Leonardo Trobbiani
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View article: AMICO-WL: an optimal filtering algorithm for galaxy cluster detections with weak lensing
AMICO-WL: an optimal filtering algorithm for galaxy cluster detections with weak lensing Open
Context. The detection of galaxy clusters, the most massive bound structures in the universe, is crucial for cosmological analysis. Weak lensing signals allow us to track the distribution of all (dark and baryonic) matter regardless of its…
View article: AMICO-WL: an optimal filtering algorithm for galaxy cluster detections with weak lensing
AMICO-WL: an optimal filtering algorithm for galaxy cluster detections with weak lensing Open
The detection of galaxy clusters, the most massive bounded structures in the universe, is crucial for cosmological analysis. Weak lensing signals allow us to track the distribution of all (dark and baryonic) matter regardless of its observ…
View article: Correlations between IR Luminosity, Star Formation Rate, and CO Luminosity in the Local Universe
Correlations between IR Luminosity, Star Formation Rate, and CO Luminosity in the Local Universe Open
We exploit the DustPedia sample of galaxies within approximately 40 Mpc, selecting 388 sources, to investigate the correlations between IR luminosity (L$_{\rm IR}$), the star formation rate (SFR), and the CO(1-0) luminosity (L$_{\rm CO}$) …
View article: Correlations between IR Luminosity, Star Formation Rate, and CO Luminosity in the Local Universe
Correlations between IR Luminosity, Star Formation Rate, and CO Luminosity in the Local Universe Open
We exploit the DustPedia sample of galaxies within approximately 40 Mpc, selecting 388 sources, to investigate the correlations between IR luminosity (LIR), the star formation rate (SFR), and the CO(1-0) luminosity (LCO) down to much lower…
View article: ALMA Band 3 Source Counts: A Machine Learning Approach to Contamination Mitigation below 5 Sigma
ALMA Band 3 Source Counts: A Machine Learning Approach to Contamination Mitigation below 5 Sigma Open
We performed differential number counts down to 4.25 sigma using ALMA Band 3 calibrator images, which are known for their high dynamic range and susceptibility to various types of contamination. Estimating the fraction of contaminants is a…