Merge branch 'master' of github.com:bmorris3/shocksgo

README.rst

@@ -1,50 +1,19 @@
-Exposure time calculator for APO/ARCES
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+shocksgo: Simple Harmonic Oscillator celerite kernels for stellar granulation and oscillations
+----------------------------------------------------------------------------------------------
 
-.. image:: https://travis-ci.org/bmorris3/arcesetc.svg?branch=master
-    :target: https://travis-ci.org/bmorris3/arcesetc
+.. image:: https://travis-ci.org/bmorris3/shocksgo.svg?branch=master
+    :target: https://travis-ci.org/bmorris3/shocksgo
 
-.. image:: https://readthedocs.org/projects/arcesetc/badge/?version=latest
-    :target: https://arcesetc.readthedocs.io/en/latest/?badge=latest
+.. image:: https://readthedocs.org/projects/shocksgo/badge/?version=latest
+    :target: https://shocksgo.readthedocs.io/en/latest/?badge=latest
     :alt: Documentation Status
 
-.. image:: http://img.shields.io/pypi/v/arcesetc.svg?text=version
-    :target: https://pypi.python.org/pypi/arcesetc/
-    :alt: Latest release
-
 .. image:: http://img.shields.io/badge/powered%20by-AstroPy-orange.svg?style=flat
     :target: http://www.astropy.org
     :alt: Powered by Astropy Badge
 
-.. image:: https://img.shields.io/badge/powered%20by-aesop-orange.svg?style=flat
-    :target: https://github.com/bmorris3/aesop
-    :alt: Powered by aesop badge
-
-Calculate S/N and exposure times for
-stellar spectroscopy with the `ARC Echelle Spectrograph (ARCES)
-<https://www.apo.nmsu.edu/arc35m/Instruments/ARCES/>`_ on the
-`ARC 3.5 m Telescope <https://www.apo.nmsu.edu/arc35m/>`_ at
-`Apache Point Observatory <https://www.apo.nmsu.edu>`_.
-
-The ARC Echelle Spectroscopic (ARCES) Exposure Time Calculator, or ``arcesetc``,
-is a simple exposure time calculator for the ARCES instrument on the
-Astrophysical Research Consortium (ARC) 3.5 m Telescope at Apache Point
-Observatory for stellar spectroscopy. Users can supply ``arcesetc`` functions
-with the spectral type of their target star, the V band magnitude, and either:
-the desired exposure time in order to determine the counts and signal-to-noise
-ratio as a function of wavelength; or the desired signal-to-noise ratio at a
-given wavelength to determine the required exposure time.
-
-We estimate the count rates for stars as a function of wavelength by fitting
-15th-order polynomials to each spectral order of real observations of a star of
-each spectral type. These polynomial coefficients and some wavelength metadata
-are stored in an HDF5 archive for compactness and easy of reconstruction. Then
-upon calling ``arcesetc``, the archive is opened and the spectral order closest
-to the wavelength of interest is reconstructed from the polynomial
-coefficients, for a star of the closest available spectral type to the one
-requested. 
+Generate light curves of the Sun and stars accounting for the effects of granulation, supergranulation and p-mode oscillations. 
 
-For more information, `read the docs <https://arcesetc.readthedocs.io/>`_.
 
 License
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