SNCosmo

SNCosmo is a Python library for supernova cosmology analysis. It aims to make such analysis both as flexible and clear as possible.

Installation

SNCosmo works on Python 2.7 and Python 3.4+ and requires the following Python packages:

• numpy
• scipy
• astropy
• extinction

Install using conda (recommended)

If you are using Anaconda or the conda package manager, you can install SNCosmo from the astropy channel:

conda install -c astropy sncosmo

The release of the conda version may lag behind the pip release, so you may want to check the available conda version. You can do this at the link above, or by running conda search -c astropy sncosmo.

Install using pip

Using pip:

pip install --no-deps extinction sncosmo

Note

The --no-deps flag is optional, but highly recommended if you already have numpy, scipy and astropy installed, since otherwise pip will sometimes try to “help” you by upgrading your Numpy installation, which may not always be desired.

Note

If you get a PermissionError this means that you do not have the required administrative access to install new packages to your Python installation. In this case you may consider using the --user option to install the package into your home directory. You can read more about how to do this in the pip documentation.

Do not install sncosmo or other third-party packages using sudo unless you are fully aware of the risks.

Note

You will need a C compiler (e.g. gcc or clang) to be installed for the installation to succeed.

Install latest development version

SNCosmo is being developed on github. To get the latest development version using git:

git clone git://github.com/sncosmo/sncosmo.git
cd sncosmo

then:

./setup.py install

As with the pip install instructions, you may want to use either setup.py install --user or setup.py develop to alter where the package is installed.

Optional dependencies

Several additional packages are recommended for enabling optional functionality in SNCosmo.

• matplotlib for plotting functions.
• iminuit for light curve fitting using the Minuit minimizer in sncosmo.fit_lc.
• emcee for MCMC light curve parameter estimation in sncosmo.mcmc_lc.
• nestle for nested sampling light curve parameter estimation in sncosmo.nest_lc.

iminuit, emcee and nestle can be installed using pip.

The corner package is also recommended for plotting results from the samplers sncosmo.mcmc_lc and sncosmo.nest_lc, but is not used by any part of sncosmo.

Supernova Models

Getting Started

Create a model using the built-in “source” named 'hsiao':

>>> import sncosmo
>>> model = sncosmo.Model(source='hsiao')

Set the redshift, time-of-zero-phase and the amplitude:

>>> model.set(z=0.5, t0=55000., amplitude=1.e-10)

Generate synthetic photometry through an observer-frame bandpass:

>>> model.bandmag('desr', 'ab', [54990., 55000., 55020.])
array([ 24.82381795,  24.41496701,  25.2950865 ])

Equivalent values in photons / s / cm^2:

>>> model.bandflux('desr', [54990., 55000., 55020.])
array([  7.22413301e-05,   1.05275209e-04,   4.68034980e-05])

Equivalent values scaled so that 1 is equivalent to an AB magnitude of 25:

>>> model.bandflux('desr', [54990., 55000., 55020.], zp=25., zpsys='ab')
array([ 1.17617737,  1.71400939,  0.7620183 ])

Generate an observer-frame spectrum at a given time and wavelengths (in ergs/s/cm^2/Angstrom):

>>> model.flux(54990., [4000., 4100., 4200.])
array([  4.31210900e-20,   7.46619962e-20,   1.42182787e-19])

Creating a model using a built-in source

A Model in sncosmo consists of

• One “source” A model of the spectral evolution of the source (e.g., a supernova).
• Zero or more “propagation effects” Models of how intervening structures (e.g., host galaxy dust, milky way dust) affect the spectrum.

In the above example, we created a model with no propagation effects, using one of the built-in Source instances that sncosmo knows about: 'hsiao'. See the full List of Built-in Sources that sncosmo knows about.

Note

In fact, the data for “built-in” sources are hosted remotely, downloaded as needed, and cached locally. So the first time you load a given model, you need to be connected to the internet. You will see a progress bar as the data are downloaded. By default, SNCosmo will use a subdirectory of the AstroPy cache directory for this purpose, e.g., $HOME/.astropy/cache/sncosmo, but this can be changed by setting the data_dir configuration parameter in $HOME/.astropy/config/sncosmo.cfg. See Directory Configuration for more information.

Some built-in source models have multiple versions, which can be explicitly retrieved using the get_source function:

>>> source = sncosmo.get_source('hsiao', version='2.0')
>>> model = sncosmo.Model(source=source)

Model parameters

Each model has a set of parameter names and values:

>>> model.param_names
['z', 't0', 'amplitude']
>>> model.parameters
array([ 0.,  0.,  1.])

These can also be retrieved as:

>>> model.get('z')
0.0
>>> model['z']
0.0

Parameter values can be set by any of the following methods:

>>> model.parameters[0] = 0.5
>>> model.parameters = [0.5, 0., 1.]  # set the entire array
>>> model['z'] = 0.5
>>> model.set(z=0.5)
>>> model.set(z=0.5, amplitude=2.0)  # Can specify multiple parameters
>>> model.update({'z': 0.5, 'amplitude': 2.0})

What do these parameters mean? The first two, z and t0 are common to all Model instances:

• z is the redshift of the source.
• t0 is the observer-frame time corresponding to the source’s phase=0.

Note that in some sources phase=0 might be at explosion while others might be at max: the definition of phase is arbitrary. However, observed time is always related to phase via time = t0 + phase * (1 + z)

The next, amplitude, is specific to the particular type of source. In this case, the source is a simple spectral timeseries that can only be scaled up and down. Other sources could have other parameters that affect the shape of the spectrum at each phase.

For a given model, you can set the amplitude (or x0 in case you are using a SALT model) according to a desired absolute magnitude in a specific band by using the method set_source_peakabsmag(). Note that the redshift z affects your result. Therefore, you could specify:

>>> model.set(z=1.6)
>>> model.set_source_peakabsmag(-19.0, 'bessellb', 'ab')

Specifically, for SALT models, it is recommended to call set_source_peakabsmag() after setting the other model parameters, such as x1 and c. It probably won’t make a difference if you are using the 'bessellb' bandpass, but if you were setting the absolute magnitude in another band, it would make a small difference.

The reason for this peculiarity is that “absolute magnitude” is not a parameter in the SALT2 model, per se. The parameters are x0, x1, c, t0, and z. x0 is a simple multiplicative scaling factor on the whole spectral timeseries. The set_source_peakabsmag() method is a convenience for setting x0 such that the integrated flux through a given bandpass is as desired. Since the integrated flux depends on the spectral shape, it will depend on x1 and c.

Creating a model with a source and effect(s)

Let’s create a slightly more complex model. Again we will use the Hsiao spectral time series as a source, but this time we will add host galaxy dust.

>>> dust = sncosmo.CCM89Dust()
>>> model = sncosmo.Model(source='hsiao',
...                       effects=[dust],
...                       effect_names=['host'],
...                       effect_frames=['rest'])

The model now has additional parameters that describe the dust, hostebv and hostr_v:

>>> model.param_names
['z', 't0', 'amplitude', 'hostebv', 'hostr_v']
>>> model.parameters
array([ 0. ,  0. ,  1. ,  0. ,  3.1])

These are the parameters of the CCM89Dust instance we created:

>>> dust.param_names
['ebv', 'r_v']

In the model, the parameter names are prefixed with the name of the effect (host).

At any time you can print the model to get a nicely formatted string representation of its components and current parameter values:

>>> print(model)
<Model at 0x...>
source:
  class      : TimeSeriesSource
  name       : hsiao
  version    : 3.0
  phases     : [-20, .., 85] days (22 points)
  wavelengths: [1000, .., 25000] Angstroms (481 points)
effect (name='host' frame='rest'):
  class           : CCM89Dust
  wavelength range: [1250, 33333] Angstroms
parameters:
  z         = 0.0
  t0        = 0.0
  amplitude = 1.0
  hostebv   = 0.0
  hostr_v   = 3.1000000000000001

Also, str(model) will return this string rather than printing it.

Adding Milky Way dust

Dust in the Milky Way will affect the shape of an observed supernova spectrum. It is important to take this into account in our model when fitting the model to observed data. As with host galaxy dust treated above, we can model Milky Way dust as a “propagation effect”. The only difference is that Milky Way dust is in the observer frame rather than the supernova rest frame. Here, we create a model with dust in both the SN rest frame and the observer frame:

>>> dust = sncosmo.CCM89Dust()
>>> model = sncosmo.Model(source='hsiao',
...                       effects=[dust, dust],
...                       effect_names=['host', 'mw'],
...                       effect_frames=['rest', 'obs'])

We can see that the model includes four extra parameters (two describing the host galaxy dust and two describing the milky way dust):

>>> model.param_names
['z', 't0', 'amplitude', 'hostebv', 'hostr_v', 'mwebv', 'mwr_v']
>>> model.parameters  # default values
array([ 0. ,  0. ,  1. ,  0. ,  3.1,  0. ,  3.1])

The host galaxy dust parameters are prefixed with 'host' and the Milky Way dust parameters are prefixed with 'mw'. These are just the names we supplied when constructing the model. The effect names have no significance beyond this. The effect frames, on the other hand, are significant. The only allowed values are 'rest' (rest frame) and 'obs' (observer frame).

A typical use pattern is to get an estimate of the amount of Milky Way dust at the location of the supernova from a dust map, and then to fix that amount of dust in the model. The following example illustrates how to do this using the Schlegel, Finkbeiner and Davis (1998) dust map with the sfdmap package. First, load the dust map (do this only once):

>>> import sfdmap

>>> dustmap = sfdmap.SFDMap("/path/to/dust/maps")

Now, for each SN you wish to fit, get the amount of dust at the SN location and set the mwebv model parameter appropriately. For example, if the SN is located at RA=42.8 degrees, Dec=0 degrees:

>>> ebv = dustmap.ebv(42.8, 0.0)

>>> model.set(mwebv=ebv)

>>> # proceed with fitting the other model parameters to the data.

Note that we wish to fix the mwebv model parameter rather than fitting it to the data like the other parameters: We’re supposing that this value is perfectly known from the dust map. Therefore, when using a function such as fit_lc to fit the parameters, be sure not to include 'mwebv' in the list of parameters to vary.

Model spectrum

To retrieve a spectrum (in ergs / s / cm^2 / Angstrom) at a given observer-frame time and set of wavelengths:

>>> wave = np.array([3000., 3500., 4000., 4500., 5000., 5500.])
>>> model.flux(-5., wave)
array([  5.29779465e-09,   7.77702880e-09,   7.13309678e-09,
         5.68369041e-09,   3.06860759e-09,   2.59024291e-09])

We can supply a list or array of times and get a 2-d array back, representing the spectrum at each time:

>>> model.flux([-5., 2.], wave)
array([[  5.29779465e-09,   7.77702880e-09,   7.13309678e-09,
          5.68369041e-09,   3.06860759e-09,   2.59024291e-09],
       [  2.88166481e-09,   6.15186858e-09,   7.87880448e-09,
          6.93919846e-09,   3.59077596e-09,   3.27623932e-09]])

Changing the model parameters changes the results:

>>> model.parameters
array([0., 0., 1., 0., 3.1])
>>> model.flux(-5., [4000., 4500.])
array([  7.13309678e-09,   5.68369041e-09])
>>> model.set(amplitude=2., hostebv=0.1)
>>> model.flux(-5., [4000., 4500.])
array([  9.39081327e-09,   7.86972003e-09])

Synthetic photometry

To integrate the spectrum through a bandpass, use the bandflux method:

>>> model.bandflux('sdssi', -5.)
180213.72886169454

Here we are using the SDSS I band, at time -5. days. The return value is in photons / s / cm^2. It is also possible to supply multiple times or bands:

>>> model.bandflux('sdssi', [-5., 2.])
array([ 180213.72886169,  176662.68287381])
>>> model.bandflux(['sdssi', 'sdssz'], [-5., -5.])
array([ 180213.72886169,   27697.76705621])

Instead of returning flux in photons / s / cm^2, the flux can be normalized to a desired zeropoint by specifying the zp and zpsys keywords, which can also be scalars, lists, or arrays.

>>> model.bandflux(['sdssi', 'sdssz'], [-5., -5.], zp=25., zpsys='ab')
array([  5.01036850e+09,   4.74414435e+09])

Instead of flux, magnitude can be returned. It works very similarly to flux:

>>> model.bandmag('sdssi', 'ab', [0., 1.])
array([ 22.6255077 ,  22.62566363])
>>> model.bandmag('sdssi', 'vega', [0., 1.])
array([ 22.26843273,  22.26858865])

We have been specifying the bandpasses as strings ('sdssi' and 'sdssz'). This works because these bandpasses are in the sncosmo “registry”. However, this is merely a convenience. In place of strings, we could have specified the actual Bandpass objects to which the strings correspond. See Bandpasses for more on how to directly create Bandpass objects.

The magnitude systems work similarly to bandpasses: 'ab' and 'vega' refer to built-in MagSystem objects, but you can also directly supply custom MagSystem objects. See Magnitude Systems for details.

Initializing Sources directly

You can initialize a source directly from your own template rather than using the built-in source templates.

Initializing a TimeSeriesSource

These sources are created directly from numpy arrays. Below, we build a very simple model, of a source with a flat spectrum at all times, rising from phase -50 to 0, then declining from phase 0 to +50.

>>> import numpy as np
>>> phase = np.linspace(-50., 50., 11)
>>> disp = np.linspace(3000., 8000., 6)
>>> flux = np.repeat(np.array([[0.], [1.], [2.], [3.], [4.], [5.],
...                            [4.], [3.], [2.], [1.], [0.]]),
...                  6, axis=1)
>>> source = sncosmo.TimeSeriesSource(phase, disp, flux)

Typically, you would then include this source in a Model:

>>> model = sncosmo.Model(source)

Initializing a SALT2Source

The SALT2 model is initialized directly from data files representing the model. You can initialize it by giving it a path to a directory containing the files.

>>> source = sncosmo.SALT2Source(modeldir='/path/to/dir')

By default, the initializer looks for files with names like 'salt2_template_0.dat', but this behavior can be altered with keyword parameters:

>>> source = sncosmo.SALT2Source(modeldir='/path/to/dir',
...                              m0file='mytemplate0file.dat')

See SALT2Source for more details.

Bandpasses

Constructing a Bandpass

Bandpass objects represent the transmission fraction of an astronomical filter as a function of dispersion (photon wavelength, frequency or energy). They are basically simple containers for arrays of these values, with a couple special features. To get a bandpass that is in the registry (built-in):

>>> import sncosmo
>>> band = sncosmo.get_bandpass('sdssi')
>>> band
<Bandpass 'sdssi' at 0x...>

To create a Bandpass directly, you can supply arrays of wavelength and transmission values:

>>> wavelength = [4000., 5000.]
>>> transmission = [1., 1.]
>>> sncosmo.Bandpass(wavelength, transmission, name='tophatg')
<Bandpass 'tophatg' at 0x...>

By default, the first argument is assumed to be wavelength in Angstroms. To specify a different dispersion unit, use a unit from the astropy.units package:

>>> import astropy.units as u
>>> wavelength = [400., 500.]
>>> transmission = [1., 1.]
>>> Bandpass(wavelength, transmission, wave_unit=u.nm)
<Bandpass 'tophatg' at 0x...>

Using a Bandpass

A Bandpass acts like a continuous 1-d function, returning the transmission at supplied wavelengths (always in Angstroms):

>>> band([4100., 4250., 4300.])
array([ 0.,  1.,  1.])

Note that the transmission is zero outside the defined wavelength range. Linear interpolation is used between the defined wavelengths.

Bnadpasses have a few other useful properties. You can get the range of wavelengths where the transmission is non-zero:

>>> band.minwave(), band.maxwave()
(4000.0, 5000.0)

Or the transmission-weighted effective wavelength:

>>> band.wave_eff
4500.0

Or the name:

>>> band.name
'tophatg'

Adding Bandpasses to the Registry

You can create your own bandpasses and use them like built-ins by adding them to the registry. Suppose we want to register the ‘tophatg’ bandpass we created:

>>> sncosmo.register(band, 'tophatg')

Or if band.name has been set:

>>> sncosmo.register(band)  # registers band under band.name

After doing this, we can get the bandpass object by doing

>>> band = sncosmo.get_bandpass('tophatg')

Also, we can pass the string 'tophatg' to any function that takes a Bandpass object. This means that you can create and register bandpasses at the top of a script, then just keep track of string identifiers throughout the rest of the script.

Magnitude Systems

SNCosmo has facilities for converting synthetic model photometry to magnitudes in a variety of magnitude systems (or equivalently, scaling fluxes to a given zeropoint in a given magnitude system). For example, in the following code snippet, the string 'ab' specifies that we want magnitudes on the AB magnitude system:

>>> model.bandmag('desr', 'ab', [54990., 55000., 55020.])

The string 'ab' here refers to a built-in magnitude system ('vega' is another option). Behind the scenes magnitude systems are represented with MagSystem objects. As with Bandpass objects, most places in SNCosmo that require a magnitude system can take either the name of a magnitude system in the registry or an actual MagSystem instance. You can access these objects directly or create your own.

MagSystem objects represent the spectral flux density corresponding to magnitude zero in the given system and can be used to convert physical fluxes (in photons/s/cm^2) to magnitudes. Here’s an example:

>>> ab = sncosmo.get_magsystem('ab')
>>> ab.zpbandflux('sdssg')
546600.83408598113

This example gives the number of counts (in photons) when integrating the AB spectrum (which happens to be F_nu = 3631 Jansky at all wavelengths) through the SDSS g band. This works similarly for other magnitude systems:

>>> vega = sncosmo.get_magsystem('vega')
>>> vega.zpbandflux('sdssg')
597541.25707788975

You can see that the Vega spectrum is a bit brighter than the AB spectrum in this particular bandpass. Therefore, SDSS g magnitudes given in Vega will be larger than if given in AB.

There are convenience methods for converting an observed flux in a bandpass to a magnitude:

>>> ab.band_flux_to_mag(1., 'sdssg')
14.344175725172901
>>> ab.band_mag_to_flux(14.344175725172901, 'sdssg')
0.99999999999999833

So, one count per second in this band is equivalent to an AB magnitude of about 14.34.

“Composite” magnitude systems

Sometimes, photometric data is reported in “magnitude systems” that don’t correspond directly to any spectrophotometric standard. One example is “SDSS magnitudes” which are like AB magnitudes but with an offset in each band. These are represented in SNCosmo with the CompositeMagSystem class. For example:

>>> magsys = sncosmo.CompositeMagSystem(bands={'sdssg': ('ab', 0.01),
...                                            'sdssr': ('ab', 0.02)})

This defines a new magnitude system that knows about only two bandpasses. In this magnitude system, an object with magnitude zero in AB would have a magntide of 0.01 in SDSS g and 0.02 in SDSS r. Indeed, you can see that the flux corresponding to magnitude zero is slightly higher in this magnitude system than in AB:

>>> magsys.zpbandflux('sdssr')
502660.28545283229

>>> ab.zpbandflux('sdssr')
493485.70128115633

Since we’ve only defined the offsets for this magnitude system in a couple bands, using other bandpasses results in an error:

>>> magsys.zpbandflux('bessellb')
ValueError: band not defined in composite magnitude system

Photometric Data

Photometric data stored in AstroPy Table

In sncosmo, photometric data for a supernova is stored in an astropy Table: each row in the table is a photometric observation. The table must contain certain columns. To see what such a table looks like, you can load an example with the following function:

>>> data = sncosmo.load_example_data()
>>> print data
     time      band        flux          fluxerr      zp  zpsys
------------- ----- ----------------- -------------- ---- -----
      55070.0 sdssg    0.813499900062 0.651728140824 25.0    ab
55072.0512821 sdssr  -0.0852238865812 0.651728140824 25.0    ab
55074.1025641 sdssi -0.00681659003089 0.651728140824 25.0    ab
55076.1538462 sdssz     2.23929135407 0.651728140824 25.0    ab
55078.2051282 sdssg  -0.0308977349373 0.651728140824 25.0    ab
55080.2564103 sdssr     2.35450321853 0.651728140824 25.0    ab
... etc ...

This example data table above has the minimum six columns necessary for sncosmo’s light curve fitting and plotting functions to interpret the data. (There’s no harm in having more columns for other supplementary data.)

Additionally, metadata about the photometric data can be stored with the table: data.meta is an OrderedDict of the metadata.

Including Covariance

If your table contains a column 'fluxcov' (or any similar name; see below) it will be interpreted as covariance between the data points and will be used instead of the 'fluxerr' column when calculating a \(\chi^2\) value in fitting functions. For each row, the 'fluxcov' column should be a length N array, where N is the number of rows in the table. In other, words, table['fluxcov'] should have shape (N, N), where other columns like table['time'] have shape (N,).

As an example, let’s add a 'fluxcov' column to the example data table above.

>>> data['fluxcov'] = np.diag(data['fluxerr']**2)
>>> len(data)
40
>>> data['fluxcov'].shape
(40, 40)

# diagonal elements are error squared:
>>> data['fluxcov'][0, 0]
0.45271884317377648

>>> data['fluxerr'][0]
0.67284384754100002

# off diagonal elements are zero:
>>> data['fluxcov'][0, 1]
0.0

As is, this would be completely equivalent to just having the 'fluxerr' column. But now we have the flexibility to represent non-zero off-diagonal covariance.

Note

When sub-selecting data from a table with covariance, be sure to use sncosmo.select_data. For example, rather than table[mask], use sncosmo.select_data(table, mask). This ensures that the covariance column is sliced appropriately! See the documentation for select_data for details.

Flexible column names

What if you’d rather call the time column 'date', or perhaps 'mjd'? Good news! SNCosmo is flexible about the column names. For each column, it accepts a variety of alias names:

Column	Acceptable aliases (case-independent)	Description	Type
time	‘mjd_obs’, ‘time’, ‘date’, ‘mjd’, ‘mjdobs’, ‘jd’	Time of observation in days	float
band	‘band’, ‘flt’, ‘bandpass’, ‘filter’	Bandpass of observation	str
flux	‘f’, ‘flux’	Flux of observation	float
fluxerr	‘flux_err’, ‘fluxerror’, ‘flux_error’, ‘fluxerr’, ‘fe’	Gaussian uncertainty on flux	float
zp	‘zpt’, ‘zeropoint’, ‘zp’, ‘zero_point’	Zeropoint corresponding to flux	float
zpsys	‘zpsys’, ‘magsys’, ‘zpmagsys’	Magnitude system for zeropoint	str
fluxcov	‘covariance’, ‘covmat’, ‘covar’, ‘cov’, ‘fluxcov’	Covariance between observations (array; optional)	ndarray

Note that each column must be present in some form or another, with no repeats. For example, you can have either a 'flux' column or a 'f' column, but not both.

The units of the flux and flux uncertainty are effectively given by the zeropoint system, with the zeropoint itself serving as a scaling factor: For example, if the zeropoint is 25.0 and the zeropoint system is 'vega', a flux of 1.0 corresponds to 10**(-25/2.5) times the integrated flux of Vega in the given bandpass.

Reading and Writing photometric data from files

SNCosmo strives to be agnostic with respect to file format. In practice there are a plethora of different file formats, both standard and non-standard, used to represent tables. Rather than picking a single supported file format, or worse, creating yet another new “standard”, we choose to leave the file format mostly up to the user: A user can use any file format as long as they can read their data into an astropy Table.

That said, SNCosmo does include a couple convenience functions for reading and writing tables of photometric data: sncosmo.read_lc and sncosmo.write_lc:

>>> data = sncosmo.load_example_data()
>>> sncosmo.write_lc(data, 'test.txt')

This creates an output file test.txt that looks like:

@x1 0.5
@c 0.2
@z 0.5
@x0 1.20482820761e-05
@t0 55100.0
time band flux fluxerr zp zpsys
55070.0 sdssg 0.36351153597 0.672843847541 25.0 ab
55072.0512821 sdssr -0.200801295864 0.672843847541 25.0 ab
55074.1025641 sdssi 0.307494232981 0.672843847541 25.0 ab
55076.1538462 sdssz 1.08776103656 0.672843847541 25.0 ab
55078.2051282 sdssg -0.43667895645 0.672843847541 25.0 ab
55080.2564103 sdssr 1.09780966779 0.672843847541 25.0 ab
... etc ...

Read the file back in:

>>> data2 = sncosmo.read_lc('test.txt')

There are a few other available formats, which can be specified using the format keyword:

>>> data = sncosmo.read_lc('test.json', format='json')

The supported formats are listed below. If your preferred format is not included, use a standard reader/writer from astropy or the Python universe.

Format name	Description	Notes
ascii (default)	ASCII with metadata lines marked by ‘@’	Not readable by standard ASCII table parsers due to metadata lines.
json	JavaScript Object Notation	Good performance, but not as human-readable as ascii
salt2	SALT2 new-style data files
salt2-old	SALT2 old-style data files

Manipulating data tables

Because photometric data tables are astropy Tables, they can be manipulated any way that Tables can. Here’s a few things you might want to do.

Rename a column:

>>> data.rename_column('oldname', 'newname')

Add a column:

>>> data['zp'] = 26.

Add a constant value to all the entries in a given column:

>>> data['zp'] += 0.03

See the documentation on astropy tables for more information.

Applying Cuts

It is useful to be able to apply “cuts” to data before trying to fit a model to the data. This is particularly important when using some of the “guessing” algorithms in fit_lc and nest_lc that use a minimum signal-to-noise ratio to pick “good” data points. These algorithms will raise an exception if there are no data points meeting the requirements, so it is advisable to check if the data meets the requirements beforehand.

Signal-to-noise ratio cuts

Require at least one datapoint with signal-to-noise ratio (S/N) greater than 5 (in any band):

>>> passes = np.max(data['flux'] / data['fluxerr']) > 5.
>>> passes
True

Require two bands each with at least one datapoint having S/N > 5:

>>> mask = data['flux'] / data['fluxerr'] > 5.
>>> passes = len(np.unique(data['band'][mask])) >= 2
>>> passes
True

Simulation

First, define a set of “observations”. These are the properties of our observations: the time, bandpass and depth.

import sncosmo
from astropy.table import Table
obs = Table({'time': [56176.19, 56188.254, 56207.172],
             'band': ['desg', 'desr', 'desi'],
             'gain': [1., 1., 1.],
             'skynoise': [191.27, 147.62, 160.40],
             'zp': [30., 30., 30.],
             'zpsys':['ab', 'ab', 'ab']})
print obs

skynoise zpsys band gain    time    zp
-------- ----- ---- ---- --------- ----
  191.27    ab desg  1.0  56176.19 30.0
  147.62    ab desr  1.0 56188.254 30.0
   160.4    ab desi  1.0 56207.172 30.0

Suppose we want to simulate a SN with the SALT2 model and the following parameters:

model = sncosmo.Model(source='salt2')
params = {'z': 0.4, 't0': 56200.0, 'x0':1.e-5, 'x1': 0.1, 'c': -0.1}

To get the light curve for this single SN, we’d do:

lcs = sncosmo.realize_lcs(obs, model, [params])
print lcs[0]

   time   band      flux        fluxerr     zp  zpsys
--------- ---- ------------- ------------- ---- -----
 56176.19 desg 96.0531272705  191.27537908 30.0    ab
56188.254 desr 456.360196623  149.22627064 30.0    ab
56207.172 desi  655.40885611 162.579572369 30.0    ab

Note that we’ve passed the function a one-element list, [params], and gotten back a one-element list in return. (The realize_lcs function is designed to operate on lists of SNe for convenience.)

Generating SN parameters

We see above that it is straightforward to simulate SNe once we already know the parameters of each one. But what if we want to pick SN parameters from some defined distribution?

Suppose we want to generate SN parameters for all the SNe we would find in a given search area over a defined period of time. We start by defining an area and time period, as well as a maximum redshift to consider:

area = 1.  # area in square degrees
tmin = 56175.  # minimum time
tmax = 56225.  # maximum time
zmax = 0.7

First, we’d like to get the number and redshifts of all SNe that occur over our 1 square degree and 50 day time period:

redshifts = list(sncosmo.zdist(0., zmax, time=(tmax-tmin), area=area))
print len(redshifts), "SNe"
print "redshifts:", redshifts

9 SNe
redshifts: [0.4199710008856507, 0.3500118339133868, 0.5915676316485601, 0.5857452631151785, 0.49024466410556855, 0.5732679644841575, 0.6224436826380927, 0.5853477892182203, 0.5522300320124105]

Generate a list of SN parameters using these redshifts, drawing x1 and c from normal distributions:

from numpy.random import uniform, normal
params = [{'x0':1.e-5, 'x1':normal(0., 1.), 'c':normal(0., 0.1),
           't0':uniform(tmin, tmax), 'z': z}
          for z in redshifts]
for p in params:
    print p

{'z': 0.4199710008856507, 'x0': 1e-05, 'x1': -0.9739877070754421, 'c': -0.1465835504611458, 't0': 56191.57686616353}
{'z': 0.3500118339133868, 'x0': 1e-05, 'x1': 0.04454878604727126, 'c': -0.04920811869083081, 't0': 56222.76963606611}
{'z': 0.5915676316485601, 'x0': 1e-05, 'x1': -0.26765265677262423, 'c': -0.06456008680932701, 't0': 56211.706219411404}
{'z': 0.5857452631151785, 'x0': 1e-05, 'x1': 0.8255953341731204, 'c': 0.08520083775049729, 't0': 56209.33583211229}
{'z': 0.49024466410556855, 'x0': 1e-05, 'x1': -0.12051827966517584, 'c': -0.09490756669333822, 't0': 56189.37571007927}
{'z': 0.5732679644841575, 'x0': 1e-05, 'x1': 0.3051310078192594, 'c': -0.10967604820261241, 't0': 56198.04368422346}
{'z': 0.6224436826380927, 'x0': 1e-05, 'x1': -0.6329407028587257, 'c': -0.009789183239376284, 't0': 56179.88133113836}
{'z': 0.5853477892182203, 'x0': 1e-05, 'x1': 0.6373371286596669, 'c': 0.05151693090038232, 't0': 56212.04579735962}
{'z': 0.5522300320124105, 'x0': 1e-05, 'x1': 0.04762095339856289, 'c': -0.005018877828783951, 't0': 56182.14827040906}

So far so good. The only problem is that x0 doesn’t vary. We’d like it to be randomly distributed with some scatter around the Hubble line, so it should depend on the redshift. Here’s an alternative:

params = []
for z in redshifts:
    mabs = normal(-19.3, 0.3)
    model.set(z=z)
    model.set_source_peakabsmag(mabs, 'bessellb', 'ab')
    x0 = model.get('x0')
    p = {'z':z, 't0':uniform(tmin, tmax), 'x0':x0, 'x1': normal(0., 1.), 'c': normal(0., 0.1)}
    params.append(p)

for p in params:
    print p

{'c': -0.060104568346581566, 'x0': 2.9920355958896461e-05, 'z': 0.4199710008856507, 'x1': -0.677121283126299, 't0': 56217.93979718883}
{'c': 0.10405991801014292, 'x0': 2.134500759148091e-05, 'z': 0.3500118339133868, 'x1': 1.6034252041294512, 't0': 56218.008314206476}
{'c': -0.14777109151711296, 'x0': 7.9108889725043354e-06, 'z': 0.5915676316485601, 'x1': -2.2082282760850993, 't0': 56218.013686428785}
{'c': 0.056034777154805086, 'x0': 6.6457371815973038e-06, 'z': 0.5857452631151785, 'x1': 0.675413080007434, 't0': 56189.03517395757}
{'c': -0.0709158052635228, 'x0': 1.2228145655148946e-05, 'z': 0.49024466410556855, 'x1': 0.5449847454420981, 't0': 56198.02895700289}
{'c': -0.22101146234021096, 'x0': 7.4299221264917702e-06, 'z': 0.5732679644841575, 'x1': -1.543245858395605, 't0': 56189.04585414441}
{'c': 0.06964843664572477, 'x0': 9.7121906557832662e-06, 'z': 0.6224436826380927, 'x1': 1.7419604610283943, 't0': 56212.827270197355}
{'c': 0.07320513053870191, 'x0': 3.22205341646521e-06, 'z': 0.5853477892182203, 'x1': -0.39658066375434153, 't0': 56200.421464066916}
{'c': 0.18555773972769227, 'x0': 7.5955258508017471e-06, 'z': 0.5522300320124105, 'x1': -0.24463691193386283, 't0': 56190.492271332616}

Now we can generate the lightcurves for these parameters:

lcs = sncosmo.realize_lcs(obs, model, params)
print lcs[0]

   time   band      flux       fluxerr     zp  zpsys
--------- ---- ------------- ------------ ---- -----
 56176.19 desg 6.70520005464       191.27 30.0    ab
56188.254 desr 106.739113709       147.62 30.0    ab
56207.172 desi  1489.7521011 164.62420476 30.0    ab

Note that the “true” parameters are saved in the metadata of each SN:

lcs[0].meta

{'c': -0.060104568346581566,
 't0': 56217.93979718883,
 'x0': 2.9920355958896461e-05,
 'x1': -0.677121283126299,
 'z': 0.4199710008856507}

Registry

What is it?

The registry (sncosmo.registry) is responsible for translating string identifiers to objects, for user convenience. For example, it is used in sncosmo.get_bandpass and sncosmo.get_source to return a Bandpass or sncosmo.Model object based on the name of the bandpass or model:

>>> sncosmo.get_bandpass('sdssi')
<Bandpass 'sdssi' at 0x28e7c90>

It is also used in methods like bandflux to give it the ability to accept either a Bandpass object or the name of a bandpass:

>>> model = sncosmo.Model(source='hsiao')
>>> model.bandflux('sdssg', 0.)  # works, thanks to registry.

Under the covers, the bandflux method retrieves the Bandpass corresponding to 'sdssg' by calling the sncosmo.get_bandpass function.

The registry is actually quite simple: it basically amounts to a dictionary and a few functions for accessing the dictionary. Most of the time, a user doesn’t need to know anything about the registry. However, it is useful if you want to add your own “built-ins” or change the name of existing ones.

Using the registry to achieve custom “built-ins”

There are a small set of “built-in” models, bandpasses, and magnitude systems. But what if you want additional ones?

Create a file mydefs.py that registers all your custom definitions:

# contents of mydefs.py
import numpy as np
import sncosmo

wave = np.array([4000., 4200., 4400., 4600., 4800., 5000.])
trans = np.array([0., 1., 1., 1., 1., 0.])
band = sncosmo.Bandpass(wave, trans, name='tophatg')

sncosmo.registry.register(band)

Make sure mydefs.py is somewhere in your $PYTHONPATH or the directory you are running your main script from. Now in your script import your definitions at the beginning:

>>> import sncosmo
>>> import mydefs
>>> # ... proceed as normal
>>> # you can now use 'tophatg' as a built-in

Changing the name of built-ins

To change the name of the 'sdssg' band to 'SDSS_G':

# contents of mydefs.py
import sncosmo

band = sncosmo.get_bandpass('sdssg')
band.name = 'SDSS_G'
sncosmo.register(band)

Large built-ins

What if your built-ins are really big or you have a lot of them? You might only want to load them as they are needed, rather than having to load everything into memory when you do import mydefs. You can use the sncosmo.registry.register_loader function. Suppose we have a bandpass that requires a huge data file (In reality it is unlikely that loading bandpasses would take a noticeable amount of time, but it might for models or spectra.):

# contents of mydefs.py
import sncosmo

def load_bandpass(filename, name=None, version=None):
    # ...
    # read data from filename, create a Bandpass object, "band"
    # ...
    return band

filename = 'path/to/datafile/for/huge_tophatg'
sncosmo.register_loader(
    sncosmo.Bandpass,      # class of object returned.
    'huge_tophatg',        # name
    load_bandpass,         # function that does the loading
    [filename]             # arguments to pass to function
    )

Now when you import mydefs the registry will know how to load the Bandpass named 'huge_tophatg' when it is needed. When loaded, it will be saved in memory so that subsequent operations don’t need to load it again.

Directory Configuration

The “built-in” Sources and Spectra in SNCosmo depend on some sizable data files. These files are hosted remotely, downloaded as needed, and cached locally. This all happens automatically, but it is helpful to know where the files are stored if you want to inspect them or share a common download directory between multiple users.

By default, SNCosmo will create and use an sncosmo subdirectory in the AstroPy cache directory for this purpose. For example, $HOME/.astropy/cache/sncosmo. After using a few models and spectra for the first time, here is what that directory might look like:

$ tree ~/.astropy/cache/sncosmo
/home/kyle/.astropy/cache/sncosmo
├── models
│   ├── hsiao
│   │   └── Hsiao_SED_V3.fits
│   └── sako
│       ├── S11_SDSS-000018.SED
│       ├── S11_SDSS-001472.SED
│       └── S11_SDSS-002000.SED
└── spectra
    ├── alpha_lyr_stis_007.fits
    └── bd_17d4708_stisnic_005.fits

You can see that within the top-level $HOME/.astropy/cache/sncosmo directory, a particular directory structure is created. This directory structure is fixed in the code, so it’s best not to move things around within the top-level directory. If you do, sncosmo will think the data have not been downloaded and will re-download them.

Configuring the Directories

What if you would rather use a different directory to store downloaded data? Perhaps you’d rather the data not be in a hidden directory, or perhaps there are multiple users who wish to use a shared data directory. There are two options:

1. Set the environment variable SNCOSMO_DATA_DIR to the directory you wish to use. For example, in bash:

   export SNCOSMO_DATA_DIR=/home/user/data/sncosmo
   

   If this environment variable is set, it takes precedence over the second option (below).

2. Set the data_dir variable in the sncosmo configuartion file. This file is found in the astropy configuration directory, e.g., $HOME/.astropy/config/sncosmo.cfg. When you import sncosmo it checks for this file and creates a default one if it doesn’t exist. The default one looks like this:

   $ cat ~/.astropy/config/sncosmo.cfg
   
   ## Directory containing SFD (1998) dust maps, with names:
   ## 'SFD_dust_4096_ngp.fits' and 'SFD_dust_4096_sgp.fits'
   ## Example: sfd98_dir = /home/user/data/sfd98
   # sfd98_dir = None
   
   ## Directory where sncosmo will store and read downloaded data resources.
   ## If None, ASTROPY_CACHE_DIR/sncosmo will be used.
   ## Example: data_dir = /home/user/data/sncosmo
   # data_dir = None
   

To change the data directory, simply uncomment the last line and set it to the desired directory. You can even move the data directory around, as long as you update this configuration parameter accordingly.

orphan:

Examples

Fitting a light curve

Fitting a light curve

This example shows how to fit the parameters of a SALT2 model to photometric light curve data.

First, we’ll load an example of some photometric data.

from __future__ import print_function

import sncosmo

data = sncosmo.load_example_data()

print(data)

Out:

time      band       flux         fluxerr      zp  zpsys
------------- ----- --------------- -------------- ---- -----
      55070.0 sdssg   0.36351153597 0.672843847541 25.0    ab
55072.0512821 sdssr -0.200801295864 0.672843847541 25.0    ab
55074.1025641 sdssi  0.307494232981 0.672843847541 25.0    ab
55076.1538462 sdssz   1.08776103656 0.672843847541 25.0    ab
55078.2051282 sdssg  -0.43667895645 0.672843847541 25.0    ab
55080.2564103 sdssr   1.09780966779 0.672843847541 25.0    ab
55082.3076923 sdssi    3.7562685627 0.672843847541 25.0    ab
55084.3589744 sdssz   5.34858894966 0.672843847541 25.0    ab
55086.4102564 sdssg   2.82614187269 0.672843847541 25.0    ab
55088.4615385 sdssr   7.56547045054 0.672843847541 25.0    ab
          ...   ...             ...            ...  ...   ...
55129.4871795 sdssr    2.6597485586 0.672843847541 25.0    ab
55131.5384615 sdssi   3.99520404021 0.672843847541 25.0    ab
55133.5897436 sdssz   5.73989458094 0.672843847541 25.0    ab
55135.6410256 sdssg  0.330702283107 0.672843847541 25.0    ab
55137.6923077 sdssr  0.565286726579 0.672843847541 25.0    ab
55139.7435897 sdssi   3.04318346795 0.672843847541 25.0    ab
55141.7948718 sdssz   5.62692686384 0.672843847541 25.0    ab
55143.8461538 sdssg -0.722654789013 0.672843847541 25.0    ab
55145.8974359 sdssr   1.12091764262 0.672843847541 25.0    ab
55147.9487179 sdssi    2.1246695264 0.672843847541 25.0    ab
      55150.0 sdssz    5.3482175645 0.672843847541 25.0    ab
Length = 40 rows

An important additional note: a table of photometric data has a band column and a zpsys column that use strings to identify the bandpass (e.g., 'sdssg') and zeropoint system ('ab') of each observation. If the bandpass and zeropoint systems in your data are not built-ins known to sncosmo, you must register the corresponding Bandpass or MagSystem to the right string identifier using the registry.

# create a model
model = sncosmo.Model(source='salt2')

# run the fit
result, fitted_model = sncosmo.fit_lc(
    data, model,
    ['z', 't0', 'x0', 'x1', 'c'],  # parameters of model to vary
    bounds={'z':(0.3, 0.7)})  # bounds on parameters (if any)

Out:

Downloading http://supernovae.in2p3.fr/salt/lib/exe/fetch.php?media=salt2_model_data-2-4.tar.gz [Done]
Downloading http://sncosmo.github.io/data/bandpasses/sdss/sdss_g.dat [Done]
Downloading http://sncosmo.github.io/data/bandpasses/sdss/sdss_r.dat [Done]
Downloading http://sncosmo.github.io/data/bandpasses/sdss/sdss_i.dat [Done]
Downloading http://sncosmo.github.io/data/bandpasses/sdss/sdss_z.dat [Done]

The first object returned is a dictionary-like object where the keys can be accessed as attributes in addition to the typical dictionary lookup like result['ncall']:

print("Number of chi^2 function calls:", result.ncall)
print("Number of degrees of freedom in fit:", result.ndof)
print("chi^2 value at minimum:", result.chisq)
print("model parameters:", result.param_names)
print("best-fit values:", result.parameters)
print("The result contains the following attributes:\n", result.keys())

Out:

Number of chi^2 function calls: 133
Number of degrees of freedom in fit: 35
chi^2 value at minimum: 33.80988236076302
model parameters: ['z', 't0', 'x0', 'x1', 'c']
best-fit values: [5.15154859e-01 5.51004778e+04 1.19625368e-05 4.67270999e-01
 1.93951997e-01]
The result contains the following attributes:
 dict_keys(['ndof', 'nfit', 'message', 'success', 'param_names', 'data_mask', 'errors', 'parameters', 'vparam_names', 'chisq', 'covariance', 'ncall'])

The second object returned is a shallow copy of the input model with the parameters set to the best fit values. The input model is unchanged.

sncosmo.plot_lc(data, model=fitted_model, errors=result.errors)

Suppose we already know the redshift of the supernova we’re trying to fit. We want to set the model’s redshift to the known value, and then make sure not to vary z in the fit.

model.set(z=0.5)  # set the model's redshift.
result, fitted_model = sncosmo.fit_lc(data, model,
                                      ['t0', 'x0', 'x1', 'c'])
sncosmo.plot_lc(data, model=fitted_model, errors=result.errors)

Total running time of the script: ( 0 minutes 5.582 seconds)

Using a custom fitter or sampler

Using a custom fitter or sampler

How to use your own minimizer or MCMC sampler for fitting light curves.

SNCosmo has three functions for model parameter estimation based on photometric data: sncosmo.fit_lc, sncosmo.mcmc_lc and sncosmo.nest_lc. These are wrappers around external minimizers or samplers (respectively: iminuit, emcee and nestle). However, one may wish to experiment with a custom fitting or sampling method.

Here, we give a minimal example of using the L-BFGS-B minimizer from scipy.

from __future__ import print_function

import numpy as np
from scipy.optimize import fmin_l_bfgs_b
import sncosmo

model = sncosmo.Model(source='salt2')
data = sncosmo.load_example_data()

# Define an objective function that we will pass to the minimizer.
# The function arguments must comply with the expectations of the specfic
# minimizer you are using.
def objective(parameters):
    model.parameters[:] = parameters  # set model parameters

    # evaluate model fluxes at times/bandpasses of data
    model_flux = model.bandflux(data['band'], data['time'],
                                zp=data['zp'], zpsys=data['zpsys'])

    # calculate and return chi^2
    return np.sum(((data['flux'] - model_flux) / data['fluxerr'])**2)

# starting parameter values in same order as `model.param_names`:
start_parameters = [0.4, 55098., 1e-5, 0., 0.]  # z, t0, x0, x1, c

# parameter bounds in same order as `model.param_names`:
bounds = [(0.3, 0.7), (55080., 55120.), (None, None), (None, None),
          (None, None)]

parameters, val, info = fmin_l_bfgs_b(objective, start_parameters,
                                      bounds=bounds, approx_grad=True)

print(parameters)

Out:

[ 4.25825914e-01  5.50980000e+04  1.10729251e-05 -4.88206597e-03
  3.54030794e-01]

The built-in parameter estimation functions in sncosmo take care of setting up the likelihood function in the way that the underlying fitter or sampler expects. Additionally, they set guesses and bounds and package results up in a way that is as consistent as possible. For users wishing use a custom minimizer or sampler, it can be instructive to look at the source code for these functions.

Total running time of the script: ( 0 minutes 0.781 seconds)

Creating a new Source class

Creating a new Source class

Extending sncosmo with a custom type of Source.

A Source is something that specifies a spectral timeseries as a function of an arbitrary number of parameters. For example, the SALT2 model has three parameters (x0, x1 and c) that determine a unique spectrum as a function of phase. The SALT2Source class implements the behavior of the model: how the spectral time series depends on those parameters.

If you have a spectral timeseries model that follows the behavior of one of the existing classes, such as TimeSeriesSource, great! There’s no need to write a custom class. However, suppose you want to implement a model that has some new parameterization. In this case, you need a new class that implements the behavior.

In this example, we implement a new type of source model. Our model is a linear combination of two spectral time series, with a parameter w that determines the relative weight of the models.

from __future__ import print_function

import numpy as np
from scipy.interpolate import RectBivariateSpline
import sncosmo


class ComboSource(sncosmo.Source):

    _param_names = ['amplitude', 'w']
    param_names_latex = ['A', 'w']   # used in plotting display

    def __init__(self, phase, wave, flux1, flux2, name=None, version=None):
        self.name = name
        self.version = version
        self._phase = phase
        self._wave = wave

        # ensure that fluxes are on the same scale
        flux2 = flux1.max() / flux2.max() * flux2

        self._model_flux1 = RectBivariateSpline(phase, wave, flux1, kx=3, ky=3)
        self._model_flux2 = RectBivariateSpline(phase, wave, flux2, kx=3, ky=3)
        self._parameters = np.array([1., 0.5])  # initial parameters

    def _flux(self, phase, wave):
        amplitude, w = self._parameters
        return amplitude * ((1.0 - w) * self._model_flux1(phase, wave) +
                            w * self._model_flux2(phase, wave))

… and that’s all that we need to define!: A couple class attributes (_param_names and param_names_latex, an __init__ method, and a _flux method. The _flux method is guaranteed to be passed numpy arrays for phase and wavelength.

We can now initialize an instance of this source from two spectral time series:

#Just as an example, we'll use some undocumented functionality in
# sncosmo to download the Nugent Ia and 2p templates. Don't rely on this
# the `DATADIR` object, or these paths in your code though, as these are
# subject to change between version of sncosmo!
from sncosmo.builtins import DATADIR
phase1, wave1, flux1 = sncosmo.read_griddata_ascii(
    DATADIR.abspath('models/nugent/sn1a_flux.v1.2.dat'))
phase2, wave2, flux2 = sncosmo.read_griddata_ascii(
    DATADIR.abspath('models/nugent/sn2p_flux.v1.2.dat'))

# In our __init__ method we defined above, the two fluxes need to be on
# the same grid, so interpolate the second onto the first:
flux2_interp = RectBivariateSpline(phase2, wave2, flux2)(phase1, wave1)

source = ComboSource(phase1, wave1, flux1, flux2_interp, name='sn1a+sn2p')

Out:

Downloading http://c3.lbl.gov/nugent/templates/sn1a_flux.v1.2.dat.gz [Done]
Downloading http://c3.lbl.gov/nugent/templates/sn2p_flux.v1.2.dat.gz [Done]

We can get a summary of the Source we created:

print(source)

Out:

class      : ComboSource
name       : 'sn1a+sn2p'
version    : None
phases     : [0, .., 90] days
wavelengths: [1000, .., 25000] Angstroms
parameters:
  amplitude = 1.0
  w         = 0.5

Get a spectrum at phase 10 for different parameters:

from matplotlib import pyplot as plt

wave = np.linspace(2000.0, 10000.0, 500)
for w in (0.0, 0.2, 0.4, 0.6, 0.8, 1.0):
    source.set(w=w)
    plt.plot(wave, source.flux(10., wave), label='w={:3.1f}'.format(w))

plt.legend()
plt.show()

The w=0 spectrum is that of the Ia model, the w=1 spectrum is that of the IIp model, while intermediate spectra are weighted combinations.

We can even fit the model to some data!

model = sncosmo.Model(source=source)
data = sncosmo.load_example_data()
result, fitted_model = sncosmo.fit_lc(data, model,
                                      ['z', 't0', 'amplitude', 'w'],
                                      bounds={'z': (0.2, 1.0),
                                              'w': (0.0, 1.0)})

sncosmo.plot_lc(data, model=fitted_model, errors=result.errors)

The fact that the fitted value of w is closer to 0 than 1 indicates that the light curve looks more like the Ia template than the IIp template. This is generally what we expected since the example data here was generated from a Ia template (although not the Nugent template!).

Total running time of the script: ( 0 minutes 4.317 seconds)

Examples

Fitting a light curve

Using a custom fitter or sampler

Creating a new Source class

Reference / API

Model & Components

Model(source[, effects, effect_names, …])

An observer-frame model, composed of a Source and zero or more effects.

Source component of Model

Source()	An abstract base class for transient models.
TimeSeriesSource(phase, wave, flux[, …])	A single-component spectral time series model.
StretchSource(phase, wave, flux[, name, version])	A single-component spectral time series model, that “stretches” in time.
SALT2Source([modeldir, m0file, m1file, …])	The SALT2 Type Ia supernova spectral timeseries model.

Effect components of Model: interstellar dust extinction

PropagationEffect	Abstract base class for propagation effects.
CCM89Dust()	Cardelli, Clayton, Mathis (1989) extinction model dust.
OD94Dust()	O’Donnell (1994) extinction model dust.
F99Dust([r_v])	Fitzpatrick (1999) extinction model dust with fixed R_V.

Bandpass & Magnitude Systems

Bandpass(wave, trans[, wave_unit, …])	Transmission as a function of spectral wavelength.
AggregateBandpass(transmissions[, …])	Bandpass defined by multiple transmissions in series.
BandpassInterpolator(transmissions, …[, …])	Bandpass generator defined as a function of focal plane position.
MagSystem([name])	An abstract base class for magnitude systems.
ABMagSystem([name])	Magnitude system where a source with F_nu = 3631 Jansky at all frequencies has magnitude 0 in all bands.
SpectralMagSystem(refspectrum[, name])	A magnitude system defined by a fundamental spectrophotometric standard.
CompositeMagSystem([bands, families, name])	A magnitude system defined in a specific set of bands.

I/O

Functions for reading and writing photometric data, gridded data, extinction maps, and more.

read_lc(file_or_dir[, format])	Read light curve data for a single supernova.
write_lc(data, fname[, format])	Write light curve data.
read_bandpass(fname[, fmt, wave_unit, …])	Read bandpass from two-column ASCII file containing wavelength and transmission in each line.
load_example_data()	Load an example photometric data table.
read_snana_ascii(fname[, default_tablename])	Read an SNANA-format ascii file.
read_snana_fits(head_file, phot_file[, snids, n])	Read the SNANA FITS format: two FITS files jointly representing metadata and photometry for a set of SNe.
read_snana_simlib(fname)	Read an SNANA ‘simlib’ (simulation library) ascii file.
read_griddata_ascii(name_or_obj)	Read 2-d grid data from a text file.
read_griddata_fits(name_or_obj[, ext])	Read a multi-dimensional grid of data from a FITS file, where the grid coordinates are encoded in the FITS-WCS header keywords.
write_griddata_ascii(x0, x1, y, name_or_obj)	Write 2-d grid data to a text file.
write_griddata_fits(x0, x1, y, name_or_obj)	Write a 2-d grid of data to a FITS file

Fitting Photometric Data

Estimate model parameters from photometric data

fit_lc(data, model, vparam_names[, bounds, …])	Fit model parameters to data by minimizing chi^2.
mcmc_lc(data, model, vparam_names[, bounds, …])	Run an MCMC chain to get model parameter samples.
nest_lc(data, model, vparam_names, bounds[, …])	Run nested sampling algorithm to estimate model parameters and evidence.

Convenience functions

select_data(data, index)	Convenience function for indexing photometric data with covariance.
chisq(data, model[, modelcov])	Calculate chisq statistic for the model, given the data.
flatten_result(res)	Turn a result from fit_lc into a simple dictionary of key, value pairs.

Plotting

Convenience functions for quick standard plots (requires matplotlib)

plot_lc([data, model, bands, zp, zpsys, …])

Plot light curve data or model light curves.

Simulation

zdist(zmin, zmax[, time, area, ratefunc, …])	Generate a distribution of redshifts.
realize_lcs(observations, model, params[, …])	Realize data for a set of SNe given a set of observations.

Registry

Register and retrieve custom built-in sources, bandpasses, and magnitude systems

register(instance[, name, data_class, force])	Register a class instance.
register_loader(data_class, name, func[, …])	Register a data reading function.
get_source(name[, version, copy])	Retrieve a Source from the registry by name.
get_bandpass(name, *args)	Get a Bandpass from the registry by name.
get_magsystem(name)	Get a MagSystem from the registry by name.

Class Inheritance Diagrams

List of Built-in Sources

Name	Version	Type	Subclass	Reference	Website	Notes
‘nugent-sn1a’	‘1.2’	SN Ia	TimeSeriesSource	[Rb0467a492107-N02]		a
‘nugent-sn91t’	‘1.1’	SN Ia	TimeSeriesSource	[Rb0467a492107-S04]		a
‘nugent-sn91bg’	‘1.1’	SN Ia	TimeSeriesSource	[Rb0467a492107-N02]		a
‘nugent-sn1bc’	‘1.1’	SN Ib/c	TimeSeriesSource	[Rb0467a492107-L05]		a
‘nugent-hyper’	‘1.2’	SN Ib/c	TimeSeriesSource	[Rb0467a492107-L05]		a
‘nugent-sn2p’	‘1.2’	SN IIP	TimeSeriesSource	[Rb0467a492107-G99]		a
‘nugent-sn2l’	‘1.2’	SN IIL	TimeSeriesSource	[Rb0467a492107-G99]		a
‘nugent-sn2n’	‘2.1’	SN IIn	TimeSeriesSource	[Rb0467a492107-G99]		a
‘s11-2004hx’	‘1.0’	SN IIL/P	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘s11-2005lc’	‘1.0’	SN IIP	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘s11-2005hl’	‘1.0’	SN Ib	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘s11-2005hm’	‘1.0’	SN Ib	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘s11-2005gi’	‘1.0’	SN IIP	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘s11-2006fo’	‘1.0’	SN Ic	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘s11-2006jo’	‘1.0’	SN Ib	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘s11-2006jl’	‘1.0’	SN IIP	TimeSeriesSource	[Rb0467a492107-S11]		b [Rb0467a492107-1]
‘hsiao’	‘1.0’	SN Ia	TimeSeriesSource	[Rb0467a492107-H07]		c [Rb0467a492107-2]
‘hsiao’	‘2.0’	SN Ia	TimeSeriesSource	[Rb0467a492107-H07]		c [Rb0467a492107-2]
‘hsiao’	‘3.0’	SN Ia	TimeSeriesSource	[Rb0467a492107-H07]		c [Rb0467a492107-2]
‘hsiao-subsampled’	‘3.0’	SN Ia	TimeSeriesSource	[Rb0467a492107-H07]		c [Rb0467a492107-2]
‘salt2’	‘2.0’	SN Ia	SALT2Source	[Rb0467a492107-G10]		d
‘salt2’	‘2.4’	SN Ia	SALT2Source	[Rb0467a492107-B14b]		d
‘salt2-extended’	‘1.0’	SN Ia	SALT2Source		b	[Rb0467a492107-3]
‘salt2-h17’	‘1.0’	SN Ia	SALT2Source	[Rb0467a492107-H17]		e [Rb0467a492107-4]
‘snf-2011fe’	‘1.0’	SN Ia	TimeSeriesSource	[Rb0467a492107-P13]		f
‘snana-2004fe’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2004gq’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-sdss004012’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006fo’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-sdss014475’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006lc’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007ms’	‘1.0’	SN II-pec	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-04d1la’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-04d4jv’	‘1.0’	SN Ic	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2004gv’	‘1.0’	SN Ib	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006ep’	‘1.0’	SN Ib	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007y’	‘1.0’	SN Ib	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2004ib’	‘1.0’	SN Ib	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2005hm’	‘1.0’	SN Ib	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006jo’	‘1.0’	SN Ib	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007nc’	‘1.0’	SN Ib	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2004hx’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2005gi’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006gq’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006kn’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006jl’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006iw’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006kv’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006ns’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007iz’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007nr’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007kw’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007ky’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007lj’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007lb’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007ll’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007nw’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007ld’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007md’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007lz’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007lx’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007og’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007ny’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007nv’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2007pg’	‘1.0’	SN IIP	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006ez’	‘1.0’	SN IIn	TimeSeriesSource		g	[Rb0467a492107-5]
‘snana-2006ix’	‘1.0’	SN IIn	TimeSeriesSource		g	[Rb0467a492107-5]
‘whalen-z15b’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘whalen-z15d’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘whalen-z15g’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘whalen-z25b’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘whalen-z25d’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘whalen-z25g’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘whalen-z40b’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘whalen-z40g’	‘1.0’	PopIII	TimeSeriesSource	[Rb0467a492107-Whalen13]		[Rb0467a492107-6]
‘mlcs2k2’	‘1.0’	SN Ia	MLCS2k2Source	[Rb0467a492107-Jha07]		[Rb0467a492107-7]
‘snemo2’	‘1.0’	SN Ia	SNEMOSource	[Rb0467a492107-Saunders18]		h
‘snemo7’	‘1.0’	SN Ia	SNEMOSource	[Rb0467a492107-Saunders18]		h
‘snemo15’	‘1.0’	SN Ia	SNEMOSource	[Rb0467a492107-Saunders18]		h

[Rb0467a492107-N02]

(1, 2) Nugent, Kim & Permutter 2002

[Rb0467a492107-S04]

Stern, et al. 2004

[Rb0467a492107-L05]

(1, 2) Levan et al. 2005

[Rb0467a492107-G99]

(1, 2, 3) Gilliland, Nugent & Phillips 1999

[Rb0467a492107-S11]

(1, 2, 3, 4, 5, 6, 7, 8) Sako et al. 2011

[Rb0467a492107-H07]

(1, 2, 3, 4) Hsiao et al. 2007

[Rb0467a492107-G10]

Guy et al. 2010

[Rb0467a492107-B14b]

Betoule et al. 2014

[Rb0467a492107-H17]

Hounsell et al. 2017

[Rb0467a492107-P13]

Pereira et al. 2013

[Rb0467a492107-Whalen13]

(1, 2, 3, 4, 5, 6, 7, 8) Whalen et al. 2013

[Rb0467a492107-Jha07]

Jha, Riess and Kirshner 2007

[Rb0467a492107-Saunders18]

(1, 2, 3) Saunders et al. 2018

[Rb0467a492107-1]

(1, 2, 3, 4, 5, 6, 7, 8) extracted from SNANA’s SNDATA_ROOT on 29 March 2013.

[Rb0467a492107-2]

(1, 2, 3, 4) extracted from the SNooPy package on 21 Dec 2012.

[Rb0467a492107-3]

extracted from SNANA’s SNDATA_ROOT on 15 August 2013.

[Rb0467a492107-4]

extracted from SNANA’s SNDATA_ROOT on 24 April 2018. SALT2 model with wide wavelength range, Hounsell et al. 2017

[Rb0467a492107-5]

(1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15, 16, 17, 18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34, 35, 36, 37, 38, 39, 40, 41, 42) extracted from SNANA’s SNDATA_ROOT on 5 August 2014.

[Rb0467a492107-6]

(1, 2, 3, 4, 5, 6, 7, 8) private communication (D.Whalen, May 2014).

[Rb0467a492107-7]

In MLCS2k2 language, this version corresponds to “MLCS2k2 v0.07 rv19-early-smix vectors”

List of Built-in Bandpasses

bessell

Name	Description	Reference	Data URL	Retrieved
‘bessellux’	Representation of Johnson-Cousins UBVRI system	[R98e64ca268e7-B90]
‘bessellb’	Representation of Johnson-Cousins UBVRI system	[R98e64ca268e7-B90]
‘bessellv’	Representation of Johnson-Cousins UBVRI system	[R98e64ca268e7-B90]
‘bessellr’	Representation of Johnson-Cousins UBVRI system	[R98e64ca268e7-B90]
‘besselli’	Representation of Johnson-Cousins UBVRI system	[R98e64ca268e7-B90]

[R98e64ca268e7-B90]

(1, 2, 3, 4, 5) Bessell 1990, Table 2

(Source code, png, hires.png, pdf)

snls3-landolt

Name	Description	Reference	Data URL	Retrieved
‘standard::u’	Bessell bandpasses shifted as in JLA analysis	[R98e64ca268e7-B14a]		a 13 February 2017
‘standard::b’	Bessell bandpasses shifted as in JLA analysis	[R98e64ca268e7-B14a]		a 13 February 2017
‘standard::v’	Bessell bandpasses shifted as in JLA analysis	[R98e64ca268e7-B14a]		a 13 February 2017
‘standard::r’	Bessell bandpasses shifted as in JLA analysis	[R98e64ca268e7-B14a]		a 13 February 2017
‘standard::i’	Bessell bandpasses shifted as in JLA analysis	[R98e64ca268e7-B14a]		a 13 February 2017

[R98e64ca268e7-B14a]

(1, 2, 3, 4, 5) Betoule et al. (2014), Footnote 21

(Source code, png, hires.png, pdf)

des

Name	Description	Reference	Data URL	Retrieved
‘desg’	Dark Energy Camera grizy filter set at airmass 1.3			22 March 2013
‘desr’	Dark Energy Camera grizy filter set at airmass 1.3			22 March 2013
‘desi’	Dark Energy Camera grizy filter set at airmass 1.3			22 March 2013
‘desz’	Dark Energy Camera grizy filter set at airmass 1.3			22 March 2013
‘desy’	Dark Energy Camera grizy filter set at airmass 1.3			22 March 2013

(Source code, png, hires.png, pdf)

sdss

Name	Description	Reference	Data URL	Retrieved
‘sdssu’	SDSS 2.5m imager at airmass 1.3 (including atmosphere), normalized	[R98e64ca268e7-D10]
‘sdssg’	SDSS 2.5m imager at airmass 1.3 (including atmosphere), normalized	[R98e64ca268e7-D10]
‘sdssr’	SDSS 2.5m imager at airmass 1.3 (including atmosphere), normalized	[R98e64ca268e7-D10]
‘sdssi’	SDSS 2.5m imager at airmass 1.3 (including atmosphere), normalized	[R98e64ca268e7-D10]
‘sdssz’	SDSS 2.5m imager at airmass 1.3 (including atmosphere), normalized	[R98e64ca268e7-D10]

[R98e64ca268e7-D10]

(1, 2, 3, 4, 5) Doi et al. 2010, Table 4

(Source code, png, hires.png, pdf)

acs

Name	Description	Reference	Data URL	Retrieved
‘f435w’	Hubble Space Telescope ACS WFC filters		b	direct download
‘f475w’	Hubble Space Telescope ACS WFC filters		b	direct download
‘f555w’	Hubble Space Telescope ACS WFC filters		b	direct download
‘f606w’	Hubble Space Telescope ACS WFC filters		b	direct download
‘f625w’	Hubble Space Telescope ACS WFC filters		b	direct download
‘f775w’	Hubble Space Telescope ACS WFC filters		b	direct download
‘f850lp’	Hubble Space Telescope ACS WFC filters		b	direct download

(Source code, png, hires.png, pdf)

nicmos-nic2

Name	Description	Reference	Data URL	Retrieved
‘nicf110w’	Hubble Space Telescope NICMOS2 filters		c	05 Aug 2014
‘nicf160w’	Hubble Space Telescope NICMOS2 filters		c	05 Aug 2014

(Source code, png, hires.png, pdf)

wfc3-ir

Name	Description	Reference	Data URL	Retrieved
‘f098m’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f105w’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f110w’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f125w’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f127m’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f139m’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f140w’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f153m’	Hubble Space Telescope WFC3 IR filters		d	direct download
‘f160w’	Hubble Space Telescope WFC3 IR filters		d	direct download

(Source code, png, hires.png, pdf)

wfc3-uvis

Name	Description	Reference	Data URL	Retrieved
‘f218w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f225w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f275w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f300x’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f336w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f350lp’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f390w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f689m’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f763m’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f845m’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘f438w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘uvf475w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘uvf555w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘uvf606w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘uvf625w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘uvf775w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘uvf814w’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download
‘uvf850lp’	Hubble Space Telescope WFC3 UVIS filters (CCD 2)		d	direct download

(Source code, png, hires.png, pdf)

kepler

Name	Description	Reference	Data URL	Retrieved
‘kepler’	Bandpass for the Kepler spacecraft		e	direct download

(Source code, png, hires.png, pdf)

csp

Name	Description	Reference	Data URL	Retrieved
‘cspb’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘csphs’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘csphd’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspjs’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspjd’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspv3009’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspv3014’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspv9844’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspys’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspyd’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspg’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspi’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspk’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspr’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017
‘cspu’	Carnegie Supernova Project filters (Swope+DuPont Telescopes) updated 6 Oct 2016		f	8 Feb 2017

(Source code, png, hires.png, pdf)

jwst-nircam

Name	Description	Reference	Data URL	Retrieved
‘f070w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f090w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f115w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f150w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f200w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f277w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f356w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f444w’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f140m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f162m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f182m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f210m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f250m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f300m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f335m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f360m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f410m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f430m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f460m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014
‘f480m’	James Webb Space Telescope NIRCAM Wide+Medium filters		g	09 Sep 2014

(Source code, png, hires.png, pdf)

jwst-miri

Name	Description	Reference	Data URL	Retrieved
‘f560w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f770w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f1000w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f1130w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f1280w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f1500w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f1800w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f2100w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017
‘f2550w’	James Webb Space Telescope MIRI filters		h	16 Feb 2017

(Source code, png, hires.png, pdf)

jwst-miri-tophat

Name	Description	Reference	Data URL	Retrieved
‘f1065c’	James Webb Space Telescope MIRI filters (idealized tophat)		i	09 Sep 2014
‘f1140c’	James Webb Space Telescope MIRI filters (idealized tophat)		i	09 Sep 2014
‘f1550c’	James Webb Space Telescope MIRI filters (idealized tophat)		i	09 Sep 2014
‘f2300c’	James Webb Space Telescope MIRI filters (idealized tophat)		i	09 Sep 2014

(Source code, png, hires.png, pdf)

lsst

Name	Description	Reference	Data URL	Retrieved
‘lsstu’	LSST baseline total throughputs, v1.1.		j	16 Nov 2016
‘lsstg’	LSST baseline total throughputs, v1.1.		j	16 Nov 2016
‘lsstr’	LSST baseline total throughputs, v1.1.		j	16 Nov 2016
‘lssti’	LSST baseline total throughputs, v1.1.		j	16 Nov 2016
‘lsstz’	LSST baseline total throughputs, v1.1.		j	16 Nov 2016
‘lssty’	LSST baseline total throughputs, v1.1.		j	16 Nov 2016

(Source code, png, hires.png, pdf)

keplercam

Name	Description	Reference	Data URL	Retrieved
‘keplercam::us’	Keplercam transmissions as used in JLA		a	13 Feb 2017
‘keplercam::b’	Keplercam transmissions as used in JLA		a	13 Feb 2017
‘keplercam::v’	Keplercam transmissions as used in JLA		a	13 Feb 2017
‘keplercam::r’	Keplercam transmissions as used in JLA		a	13 Feb 2017
‘keplercam::i’	Keplercam transmissions as used in JLA		a	13 Feb 2017

(Source code, png, hires.png, pdf)

4shooter2

Name	Description	Reference	Data URL	Retrieved
‘4shooter2::us’	4Shooter filters as used in JLA		a	13 Feb 2017
‘4shooter2::b’	4Shooter filters as used in JLA		a	13 Feb 2017
‘4shooter2::v’	4Shooter filters as used in JLA		a	13 Feb 2017
‘4shooter2::r’	4Shooter filters as used in JLA		a	13 Feb 2017
‘4shooter2::i’	4Shooter filters as used in JLA		a	13 Feb 2017

(Source code, png, hires.png, pdf)

megacampsf

These are radially-variable bandpasses. To get a Bandpass at a given radius, use band = sncosmo.get_bandpass('megacampsf::g', 13.0)

(Source code, png, hires.png, pdf)

List of Built-in Magnitude Systems

Name	Description	Subclass	Spectrum Source
‘jla1’	JLA1 magnitude system based on BD+17 STIS v003 spectrum	CompositeMagSystem	a
‘ab’	Source of 3631 Jy has magnitude 0 in all bands	ABMagSystem
‘vega’	Vega (alpha lyrae) has magnitude 0 in all bands.	SpectralMagSystem	b
‘bd17’	BD+17d4708 has magnitude 0 in all bands.	SpectralMagSystem	b
‘csp’	Carnegie Supernova Project magnitude system.	CompositeMagSystem	c
‘ab-b12’	Betoule et al (2012) calibration of SDSS system.	CompositeMagSystem	a

Reference / API

More…

Version History

Note: SNCosmo uses Semantic Versioning for its version numbers. Specifically, this means that code written for sncosmo v1.0 will continue to work with any v1.x version. However, exact results may differ between versions in the 1.x series. (For example, due to changes in integration method.)

v1.7.0 (2019-02-02)

• Add SNEMO2, SNEMO7, SNEMO15 source models from Saunders et al. (2018) to built-ins.

v1.6.0 (2018-04-27)

• Add Hounsell et al. (2017) SALT2 model to built-ins.
• Add remote_timeout configuration option.
• Build system: remove build-time dependency on astropy helpers.
• Bugfixes:
  • Correctly delete empty files created when a download fails.
  • Use pseudo-inverse when inverting covariance matrix for increased stability.
  • Fix an issue with pickling on Cython 0.26+.
  • Fixed problem where data['fluxcov'] was unintentionally being modified in-place when passed to fit_lc.
  • Fixed problem where 'fluxcov' not recognized as a valid name for covariance column in data in fit_lc.

v1.5.0 (2017-04-20)

This is a major new release. The highlight is really close compatibility of the SALT2 model and fitting procedure with snfit, the “official” SALT2 fitter.

• SALT2Source: Internal interpolation scheme of SALT2Source updated to match snfit implementation exactly. Test suite now tests against snfit implementation.

• fit_lc():

  • Handling of model covariance updated to match that of snfit: model covariance is fixed for each fit and fit is repeated until convergence.
  • New arguments phase_range and wave_range. If given, data outside this range will be discarded after an initial fit and additional fits will be performed until convergence. With phase_range=(-15., 45.) and wave_range=(3000., 7000.), behavior approximates that of snfit with default arguments.
  • Added support for covariance in photometric data measurements, and this covariance is used in fit_lc() if present. Covariance is stored as a 'fluxcov' column in the table of measurements.
  • Result includes two new attributes: data_mask, a boolean array indicating which rows in the input data were used in the final fit (since multiple fits might be performed), and nfit, the number of fits performed.
  • New argument warn can be set to False to turn off warnings about dropping bands outside model wavelength range.

• read_lc():

  • Added support for reading snfit-format “covmat” files into a table of photometry:

    >>> data = read_lc('filename', format='salt2', read_covmat=True)
    >>> data['Fluxcov'].shape == (len(data), len(data))
    True
    

  • New keyword argument expand_bands. When True, the returned band column will contain Bandpass objects instead of strings. (Strings converted to bandpass objects using sncosmo.get_bandpass().) This is particularly useful for position-dependent bandpasses in the salt2 file format, such as megacampsf: read_lc() reads the position from the header and feeds the position to get_bandpass() to get a Bandpass object for the correct position.

• Built-in bandpasses and magnitude systems: Many new built-in bandpasses and magnitude systems.

• Configuration: The environment variable SNCOSMO_DATA_DIR can be used to set the path to the data directory. If set, it takes precedence over the data_dir variable in the configuration file ($HOME/.astropy/config/sncosmo.cfg).

v1.4.0 (2016-11-16)

• SFD98Map and get_ebv_from_map deprecated in favor of separate package sfdmap which has vastly improved performance (200x faster) for the typical case of scalar coordinates in ICRS frame.
• animate_source() deprecated. This is a “fun extra” that is difficult to test and no longer seems to work.
• Cython implementation of extinction functions has been factored out into a separate Python module called extinction, which is now a dependency.
• Model.bandflux() and Source.bandflux() now integrate on a fixed wavelength grid of 5 angstroms regardless of the wavelength grid of the bandpass. This will result in small differences in results from previous sncosmo versions.
• The internal (publicly undocumented) Spectrum class now acts more like Model; in particular, its bandflux() method now behaves the same way. As Spectrum backs SpectralMagSystem, this makes the integration of models and zeropoint spectra more consistent.
• Experimental (non-public) support for aliases for bandpasses, such as 'SDSS::g' for 'sdssg'.
• Sources now use cubic rather than quadratic spline interpolation internally.
• Model.source_peakmag() and Model.set_source_peakmag() added as convenience functions for Model.source.peakmag() and Model.source.set_peakmag() respectively.
• [Bugfix] Fixed missing import of math module in mcmc_lc() when using the priors keyword. [Backported to v1.3.1] [#143]

v1.3.0 (2016-06-30)

This is mostly a bugfix release, but it also drops support for Python 2.6. Python 2.7 is now the minimum supported Python version.

• Updates for compatibility with AstroPy 1.2.

• The registry now handles subclasses more robustly. For example, if magsys is an instance of SpectralMagSystem, the following used to fail:

  sncosmo.register(magsys, 'name')
  sncosmo.get_magsystem('name')
  

  Now this works. [#132]

• [Bugfix] SALT2Source had a bug under Python 3 (only) yielding drastically wrong fluxes. Python 2 was not affected. [#138]

v1.2.0 (2015-12-01)

• [API change] Registry functions moved to the top-level namespace, as follows:

  • sncosmo.registry.register() -> sncosmo.register()
  • sncosmo.registry.register_loader() -> sncosmo.register_loader()
  • sncosmo.registry.retrieve() -> deprecated, use class-specific functions such as sncosmo.get_bandpass().

  The old import paths will still work for backwards compatibility.

• nest_lc() now uses the nestle module under the hood. A new keyword method is available which selects different sampling methods implemented by nestle. The new methods provide potential efficiency gains.

• The MLCS2k2 model is now available as a built-in Source, with the name 'mlcs2k2'.

• Bandpasses from the Carnegie Supernova Project added to built-ins.

• In realize_lcs(), a new scatter keyword makes adding noise optional.

• [Bugfix] Fix built-in Bessell bandpass definitions, which were wrong by a term proportional to inverse wavelength. This was due to misinterpretation of the trasmission units. [backported to v1.1.1] [#111]

v1.1.0 (2015-08-12)

This is a mostly bugfix release with more solid support for Python 3.

• Added Model.color() method.
• Remove loglmax from result of nest_lc(), which was not officially documented or supported. Use np.max(res.logl) instead.
• Fixed bug that caused non-reproducible behavior in nest_lc() even when numpy.random.seed() was called directly beforehand. [#102]
• Fixed file I/O problems on Python 3 related to string encoding. [#83, #85]
• Fixed problem with SDSS bandpasses being stored as integers internally, preventing them from being used with models with dust. [#100, #101]
• Fixed problem where built-in source name and version strings were being dropped. [#82]
• Minor doc fixes.

v1.0.0 (2015-02-23)

• [API change] The API of mcmc_lc has changed significantly

  (the function was marked experimental in previous release).

• [Deprecation] In result of fit_lc, res.cov_names changed to res.vparam_names.
• [Deprecation] In result of nest_lc, res.param_names changed to res.vparam_names. This is for compatibility between the results of fit_lc and nest_lc. [#30]
• [Deprecation] Deprecate flatten keyword argument in fit_lc() in favor of explicit use of flatten_result() function.
• Many new built-in models.
• Many new built-in bandpasses.
• New remote data fetching system.
• SALT2 model covariance available via Model.bandfluxcov() method and modelcov=True keyword argument passed to fit_lc.
• New simulation function, zdist, generates a distribution of redshifts given a volumetric rate function and cosmology.
• New simulation function, realize_lcs, simulates light curve data given a model, parameters, and observations.
• Add color-related keyword arguments to plot_lc().
• Add tighten_ylim keyword argument to plot_lc().
• Add chisq() function and use internally in fit_lc().
• Add SFD98Map class for dealing with SFD (1998) dust maps persistently so that the underlying FITS files are opened only once.
• Update get_ebv_from_map() to work with new SkyCoord class in astropy.coordinates available in astropy v0.3 onward. Previously, this function did not work with astropy v0.4.x (where older coordinates classes had been removed).
• Update to new configuration system available in astropy v0.4 onward. This makes this release incompatible with astropy versions less than 0.4.
• Now compatible with Python 3.
• Increased test coverage.
• Numerous minor bugfixes.

v0.4.0 (2014-03-26)

This is non-backwards-compatible release, due to changes in the way models are defined. These changes were made after feedback on the initial design.

The most major change is a new central class Model used throughout the pacakge. A Model instance encompasses a Source and zero or more PropagationEffect instances. This is so that different source models (e.g., SALT2 or spectral time series models) can be combined with arbitrary dust models. The best way to think about this is Source and PropagationEffect define the rest-frame behavior of a SN and dust, and a Model puts these together to determine the observer-frame behavior.

• New classes:
  • sncosmo.Model: new main container class
  • sncosmo.Source: replaces existing Model
  • sncosmo.TimeSeriesSource: replaces existing TimeSeriesModel
  • sncosmo.StretchSource: replaces existing StretchModel
  • sncosmo.SALT2Source: replaces existing SALT2Model
  • sncosmo.PropagationEffect
  • sncosmo.CCM89Dust
  • sncosmo.OD94Dust
  • sncosmo.F99Dust
• New public functions:
  • sncosmo.read_griddata_ascii: Read file with phase wave flux rows
  • sncosmo.read_griddata_fits
  • sncosmo.write_griddata_fits
  • sncosmo.nest_lc: Nested sampling parameter estimation of SN model
  • sncosmo.simulate_vol (EXPERIMENTAL): simulation convenience function.
• Built-ins:
  • updated SALT2 model URLs
  • added SALT2 version 2.4 (Betoule et al 2014)
• Improvements to sncosmo.plot_lc: flexibility and layout
• Many bugfixes

v0.3.0 (2013-11-07)

This is a release with mostly bugfixes but a few new features, designed to be backwards compatible with v0.2.0 ahead of API changes coming in the next version.

• New Functions:

  • sncosmo.get_ebv_from_map: E(B-V) at given coordinates from SFD map.
  • sncosmo.read_snana_ascii: Read SNANA ascii format files.
  • sncosmo.read_snana_fits: Read SNANA FITS format files.
  • sncosmo.read_snana_simlib: Read SNANA ascii “SIMLIB” files.

• registry is now case-independent. All of the following now work:

  sncosmo.get_magsystem('AB')
  sncosmo.get_magsystem('Ab')
  sncsomo.get_magsystem('ab')
  

• Photometric data can be unordered in time. Internally, the data are sorted before being used in fitting and typing.

• Numerous bugfixes.

v0.2.0 (2013-08-20)

• Added SN 2011fe Nearby Supernova Factory data to built-in models as '2011fe'

• Previously “experimental” functions now included:

  • sncosmo.fit_lc (previously sncosmo.fit_model)
  • sncosmo.read_lc (previously sncosmo.readlc)
  • sncosmo.write_lc (previously sncosmo.writelc)
  • sncosmo.plot_lc (previously sncosmo.plotlc)

• New functions:

  • sncosmo.load_example_data: Example photometric data.
  • sncosmo.mcmc_lc: Markov Chain Monte Carlo parameter estimation.
  • sncosmo.animate_model: Model animation using matplotlib.animation.

• Fitting: sncosmo.fit_lc now uses the iminuit package for minimization by default. This requires the iminuit package to be installed, but the old minimizer (from scipy) can still be used by setting the keyword method='l-bfgs-b'.

• Plotting: Ability to plot model synthetic photometry without observed data, using the syntax:

  >>> sncosmo.plot_lc(model=model, bands=['band1', 'band2'])
  

• Photometric data format: Photometric data format is now more flexible, allowing various names for table columns.

v0.1.0 (2013-07-15)

Initial release.

About SNCosmo

Package Features

• SN models: Synthesize supernova spectra and photometry from SN models.
• Fitting and sampling: Functions for fitting and sampling SN model parameters given photometric light curve data.
• Dust laws: Fast implementations of several commonly used extinction laws; can be used to construct SN models that include dust.
• I/O: Convenience functions for reading and writing peculiar data formats used in other packages and getting dust values from SFD (1998) maps.
• Built-in supernova models such as SALT2, MLCS2k2, Hsiao, Nugent, PSNID, SNANA and Whalen models, as well as a variety of built-in bandpasses and magnitude systems.
• Extensible: New models, bandpasses, and magnitude systems can be defined, using an object-oriented interface.

Relation to other SN cosmology software

There are several other publicly available software packages for supernova cosmology. These include (but are not limited to) snfit (SALT fitter), SNANA and SNooPy (or snpy).

• snfit and SNANA both provide functionality overlapping with this package to some extent. The key difference is that these packages provide several (or many) executable applications, but do not provide an API for writing new programs building on the functionality they provide. This package, in contrast, provides no executables; instead it is a library of functions and classes designed to provide the building blocks commonly used in many aspects of SN analyses.
• SNooPy (or snpy) is also a Python library for SN analysis, but with a (mostly) different feature set. SNCosmo is based on spectral timeseries models whereas SNooPy is more focussed on models of light curves in given bands.

The name SNCosmo

A natural choice, “snpy”, was already taken (SNooPy) so I tried to be a little more descriptive. The package is really specific to supernova cosmology, as it doesn’t cover other types of supernova science (radiative transfer simulations for instance). Hence “sncosmo”.

Contributors

Alphabetical by last name:

• Stephen Bailey
• Kyle Barbary
• Tom Barclay
• Rahul Biswas
• Matt Craig
• Ulrich Feindt
• Brian Friesen
• Danny Goldstein
• Saurabh Jha
• Steve Rodney
• Caroline Sofiatti
• Rollin C. Thomas
• Michael Wood-Vasey

Contributing

Overview

SNCosmo follows the same general development workflow as astropy and many other open-source software projects. The astropy development workflow page documents the process in some detail. While you should indeed read that page, it can seem a bit overwhelming at first. So, we present here a rough outline of the process, and try to explain the reasoning behind it.

The process is centered around git and GitHub, so you need to know how to use basic git commands and also have a GitHub account. There is a “blessed” copy of the repository at https://github.com/sncosmo/sncosmo. Individual contributors make changes to their own copy (or “fork” or “clone” in git parlance) of the repository, e.g., https://github.com/kbarbary/sncosmo, then ask that their changes be merged into the “blessed” copy via a Pull Request (PR) on GitHub. A maintainer (currently Kyle) will review the changes in the PR, possibly ask for alterations, and then eventually merge the change.

This seems overly complex at first glance, but there are two main benefits to this process: (1) Anyone is free to try out any crazy change they want and share it with the world on their own GitHub account, without affecting the “blessed” repository, and (2) Any proposed changes are reviewed and discussed by at least one person (the maintainer) before being merged in.

Detailed steps

Do once:

1. Hit the “fork” button in the upper right hand corner of the https://github.com/sncosmo/sncosmo page. This creates a clone of the repository on your personal github account.

2. Get it onto your computer (replace username with your GitHub username):

   git clone git@github.com:username/sncosmo.git
   

3. Add the “blessed” version as a remote:

   git remote add upstream git@github.com:sncosmo/sncosmo.git
   

   This will allow you to update your version to reflect new changes to the blessed repository that others have made).

4. Check that everything is OK:

   $ git remote -v
   origin    git@github.com:username/sncosmo.git (fetch)
   origin    git@github.com:username/sncosmo.git (push)
   upstream    git@github.com:sncosmo/sncosmo.git (fetch)
   upstream    git@github.com:sncosmo/sncosmo.git (push)
   

   You can call the remotes anything you want. “origin” and “upstream” have no intrinsic meaning for git; they’re just nicknames. The astropy documentation calls them “your-github-username” and “astropy” respectively.

Every time you want to make a contribution:

1. Ensure that the clone of the repository on your local machine is up-to-date with the latest upstream changes by doing git fetch upstream. This updates your local “remote tracking branch”, called upstream/master.

2. Create a “topic branch” for the change you want to make. If you plan to make enhancements to the simulation code, name the branch something like “simulation-enhancements”:

   git branch simulation-enhancements upstream/master
   

   (upstream/master is where the branch branches off from.)

3. Move to the branch you just created:

   git checkout simulation-enhancements
   

4. Make changes, ensure that they work, etc. Make commits as you go.

5. Once you’re happy with the state of your branch, push it to your GitHub account for the world to see:

   git push origin simulation-enhancements
   

6. Create a PR: Go to your copy on github (https://github.com/username/sncosmo) select the branch you just pushed in the upper left-ish of the page, and hit the green button next to it. (It has a mouse-over “compare, review, create a pull request”)

What happens when the upstream branch is updated?

Suppose that you are following the above workflow: you created a topic branch simulation-enhancements and made a few commits on that branch. You now want to create a pull request, but there’s a problem: while you were working, more commmits were added to the upstream/master branch on GitHub. The history of your branch has now diverged from the main development branch! What to do?

1. Fetch the changes made to the upstream branch on so that you can deal with the changes locally:

   git fetch upstream
   

   This will update your local branch upstream/master (and any other upstream branches) to the match the state of the upstream branch on GitHub. It doesn’t do any merging or resolving, it just makes the new changes to upstream/master visible locally.

2. There are two options for this next step: merge or rebase with the latter being preferred for this purpose. Assuming you are on your branch simulation-enhancements, you could do git merge upstream/master. This would create a merge commit that merges the diverged histories back together. This works, but it can end up creating a confusing commit history, particularly if you repeat this process several times while working on your new branch. Instead, you can do:

   git rebase upstream/master
   

   This actually rewrites your commits to make it look like they started from where upstream/master now is, rather than where it was when you started work on your simulation-enhancements branch. Your branch will have the exact same contents as if you had used git merge, but the history will be different than it would have been if you had merged. In particular, there is no merge commit created, because the history has been rewritten so that your branch starts where upstream/master ends, and there is no divergent history to resolve. This means you can rebase again and again without creating a convoluted history full of merges back and forth between the branches.

Trying out new ideas

git branches are the best way to try out new ideas for code modifications or additions. You don’t even have to tell anyone about your bad ideas, since branches are local! They only become world visible when you push them to GitHub. If, after making several commits, you decide that your new branch simulation-enhancements sucks, you can just create a new branch starting from upstream/master again. If it is a really terrible idea you never want to see again, you can delete it by doing git branch -D simulation-enhancements.

Obviously this isn’t a complete guide to git, but hopefully it jump-starts the git learning process.

Developer’s documentation: release procedure

These are notes mainly for the one person that manages releases. Yes, this could be more automated, but it isn’t done very often, and involves some human verification.

• Update docs/history.rst with a summary of the new version’s changes.
• Bump version in setup.py.
• Check copyright year in docs/conf.py.
• Build package and docs and check that docs look good.
• Commit.
• git clean -dfx
• setup.py sdist
• Check that the tarball in dist/ can be unpacked and that setup.py test succeeds. Bonus: create a fresh conda environment (or virtual environment) with minimal requirements and install and test in that.
• setup.py register
• setup.py sdist upload

Post-release steps:

• If not a bugfix release, create a feature branch. For example, git branch v1.1.x.
• Tag the release. For example, git tag v1.1.0.
• On master, bump version in setup.py to the next development version and add the next development version to docs/whatsnew.rst.
• Commit.
• Push repo changes to GitHub. For example: git push upstream master v1.1.x v1.1.0.

Docs and conda

• On readthedocs.org, set the new feature branch to “active”.
• To trigger new conda build, edit version number in requirements.txt in https://github.com/astropy/conda-builder-affiliated and submit a pull request.
• Once conda build succeeds, make the new feature branch the default on readthedocs.org.

• Check out the source code: https://github.com/sncosmo/sncosmo
• Report bugs, request features: https://github.com/sncosmo/sncosmo/issues
• User & developer mailing list: https://groups.google.com/forum/#!forum/sncosmo