Spectracular Performance!

During the past 10 years Galaxy Zoo volunteers have done amazing work helping to classify the visual appearance (or “morphology”) of distant galaxies, which has enabled fantastic science that wouldn’t have been possible without your help. 

Morphology alone encodes a wealth information about the physical processes that drive the formation and ongoing evolution of galaxies, but we can learn even more if we analyze the spectrum of light they emit.

For the 100th Zooniverse project we designed the Galaxy Nurseries project to get your help analyzing galaxy spectra obtained by the Hubble Space Telescope (you can find many more details about Galaxy Nurseries on the main project research pages and this previous blog post).

If you participated in Galaxy Nurseries, then the data you analyzed were generated using a technique called slitless spectroscopy. In slitless spectroscopy all the light entering the HST aperture is dispersed (or split) into its separate frequencies before being projected directly into the telescope’s camera. Figure 1 illustrates a typically confusing result!

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Figure 1: Example of data obtained by the Hubble Space Telescope using slitless spectroscopy.

Each bright horizontal streak in the image shown in Figure 1 is actually the spectrum of a different galaxy or star. Analyzing these data can be very tricky, especially when nearby galaxy spectra overlap and cross-contaminate each other. Automatic algorithms really struggle to reliably distinguish between spectral contamination and scientifically interesting features that are present in the spectra. This means that scientists almost aways need to visually inspect any features that are automatically detected in order to ensure that they are really there!

In Galaxy Nurseries, we asked volunteers to help with this verification process. We asked you to double-check over 27,000 automatically detected emission lines in galaxy spectra obtained by the WISP galaxy survey, labelling them as either real or fake. Even for professional astronomers and experienced Galaxy Zoo volunteers, verifying the presence of emission lines in slitless spectroscopic data can be very difficult. To help you discriminate between real and fake emission lines we showed you three different views of the data. Figure 2 shows an example of one of the Galaxy Nurseries subject images.

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Figure 2: A Galaxy Nurseries subject showing a real emission line. The different panels show A) a 1-dimensional representation of the spectrum with the potential emission line marked ; B) a 2-dimensional “cutout” from the full slitless spectroscopic image, with the potential emission line and the expected extent of the galaxy spectrum marked; C) a direct image of the galaxy for which the spectrum was generated.

As well as the 1 dimensional spectrum shown in Figure 2 (Panel A), we also showed a “cutout” from the full slitless spectroscopic image, which isolated the target spectrum (Panel B), and a direct image of the galaxy that produced the spectrum (Panel C). The cutout in Panel B can be really useful for identifying contamination from adjacent spectra. For example, something that looks like a feature in the target spectrum might actually originate in an adjacent spectrum and would therefore appear slightly vertically off-centre in the 2-dimensional image.

Why is the direct image useful for spectroscopic analysis? Well, emission lines often appear like very slightly blurred images of the target galaxy at a specific position in the slitless spectrum. Look again at the emission line and the direct image in Figure 2. Can you see the similarity? If the shape of the automatically detected line feature in the slitless spectroscopic image doesn’t match the shape of the galaxy in the direct image, then this can indicate that the feature is just contamination masquerading as an emission line.

The response to Galaxy Nurseries was fantastic! Following its launch the project was completed in only 40 days, gathering 414,360 classifications (that’s 15 classifications per emission line) from 3003 volunteers. Huge thanks for everyones’ help! The results of the project were published in a Research Note, and the rest of this post summarizes what we learned.

Using the labels assigned to each potential emission line by galaxy zoo volunteers we computed the fraction of volunteers who classified the line and thought it was real (hereafter freal). We wanted to compare the responses of the Galaxy Zoo volunteers with those of professional astronomers from the WISP survey team (WST). To do this, we divided the potential emission lines into two sets. The verified set contained emission lines that the WST thought were real and the vetoed set contained emission lines that the WST thought were fake. We assumed that the WST assessments were correct in the vast majority of cases, but this might not be completely accurate. Even professional astronomers make mistakes!

Figure 3 shows the distributions of freal for the two sets of emission lines. The great news is that for the vast majority of lines that the WST thought were fake, over half of the volunteers agreed with them (i.e. freal < 0.5). Similarly for most of the WST-verified set of line, the majority volunteers also labeled them as real. These results show us that Zooniverse and Galaxy Zoo volunteers are very capable when it comes to separating real emission lines from the fakes.

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Figure 3: The distributions of freal for sets of emission lines that were verified (blue) or vetoed (orange) by the WISP survey team.

What can we say about the lines for which the volunteers and the WST disagreed? Is there something about them that makes them particularly hard to classify? Well, it turns out that the answer is “yes”!

We computed two statistical metrics to quantify the level of agreement between the Zooniverse volunteers and the WST for a particular sample of the emission lines that were classified.

  1. The sample purity is defined as the ratio between the number of true positives (for which both the volunteers and the WST believe the the line is real)  and the combined number of true positives and false positives (for which a feature labeled as fake by the WST was labeled as real by the volunteers). The purity tells us the fraction of lines in the sample that were labeled real by the volunteers that were also labeled as real by the WST. If volunteers don’t mislabel any fake lines as real then purity is 1.
  2. The sample completeness is the ratio between the number of true positives and combined number of true positives and true negatives (for which the WST labeled the line as real, but the volunteer consensus was that the line was fake). The completeness tells us the fraction of lines in the sample that were labeled as real by the WST that were also labeled as real by the volunteers. If volunteers spot all the real lines identified by the WST then the completeness is 1.

Figure 4 plots purity and completeness as a function of freal  and the emission line signal-to-noise ratio (S/N). Lines with higher S/N stand out more relative to the noise in the spectrum and should be easier to analyze for volunteers and the WST alike. Examining Figure 4 reveals that for subsets of candidate lines having freal less than a particular threshold value (shown on the horizontal axis), the completeness values are higher for higher S/N. This indicates that spotting real lines is much easier when the features being examined are bright, which makes intuitive sense. On the other hand, higher purities can be achieved for similar threshold values of  freal as the S/N value decreases, which indicates that volunteers are reluctant to label faint lines as real. At low S/N, sample purities as high as 0.8 can be achieved when only 50% of volunteers agreed that the corresponding emission lines were real. At higher S/N, volunteers become more confident, but also seem slightly more likely to identify noise and contaminants as real lines. This is probably a reflection of just how difficult the line identification task really is. Nonetheless, samples that are 70% pure can be selected by requiring a marginal majority of votes for real ( freal value of at least 0.6), which is pretty impressive!

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Figure 4: Sample purity (left) and completeness (right) plotted as a function of minimum freal value for any potential line in the sample, and that line’s signal-to-noise ratio.

We can use the plots in Figure 4  to select samples that have desirable properties for scientific analysis. For example, if we want to be sure that we include 75% of all the real lines but we don’t mind a few fakes sneaking in, then we could choose  freal = 0.5 which would give a completeness larger than 0.75 for all S/N values. However, if we choose freal = 0.5, then the purity of our sample could be as low as 0.6 for high S/N, with about 40% of accepted lines being fake in reality.

The ability to extract very complete but impure emission line samples can be very useful. By selecting a sample that removes a sizable fraction of fakes from the automatically detected candidates, the number of potential lines that the WST need to visually inspect is dramatically reduced. It took the WST almost 5 months before each line in Galaxy Nurseries could be inspected by just two independent astronomers. By providing 15 independent classifications for each line, Zooniverse volunteers did the 8 times as much work in just 40 days! In the future, large-scale slitless spectroscopic surveys will be performed by new space telescopes like Euclid and WFIRST. These surveys will measure millions of spectra containing many millions of potential emission lines and individual science teams will simply not be able to visually inspect all of these lines. Eventually, deep learning algorithms may be able to succeed where current automatic algorithms fail. In the meantime, it is only with the help of Zooniverse and Galaxy Zoo volunteers that scientists will be able to exploit more than the tiniest fraction of the fantastic data that will soon arrive.

Enhancing Galaxy Zoo

We’ve just switched on what may be the biggest change to Galaxy Zoo since the project started more than a decade ago. In order to prepare for future surveys like Euclid and LSST which might overwhelm even the stalwart efforts of Galaxy Zoo volunteers, we’re now running an automatic classifier which works with those results from volunteers.

This machine – even when trained on the existing Galaxy Zoo results – is not perfect, and so we still need classifications from you all. Each night, the machine will learn from the day’s results, and then calculate which galaxies it thinks it most needs human help with – and if you select the ‘Enhanced’ workflow, then you’ll be much more likely to see these galaxies.

You can read more about the machine learning we’re using in a blogpost from Mike Walmsley here, and in more technical detail here. (There’s a paper available on the arXiv from this morning too). We’re also running a messaging experiment you can read about here.

We do still need volunteers to look at each and every galaxy to make sure we’re not missing anything. If you prefer to classify the old-fashioned way, then the ‘Classic’ workflow is Galaxy Zoo just as it always was.

I and the rest of the team are looking forward to seeing what we can find with this new approach – and with your help.

Chris

Machine Learning Messaging Experiment

Alongside the new workflow that Galaxy Zoo has just launched (read more in this blog post: https://wp.me/p2mbJY-2tJ), we’re taking the opportunity to work once again with researchers from Ben Gurion University and Microsoft Research to run an experiment which looks at how we can communicate with volunteers. As part of this experiment volunteers classifying galaxies on the new workflow may see short messages about the new machine learning elements. Anyone seeing these messages will be given the option to withdraw from the experiment’; just select the ‘opt out’ button to avoid seeing any further messages.

After the experiment is finished we will publish a debrief blog here describing more of the details and presenting our results.

This messaging experiment has ethics approval from Ben Gurion University (reference: SISE-2019-01) and the University of Oxford (reference: R63818/RE001).

Galaxy Zoo Upgrade: Better Galaxies, Better Science

Since I joined the team in 2018, citizen scientists like you have given us over 2 million classifications for 50,000 galaxies. We rely on these classifications for our research: from spiral arm winding, to merging galaxies, to star formation – and that’s just in the last month!

We want to get as much science as possible out of every single click. Your time is valuable and we have an almost unlimited pile of galaxies to classify. To do this, we’ve spent the past year designing a system to prioritise which galaxies you see on the site – which you can choose to access via the ‘Enhanced’ workflow.

This workflow depends on a new automated galaxy classifier using machine learning – an AI, if you like. Our AI is good at classifying boring, easy galaxies very fast. You are a much better classifier, able to make sense of the most difficult galaxies and even make new discoveries like Voorwerpen, but unfortunately need to eat and sleep and so on. Our idea is to have you and the AI work together.

The AI can guess which challenging galaxies, if classified by you, would best help it to learn. Each morning, we upload around 100 of these extra-helpful galaxies. The next day, we collect the classifications and use them to teach our AI. Thanks to your classifications, our AI should improve over time. We also upload thousands of random galaxies and show each to 3 humans, to check our AI is working and to keep an eye out for anything exciting.

With this approach, we combine human skill with AI speed to classify far more galaxies and do better science. For each new survey:

  • 40 humans classify the most challenging and helpful galaxies
  • Each galaxy is seen by 3 humans
  • The AI learns to predict well on all the simple galaxies not yet classified

What does this mean in practice? Those choosing the ‘Enhanced’ workflow will see somewhat fewer simple galaxies (like the ones on the right), and somewhat more galaxies which are diverse, interesting and unusual (like the ones on the left). You will still see both interesting and simple galaxies, and still see every galaxy if you make enough classifications.

With our new system, you’ll see somewhat more galaxies like the ones on the left, and somewhat fewer like the ones on the right.

We would love for you to join in with our upgrade, because it helps us do more science. But if you like Galaxy Zoo just the way it is, no problem – we’ve made a copy (the ‘Classic’ workflow) that still shows random galaxies, just as we always have. If you’d like to know more, check out this post for more detail or read our paper. Separately, we’re also experimenting with sending short messages – check out this post to learn more.

Myself and the Galaxy Zoo team are really excited to see what you’ll discover. Let’s get started.

Scaling Galaxy Zoo with Bayesian Neural Networks

This is a technical overview of our recent paper (Walmsley 2019) aimed at astronomers. If you’d like an introduction to how machine learning improves Galaxy Zoo, check out this blog.

I’d love to be able to take every galaxy and say something about it’s morphology. The more galaxies we label, the more specific questions we can answer. When you want to know what fraction of low-mass barred spiral galaxies host AGN, suddenly it really matters that you have a lot of labelled galaxies to divide up.

But there’s a problem: humans don’t scale. Surveys keep getting bigger, but we will always have the same number of volunteers (applying order-of-magnitude astronomer math).

We’re struggling to keep pace now. When EUCLID (2022), LSST (2023) and WFIRST (2025ish) come online, we’ll start to look silly.

Galaxies/day required to keep pace with upcoming surveys now, by 2019 year-end, and by 2022 year-end. Estimates from internal science plan.

To keep up, Galaxy Zoo needs an automatic classifier. Other researchers have used responses that we’ve already collected from volunteers to train classifiers. The best performing of these are convolutional neural networks (CNNs) – a type of deep learning model tailored for image recognition. But CNNs have a drawback. They don’t easily handle uncertainty.

When learning, they implicitly assume that all labels are equally confident – which is definitely not the case for Galaxy Zoo (more in the section below). And when making (regression) predictions, they only give a ‘best guess’ answer with no error bars.

In our paper, we use Bayesian CNNs for morphology classification. Our Bayesian CNNs provide two key improvements:

  1. They account for varying uncertainty when learning from volunteer responses
  2. They predict full posteriors over the morphology of each galaxy

Using our Bayesian CNN, we can learn from noisy labels and make reliable predictions (with error bars) for hundreds of millions of galaxies.

How Bayesian Convolutional Neural Networks Work

There’s two key steps to creating Bayesian CNNs.

1. Predict the parameters of a probability distribution, not the label itself

Training neural networks is much like any other fitting problem: you tweak the model to match the observations. If all the labels are equally uncertain, you can just minimise the difference between your predictions and the observed values. But for Galaxy Zoo, many labels are more confident than others. If I observe that, for some galaxy, 30% of volunteers say “barred”, my confidence in that 30% massively depends on how many people replied – was it 4 or 40?

Instead, we predict the probability that a typical volunteer will say “Bar”, and minimise how surprised we should be given the total number of volunteers who replied. This way, our model understands that errors on galaxies where many volunteers replied are worse than errors on galaxies where few volunteers replied – letting it learn from every galaxy.

2. Use Dropout to Pretend to Train Many Networks

Our model now makes probabilistic predictions. But what if we had trained a different model? It would make slightly different probabilistic predictions. We need to marginalise over the possible models we might have trained. To do this, we use dropout. Dropout turns off many random neurons in our model, permuting our network into a new one each time we make predictions.

Below, you can see our Bayesian CNN in action. Each row is a galaxy (shown to the left). In the central column, our CNN makes a single probabilistic prediction (the probability that a typical volunteer would say “Bar”). We can interpret that as a posterior for the probability that k of N volunteers would say “Bar” – shown in black. On the right, we marginalise over many CNN using dropout. Each CNN posterior (grey) is different, but we can marginalise over them to get the posterior over many CNN (green) – our Bayesian prediction.

Read more about it in the paper.

Active Learning

Modern surveys will image hundreds of millions of galaxies – more than we can show to volunteers. Given that, which galaxies should we classify with volunteers, and which by our Bayesian CNN?

Ideally we would only show volunteers the images that the model would find most informative. The model should be able to ask – hey, these galaxies would be really helpful to learn from– can you label them for me please? Then the humans would label them and the model would retrain. This is active learning.

In our experiments, applying active learning reduces the number of galaxies needed to reach a given performance level by up to 35-60% (See the paper).

We can use our posteriors to work out which galaxies are most informative. Remember that we use dropout to approximate training many models (see above). We show in the paper that informative galaxies are galaxies where those models confidently disagree.

Informative galaxies are galaxies where the each model is confident (entropy H in the posterior from each model is low) but the average prediction over all the models is uncertain (entropy across all averaged posteriors is high). See the paper for more.

This is only possible because we think about labels probabilistically and approximate training many models.

What galaxies are informative? Exactly the galaxies you would intuitively expect.

  • The model strongly prefers diverse featured galaxies over ellipticals
  • For identifying bars, the model prefers galaxies which are better resolved (lower redshift)

This selection is completely automatic. Indeed, I didn’t realise the lower redshift preference until I looked at the images!

I’m excited to see what science can be done as we move from morphology catalogs of hundreds of thousands of galaxies to hundreds of millions. If you’d like to know more or you have any questions, get in touch in the comments or on Twitter (@mike_w_ai, @chrislintott, @yaringal).

Cheers,
Mike

Classify Now

Excited to join in? Click here to go to Galaxy Zoo and start classifying! What could you discover?

Thanks for the millions!

Congratulations Radio Galaxy Zoo citizen scientists on a job well done! The Radio Galaxy Zoo 1 project has now finished with ~2.29 million classifications! Well done on helping us push towards the finish line.

We have at least two second-generation Radio Galaxy Zoo projects in the pipeline for which we hope to launch next. Therefore please stay tuned for the announcement of the Radio  Galaxy Zoo 2 projects where we will be presenting you with new data from the next-generation radio telescopes.

Thank you very much again for all your support and we will continue to keep you updated on our progress in the interim.

Cheers,
Ivy & Stas

Winding Problems

I’m delighted to announce the acceptance of another paper based on your classifications at Galaxy Zoo, “Galaxy Zoo: Unwinding the Winding Problem – Observations of Spiral Bulge Prominence and Arm Pitch Angles Suggest Local Spiral Galaxies are Winding”, which has just been released on the arxiv pre-print server, and appear in the Monthly Notices of the Royal Astronomical Society (MNRAS) soon.

Here’s the title and author page.

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This paper has been a long time coming, and is based significantly on the excellent thesis work of Ross Hart (PhD from Nottingham University). Ross wrote about some of his work for the blog previously “How Do Spiral Arms Affect Star Formation“. One of the things Ross’s PhD work showed was just how good your identification of spiral arm winding is, and that allowed us to be confident to use it in this paper.

You might notice the appearance of some of your fellow citizen scientists in this author list. Dennis, Jean and Satoshi provided help via the “Galaxy Zoo Literature Search” call which ended up contributing significantly to the paper.

Our main result is that we do not find any significant correlation between how large the bulges are and how tightly wound the spirals are in Galaxy Zoo spiral galaxies…. this non-detection was a big surprise, because this correlation is discussed in basically all astronomy text books – it forms the basis of the spiral sequence described by Hubble.

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The Hubble Tuning Fork illustrated with SDSS images of nearby galaxies.

Way back in 1927 Hubble wrote (about the spiral nebula he had observed) that: “three [properties] determine positions in the sequence: (1) the relative size of the unresolved nuclear region, (2) the extent to which the arms are unwound (the openness or angle of the spiral), (3) the degree of condensation in the arms.” He goes on to explain that “These three criteria are quite independent, but as an empirical fact of observation they develop in the same direction, and can be treated as various aspects of the same process.” (i.e. Hubble observed them to be correlated).

It’s been known for a long time that there are examples where bulge (or “unresolved nuclear region”) size and arm winding did not agree, but these are usually treated as exceptions. What we’ve shown in this paper, is that for a sample selection which goes beyond just the brightest nearby galaxies Hubble could see, the correlation is not strong at all. Below is an annotated version of our main result figure – each point is a spiral with Galaxy Zoo classifications, and the contours show where there are lots of points. We find spirals all over this plot (except not many with big bulges and loosely wound arms), and the red and blue lines show the lack of any strong trend in either direction.

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Figure 5 from Masters et al. (2019) paper.

 

This has significantly implications for how we interpret spiral winding angles, and could be explained by many/most spiral arms winding up over time (at rates which depend on the bulge size) rather than being density waves. We need to do more work to really understand what this observation tells us (which is a great place to be in science!).

We have also known for a while, that bulge size correlates best with modern expert galaxy classification on the Hubble sequence (e.g. when we compared you classifications to the largest samples done in that way).  So another point we make in this paper is how different these modern classifications are to the traditional classifications done by Hubble and others. That’s OK – classifications should (and do) shift in science (part of the scientific method is to change on the basis of evidence), but it does mean care needs to be taken to be precise about what is meant by “morphology of galaxies”.

I ended the abstract of the paper with: “It is remarkable that after over 170 years of observations of spiral arms in galaxies our understanding of them remains incomplete.” and I really think that’s a good place to end. Galaxy morphology provides a rich source of data for understanding the physics of galaxies, and thanks to you we have access to the largest and most reliable set of galaxy morphologies ever. 


 

If you’re inspired to keep classifying, head over to the main Galaxy Zoo project, or why not draw a few spiral arms over at Galaxy Zoo: 3D where we’re trying to understand spiral arms in more detail.

 

Radio Galaxy Zoo final sprint !

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Radio Galaxy Zoo logo

Here is a bittersweet announcement that the current first-generation Radio Galaxy Zoo project will be retiring on the 1st May 2019. We are so grateful to have worked with such a productive team of citizen and professional scientists for the past 5.5 years.
To-date, we have made over 2.27 million classifications and published 10 refereed journal articles. We have another 1 submitted and another to be submitted in the next few weeks.

Looking towards the future, we are of course in the process of developing the next-generation of Radio Galaxy Zoo projects. For that, we ask that you stay tune for our future announcements of the suite of Radio Galaxy Zoo 2 projects that we are planning to launch.  Of course, we will be keeping you all informed about our latest RGZ-based follow-up observations (e.g. the Zoo Gems programme with the Hubble Space Telescope). Therefore, this is not the last message from us.

To cap-off this impending retirement, I propose that we make a final RGZ sprint to the finish in the remaining days April 2019 –that is, let’s all try to classify as many sources as we can in the next few weeks!

Thank you very much again and let’s all make a concerted push to the  finish line!

Cheers,
Ivy & Stas

Radio Galaxy Zoo studies cluster environment impact on radio galaxy morphologies

The following blogpost is from Avery Garon who led the publication of Radio Galaxy Zoo’s latest science result. Congratulations to Avery and team!

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Radio Galaxy Zoo is starting the new year strong, with another paper just accepted for publication. “Radio Galaxy Zoo: The Distortion of Radio Galaxies by Galaxy Clusters” will appear soon in The Astronomical Journal and is available now as a pre-print on the arXiv: https://arxiv.org/abs/1901.05480. This paper was led by University of Minnesota graduate student Avery Garon and investigates several ways in which the shape of a galaxy’s radio emission is affected by and informs us about the environment in which we find the galaxy.

Like the previous RGZ paper, we are looking for how the radio tails extend into the hot plasma that fills galaxy clusters (the intracluster medium, or ICM). This time, we measure how much the two tails deviate from a straight line, marked in the example below by the value θ. The standard model is that the ICM exerts ram pressure on the galaxy as it travels though the cluster and causes its tails to bend away from the direction of motion. However, while individual clusters have been studied in great detail, no one has had a large enough sample of radio galaxies to statistically validate this model. Thanks to RGZ, we were able to observe the effect of ram pressure as a trend for the bending angle θ to increase for galaxies closer to the center of clusters (where the ICM density is higher) and in higher mass clusters (where the galaxies orbit with higher speeds).

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Example source RGZ J080641.4+494629. The magenta arrows extend from the host galaxy identified by RGZ users and terminate at the peaks of the radio emission, defining the bending angle θ. The cyan arrow is used to define an orientation for the galaxy with respect to the cluster.

Because ram pressure causes the tails to bend away from the direction in which the galaxy is travelling, we can use this knowledge to map out the kinds of orbits that these galaxies are on. Unlike planetary orbits, which are nearly circular and all in the same plane, the orbits of galaxies in clusters tend to be randomly distributed in orientation and eccentricity. Our sample of bent radio galaxies shows an even more striking result: they are preferentially found in highly radial orbits that plunge through the center of their clusters, which suggests that they are being bent as their orbits take them through the dense central regions.

Finally, we looked at radio galaxies that were far from clusters. Even though the median bending angle is 0° away from clusters, there is still a small fraction of highly bent galaxies out there. By counting the number of optical galaxies that are near the radio galaxies, we observed a sharp increase in the number of companions within a few hundred kiloparsecs of our bent radio galaxies. This suggests that even outside of true cluster environments, we are still observing bending induced by local overdensities in the intergalactic medium.