistent performance with weak-lensing calibrated masses. In this measurement, we did not use weak-lensing information and we only used previous cluster mass information, which was used to calibrate the cluster properties in the simulations. When compared to the simulated data, we observe a reduced scatter with respect to luminosity and count rate based scaling relations. We also comment on the application for other upcoming eROSITA All-Sky Survey observations.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/202346826