# Acknowledging brutus¶

Only use lower case letters when mentioning brutus, and always include the release number, e.g.:

brutus 0.3.1

brutus will be described in detail in

Vogt et al., in prep.

If you find brutus useful for your research, please cite this reference accordingly.

brutus uses several packages that should also be acknowledged in their own right. The following Tex-formatted acknowledgment is one way to do so:

This research has made use of \textsc{brutus}, a Python module to process data cubes
from integral field spectrographs hosted at \url{http://fpavogt.github.io/brutus/}.
\textsc{brutus} relies on \textsc{statsmodel} (Seabold & Perktold 2010),
\textsc{ppxf} (Cappellari & Emsellem 2004), \textsc{fit_kinematic_pa} as described in
Appendix C of Krajnovic et al. (2006), \textsc{matplotlib} (Hunter 2007),
\textsc{astropy}, a community-developed core Python package for Astronomy
(Astropy Collaboration et al., 2013), \textsc{photutils}, an affiliated package of
\textsc{astropy} for photometry, \textsc{aplpy}, an open-source plotting package for
Python hosted at \url{http://aplpy.github.com}, \textsc{montage}, funded by the
National Science Foundation under Grant Number ACI-1440620 and previously funded by
the National Aeronautics and Space Administration’s Earth Science Technology Office,
Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between
NASA and the California Institute of Technology, and \textsc{mpfit}, a Python script
that uses the Levenberg-Marquardt technique (Moré 1978) to solve least-squares
problems, based on an original Fortran code part of the \textsc{minpack}-1 package.


Finally, you also ought to cite the following works, depending on your use of brutus:

1. Cleveland(1979);

the reference for the Locally Weighted Scatterplot Smoothing (LOWESS) algorithm used by brutus (via statsmodels) to fit the continuum.

2. The default SSP models shipped with brutus are:

Stellar population synthesis model predictions using the MILES stellar libraries
(Sánchez-Blázquez et al. 2006, Falcón-Barroso et al. 2011) at FWHM=2.5 Å, based on
the code presented in Vazdekis et al. (2010), using a Kroupa revised IMF with
slope 1.3 (Kroupa 2001), Padova +00  (Girardi et al. 2000) isochrones, metallicities
ranging from -2.32 to +0.22, and ages of 0.0631 to 17.7828 Gyr.

3. The reddening laws:

Either the Cardelli, Clayton & Mathis (1989) law, the Calzetti et al. (2000) law or the theoretical model of a turbulent dust screen of Fischera & Dopita (2005) [default] for the extragalactic attenuation corrections, and the Fitzpatrick (1999) law [default] for the galactic extinction.

If you use the extinction values $$A_V$$ and $$A_B$$ from the NASA Extragalactic Database (NED) to correct for the Galactic extinction [default], then to be thorough, you should mention that:

The Galactic extinction is derived using NED from the Schlafly & Finkbeiner
(2011) recalibration of the Schlegel, Finkbeiner & Davis (1998) infrared-based
dust map. The map is based on dust emission from COBE/DIRBE and IRAS/ISSA;
the recalibration assumes a Fitzpatrick (1999) reddening law with Rv = 3.1 and
different source spectrum than Schlegel, Finkbeiner & Davis (1998).


and you also ought to acknowledge NED itself:

This research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space Administration.

References: