# Frequently Asked/Anticipated Questions¶

Contents

- Frequently Asked/Anticipated Questions
- General
- How should I cite CoSMoMVPA?
- What is the history of CoSMoMVPA?
- What are the main features?
- What does CoSMoMVPA
*not*provide? - Does it integrate with PyMVPA?
- Does it run on GNU Octave?
- How fast does it run?
- What should I use as input for MVPA?
- Who are the developers of CoSMoMVPA?
- Which classifiers are available?
- Which platforms does it support?
- What future features can be expected?
- How can I contact the developers directly?
- Is there a mailinglist?
- Why do you encourage balanced partitions?

- How do I …
- Find the correspondence between voxel indices in AFNI and feature indices in CoSMoMVPA
- Get ECoG data in a CoSMoMVPA struct
- Get temporal data in a CoSMoMVPA struct
- Run group analysis
- Make an intersection mask across participants
- Compute for a group of participants who were scanned with MRI the overlap of their masks
- Run group analysis on time-by-time generalization measures
- Use LIBSVM
- Use surface-based mapping with a low-resolution output surface
- Correct for multiple comparisons
- Do cross-modal decoding across three modalities
- Compute classification accuracies manually
- Merge surface data from two hemispheres
- Visualize and store multiple fMRI volumes
- Average along features in a neighborhood
- Select a time interval in an MEEG dataset
- Select a particular channel type in an MEEG dataset
- Use only a subset of channels for my analysis?
- Should I Fisher-transform correlation values?
- Average samples in a deterministic manner?
- Select only a subset of features in a neighborhood?
- Use multiple-comparison correction for a time course?
- Classify different groups of participants (such as patients versus controls)?
- When running an MEEG searchlight, have the same channels in the output dataset as in the input dataset?
- Save MEEG data when I get the error “value for fdim channel label is not supported”?
- Run a 2 x 2 within-subject ANOVA?
- Use a FieldTrip source dataset that uses a ‘fake’ channel structure
- Run cosmo_montecarlo_cluster_stat on a cluster with multiple nodes

- General

## General¶

### How should I cite CoSMoMVPA?¶

Please cite [OCH16]:

Oosterhof, N. N., Connolly, A. C., and Haxby, J. V. (2016). CoSMoMVPA: multi-modal multivariate pattern analysis of neuroimaging data in Matlab / GNU Octave. Frontiers in Neuroinformatics, doi:10.3389/fninf.2016.00027.

BiBTeX record:

```
@article{OCH16,
author = {Oosterhof, Nikolaas N and Connolly, Andrew C and Haxby, James V},
title = {{CoSMoMVPA: multi-modal multivariate pattern analysis of neuroimaging data in Matlab / GNU Octave}},
journal = {Frontiers in Neuroinformatics},
doi = {10.3389/fninf.2016.00027},
year = {2016}
}
```

### What is the history of CoSMoMVPA?¶

CoSMoMVPA was started when Gunnar Blohm and Sara Fabri invited the developers (ACC and NNO) to speak at the

2013 Summer School in Computational Sensory-Motor Neuroscience( CoSMo 2013 workshop ) about multivariate pattern analysis methods.In a few days they wrote the basic functionality including the dataset structure (inspired by PyMVPA), basic input/output support for the NIFTI format, correlation analysis, several classifiers, cross-validation, and representational similarity analysis. They also decided to use restructured text to build a website, and wrote a custom build script to generate documentation for the website, including multiple versions of Matlab files to generate both exercises files (with some code to be filled in) and solution files (with all the code).

Their plan was to let participants write a basic MVPA toolbox in two days (see the exercises). This was, with hindsight, a tad ambitious.

The initial components in CoSMoMVPA still stand, but quite a few things have changed in the meantime. CoSMoMVPA has added support for various file formats, including surface-based data and MEEG data. It also supports a wider range of analyses. Finally, there is a new set of exercises, less aimed at writing your own toolbox, but more at understanding and implementing basic MVPA techniques using CoSMoMVPA.

For recent changes, see the Changelog.

### What are the main features?¶

CoSMoMVPA provides:

A simple, yet powerful, data structure that treats fMRI and MEEG data both as first-class citizens.

Simple,light-weight, andmodularfunctions.Implementations of

all common MVPA analysesthrough measures, such as:

- correlation split-half
- representational similarity
- crossvalidation with classifiers
- generalization over time
Neighborhoods in various spaces, including

volumetric and surface-based (fMRI)

time, frequency, sensors, and source elements (MEEG)

all combinations of the above, for example:

- voxel x time (volumetric fMRI)
- node x time (surface-based fMRI)
- time x sensor (MEEG)
- time x frequency x sensor (MEEG)
- time x source element (MEEG)
- time x frequency x source element (MEEG)
where each of the above measures can be used with a neighborhood to run searchlights in all the above spaces.

Support for a wide variety of image formats, including:

proper Monte Carlo cluster-based multiple comparison correction (example), using either Threshold-Free Cluster Enhancement or traditional cluster-size based Monte Carlo simulations, in all the supported neighborhood spaces..

various runnable example scripts and exerices, describing both on how to perform certain types of analyses (i.e., from a user perspective), and on how typical MVP analyses can be implemented (from a programmer persective).

### What does CoSMoMVPA *not* provide?¶

It does not provide (and probably never will):

- Preprocessing of data. It assumed that the data has been preprocessed using other packages (such as AFNI, SPM, or FieldTrip). For fMRI analyses, in most use-case scenarios, it is preferable to use response estimates from a General Linear Model.
- Implementations of complicated analyses (such as hyperalignment, nested cross validation, recursive feature elimination). If you want to do these, consider using PyMVPA.
- A Graphical User Interface (GUI). First, it’s a lot of work to build such a thing. Second, writing the code to perform the analyses could be considered as more instructive: it requires one to actually
thinkabout the analysis, rather than just clicking on buttons.- Pretty visualization of fMRI data. Although there is basic functionality for showing slices of fMRI data (through
`cosmo_plot_slices`

, for better visualization we suggest to use either your preferred fMRI analysis package, or MRIcron.Also, it does not make coffee for you.

### Does it integrate with PyMVPA?¶

Yes. Dataset structures are pretty much identical in CoSMoMVPA (PyMVPA provided inspiration for the data structures). The`mvpa2/datasets/cosmo.py`

module in PyMVPA provides input and output support between CoSMoMVPA and PyMVPA datasets and neighborhoods. This means that, for example, searchlights defined in CoSMoMVPA can be run in PyMVPA (possibly benefitting from its multi-threaded implementation), and the results converted back to CoSMoMVPA format.

### Does it run on GNU Octave?¶

Almost all functionality runs in Octave 3.8, including unit tests through MOxUnit, but there may be parts that function with limitations:

- Unit tests require MOxUnit (because xUnit uses object-oriented features not supported by Octave), and doc-tests are not supported in MOxUnit (because Octave does not provide
`evalc_`

).- BrainVoyager support through NeuroElf is not supported, because NeuroElf uses object-oriented features not supported by Octave.

### How fast does it run?¶

CoSMoMVPA is not a speed monster, but on our hardware (Macbook Pro early 2012) a searchlight using typical fMRI data takes one minute for simple analyses (correlation split-half), and a few minutes for more advanced analyses (classifier with cross-validation). The naive Bayes searchlights takes a few seconds for whole-brain fMRI per classification fold. Analyses on regions of interest are typically completed in seconds.

### What should I use as input for MVPA?¶

We suggest the following:

fMRI options:

- Apply the GLM for each run seperately, with separate predictors for each condition. Each run is a chunk, and each experimental condition is a target. You can use either beta estimates or t-statistics.
- Split the data in halves (even and odd) and apply the GLM to each of these (i.e. treat the experiment as consisting of two ‘runs’). In this case there are two chunks, and the same number of unique targets as there are experimental conditions.
MEEG options:

Preprocess the data (e.g. bandpassing, artifact rejection, downsampling).

For chunk assignment, either:

- Assign chunks based on the run number.
- If the data in different trials in the same run can be assumed to be independent, use unique chunk values for each trial. If that gives you a lot of chunks (which makes crossvalidation slow), use cosmo chunkize.

### Who are the developers of CoSMoMVPA?¶

Currently the developers are Nikolaas N. Oosterhof and Andrew C. Connolly. In the code you may find their initials (`NNO`

,`ACC`

) in commented header sections.

### Which classifiers are available?¶

- Naive Bayes (cosmo classify naive bayes).
- Nearest neighbor (cosmo classify nn).
- k-nearest neighbor (cosmo classify knn).
- Support Vector Machine (cosmo classify svm); requires the Matlab
`stats`

or`bioinfo`

toolbox, or LIBSVM.- Linear Discriminant Analysis (cosmo classify lda).

### Which platforms does it support?¶

It has been tested with Windows, Mac and Linux.

### What future features can be expected?¶

Time permitting, there are some features that may be added in the future:

- MEEG tutorial.
- Snippets of useful code no the website.

### How can I contact the developers directly?¶

Please send an email to a@c or b@d, where a=andrew.c.connolly, b=nikolaas.oosterhof, c=dartmouth.edu, d=unitn.it.

### Is there a mailinglist?¶

There is the CoSMoMVPA Google group.

### Why do you encourage balanced partitions?¶

‘I noticed that CoSMoMVPA heavily ‘encourages’ balanced class distributions (with equal number of samples in each class), and recommends to remove data to balance; why?’

TL;DR: it’s much simpler and you don’t lose much by enforcing balanced partitions.

Longer version:the main reason for encouraging (almost enforcing) balanced partitions is a combination of simplicity and avoiding mistakes with ‘above chance’ classification. It is considerably simple when chance is 1/c, with c the number of classes; in particular, this simplifies second level (group) analysis and allows for a relatively quick Monte Carlo based multiple-comparison correction through sign-swapping (as implemented in cosmo montecarlo cluster stat). In addition, most paradigms use quite balanced designs anyway, so you do not loose much trials by enforcing balancing. If not using all trials would be a concern, one can re-use the same samples multiple times in different cross-validation folds through cosmo_balance_partitions with the ‘nrepeats’ or ‘nmin’ arguments.

## How do I …¶

- Find the correspondence between voxel indices in AFNI and feature indices in CoSMoMVPA
- Get ECoG data in a CoSMoMVPA struct
- Get temporal data in a CoSMoMVPA struct
- Run group analysis
- Make an intersection mask across participants
- Compute for a group of participants who were scanned with MRI the overlap of their masks
- Run group analysis on time-by-time generalization measures
- Use LIBSVM
- Use surface-based mapping with a low-resolution output surface
- Correct for multiple comparisons
- Do cross-modal decoding across three modalities
- Compute classification accuracies manually
- Merge surface data from two hemispheres
- Visualize and store multiple fMRI volumes
- Average along features in a neighborhood
- Select a time interval in an MEEG dataset
- Select a particular channel type in an MEEG dataset
- Use only a subset of channels for my analysis?
- Should I Fisher-transform correlation values?
- Average samples in a deterministic manner?
- Select only a subset of features in a neighborhood?
- Use multiple-comparison correction for a time course?
- Classify different groups of participants (such as patients versus controls)?
- When running an MEEG searchlight, have the same channels in the output dataset as in the input dataset?
- Save MEEG data when I get the error “value for fdim channel label is not supported”?
- Run a 2 x 2 within-subject ANOVA?
- Use a FieldTrip source dataset that uses a ‘fake’ channel structure
- Run cosmo_montecarlo_cluster_stat on a cluster with multiple nodes

### Find the correspondence between voxel indices in AFNI and feature indices in CoSMoMVPA¶

In the AFNI GUI, you can view voxel indices by right-clicking on the coordinate field in the very left-top corner. Note that:

`ds.fa.i`

,`ds.fa.j`

, and`ds.fa.k`

are base-`1`

whereas AFNI uses base-`0`

. So, to convert AFNI’s`ijk`

-indices to CoSMoMVPA’s, add`1`

to AFNI’s coordinates.- CoSMoMVPA’s coordinates are valid for LPI-orientations, meaning that the first dimension is from left (lower values) to right (higher values), the second dimension is from posterior (lower values) to anterior (higher values), and the third dimension from inferior (lower values) to superior (higher values). To convert a dataset to LPI-orientation using AFNI, do:
3dresample -orient LPI -inset my_data+orig -prefix my_data_lpi+orig.

### Get ECoG data in a CoSMoMVPA struct¶

‘I have eCog data in a 3D array (`channels x time x trials`

). How can I get this in a CoSMoMVPA struct?’Let’s assume there is data with those characteristics; here we generate synthetic data for illustration. This data has 7 time points, 3 channels, and 10 trials:

time_axis=-.1:.1:.5; channel_axis={'chan1','chan2','chan3'}; n_trials=10; n_time=numel(time_axis); n_channels=numel(channel_axis); data=randn([n_channels,n_time,n_trials]); % Gaussian random dataBecause in CoSMoMVPA, samples are in the first dimension, the order of the dimensions have to be shifted so that the

`trials`

(samples) dimension comes first:data_samples_first_dim=shiftdim(data,2);Now the data can be flattened to a CoSMoMVPA data struct with:

ds=cosmo_flatten(data_samples_first_dim,... {'chan','time'},... {channel_axis,time_axis});Combinations of

`chan`

and`time`

are the features of the dataset. For example, to see how informative the data is for different time points (across all channels), one could define a cosmo interval neighborhood for the time dimension and run a searchlight.If one would only want to consider the

`chan`

dimension as features, and consider`time`

as a sample dimension, do:ds_time_in_sample_dim=cosmo_dim_transpose(ds,{'time'},1);When the data is in this form, one can analyse how well information generalizes over time .

### Get temporal data in a CoSMoMVPA struct¶

‘Using MEEG dataset, using custom written software I have precomputed RSA correlations across channels for a group of subjects for each timepoints; the result is`data`

matrix of size`17x300`

, corresponding to`subjects x time`

. How can I get this in a CoSMoMVPA dataset struct, and use cosmo montecarlo cluster stat for multiple comparison correction?’We will generate some (random) data with these characteristics:

% generate pseudo-random data data=cosmo_rand(17,300); % set the time (in seconds) for each column % Here, the first time point is 200ms pre-stimulus % and each time step is 2ms. The last time point % is at 398 ms time_axis=-.2:.002:.398;To get the data in a dataset structure, a similar approach is followed as in another FAQ entry (Get ECoG data in a CoSMoMVPA struct) - but note that there is only a time axis here to use as a feature dimension:

ds=cosmo_flatten(data,{'time'},{time_axis},2)Clustering with cosmo montecarlo cluster stat requires (as usual) a clustering neighborhood computed by cosmo cluster neighborhood:

% cluster neighborhood over time points cl_nh=cosmo_cluster_neighborhood(ds);To use cosmo montecarlo cluster stat, it is required to set targets and chunks. In this case there is a single sample per subject, which is reflected in

`.sa.targets`

and`.sa.chunks`

.n_subjects=size(data,1); ds.sa.targets=ones(n_subjects,1); ds.sa.chunks=(1:n_subjects)';To run cosmo montecarlo cluster stat it is required to set the number of iterations and (for a one-sample t-test) the expected mean under the null hypothesis.

opt=struct(); % use at least 10000 iterations for publication-quality analyses opt.niter=10000; % expected mean under null hypothesis. % For this example (pre-computed RSA correlation values) % the expected mean is zero. opt.h0_mean=0; % compute z-scores after TFCE correction tfce_z_ds=cosmo_montecarlo_cluster_stat(ds,cl_nh,opt);Note that clusters are computed across the time dimension, so if a cluster survives between (say) 100 and 150 ms, one

cannotinfer that at 100 ms there is significant information present that explains the non-zero correlations. Instead, the inferences can only be made at the cluster level, i.e. there is evidence for significant information at a cluster of time points. To be able to make inferences at the individual time point level, use a cluster neighborhood that does not connect clusters across the time dimension:% cluster neighborhood not connecting time points cl_nh_not_over_time=cosmo_cluster_neighborhood(ds,'time',false);in which case a significant feature at (say) 100 ms can directly be interpreted as evidence for information being present at 100 ms. However, such a test is less sensitive than a neighborhood that connects features across time.

### Run group analysis¶

‘I ran an fMRI searchlight analysis using cosmo searchlight with cosmo spherical neighborhood and got a result map for a single participant. Now I want to repeat this for my other participants, and then do a group analysis. It is my understanding that I should use cosmo montecarlo cluster stat, but the documentation refers to cosmo cluster neighborhood.’Indeed cosmo cluster neighborhood should be used with cosmo montecarlo cluster stat, because that neighborhood function returns a neighborhood structure indicating which features (voxels) are next to each other. This is different from, say, a spherical neighborhood with a radius of 3 voxels.

(Technically cosmo cluster neighborhood, when applied on a typical fMRI dataset (that is, without other feature dimensions), returns by default a neighborhood that is equivalent to a spherical neighborhood with a radius between

`sqrt(3)`

and`2`

, meaning that under the assumption of isotropocy, voxels are neighbors if they share at least a vertex (corner).Also, cosmo cluster neighborhood works on other types of datasets, including surface-based fMRI, timelocked MEEG, and time-frequency MEEG.)

Assuming that

`result`

was constructed as above, a group analysis using Threshold-Free Cluster Enhancement and using 1000 permutations can now by done quite easily. For a one-sample t-test (one sample per participant, it is however required to specify the mean under the null hypothesis. When the cosmo correlation measure or cosmo target dsm corr measure is used, this is typically zero, whereas for cosmo crossvalidation measure, this is typically 1 divided by the number of classes (e.g.`0.25`

for 4-class discrimination).% one-sample t-test against 0 % (for representational similarity analysis) h0_mean=0; % number of null iterations. % values of at least 10,000 are recommended for publication-quality niter=1000; % % Set neighborhood for clustering cluster_nbrhood=cosmo_cluster_neighborhood(result); stat_map=cosmo_montecarlo_cluster_stat(result, cluster_nbrhood,... 'niter', niter,... 'h0_mean', h0_mean);

### Make an intersection mask across participants¶

‘I ran my analysis for multiple participants, each with their own mask. Now I want to do group analysis, but combining the data using cosmo stack gives an error because feature attributes do not match. How can I combine data across participants?

If `ds_cell`

is a cell so that `ds_cell{k}`

contains the dataset from the `k`

-th participant, an intersection (based on features common across participants) can be computed though:

[idxs,ds_intersect_cell]=cosmo_mask_dim_intersect(ds_cell);

For (second level) group analysis, in general, it is a good idea to assign `chunks`

(if not done already) and `targets`

. The general approach to setting chunks is by indicating that data from different participants is assumed to be independent; for setting targets, see the help of cosmo stat:

n_subjects=numel(ds_intersect_cell); for subject_i=1:n_subjects % get dataset ds=ds_intersect_cell{subject_i]; % assign chunks n_samples=size(ds.samples,1); ds.sa.chunks=ones(nsamples,1)*subject_i; % assign targets % Your code comes here; see cosmo_stat on how to assign % targets depending on subsequent analysis % (one-sample or two-sample t-test, or one-way or % repeated-measures ANOVA). % store results ds_intersect_cell{subject_i}=ds; end

The the resulting datasets can be combined through:

ds_all=cosmo_stack(ds_intersect_cell,1);

Note: The above line may give an error `non-unique elements in fa.X`

, with `X`

some feature attribute such as `center_ids`

or `radius`

. This is to be expected if the datasets are the result from another analysis, such as cosmo searchlight. In that case, the data can be combined using:

ds_all=cosmo_stack(ds_intersect_cell,1,'drop_nonunique');

### Compute for a group of participants who were scanned with MRI the overlap of their masks¶

‘I analyzed data for individual fMRI participants that are all in a common MNI space, but with individual masks. When using cosmo mask dim intersect I seem to lose about a third of the voxels present in each participant. How can I visualize which voxels are not shared across participants?’

The following code illustrates how this can be done, using synthetic data.

keep_ratio=0.95; n_subj=10; % simulate data for all subjects with their masks mostly overlapping ds_cell=cell(n_subj,1); for k=1:n_subj ds_full=cosmo_synthetic_dataset('seed',0,'size','big'); n_features=size(ds_full.samples,2); keep=cosmo_randperm(n_features,round(n_features*keep_ratio)); ds=cosmo_slice(ds_full,keep,2); ds_cell{k}=ds; end % do simple intersection mask [idxs,ds_cell_common]=cosmo_mask_dim_intersect(ds_cell); ds_common=cosmo_stack(ds_cell_common); fprintf('Ratio in common: %d / %d\n',size(ds_common.samples,2),n_features); % see how often each voxel was in the mask for each participant for k=1:n_subj ds_single_volume=cosmo_slice(ds_cell{k},1); ds_single_volume.samples(:)=1; ni=cosmo_map2fmri(ds_single_volume,'-nii'); img=ni.img; if k==1 img_sum=zeros(size(img)); end img_sum=img_sum+img; end % convert to a ratio between 0 and 1 (for each voxel) ni.img=img_sum / n_subj; % convert to dataset structure ds_ratio=cosmo_fmri_dataset(ni); % the ds_ratio dataset can be visualized as shown here, % or stored to disc using cosmo_map2fmri cosmo_plot_slices(ds_ratio)

### Run group analysis on time-by-time generalization measures¶

‘I used cosmo dim generalization measure on MEEG data to get time-by-time generalization results. How do I run group analysis with cluster correction (cosmo montecarlo cluster stat) on these?’

Let’s assume the data from all subjects is stored in a cell

`ds_cell`

, with`ds_cell{k}`

is a dataset struct with the output from cosmo dim generalization measure for the`k`

-th subject. Each dataset has the`train_time`

and`test_time`

attribute in the sample dimension, and they have to be moved to the feature dimension to use cosmo montecarlo cluster stat):n_subjects=numel(ds_cell); ds_cell_tr=cell(n_subjects,1); for k=1:n_subjects ds_cell_tr{k}=cosmo_dim_transpose(ds_cell{k},... {'train_time','test_time'},2); endThen, it is almost always necessary to set the

`.sa.targets`

and`.sa.chunks`

attributes. The former refers to conditions; the latter to (in this case) the subject. See cosmo montecarlo cluster stat how to define these generally for various tests. In the simple case of a one-sample t-test, these would be set as follows:for k=1:n_subjects % here we assume a single output (sample) for each % searchlight. For statistical analysis later, where % we want to do a one-sample t-test, we set % .sa.targets to 1 (any constant value will do) and % .sa.chunks to the subject number. % nsamples=size(result.samples,1); % % Notes: % - these values can also be set after the analysis is run, % although that may be more error-prone % - for other statistical tests, such as one-way ANOVA, % repeated-measures ANOVA, paired-sample t-test and % two-sample t-tests, chunks and targets have to be % set differently. See the documentation of % cosmo_montecarlo_cluster_stat for details. ds_cell_tr{k}.sa.chunks=k; % k-th subject ds_cell_tr{k}.sa.targets=1; % all same condition endand results would be joined into a single dataset by:

ds_tr=cosmo_stack(ds_cell_tr);Now group analysis can proceed using cosmo montecarlo cluster stat as described in faq_run_group_analysis.

To convert the output (say

`stat_map`

) from cosmo montecarlo cluster stat to matrix form (time by time), do[data, labels, values]=cosmo_unflatten(stat_map,2); data_mat=squeeze(data);

### Use LIBSVM¶

Download LIBSVM, then in Matlab or Octave, do

cd libsvm; % change this to the directory where you put LIBSVM cd matlab % go to matlab sub-directory make % compile libsvm mex functions; requires a working compiler rmpath(pwd) % } ensure directory is on top addpath(pwd) % } of the search path % verify it worked. cosmo_check_external('libsvm'); % should not give an error

If the

`make`

command failed, make sure you are in the LIBSVM’s`matlab`

subdirectory, and that you have a working compiler under Matlab or compiler under Octave.If you want to store the path, you can also do

`savepath`

so that the next time you start Matlab or Octave, the correct path is used.

Matlab also provides an SVM implementation in the

`stats`

(and possible other) toolboxes, and the naming of the training functions are not compatible with LIBSVM. Thus, you can use either Matlab’s SVM or LIBSVM, but not both at the same time. To select which SVM implementation is used, set the Matlab search path so that either LIBSVM is on top (comes earlier; to use LIBSVM) or at the bottom (comes later; to use Matlab’s SVM).

### Use surface-based mapping with a low-resolution output surface¶

The typical use case scenarion is using FreeSurfer pial and white matter surfaces that are resampled to standard topology using MapIcosahedron. Then, the high-resolution surfaces are used to define which voxels are associated with each searchlight, whereas the low-resolution surface is used as centers for the searchlight. The former aims to result in more precise selection of voxels; the latter in fewer centers, and thus reduced execution time for the searchlight.

In this scenario, it is required that the vertices in low-resolution surface are a subset of the pair-wise averages of vertices in the high-resolution pial and white surfaces. A typical use case is using standard topologies from AFNI’s MapIcosahedron, where the high resolution surfaces are constructed using X linear divisionsof the triangles of an icosahedron, the low-resolution surface is constructed with Y linear divisions, and Y<X and X is an integer multiple of Y.

The pymvpa2-prep-afni-surf script (part of PyMVPA, which is required to run it) provides exactly this functionality. It will resample the surfaces to various resolutions, ranging from 4 linear divisions (162 nodes per hemisphere) to 128 linear divisions (163842 nodes per hemisphere) in steps of powers of two. It will also generate intermediate surfaces (pair-wise avarages of the nodes of the pial and white matter surfaes), and merge left (`lh`

) and right (`rh`

) hemisphere into a single hemisphere (`mh`

). The merged surfaces have the advantages that the searchlight has to be run only once to get results for both hemispheres.

### Correct for multiple comparisons¶

For second level (group analysis), cosmo montecarlo cluster stat provides cluster-based correction.

There are three *components* in this, and they can be crossed arbitrarily:

- clustering method: either ‘standard’ fixed-uncorrected thresholding, or using Threshold-Free Cluster Enhancement (TFCE). The latter is the default in CoSMoMVPA, as it has been proposed it has several advantages (Nichols & Smith, 2009, Neuroimage), including:

- “TFCE gives generally better sensitivity than other methods over a wide range of test signal shapes and SNR values”.
- avoids “the need to define the initial cluster-forming threshold (e.g., threshold the raw t-statistic image at t>2.5)”.
- avoids the issue that “initial hard thresholding introduces instability in the overall processing chain; small variations in the data around the threshold level can have a large effect on the final output.”
- deals properly with different smoothing levels of the data.
- makes it easier to “directly interpret the meaning of (what may ideally be) separable sub-clusters or local maxima within very extended clusters”.
- is less affected by nonstationarity.
support for any type of modality that CoSMoMVPA supports, including:

- fMRI volumetric, e.g. voxel, or voxel x time
- fMRI surface-based, e.g. node, or node x time
- MEEG time x channel (both in sensor and source space)
- MEEG time x channel x frequency (both in sensor and source space)
In the case of multiple dimensions (such as time x channel x frequency) it is possible to cluster only over a subset of the dimensions. For example, a time x channel x frequency dataset can be clustered over all dimensions, or clustered over channel x frequency (which allows for more precise temporal inferences), or over channel x time (for more precise frequency inferences).

support for either standard permutation test, or the method by Stelzer et al. (2012). To use the Stelzer approach, the user has to generate null datasets themselves. cosmo randomize targets can be used for this, but requires using a for-loop to generate multiple null datasets.

Because components 1-3 can be crossed arbitrarily, it allows for multiple comparison correction for a wide variety of applications.

- Notes:
- There is no function for within-subject significance testing; through cosmo_randomize_targets and a
`for`

-loop the user can do that themselves. - There is also univariate cosmo_stat for one-sample and two-sample t-tests, and one-way and repeated measures ANOVA.

- There is no function for within-subject significance testing; through cosmo_randomize_targets and a

### Do cross-modal decoding across three modalities¶

‘I have a dataset with three modalities (visual, auditory, tactile) and would like to do both within-modality and cross-modality decoding. How should I proceed?’

cosmo nchoosek partitioner can deal with two modalities quite easily, but three or more is not directly supported. Instead you can slice the dataset multiple times to select the samples of interest, as in this example:

% generate synthetic example data with 3 modalities, 8 chunks n_modalities=3; ds=cosmo_synthetic_dataset('nchunks',n_modalities*8,'sigma',1); ds.sa.modality=mod(ds.sa.chunks,n_modalities)+1; % in range 1:n_modalities ds.sa.chunks=ceil(ds.sa.chunks/n_modalities); % 8 chunks % allocate space for output accuracies=NaN(n_modalities); % do all combinations for training and test modalities for train_modality=1:n_modalities for test_modality=1:n_modalities % select data in train and test modality msk=cosmo_match(ds.sa.modality,[train_modality test_modality]); ds_sel=cosmo_slice(ds,msk); if train_modality==test_modality % within-modality cross-validation partitions=cosmo_nchoosek_partitioner(ds_sel,1); else % cross-modality cross-validation partitions=cosmo_nchoosek_partitioner(ds_sel,1,... 'modality',test_modality); end opt=struct(); opt.partitions=partitions; opt.classifier=@cosmo_classify_lda; measure=@cosmo_crossvalidation_measure; % Run the measure. % % (alternatively a searchlight can be used, through % % ds_searchlight_result=cosmo_searchlight(ds,nh,measure,opt); % % where nh is a neighborhood) ds_result=measure(ds_sel,opt); accuracies(train_modality,test_modality)=ds_result.samples; end end

### Compute classification accuracies manually¶

‘I computed predictions using cosmo crossvalidation measure with the `output`

option set to `'predictions'`

, but now I would like to compute the classification accuracies afterwards. How can I do that?’

If `pred_ds`

is the dataset with predictions, then accuracies can be computed by:

acc_ds=cosmo_slice(pred_ds,1); % take single slice acc_ds.sa=struct(); % reset sample attributes acc_ds.samples=nanmean(bsxfun(@eq,pred_ds.samples,pred_ds.sa.targets));

### Merge surface data from two hemispheres¶

‘I have surface-based data from two hemispheres. How can I combine these into a single surface dataset structure?’

In the following example, `ds_left`

and `ds_right`

are two dataset structs (for example, obtained through cosmo surface dataset) from the left and right hemisphere. They can be combined into a single dataset as follows:

% generate synthetic left and right hemisphere data % (this is just example data for illustration) ds_left=cosmo_synthetic_dataset('type','surface','seed',1); ds_right=cosmo_synthetic_dataset('type','surface','seed',2); % Set the number of vertices of the left surface. % If the surface is sparse (it does not have data for all nodes), it *may* % be necessary to adjust this value manually. In that case, consider to: % % - compute the number of vertices, if it is a standardized surface from % MapIcosahedron. If the ld parameter was set to 64, then the number of % vertices is 10*64^2+2=40962. % - get the number of vertices using: % [v,f]=surfing_read('left_surface.asc'); % nverts=max(size(v)); % [unused, index]=cosmo_dim_find(ds_left, 'node_indices'); nverts_left=max(ds_left.a.fdim.values{index}); % get the offset to set the feature attribute index later offset_left=numel(ds_left.a.fdim.values{index}); % update node indices to support indexing data from two hemispheres node_indices=[ds_left.a.fdim.values{index}, ... nverts_left+ds_right.a.fdim.values{index}]; ds_left.a.fdim.values{index}=node_indices; ds_right.a.fdim.values{index}=node_indices; % update node indices for right hemisphere assert(all(ds_left.fa.node_indices<=offset_left)); % safety check ds_right.fa.node_indices=ds_right.fa.node_indices+offset_left; % merge hemisphes ds_left_right=cosmo_stack({ds_left,ds_right},2);

The resulting dataset `ds_left_right`

can be stored in a file using cosmo map2surface.

### Visualize and store multiple fMRI volumes¶

‘I have an fMRI volumetric dataset with three volumes. cosmo plot slices gives an error when trying to visualize this dataset. How can I visualize the volumes and store them as NIFTI files?’

In this example, `ds`

is a dataset structure with three volumes. To visualize and store the third volume, do:

ds3=cosmo_slice(ds,3); % select third sample (volume) cosmo_plot_slices(ds3); % visualization in CoSMoMVPA cosmo_map2fmri(ds3,'volume3.nii'); % for visualization in % other programs

Note that several fMRI visualization packages can also visualize fMRI datasets with multiple volumes. To store all volumes in a single NIFTI file, simply do:

cosmo_map2fmri(ds,'all_volumes.nii');

For example, MRIcron can be used to visualize each of the volumes in the resulting NIFTI file.

### Average along features in a neighborhood¶

‘I have defined a neighborhood for my dataset, and now I would like to compute the average across features at each searchlight location. How can I do that?’

To average along features, you can define a new measure:

function ds_mean=my_averaging_measure(ds) % compute the average along features, and copies .sa % and .a.sdim, if present ds_mean=struct(); ds_mean.samples=mean(ds.samples,2); if cosmo_isfield(ds,'sa') ds_mean.sa=ds.sa; end if cosmo_isfield(ds,'a.sdim') ds_mean.a.sdim=ds.a.sdim; end

This measure can then be used directly with cosmo searchlight. Note that the output has the same number of samples as the input dataset (i.e., `.samples`

has the same number of rows); depending on how the neighborhood is defined, the number of features in the output dataset may either be the same as or different from the input dataset.

It is also possible to define such a measure *inline*; for example, if the input dataset has `.sa`

but not `.a.sdim`

(this is the most common case; but exceptions are outputs from cosmo dim generalization measure and cosmo dissimilarity matrix measure), then the following computes the average across voxels at each neighborhood location:

% tiny dataset: 6 voxels ds=cosmo_synthetic_dataset(); % tiny radius: 1 voxel nh=cosmo_spherical_neighborhood(ds,'radius',1); % define averaging measure inline my_averageing_measure=@(x,opt) cosmo_structjoin(... 'samples',mean(x.samples,2),... 'sa',x.sa); % compute average in each neighorhood location across features (voxels) ds_mean=cosmo_searchlight(ds,nh,my_averageing_measure);

The line approach may be a bit slower than defining a separate function, but the speed difference is usually not substantial.

### Select a time interval in an MEEG dataset¶

To select only a particular time range, consider the following:

% for this example, generate synthetic data ds=cosmo_synthetic_dataset('type','meeg',... 'size','huge'); % Select time points between 50 and 300 ms time_selector=@(t) t>=.04999 & t<=0.3001; time_msk=cosmo_dim_match(ds,'time',time_selector=@); % % (alternative to the above is % slice dataset ds_time=cosmo_slice(ds,time_msk,2); % Optionally prune the dataset % - without cosmo_dim_prune: the output of map2meeg(ds_time) will % have all the time points of the original dataset; data for % missing time points will be set to zero or NaN. % - with cosmo_dim_prune: the output of map2meeg(ds_time) will % not contain the removed time points. ds_time=cosmo_dim_prune(ds_time);

Note that in the example above, the time_selector variable is a function handle that is used to specify a time range. The minimal and maximum values of 0.04999 and 0.30001 (instead of 0.05 and 0.30) are used to address potential tiny rounding errors, as it may be the case that the time points stored in the datasets are not exact multiples of 1/1000. For example, in the following expression:

(((0:.1:1)/70)*70)-(0:.1:1)

one might expect a vector of only zeros because of the identities a==(a+b)-b and a==(a/b)/b (for finite, non-zero values of a and b), yet both Matlab and GNU Octave return:

ans = 1.0e-15 * Columns 1 through 6 0 0 0 -0.0555 0 0 Columns 7 through 11 0 0.1110 0 0 0

See also: cosmo dim match, cosmo slice, cosmo dim prune.

### Select a particular channel type in an MEEG dataset¶

To select channels of a particular type, consider the following:

% for this example, generate synthetic data ds=cosmo_synthetic_dataset('type','meeg',... 'size','huge'); %% % select channels % (the output of chantypes in the command below % indicates which channel types can be selected) [chantypes,senstypes]=cosmo_meeg_chantype(ds); % in this example, select MEG planar combined channel chan_type_of_interest='meg_planar_combined'; chan_indices=find(cosmo_match(chantypes,... chan_type_of_interest)); % define channel mask chan_msk=cosmo_match(ds.fa.chan,chan_indices); % slice the dataset ds_chan=cosmo_slice(ds,chan_msk,2); % Optionally prune the dataset % - without cosmo_dim_prune: the output of map2meeg(ds_chan) will % have all the channels of the original dataset; data for % missing channels will be set to zero or NaN. % - with cosmo_dim_prune: the output of running map2meeg(ds_chan) will % not contain the removed channels. ds_chan=cosmo_dim_prune(ds_chan); % to really remove channels

See also: cosmo meeg chantype, cosmo slice, cosmo match, cosmo dim prune.

### Use only a subset of channels for my analysis?¶

‘I have time-frequency MEEG data for all channels in the layout. How can I select data from a region of interest, in other words use only a subset? Also, how can I compute the response averaged over the selected channels?’

First, in order to select a subset of channels of interest, consider the following:

% generate some example data ds=cosmo_synthetic_dataset('size','huge','type','timefreq',... 'ntargets',1,'nchunks',1); % define channels of interest channels_of_interest={'MEG0941','MEG0942',... 'MEG1831','MEG1832',... }; % define mask msk=cosmo_dim_match(ds,'chan', channels_of_interest); fprintf('Selecting %.1f%% of the channels\n',100*mean(msk)); % select data ds=cosmo_slice(ds,msk,2); % prune dataset ds=cosmo_dim_prune(ds);

Then, to compute the average for each time point and frequency bin:

% average for each time point and frequency bin seperately other_dims={'time','freq'}; feature_averager=@(x)mean(x,2); ds_avg=cosmo_fx(ds,feature_averager,other_dims,2); % remove the channel dimension ds_avg=cosmo_dim_remove(ds_avg,'chan');

In this case the data is in time-frequency space. If there is only one sample (i.e. .samples is a row vector), it can be visualized as a time by frequency matrix:

% safety check assert(size(ds_avg.samples,1)==1,'only a single sample is supported'); % unflatten [data,labels,values]=cosmo_unflatten(ds_avg); assert(isequal(labels,{'freq';'time'})); % safety check % make it a matrix freq_time=squeeze(data); % visualize data label_step=5; freq_values=values{1}; n_freq=numel(freq_values); keep_freq=1:label_step:n_freq; time_values=values{2}; n_time=numel(time_values); keep_time=1:label_step:n_time; imagesc(freq_time,[-3 3]); colorbar(); set(gca,'XTickLabel',time_values(keep_time),'XTick',keep_time); set(gca,'YTickLabel',freq_values(keep_freq),'YTick',keep_freq);

### Should I Fisher-transform correlation values?¶

‘When using cosmo correlation measure, cosmo target dsm corr measure, or cosmo dissimilarity matrix measure, should I transform the data, for example using Fisher transformation (`atanh`

)?’

Assuming you would like to do second-level (group) anaysis:

- cosmo correlation measure: the correlations are already Fisher transformed (the transformation can be changed and/or disabled using the
`post_corr_func`

option) - cosmo target dsm corr measure: correlation values are not Fisher transformed. You could consider applying
`atanh`

to the`.samples`

output - cosmo dissimilarity matrix measure: the
`.samples`

field contains, by default, one minus the correlation, and thus its range is the interval`[0, 2]`

. Fisher-transformation should not be used, as values greater than 1 are transformed to complex (non-real) numbers.

### Average samples in a deterministic manner?¶

‘When using cosmo average samples multiple times on the same dataset, I get different avaraged datasets. How can I get the same result every time?’

cosmo average samples has a `seed`

option; you can use any integer for a seed. For example, if `ds`

is a dataset, then

ds_avg=cosmo_average_samples(ds,'seed',1);

will pseudo-deterministically select the same samples upon repeated evaluations of the expression, and thus return the same result

### Select only a subset of features in a neighborhood?¶

‘When using cosmo spherical neighborhood with the `radius`

option, some elements in `.neighborhood`

have only a few elements. How can I exclude them from subsequent searchlight analyses?

Although cosmo slice does not support neighborhood structures (yet), consider the following example using tiny example datasets and neighborhoods:

min_count=4; % in most use cases this is more than 4 ds=cosmo_synthetic_dataset(); nh=cosmo_spherical_neighborhood(ds,'radius',1); keep_msk=nh.fa.nvoxels>=min_count; nh.fa=cosmo_slice(nh.fa,keep_msk,2,'struct'); nh.neighbors=cosmo_slice(nh.neighbors,keep_msk); cosmo_check_neighborhood(nh,ds); % sanity check

Alternatively, cosmo spherical neighborhood (and cosmo surficial neighborhood) can be used with a ‘count’ argument - it keeps the number of elements across neighborhoods more constant.

### Use multiple-comparison correction for a time course?¶

‘I have a matrix of beta values (Nsubjects x Ntimepoints) for each predictor and I want to test for each timepoint (i.e. each column) if the mean beta is significantly different from zero. I ran a t-test but I wonder if I should test for multiple comparisons as well. What would be the best way to test for significance here?’

You could use multiple comparison correction using Threshold-Free Cluster Enhancement with a temporal neighborhood. Suppose your data is in the following data matrix:

% generate gaussian example data with no signal; n_subjects=15; time_axis=-.1:.01:.5; n_time=numel(time_axis); data=randn(n_subjects,n_time);

then the first step is to put this data in a dataset structure:

% make a dataset ds=struct(); ds.samples=data; % insert time dimension ds=cosmo_dim_insert(ds,2,0,{'time'},{time_axis},{1:numel(time_axis)});

You would have to decide how to form clusters, i.e. whether you want to make inferences at the individual time point level, or at the cluster-of-timepoints level. Then use cosmo montecarlo cluster stat to estimate significance.

% Make a temporal neighborhood for clustering % % In the following, if % % allow_clustering_over_time=true % then clusters can form over multiple time points. This makes the analysis % more sensitive if there is a true effect in the data over multiple % consecutive time points. However, when allow_clustering_over_time=true % then one cannot make inferences about a specific time point (i.e. % "the effect was significant at t=100ms"), only about a cluster (i.e % "the effect was significant in a cluster stretching between t=50 and % t=150 ms"). If, on the ohter hand, % % allow_clustering_over_time=false % % then inferences can be made at the individual time point level, at the % expensive of sensitivity of detecting any significant effect if there is % a true effect that spans multiple consecutive time points allow_clustering_over_time=false; % true or false % define the neighborhood nh_cl=cosmo_cluster_neighborhood(ds,'time',allow_clustering_over_time); % set subject information n_samples=size(ds.samples,1); ds.sa.chunks=(1:n_samples)'; % all subjects are independent ds.sa.targets=ones(n_samples,1); % one-sample t-test % set clustering opt=struct(); opt.h0_mean=0; % expected mean against which t-test is run opt.niter=10000; % 10,000 is recommdended for publication-quality analyses % run TFCE Monte Carlo multiple comparison correction % in the output map, z-scores above 1.65 (for one-tailed) or 1.96 (for % two-tailed) tests are significant ds_tfce=cosmo_montecarlo_cluster_stat(ds,nh_cl,opt);

### Classify different groups of participants (such as patients versus controls)?¶

‘I have participants in three groups, patients1, patients2, and controls. How can I see where in the brain people these groups can be discriminated above chance level?’

To do so, consider a standard searchlight using cosmo searchlight with cosmo_crossvalidation_measure. Group membership is set in

`.sa.targets`

. Since all participants are assumed to be independent, values in`.sa.chunks`

are all unique.Correcting for multiple comparisons is more difficult. Since it is not possible to do a ‘standard’ t-test (two groups) or ANOVA F-test (three or more groups), instead generate null datasets manually by randomly permuting the

`.sa.targets`

labels. Then use these null datasets directly as input for cosmo montecarlo cluster stat without computing a feature statistic.Consider the following example:

% set number of groups and number of participants in each group ngroups=3; nchunks=10; % generate example dataset with some signal that discriminates % the participants ds=cosmo_synthetic_dataset('ntargets',ngroups,'nchunks',nchunks); % since all participants are independent, all chunks are set to % unique values ds.sa.chunks(:)=1:(ngroups*nchunks); % define partitions fold_count=50; test_count=1; partitions=cosmo_independent_samples_partitioner(ds,... 'fold_count',fold_count,... 'test_count',test_count); % define neighborhood radius_in_voxels=1; % typical is 3 voxels nh=cosmo_spherical_neighborhood(ds,'radius',radius_in_voxels); % run searchlight on original data opt=struct(); opt.classifier=@cosmo_classify_lda; opt.partitions=partitions; result=cosmo_searchlight(ds,nh,... @cosmo_crossvalidation_measure,opt); % generate null dataset niter=100; % at least 1000 is iterations is recommended, 10000 is better ds_null_cell=cell(niter,1); for iter=1:niter ds_null=ds; ds_null.sa.targets=cosmo_randomize_targets(ds_null); % update partitions opt.partitions=cosmo_independent_samples_partitioner(ds_null,... 'fold_count',fold_count,... 'test_count',test_count); null_result=cosmo_searchlight(ds_null,nh,... @cosmo_crossvalidation_measure,opt); ds_null_cell{iter}=null_result; end %% % Since partitions are balanced, chance level % is the inverse of the number of groups. For example, % with 4 groups, chance level is 1/4 = 0.25 = 25%. chance_level=1/ngroups; tfce_dh=0.01; % should be sufficient for accuracies opt=struct(); opt.h0_mean=chance_level; opt.dh=tfce_dh; opt.feature_stat='none'; opt.null=ds_null_cell; cl_nh=cosmo_cluster_neighborhood(result); %% compute TFCE map with z-scores % z-scores above 1.65 are signficant at p=0.05 one-tailed. tfce_map-cosmo_montecarlo_cluster_stat(result,cl_nh,opt);

### When running an MEEG searchlight, have the same channels in the output dataset as in the input dataset?¶

‘When I run an MEEG searchlight over channels, the searchlight dataset map has more channels than the input dataset. Is this normal?’

This is quite possible because the cosmo meeg chan neighborhood uses, by default, the layout that best fits the dataset. The output from the searchlight has then all channels from this layout, rather than only the channels from the input dataset. This is done so that in individual particpants different channels can be removed in the preprocessing step, while group analysis on the output maps can be done on maps that have the same channels for all participants.

If you want to use only the channels from the input dataset (say `ds`

) you can set the `label`

option to ‘dataset’. See the following example, where `chan_nh`

has only channels from the input dataset.

chan_nh=cosmo_meeg_chan_neighborhood(ds,'count',5,'label','dataset')

### Save MEEG data when I get the error “value for fdim channel label is not supported”?¶

‘When I try to export MEEG searchlight maps with channel information as MEEG data using `cosmo_map2meeg(ds,'-dattimef')`

, I get the error “value for fdim channel label is not supported”? Also I am unable to visualize the data in FieldTrip. Any idea how to fix this?’

This is probably caused by a wrong feature dimension order when crossing the neighborhood with cosmo cross neighborhood. The FieldTrip convention for the order is `'chan','time'`

(for time-locked data) or `'chan','time','freq'`

(for time-frequency data). (As of 16 December 2016, a warning has been added if a non-standard dimension order is detected).

It is possible to change the feature dimension order afterwards. First, the feature dimension order for a dataset struct `ds`

can be displayed by running:

disp(ds.a.fdim.labels)

If the order is, for example, `'freq', 'time', 'chan'`

then the channel dimension should be moved from position 3 to position 1 to become `'chan','freq','time'`

. To move the channel dimension, first remove the dimension, than insert it at another position, as follows:

label_to_move='chan'; target_pos=1; [ds,attr,values]=cosmo_dim_remove(ds,{label_to_move}); ds=cosmo_dim_insert(ds,2,target_pos,{label_to_move},values,attr);

### Run a 2 x 2 within-subject ANOVA?¶

‘I would like to run a 2 x 2 ANOVA over participants where both factors are within-participant (also known as repeated-measures ANOVA). Can I use CoSMoMVPA to get the main effects and interaction statistics?’

You can, but currently not directly: it involves a bit of manual work. The key thing is that in a 2 x 2 repeated measures ANOVA, main effects and interaction can all be expressed as one-sample t-tests. Say that for a single participant there are four conditions: A1, A2, B1, and B2. In CoSMoMVPA we would express this as a dataset structure `ds`

with `ds.samples`

of size `4 x NF`

, where `NF`

is the number of features. Now compute:

% main effect A vs B: A1+A2-B1-B2. dsAvsB=cosmo_slice(ds,1); dsAvsB.samples=ds.samples(1,:)+ds.samples(2,:)-ds.samples(3,:)-ds.samples(4,:) % main effect 1 vs 2: A1-A2+B1-B2 ds1VS2=cosmo_slice(ds,1); ds1VS2 =ds.samples(1,:)-ds.samples(2,:)+ds.samples(3,:)-ds.samples(4,:) % interaction: A1-A2-B1+B2 dsinteraction=cosmo_slice(ds,1); dsinteraction=ds.samples(1,:)-ds.samples(2,:)-ds.samples(3,:)+ds.samples(4,:)

Repeat the process for each participant. For each analysis of interest (two main effects and the interaction) separately, follow the process of a one-sample t-test as explained elsewhere in the FAQ: stack the dataset from the participants using cosmo stack, assign `.sa.chunks`

to be all unique, assign `.sa.targets`

to be all the same, and then use cosmo stat (for feature-wise stats with no correction for multiple correction) or cosmo montecarlo cluster stat (for correction with multiple comparisons).

Note the advantage of a (signed) t-test over an (always positive) F value: the t value tells you which way the main effect or interaction goes, whereas the F value does not tell this.

### Use a FieldTrip source dataset that uses a ‘fake’ channel structure¶

‘I use an analysis pipeline where MEEG source data in MNI space is represented (faked) as a sensor-like structure [such as done by some at CIMeC, Trento; or University of Salzberg, Austria]. In particular, the FieldTrip dataset structure is ``src_ft = “

label: {2982x1 cell} dimord: 'chan_freq_time' freq: [1x25 double] time: [1x15 double] powspctrm: [2982x25x15 double] cfg: [1x1 struct]

where the labels are strings from `'1'`

to `'2972'`

. These labels refer to positions in source space using a `template_grid =`

xgrid: [-8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8] ygrid: [-11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8] zgrid: [-7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8 9] dim: [17 20 17] pos: [5780x3 double] unit: 'cm' inside: [5780x1 logical] cfg: [1x1 struct]

where there are 2972 positions in the .inside field that are equal to `true`

representing the voxels in the brain. How can I use these dataset structures in CoSMoMVPA?’

The `src_ft`

struct can be converted to a dataset structure using

src_ds=cosmo_meeg_dataset(src_ft);

but it uses channel labels (representing voxels) for which the positions are not known (and thus, neighborhoods cannot be used). To add the position information, you can use the following helper function

function ds=convert_ds_mni_grid(ds,template_grid) % Converts dataset with 'fake' channels numbered '1' to 'N' (N numeric) % and an mni template structure % % Inputs: % ds dataset struct with first fdim dimension being % 'chan' with "fake" channels representing MEEG source % structure % template_grid struct with fields .{x,y,z}grid and .inside check_inputs(ds,template_grid); % voxels representing the brain inside=template_grid.inside; pos=template_grid.pos(inside,:)'; % change first dimension to position ds.a.fdim.values{1}=pos; ds.a.fdim.labels{1}='pos'; chan=ds.fa.chan; ds.fa=rmfield(ds.fa,'chan'); ds.fa.pos=chan; % sanity check cosmo_check_dataset(ds); function check_inputs(ds,template_grid) if isfield(ds,'label') error(['First input is not a CoSMo dataset structure. '... 'Use cosmo_meeg_dataset to convert to a CoSMo structure']); end cosmo_check_dataset(ds); if ~isequal(ds.a.fdim.labels{1},'chan') error('First fdim must be channel'); end raise=true; cosmo_isfield(template_grid,... {'xgrid','ygrid','zgrid','pos','inside'},... raise); labels=ds.a.fdim.values{1}; n_inside=sum(template_grid.inside); if n_inside~=numel(labels) error('Source count mismatch: %d ~= %d', n_inside, numel(labels)); end numeric_labels=cellfun(@str2num,labels,'UniformOutput',false); expected_numeric_labels=arrayfun(@(x)x,1:n_inside,... 'UniformOutput',false); if ~isequal(expected_numeric_labels,numeric_labels) error(['Labels are not as expected. This could mean that '... 'you are using this function not as intended. '... 'Proceed carefully']); end

and then get a ‘proper’ dataset in source space using

ds=convert_ds_mni_grid(src_ds,template_grid);

### Run cosmo_montecarlo_cluster_stat on a cluster with multiple nodes¶

‘I am running group statistics using cosmo montecarlo cluster stat but it is very slow when using the recommended 10,000 iterations. I have access to a computer cluster. Can I use the cluster to speed up the computations?’

Yes, although it requires a bit of extra work. You would run cosmo montecarlo cluster stat on multiple computer nodes with fewer iterations, then combine their results. Consider the following script (and comments in there):

% example on combining results of multiple invocations of % cosmo_montecarlo_cluster_stat into a single dataset with effectively % more iterations % % Use case: running 10,000 iterations with cosmo_montecarlo_cluster_stat % on a single machine takes to long, but there are 50 computer nodes % available in a computer cluster. Then each node can do 200 iterations; % results from each node are combined afterwards to get % effectively 10,000 iteraations % % generate some random data for 20 participants nsubjects=20; ds=cosmo_synthetic_dataset('ntargets',1,'nchunks',nsubjects,... 'sigma',0,'size','normal','seed',2); % Generate TFCE z-scores in 50 blocks, each with 20 iterations. % % In this example a simple for-loop is used to compute results for each % block, but typically results in each block are computed in different % Matlab sessions (e.g. when using multiple computer nodes in a clusters). % In that case, a script or function should be used that stores the result % (a dataset with TFCE z-scores) for each block in a .mat file. For % example, the following function could be run on each computing node (each % with a different value for block_id): % % function run_tfce_block(block_id,niter_per_block) % % % load dataset with data from each subject % ds=load('my_subject_data.mat'); % % % define neighborhood % nh=cosmo_cluster_neighborhood(ds); % % % set TFCE options % opt=struct(); % opt.niter=niter_per_block; % opt.h0_mean=0; % opt.seed=block_id; % % % compute TFCE z-scores % z_ds=cosmo_montecarlo_cluster_stat(ds,nh,opt); % % % save results to disk % fn=sprintf('tfce_z_block%02d.mat',block_id); % save(fn,'-struct','z_ds'); % % After running this function for aech block, the resulting .mat files % would then be loaded and combined with cosmo_stack as illustrated below. % % If a seed is set for cosmo_montecarlo_cluster_stat, then it is crucial % that different seed values are used in different blocks (otherwise each % block would yield identical results) nblocks=50; niter_per_block=20; ds_tfce_cell=cell(nblocks,1); for k=1:nblocks % Set TFCE options for each block. % A different seed value is used for each block to obtain repeatable % (determnistic) but different results in each block opt=struct(); opt.niter=niter_per_block; opt.h0_mean=0; opt.seed=k; % define the neighborhood nbrhood=cosmo_cluster_neighborhood(ds); % compute TFCE z-scores ds_tfce_k=cosmo_montecarlo_cluster_stat(ds,nbrhood,opt); % store result ds_tfce_cell{k}=ds_tfce_k; end % combine TFCE z-scores from all blocks into one dataset % (due to a tail cutoff protection this approach is very minorly % conservative in its p-value computation) ds_tfce_all=cosmo_stack(ds_tfce_cell); % convert TFCE z-scores to TFCE p-values % (the p-values represent the left tail probability) ps_all=normcdf(ds_tfce_all.samples); % compute the average p value over blocks, for each feature separately combined_ps=mean(ps_all,1); % convert TFCE p value back to TFCE z-scores combined_z=norminv(combined_ps); % make a new dataset in which the combined z-scores % are going to be stored ds_tfce=cosmo_slice(ds_tfce_all,1); % ensure empty sample attributes ds_tfce.sa=struct(); % store dataset ds_tfce.samples=combined_z; cosmo_check_dataset(ds_tfce)