iiinova — where your digital self keeps evolving

Dr. Scott W. Fleming @scottwfleming.bsky.social · 06/01/2026

Really proud to advertise our accepted peer-reviewed paper analyzing the impact of MAST through analysis of 37,000 papers published in 40 journals over the last 50 years. It's a capstone to decades of work by dozens of MAST staff. Check out the preprint: arxiv.org/abs/2512.18101 (1/3) 🔭

Screenshot showing the title, authors, and abstract. Title is "The Impact of the MAST Data Archive". The abstract is "The Barbara A. Mikulski Archive for Space Telescopes (MAST) hosts science-ready data products from over twenty NASA missions, plus community-contributed data collections, and other select surveys. The data support forefront research in the ultraviolet, optical, and near-infrared wavelength bands. We have constructed bibliographies for each mission from publications in nearly 40 professional journals, and have identified more than 37,000 refereed articles where investigators made a science usage of data hosted in MAST. The publication rate over the last 50 years shows that most MAST missions have had very high productivity during their in-service lifetimes, and have remained so for years or decades afterward. Annual citations to these publications, a measure of impact on research, are robust for most missions, with citations that grow over more than a decade. Most of the citations come from about 10% of articles within each mission.
We examined the bibliographies of the active missions HST and JWST in greater detail. For HST the rate of archival publications exceeded those authored by the original observing teams within a decade of launch, and is now more than 3 times higher. Early indications hint that JWST archival articles could dominate the publication rate even sooner. The production of articles resulting from any given observing program can extend for decades. Programs with small and very large allocations of observing time tend to be particularly productive per unit of observing time. For HST in general, a first publication appears within 1.5 yr for 50% of observing programs, and within 3.8 yr for 80% of programs. We discuss various external factors that affect publication metrics, their strengths and limitations for measuring scientific impact, and the challenges of making meaningful comparisons of publication metrics across missions."

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 25/11/2025

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 31/07/2025

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 14/01/2025

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 05/11/2024

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... 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 29/10/2024

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...

$The distribution of redshifts in this sample vs. F160W magnitude is shown in the lower-left panel, with symbols indicating observations from the GLASS-JWST program (circles, representing a significant fraction of the data points spread throughout redshift values) and JWST DD-2756 (x marks, much fewer in number but also spread throughout redshift values). Symbols are color-coded by data quality flag value from red (1) to green (4). The redshifts range from 0 to 10, which a large pile-up between 0-1 but a fair sampling out to redshift of 6 and several near redshift 8. The completeness of redshifts is shown in the upper panel, comparing spectroscopically determined redshifts (blue) and redshift estimates from photometry (red), where blue dominates the redshift bins except in the lowest range of 0-1 where a fair fraction are in red. The right panel shows the completeness with F160W magnitude, following the same color scheme, mostly blue except the 29-30 mag range is all red.$

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 25/10/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 23/10/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 22/10/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 22/10/2024

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).

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 22/10/2024

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

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 22/10/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 19/09/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 12/09/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 09/09/2024

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

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 06/09/2024

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).

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 06/09/2024

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

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 23/08/2024

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 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 19/08/2024

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

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 19/08/2024

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

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 16/08/2024

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!

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 16/08/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 12/08/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 07/08/2024

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 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 02/08/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 02/08/2024

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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 16/07/2024

HLSP Update: BOSZ 2024 synthetic stellar spectra (Mészáros et al. 2024). ATLAS9 and MARCS models 628,620 total spectra, from 50 nm to 32 microns at resolutions from 500 up to 600,000, including line identifiers. This was a lot of models to get ready for you all! 🔭 archive.stsci.edu/hlsp/bosz

Three-panel plot showing log(g) vs. T_eff, alpha vs. metallicity, and carbon vs. metallicity for the model grid. The models cover a wide range of parameter space, with finer sampling for lower stellar temperatures. Plotted in the background of each plot is the sample of APOGEE stellar parameters, showing the grid samples the parameter space well.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 28/06/2024

HLSP Update: QLP calibrated light curves from #TESS full frame images for Sector 74 are now available at MAST. This Sector adds 911640 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 28/06/2024

HLSP Update: BOSZ 2017 model files had wavelengths in air rather than in vacuum. Revised models are in vacuum from Meszaros, S, et al. (2024) and supersede the 2017 legacy models. This delivery updates both the STIS and the model files for 55 stars. archive.stsci.edu/hlsp/referen... 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 20/06/2024

HLSP Update: QLP calibrated light curves from TESS full frame images for Sector 73 are now available at MAST. This Sector adds 862017 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 14/06/2024

New HLSP: The Plane Quasar Survey (PQS) is a catalog of 305 UV-bright QSO candidates at low Galactic latitudes, with 193 spectroscopically-confirmed AGN. The sample will enable new studies of the Milky Way and Local Group circumgalactic medium! archive.stsci.edu/hlsp/pqs 🔭

An all-sky Aitoff projection in Galactic coordinates showing the distribution of different UV-bright QSO samples, including the QSO candidates from the Plane Quasar Survey (dark and light purple shapes).

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 10/06/2024

New Hello Universe project: Interpreting Convolutional Neural Networks - a tutorial of techniques that can be used to visualize the importance of data features in machine learning models. archive.stsci.edu/hello-univer...

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 03/06/2024

HLSP Update: QLP calibrated light curves from TESS full frame images for Sector 72 are now available at MAST. This Sector adds 721754 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 16/05/2024

HLSP Update: OPAL outer planet legacy survey releases HST observations of Jupiter from Cycle 30. Now includes 9 years worth of observations monitoring its atmosphere. archive.stsci.edu/hlsp/opal 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 08/05/2024

HLSP Update: The JADES Collaboration releases a third set of mosaics, spectra, and catalogs. The new mosaics cover 56 sq arc minutes of the GOODS-N field while over 4000 spectra with 2375 sources with measured redshifts comprise the spectroscopic release. archive.stsci.edu/hlsp/jades 🔭

The figure shows a cutout from the full GOODS-N image covering the original HDF. It is a mosaic of JADES JWST/NIRCam data covering the original Hubble Deep Field region. Shown are the F444W, F200W, and F090W mosaics as the red-green-blue channels of this multicolor image. Hundreds of galaxies, some resolved enough to see their shape, others unresolved and left as dots of light, are seen in a variety of colors ranging from blues to yellows and reds. The iconic Hubble Deep Field (Williams et al. 1996) footprint is shown as a silver line.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 04/05/2024

QLP calibrated light curves from TESS full frame images for Sector 71 are now available at MAST. This Sector adds 845012 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/qlp 🔭

Sky projected plot of the Sectors 56-69 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.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 17/04/2024

HLSP Update: The MUDF team releases a spectroscopic catalog with redshifts of 419 galaxies from z = 0-6 with measurements of up to 32 emission lines from the rest-frame UV to NIR. The catalog and new science results are presented in Revalski et al. 2024. archive.stsci.edu/hlsp/mudf 🔭

A color-composite HST image of the MUDF field. The deep central regions contain numerous distant galaxies as well as foreground stars in our galaxy. Spectral traces from the HST WFC3 G141 Grism are superimposed on each source, appearing as a bright rainbow vertical line for each target in the image. Image processing done by Joseph DePasquale (STScI).

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 17/04/2024

More TESS-SPOC calibrated light curves and target pixel files, these from Sector 66, are now available at MAST. This Sector adds 159998 targets derived from 200 second cadence FFIs. archive.stsci.edu/hlsp/tess-spoc 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 10/04/2024

More TESS-SPOC calibrated light curves and target pixel files from TESS full frame images for Sector 69 are now available at MAST! This Sector adds 159,997 targets derived from 200 second cadence FFIs. 🔭 archive.stsci.edu/hlsp/tess-spoc

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 26/03/2024

New HLSP: CANDELSNIWRL - New F160W mosaics of the CANDELS fields from the NIRWL team. Updated alignment to the Gaia DR3 catalog and correction of systematic effects from previous versions. See archive.stsci.edu/hlsp/candels... and Finner et al. 2023: ui.adsabs.harvard.edu/abs/2023ApJ.... 🔭

The figure presents a color image of a region of the COSMOS field that is rich in galaxies. The variety of galaxies presented is vast. Elliptical galaxies of varying colors of yellow, orange, and red show the effect of redshift and environment. Spiral disks and irregular galaxies tend to be blue and have distinct morphologies. On the right of the figure are five histograms, one for each of the CANDELS fields, that display the astrometric offset of Gaia DR3 star positions from star positions in the CANDELS Treasury mosaics and those in the NIRWL mosaics. The histograms show that the NIRWL mosaics are better aligned to Gaia than the Treasury mosaics.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 19/03/2024

Late post from back in January - New HLSP: PHATHIGHMASS! Physical properties for 42,107 main-sequence massive star candidates in Andromeda. Catalog includes stellar and line-of-sight extinction estimates. If you're interested, you can find more details here: archive.stsci.edu/hlsp/phathig... 🔭

Distribution of PHATHIGHMASS stars, illustrated as red and orange dots and colored by BEAST-derived extinction, atop a black and white 24-micron Spitzer image showing dust within the Andromeda galaxy. Most of the stars appear to dot the spiral arms of Andromeda.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 19/03/2024

Late post about an HLSP update (back from 22 Nov. 2023 😅) - CDIPS (Cluster Difference Imaging Photometric Survey) sixth data release from TESS Cycles 3+4 (Sectors 27-55). CDIPS targets include age-dated and age-dateable stars within one kiloparsec of the Sun. archive.stsci.edu/hlsp/cdips 🔭

Sky projection in Galactic latitude and longitude showing the location of CDIPS stars in blue. They are primarily along the Galactic plane. A few clusters of targets are at higer and lower Galactic longitudes.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 19/02/2024

New HLSP: PHANGS-JWST. PHANGS is a panchromatic dataset to study star formation in nearby spiral galaxies, combining ALMA+VLT+HST+JWST and more. Their JWST Cycle 1 Treasury survey has released 8 JWST bands for 19 galaxies. 🔭 archive.stsci.edu/hlsp/phangs/... Look at these images!

This collection of images from the NASA/ESA/CSA James Webb Space Telescope shows 19 face-on spiral galaxies captured by NIRCam and MIRI.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 15/02/2024

New HLSP: JWST sees stars galore! New data and software from the Resolved Stellar Population Early Release Science team showcase how JWST can resolve individual stars in nearby galaxies and star clusters. 🔭 archive.stsci.edu/hlsp/jwststars

The NIRCam observation of Wolf–Lundmark–Melotte (WLM), a star-forming dwarf galaxy, displays a spectacular composite color image of a vast tapestry of stars and background galaxies. The zoomed images within the red, orange, and blue boxes highlight JWST's ability to resolve its diverse stellar populations, from young to old, in various colors. The red and orange boxes highlight a young star-forming complex and a more typical region in WLM. The blue box displays both the member stars and several background red galaxies. The right panel shows a color-magnitude diagram (CMD) of WLM using NIRCam F090W-F150W. It displays a wide variety of stellar sequences that span a range of ages, from young to ancient stars that span a wide range of colors and magnitudes. This CMD of WLM is the deepest taken for a galaxy outside the immediate vicinity of the Milky Way.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 13/02/2024

GSFC-ELEANOR-LITE TESS light curves for Sector 10 are now available at MAST. This Sector adds 9,717,705 light curves to the collection. There are now a total of 49 million light curves in this collection. archive.stsci.edu/hlsp/gsfc-el...

Top panel shows number of stars per 0.1 magnitude bin in the TESS band. X-axis ranges from 0 to 16. The number of stars in each bin increases steadily, up to a maximum at the last bin of more than 5x10^6. The bottom panel shows the number of light curves from GSFC-ELEANOR-LITE per TESS Sector. The x-axis ranges from Sector 1 to Sector 26. The largest Sector is Sector 12, with 2x10^7 light curves.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 09/02/2024

More QLP calibrated TESS light curves for Sector 70 are now available at MAST. This release adds 368,003 light curves to the collection. archive.stsci.edu/hlsp/qlp 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 05/02/2024

More QLP calibrated TESS light curves for Sector 69 are now available at MAST. This release adds 416,694 light curves to the collection. archive.stsci.edu/hlsp/qlp 🔭

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 11/01/2024

More TESS-SPOC calibrated light curves and target pixel files from TESS FFIs (Sectors 67+68.) These add 159,998 and 159,999 targets each, derived from 200s cadence FFIs. Sector 66 data are under review by the TESS-SPOC team...coming soon. 🔭https://archive.stsci.edu/hlsp/tess-spoc

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 07/01/2024

The Hilton key cards are awesome this year!

Hotel key card with a nebula in the background and a puppy and kitty in the foreground.

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Dr. Scott W. Fleming @scottwfleming.bsky.social · 07/01/2024

HLSP Update: More QLP calibrated TESS light curves, these from Sector 67, now available at MAST. This release adds 720,775 light curves to the collection. archive.stsci.edu/hlsp/qlp 🔭

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