Nonparametric Star Formation History Reconstruction with Gaussian Processes. I. Counting Major Episodes of Star Formation

The star formation histories (SFHs) of galaxies contain imprints of the physical processes responsible for regulating star formation during galaxy growth and quenching. We improve the Dense Basis SFH reconstruction method of Iyer & Gawiser, introducing a nonparametric description of the SFH base...

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Bibliographic Details
Published in:The Astrophysical journal 2019-07, Vol.879 (2), p.116
Main Authors: Iyer, Kartheik G., Gawiser, Eric, Faber, Sandra M., Ferguson, Henry C., Kartaltepe, Jeyhan, Koekemoer, Anton M., Pacifici, Camilla, Somerville, Rachel S.
Format: Article
Language:English
Subjects:
Astrophysics
Galactic evolution
Galactic structure
Galaxies
galaxies: evolution
galaxies: fundamental parameters
galaxies: star formation
galaxies: statistics
Gaussian process
Morphology
Nonparametric statistics
Parameter estimation
Parameterization
Physical properties
Quantiles
Reconstruction
Red shift
Spheroids
Star & galaxy formation
Star formation
Stars & galaxies
Stellar mass
techniques: photometric
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Summary:The star formation histories (SFHs) of galaxies contain imprints of the physical processes responsible for regulating star formation during galaxy growth and quenching. We improve the Dense Basis SFH reconstruction method of Iyer & Gawiser, introducing a nonparametric description of the SFH based on the lookback times at which a galaxy assembles certain quantiles of its stellar mass. The method uses Gaussian processes to create smooth SFHs independent of any functional form, with a flexible number of parameters that is adjusted to extract the maximum amount of information from the SEDs being fit. Applying the method to reconstruct the SFHs of 48,791 galaxies with H < 25 at 0.5 < z < 3.0 across the five Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey fields, we study the evolution of galaxies over time. We quantify the fraction of galaxies that show multiple major episodes of star formation, finding that the median time between two peaks of star formation is , where tuniv is the age of the universe at a given redshift and remains roughly constant with stellar mass. Correlating SFHs with morphology allows us to compare the timescales on which the SFHs decline for different morphological classifications, ranging from for galaxies with spiral arms to for spheroids at 0.5 < z < 1.0 with 1010 < M* < 1010.5M . The Gaussian process-based SFH description provides a general approach to reconstruct smooth, flexible, nonparametric SFH posteriors for galaxies that can be incorporated into Bayesian SED fitting codes to minimize the bias in estimating physical parameters due to SFH parameterization.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ab2052