Morphology-assisted galaxy mass-to-light predictions using deep learning
| Autor: | Samir Salim, Wouter Dobbels, Sébastien Viaene, Maarten Baes, Serge Krier, Gert De Geyter, Stephan Pirson |
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| Rok vydání: | 2019 |
| Předmět: |
Stellar population
Stellar mass MODELS FOS: Physical sciences PHYSICAL-PROPERTIES POPULATION SYNTHESIS Context (language use) Astrophysics::Cosmology and Extragalactic Astrophysics SPECTRAL ENERGY-DISTRIBUTIONS Astrophysics 01 natural sciences Luminosity 0103 physical sciences STAR-FORMING GALAXIES fundamental parameters [galaxies] RATES 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Physics METALLICITY RELATION 010308 nuclear & particles physics Astronomy and Astrophysics Observable CONVOLUTIONAL NEURAL-NETWORKS stellar content [galaxies] Astrophysics - Astrophysics of Galaxies EVOLUTION Redshift Galaxy Physics and Astronomy Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Spectral energy distribution STELLAR MASS |
| Zdroj: | ASTRONOMY & ASTROPHYSICS |
| ISSN: | 1432-0746 0004-6361 |
| DOI: | 10.1051/0004-6361/201834575 |
| Popis: | One of the most important properties of a galaxy is the total stellar mass, or equivalently the stellar mass-to-light ratio (M/L). It is not directly observable, but can be estimated from stellar population synthesis. Currently, a galaxy's M/L is typically estimated from global fluxes. For example, a single global g - i colour correlates well with the stellar M/L. Spectral energy distribution (SED) fitting can make use of all available fluxes and their errors to make a Bayesian estimate of the M/L. We want to investigate the possibility of using morphology information to assist predictions of M/L. Our first goal is to develop and train a method that only requires a g-band image and redshift as input. This will allows us to study the correlation between M/L and morphology. Next, we can also include the i-band flux, and determine if morphology provides additional constraints compared to a method that only uses g- and i-band fluxes. We used a machine learning pipeline that can be split in two steps. First, we detected morphology features with a convolutional neural network. These are then combined with redshift, pixel size and g-band luminosity features in a gradient boosting machine. Our training target was the M/L acquired from the GALEX-SDSS-WISE Legacy Catalog, which uses global SED fitting and contains galaxies with z ~ 0.1. Morphology is a useful attribute when no colour information is available, but can not outperform colour methods on its own. When we combine the morphology features with global g- and i-band luminosities, we find an improved estimate compared to a model which does not make use of morphology. While our method was trained to reproduce global SED fitted M/L, galaxy morphology gives us an important additional constraint when using one or two bands. Our framework can be extended to other problems to make use of morphological information. 17 pages, 8 figures, accepted by A&A |
| Databáze: | OpenAIRE |
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