Preparations for Next Moonwalk Simulations Underway (and Underwater)
The engineering club from Palmdale High School in Palmdale, California, visits NASA's Armstrong Research Flight Center in Edwards, California. The students took a group photo in front of the historic X-1E aircraft on display at the center.
NASA/Genaro Vavuris
A group of enthusiastic high school students recently visited NASA to learn about facilities and capabilities that enable the agency's researchers to explore, innovate, and inspire for the benefit of humanity.
Engineering club students from Palmdale High School in California were able to connect classroom lessons to real-world applications, sparking curiosity and ambition while at NASA's Armstrong Flight Research Center in Edwards, California. "I learned a lot about the different
careers
that you can get at a place like NASA," student Roberto Cisnero said.
Through partnerships with the regional STEM community, NASA's
STEM Engagement
provides local students with hands-on opportunities aligned with NASA's missions. "Many students do not get the opportunity to be encouraged to pursue STEM careers. Part of our NASA mission is to be that encourager," said Randy Thompson, deputy director for NASA Armstrong Research and Engineering.
Highlights from the visit included demonstrations at a mission control room, the Subscale Flight Research Laboratory, the
Flight Loads Laboratory
, and the Experimental Fabrication Shop, all of which support high-risk, atmospheric flight research and test projects. Students engaged with laboratory technicians, engineers, and program managers, asking questions about the work they do. "It was fun to see what the valued people at NASA do with all of the resources,” student Jonathan Peitz said.
NASA's California Office of STEM Engagement hosted the visit in celebration of National Aviation History Month. By supporting students, educators, and expanding STEM participation, NASA aims to inspire future leaders and build a diverse, skilled workforce.
Students examine the Global Hawk Fairing Load Test at the Experimental Fabrication Shop at NASA's Armstrong Research Flight Center in Edwards, California. The students are from the engineering club from Palmdale High School in Palmdale, California.
NASA/Steve Freeman
Students tour a control room at NASA's Armstrong Research Flight Center in Edwards, California. The students are from the engineering club at Palmdale High School in Palmdale, California.
NASA/Steve Freeman
Students look at a subscale model at the Dale Reed Subscale Flight Research Laboratory at NASA's Armstrong Research Flight Center in Edwards, California. The students are from the engineering club from Palmdale High School in Palmdale, California.
NASA/Steve Freeman
Students examine small parts made at the Experimental Fabrication Shop at NASA's Armstrong Research Flight Center in Edwards, California. The students are from the engineering club from Palmdale High School in Palmdale, California.
NASA's Small Spacecraft Systems Virtual Institute (S3VI) is pleased to announce the official release of the highly anticipated 2024 State-of-the-Art Small Spacecraft Technology report. This significant accomplishment was made possible by the contributions of numerous dedicated people across NASA who graciously supported the preparation of the document as authors and reviewers. We also want to extend our gratitude to all the companies, universities, and organizations that provided content for this report.
The 2024 report can be found online at
https://www.nasa.gov/smallsat-institute/sst-soa
. The report is also available in PDF format as a single document containing all report content as well as individual chapters available on their respective chapter webpages. This 2024 edition reflects updates in several chapters to include: the Formation Flying and Rendezvous and Proximity Operations section within the "Guidance, Navigation, and Control" chapter; the Additive Manufacturing section within the "Structures, Materials, and Mechanisms" chapter; the Free Space Optical Communications section within the "Communications" chapter; and the Hosted Orbital Services section within the "Complete Spacecraft Platforms" chapter.
As in previous editions, the report contains a general overview of current state-of-the-art SmallSat technologies and their development status as discussed in open literature. The report is not intended to be an exhaustive representation of all technologies currently available to the small spacecraft community, nor does the inclusion of technologies in the report serve as an endorsement by NASA. Sources of publicly available date commonly used as sources in the development of the report include manufacturer datasheets, press releases, conference papers, journal papers, public filings with government agencies, and news articles. Readers are highly encouraged to reach out to companies for further information regarding the performance and maturity of described technologies of interest. During the report's development, companies were encouraged to release test information and flight data when possible so it may be appropriately captured. It should be noted that technology maturity designations may vary with change to payload, mission requirements, reliability considerations, and the associated test/flight environment in which performance was demonstrated.
Suggestions or corrections to the 2024 report toward a subsequent edition, should be submitted to the NASA Small Spacecraft Systems Virtual Institute
Agency-SmallSat-Institute@mail.nasa.gov
for consideration prior to the publication of the future edition. When submitting suggestions or corrections, please cite appropriate publicly accessible references. Private correspondence is not considered an adequate reference. Efforts are underway for the 2025 report and organizations are invited to submit technologies for consideration for inclusion by August 1, 2025.
NASA's Small Spacecraft Technology program within the Space Technology Mission Directorate funds the Small Spacecraft Systems Virtual Institute.
Summary of the 10th DSCOVR EPIC and NISTAR Science Team Meeting
Introduction
The 10
th
Deep Space Climate Observatory
(DSCOVR)
Earth Polychromatic Camera
(EPIC) and
National Institute of Standards and Technology (NIST) Advanced Radiometer
[NISTAR] Science Team Meeting (STM) was held October 16-18, 2024. Over 50 scientists attended, most of whom were from NASA's Goddard Space Flight Center (GSFC), with several participating from other NASA centers, U.S. universities, and U.S. Department of Energy laboratories. There was one international participant - from Estonia. A full overview of
DSCOVR's Earth-observing instruments
was published in a previous article in
The
Earth Observer
and will not be repeated here. This article provides the highlights of the 2024 meeting. The meeting agenda and full presentations can be downloaded from GSFC's
Aura Validation Data Center
.
Opening Presentations
The opening session of the 10
th
DSCOVR STM was special.
Former
U.S., Vice President Al Gore
attended the opening session and gave a presentation at the panel discussion "Remote Sensing and the Future of Earth Observations" - see
Photo
. Gore was involved in the early days of planning the DSCOVR mission, which at that time was known as Triana. He reminisced about his involvement and praised the team for the work they've done over the past decade to launch and maintain the DSCOVR mission. Following the STM Opening Session, Gore spoke at a GSFC Engage session in Building 3 later that afternoon on the same topic, but before a wider audience. [Link forthcoming.]
Following Gore's remarks, the remainder of the opening session consisted of a series of presentations from DSCOVR mission leaders and representatives from GSFC and National Oceanic and Atmospheric Administration (NOAA).
Thomas Neumann
[GSFC, Earth Sciences Division (ESD)-
Deputy Director
] opened the meeting and welcomed Vice President Gore and the STM participants on behalf of the ESD.
Adam Szabo
[GSFC-
DSCOVR Project Scientist
] briefly reported that the spacecraft was still in "good health." The EPIC and NISTAR instruments on DSCOVR continue to return their full science observations. He also gave an update on DSCOVR Space Weather research.
Alexander Marshak
[GSFC-
DSCOVR Deputy Project Scientist
] briefly described DSCOVR mission history and the science results based on DSCOVR observations from the first Sun-Earth
Lagrange point
(hereinafter, the L1 point). He also summarized the major EPIC and NISTAR results to date. At this time, more than 125 papers related to DSCOVR are listed on the
EPIC website
.
Elsayed Talaat
[NOAA, Office of Space Weather observations-
Director
] discussed the future of Earth and space science studies from the L1 point.
Photo.
Former U.S. Vice President Al Gore
spoke at the opening session of the 10
th
DSCOVR Science Team Meeting. This photo shows Gore together with
Makenzie Lystrup
[NASA's Goddard Space Flight Center (GSFC)-
Center Director
],
Christa Peters-Lidard
[GSFC,
Director of the Science and Exploration Directorate
],
Elsayed Talaat
[National Oceanic and Atmospheric Administration (NOAA)-
Director of the Office of Space Weather Observations
],
Dalia Kirschbaum
[GSFC-
Director of Earth Sciences
], other GSFC management, and members of the DSCOVR Science Team.
Photo credit:
Katy Comber (GSFC)
Updates on DSCOVR Operations
The DSCOVR mission components continue to function nominally. The meeting was an opportunity to update participants on progress over the past year on several fronts, including data acquisition, processing, and archiving, and release of new versions of several data products. The number of people using DSCOVR data continues to increase, with a new Science Outreach Team having been put in place to aid users in several aspects of data discovery, access, and user friendliness.
Amanda Raab
[NOAA, DSCOVR Mission Operations and Systems] reported on the current status of the DSCOVR mission. She also discussed spacecraft risks and issues such as memory fragmentation and data storage task anomalies but indicated that both these issues have been resolved.
Hazem Mahmoud
[NASA's Langley Research Center (LaRC)] discussed the work of the
Atmospheric Science Data Center
(ASDC), which is based at LaRC. He showed DSCOVR mission metrics since 2015, focusing on data downloads and the global outreach of the mission. He noted that there has been a significant rise in the number of downloads and an increasing diversity of countries accessing ozone (O
3
), aerosol, and cloud data products. Mahmoud also announced that the ASDC is transitioning to the
Amazon Web Services
cloud, which will further enhance global access and streamline DSCOVR data processing.
Karin Blank
[GSFC] covered the discovery of a new type of mirage that can only be seen in deep space from EPIC. The discussion included the use of a ray tracer in determining the origin of the phenomenon, and under what conditions it can be seen.
Alexander Cede
[SciGlob] and
Ragi Rajagopalan
[LiftBlick OG] gave an overview of the stability of the EPIC Level-1A (L1A) data over the first decade of operation. They explained that the only observable changes in the EPIC calibration are to the dark count and flat field can - and that these changes can be entirely attributed to the temperature change of the system in orbit compared to prelaunch conditions. No additional hot or warm pixels have emerged since launch and no significant sensitivity drifts have been observed. The results that Cede and Rajagopalan showed that EPIC continues to be a remarkably stable instrument, which is attributed to a large extent to its orbit around the L1 point, which is located outside the Earth's radiation belts and thus an extremely stable temperature environment. Consequently, in terms of stability, the L1 point is far superior to other Earth observation points, e.g., ground-based, low-Earth orbit (LEO), polar orbit, or geostationary Earth orbit (GEO).
Marshall Sutton
[GSFC] discussed the state of the DSCOVR Science Operation Center (DSOC). He also talked about processing EPIC Level-1 (L1) data into L2 science products, daily images available on the EPIC website, and special imaging opportunities, e.g., volcanic eruptions.
EPIC Calibration
After 10 years of operation in space, the EPIC instrument on DSCOVR continues to be a remarkably stable instrument. The three presentations describe different ways that are used to verify the EPIC measurements remain reliable.
Conor
Haney
[LaRC] reported on anomalous outliers during February and March 2023 from the broadband shortwave (SW) flux using EPIC L1B channel radiances. To ensure that these outliers were not a result of fluctuations in the EPIC L1B channel radiances, both the EPIC radiance measurements and coincident, ray-matched radiance measurements from the
Visible Infrared Imaging Radiometer Suite
(VIIRS), on the
Suomi National Polar-orbiting Partnership
(Suomi NPP) platform, were processed using the same deep convective cloud invariant target (DCC-IT) algorithm. This analysis confirmed that the anomalous behavior was due to the DCC-IT algorithm - and not because of fluctuations in the EPIC L1B channel radiances. The improved DCC-IT methodology was also applied to the EPIC L1B radiances. The results indicate that the EPIC record is quite stable with a lower uncertainty than when processed using the previous DCC-IT methodology.
Igor Geogdzhaev
[NASA's Goddard Institute for Space Studies (GISS)/Columbia University] reported that EPIC Visible-Near Infrared (VIS-NIR) calibration based on VIIRS (on Suomi NPP) data has showed excellent stability, while VIIRS (on NOAA-20 and -21) derived gains agree to within 1-2%. Preliminary analysis showed continuity in the gains derived from
Advanced Baseline Imager
(ABI) data. (ABI flies on NOAA's two operational
Geostationary Operational Environmental Satellite-Series R
satellites - GOES-17 and GOES-18.
Liang-Kang Huang
[Science Systems and Applications, Inc. (SSAI)] reported on updates to the EPIC ultraviolet (UV) channel sensitivity time dependences using Sun-normalized radiance comparisons between EPIC and measurements from the Ozone Mapping and Profiler Suite (OMPS) Nadir Mapper (NM) on Suomi NPP, with coinciding footprints and solar/satellite angles. Huang's team determined vignetting factors in the sensitivity calibration between 2021-2024, as a function of charge coupled device (CCD) pixel radius and pixel polar angles, using special lunar measurement sequences.
NISTAR Status and Science with Its Observations
The NISTAR instrument remains fully functional and continues its uninterrupted data record. The NISTAR-related presentations during this meeting included more details on specific topics related to NISTAR as well as on efforts to combine information from both EPIC and NISTAR.
Steven Lorentz
[L-1 Standards and Technology, Inc.] reported that the NISTAR on DSCOVR has been measuring the irradiance from the sunlit Earth in three bands for more than nine years. The three bands measure the outgoing total and reflected-solar radiation from Earth at a limited range of solar angles. To compare the long-term stability of EPIC and NISTAR responses, researchers developed a narrowband to wideband conversion model to allow the direct comparison of the EPIC multiband imagery and NISTAR SW - see
Figure 1
- and silicon photodiode channels. Lorentz presented daily results spanning several years. The comparison employed different detectors from the same spacecraft - but with the same vantage point - thereby avoiding any model dependent orbital artifacts.
Figure 1.
NISTAR daily average shortwave (SW) radiance plotted for each year from 2017-2024. The results indicated a 10% increase in the shortwave radiance as the backscattering angle approaches 178° in December 2020. A 6% increase is noted in September of the same year.
Figure credit
: Steven Lorentz (L-1 Standards and Technology)
Clark Weaver
[University of Maryland, College Park (UMD)] used spectral information from the
SCanning Imaging Absorption spectroMeter for Atmospheric CartograpHY
(SCIAMACHY), which flew on the European Space Agency's (ESA) Envisat satellite from 2002-2012, to fill EPIC spectral gaps. He reported on construction of a composite height resolution spectrum that was spectrally integrated to produce SW energy. Weaver explained that he compared the EPIC reflected SW with four-hour averages from Band 4 on NISTAR. He used spectral information from SCIAMACHY to fill in gaps. Weaver also discussed results of a comparison of area integrated EPIC SW energy with observations from NISTAR .
Andrew Lacis
[GISS] reported on results of analysis of seven years of EPIC-derived planetary albedo for Earth, which reveal global-scale longitudinal variability occurring over a wide range of frequencies - with strong correlation between nearby longitudes and strong anticorrelation between diametrically opposed longitudes. This behavior in the Earth's global-scale energy budget variability is fully corroborated by seven years of NISTAR silicon photodiode measurements, which view the Earth with 1º longitudinal resolution. This analysis establishes the DSCOVR mission EPIC/NISTAR measurements as a new and unmatched observational data source for evaluating global climate model performance- e.g., see
Figure 2
.
Figure 2.
This graph shows the diurnal variation in planetary albedo as measured by EPIC for five different eight-day-Blurred Meridians relative to Global Mean for 2021 [
left
] and 2022 [
right
].
Figure credit
: Andrew Lacis [GISS]
Wenying Su
[LaRC] discussed global daytime mean SW fluxes within the EPIC field of view produced from January 2016-June 2024. These quasi-hourly SW fluxes agree very well with the Synoptic data product from the
Clouds and the Earth's Radiant Energy System
(CERES) instruments (currently flying on the
Terra
and
Aqua
, Suomi NPP, and NOAA-20 platforms) with the root mean square errors (rmse) less than 3 W/m
2
. This SW flux processing framework will be used to calculate NISTAR SW flux when Version 4 (V4) of the NISTAR radiance becomes available. Su noted that SW fluxes from EPIC are not suitable to study interannual variability as the magnitude of EPIC flux is sensitive to the percentage of daytime area visible to EPIC.
Update on EPIC Products and Science Results
EPIC has a
suite of data products available
. The following subsections summarize content during the DSCOVR STM related to these products. The updates focus on several data products and the related algorithm improvements.
Total Column Ozone
Jerry Ziemke
[Morgan State University (MSU), Goddard Earth Sciences Technology and Research-II (GESTAR II)] and
Natalya Kramarova
[GSFC] reported that tropospheric O
3
from DSCOVR EPIC shows anomalous reductions of ~10% throughout the Northern Hemisphere (NH) starting in Spring 2020 that continues to the present. The EPIC data, along with other satellite-based (e.g.,
Ozone Monitoring Instrument
(OMI) on NASA's
Aura
platform) and ground-based (e.g.,
Pandora
) data, indicate that the observed NH reductions in O
3
are due to combined effects from meteorology and reduced pollution, including reduced shipping pollution in early 2020 (during COVID) - see
Figure 3
. EPIC 1-2 hourly data are also used to evaluate hourly total O
3
and derived tropospheric O
3
from NASA's
Tropospheric Emissions: Monitoring of Pollution
(TEMPO) geostationary instrument. Ziemke explained that comparison of TEMPO data with EPIC data has helped the researchers characterize a persistent latitude-dependent offset in TEMPO total O
3
data of ~10-15% from south to north over the North American continent.
Figure 3.
This dataset combines input from EPIC, OMPS, and OMI from 2004-2022. The onset of the COVID-19 pandemic in 2020 can be seen clearly in the data as it corresponds to a sudden drop in tropospheric column ozone by ~3 Dobson Units in the Northern Hemisphere.
Figure credit
: Jerry Ziemke (Morgan State University, GESTAR-II)
Algorithm Improvement for Ozone and Sulfur Dioxide Products
Kai Yang
[UMD] presented a comprehensive evaluation of total and tropospheric O
3
retrievals, highlighting the long-term stability and high accuracy of EPIC measurements. He also validated EPIC's volcanic sulfur dioxide (SO
2
) retrievals by comparing them with ground-based
Brewer
spectrophotometer measurements and summarized EPIC's observations of SO
2
from recent volcanic eruptions.
Simon Carn
[University of Michigan] showed the first comparisons between the EPIC L2 volcanic SO
2
product and SO
2
retrievals from the
Geostationary Environment Monitoring Spectrometer
(GEMS) on the
Korean GEO-Kompsat-2B
satellite. GEMS observes East Asia as part of the new geostationary UV air quality (GEO-AQ) satellite constellation (which also includes TEMPO that observes North America and will include the Ultraviolet-Visible-Near Infrared (UVN) instrument on the European Copernicus Sentinel-4 mission, that will be launched in 2025 to observe Europe and surrounding areas) - but is not optimized for measurements of high SO
2
columns during volcanic eruptions. EPIC SO
2
data for the 2024 eruption of Ruang volcano in Indonesia are being used to validate a new GEMS volcanic SO
2
product. Initial comparisons show good agreement between EPIC and GEMS before volcanic cloud dispersal and confirm the greater sensitivity of the hyperspectral GEMS instrument to low SO
2
column amounts.
Aerosols
Alexei Lyapustin
[GSFC] reported that the latest EPIC aerosols algorithm (V3) simultaneously retrieves aerosol optical depth, aerosol spectral absorption, and aerosol layer height (ALH) - achieving high accuracy. He showed that global validation of the single scattering albedo in the blue and red shows 66% and 81-95% agreement respectively, with Aerosol Robotic Network (AERONET) observations - which is within the expected error of 0.03 for smoke and dust aerosols. Lyapustin also reported on a comparison of EPIC aerosol data collected from 2015-2023 by the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP), which flew on the
Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations
(CALIPSO) mission. The results show that ALH is retrieved with rmse ~1.1 km (0.7 mi). ALH is unbiased over the ocean and is underestimated by 450 m (1470 ft) for the smoke and by 750 m (2460 ft) for the dust aerosols over land.
Myungje Choi
and
Sujung Go
[both from University of Maryland, Baltimore County's (UMBC), GESTAR II] presented results from a global smoke and dust characterization using
Multi-Angle Implementation of Atmospheric Correction
(MAIAC) algorithm. This study characterized smoke and dust aerosol properties derived from MAIAC EPIC processing, examining spectral absorption, ALH, and chemical composition (e.g., black and brown carbon). Regions with smoldering wildfires, e.g., North America and Siberia, exhibited high ALH and a significant fraction of brown carbon, while Central Africa showed lower ALH with higher black carbon emissions.
Omar Torres
[GSFC] discussed how L1 DSCOVR-EPIC observations are being used to study air quality (i.e., tropospheric O
3
and aerosols) globally. Torres noted that this application of EPIC-L1 observations is of particular interest in the Southern Hemisphere (SH) where, unlike over the NH, there are currently no space GEO-based air quality measurements - and no plans for them in the foreseeable future.
Hiren Jethva
[MSU, GESTAR II] presented the new results of the aerosol optical centroid height retrieved from the EPIC Oxygen-B band observations. He described the algorithm details, showed retrieval maps, and reviewed the comparative analysis against CALIOP backscatter-weighted measurements. The analysis showed a good level of agreement with more than 70% of matchup data within 1-1.5 km (0.6-0.9 mi) difference.
Jun Wang
[University of Iowa] presented his team's work on advancing the second generation of the aerosol optical centroid height (AOCH) algorithm for EPIC. Key advancements included: constraining surface reflectance in aerosol retrieval using an EPIC-based climatology of surface reflectance ratios between 442-680 nm; incorporating a dynamic aerosol model to characterize aged smoke particles; and employing a spectral slope technique to distinguish thick smoke plumes from clouds. Results show that both atmospheric optical depth (AOD) and AOCH retrievals are improved in the second generation of AOCH algorithm.
Olga Kalashnikova
[NASA/Jet Propulsion Laboratory (JPL)] reported on improving brown carbon evolution processes in the
Weather Research and Forecasting model coupled with Chemistry
(WRF-Chem) model with EPIC products. She indicated that DSCOVR product evaluation, using lidar aerosol height measurements from CALIOP, led to an improved operational brown carbon product. To better resolve the temporal evolution of brown carbon, chemical transport models need to include more information about near-source fires.
Mike Garay
[NASA/Jet Propulsion Laboratory (JPL)] discussed constraining near-source brown carbon emissions from 2024 Canadian 'zombie' fires with EPIC products. He reported that fires in British Columbia, Canada showed differences in brown carbon emission near the sources. Garay explained that their investigation has revealed that these differences were related to fire intensity and variations in vegetation/soil content.
Yuekui Yang
[GSFC] presented work that examined the impact of Earth's curvature consideration on EPIC cloud height retrievals. Biases under the Plane Parallel (PPL) assumption is studied by comparing results using the improved pseudo-spherical shell approximation. PPL retrievals in general bias high and for a cloud with height of 5 km (3 mi), the bias is about 6%.
Alfonso Delgado Bonal
[UMBC] stated that the EPIC vantage point offers a unique opportunity to observe not only the current state of the Earth but also its temporal evolution. By capturing multiple observations of the planet throughout the day, EPIC enables statistical reconstruction of diurnal patterns in clouds and other atmospheric parameters. Bonal's team focused their research on O
3
(primarily tropospheric) over the U.S. to demonstrate the presence of a diurnal cycle in the western regions of the continental U.S. However, ground-based data from PANDORA for specific locations do not support these diurnal variations - underscoring the critical role of space-based O
3
retrievals. The proposed methodology is not limited to clouds or O
3
but is broadly applicable to other EPIC measurements for the dynamic nature of our planet.
Elizabeth Berry
[Atmospheric and Environmental Research (AER)] presented results from a coincident DSCOVR-CloudSat dataset [covering 2015-2020]. Cloud properties (e.g., cloud height and optical depth) from DSCOVR and CloudSat are moderately correlated and show quite good agreement given differences in the instruments sensitivities and footprints. Berry explained that a machine-learning model trained on the coincident data demonstrates high accuracy at predicting the presence of vertical cloud layers. However, precision and recall metrics highlight the challenge of predicting the precise location of cloud boundaries.
Anthony Davis
[JPL] presented a pathway toward accurate estimation of the cloud optical thickness (COT) of opaque clouds and cloud systems, e.g., supercells, mesoscale convective complexes, and tropical cyclones (TCs). He described the approach, which uses differential oxygen absorption spectroscopy (DOAS) that has resolving power greater than 10
4
- which is comparable to that of the high-resolution spectrometers on NASA's
Orbiting Carbon Observatory-2
(OCO-2) - but is based upon the cloud information content of EPIC's O
2
A- and B-band radiances. Unlike the current operational retrieval of COT - which uses data from the Moderate Resolution Imaging Spectroradiometer (MODIS) on Terra and Aqua - the DOAS-based technique does not saturate at COT exceeding ~60. According to a popular TC model with two-moment microphysics, COT in a tropical storm or hurricane can reach well into the hundreds, sometimes exceeding 1000. Davis said that once the new COT estimates become available, they will provide new observational constraints on process and forecast models for TCs.
Ocean
Robert Frouin
[Scripps Institution of Oceanography, University of California] discussed ocean surface radiation products derived from EPIC data. He explained that significant advancements have been achieved in processing and evaluating ocean biology and biogeochemistry products derived from EPIC imagery. V1 updates enhanced accuracy by integrating
Modern-Era Retrospective analysis for Research and Applications V2
(MERRA-2) ancillary data and refining calculations for atmospheric and surface parameters. Frouin introduced several diurnal products, including hourly photosynthetically active radiation (PAR) fluxes, spectral water reflectance, and chlorophyll-a concentrations. He said that these new MODIS-derived products have been validated through comparisons with data from the
Advanced Himawari Imager
on the Japanese Himawar-8 and -9 satellites. In order to address the gaps in these diurnal products, Frouin explained that the team developed a convolutional neural network that has been used effectively to reconstruct missing PAR values with high accuracy.
Vegetation
Yuri Knyazikhin
[Boston University] reported on the status of the
Vegetation Earth System Data Record
(VESDR) that provides a variety of parameters including: Leaf Area Index (LAI), diurnal courses of Normalized Difference Vegetation Index (NDVI), Sunlit LAI (SLAI), Fraction of incident Photosynthetically Active Radiation (FPAR) absorbed by the vegetation, Directional Area Scattering Function (DASF), Earth Reflector Type Index (ERTI), and Canopy Scattering Coefficient (CSC). Knyazikhin discussed analysis of the diurnal and seasonal variations of these quantities. EPIC LAI and FPAR are consistent with MODIS-derived measurements of the same parameters.
Jan Pisek
[University of Tartu/Tartu Observatory,
Estonia
] discussed efforts to derive leaf inclination information from EPIC data. The very first evaluation over Tumbarumba site (in New South Wales, Australia) showed that the angular variation in parameters obtained from EPIC reflects the expected variations due to the erectophile vegetation present at the site.
Sun Glint
Tamás Várnai
[UMBC, JCET] discussed EPIC observations of Sun glint from ice clouds. The cloud glints come mostly from horizontally oriented ice crystals and have strong impact in EPIC cloud retrievals. Várnai reported that the
EPIC glint product
is available from the ASDC - see
Figure 4
. Glint data can help reduce the uncertainties related to horizontally oriented ice crystals and yield additional new insights about the microphysical and radiative properties of ice clouds.
Figure 4.
[
top row
]
EPIC glint mask
examples over land in [
left to right
] Paraguay, Sudan, Thailand, and Brazil. [
bottom row
] The corresponding EPIC
glint mask
for each image on the top row indicates the band (red, green and blue) and the size of sun glint for each of them.
Figure credit
: Tamás Várnai (University of Maryland, Baltimore County)
Alexander Kostinski
[Michigan Technology University] explained that because they detected climatic
signals
(i.e., longer-term changes and semi-permanent features, e.g., ocean glitter), they developed a technique to suppress geographic "noise" in EPIC images that involves introducing temporally (monthly) and conditionally (classifying by surface/cover type, e.g., land, ocean, clouds) averaged reflectance images - see
Figure 5
. The resulting images display seasonal dependence in a striking manner. Additionally, cloud-free, ocean-only images highlight prominent regions of ocean glitter.
Figure 5.
Monthly reflectances for clear land pixels. Earth masquerading as Jupiter; latitudinal bright bands are caused by features such as the Sahara and Antarctica. Black spots are due to the lack or dearth of clear land pixels at that latitude. Repeated spots within latitudinal bands reflect roughly bi-hourly image sampling.
Figure credit
: Alexander Kostinski (Michigan Technology University); from a 2024 paper published in
Frontiers of Remote Sensing
Jiani Yang
[Caltech] reported that spatially resolving light curves from DSCOVR is crucial for evaluating time-varying surface features and the presence of an atmosphere. Both of these features are essential for sustaining life on Earth - and thus can be used to assess the potential habitability of exoplanets. Using epsilon machine reconstruction, the statistical complexity from the time series data of these light curves can be calculated. The results show that statistical complexity serves as a reliable metric for quantifying the intricacy of planetary features. Higher levels of planetary complexity qualitatively correspond to increased statistical complexity and Shannon entropy, illustrating the effectiveness of this approach in identifying planets with the most dynamic characteristics.
Other EPIC Science Results
Guoyong Wen
[MSU, GESTAR II] analyzed the variability of global spectral reflectance from EPIC and the integrated broadband reflectance on different timescales. He reported that on a diurnal timescale, the global reflectance variations in UV and blue bands are statistically similar - and drastically different from those observed in longer wavelength bands (i.e., green to NIR). The researchers also did an analysis of monthly average results and found that temporal averaging of the global reflectance reduces the variability across the wavelength and that the variability of broadband reflectance is similar to that for the red band on both timescales. These results are mainly due to the rotation of the Earth on diurnal timescale and the change of the Earth's tilt angle.
Nick Gorkavyi
[Science Systems and Applications, Inc. (SSAI)] reported that EPIC - located at the L1 point, 1.5 million km (0.9 million mi) away from Earth - can capture images of the far side of the Moon in multiple wavelengths. These images, taken under full solar illumination, can be used to calibrate photographs obtained by lunar artificial satellites. Additionally, he discussed the impact of
lunar libration
- the changing view of the Moon from Earth, or it's apparent "wobble" - on Earth observations from the Moon.
Jay Herman
[UMBC] discussed a comparison of EPIC O
3
with TEMPO satellite and Pandora ground-based measurement. The results show that total column O
3
does not have a significant photochemical diurnal variation. Instead, the daily observed diurnal variation is caused by weather changes in atmospheric pressure. This measurement result agrees with model calculations.
Conclusion
Alexander Marshak
,
Jay Herman
, and
Adam Szabo
led a closing discussion with ST participants on how to make the EPIC and NISTAR instruments more visible in the community. It was noted that the EPIC website now allows visitors to observe daily fluctuations of aerosol index, cloud fraction, cloud height, and the ocean surface - as observed from the L1 point. More daily products, (e.g., aerosol height and sunlit leaf area index) will be added soon, which should attract more users to the website.
Overall, the 2023 DSCOVR EPIC and NISTAR STM was successful. It provided an opportunity for participants to learn the status of DSCOVR's Earth-observing instruments, EPIC and NISTAR, the status of recently released L2 data products, and the science results being achieved from the L1 point. As more people use DSCOVR data worldwide, the ST hopes to hear from users and team members at its next meeting. The latest updates from the mission can be found on the
EPIC website
.
Alexander Marshak
NASA's Goddard Space Flight Center
alexander.marshak@nasa.gov
Adam Szabo
NASA's Goddard Space Flight Center
adam.szabo@nasa.gov
Firefly's Blue Ghost lunar lander captured a bright image of the Moon's South Pole (on the far left) through the cameras on its top deck, while it travels to the Moon as part of NASA's CLPS (Commercial Lunar Payload Services) initiative and Artemis campaign.
Credits: Firefly Aerospace
With a suite of NASA science and technology on board, Firefly Aerospace is targeting no earlier than 3:45 a.m. EST on Sunday, March 2, to land the Blue Ghost lunar lander on the Moon. Blue Ghost is slated to touch down near Mare Crisium, a plain in the northeast quadrant on the near side of the Moon, as part of NASA's CLPS (Commercial Lunar Payload Services) initiative and Artemis campaign to establish a long-term lunar presence.
Live coverage of the landing, jointly hosted by NASA and Firefly, will air on
NASA+
starting at 2:30 a.m. EST, approximately 75 minutes before touchdown on the Moon's surface. Learn how to
watch NASA conten
t through a variety of platforms, including social media. The broadcast will also stream on
Firefly's YouTube
channel. Coverage will include live streaming and
blog updates
as the descent milestones occur.
Accredited media interested in attending the in-person landing event hosted by Firefly in the Austin, Texas, area may request media credentials through
this form
by Monday, Feb. 24.
Following the landing, NASA and Firefly will host a news conference to discuss the mission and science opportunities that lie ahead as they begin lunar surface operations. The time of the briefing will be shared after touchdown.
Blue Ghost
launched
Jan. 15, at 1:11 a.m. EST on a SpaceX Falcon 9 rocket from Launch Complex 39A at NASA's Kennedy Space Center in Florida. The lander is carrying a suite of 10 NASA scientific investigations and technology demonstrations, which will provide insights into the Moon's environment and test technologies to support future astronauts landing safely on the lunar surface, as well as Mars.
NASA continues to work with multiple American companies to deliver science and technology to the lunar surface through the agency's CLPS initiative. This pool of companies may bid on contracts for end-to-end lunar delivery services, including payload integration and operations, launching from Earth, and landing on the surface of the Moon. NASA's CLPS contracts are indefinite-delivery/indefinite-quantity contracts with a cumulative maximum value of $2.6 billion through 2028. In February 2021, the agency awarded Firefly this delivery of 10 NASA science investigations and technology demonstrations to the Moon using its American-designed and -manufactured lunar lander for approximately $93.3 million (modified to $101.5 million).
Through the Artemis campaign, commercial robotic deliveries will perform science experiments, test technologies, and demonstrate capabilities on and around the Moon to help NASA explore in advance of Artemis Generation astronaut missions to the lunar surface, and ultimately crewed missions to Mars.
Watch, engage on social media
Let people know you’re following the mission on X, Facebook, and Instagram by using the hashtag #Artemis. You can also stay connected by following and tagging these accounts:
X:
@
NASA
, @
NASA_Johnson
, @
NASAArtemis
, @
NASAMoon
Facebook:
NASA
,
NASAJohnsonSpaceCenter
,
NASAArtemis
Instagram:
@
NASA
, @
NASAJohnson
, @
NASAArtemis
For more information about the agency's Commercial Lunar Payload Services initiative:
An Afternoon of Family Science and Rocket Exploration in Alaska
On Tuesday, January 28th,
Fairbanks BEST Homeschool
joined the Geophysical Institute for an afternoon of rocket exploration, hands-on activities, and stargazing inside a planetarium. This event was free and open to the public. Despite their frigid winter weather, 200 attendees were curious about the scientific endeavors of Alaska-based researchers alongside cutting-edge investigations conducted by NASA rocket scientists.
Families and friends in attendance learned about two NASA rocket missions that would study the flickering and vanishing auroras:
Ground Imaging to Rocket investigation of Auroral Fast Features (GIRAFF) and Black and Diffuse Aurora Science Surveyor (BaDASS)
. Visitors had an opportunity to sign up for text notifications related to the launch window. The planetarium presentations touch on Heliophysics Big Ideas that align with the three questions that drive NASA's heliophysics research:
What are the impacts of the changing sun on humanity?
How do Earth, the solar system, and the heliosphere respond to changes on the sun?
What causes the sun to vary?
The event also offered
sun-related hands-on activities provided by the University of Alaska Museum of the North
.
This event was offered to the community in association with the Science For Alaska Lecture Series and the 2025 NASA Sounding Rocket campaign. Every attendee left with something inspiring to think about. Parents and educators interested in learning more about auroras and do participatory science may check out NASA's
Aurorasaurus
citizen science project
.
The Geophysical Institute at the University of Alaska Fairbanks is a Co-Investigating team for the NASA Heliophysics Education Activation Team (NASA HEAT), which is part of NASA's Science Activation Portfolio. Learn more about how Science Activation connects NASA science experts, content, and experiences with community leaders to do science in ways that activate minds and promote deeper understanding of our world and beyond:
https://science.nasa.gov/learn
Aurora Educational Resource List by Aurorasaurus
Families constructed and decorated their paper rockets.
Katelin Avery
It was so much fun! We are receiving rave reviews from our families and the surrounding community. THANK YOU AGAIN FOR COLLABORATING WITH US!
X-ray: NASA/CXC/Penn State Univ./L. Townsley et al.; Infrared: NASA/JPL-CalTech/SST; Optical: NASA/STScI/HST; Radio: ESO/NAOJ/NRAO/ALMA; Image Processing: NASA/CXC/SAO/J. Schmidt, N. Wolk, K. Arcand
This image, released on Feb. 12, 2025, is the deepest X-ray image ever made of the spectacular star forming region called 30 Doradus. By combining X-ray data from
NASA's Chandra X-ray Observatory
(blue and green) with optical data from
NASA's Hubble Space Telescope
(yellow) and radio data from the
Atacama Large Millimeter/submillimeter Array
(orange), this stellar arrangement comes alive.
Otherwise known as the Tarantula Nebula, 30 Dor is located about 160,000 light-years away in a small neighboring galaxy to the Milky Way known as the Large Magellanic Cloud. Because it one of the brightest and populated star-forming regions to Earth, 30 Dor is a frequent target for scientists trying to learn more about how stars are born.
Learn more about this new image and what it reveals.
Image credit: X-ray: NASA/CXC/Penn State Univ./L. Townsley et al.; Infrared: NASA/JPL-CalTech/SST; Optical: NASA/STScI/HST; Radio: ESO/NAOJ/NRAO/ALMA; Image Processing: NASA/CXC/SAO/J. Schmidt, N. Wolk, K. Arcand
This NASA/ESA Hubble Space Telescope reveals clouds of gas and dust near the Tarantula Nebula, located in the Large Magellanic Cloud about 160,000 light-years away.
The universe is a dusty place, as this NASA/ESA
Hubble Space Telescope
image featuring swirling clouds of gas and dust near the Tarantula Nebula reveals. Located in the Large Magellanic Cloud about 160,000 light-years away in the constellations Dorado and Mensa, the Tarantula Nebula is the most productive star-forming region in the nearby universe, home to the most massive stars known.
The nebula's colorful gas clouds hold wispy tendrils and dark clumps of dust. This dust is different from ordinary household dust, which may include of bits of soil, skin cells, hair, and even plastic. Cosmic dust is often comprised of carbon or of molecules called silicates, which contain silicon and oxygen. The data in this image was part of an observing program that aims to characterize the properties of cosmic dust in the Large Magellanic Cloud and other nearby galaxies.
Dust plays several important roles in the universe. Even though individual dust grains are incredibly tiny, far smaller than the width of a single human hair, dust grains in disks around young stars clump together to form larger grains and eventually planets. Dust also helps cool clouds of gas so that they can condense into new stars. Dust even plays a role in making new molecules in interstellar space, providing a venue for individual atoms to find each other and bond together in the vastness of space.
NASA's Mars rover Curiosity acquired this image of the science targets before it, including "Catalina Island," the flat rock at image center, using its Left Navigation Camera. The rover captured the image on sol 4450 - or Martian day 4,450 of the Mars Science Laboratory mission - on Feb. 11, 2025, at 13:11:14 UTC.
NASA/JPL-Caltech
Earth planning date: Wednesday, Feb. 12, 2025
I woke up this morning to my weather app telling me it felt like minus 15° C (5°F) outside. On days like this, it can take me a little longer to get myself up and out into the world. Curiosity has a similar problem - as we head toward winter and it gets colder and colder in Gale Crater, Curiosity has to spend more time warming up to do things like driving and all our good science. I've also been watching a couple winter storms that are expected in the next few days here in Toronto. Luckily, Curiosity doesn't have to deal with snowstorms, and our drive in the last plan went ahead as planned and put us in a good position to go ahead with contact science today, a relief after having to
forego it on Monday
.
The contact science location that the geology team chose is called "Catalina Island," the flat rock you can see in almost the center of the image above. As you can likely also see above, there's a whole jumble of rocks in that image, and Mastcam and ChemCam have picked out a couple others to take a look at. These are "Point Dume," which will be the target of ChemCam's laser spectrometer, and "Whittier Narrows," on which Mastcam will image some linear features. Mastcam and ChemCam are also turning their gazes further afield for Mastcam targets "Cleghorn Ridge," "Cuyamaca Peak," "Kratka Ridge," and two long-distance ChemCam mosaics of the top of the Wilkerson butte and a spot a little further down known as "Pothole Trail."
Much like I'm keeping an eye out the window on the changing weather here, Curiosity is also continuing to keep an eye on the environment in Gale Crater. Even though it's not the dusty season, we continue to monitor the dust around us and in the atmosphere with a dust-devil survey and a tau. But we're especially interested in
what the clouds are up to right now
, which we're checking in on with our normal zenith and suprahorizon movies, and our cloud-season-only Phase Function Sky Survey. This is a series of movies covering the whole sky that we can use to determine how sunlight interacts with the individual water-ice crystals in the clouds.
Written by Alex Innanen, Atmospheric Scientist at York University
NASA Tests Drones to Provide Micrometeorology, Aid in Fire Response
Pilot in command Brayden Chamberlain performs pre-flight checks on the NASA Alta X quadcopter during the FireSense uncrewed aerial system (UAS) technology demonstration in Missoula.
Credits:
NASA ARC/Milan Loiacono
In Aug. 2024, a team of NASA researchers and partners gathered in Missoula, Montana to test new drone-based technology for localized forecasting, or micrometeorology. Researchers attached wind sensors to a drone, NASA's Alta X quadcopter, aiming to provide precise and sustainable meteorological data to help predict fire behavior.
Wildfires are
increasing in number and severity
around the world, including the United States, and wind is a major factor. It leads to unexpected and unpredictable fire growth, public threats, and fire fatalities, making micrometeorology a very effective tool to combat fire.
This composite image shows the NASA Alta X quadcopter taking off during one of eight flights it performed for the 2024 FireSense UAS technology demonstration in Missoula. Mounted on top of the drone is a unique infrastructure designed at NASA's Langley Research Center in Hampton,Virginia, to carry sensors that measure wind speed and direction into the sky. On the ground, UAS pilot in command Brayden Chamberlain performs final pre-flight checks.
NASA/Milan Loiacono
The campaign was run by NASA's
FireSense
project, focused on addressing challenges in wildland fire management by putting NASA science and technology in the hands of operational agencies.
"Ensuring that the new technology will be easily adoptable by operational agencies such as the U.S. Forest Service and the National Weather Service was another primary goal of the campaign," said Jacquelyn Shuman, FireSense project scientist at NASA's Ames Research Center in California's Silicon Valley.
The FireSense team chose the Alta X drone because the U.S. Forest Service already has a fleet of the quadcopters and trained drone pilots, which could make integrating the needed sensors - and the accompanying infrastructure - much easier and more cost-effective for the agency.
The UAS pilot in command, Brayden Chamberlain, flashes a "good to go" signal to the command tent, indicating that the NASA Alta X quadcopter is prepped for takeoff. Behind Chamberlain, the custom structure attached to the quadcopter holds a radiosonde (small white box) and an anemometer (hidden from view), which will collect data on wind speed and direction, humidity, temperature, and pressure.
NASA/Milan Loiacono
The choice of the two sensors for the drone's payload was also driven by their adoptability.
The first, called a radiosonde, measures wind direction and speed, humidity, temperature, and pressure, and is used daily by the National Weather Service. The other sensor, an anemometer, measures wind speed and direction, and is used at weather stations and airports around the world.
The two sensors mounted on the NASA Alta X quadcopter are a radiosonde (left) and an anemometer (right), which measure wind speed and direction. The FireSense teams hopes that by giving them wings, researchers can enable micrometeorology to better predict fire and smoke behavior.
NASA/Milan Loiacono
"Anemometers are everywhere, but are usually stationary," said Robert McSwain, the FireSense uncrewed aerial system (UAS) lead, based at NASA's Langley Research Center in Hampton, Virginia. "We are taking a sensor type that is already used all over the world, and giving it wings."
Anemometers are everywhere, but are usually stationary. We are taking a sensor type that is already used all over the world, and giving it wings.
Robert Mcswain
FireSense Uncrewed Aerial System (UAS) Lead
Both sensors create datasets that are already familiar to meteorologists worldwide, which opens up the potential applications of the platform.
Current Forecasting Methods: Weather Balloons
Traditionally, global weather forecasting data is gathered by attaching a radiosonde to a weather balloon and releasing it into the air. This system works well for regional weather forecasts. But the rapidly changing environment of wildland fire requires more recurrent, pinpointed forecasts to accurately predict fire behavior. It's the perfect niche for a drone.
Left: Steven Stratham (right) attaches a radiosonde to the string of a weather balloon as teammates Travis Christopher (left) and Danny Johnson (center) prepare the balloon for launch. This team of three from Salish Kootenai College is one of many college teams across the nation trained to prepare and launch weather balloons.
Right: One of these weather balloons lifts into the sky, with the radiosonde visible at the end of the string.
NASA/Milan Loiacono
"These drones are not meant to replace the weather balloons," said Jennifer Fowler, FireSense's project manager at Langley. "The goal is to create a drop-in solution to get more frequent, localized data for wildfires – not to replace all weather forecasting."
The goal is to create a drop-in solution to get more frequent, localized data for wildfires – not to replace all weather forecasting.
Jennifer Fowler
FireSense Project Manager
Drones Provide Control, Repeat Testing, Sustainability
Drones can be piloted to keep making measurements over a precise location - an on-site forecaster could fly one every couple of hours as conditions change - and gather timely data to help determine how weather will impact the direction and speed of a fire.
Fire crews on the ground may need this information to make quick decisions about where to deploy firefighters and resources, draw fire lines, and protect nearby communities.
A reusable platform, like a drone, also reduces the financial and environmental impact of forecasting flights.
"A weather balloon is going to be a one-off, and the attached sensor won't be recovered," Fowler said. “The instrumented drone, on the other hand, can be flown repeatedly."
The NASA Alta X quadcopter sits in a field in Missoula, outfitted with a special structure to carry a radiosonde (sensor on the left) and an anemometer (sensor on the right) into the air. This structure was engineered at NASA's Langley Research Center to ensure the sensors are far enough from the rotors to avoid interfering with the data collected, but without compromising the stability of the drone.
NASA/Milan Loiacono
The Missoula Campaign
Before such technology can be sent out to a fire, it needs to be tested. That's what the FireSense team did this summer.
Smoke from the nearby Miller Peak Fire drifts by the air control tower at Missoula Airport on August 29, 2024. Miller Peak was one of several fires burning in and around Missoula that month, creating a smokey environment which, combined with the mountainous terrain, made the area an ideal location to test FireSense's new micrometeorology technology.
NASA/Milan Loiacono
McSwain described the conditions in Missoula as an "alignment of stars" for the research: the complex mountain terrain produces erratic, historically unpredictable winds, and the sparsity of monitoring instruments on the ground makes weather forecasting very difficult. During the three-day campaign, several fires burned nearby, which allowed researchers to test how the drones performed in smokey conditions.
A drone team out of NASA Langley conducted eight data-collection flights in Missoula. Before each drone flight, student teams from the University of Idaho in Moscow, Idaho, and Salish Kootenai College in Pablo, Montana, launched a weather balloon carrying the same type of radiometer.
Left: Weather balloon teams from University of Idaho and Salish Kootenai College prepare a weather balloon for launch on the second day of the FireSense campaign in Missoula.
Right: NASA Langley drone crew members Todd Ferrante (left) and Brayden Chamberlain (right) calibrate the internal sensors of the NASA Alta X quadcopter before its first test flight on Aug. 27, 2024.
Once those data sets were created, they needed to be transformed into a usable format. Meteorologists are used to the numbers, but incident commanders on an active fire need to see the data in a form that allows them to quickly understand which conditions are changing, and how. That's where data visualization partners come in. For the Missoula campaign, teams from MITRE, NVIDIA, and Esri joined NASA in the field.
An early data visualization from the Esri team shows the flight paths of weather balloons launched on the first day of the FireSense UAS technology demonstration in Missoula. The paths are color-coded by wind speed, from purple (low wind) to bright yellow (high wind).
NASA/Milan Loiacono
Measurements from both the balloon and the drone platforms were immediately sent to the on-site data teams. The MITRE team, together with NVIDIA, tested high-resolution artificial intelligence meteorological models, while the Esri team created comprehensive visualizations of flight paths, temperatures, and wind speed and direction. These visual representations of the data make conclusions more immediately apparent to non-meteorologists.
What's Next?
Development of drone capabilities for fire monitoring didn't begin in Missoula, and it won't end there.
"This campaign leveraged almost a decade of research, development, engineering, and testing," said McSwain. "We have built up a UAS flight capability that can now be used across NASA."
This campaign leveraged almost a decade of research, development, engineering, and testing. We have built up a UAS flight capability that can now be used across NASA.
Robert Mcswain
FireSense Uncrewed Aerial System (UAS) Lead
The NASA Alta X and its sensor payload will head to Alabama and Florida in spring 2025, incorporating improvements identified in Montana. There, the team will perform another technology demonstration with wildland fire managers from a different region.
To view more photos from the FireSense campaign visit:
https://nasa.gov/firesense
The FireSense project is led by NASA Headquarters in Washington and sits within the Wildland Fires program, with the project office based at NASA Ames. The goal of FireSense is to transition Earth science and technological capabilities to operational wildland fire management agencies, to address challenges in U.S. wildland fire management before, during, and after a fire.
About the Author
Milan Loiacono
Science Communication Specialist
Milan Loiacono is a science communication specialist for the Earth Science Division at NASA Ames Research Center.
The next full moon will be Wednesday morning, Feb. 12, 2025, appearing opposite the Sun (in Earth longitude) at 8:53 a.m. EST. The Moon will appear full for about three days around this time, from Monday night into early Thursday evening. The bright star Regulus will appear near the full moon.
Sky chart showing Jupiter and Mars high overhead after nightfall in February.
NASA/JPL-Caltech
The Maine Farmers' Almanac began publishing Native American names for full moons in the 1930s, and these names are now widely known and used. According to this almanac, as the full moon in February, the tribes of the northeastern U.S. called this the Snow Moon or the Storm Moon because of the heavy snows in this season. Bad weather and heavy snowstorms made hunting difficult, so this Moon was also called the Hunger Moon. NOAA monthly averages for the Washington, D.C. area airports from 1991 to 2020 show January and February nearly tied as the snowiest months of the year (with February one tenth of an inch ahead).
Here are the other celestial events between now and the full moon after next with times and angles based on the location of NASA Headquarters in Washington:
As winter continues in the Northern Hemisphere, the daily periods of sunlight continue to lengthen. Wednesday, Feb. 12 (the day of the full moon), morning twilight will begin at 6:04 a.m. EST, sunrise will be at 7:03 a.m., solar noon will be at 12:23 p.m. when the Sun will reach its maximum altitude of 37.7 degrees, sunset will be at 5:43 p.m., and evening twilight will end at 6:41 p.m.
Daylight Saving Time starts on the second Sunday in March for much of the United States. The day before, Saturday, March 8, morning twilight will begin at 5:32 a.m., sunrise will be at 6:30 a.m., solar noon will be at 12:19 p.m. when the Sun will reach its maximum altitude of 46.5 degrees, sunset will be at 6:08 p.m., and evening twilight will end at 7:06 p.m. Early on Sunday morning, March 9, the clock will "spring forward" from 1:59:59 a.m. EST to 3:00:00 a.m. EDT. Sunday, March 9, morning twilight will begin at 6:30 a.m., sunrise will be at 7:28 a.m., solar noon will be at 1:19 p.m. when the Sun will reach its maximum altitude of 46.9 degrees, sunset will be at 7:09 p.m., and evening twilight will end at 8:07 p.m. By Friday, March 14 (the day of the full moon after next), morning twilight will begin at 6:23 a.m., sunrise will be at 7:20 a.m., solar noon will be at 1:17 p.m. when the Sun will reach its maximum altitude of 48.9 degrees, sunset will be at 7:14 p.m., and evening twilight will end at 8:12 p.m.
This should still be a good time for planet watching, especially with a backyard telescope. On the evening of the March 14, the full moon, Venus, Jupiter, Mars, Saturn, and Uranus will all be in the evening sky. The brightest of the planets, Venus, will be 28 degrees above the west-southwestern horizon, appearing as a 29% illuminated crescent through a telescope. Second in brightness will be Jupiter at 71 degrees above the south-southeastern horizon. With a telescope you should be able to see Jupiter's four bright moons, Ganymede, Callisto, Europa, and Io, noticeably shifting positions in the course of an evening. Jupiter was at its closest and brightest in early December. Third in brightness will be Mars at 48 degrees above the eastern horizon. Mars was at its closest and brightest for the year just a month ago. Fourth in brightness (and appearing below Venus) will be Saturn at 11 degrees above the west-southwestern horizon. With a telescope you may be able to see Saturn's rings and its bright moon Titan. The rings will appear very thin and will be edge-on to Earth in March 2025. Saturn was at its closest and brightest in early September. The planet Uranus will be too dim to see without a telescope when the Moon is in the sky, but later in the lunar cycle, if you are in a very dark area with clear skies and no interference from moonlight, it will still be brighter than the faintest visible stars. Uranus was at its closest and brightest in mid-November.
During this lunar cycle, these planets, along with the background of stars, will rotate westward by about a degree each night around the pole star Polaris. Venus, named after the Roman goddess of love, will reach its brightest around Feb. 14, making this a special Valentine's Day. After about Feb. 17, the planet Mercury, shining brighter than Mars, will begin emerging from the glow of dusk about 30 minutes after sunset. Feb. 24 will be the first evening Mercury will be above the western horizon as twilight ends, while Feb. 25 will be the last evening Saturn will be above the western horizon as twilight ends, making these the only two evenings that all of the visible planets will be in the sky after twilight ends. For a few more evenings after this, Saturn should still be visible in the glow of dusk during twilight. Around March 8 or 9, Mercury will have dimmed to the same brightness as Mars, making Mars the third brightest visible planet again. By the evening of March 13 (the evening of the night of the full moon after next), as twilight ends, Venus and Mercury will appear low on the western horizon, making them difficult targets for a backyard telescope, while Jupiter and Mars (and Uranus) will appear high overhead and much easier to view.
Comets and Meteor Showers
No meteor shower peaks are predicted during this lunar cycle. No comets are expected to be visible without a telescope for Northern Hemisphere viewers. Southern Hemisphere viewers may still be able to use a telescope to see comet C/2024 G3 (ATLAS), although it is fading as it moves away from Earth and the Sun, and some recent reports suggest that it might be breaking apart and disappearing from view.
Evening Sky Highlights
On the evening of Wednesday, Feb. 12 (the evening of the full moon), as twilight ends at 6:41 p.m. EST, the rising Moon will be 7 degrees above the east-northeastern horizon with the bright star Regulus 2 degrees to the right. The brightest planet in the sky will be Venus at 28 degrees above the west-southwestern horizon, appearing as a crescent through a telescope. Next in brightness will be Jupiter at 71 degrees above the south-southeastern horizon. Third in brightness will be Mars at 48 degrees above the eastern horizon. The fourth brightest planet will be Saturn at 11 degrees above the west-southwestern horizon. Uranus, on the edge of what is visible under extremely clear, dark skies, will be 68 degrees above the south-southwestern horizon. The bright star closest to overhead will be Capella at 75 degrees above the northeastern horizon. Capella is the 6th brightest star in our night sky and the brightest star in the constellation Auriga (the charioteer). Although we see Capella as a single star, it is actually four stars (two pairs of stars orbiting each other). Capella is about 43 light years from us.
Also high in the sky will be the constellation Orion, easily identifiable because of the three stars that form Orion's Belt. This time of year, we see many bright stars in the sky at evening twilight, with bright stars scattered from the south-southeast toward the northwest. We see more stars in this direction because we are looking toward the Local Arm of our home galaxy (also called the Orion Arm, Orion-Cygnus Arm, or Orion Bridge). This arm is about 3,500 light years across and 10,000 light years long. Some of the bright stars from this arm that we see are the three stars of Orion's Belt, and Rigel (860 light years from Earth), Betelgeuse (548 light years), Polaris (about 400 light years), and Deneb (about 2,600 light years).
Facing toward the south from the Northern Hemisphere, to the upper left of Orion's Belt is the bright star Betelgeuse (be careful not to say this name three times). About the same distance to the lower right is the bright star Rigel. Orion's belt appears to point down and to the left about seven belt lengths to the bright star Sirius, the brightest star in the night sky. Below Sirius is the bright star Adhara. To the upper right of Orion's Belt (at about the same distance from Orion as Sirius) is the bright star Aldebaran. Nearly overhead is the bright star Capella. To the left (east) of Betelgeuse is the bright star Procyon. The two stars above Procyon are Castor and Pollux, the twin stars of the constellation Gemini (Pollux is the brighter of the two). The bright star Regulus appears farther to the left (east) of Pollux near the eastern horizon. For now, Mars is near Castor and Pollux, while Jupiter is near Aldebaran, but these are planets (from the Greek word for wanderers) and continue to shift relative to the background of the stars. Very few places on the East Coast are dark enough to see the Milky Way (our home galaxy), but if you could see it, it would appear to stretch overhead from the southeast to the northwest. Since we are seeing our galaxy from the inside, the combined light from its 100 to 400 billion stars make it appear as a band surrounding Earth.
As this lunar cycle progresses, the planets and the background of stars will rotate westward by about a degree each evening around the pole star Polaris. The brightest of the planets, Venus, will reach its brightest around Valentine's Day, Feb. 14. Bright Mercury will begin emerging from the glow of dusk around Feb. 17 and will be above the horizon as twilight ends beginning Feb. 24, initiating a brief period when all the visible planets will be in the evening sky at the same time that will end after Feb. 25, the last evening Saturn will be above the horizon as twilight ends. Feb. 24 and 25 will also be the two evenings when Mercury and Saturn will appear closest together.
The waxing crescent "Wet" or "Cheshire" Moon will appear near Mercury on Feb. 28 and Venus on March 1, appearing like a bowl or a smile above the horizon. The waxing gibbous Moon will appear near Mars and Pollux on March 8. Mercury will reach its highest above the horizon as twilight ends on March 8 but will be fading, appearing fainter than Mars. The nearly full moon will appear near Regulus on March 11. Venus and Mercury will be closest to each other on March 12.
By the evening of Thursday, March 13 (the evening of the night of the full moon after next), as twilight ends at 8:11 p.m. EDT, the rising Moon will be 14 degrees above the eastern horizon. The brightest planet in the sky will be Venus at 4 degrees above the west-southwestern horizon, appearing as a thin, 4% illuminated crescent through a telescope. Next in brightness will be Jupiter at 62 degrees above the west-southwestern horizon. Third in brightness will be Mars at 72 degrees above the southeastern horizon. Mercury, to the left of Venus, will also be 4 degrees above the western horizon. Uranus, on the edge of what is visible under extremely clear, moonless dark skies, will be 45 degrees above the western horizon. The bright star closest to overhead will still be Capella at 75 degrees above the northwestern horizon.
Morning Sky Highlights
On the morning of Wednesday, Feb. 12, 2025 (the morning of the night of the full moon), as twilight begins at 6:04 a.m. EST, the setting full moon will be 13 degrees above the western horizon. No planets will appear in the sky. The bright star appearing closest to overhead will be Arcturus at 65 degrees above the southeastern horizon. Arcturus is the brightest star in the constellation Boötes (the herdsman or plowman) and the 4th brightest star in our night sky. It is 36.7 light years from us. While it has about the same mass as our Sun, it is about 2.6 billion years older and has used up its core hydrogen, becoming a red giant 25 times the size and 170 times the brightness of our Sun. One way to identify Arcturus in the night sky is to start at the Big Dipper, then follow the arc of the dipper's handle as it "arcs toward Arcturus."
As this lunar cycle progresses the background of stars will rotate westward by about a degree each morning around the pole star Polaris. The waning Moon will appear near Regulus on Feb. 13, Spica on Feb. 17, and Antares on Feb. 21. The nearly full moon will appear near Regulus on March 12.
By the morning of Friday, March 14 (the morning of the full moon after next), as twilight begins at 6:23 a.m. EDT, the setting full moon will be 12 degrees above the western horizon. No visible planets will appear in the sky. The bright star closest to overhead will be Vega at 68 degrees above the eastern horizon. Vega is the 5th brightest star in our night sky and the brightest star in the constellation Lyra (the lyre). Vega is one of the three bright stars of the "Summer Triangle" (along with Deneb and Altair). It is about 25 light-years from Earth, has twice the mass of our Sun, and shines 40 times brighter than our Sun.
Detailed Daily Guide
Here is a day-by-day listing of celestial events between now and the full moon on March 14, 2025. The times and angles are based on the location of NASA Headquarters in Washington, and some of these details may differ for where you are (I use parentheses to indicate times specific to the D.C. area). If your latitude is significantly different than 39 degrees north (and especially for my Southern Hemisphere readers), I recommend using an astronomy app that is set up for your location or a star-watching guide from a local observatory, news outlet, or astronomy club.
Sunday morning, Feb. 9
Mars will appear to the upper left of the waxing gibbous Moon. In the early morning at about 2 a.m. EST, Mars will be 8 degrees from the Moon. By the time the Moon sets on the northwestern horizon at 5:58 a.m., Mars will have shifted to 6 degrees from the Moon. For parts of Asia and Northern Europe the Moon will pass in front of Mars. Also, Sunday morning, the planet Mercury will be passing on the far side of the Sun as seen from Earth, called superior conjunction. Because Mercury orbits inside of the orbit of Earth it will be shifting from the morning sky to the evening sky and will begin emerging from the glow of dusk on the west-southwestern horizon after about Feb. 17 (depending upon viewing conditions).
Sunday evening into Monday morning, Feb. 9 - 10
The waxing gibbous Moon will have shifted to the other side of the Mars (having passed in front of Mars in the afternoon when we could not see them). As evening twilight ends (at 6:38 p.m. EST) the Moon will be between Mars and the bright star Pollux, with Mars 3 degrees to the upper right and Pollux 3 degrees to the lower left. By the time the Moon reaches its highest for the night at 10:27 p.m., Mars will be 4.5 degrees to the right of the Moon and Pollux 2.5 degrees to the upper left of the Moon. Mars will set first on the northwestern horizon Monday morning at 5:44 a.m., just 22 minutes before morning twilight begins at 6:06 a.m.
Wednesday morning, Feb. 12
As mentioned above, the full moon will be Wednesday morning, Feb. 12, at 8:53 a.m. EST. This will be on Thursday morning from Australian Central Time eastward to the international date line in the mid-Pacific. The Moon will appear full for about three days around this time, from Monday night into early Thursday evening.
Wednesday evening into Thursday morning, Feb. 12 to 13
The bright star Regulus will appear near the full moon. As evening twilight ends at 6:41 p.m. EST, Regulus will be less than 2 degrees to the right of the Moon, very near its closest. By the time the Moon reaches its highest for the night at 12:55 a.m., Regulus will be 3 degrees to the right. As morning twilight begins at 6:03 a.m., Regulus will be 5 degrees to the lower right of the Moon.
Friday evening, Feb. 14
Venus, the brightest of the planets, will be near its brightest for the year (based on a geometric estimate called greatest brilliancy). As evening twilight ends at 6:43 p.m. EST, Venus will be 28 degrees above the west-southwestern horizon. Venus will set on the western horizon about 2.5 hours later at 9:09 p.m. Having Venus, named after the Roman goddess of love, shining at its brightest on this evening will make for a special Valentine's Day!
Sunday night into Monday morning Feb. 16 to 17
Bright star Spica will appear near the waning gibbous Moon. As Spica rises on the east-southeastern horizon at 10:19 p.m. EST, it will be 3.5 degrees to the lower left of the Moon. Throughout the night Spica will appear to rotate clockwise around the Moon. As the Moon reaches its highest at 3:37 a.m., Spica will be 2 degrees to the left of the Moon. By the time morning twilight begins at 5:58 a.m., Spica will be a little more than a degree above the Moon.
Monday evening, Feb. 17
This will be the first evening Mercury will be above the west-southwestern horizon 30 minutes after sunset, a rough approximation of when it might start emerging from the glow of dusk before evening twilight ends. Increasing the likelihood it will be visible, Mercury will be brighter than Mars, but not as bright as Jupiter.
Monday evening, Feb. 17
At 8:06 p.m. EST, the Moon will be at apogee, its farthest from Earth for this orbit.
Midday on Thursday, Feb. 20
The waning Moon will appear half full as it reaches its last quarter at 12:32 p.m. EST.
Friday morning, Feb. 21
The bright star Antares will appear quite near the waning crescent Moon. As the Moon rises on the southeastern horizon at 2:05 a.m. EST, Antares will be one degree to the upper left. Antares will appear to rotate clockwise and shift away from the Moon as morning progresses. By the time morning twilight begins at 5:53 a.m., Antares will be 2 degrees to the upper right of the Moon. From the southern part of South America, the Moon will actually block Antares from view.
Monday, Feb. 24
This will be the first evening Mercury will be above the western horizon as evening twilight ends at 6:54 p.m. EST, setting three minutes later at 6:57 p.m. This will be the first of two evenings when all the visible planets will be in the evening sky at the same time after twilight ends.
This also will be the evening when Mercury and Saturn will appear nearest to each other, 1.6 degrees apart. To see them you will need a very clear view toward the western horizon and will likely have to look before evening twilight ends at 6:54 p.m. EST, as Mercury will set three minutes later at 6:57 p.m., and Saturn two minutes after Mercury at 6:59 p.m.
Tuesday, Feb. 25
This will be the last evening Saturn will be above the western horizon as evening twilight ends at 6:55 p.m. EST, setting one minute later at 6:56 p.m. This will be the last of two evenings when all of the visible planets will be in the evening sky at the same time after twilight ends. Mercury and Saturn will appear almost as close together as the night before, with Mercury setting six minutes after Saturn at 7:02 p.m. Saturn, appearing about as bright as the star Pollux, may still be visible in the glow of dusk before evening twilight ends for a few evenings after this.
Thursday evening, Feb. 27
At 7:45 p.m. EST will be the new Moon, when the Moon passes between Earth and the Sun and will not be visible from Earth.
The day of, or the day after, the new Moon marks the start of the new month for most lunisolar calendars. The second month of the Chinese calendar starts on Friday, Feb. 28. Sundown on Feb. 28 also marks the start of Adar in the Hebrew calendar. In the Islamic calendar the months traditionally start with the first sighting of the waxing crescent Moon. Many Muslim communities now follow the Umm al-Qura Calendar of Saudi Arabia, which uses astronomical calculations to start months in a more predictable way (intended for civil and not religious purposes). This calendar predicts the holy month of Ramadan will start with sunset on Feb. 28, but because of Ramadan's religious significance, it is one of four months in the Islamic year where the start of the month is updated based upon the actual sighting of the crescent Moon. Ramadan is honored as the month in which the Quran was revealed. Observing this annual month of charitable acts, prayer, and fasting from dawn to sunset is one of the Five Pillars of Islam.
Friday evening, Feb. 28
As evening twilight ends at 6:58 p.m. EST, you may be able to see the thin, waxing crescent Moon barely above the western horizon. The Moon will set two minutes later at 7 p.m. Mercury will be 3.5 degrees above the Moon. For this and the next few evenings the waxing crescent Moon will appear most like an upward-facing bowl or a smile in the evening sky (for the Washington, D.C. area and similar latitudes, at least). This is called a "wet" or a "Cheshire" Moon. The term "wet Moon" appears to originate from Hawaiian mythology. It's when the Moon appears like a bowl that could fill up with water. The time of year when this occurs as viewed from the latitudes of the Hawaiian Islands roughly corresponds with Kaelo the Water Bearer in Hawaiian astrology. As the year passes into summer, the crescent shape tilts, pouring out the water and causing the summer rains. The term "Cheshire Moon" is a reference to the smile of the Cheshire Cat in Lewis Carroll's book "Alice's Adventures in Wonderland."
Saturday afternoon, March 1
At 4:14 p.m. EST, the Moon will be at perigee, its closest to Earth for this orbit.
Saturday evening, as evening twilight ends at 6:59 p.m. EST, the thin, waxing crescent Moon will be 13 degrees above the western horizon, with Venus 7 degrees to the upper right of the Moon. Mercury will appear about 10 degrees below the Moon. The Moon will set 76 minutes later at 8:15 p.m.
Tuesday, March 4
This is Mardi Gras (Fat Tuesday), which marks the end of the Carnival season that began on January 6. Don't forget to march forth on March Fourth!
Thursday, March 6
The Moon will appear half-full as it reaches its first quarter at 11:32 a.m. EST.
Saturday morning, March 8
Just after midnight, Mercury will reach its greatest angular separation from the Sun as seen from Earth for this apparition (called greatest elongation).
Saturday evening, will be when Mercury will appear at its highest (6 degrees) above the western horizon as evening twilight ends at 7:06 p.m. EST. Mercury will set 34 minutes later at 7:40 p.m. This will also be the evening Mercury will have dimmed to the brightness as Mars, after which Mars will be the third brightest visible planet again.
Also on Saturday evening into Sunday morning, March 8 to 9, Mars will appear near the waxing gibbous Moon with the bright star Pollux (the brighter of the twin stars in the constellation Gemini) nearby. As evening twilight ends at 7:06 p.m. EST, Mars will be 1.5 degrees to the lower right of the Moon and Pollux will be 6 degrees to the lower left. As the Moon reaches its highest for the night 1.25 hours later at 8:22 p.m., Mars will be 1.5 degrees to the lower right of the Moon and Pollux will be 5.5 degrees to the upper left. By the time Mars sets on the northwestern horizon at 4:53 a.m., it will be 4 degrees to the lower left of the Moon and Pollux will be 3 degrees above the Moon.
Sunday morning, March 9
Daylight Saving Time begins. Don't forget to reset your clocks (if they don't automatically set themselves) as we "spring forward" to Daylight Saving Time! For much of the U.S., 2 to 3 a.m. on March 9, 2025, might be a good hour for magical or fictional events (as it doesn't actually exist).
Tuesday evening into Wednesday morning, March 11 to 12
The bright star Regulus will appear close to the nearly full moon. As evening twilight ends at 8:09 p.m. EDT, Regulus will be 4 degrees to the lower right of the Moon. When the Moon reaches its highest for the night at 11:52 p.m., Regulus will be 3 degrees to the lower right. By the time morning twilight begins at 6:26 a.m., Regulus will be about one degree below the Moon.
Wednesday morning, March 12
Saturn will be passing on the far side of the Sun as seen from Earth, called a conjunction. Because Saturn orbits outside of the orbit of Earth it will be shifting from the evening sky to the morning sky. Saturn will begin emerging from the glow of dawn on the eastern horizon in early April (depending upon viewing conditions).
Wednesday evening, March 12
The planets Venus and Mercury will appear closest to each other low on the western horizon, 5.5 degrees apart. They will be about 5 degrees above the horizon as evening twilight ends at 8:10 p.m. EDT, and Mercury will set first 27 minutes later at 8:37 p.m.
Friday morning, March 14: Full Moon After Next
The full moon after next will be at 2:55 a.m. EDT. This will be on Thursday evening from Pacific Daylight Time and Mountain Standard Time westward to the international date line in the mid Pacific. The Moon will appear full for about three days around this time, from Wednesday evening into Saturday morning.
Total Lunar Eclipse
As the Moon passes opposite the Sun on March 14, it will move through Earth's shadow, creating a
total eclipse of the Moon
. The Moon will begin entering the partial shadow Thursday night at 11:57 p.m., but the gradual dimming of the Moon will not be noticeable until it starts to enter the full shadow Friday morning at 1:09 a.m. The round shadow of Earth will gradually shift across the face of the Moon (from lower left to upper right) until the Moon is fully shaded beginning at 2:26 a.m.
The period of full shadow, or total eclipse, will last about 65 minutes, reaching the greatest eclipse at 2:59 a.m. and ending at 3:31 a.m. Even though it will be in full shadow, the Moon will still be visible. The glow of all of the sunrises and sunsets on Earth will give the Moon a reddish-brown hue, sometimes called a "blood" Moon (although this name is also used for one of the full moons near the start of fall). From 3:31 until 4:48 a.m., the Moon will exit the full shadow of Earth, with the round shadow of Earth again shifting across the face of the Moon (from upper left to lower right). The Moon will leave the last of the partial shadow at 6 a.m. ending this eclipse.