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Probabilistic graphical models (@Lauritzen:1996) have become an important scientific tool for finding and describing patterns in high-dimensional data. Learning a graphical model from data requires a simultaneous estimation of the graph and of the probability distribution that factorizes according to this graph. In the Gaussian case, the underlying graph is determined by the non-zero entries of the precision matrix (the inverse of the population covariance matrix). Gaussian graphical models have become popular after the advent of computationally tractable estimators, such as neighborhood selection (@Meinshausen:2010) and sparse inverse covariance estimation (@Banerjee2008, @Yuan:2007). State-of-the-art solvers are the Graphical Lasso (GLASSO) (@Friedman2008) and the QUadratic approximation for sparse Inverse Covariance estimation (QUIC) method (@Hsieh2014).
Any neighborhood selection and inverse covariance estimation method requires a careful calibration of a regularization parameter “λ” (lambda) because the actual model complexity is not known a priori. State-of-the- art tuning parameter calibration schemes include cross-validation, (extended) information criteria (IC) such as Akaike IC and Bayesian IC (@Yuan:2007; @Foygel2010), and the Stability Approach to Regularization Selection (StARS) (@Liu2010). The StARS method is particularly appealing because it shows superior empirical performance on synthetic and real-world test cases and has a clear interpretation: StARS seeks the minimum amount of regularization that results in a sparse graph whose edge set is reproducible under random subsampling of the data at a fixed proportion β (@Zhao2012). Regularization parameter selection is thus determined by the concept of stability rather than regularization strength.
Two major shortcomings in StARS are computational cost and optimal setting of beta. StARS must repeatedly solve costly global optimization problems (neighborhood or sparse inverse covariance selection) over the entire regularization path for N sets of subsamples (where the choice of N is user-defined). Also, there may be no universally optimal setting of β as edge stability is strongly influenced by the underlying unknown topology of the graph (@Ravikumar2011b).
We alleviated both of these shortcomings (see @Mueller:2016). Firstly, we speed up StARS by proposing β-dependent lower and upper bounds on the regularization path from as few as N = 2 subsamples (Bounded StARS (B-StARS)). This implies that the lower part of regularization path (resulting in dense graphs and hence computationally expensive optimization) does not need to be explored for future samples without compromising selection quality. Secondly, we generalized the concept of edge stability to induced subgraph (graphlet) stability. We use the graphlet correlation distance (gcd) (@Yaveroglu2014) as a novel variability measure for small induced subgraphs across graph estimates. Requiring simultaneously edge and graphlet stability (gcd+StARS or G-StARS) leads to superior regularization parameter selection on synthetic benchmarks and real-world data.
The pulsar package comprises parallelized utilities for lambda selection along a regularization path using the StARS methodology and our recent extensions. Pulsar includes additional options for speedups, parallelizations and complementary metrics (e.g., graphlet stability (gcd), natural connectivity, …). This R package uses function passing to allow you to use your favorite graphical model learning method (e.g, GLASSO, neighborhood selection, QUIC, clime, etc). Since the tools are quite generic, pulsar can be used for other regularized problem formulations, e.g., for regularized regression (with the LASSO) or by using other sparsity-inducing norms (e.g., SCAD, MCP, …)
The option to find lower/upper bounds on the StARS-selected lambda from N=2 subsamples works particularly well when the underlying target graphs are sparse or when the dimensionality is high (above 20 variables or so). The bounds greatly reduce computational burden even when running in embarrassingly parallel (batch) mode.
In batch computing systems, we use the batchtools Map/Reduce strategy (for batch computing systems such as Torque, LSF, SLURM or SGE) and well as Interactive and multicore, socket, ssh clusters and Docker swams. which can significantly reduce the computation and memory burdens for StARS. This is useful for hpc users, when the number of processors available on a multicore machine would otherwise allow for only modest parallelization.
Please see the paper preprint on arXiv.
The most recent version of pulsar is on github and installation
requires the devtools package. For the purposes of this tutorial
suggested but not-imported packages will be prompted as needed
(e.g. huge, orca, …).
library(devtools)
install_github("zdk123/pulsar")
library(pulsar)In this example, we will use synthetic data generated from the
huge package.
library(huge)
set.seed(10010)
p <- 40 ; n <- 3000
dat <- huge.generator(n, p, "hub", verbose=FALSE, v=.1, u=.5)
lmax <- getMaxCov(dat$sigmahat)
lams <- getLamPath(lmax, lmax*.05, len=40)You can use the pulsar package to run StARS, serially,
as a drop-in replacement for the huge.select function in
the huge package. Pulsar differs in that we run the model
selection step first and then refit using arguments stored in the
original call. Remove the seed argument for real data (this
seeds the pseudo-random number generator to fix subsampling for
reproducing test code).
hugeargs <- list(lambda=lams, verbose=FALSE)
time1 <- system.time(
out.p <- pulsar(dat$data, fun=huge, fargs=hugeargs, rep.num=20,
criterion='stars', seed=10010))
fit.p <- refit(out.p)
## Inspect the output ##
out.p
fit.pIncluding the lower bound option lb.stars and upper
bound option ub.stars can improve runtime for same StARS
result (referred to as B-StARS in Mueller et al., 2016).
time2 <- system.time(
out.b <- pulsar(dat$data, fun=huge, fargs=hugeargs, rep.num=20,
criterion='stars', lb.stars=TRUE, ub.stars=TRUE, seed=10010))Compare runtimes and StARS-selected lambda index for each method.
time2[[3]] < time1[[3]]
opt.index(out.p, 'stars') == opt.index(out.b, 'stars')You can pass in an arbitrary graphical model estimation function to
fun. The function has some requirements: the first argument
must be the nxp data matrix, and one argument must be named
lambda, which should be a decreasing numeric vector
containing the lambda path. The output should be a list of adjacency
matrices (which can be of sparse representation from the
Matrix package to save memory). Here is an example from
QUIC.
library(BigQuic)
quicr <- function(data, lambda, seed=NULL) {
est <- BigQuic::BigQuic(data, lambda=lambda, epsilon=1e-2, use_ram=TRUE, seed=seed)
est <- setNames(lapply(ls(envir=est), mget, envir=attr(unclass(est), '.xData')), ls(envir=est))
path <- lapply(seq(length(lambda)), function(i) {
tmp <- est$precision_matrices[[1]][[i]]; diag(tmp) <- 0
as(tmp!=0, "lgCMatrix")
})
est$path <- path
est
}We can use pulsar with a similar call. We can also
parallelize this a bit for multi-processor machines by specifying
ncores (which wraps mclapply in the parallel
package).
quicargs <- list(lambda=lams)
nc <- if (.Platform$OS.type == 'unix') 2 else 1
out.q <- pulsar(dat$data, fun=quicr, fargs=quicargs, rep.num=100,
criterion='stars', lb.stars=TRUE, ub.stars=TRUE,
ncores=nc, seed=10010)We can use the graphlet correlation distance (gcd) as an additional
stability criterion (G-StARS). We could call pulsar again
with a new criterion, or simply update the arguments for
model we already used. Then, we can use our default approach for
selecting the optimal index, based on the gcd+StARS criterion: choose
the minimum gcd summary statistic between the upper and lower StARS
bounds.
out.q2 <- update(out.q, criterion=c('stars', 'gcd'))
opt.index(out.q2, 'gcd') <- get.opt.index(out.q2, 'gcd')
fit.q2 <- refit(out.q2)Compare model error by relative Hamming distances between refit adjacency matrices and the true graph and visualize the results:
plot(out.q2, scale=TRUE)starserr <- sum(fit.q2$refit$stars != dat$theta)/p^2
gcderr <- sum(fit.q2$refit$gcd != dat$theta)/p^2
gcderr < starserr
## install.packages('network')
truenet <- network::network(as.matrix(dat$theta))
starsnet <- network::network(summary(fit.q2$refit$stars))
gcdnet <- network::network(summary(fit.q2$refit$gcd))
par(mfrow=c(1,3))
coords <- plot(truenet, usearrows=FALSE, main="TRUE")
plot(starsnet, coord=coords, usearrows=FALSE, main="StARS")
plot(gcdnet, coord=coords, usearrows=FALSE, main="gcd+StARS")For large graphs, we could reduce pulsar run time by
running each subsampled dataset in parallel (i.e., each run as an
independent job). This is a natural choice since we want to infer an
independent graphical model for each subsampled dataset.
Enter batchtools. This package lets us invoke the queuing system in a high performance computing (hpc) environment so that we don’t have to worry about any of the job-handling procedures in R.
pulsar has only been tested for Torque so far, but
should work without too much effort for LSF, SLURM, SGE, …
We also potentially gain efficiency in memory usage. Even for memory
efficient representations of sparse graphs, for a lambda path of size L
and for number N subsamples we must hold L*N
p*p- sized adjacency matrices in memory to compute the
summary statistic. batchtools lets us use a MapReduce strategy, so that
only one p*p graph and one p*p aggregation
matrix needs to be held in memory at any time. For large p, it can be
more efficient to read data off the disk.
This also means we will need access to a writable directory to write
intermediate files (where the batchtools registry is stored). These will
be automatically generated R scripts, error and output files and sqlite
files so that batchtools can keep track of everything (although a
different database can be used). Please see that package’s documentation
for more information. By default, pulsar will create the
registry directory under R’s (platform-dependent) tmp directory but this
can be overridden(regdir argument to
batch.pulsar).
For generating batchtools, we need a configuration file (supply a
path string to conffile argument, a good choice is the
working directory) and, for an hpc with a queuing system, a template
file. Example config (batchtools.conf.torque.R) and PBS template file
(simpletorque.tmpl) for Torque can be found in the inst/config/ and
inst/templates/ subdirectories of this repo, respectively. See the batchtools
help page for creating templates for other systems.
For this example I suggest using batchtools interactive clusters (serial) mode to get things up and running. The necessary config file is included in this package.
conffile <- pulsar::findConfFile()Since batchtools is not imported by pulsar, it needs to
be loaded. Verbosity and progressbar options for batchtools is set by
global options. Uncomment cleanup=TRUE to remove registry
directory (useful if running through the example code multiple
times).
## uncomment below if batchtools is not already installed
# install.packages('batchtools')
library(batchtools)
options(batchtools.progress=TRUE, batchtools.verbose=FALSE)
out.batch <- batch.pulsar(dat$data, fun=quicr, fargs=quicargs, rep.num=100,
criterion='stars', seed=10010 #, cleanup=TRUE
)Check that we get the same result from batch mode pulsar:
opt.index(out.q, 'stars') == opt.index(out.batch, 'stars')It is also possible to run B-StARS in batch. The first two jobs (representing the first 2 subsamples) will run to completion before the final N-2 are run. This serializes the batch mode a bit but is, in general, faster whenever individual jobs require costly computation outside the lambda bounds, e.g., when some of the provided lambda values along the regularization path induce dense graph estimates.
To keep the initial two jobs separate from the rest, the string
provided to the init argument (“subtwo” by default) is
concatenated to the basename of regdir. The registry/id is
returned but named init.reg and init.id from
batch.pulsar. If missing (the default), a random string is
used for both registries.
out.bbatch <- update(out.batch, criterion=c('stars', 'gcd'),
lb.stars=TRUE, ub.stars=TRUE)Check that we get the same result from bounded/batch mode pulsar:
opt.index(out.bbatch, 'stars') == opt.index(out.batch, 'stars')In real applications, on an hpc, it is important to specify the
res.list argument, which is a named list
of PBS resources that matches the template file. For example if using
the simpletorque.tml file provided here
one would provide
res.list=list(walltime="4:00:00", nodes="1", memory="1gb")
to give the PBS script 4 hours and 1GB of memory and 1 node to the
resource list for qsub.
Gains in efficiency and run time (especially when paired with lower/upper bound mode) will largely depend on your hpc setup. E.g - do you have sufficient priority in the queue to run your 100 jobs in perfect parallel? Because settings vary so widely, we cannot provide support for unexpected hpc problems or make specific recommendations about requesting the appropriate resource requirements for jobs.
One final note: we assume that a small number of jobs could fail
at random. If jobs fail to complete, a warning will be given, but
pulsar will complete the run and summary statistics will be
computed only over the successful jobs (with normalization constants
appropriately adjusted). It is up to the user to re-start
pulsar if there is a sampling-dependent reason for job
failure, e.g., when an outlier data point increases computation time or
graph density and insufficient resources are allocated.
These binaries (installable software) and packages are in development.
They may not be fully stable and should be used with caution. We make no claims about them.
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