Introduction to astroML: Machine Learning for Astrophysics
arXiv:1411.5039 · doi:10.1109/CIDU.2012.6382200
Abstract
Astronomy and astrophysics are witnessing dramatic increases in data volume as detectors, telescopes and computers become ever more powerful. During the last decade, sky surveys across the electromagnetic spectrum have collected hundreds of terabytes of astronomical data for hundreds of millions of sources. Over the next decade, the data volume will enter the petabyte domain, and provide accurate measurements for billions of sources. Astronomy and physics students are not traditionally trained to handle such voluminous and complex data sets. In this paper we describe astroML; an initiative, based on Python and scikit-learn, to develop a compendium of machine learning tools designed to address the statistical needs of the next generation of students and astronomical surveys. We introduce astroML and present a number of example applications that are enabled by this package.
8 pages, 6 figures. Proceedings of the 2012 Conference on Intelligent Data Understanding; Proceedings of the Conference on Intelligent Data Understanding, pp. 47-54 (2012)
References in corpus (4)
Cited by in corpus (31)
- Discovering Phases, Phase Transitions and Crossovers through Unsupervised Machine Learning: A critical examination
- Galaxy Zoo: comparing the demographics of spiral arm number and a new method for correcting redshift bias
- ASteCA - Automated Stellar Cluster Analysis
- The ultracompact nature of the black hole candidate X-ray binary 47 Tuc X9
- Galaxy Zoo: Morphological Classifications for 120,000 Galaxies in HST Legacy Imaging
- VDES J2325-5229 a z=2.7 gravitationally lensed quasar discovered using morphology independent supervised machine learning
- Aperture-free star formation rate of SDSS star-forming galaxies
- A Hero's Little Horse: Discovery of a Dissolving Star Cluster in Pegasus
- Galaxy Zoo and SpArcFiRe: Constraints on spiral arm formation mechanisms from spiral arm number and pitch angles
- Dissecting the molecular structure of the Orion B cloud: Insight from Principal Component Analysis
- Radial velocity confirmation of Kepler-91 b. Additional evidence of its planetary nature using the Calar Alto/CAFE instrument
- Inference of Heating Properties from "Hot" Non-flaring Plasmas in Active Region Cores. II. Nanoflare Trains
- Temperature structures in Galactic Center clouds - Direct evidence for gas heating via turbulence
- Star cluster formation history along the minor axis of the Large Magellanic Cloud
- Mapping young stellar populations towards Orion with Gaia DR1
- Precise radial velocities of giant stars IX. HD 59686 Ab: a massive circumstellar planet orbiting a giant star in a ~13.6 au eccentric binary system
- Color-Magnitude Distribution of Face-on Nearby Galaxies in SDSS DR7
- Extended stellar substructure surrounding the Boötes I dwarf spheroidal galaxy
- Serendipitous discovery of RR Lyrae stars in the Leo V ultra-faint galaxy
- Three planets around HD 27894. A close-in pair with a 2:1 period ratio and an eccentric Jovian planet at 5.4 AU
- Extra-tidal structures around the Gaia Sausage candidate globular cluster NGC6779 (M56)
- Relationship between the Line Width of the Atomic and Molecular ISM in M33
- The study of unclassified B[e] stars and candidates in the Galaxy and Magellanic Clouds
- Frequentist model comparison tests of sinusoidal variations in measurements of Newton's gravitational constant
- Carbon Stars in the Satellites and Halo of M31
- Large-scale comparative visualisation of sets of multidimensional data
- The vertical metallicity gradients of mono-age stellar populations in the Milky Way with the RAVE and Gaia data
- Prospects for the detection of high-energy (E>25 GeV) Fermi pulsars with the Cherenkov Telescope Array
- Today a Duo, But Once a Trio? The Double White Dwarf HS 22202146 May Be A Post-Blue Straggler Binary
- Shape Profiles and Orientation Bias for Weak and Strong Lensing Cluster Halos
- Using the Agile software development lifecycle to develop a standalone application for generating colour magnitude diagrams