Stellar deaths and their afterlives are laboratories that test fundamental physics through astrophysics. The advent of extremely wide‐field surveys will revolutionize this field, and we will be able to probe new time and energy scales. The community will need to build new infrastructure and change existing paradigms to maximize the science return of these facilities. This workshop will connect scientists with expertise in multi‐ messenger astrophysics with statisticians, data scientists, and software developers. Together, they will highlight what infrastructure exists, identify how these pieces may be connected together into a larger ecosystem, and develop a roadmap to prepare for future surveys.

Agenda

AGENDA

Thursday, April 25, 2019

8:00 – 9:00 AM Registration/Breakfast Lobby/Café Azafran 9:00 Welcome Nancy Levenson, Deputy Director, STScI Chair: Gautham CHALLENGES FACING TIME‐DOMAIN Narayan ASTROPHYSICS 9:15 Iair Arcavi Coordinating Followup of GW Events 9:30 Arfon Smith MAST Archive and Operations in the MMA Era. 9:45 Saurabh Jha Multi‐Messenger Astrophysics: We Are The Messengers 10:00 10:15 10:30 – 11:00 AM AM Coffee Break Café Azafran Chair: Renée Hložek DATA SCIENCE AND MACHINE LEARNING FOR MMA 11:00 Emilie Ishida Human in the Loop: Adaptive Learning in Astronomy 11:15 Wolfgang Kerzendorf DALEK ‐ Supernova Physics Meets Machine Learning 11:30 Victor Francisco Ksoll Characterizing Extragalactic Pre‐Main‐Sequence Stars with Machine and Deep Learning Techniques 11:45 Daniel Muthukrishna RAPID: Early Classification of Explosive Transients using Deep Learning 12:00 Darryl Wright Supporting Transient Surveys with Citizen Science 12:15 Kyle Rocha Using Machine Learning to Predict Outcomes for Binary Stellar Evolution 12:30 – 2:00 PM Lunch/Posters Chair: Massimo PUTTING THE MULTI IN MULTI‐MESSENGER Robberto 2:00 Jennifer Lotz GEMMA: Gemini in the Era of Multi‐Messenger Astronomy 2:15 Eric Burns Joint Gravitational Wave and Gamma‐ray Burst Online Searches 2:30 Jeff Cooke The Deeper, Wider, Faster Program: Pioneering Multi‐facility, Multi‐wavelength, Multi‐messenger Fast Transient Exploration 2:45 Michael Coughlin Finding LISA Gravitational‐wave Sources in the Optical Time Domain 3:00 Azadeh Keivani Multi‐messenger Gravitational‐Wave + High‐Energy Neutrino Searches 3:15 Group Photo Front Steps of Muller Building 3:30 – 4:00 PM PM Coffee Break Café Azafran Chair: Federica Bianco BROKERS, TOMS, AND DATA HUBS 4:00 Dave Coulter Software Platforms to Enhance Decision Making for Multi‐Messenger Astronomy 4:15 Francisco Forster The Universe in a Stream: Challenges and Progress of the ALeRCE Broker 4:30 Monika Soraisam ANTARES: Brokering Alerts in Real‐time in the Big‐ Data Era 4:45 Rachel Street Microlensing as a Case Study of Alert‐based Science and Technologies 5:00 Ken Smith Lasair: The Transient Alert Broker for LSST:UK

5:30 – 7:00 PM Welcome Reception Café Azafran 7:00 PM Dinner Various

*Talk Times: Invited Speakers 15 + 2

Contributing Speakers 10 + 2

Friday, April 26, 2016

8:15 – 9:00 AM Registration/Breakfast Café Azafran Chair: Ivelina DATABASES AND ARCHIVES Momcheva 9:00 Melissa Graham The LSST Data Management Systems: Infrastructures for EMMA 9:15 Dmitry Duev The Zwicky Transient Facility (ZTF) Data Ecosystem 9:30 Jan‐Uwe Ness Multi‐mission Coordinations 9:45 Kyle Chard Parsl, a Python‐based Parallel Scripting Library 10:00 Jamie Kinney From Zero to ML ‐ Managing and Analyzing Astronomy Data on Google Cloud 10:30 – 11:00 AM AM Coffee Break Café Azafran Chair: Leo Singer MULTI‐MESSENGER P2 11:00 John Graham Limitations on IMF Variability as a Function of 11:15 Kshitij Aggarwal Finding Fast Radio Bursts with Realfast at the VLA 11:30 Carl‐Johann Haster Gravitational Waves as a Piece of the Astrophysical Multi‐messenger Puzzle 11:45 Joshua Schleider Nimble: A Mission Concept for Gravitational Wave Counterpart Astrophysics 12:00 Nao Suzuki HSC Transient Survey 12:15 Ann Hornschemeier Stellar‐origin Black Holes and Neutron Stars in the 2020’s and Beyond: The Post Chandra and XMM‐ Newton Era 12:30 – 2:00 PM Lunch/Posters Chair: Ryan Foley FOLLOWUP STRATEGY AND INSTRUMENTATION 2:00 Alexander van der Probing the Transient Sky with SCORPIO Horst 2:15 Morten Anderson Gemini in LSST/SCORPIO Era 2:30 Igor Andreoni ZTF and DECam Follow‐up of Neutron Star Mergers during O3 2:45 Aaron Tohuvavohu Swift in the Multi‐messenger Era 3:00 David Cook The Role of NED in Identifying EM Counterparts to GW Events 3:15 Sarah Burke‐Spoalar MMA in the Nanohertz Gravitational Wave‐band 3:30 – 4:00 PM Coffee Café Azafran Chair: Armin Rest DISCUSSION 4:00 – 5:00 PM Workshop Adjourns

*Talk Times: Invited Speakers 15 + 2

Contributing Speakers 10 + 2

Talk Abstracts Kshitij Aggarwal (West Virginia University)

Realfast: Real‐time, Commensal Fast Transient Search at the Very Large Array Localization of a Fast Radio Burst (FRB) to ~arcsecond precision is necessary for confident host association, and is likely to prove essential to studying FRB environments, host electron densities, the structure and fields of intervening media. The Realfast commensal FRB detection system on the Karl G. Jansky Very Large Array (VLA) will detect and precisely localize FRBs in real time by performing fast imaging (~5ms) of dedispersed data. In late 2016, Realfast performed the first FRB localization, pinning down the repeating FRB121102 to a precision of 0.2”, which enabled the identification of its host and further studies of its environment. This talk will review the current status and ongoing development of the commensal Realfast system. This will include results from the observing run using the prototype (non‐commensal, CPU‐based) system, insights into the unique issues and benefits of imaging searches, and the use of machine learning techniques to cluster and classify the vast amount of candidates expected from this pipeline. Morten Andersen (Gemini Observatory)

Gemini in LSST/SCORPIO Era The advent of LSST will dramatically alter the approach to observe newly discovered transient objects. Gemini is currently in the process of building the SCORPIO instrument that will be very well suited for rapid followup observations. Gemini further have rapid target of opportunity capabilities to take advantage take advantage of triggers from the community. However the system will have to change to cope with the expected rate of triggers in the near future. Here we present both briefly the SCORPIO instrument as well as Geminis plans in collaboration with other observatories in in the future to handle numerous triggers from the community. Igor Andreoni (Caltech)

ZTF and DECam Follow‐up of Neutron Star Mergers during O3 After GW170817, we are looking forward to the next binary neutron star merger detection and the very first neutron star – black hole merger. Both types of merger are expected to generate a transient called kilonova, observable at optical/infrared wavelengths. The GROWTH collaboration can count on major facilities for discovery, characterization, and monitoring of gravitational‐wave counterparts. In particular, the Zwicky Transient Facility (ZTF) at Palomar and the Dark Energy Camera (DECam) at CTIO are wide‐field instruments perfectly placed to discover faint kilonovae shortly after gravitational‐wave triggers are issued. I will present our plans for kilonova discovery with ZTF and DECam, touching on rapid transient detection techniques and infrastructure. Iair Arcavi (Tel Aviv University)

Coordinating Followup of GW Events As we enter the era of the first NS merger samples, we need to better coordinate our search for EM counterparts. The early (first hours ‐ day) emission of such counterparts turns out to be crucial for distinguishing between models of the ejecta structure and properties, and the merger physics. Localizations will still be as large (or larger) than in the GW170817 case, and the amount of observing time devoted to that event is not sustainable in the sample era. We must be more efficient with our telescopes. We should therefore design and build a system for coordinating observations between groups to avoid duplication, maximize our coverage of the localization region as quickly as possible, and divide vetting and followup chores of identified candidates. I will present some ideas on how to start doing this, based on similar systems I developed for coordinating followup of supernovae and tidal disruption events in large collaborations.

Sarah Burke‐Spolaor (West Virginia University)

MMA in the Nanohertz Gravitational Wave‐band Pulsar timing arrays are already placing limits on the evolution of binary supermassive black holes in mergers, and in the near future should begin to detect these objects. I will discuss the prospects of, methods for, and good practices for multi‐messenger detection of these objects with Pulsar Timing Arrays and other electromagnetic observatories. Eric Burns (NASA Goddard)

Joint Gravitational Wave and Gamma‐ray Burst Online Searches The Fermi Gamma‐ray Burst Monitor team and the LIGO and Virgo Collaborations are working together to automatically associate and localize neutron star mergers in real‐time starting with the O3 observing run. Overall this promises to increase the number of gravitational wave signals reported in real‐time and to shrink the localization regions available shortly after merger time. These events and joint localizations will be reported to the follow‐up community. We will discuss what is being done, the expected improvements, what follow‐up observers need to know, and prospects for future improvements. David Cook (IPAC/Caltech)

The Role of NED in Identifying EM Counterparts to GW Events The detection of gravitational waves (GWs) has opened a new window into the Universe by enabling direct studies of mergers of massive, compact objects. Some of the largest impacts on our understanding of these events will come when combining the GW data with their electromagnetic (EM) counterparts. However, due to the large area (> 100 deg^2) localization of LIGO events, identifying their correct EM counterparts is no small feat and is akin to finding a needle in a haystack. This search is and will continue to be difficult task due to the large (>100 deg^2) localization of LIGO events. To overcome this challenge several teams used a galaxy‐ targeted approach to successfully locate the EM counterpart to the neutron star‐neutron star merger event GW20170717. In this talk I introduce a new service of the NASA/IPAC Extragalactic Database (NED) that will provide prioritized lists of located within future LIGO 90% probability contours to facilitate searches for EM counterparts, starting with the O3 run scheduled to begin in April 2019. I will give an overview of the service, as well as an analysis of the local Universe NED galaxy sub‐sample and comparisons with other local galaxy lists.

Jeff Cooke (Swinburne University)

The Deeper, Wider, Faster Program: Pioneering Multi‐facility, Multi‐wavelength, Multi‐messenger Fast Transient Exploration I will discuss the structure and strategy behind our ongoing Deeper, Wider, Faster program (DWF) to detect and study transients with millisecond‐to‐hours duration in real time. Fast transients include supernova shock breakouts, very early supernovae, fast radio bursts, flare stars, and kilonovae. DWF coordinates over 50 telescopes worldwide and in space, from radio through gamma‐ray, organized along with neutrino, cosmic ray, and gravitational wave detectors. Multi‐ wavelength, sensitive, wide‐field telescopes are coordinated to acquire fast‐cadenced data at the same time on the same fields, generating large datasets and high computational demand when processing the data in real time. DWF also acquires simultaneous fast‐cadenced CTIO DECam or NAOJ Subaru HSC optical imaging and processes the data in real time (seconds) on the Swinburne supercomputer throughout the night. The candidates are identified in near real‐time (minutes after outburst), with the help from sophisticated data visualisation, to trigger rapid‐response spectroscopy and imaging. DWF has been a trailblazer for LSST and future large transient survey programs and is an excellent platform for machine and deep learning techniques, Big Data transfer and processing, and real‐time and ‘streaming’ data analyses. Michael William Coughlin (California Institute of Technology)

Finding LISA Gravitational‐wave Sources in the Optical Time Domain The wealth of optical time domain data coming out of surveys such as ZTF and ATLAS is useful for identifying steady‐state gravitational wave sources detectable in the LISA band, such as double white dwarf binaries. In this talk, I will discuss techniques for discovering such systems in the optical time domain. This includes the use of the Kitt Peak EMCCD Demonstrator (KPED), a new high‐cadence photometer on the Kitt Peak 84 inch, as a follow‐up tool from these surveys. I will describe how the combination of the wide‐field surveys and this system have enabled recent discoveries with ZTF, and their implications for the future of gravitational science in the era of LISA. Dave Coulter (University of California, Santa Cruz)

Software Platforms to Enhance Decision Making for Multi‐Messenger Astronomy GW170817 was a watershed event for multi‐messenger astronomy. Positional information from LIGO was combined with galaxy catalogs to quickly locate the optical counterpart, SSS17a/AT2017gfo, which provided a wealth of insight into topics as diverse as the origin of the heavy elements to measurements of the neutron star equation of state. While our team's galaxy‐ targeted approach was successful, it was also a largely manual process. With LIGO's O3 run, LIGO and Virgo's detector range will be greatly improved, increasing both the number of mergers detected and their average detected distance. This new paradigm introduces several challenges to our original process, ranging from incomplete galaxy catalogs to vastly larger data sets to be analyzed. We have addressed these challenges by creating a suite of open‐source tools which evolve our galaxy‐targeted approach to effectively search larger volumes, optimize and coordinate a network of heterogeneous telescopes, and manage, query, and visualize multiple sources of data in real‐time to streamline our decision making ability. I will present these tools, as well as selected case studies to demonstrate their flexibility, and show how our platform will scale in a future dominated by Big Data. Dmitry Duev (Caltech)

The Zwicky Transient Facility (ZTF) Data Ecosystem The Zwicky Transient Facility (ZTF) is a new robotic optical time‐domain survey that uses the Palomar 48 inch Schmidt telescope. With its wide‐field camera providing a 47 square degrees field of view, ZTF is capable of visiting the entire visible sky north of ‐30 degrees declination every three nights in the g and r bands, and at higher cadences in selected sky regions with the addition of the i‐band filter. I will present the ZTF data "ecosystem" that comprises the data‐processing pipelines, transient alert production and distribution system, machine learning frameworks, databases and data archives, as well as some of the endpoints and user interfaces for accessing and analyzing the data products. Francisco Förster (Center for Mathematical Modeling (CMM‐UChile) / Millennium Institute for Astrophysics (MAS))

The Universe in a Stream: Challenges and Progress of the ALeRCE Broker I will review the challenges and progress of the Automatic Learning for the Rapid Classification of Events (ALeRCE) astronomical alert broker. ALeRCE is a new alert annotation and classification system led by an interdisciplinary and interinstitutional group of scientists from U. Católica (DCC), U. Chile (CMM, DIE), U. Concepción (DCC), the Millennium Institute for Astrophysics (MAS) and U. Nacional Andres Bello (DCF) in Chile, in collaboration with international researchers from Caltech (CD3) and Harvard U. (IACS–SEAS). In this talk I will discuss some of the challenges associated to the problem of alert classification, including the ingestion, annotation, database management, training set building, distributed processing, machine learning classification and visualization of these alerts. I will show some early results based on the real‐time classification of image streams for the problem of alert classification and applications to the ZTF alert stream.

John Graham (Kavli Institute for Astronomy and Astrophysics, Peking University)

Limitations on IMF Variability as a Function of Metallicity By comparing SDSS data on hundreds of Supernovae host galaxies and a thousands of typical galaxies we can place unique limits on the ability of the Initial Mass Function (IMF) to vary as a function of the metallicity of the star‐forming environment. This puts considerable constraints on theoretical stellar population models which use a varying IMF at different stages of galaxy evolution. Melissa Graham (LSST/University of Washington)

The LSST Data Management Systems: Infrastructures for EMMA In the coming era of big telescopes, big surveys, and big data, breakthrough time‐domain science such as enabling multi‐messenger astrophysics will require breakthrough technologies. This talk will review the LSST Data Management System, with a particular emphasis on the data products most relevant for MMA and the practical aspects of how they will be accessed and analyzed by future users. Carl‐Johan Haster (LIGO Laboratory ‐ MIT Kavli Institute for Astrophysics and Space Research)

Gravitational Waves as a Piece of the Astrophysical Multi‐messenger Puzzle When gravitational waves finally joined the field of Multi‐Messenger Astrophysics in August 2017 it did so with both a bang and a flash. I will present the latest observational results from the Binary Neutron Star detection GW170817, focusing on the gravitational wave analyses, and their implications on the Neutron star Equation of State, Cosmological measurements and merger rates. I will also discuss the current and future strategies with which gravitational wave observations will aid with studies in Multi‐Messenger Astrophysics of both compact‐object binaries and other gravitational wave sources. Here I will put a special focus on the implications of the predicted increase in the detection rate of gravitational wave signals that will follow in tandem with the improvements of the sensitivities in the global network of gravitational wave detectors over the next decade.

Ann Hornschemeier (NASA GSFC)

Stellar‐origin Black Holes and Neutron Stars in the 2020’s and Beyond: The Post Chandra and XMM‐Newton Era

We present prospects for studying black hole (BH) and neutron star (NS) populations in nearby galaxies, focusing on science topics that will require next generation X‐ray telescopes. Higher‐ throughput X‐ray telescopes in the future will open up parameter space for time‐domain studies of accreting stellar origin BH and NS populations. The topics are wide‐ranging, from understanding gravitational wave merger progenitor populations such as Wolf‐Rayet X‐ray binaries to unraveling the complicated physics that allows for a population of “ultraluminous” pulsars which currently appear to defy our picture of how accretion works. We can also understand the birth of compact objects via supernova events through constraint of SN kicks in the dynamical evolution of X‐ray binaries. Capabilities such as a large field of view, improved angular resolution, increased sensitivity/effective area, and timing resolution are required to answer such questions and expand our understanding of accreting BH and NS systems. We will summarize the prospects for answering these questions based on our current knowledge and simulations of Athena Wide Field Imager observations of galaxies. Athena is an ESA mission planned for launch in ~2031 and the Wide Field Imager is an example of a next generation instrument that will be excellent for studies of BH and NS populations.

Emille Ishida (CNRS/LPC‐Clermont)

Human in the Loop: Adaptive Learning in Astronomy The full exploitation of the next generation of large scale photometric surveys depends heavily on our ability to provide reliable classifications based solely on photometric data. In preparation for this scenario, there has been many attempts to apply different machine learning algorithms to the transient photometric classification problem. Although different methods present different degree of success, text‐book machine learning methods fail to address the crucial issue of lack of representativeness between spectroscopic (training) and photometric (target) samples. In this talk I will show how Active Learning (or optimal experiment design) can be used as a tool for optimizing the construction of spectroscopic samples for classification purposes. I will present results on how the design of spectroscopic samples from the beginning of the survey can achieve optimal classification results with a much lower number of spectra than the current adopted strategy. Saurabh Jha (Rutgers University)

Multi‐Messenger Astrophysics: We Are The Messengers I'll talk about what kind of community we want for multi‐messenger astrophysics. Enabling science means enabling scientists.

Azadeh Keivani (Columbia University)

Multi‐messenger Gravitational‐Wave + High‐Energy Neutrino Searches Recent discoveries in multi‐messenger astrophysics have opened up new windows of exploration to the universe. The detection of gravitational waves (GW) from a binary neutron star merger followed by a short gamma‐ray burst recorded the first multi‐messenger event involving GWs. In addition, the detection of a high‐energy neutrino (HEN) followed by electromagnetic emissions from a flaring was the first compelling evidence for HEN source association. However, no astrophysical source has yet been observed to generate both GWs and HENs. Multi‐messenger searches for GWs and HENs provide important insights into the dynamics of and particle acceleration by black holes and neutron stars. The rapid identification of joint signals is crucial for electromagnetic follow‐up observations of transient emission that is only detectable for short periods of time. I will present the the latest sensitivity of realtime searches of HENs and GWs, and discuss the role of LSST in identifying electromagnetic counterparts to joint GW+HEN events. Wolfgang Kerzendorf (New York University)

DALEK ‐ Supernova Physics Meets Machine Learning Comparing sophisticated simulations with complex observations is one of the main challenges in modern astrophysics. The computational time requirements (several minutes for some of the simplest simulations) and large parameter spaces (sometimes several tens of parameters) prohibit an exploration using traditional techniques. The rapid growth of observational data exacerbates the problem of the mentioned data analysis. Thus, it is essential to have tools that allow automated extraction of meaningful physical quantities from the large data vaults.

I will present our supernova radiative transfer code (TARDIS ‐ Kerzendorf & Sim 2014) that can quickly synthesize supernova spectra with some physical accuracy (using well‐tested methods). We couple this code with a novel deep‐learning enabled emulator that can interpolate in the multi‐dimensional space and allow us to extract posterior density functions given data.

In this talk, I will introduce the code, give an overview of some of the preliminary results, and will close with an overview of our future research. Jamie Kinney (Google)

From Zero to ML ‐ Managing and Analyzing Astronomy Data on Google Cloud

Google Cloud offers a broad set of services that are useful to Astronomers. This presentation will demonstrate how to work with astronomy datasets such as Kepler, Hubble, and GAIA using a range of Google machine learning services.

Victor Francisco Ksoll (University of Heidelberg)

Characterising Extragalactic Pre‐Main‐Sequence Stars with Machine and Deep Learning Techniques Deep photometric surveys with the Hubble Space Telescope, such as the Hubble Tarantula Treasury Project (HTTP), which covers the region of 30 Doradus down to the half solar mass limit, and Measuring Young Stars in Space and Time (MYSST), covering the entire bubble of the star forming complex N44, provide unprecedented coverage of entire active star forming regions. We use the deep stellar catalogues of HTTP and MYSST to identify all the pre‐main‐sequence (PMS) stars of the respective regions. The photometric distinction of these stars from more evolved populations is, however, not a trivial task due to several factors that alter their colour‐magnitude diagram positions. To overcome this hurdle, we employ Machine Learning Classification techniques, including Random Forests and Support Vector Machines (SVM), on the HTTP and MYSST surveys to unveil their PMS stellar content. Our methodology consists of 1) carefully selecting the most probable low‐mass PMS stellar population of a prominent star forming cluster within the observed fields, 2) using these samples to train classification algorithms to build predictive models for PMS stars and 3) applying these models to identify the most probable PMS content across the entire observed regions. We further develop an Invertible Neural Network (INN) in order to predict the fundamental physical parameters of age and mass of the identified young stars and evaluate the spatial variations of these parameters across the entire star forming complexes.

Jennifer Lotz (Gemini Observatory)

GEMMA: Gemini in the Era of Multi‐Messenger Astronomy The goal of the GEMMA Program (Gemini in the Era of Multi‐Messenger Astronomy), funded by a major new award from the NSF, is to advance the role of Gemini Observatory in the MMA era. The program has been designed to maximize synergies with the transformative facilities coming online in the near future. The projects within GEMMA specifically focus on the areas of high spatial resolution and rapid‐response astronomy. The GEMMA Time Domain Astronomy (TDA) project will develop the infrastructure for incorporating Gemini’s telescopes into an efficient new system for following up transients identified by LSST, LIGO, and other time‐domain and multi‐ messenger surveys. The TDA project also includes development of automated data pipelines for rapid delivery of science‐quality reduced data. The Gemini North Adaptive Optics (GNAO) upgrade project will deliver the first queue‐operated multi‐conjugate AO system in the northern hemisphere. With a corrected field of about 2 arcmin and spatial resolution similar to that of JWST, GNAO will take advantage of Maunakea’s outstanding conditions for AO performance; the plan also includes eventual development of a ground‐layer AO system. This talk will provide an overview of the GEMMA Program and summarize our progress. Daniel Muthukrishna (University of Cambridge)

RAPID: Early Classification of Explosive Transients using Deep Learning

We present RAPID (Real‐time Automated Photometric IDentification), a novel time‐series classification tool capable of automatically identifying transients from within a day of the initial alert, to the full lifetime of a light curve. Using a deep recurrent neural network with Gated Recurrent Units (GRUs), we present the first method specifically designed to provide early classifications of astronomical time‐series data, typing 12 different transient classes (including supernovae, kilonovae, and rare transients). Our classifier can process light curves with any phase coverage, and it does not rely on deriving computationally expensive features from the data, making RAPID well‐suited for processing the millions of alerts that ongoing and upcoming wide‐ field surveys such as the Zwicky Transient Facility (ZTF), and the Large Synoptic Survey Telescope (LSST) will produce. The classification accuracy improves over the lifetime of the transient as more photometric data becomes available, and across the 12 transient classes, we obtain an average area under the receiver operating characteristic curve of 0.95 and 0.98 at early and late epochs, respectively. We have made RAPID available as a software package for machine learning‐ based alert‐brokers to use for the autonomous and quick classification of several thousand light curves within a few seconds. Jan‐Uwe Ness (ESAC)

Multi‐mission Coordinations The demand for multi‐observatory coordinated observations has continuously increased over the last decade, and the traditional way of achieving overlap between observations will become increasingly complex in the near future. We propose international standards, certified by VO, for observatories to provide their visibility and planning information in order to make better use of automated processes. Public automated access to visibility and past/present/future observations will allow a number of additional activities. We will describe the proposed VO standards and give examples of use cases. Kyle Rocha (Northwestern University)

Using Machine Learning to Predict Outcomes for Binary Stellar Evolution

Future big data surveys will provide new insights into stellar populations, gravitational wave sources, supernovae, and other transients, pushing the boundaries of current theoretical models. Work in these fields frequently relies on rapid binary population synthesis codes like Binary Star Evolution (BSE). Most of these codes use simple approximations to calculate the complicated processes that occur in binary stellar evolution. These codes have low computational cost but, as a result, may produce unreliable predictions. There exist much more accurate binary stellar evolution codes such as the Modules for Experiments in Stellar Astrophysics (MESA). These codes are three orders of magnitude more computationally demanding, making direct incorporation into population synthesis codes intractable. To effectively utilize the accuracy of MESA, we must develop methods for sampling high‐dimensional parameter space (e.g., initial mass, period, metallicity, etc.) which minimize the computational cost while maximizing accuracy. We investigate the potential use of machine‐learning techniques like Gaussian processes classification and regression to inform parameter space sampling. We demonstrate this technique on a set of MESA models and discuss how these methods can be transferable to other high dimensionality interpolation problems. Joshua Schlieder (NASA GSFC)

Nimble: A Mission Concept for Gravitational Wave Counterpart Astrophysics In August 2017, the first gravitational waves from merging neutron stars were detected coincident with a short gamma‐ray burst (sGRB) and triggered a world‐wide observing campaign to identify and characterize the associated kilonova emission. This event led to numerous firsts and discoveries that began to unveil the mysteries of these energetic astronomical phenomena. However, many questions remain and the field of multimessenger astrophysics is prime for further discovery. Here we describe Nimble, a NASA Explorers class mission concept that couples a very wide‐field gamma ray monitor with a multiwavelength telescope and rapid response spacecraft to enable the prompt detection and localization of sGRBs and follow‐up of kilonovae. We will describe the science drivers for Nimble and detail the current engineering concept. Nimble will discover and characterize the counterparts of neutron star merger gravtitational wave events and its flexible platform will allow for a wide range of additional multiwavelength time domain science. Ken Smith (Queen's University Belfast)

Lasair: The Transient Alert Broker for LSST:UK As more time‐domain surveys come online, producing ever increasing streams of data, the need to rapidly mine this data and produce timely, digestible alerts is more urgent than ever. The Zwicky Transient Factory (ZTF) is currently producing up to 10^6 real transient alerts per night. LSST is expected to increase that to 10^7 per night. We present Lasair ‐ the LSST:UK Transient Broker, a prototype interface to a relational database of explosive and eruptive transients based on the ZTF transient stream. ZTF detections are assimilated into objects, lightcurves rendered and objects are context crossmatched with large star and galaxy catalogues. Some example streams of objects are provided, and optional registration allows users to be alerted when transients are detected close to objects of interest. The database can be viewed via a web browser, and can also be queried via SQL and Jupyter notebooks. Additionally, as previously done with Pan‐STARRS1 and ATLAS transients, Lasair will be able to trigger alerts for ZTF transients within the high probability localisation regions of GW event skymaps.

* Scots and Irish Gaelic for 'flash' or 'flame'. Monika Soraisam (NOAO)

ANTARES: Brokering Alerts in Real‐time in the Big‐Data Era Current and upcoming optical surveys, first and foremost LSST, are poised to open up new avenues in almost all fields of astronomy, particularly in time‐domain astronomy, by going deeper, faster, and wider in panchromatic passbands. Taming the expected onslaught of their data is one of the biggest data challenges in astronomy. Up to 10 million alerts per night are expected from LSST, hidden in which will be rare time‐critical events requiring immediate follow‐ up. ANTARES is an automated software system that will sift through this barrage of data and select events that are deemed high‐priority by the community. The beta version of ANTARES is online and performing real‐time alert filtering of the public alert stream of the ZTF survey, which can be considered a precursor survey to LSST. In this talk, I will describe the various features of the ANTARES system, development efforts to scale to LSST, and how the community needs to be involved. Rachel Street (Las Cumbres Observatory)

Microlensing as a Case Study of Alert‐based Science and Technologies Like other transient phenomena, observations of microlensing events are by their nature, urgent ‐ virtually all observations must be acquired during a non‐repeating event of finite duration. The technological limitations of early microlensing surveys meant that follow‐up observations had to be made in rapid response to real‐time alerts, making it a case‐study for alert‐based science, and the technologies that evolved to achieve the scientific goals. These technologies are now being expanded to meet the demands of the Big Data era. I will describe the MARS alert broker system, and the Target and Observation Manager systems (TOMs) designed to harvest from it alerts of interest, including a machine learning approach to pre‐selecting high priority targets. I will outline plans to build a meta‐network of programmably‐interact$ telescope resources, AEON, with which TOMs will be able to conduct follow‐up observing campaigns on an industrial scale.

Nao Suzuki (Kavli IPMU, Univ of Tokyo)

HSC Transient Survey Hyper‐Suprime Cam (HSC) on Subaru telescope enables us to prove deep space for wide field of view (1.77 sqdeg). HSC transient survey brings us high‐z Type Ia and Type II supernova for cosmological studies as well as Superlumious Supernova (SLSN), Tidal Disruption Event (TDE), Rapid Transients and ones yet to be classified. HSC also participates in gravitational wave source follow‐up and simultaneous Fast Radio Burst (FRB) survey as well. We coordinate spectroscopic follow‐up with Subaru, VLT, Keck, Gemini, GTC, AAT and Hubble Space Telescope. We are in need of fast processing of the data to automated classification. Machine Learning is one of the key components for extracting science targets and classification, and we introduce our implementation on the Big Data in practice. Aaron Tohuvavohu (Penn State/Swift)

Swift in the Multi‐messenger Era Swift's multi‐wavelength instrumentation and uniquely rapid response allow it to play a critical dual role in time‐domain astrophysics. Swift serves as both a prompt discovery engine for GRBs and other high‐energy transients, as well as the only sensitive rapid follow‐up facility in UV and X‐rays for sources discovered elsewhere. I will overview Swift's critical contributions to GW and neutrino follow‐up to date, in particular the discovery of UV emission from the kilonova associated with GW170817 and rapid X‐ray observations and monitoring of TXS 0506+056 in response to IC‐170922. I will then describe new observatory capabilities and analysis pipelines being developed that will enable Swift to increase its utility even further for the time‐domain and multi‐messenger eras, as well as outline key science cases Swift can contribute to and natural synergies with other facilities. I will address how the community can further utilize these new capabilities for their science and challenges ahead in the high alert‐rate multi‐messenger era. Alexander J. van der Horst (George Washington University)

Probing the Transient Sky with SCORPIO SCORPIO is envisioned as a workhorse instrument for the Gemini Observatory in the 2020s, capable of wide‐band medium‐resolution spectroscopy and multi‐band imaging covering a broad spectral range, combined with high time resolution. These capabilities are very well suited for efficiently characterizing a large variety of transient and static sources detected by large‐scale surveys, in particular by the Large Synoptic Survey Telescope (LSST). Spectral coverage from the optical to the near‐infrared, in imaging and spectroscopy, is also crucial for detailed studies of the most extreme and catastrophic cosmic events such as massive stellar explosions and binary neutron star mergers. The high time resolution allows for studying fast changing phenomena, something that has been largely unexplored at Gemini sensitivities. This talk will discuss the broad range of scientific applications of SCORPIO, focusing on those where the new instrument will potentially have the largest impact, and its role in the new eras of time‐domain and multi‐ messenger astronomy. Darryl Wright (University of Minnesota)

Supporting Transient Surveys with Citizen Science Efficient identification and follow‐up of scientifically interesting astronomical transients is hindered by our ability to select the most promising amongst all. Rapid decision making is impeded by image artefacts, and difficulties inferring transient types from initial detections and sparse light curves. We will discuss how machine learning and citizen science have been combined in the Zooniverse project, Supernova Hunters, to outperform either technique individually . We will also show the infrastructure and machine learning methods that Zooniverse has developed in preparation for future transient surveys.

Confirmed Speakers INVITED SPEAKERS‐Confirmed

Iair Arcavi (Tel Aviv University) Sarah Burke‐Spoalor (West Virginia University) Michael Coughlin (Caltech/LIGO) Dave Coulter (University of California, Santa Cruz) Dmitry Duev (California Institute of Technology) Francisco Förster (CMM MAS) Melissa Graham (University of Washington) Emilie Ishida (Universite Clermont‐Auvergne) Saurabh Jha (Rutgers University) Carl Johann‐Haster (MIT/LIGO) Azadeh Keivani (Columbia University) Jamie Kinney (Google) Monika Soraisam (NOAO) Rachel Street (Las Cumbres Observatory) Aaron Tohuvavohu (Penn State/Swift) Alexander van der Horst (George Washington University)

Contributing Speakers EMMA CONTRIBUTING SPEAKERS

NAME AFFILIATION EMAIL ADDRESS

Kshitij Aggarwal West Virginia University [email protected]

Morten Andersen Gemini Observatory [email protected]

Igor Andreoni Caltech [email protected]

John Blakeslee Gemini Observatory [email protected]

Eric Burns NASA GSFC [email protected]

Kyle Chard University of Chicago [email protected]

Carlos Contreras STScI [email protected]

David Cook IPAC/Caltech [email protected]

Jeff Cooke Swinburne University [email protected] Kavli Institute for Astronomy and

John Graham Astrophysics, Peking University [email protected] Wolfgang

Kerzendorf NYU [email protected] University of Heidelberg, Centre for Victor Francisco Astronomy, Institute for Theoretical

Ksoll Astrophysics [email protected]‐heidelberg.de

Jennifer Lotz Gemini Observatory [email protected] Daniel

Muthukrishna University of Cambridge [email protected]

Jan‐Uwe Ness ESAC [email protected]

Kyle Rocha Northwestern University [email protected]

Joshua Schleider NASA GSFC [email protected]

Ken Smith Queen's University Belfast [email protected];

Nao Suzuki Kavli IPMU, Univ of Tokyo nao.suzuki@kavli‐ipmu.jp

Darryl Wright University of Minnesota [email protected]

Poster Abstracts Ultraviolet SEDs and Bolometric Luminosity

Peter Brown (Texas A&M University) The detection of an ultraviolet counterpart to GW170817 showed the great value in panchromatic observations in constraining models. I will review some of the complications in interpreting ultraviolet data in creating spectral energy distributions, constraining dust reddening, and measuring bolometric luminosities in model‐dependent and model‐agnostic ways.

Glowbug, a Gamma‐Ray Telescope for Bursts and Other Transients

C.C. Teddy Cheung (Naval Research Lab) We describe Glowbug, a gamma‐ray telescope for bursts and other transients in the 30 keV to 2 MeV band. It was recently selected for funding by the NASA Astrophysics Research and Analysis program, with an expected launch in the early 2020s. Similar in concept to the Fermi Gamma Burst Monitor (GBM) and with similar sensitivity, Glowbug will join and enhance future networks of burst telescopes to increase sky coverage to short Gamma‐Ray Bursts (SGRBs) from neutron star (NS) binary mergers, including possible SGRBs from NS‐black hole mergers. With the recent discovery of the SGRB coincident with the gravitational wave transient GW170817, we know such events occur with reasonable frequency. Expanded sky coverage in gamma rays is essential, as more detections of gravitational waves from such mergers by ground‐based interferometers will come in the next few years, and detecting an electromagnetic counterpart is a powerful probe of merger dynamics.

Work on Glowbug at NRL is supported by NASA and the Chief of Naval Research.

Authors: J.E. Grove (1), C.C. Cheung (1), M. Kerr (1), L.J. Mitchell (1), B.F. Phlips (1), R.S. Woolf (1), E.A. Wulf (1), C.A. Wilson‐Hodge (2), D. Kocevski (2), M.S. Briggs (3), J. Perkins (4), S. Guiriec (5), D.H. Hartmann (6)

1 U.S. Naval Research Laboratory 2 NASA Marshall Space Flight Center 3 University of Alabama, Huntsville 4 NASA Goddard Space Flight Center 5 George Washington University 6 Clemson University ESASky for Multi‐messenger Astrophysics

Guido De Marchi (European Space Agency) Facilitating the comparison of data collected by different telescopes and instruments across all wavelength domains is a fundamental step to enable efficient multi‐messenger astrophysics. ESASky is a discovery portal giving astronomers an easy way to access high‐quality scientific data from their computer, tablet, or mobile device. It already includes over half a million images, 300,000 spectra, and more than a billion catalogue sources, and its holdings are constantly growing. From gamma rays to radio wavelengths, it allows users to explore the cosmos with data from a dozen space missions from the astronomical archives of ESA, NASA, and JAXA and does not require prior knowledge of any particular mission.

ESASky features an all‐sky exploration interface, letting users easily zoom in for stars as single targets or as part of a whole galaxy, visualise them and retrieve the relevant data taken in an area of the sky with just a few clicks. Users can easily compare observations of the same source obtained by different space missions at different times and wavelengths. These features make it an ideal tool for the exploration of multi‐messenger astrophysics data. Indeed, soon after the gravitational wave signal GW170817 was observed by LIGO and Virgo, astronomers in search of possible electromagnetic counterparts turned to ESASky.

In this presentation, we will illustrate the many options to visualise and access astronomical data: interactive footprints for each instrument, tree‐maps, filters, and solar‐system object trajectories can all be combined and displayed. We will also show how astronomers can plan future observations with the James Webb Space Telescope by easily comparing the relevant portion of the sky as observed by Hubble and other missions. Finally, ESASky also includes access to scientific publications, allowing users to visualise on the sky all astronomical objects with associated scientific publications and to link directly back to the papers in the NASA Astrophysics Data System. The Gravitational‐wave Optical Transient Observer

Martin Dyer (University of Sheffield) The Gravitational‐wave Optical Transient Observer (GOTO) is a wide‐field telescope project aimed at detecting optical counterparts to gravitational wave sources. The prototype instrument was inaugurated in 2017, on La Palma, Canary Islands, and commissioning has been ongoing throughout 2018. GOTO is a robotic telescope using custom scheduling, control and image pipeline systems written in Python. The standard operating mode for GOTO is carrying out an all‐sky survey, and when a gravitational wave signal is detected it will automatically observe the resulting sky map based on the same fixed tiling grid. Once observations have been made the image analysis pipeline will detect any transient sources and, ultimately, feed back into the telescope control system to schedule follow‐up observations GOTO currently has four “unit telescopes” (UTs) on a single mount on La Palma, with four more to be added this year to make a total field‐of‐view of 40 square degrees. A second 8‐UT system is also planned for La Palma, as well as a southern node in Australia. The multiple instruments across the globe are anticipated to operate as a single integrated system; enabling greater sky coverage, faster follow‐up of transient events and more advanced scheduling strategies in order to maximize the chance of detecting gravitational wave counterparts. RATIR: A 1.5‐m Infrared Robotic Telescope for Transient Followup

Ori Fox (Space Telescope Science Institute) The Reionization And Transient InfraRed (RATIR) camera has been built for rapid transient followup and provides simultaneous optical and infrared photometric capabilities. Mounted on a 1.5‐m robotic telescope, RATIR offers sensitivities down to u~18.5, r~20.5, J~19.4, and H~18.6. Here I present some of the transient science that is possible with RATIR. Harnessing a network of small, robotic, and infrared telescopes will be an important asset for future LSST followup.

A New Approach to Following Transients with HST: Rolling Snapshots

Andy Fruchter (STScI), David Rubin (STScI), Mansi Kasliwal (STScI), Kishalay De (Caltech) We are now entering an era in which large scale surveys of the sky will discover numerous transients each night. The number of targets that could benefit from HST observations on timescales of less than three weeks will easily exceed the ability of HST to schedule disruptive ToO observations. We have proposed and are now testing a variant of snapshot scheduling that would allow transients to be observed as soon as 11 days after discovery with little to no additional overhead compared to a standard snapshot program. We call this new observational approach ``Rolling Snapshots.'' While any one object will have a low probability of being observed in such a program, the large number of transients available will make it possible to build up statistically significant samples, with the type of transient and exact observation scheme determined by the science under investigation. We have received several orbits of DD Time to apply this method using WFC3 NUV capabilities. In this poster we describe our early implementation of Rolling Snapshots, some preliminary results, and thoughts on possible future improvements of this method.

Type Ibn Supernovae May Not All Come from Massive Stars

Griffin Hosseinzadeh (Center for Astrophysics | Harvard & Smithsonian)

Type Ibn supernovae are a rare class of transients whose spectra show signatures of interaction with hydrogen‐poor circumstellar material. Compared to other interacting supernovae, their light curves relatively homogeneous and fast‐evolving. The leading theory has been that these are the explosions of very massive Wolf–Rayet stars in which material ejected by the supernova collides with mass lost from the progenitor through winds or eruptions. These stars should have short lifetimes and thus only be found in areas with active star formation. However, one of the ~30 Type Ibn supernovae occurred in a environment with no detectable star formation. I will present new HST observations of this environment, which strengthen the star formation limit below the levels of almost all known core‐collapse supernovae. In light of this limit, I will discuss whether all Type Ibn supernovae can come from massive stars. The Cosmostatistics Initiative

Emille Ishida (LPC‐Clermont) The Cosmostatistics Initiative (COIN) was founded in 2014 with the goal of overcoming the cultural barriers preventing the daily collaboration between researchers from different fields. Most of its activities are developed within the COIN Residence Program (CRP), a non‐structured meeting which utilizes a management model similar to technological start‐ups. Our approach enables rapid innovation in data‐science methodologies driven by scientific questions. Since its conception, COIN has grown to more than 60 researchers from six continents, from fields as diverse as astrophysics, statistics, computer science, epidemiology, biostatistics, and medical sciences. Moreover, the CRPs have proven to be one of the most productive events of its kind ‐ producing 12 (and 2 other in preparation) refereed scientific papers, three software packages, four value‐added galaxy catalogues, as well as discovery of more than 40 new stellar open clusters. All of this in its first 5 years. The poster describe how CRPs are organized and how experiences like COIN can provide insights about the future of our current academic model. Electromagnetic MHz Transients with VLITE and Beyond

Emil Polisensky (Naval Research Laboratory) The Naval Research Lab and the National Radio Astronomy Observatory have expanded the low frequency capabilities of the VLA through the VLA Low‐band Ionosphere and Transient Experiment (VLITE, vlite.nrao.edu). VLITE is a commensal observing system harvesting data from the prime focus in parallel with normal Cassegrain focus observing on a subset of VLA antennas, effectively making the instrument two telescopes in one. VLITE provides over 6000 observing hours per year and generates an average of 60 images per day with 3‐50 square degree field‐of‐ views using 64 MHz bandwidth centered on 352 MHz. By operating in parallel, VLITE offers invaluable low frequency data to targeted observations of transient sources detected at higher frequencies. With arcsec resolution and mJy sensitivity, VLITE additionally offers great potential for blind searches of rare radio‐selected coherent and incoherent transient emitters. VLITE‐SLOW employs a database and source association pipeline to catalog VLITE images and search for transients on timescales of a few seconds to years. We present the current status of the VLITE‐ SLOW transient science program from VLITE’s initial deployment on 10 antennas in November 2014 through its expansion to 16 antennas in July 2017, including the detection of outbursts from several X‐ray binaries and an upper limit on low frequency emission from GW170817. We extrapolate our experience with VLITE to make predictions for a full LOw‐band Observatory (LOBO) on the VLA and a ngLOBO system on the Next Generation VLA (ngVLA).

List of Posters # First Name Last Name Affiliation Title

1 Peter Brown Texas A&M University Ultraviolet SEDs and Bolometric Luminosity Glowbug, a Gamma‐Ray Telescope for Bursts 2 CC Teddy Cheung Naval Research Lab and Other Transients 3 Guido De Marchi ESA ESASky for Multi‐messenger Astrophysics The Gravitational‐wave Optical Transient 4 Martin Dyer University Of Sheffield Observer RATIR: A 1.5‐m Infrared Robotic Telescope 5 Ori Fox STScI for Transient Followup A New Approach to Following Transients 6 Andy Fruchter STScI with HST: Rolling Snapshots Type Ibn Supernovae May Not All Come 7 Griffin Hosseinzadeh Harvard/Smithsonian from Massive Stars 8 Emille Ishida CNRS The Cosmostatistics Initiative Electromagnetic MHz Transients with VLITE 9 Emil Polisensky Naval Research Laboratory and Beyond

Attendees First Name Last Name Email Address Institution Kshitij Aggarwal [email protected]; West Virginia University David Aguilera-Dena [email protected]; University Of Bonn Edward Ajhar [email protected]; National Science Foundation Morten Anderson [email protected]; Gemini Observatory Igor Andreoni [email protected]; California Institute Of Technology Iair Arcavi [email protected]; Tel Aviv University Christopher Berry [email protected]; Northwestern University University of Delaware/New York Frederica Bianco [email protected]; University Azalee Bostroem [email protected]; University of California, Davis Peter Brown [email protected]; Texas A&M University Sarah Burke-Spolaor [email protected]; West Virginia University Eric Burns [email protected]; NASA/GSFC Camacho- Yssavo Neves [email protected]; Rutgers University Kyle Chard [email protected]; University of Chicago Ashley Chrimes [email protected]; University Of Warwick Alice Cocoros [email protected]; JHU APL David Cook [email protected]; IPAC/Caltech Jeff Cooke [email protected]; Swinburne University Michael Coughlin [email protected]; California Institute Of Technology Dave Coulter [email protected]; University of California, Santa Cruz Mi Dai [email protected]; Rutgers University Phil Daly [email protected]; Steward Observatory (UAZ) Chris Davis [email protected]; NSF Rosa Diaz [email protected]; Space Telescope Science Institute Dmitry Duev [email protected]; California Institute Of Technology Martin Dyer [email protected]; University Of Sheffield Andreas Flörs [email protected]; Max Planck Institute For Astrophysics Ryan Foley [email protected]; University of California, Santa Cruz Francisco Forster [email protected]; CMM MAS Ori Fox [email protected]; Space Telescope Science Institute Andrew Fruchter [email protected]; Space Telescope Science Institute Monica Gallegos Garcia [email protected]; Northwestern University Suvi Gezari [email protected]; University of Maryland Ben Gompertz [email protected]; University Of Warwick John Graham [email protected]; Kavli Institute Melissa Graham [email protected]; University Of Washington / Lsst Matthew Hankins [email protected]; Caltech Carl-Johan Haster [email protected]; MIT LIGO Renee Hlozek [email protected]; University of Toronto Ann Hornschemeier [email protected]; NASA/GSFC Griffin Hosseinzadeh [email protected]; Harvard/Smithsonian Andy Howell [email protected]; Las Cumbres Observatory Tiara Hung [email protected]; University of California, Santa Cruz Emille Ishida [email protected]; CNRS Saurabh Jha [email protected]; Rutgers University Jian Jiang [email protected]; University of Tokyo Azadeh Keivani [email protected]; Columbia University Wolfgang Kerzendorf [email protected]; NYU/MSU Jamie Kinney [email protected]; Google Victor Ksoll [email protected]; University Of Heidelberg, Eva Laplace [email protected]; University Of Amsterdam Jennifer Lotz [email protected]; Gemini Observatory

Michael Lundquist [email protected]; University Of Arizona, Steward Observatory Thomas Matheson [email protected]; NOAO Adam McMaster [email protected]; University Of Oxford Maryam Modjaz [email protected] University of New York Ivelina Momcheva [email protected]; Space Telescope Science Institute Daniel Muthukrishna [email protected]; University of Cambridge Gautham Narayan [email protected]; Jan-Uwe Ness [email protected]; European Space Astronomy Centre Emil Polisensky [email protected]; Naval Research Laboratory Armin Rest [email protected]; Space Telescope Science Institute Massimo Robberto [email protected]; Space Telescope Science Institute Kyle Rocha [email protected]; Northwestern University Evan Scannapieco [email protected]; NASA Hq Joshua Schleider [email protected]; NASA/GSFC Nigel Sharp [email protected]; National Science Foundation Leo Singer [email protected]; NASA/GSFC Arfon Smith [email protected]; Space Telescope Science Institute Ken Smith [email protected]; Queen's University Belfast Monica Soraisam [email protected]; NOAO Niharika Sravan [email protected]; Purdue University Rachel Street [email protected]; Las Cumbres Observatory Carl Stubens [email protected]; Antares | Noao Nao Suzuki [email protected]; Kavli IPMU, University of Tokyo Aaron Tohuvavohu [email protected]; Penn State University/swift David Tytler [email protected]; University of California, San Diego Syed Uddin [email protected]; Carnegie Observatories Alexander van der Horst [email protected]; George Washington University Darryl Wright [email protected]; Zooniverse/University of Minnesota