Dr. Scott W. Fleming
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scottwfleming.bsky.social
Dr. Scott W. Fleming
@scottwfleming.bsky.social
780 followers 300 following 120 posts
Branch Manager at Space Telescope Science Institute working in the MAST archive. Astronomy PhD. Studies stars and exoplanets. Loves programming. Opinions are my own. He/Him/His
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scottwfleming.bsky.social
Heading to the @agu.org annual meeting, interested in using sound to help interpret your complex data, AND make your research more inclusive? Data sonification can help! But don't take my word for it: www.youtube.com/watch?v=X_eU...

Attend the Geo SonNet Town Hall on Dec. 15th to network!
THis poster advertises the Geo SonNet Town Hall on December 15th 2025, from 18:00-19:00 in Room 243-244 Convention Center. Who should attend? Data scientists curious about sonification, researchers seeking more intuitive sound mapping options for complex datasets, existing projects looking for new collaborative partners. There are two QR codes, one to join the listserve, another for the Geo SonNet.
November 25, 2025 at 8:41 PM
scottwfleming.bsky.social
Ever wondered what the "MAST Sky" looks like, from our ~6 PB of data spanning 3 decades...check this out! spacetelescope.github.io/mast-blog/ma...

Really fun project led by the very talented Julie Imig at MAST, showing mission coverage sky-projected! They make VERY good video backgrounds, btw. 🔭
MAST background in "standard" sky projection, in hues of blue. Lighter blue areas mark lots of observations, while darker areas are less. Numerous patterns are visible, like the continuous viewing zones as ovals in the lower-left and upper right, patterns from overlapping TESS FFIs, or the Kepler footprint shapes stamped along the ecliptic and in the original Kepler field in the upper-right. A grid of 16 images, 4x4, showing the sky background only for specific missions to get a sense of where in the sky and how much of it each mission observed to at least some depth.
July 31, 2025 at 9:12 PM
scottwfleming.bsky.social
The annual tradition of STScI Townhall at AAS being in a small, standing-room-only room continues at #AAS245. 😞
Picture shows a crowded conference room with people standing along 3 of the walls.
January 14, 2025 at 6:06 PM
scottwfleming.bsky.social
Big news at MAST! The first survey from the SDSS Legacy Archive at MAST is now available! MAST+SDSS-V partnership to host a copy of all science-ready SDSS data side-by-side with our space missions. Read more: archive.stsci.edu/contents/new... 🔭
Logo for the SDSS Legacy Archive at MAST, a purple circle containing a white silhouette of a ship's mast on a starry purple background. This is a combination of the MAST logo (the ship) and the SDSS logo (the purple color).
November 5, 2024 at 6:17 PM
scottwfleming.bsky.social
HLSP Update: GLASS-JWST augmented with NIRSpec spectra of 245 unique sources, a spectral template, and a detection catalog of >60 emission lines. These enable an exploration of cosmic evolution from cosmic noon (z~2) to the era of reionization (z> 5). 🔭 archive.stsci.edu/hlsp/glass-j...
The distribution of redshifts in this sample vs. F160W magnitude is shown in the lower-left panel, with symbols indicating observations from the GLASS-JWST program (circles, representing a significant fraction of the data points spread throughout redshift values) and JWST DD-2756 (x marks, much fewer in number but also spread throughout redshift values). Symbols are color-coded by data quality flag value from red (1) to green (4). The redshifts range from 0 to 10, which a large pile-up between 0-1 but a fair sampling out to redshift of 6 and several near redshift 8. The completeness of redshifts is shown in the upper panel, comparing spectroscopically determined redshifts (blue) and redshift estimates from photometry (red), where blue dominates the redshift bins except in the lowest range of 0-1 where a fair fraction are in red. The right panel shows the completeness with F160W magnitude, following the same color scheme, mostly blue except the 29-30 mag range is all red.
October 29, 2024 at 4:49 PM
scottwfleming.bsky.social
HLSP Update: TESS-SPOC calibrated light curves and target pixel files from TESS full frame images for Sector 72 are now available at MAST. This Sector adds 159999 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/tess-spoc 🔭
A histogram showing the number of targets per 0.25 magnitude bin from three different categories: two-minute targets (in dark blue), FFI-included targets (in light blue) and FFI field star targets (in red). The two-minute targets are primarily between TESS magnitude 8-12 and the maximum bin count is approximately 1000. The FFI-include targets have a more strongly peaked distribution centered on TESS magnitude 11 and at the maximum bin count is approximately 6500. The FFI field star targets also follow a strongly-peaked distribution centered at TESS magnitude 12.5 and have a maximum bin count size of almost 16000.
October 25, 2024 at 5:58 PM
scottwfleming.bsky.social
HLSP Update: OPAL HST observations of Saturn from Cycle 31 are now available at MAST. OPAL is a multi-year HST survey of the outer planets to observe how their atmospheres change over time. archive.stsci.edu/hlsp/opal 🔭
An image collage showing HST observations of, from left to right, Jupiter, Uraus, Saturn, Neptune. The images are in color: Jupiter and Saturn in hues of orane, yellow, and brown, while Neptune and Uranus are shades of blue. The images are highly detailed, such that structures in their atmospheres like cloud bands are clearly visible.
October 23, 2024 at 2:35 PM
scottwfleming.bsky.social
HLSP Update: QLP calibrated light curves from TESS full frame images for Sector 80 are now available at MAST. This Sector adds 1750792 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp 🔭
Sky projected plot of the Sectors 56-80 footprints on the sky. Each footprint is shaded a different color to stand out compared to others. Right ascension is along the x-axis and declination is along the y-axis. The biggest gaps in coverage occur approximately between -20 degrees and +50 degrees declination along right ascension 10 to 20 hours, and from -60 to +20 degrees declination along right ascension 0 to 7 hours.
October 22, 2024 at 5:36 PM
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HLSP Update: REFERENCE-ATLASES, 19 new white dwarf (WD) stars were added that are fainter than most of the other CALSPEC stars. Therefore, 19 stellar spectra files (stis) and 19 model files (mod) are being delivered for the first time. archive.stsci.edu/hlsp/referen... 🔭
Ratio to the 9550 K model continuum level for the STIS measured fluxes (shown in black), the Kurucz 9550 K, log g=3.95 model (shown in green), and the Kurucz 9400 K model (shown in red). The red model has a ratio > 1 in the red/infrared part of the spectrum starting at roughly 6000 Angstroms. Top panel shows 1800-3200 Angstroms, where both green and red models ratios are below the STIS measured fluxes (shown in black).
October 22, 2024 at 5:22 PM
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HLSP Update: TESS-SPOC calibrated light curves and target pixel files from TESS full frame images for Sector 71 are now available at MAST. This Sector adds 159,999 targets derived from 200 second cadence FFIs. 🔭 archive.stsci.edu/hlsp/tess-spoc
A histogram showing the number of targets per 0.25 magnitude bin from three different categories: two-minute targets (in dark blue), FFI-included targets (in light blue) and FFI field star targets (in red). The two-minute targets are primarily between TESS magnitude 8-12 and the maximum bin count is approximately 1000. The FFI-include targets have a more strongly peaked distribution centered on TESS magnitude 11 and at the maximum bin count is approximately 6500. The FFI field star targets also follow a strongly-peaked distribution centered at TESS magnitude 12.5 and have a maximum bin count size of almost 16000.
October 22, 2024 at 5:13 PM
scottwfleming.bsky.social
New HLSP: Scylla is a pure-parallel HST-WFC3 imaging survey that operated alongside the ULLYSES survey. Named for the monster from the myth, Scylla surveyed LMC and SMC fields from the near UV to the IR. The first data release consists of 96 fields over 342 orbits. 🔭 archive.stsci.edu/hlsp/scylla
This figure has one large panel and two smaller panels to the right. The large panel has a grayscale map of the SMC, which appears as dark, wispy clouds against the white background. There are dots of different colors around the map, each labeled with a number. Two red boxes highlight regions in the map, which are expanded in the panels to the right. The two panels to the right show zoomed-in views of dense, dusty regions of the SMC, which also appear as wispy, but denser, dark clouds. These panels also have several colored dots with numbered labels.
October 22, 2024 at 4:22 PM
scottwfleming.bsky.social
New HLSP: SMILES is a 34 sq arcmin multi-band JWST/MIRI imaging survey of the GOODS-S/HUDF region with NIRSpec follow-up, aimed at "cosmic noon" science 🕛. Its first data release presents custom-reduced mosaics in 8 MIRI bands & a photometric catalog: archive.stsci.edu/hlsp/smiles 🔭
Red, green, and blue galaxies speckle a black rectangle representing representing the survey footprint. Above and below the footprint are smaller squares showing two zoomed-in regions in different filters. The views range from sharply resolved galaxies with spiral arms and dust lanes visible against the dark background, to barely resolved blobs of light amidst a speckled, gray background.
September 19, 2024 at 12:54 AM
scottwfleming.bsky.social
New HLSP: The WIDE Survey releases reduced JWST/NIRSpec spectra from the first 5 (of 31) pointings from the CANDELS/AEGIS fields, each with an average of 135 galaxies. 2D and 1D extracted spectra from low-resolution PRISM and high-resolution gratings! archive.stsci.edu/hlsp/wide 🔭
This image has two panels showing a 1D and 2D spectrum of the same galaxy. The top panel shows the 1D spectrum as a blue line with peaks and dips at various emission and absorption features. The bottom panel shows the 2D spectrum as a blue-to-yellow heatmap. The spectrum peaks are now represented by bright yellow features, while the dips are represented by bluish lines crossing the yellow-colored spectrum.
September 12, 2024 at 6:19 PM
scottwfleming.bsky.social
Very grateful and excited to be participating in the arXiv Accessibility Forum on Sonification event tomorrow! It's completely free so check out the forum accessibility2024.arxiv.org. Event is 3-5 PM US Eastern, Zoom link: cornell.zoom.us/j/9530370483... | #AccessCantWait #arXivAccessibility2024
Poster advertising the signup URL, with headshots of the participants: Kate Meredith, Sarah Kane, Dr. Leif Karlstrom, Phia Damsma, and Scott Fleming. The date is September 10th and the title is "Sonification: Why Multi-Modal Science is the Future"
September 9, 2024 at 9:29 PM
scottwfleming.bsky.social
MSTARPANSPEC adds data for LTT 1445A and GJ 486, the two closest M-dwarfs with transiting exoplanets. Panchromatic spectra are constructed from UV and X-ray observations, Ly-a reconstructions, DEM estimates, and BT-settl models. archive.stsci.edu/hlsp/mstarpa... 🔭
This figure shows the panchromatic spectrum of GJ 486, with wavelength on the x-axis and flux density on the y-axis. Different wavelength regions are shaded in color, from the X-ray observations from XMM-Newton (shaded in purple), the DEM estimate in the EUV (shaded in blue), the optical spectrum including a Ly-a reconstruction from HST observations (shaded in green), and a BT-settl model of the IR (shaded in yellow).
September 6, 2024 at 8:34 PM
scottwfleming.bsky.social
TESS-SPOC calibrated light curves and target pixel files from TESS full frame images for Sector 70 are now available at MAST. This Sector adds 159994 targets derived from 200 second cadence FFIs. 🔭 archive.stsci.edu/hlsp/tess-spoc
A histogram showing the number of targets per 0.25 magnitude bin from three different categories: two-minute targets (in dark blue), FFI-included targets (in light blue) and FFI field star targets (in red). The two-minute targets are primarily between TESS magnitude 8-12 and the maximum bin count is approximately 1000. The FFI-include targets have a more strongly peaked distribution centered on TESS magnitude 11 and at the maximum bin count is approximately 6500. The FFI field star targets also follow a strongly-peaked distribution centered at TESS magnitude 12.5 and have a maximum bin count size of almost 16000.
September 6, 2024 at 8:19 PM
scottwfleming.bsky.social
HLSP Update: QLP calibrated light curves from TESS full frame images for Sector 79 are now available at MAST. This Sector adds 668387 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp 🔭
Sky projected plot of the Sectors 56-80 footprints on the sky. Each footprint is shaded a different color to stand out compared to others. Right ascension is along the x-axis and declination is along the y-axis. The biggest gaps in coverage occur approximately between -20 degrees and +50 degrees declination along right ascension 10 to 20 hours, and from -60 to +20 degrees declination along right ascension 0 to 7 hours.
August 23, 2024 at 3:27 PM
scottwfleming.bsky.social
HLSP Update: QLP calibrated light curves from TESS full frame images for Sector 78 are now available at MAST. This Sector adds 727249 targets derived from 200 second cadence FFIs. 🔭 archive.stsci.edu/hlsp/qlp
Sky projected plot of the Sectors 56-80 footprints on the sky. Each footprint is shaded a different color to stand out compared to others. Right ascension is along the x-axis and declination is along the y-axis. The biggest gaps in coverage occur approximately between -20 degrees and +50 degrees declination along right ascension 10 to 20 hours, and from -60 to +20 degrees declination along right ascension 0 to 7 hours.
August 19, 2024 at 9:43 PM
scottwfleming.bsky.social
HLSP Update: QLP calibrated light curves from #TESS full frame images for Sector 77 are now available at MAST. This Sector adds 873052 targets derived from 200 second cadence FFIs. 🔭 archive.stsci.edu/hlsp/qlp
Sky projected plot of the Sectors 56-80 footprints on the sky. Each footprint is shaded a different color to stand out compared to others. Right ascension is along the x-axis and declination is along the y-axis. The biggest gaps in coverage occur approximately between -20 degrees and +50 degrees declination along right ascension 10 to 20 hours, and from -60 to +20 degrees declination along right ascension 0 to 7 hours.
August 19, 2024 at 9:38 PM
scottwfleming.bsky.social
Having attended Dragon*con for some 16 years, I’m super excited to be ON panels this time to talk space telescopes, exoplanets, and more!
A picture of my schedule at Dragon*con, one panel on Friday Aug 30 at 8:30 PM about next-gen telescopes in space, one Saturday at 7 PM on exoplanets, one Saturday at 11:30 PM about the Institute I work at, and one on Monday about how raw data turn into published papers!
August 16, 2024 at 8:19 PM
scottwfleming.bsky.social
New HLSP: NLR-AGN provides [O III] imaging of narrow line region outflows in nearby active galaxies. The 12 Seyfert galaxies span a moderate range in luminosity, black hole mass, and Eddington ratio to study effects of outflow parameters on AGN properties. archive.stsci.edu/hlsp/nlr-agn
This picture contains 3 panels, each showing the galaxy NGC 5135 in a different filter. The left panel shows spiral arms, dust lanes, and bright star forming regions throughout the galaxy. The middle panel is similar to the left, but more strongly emphasizes the star forming regions. The right panel shows a difference image between the first two panels, where the spiral arms are less visible, and the star forming regions glow brightly against the dark background.
August 16, 2024 at 8:05 PM
scottwfleming.bsky.social
New HLSP: Complete FUV spectroscopic atlas of young star clusters in the CLUES survey. Check out the numerous stellar and interstellar medium features in the HST COS spectra, providing unique information about the massive star census and their feedback. archive.stsci.edu/hlsp/clues 🔭
The CLUES atlas of far-ultraviolet (FUV) spectra at 0.4 Å spectral resolution is displayed, organized by the age of the star clusters. The spectra feature signatures from massive stars in the targeted clusters and ionized gas along the line of sight between the clusters and the observers. A total of 20 different spectra are plotted, stacked vertically along the y-axis. The horizontal axis shows the rest-frame wavelength, ranging from approximately 1150 Å to 1750 Å. Vertical dashed lines mark some photospheric lines, P-Cygni lines from stellar winds, and absorption lines from the interstellar medium (ISM), with labels for lines such as He II, C II, C III, N V, O IV, Al II, Si II, Si IV, and Fe II. Asymmetries in the gas features suggest strong winds driven by energy from massive stars. Certain regions, including Lyα emission, O I geocoronal lines, and detector gaps around 1300 Å and 1600 Å, are omitted for clarity.
August 12, 2024 at 6:06 PM
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HLSP Update: QLP calibrated light curves from TESS full frame images for Sector 76 are now available at MAST. This Sector adds 950787 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp 🔭
Sky projected plot of the Sectors 56-80 footprints on the sky. Each footprint is shaded a different color to stand out compared to others. Right ascension is along the x-axis and declination is along the y-axis. The biggest gaps in coverage occur approximately between -20 degrees and +50 degrees declination along right ascension 10 to 20 hours, and from -60 to +20 degrees declination along right ascension 0 to 7 hours.
August 7, 2024 at 1:47 PM
scottwfleming.bsky.social
New HLSP: LMC-FLOWS provides continuum normalized S II, Si IV, and C IV interstellar absorption lines (and their corresponding best-fit continuum models) to study diffuse ionized gas in the CGM and ISM of the Milky Way and the Large Magellanic Cloud. archive.stsci.edu/hlsp/lmc-flows 🔭
The image consists of three panels, each displaying a spectral region approximately 20 Ångströms wide, centered on the S II (top), Si IV (middle), and C IV (bottom) doublets. The vertical axis of each panel represents the UV flux in units of ergs per second per square centimeter per Ångström, while the horizontal axis shows the wavelength in Ångströms: the top panel's wavelength range is 1246–1258 Å centered on S II, the wavelength range of the middle panel centered on Si IV is 1390–1410 Å and the bottom panel centered on C IV has the wavelength range of 1540–1560 Å. Each panel contains a legend explaining the lines and shaded regions. Black solid lines indicate the original fluxes and gray solid lines represent the corresponding uncertainties from the ULLYSES DR5 data. The red curves illustrate the best-fit continuum models estimated by the team using Gaussian Process regression.
August 2, 2024 at 5:58 PM
scottwfleming.bsky.social
HLSP Update: QLP calibrated light curves from TESS full frame images for Sector 75 are now available at MAST. This Sector adds 1024065 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp
Sky projected plot of the Sectors 56-74 footprints on the sky. Each footprint is shaded a different color to stand out compared to others. Right ascension is along the x-axis and declination is along the y-axis. The biggest gaps in coverage occur approximately between -20 degrees and +50 degrees declination along right ascension 10 to 20 hours, and from -60 to +20 degrees declination along right ascension 0 to 7 hours.
August 2, 2024 at 1:14 AM