A new crowded-field light-profile fitting method yields light, kinematics, and stellar mass constraints for 289 cluster members plus the BCG and intra-cluster light in Abell S1063, feeding a future dark matter/baryon separation model.
Cauchy Loss Function: Robustness Under Gaussian and Cauchy Noise
1 Pith paper cite this work. Polarity classification is still indexing.
abstract
In supervised machine learning, the choice of loss function implicitly assumes a particular noise distribution over the data. For example, the frequently used mean squared error (MSE) loss assumes a Gaussian noise distribution. The choice of loss function during training and testing affects the performance of artificial neural networks (ANNs). It is known that MSE may yield substandard performance in the presence of outliers. The Cauchy loss function (CLF) assumes a Cauchy noise distribution, and is therefore potentially better suited for data with outliers. This papers aims to determine the extent of robustness and generalisability of the CLF as compared to MSE. CLF and MSE are assessed on a few handcrafted regression problems, and a real-world regression problem with artificially simulated outliers, in the context of ANN training. CLF yielded results that were either comparable to or better than the results yielded by MSE, with a few notable exceptions.
fields
astro-ph.GA 1years
2025 1verdicts
CONDITIONAL 1representative citing papers
citing papers explorer
-
A comprehensive separation of dark matter and baryonic mass components in galaxy clusters I: Mass constraints from Abell S1063
A new crowded-field light-profile fitting method yields light, kinematics, and stellar mass constraints for 289 cluster members plus the BCG and intra-cluster light in Abell S1063, feeding a future dark matter/baryon separation model.