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Roman at the 246th AAS Meeting
June 8th, 2025

Location: Anchorage, AK

Upcoming Events
July 14th, 2025
Cosmic Cartography with Roman: Advances in Galaxy Structures, Distributions, Dark Matter, and Dark Energy

January 8-12, 2025 (Anchorage, AK)

Town Hall: Nancy Grace Roman Space Telescope Town Hall

  • Nancy Grace Roman Space Telescope Town Hall
    (Monday, June 9, 6:30–8:00 p.m. AK; room TBD) CANCELED
    The Nancy Grace Roman Space Telescope is a NASA flagship mission planned for launch no later than May 2027. The Roman Space Telescope will perform breakthrough science in dark energy cosmology, exoplanet microlensing, and NIR sky surveys with its Wide Field Instrument. Roman will also feature the Coronagraph Instrument (CGI), a technology demonstration that will directly image and take spectra of exoplanetary systems using several novel technologies together for the first time in space. This session will cover the status of the project and upcoming opportunities for community involvement in planning and executing the science and technology demonstration aspects of Roman.

 

Workshops

(Sunday, June 8, 9:00–5:00 p.m. AK; Egan Convention Center, Room 13/14)

The Nancy Grace Roman Space Telescope is anticipated to generate close to 30 petabytes of data during its five-year primary mission, heralding a new era of big data in astronomy. As data sets grow too large for personal computers, virtual science platforms offer a solution by providing cloud-based data processing and analysis capabilities. The Roman Research Nexus is the science platform being developed to offer the astronomical community a cloud computing environment for Roman data. It couples data-code proximity with a pre-configured software environment and real-time collaboration tools, making it easier for users to work with data and in teams. The platform also includes pre-loaded notebook tutorials and scientific workflows tailored to specific astronomical use cases. Utilizing the JupyterLab environment, users can create Jupyter Notebooks that seamlessly integrate code, analysis results, data visualizations, and other functionalities for handling astronomical images, spectra, and catalogs. This one-day workshop will provide the scientific community with an introductory overview of the Roman Research Nexus, which will be made available to the science community in Summer 2025. In addition to offering hands-on training, we aim to gather feedback, understand the needs of the user community, and identify ‘early adopters’ interested in utilizing the system for precursor science prior to the Roman launch. The workshop will include both directed training and independent exploration exercises (i.e., hack hours). The training will feature presentations and short tutorials, alternating with hands-on practical exercises focused on exploring several high-level workflows. Examples include an introduction to Roman data reduction tools, learning how to work with the ASDF file format, and using visualization and simulation tools such as Jdaviz (image visualization), Pandeia (Exposure Time Calculator), RIST (Roman Interactive Sensitivity Tool), STIPS (Space Telescope Image Product Simulator), and WebbPSF for Roman (PSFs simulator). Attendees will also learn how to access and analyze state-of-the-art Roman simulations from the Open Universe project (Troxel et al. 2023), which includes simulated wide-field and time-domain Roman data, as well as how to simulate their own data using Roman simulation tools. This course is aimed at astronomers and scientists at all stages of their education and careers. A basic knowledge of Python and familiarity with astronomical data concepts (e.g., data reduction, photometry) is expected. Prior experience with science platforms, Jupyter Notebooks, or the Roman mission is not required. This workshop requires registration. Participants will need personal computers and should set up Roman Research Nexus accounts in advance with help from the workshop organizers. A group list will be compiled approximately one month before the workshop to distribute software requirements and facilitate collaborative troubleshooting.

 

Oral Splinter Sessions

  • Preparing for the Nancy Grace Roman Space Telescope's First Call for Proposals
    (Monday, June 9, 12:30–2:00 p.m. AK; Egan Convention Center, Room 11/12)
    NASA’s Nancy Grace Roman Space Telescope is scheduled for launch no later than May 2027. As the mission approaches, there are increasing opportunities for the scientific community to become actively involved, culminating in the first Call for Proposals expected to be released in Fall 2025. Since all Roman data will be public immediately, the Call for Proposals will include support for analyzing archival data as well as the opportunity to propose for new surveys. This splinter meeting is designed to provide attendees with the information and resources they need to begin to plan their Roman proposals. Representatives from the Roman project and the Roman Science Centers at IPAC and STScI will provide information about the implementation of Roman’s community-defined surveys, data products that will be available, and the Roman proposal process. Additionally, we will discuss some of the key tools to support Roman’s proposal and science planning, including the Roman Telescope Proposal System (RTPS), the Astronomer’s Proposal Tool (APT), the Exposure Time Calculator (ETC), the Roman Image Simulator (Roman I-Sim), and the Roman Research Nexus, a powerful science platform designed to support collaborative research, data analysis, and community engagement.
  • Roman Spectroscopy Data Challenge (Part 2/3)
    (Tuesday, June 10, 9:00–11:00 a.m. AK; Egan Convention Center, Room 2) CANCELED
    NASA’s Nancy Grace Roman Space Telescope, scheduled for launch in 2026/27, will provide groundbreaking insights into the universe through its widefield slitless spectroscopy capabilities. As the mission launch approaches, the scientific community must develop expertise in handling Roman's spectral data, particularly in preparation for the first call for proposals in fall 2025. This splinter session serves as the second part of the Roman spectroscopic data challenge. It will build upon the foundations laid in the first session (January 2025), but will also be accessible to newcomers. The main objectives of this session are to (1) provide a refresher on Roman grism spectroscopy, (2) an introduction to Roman prism spectroscopy; and (3) introduce spectral extraction techniques that convert two-dimensional spectroscopic data to 1D spectra. By engaging in this session, participants will gain basic understanding of spectroscopy and the unique features of Roman. The discussions are intended to foster collaborations so that the scientific community is well-prepared to maximize the potential of Roman’s spectroscopic data.

 

Oral Special Sessions

  • Roman Community Surveys
    (Monday, June 9, 10:00–11:30 a.m. AK; Egan Convention Center, Room 13/14) CANCELED
    The Nancy Grace Roman Space Telescope's Wide Field Instrument (WFI) will have a large field of view (0.28 sq deg), Hubble-like sensitivity and resolution, and highly efficient survey operations. Roman's WFI observing program will include both Core Community Surveys and General Astrophysics surveys, defined by a combination of a community-led process and traditional peer-reviewed calls for proposals. The Core Community Surveys will include a High Latitude Wide Area survey, a High Latitude Time Domain survey, and a Galactic Bulge Time Domain survey. In addition to addressing Roman's science requirements related to cosmology and exoplanet demographics, the science community has described an exciting range of science investigations that can be undertaken with data from these surveys, given appropriate observational strategies (https://roman.gsfc.nasa.gov/science/ccs_community_input.html). The community-led effort to define Roman's Core Community Surveys, and the Roman Galactic Plane General Astrophysics Survey will be completed this Spring. The Roman Observations Time Allocation Committee have reviewed the survey implementation reports from the committees tasked with defining community-defined surveys, and will provide a recommendation on the implementation of each survey. The purpose of this session is to give attendees an overview of the recommended survey strategy for Roman for each of the core community surveys and for the Galactic Plane Survey, and provide an opportunity for detailed discussion of the associated science capabilities.

 

Oral Session Talks

  • Impacts of Photometric Calibration Uncertainties on Light-Curve Models and Cosmological Constraints in Stage IV Supernova Surveys - K. Anumba (Duke U.) et al.
    (Monday, June 9, 11:00–11:10 a.m. AK; Dena'ina Civic & Convention Center, Tubughnenq' 4)
    In the coming years, upcoming stage IV surveys, such as the Legacy Survey of Space and Time (LSST) and the Nancy Grace Roman Space Telescope, are expected to discover nearly a million supernovae—several orders of magnitude beyond current discoveries. Using Type Ia Supernovae (SNe Ia) to constrain cosmological parameters, including the dark energy equation of state, requires a precise spectro-photometric model for supernova time-series data. One of the largest systematic uncertainties in cosmological analysis is the model’s accuracy and it depends on the photometric calibration of the surveys. Here, we leverage advanced simulations of the LSST and Roman surveys to train a light-curve model, assessing its accuracy and precision across the optical to near-infrared wavelengths that these surveys will explore. Additionally, we present an initial analysis of how modifications to specific aspects of the observing strategy could influence model precision. Finally, we provide guidance for reproducing this work and utilizing our trained models to forecast cosmological constraints achievable by these next-generation surveys.
  • Building Public Excitement and Awareness Around the Science Enabled by NASA’s Nancy Grace Roman Space Telescope - B. Lawton (STScI) et al
    (Monday, June 9, 10:50–11:00 a.m. AK; Dena'ina Civic & Convention Center, Tubughnenq' 5)
    In the coming years, upcoming stage IV surveys, such as the Legacy Survey of Space and Time (LSST) and the Nancy Grace Roman Space Telescope, are expected to discover nearly a million supernovae—several orders of magnitude beyond current discoveries. Using Type Ia Supernovae (SNe Ia) to constrain cosmological parameters, including the dark energy equation of state, requires a precise spectro-photometric model for supernova time-series data. One of the largest systematic uncertainties in cosmological analysis is the model’s accuracy and it depends on the photometric calibration of the surveys. Here, we leverage advanced simulations of the LSST and Roman surveys to train a light-curve model, assessing its accuracy and precision across the optical to near-infrared wavelengths that these surveys will explore. Additionally, we present an initial analysis of how modifications to specific aspects of the observing strategy could influence model precision. Finally, we provide guidance for reproducing this work and utilizing our trained models to forecast cosmological constraints achievable by these next-generation surveys.
  • Measuring Mass of a Wide Orbit planet using Roman Microlensing Mass Measurement Method - A. Bhattacharya (NASA GSFC)
    (Monday, June 9, 3:00–3:10 p.m. AK; Dena'ina Civic & Convention Center, Ballroom A)
    Roman Space Telescope is going to launch in Oct 2026 and one of the main missions of Roman is to complete the exoplanet census with detecting and measuring masses of wide orbit planets. I would talk in this presentation about OGLE-2008-BLG-355, an event that showed planetary signals in 2008 and then followed up by HST and Keck high resolution imaging in 2018. The talk will focus on the method of detecting this sub neptune planet in wide orbit and how this precursor study is going to be a building block for mass measurements of 1500+ wide orbit planets in Roman era.
  • Predicting Roman WFI’s Capability to Detect High-z Quasars - M. Singha (NASA GSFC)
    (Monday, June 9, 2:40–2:50 p.m. AK; Dena'ina Civic & Convention Center, Tubughnenq' 4)
    High-redshift quasars are important for understanding the early universe, as they provide insights into the formation of supermassive black holes and cosmic reionization. These objects serve as probes of the universe's first billion years, helping us investigate its conditions during this time.To predict Roman's capability in detecting high-redshift quasars, we simulate Roman WFI grism spectra for quasars with redshifts ranging from 6 to 10 and bolometric luminosities between 10^{42} - 10^{47} erg/s. While color selection can identify bright quasars, it struggles with faint ones (J_AB>24), necessitating spectroscopy to distinguish quasars from other objects like brown dwarfs. With the Roman WFI grism, we can detect quasars up to AB magnitudes of 25, extending its reach to faint quasars that are otherwise difficult to identify. In this talk, I will discuss how we can distinguish quasar spectra from brown dwarfs, which are potential contaminants, and highlight the implications for detecting quasars in the first billion years.
  • 3d scene reconstruction using Roman slitless spectra - T. Astraatmadja (STScI) et al.
    (Tuesday, June 10, 10:50–11:00 a.m. AK; Dena'ina Civic & Convention Center, Tubughnenq' 4)
    The Nancy Grace Roman Space Telescope will carry out a wide-field imaging and slitless spectroscopic survey of Type Ia Supernovae (SNe Ia) to improve our understanding of dark energy. Proposed SN Ia surveys will be carried out using Roman's Wide Field Instrument (WFI), consisting of seven filters covering 7500--20000 Ångstrom as well as slitless prism and grism for spectroscopy. Crucial to this endeavor is obtaining supernova spectra uncontaminated by light from their host galaxies. However, obtaining such spectra is made more difficult by the inherent problem in wide-field slitless spectroscopic surveys: the blending of spectra of close objects. The spectrum of a supernova will blend with the host galaxy, even from regions distant from the supernova on the sky. If not properly removed, this contamination will introduce systematic bias when the supernova spectra are later used to determine intrinsic supernova parameters and to infer the parameters of dark energy. We address this challenge by developing an algorithm that makes use of the spectroscopic observations of the host galaxy at all available observatory roll angles to reconstruct a three-dimensional (3d; 2d spatial, 1d spectral) representation of the underlying host galaxy that accurately matches the 2d slitless spectrum of the host galaxy when projected to an arbitrary rotation angle. We call this ``scene reconstruction''. The projection of the reconstructed scene can be subtracted from an observation of a supernova to remove the contamination from the underlying host. Using simulated Roman data, we show that our method has extremely small systematic errors and significantly less random noise than if we subtracted a single perfectly aligned spectrum of the host obtained before or after the supernova was visible.
  • Synthetic star surveys in simulated nearby galaxies in preparation for a Roman Infrared Nearby Galaxy Survey - A. Thob (U. Penn.) et al.
    (Tuesday, June 10, 10:20–10:30 a.m. AK; Dena'ina Civic & Convention Center, Tubughnenq' 3)
    The Nancy Grace Roman Space Telescope's Wide Field Instrument (WFI) will provide an unprecedented opportunity to resolve stellar populations in hundreds of nearby galaxies, enabling precise studies of their star formation histories, dark matter distributions, stellar halo structures and assembly histories. To prepare for these surveys, the Roman Infrared Nearby Galaxy Survey (RINGS) team is developing a pipeline to generate synthetic star catalogs of nearby galaxies on demand, leveraging high-resolution hydrodynamical simulations and isochrone modeling techniques. As a proof of concept, we present mock surveys of M83, M51, and the stellar halo of Cen A, constructed using the py-ananke framework applied to simulated analogs from the Latte suite of FIRE cosmological simulations of galaxy formation. These synthetic surveys provide photometry in all planned Roman WFI bands and produce key astrometric properties, including proper motions. The pipeline is optimized for efficient data management, subdividing the resulting surveys using a multi-order coverage (MOC) HEALPix tessellation in (RA, Dec) that dynamically adapts to the underlying stellar density. Future updates will incorporate both dust extinction and crowding models to further enhance the realism of the synthetic surveys. The pipeline is designed to be highly adaptable, allowing users to generate tailored mock surveys for a wide range of nearby galaxies with varying stellar density regimes, metallicities, and viewing angles. Moreover, its capabilities extend beyond Roman's WFI, enabling multi-wavelength survey planning across different observatories. We describe the current status of this pipeline, its planned integration with community-accessible data resources such as the Roman Research Nexus, and its potential applications for optimizing Roman survey planning and data analysis. Finally, we compare these synthetic surveys with expectations from Euclid and Rubin observations, highlighting their role in refining our understanding of resolved stellar populations in diverse galactic environments.
  • Survey Design Variables: Impact on Bound Planet Yields and Characterization in the Roman Galactic Bulge Time Domain Survey - F. Zohrabi & M. Penny (LSU)
    (Tuesday, June 10, 3:10–3:30 p.m. AK; Dena'ina Civic & Convention Center, Ballroom A)
    The Nancy Grace Roman Space Telescope will significantly advance our understanding of cold exoplanet demographics through its Galactic Bulge Time Domain Survey (GBTDS). As part of my dissertation, I investigate the impact of key survey design variables—including cadence, exposure time, field selections, and multi-color observing strategies—on bound planet yields for the GBTDS. Beyond detecting exoplanets, a critical challenge lies in characterizing these systems, particularly when it comes to measuring the mass and distance of lens stars. Using the GULLS simulator, I have generated a large sample of bound planet microlensing events across a range of planetary masses under various survey strategies. I have further enhanced the GULLS simulator to incorporate Fisher Matrix analysis, enabling uncertainty estimates for microlensing parameters in detectable events. These estimates allow us to evaluate Roman exoplanet survey's ability to constrain lens properties and compare the effectiveness of different observing strategies in terms of planet characterization rather than detection alone.

 

Exhibitor Theater Presentations

  • Announcing the Roman Space Telescope Community Surveys - TBD
    (Tuesday, June 10, 2:30–3:00 p.m. AK; Dena'ina Civic & Convention Center, Exhibit Hall)
    The Nancy Grace Roman Space Telescope's Wide Field Instrument (WFI) will have a large field of view (0.28 sq deg), Hubble-like sensitivity and resolution, and highly efficient survey operations. Roman's WFI observing program will include both Core Community Surveys and General Astrophysics surveys, defined by a combination of a community-led process and traditional peer-reviewed calls for proposals. The Core Community Surveys will include a High Latitude Wide Area survey, a High Latitude Time Domain survey, and a Galactic Bulge Time Domain survey. In addition to addressing Roman's science requirements related to cosmology and exoplanet demographics, the science community has described an exciting range of science investigations that can be undertaken with data from these surveys, given appropriate observational strategies. The community-led effort to define Roman's Core Community Surveys has recently concluded. The Roman Observations Time Allocation Committee (ROTAC) provided a recommendation on the implementation of each survey. A similar process is underway for the Galactic Plane Survey, a community defined Early Definition General Astrophysics Survey. This talk will give a brief overview of the community definition process and the recommended survey strategy for Roman for each of the Core Community Surveys.

 

iPoster Sessions

  • Assessing Lens Mass and Distance Precision for the Roman Galactic Exoplanet Survey: Methodologies and Implications for Exoplanet Microlensing Characterization using PyLIMASS - C. McGee & K. Cahoy (MIT)
    (Tuesday, June 10, 5:30–6:30 p.m. AK)
    Gravitational microlensing is fundamentally a manifestation of how mass curves spacetime, causing light to bend along geodesics. While we typically discuss stars and planets as discrete objects, their gravitational effects can be analyzed within the broader framework of particle physics, where massive bodies act as particles in gravitational interactions, consistent with general relativity's predictions for how mass influences the propagation of light. The upcoming Nancy Grace Roman Space Telescope (Roman) will conduct the Galactic Exoplanet Survey (RGES), designed to detect and characterize exoplanets via gravitational microlensing. A key science objective is to determine the masses and distances of exoplanet host stars with at least 20% precision. We employ three independent methodologies to evaluate the precision of lens mass and distance measurements. The first two methods analyze previously discovered ground-based microlensing events with high-resolution follow-up imaging, applying direct lens flux measurements to infer host star properties. The third method utilizes PyLIMASS to generate Fisher matrix approximations, propagating uncertainties from light curve parameters to constraints on mass and distance. Our findings indicate that image-constrained modeling of lens flux photometry provides mass measurements within 20% uncertainty for a significant fraction of the surveyed events. This study is part of an ongoing effort to refine RGES predictions and improve the accuracy of exoplanetary system characterization. The results will inform survey optimization strategies, ensuring that Roman delivers precise host star mass and distance measurements. Future work will incorporate refinements to PyLIMASS simulations, particularly in handling parameter degeneracies, to further enhance measurement precision. Our findings will be critical for exoplanet population studies, microlensing event classification, and optimizing follow-up observations for exoplanetary host star analysis. This work contributes to the broader efforts in space-based microlensing and will play a pivotal role in advancing exoplanet detection methodologies in the era of Roman's high-cadence, wide-field infrared observations.
  • Improved Characterization of Type Ia Supernovae as Standard Candles for the Roman Space Telescope's Supernova Cosmology Mission - D. Jones (U. Hawaii) et al.
    (Wednesday, June 11, 9:00–10:00 a.m. AK)
    The Roman Space Telescope, NASA's next flagship observatory, will be tasked with making a generation-defining measurement of dark energy from Type Ia supernovae (SNe Ia) and other probes. However, producing the best cosmological constraints will require accurate 1) SN classifications, 2) building of the SN standardization model, and 3) characterization of high-redshift host galaxies. I describe efforts by members of the Supernova Cosmology Project Infrastructure Team to produce these components of the broader SN Ia cosmology effort. Ongoing work includes stress-testing SN Ia classification methodologies at high redshift, building an end-to-end cosmology pipeline that includes SN Ia model training, with model and calibration uncertainties, as a core component, and building fast, reliable inference of host-galaxy properties through the Blast framework.
  • Roman Mission Pipeline Processing of Prompt Products with Efficient Data Management and Archive Access - T. Desjardin (U. Hawaii) et al.
    (Wednesday, June 11, 9:00–10:00 a.m. AK)
    The Nancy Grace Roman Space Telescope (Roman) will be NASA’s first petabyte-scale astrophysics mission, producing an unprecedented volume of imaging and spectroscopic data. Processing the data from the 302-megapixel Wide Field Instrument (WFI) will require robust, automated processing pipeline to ensure the timely release of scientific data products.. The Roman Calibration Pipeline (RomanCal) has been developed to calibrate all WFI data for instrumental effects as well as produce mosaics, catalogs, and other high-level data products for the WFI imaging mode. During operations, rate images from each detector will be made available as prompt products via the Barbara A. Mikulski Archive for Space Telescopes (MAST), shortly after the observations are completed, once the downlinked data are processed by the ground system. Prompt versions of higher-level data products include visit-level mosaics and single-band source catalogs. This presentation provides an update on Roman’s prompt data products, their creation, and planned public access to enable astronomical research.
  • The Roman Telescope Proposal System - P. Lowrance (Caltech/IPAC) et al.
    (Thursday, June 12, 9:00–10:00 a.m. AK)
    The Nancy Grace Roman Space Telescope’s General Investigator program will include funding for research analyzing data from the Core Community Surveys and acquiring new observations. The General Astrophysics Surveys (GAS), for which a minimum of 25% of Roman’s observing time will be reserved in the first five years, will primarily be selected via traditional peer-review process. The Roman Telescope Proposal System (RTPS) is currently being designed by the Science Support Center at Caltech/IPAC to facilitate proposal submission and panel review for all the General Investigations. This poster will highlight the current infrastructure built to use a web-based single-stage proposal form, allow for multiple re-submissions of proposals, and notify users of a successful submission. The current design also supports the panel review process, flexible panel creation and management, and user-friendly proposal review, all with Dual-Anonymous Peer Review (DAPR).
  • The Roman Research Nexus: Enabling Low-Barrier Access and Collaboration in the Cloud - G. De Rosa (STScI) et al.
    (Thursday, June 12, 1:00–2:00 p.m. AK)
    Science platforms offer a unified user experience for discovering, exploring, accessing, and analyzing data. As astronomy enters an era of petabyte-scale data, cloud-based science platforms will become essential interfaces between researchers and observational data. The Nancy Grace Roman Space Telescope (Roman) is NASA's next flagship astrophysics mission. With its wide field of view and unprecedented survey speed, Roman’s Wide Field Instrument is anticipated to generate an estimated 30 petabytes (PB) of data during its five-year primary mission. The Space Telescope Science Institute (Roman Science Operations Center) has developed the Roman Research Nexus, a user-friendly science platform focused on low-barrier access and collaboration to prepare for Roman’s scientific discoveries. In this poster, we present simulated datasets, Jupyter notebook tutorials, science workflows, and other tools for the community to prepare for and engage with Roman. These resources demonstrate the Nexus's capabilities and ease of use to help prepare users for a new era in observational astronomy.
  • Overview of the Astronomer's Proposal Tool for the Roman Space Telescope - C.-P. Lajoie (STScI) et al.
    (Thursday, June 12, 1:00–2:00 p.m. AK)
    The Nancy Grace Roman Space Telescope is NASA’s next flagship astrophysics mission, with a planned five-year primary mission comprised mainly of Core Community-defined Surveys and, to a lesser extent, General Astrophysics Surveys. The latter will be solicited via calls for proposals and will be peer reviewed, with the first call planned for the Fall of 2025. Roman General Investigators will design their observations with Roman’s Wide Field Instrument through the Astronomer's Proposal Tool (APT). The Roman APT offers a new hierarchy to design large surveys and includes tools for creating mosaics and large region targets, as well as on-sky visualizations using Aladin. Demonstration programs are available in the APT menu, and extensive user documentation is provided in the Roman APT Users Guide, available on the Roman documentation system. Here, we provide an overview of the Roman APT and highlight key features of interest to Roman observers. Questions or feedback can be sent to the Roman help desk.
  • Desktop-based Simulation Tools for the Roman Space Telescope - W. Schultz (STScI) et al.
    (Thursday, June 12, 1:00–2:00 p.m. AK)
    With an expected data volume that surpasses the combined output of all previous NASA flagship astrophysics missions, the upcoming Nancy Grace Roman Space Telescope (Roman) is primed to produce arrays of unique data products. The Roman Science Operations Center (SOC) at the Space Telescope Science Institute maintains a suite of software and documentation made to help the astronomical community prepare to analyze these data. These tools simulate imaging data produced by Roman's Wide Field Instrument with varying levels of fidelity tailored to their intended purposes. This poster highlights the SOC's desktop-based simulation offerings, including point-spread function modeling through STPSF (formerly WebbPSF) and image simulation via the Space Telescope Imaging Product Simulator (STIPS) and Roman I-Sim. The SOC also supports the Roman Exposure Time Calculator, which is covered in a companion poster.