============
Introduction
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*The Cannon* is a data-driven method for determining stellar parameters 
and chemical abundances from stellar spectra in the context of large 
spectroscopic surveys. 
The method uses no physical stellar models, is very fast, 
and achieves comparable accuracy to existing survey pipelines 
using significantly lower SNR spectra; 
it requires only a set of objects observed in common between the surveys. 
Because of these strengths, it has been used to
bring different stellar surveys onto a consistent physical scale,
and even transfer information from one survey to another.

For a more detailed description, see `Ness et al. 2015`_. 

Applications
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(Current as of 8 Feb. 2018)

- Re-analysis of APOGEE DR10: `Ness et al. 2015`_
- Measuring mass (and inferring age) from spectra: `Ness et al. 2016`_
- Chemical tagging: `Hogg et al. 2016`_
- Tying LAMOST to the APOGEE label scale: `Ho et al. 2017a`_
- Detailed element abundances (using regularization): `Casey et al. 2016a`_
- Analysis of GALAH spectra: `Martell et al. 2017`_
- Re-analysis of RAVE using TGAS and K2: `Casey et al. 2016b`_
- Masses and ages for 230,000 LAMOST giants via carbon and nitrogen abundances:
  `Ho et al. 2017b`_
- Galactic Doppelganger (chemical similarity): `Ness et al. 2017`_


.. _Ness et al. 2015: https://arxiv.org/abs/1501.07604
.. _Ness et al. 2016: https://arxiv.org/abs/1511.08204
.. _Hogg et al. 2016: https://arxiv.org/abs/1601.05413
.. _Ho et al. 2017a: https://arxiv.org/abs/1602.00303
.. _Casey et al. 2016a: https://arxiv.org/abs/1603.03040
.. _Martell et al. 2017: https://arxiv.org/abs/1609.02822
.. _Casey et al. 2016b: https://arxiv.org/abs/1609.02914
.. _Ho et al. 2017b: https://arxiv.org/abs/1609.03195
.. _Ness et al. 2017: https://arxiv.org/abs/1701.07829