adsabs/AstroCLIMB huggingface dataset:
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: Heatmap of the (equatorial) on-sky positions of discovered objects over the full survey (top panel), first 2 yr (second panel), and final 2 yr (bottom panel). Discoveries are concentrated on the ecliptic plane. The discoveries in the first 2 yr comprise a large fraction of the full survey’s discoveries, though late-survey discoveries are still substantial. Bright objects in the NES that happen to not be discovered early in the survey are often discovered as they enter the WFD survey area, leading to an overdensity of objects at the western NES-WFD boundary and an underdensity at the eastern boundary.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: Fraction of simulated objects discovered (“discovery completeness”) for NEOs, MBAs, and Jupiter Trojans. The NEO population is measured in diameter while the MBAs and Trojans are measured in Hr. Bright-end loss of completeness is due to bright source saturation. The Hr and diameter axes are aligned assuming a reference albedo of 0.25. The Jupiter Trojans, being relatively spatially confined, drop sharply from very high to very low completeness over a small range of absolute magnitudes. NEO completeness shrinks, but does not reach zero even at diameters of 1 m.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: A heatmap of the simulated detections from a typical night (2025 August 17), with the ecliptic plane dashed in black. The night is spent observing a mostly contiguous section of the WFD survey, with no time spent on the deep drilling fields or mini-surveys. As expected, detections are much more numerous close to the ecliptic.
Paper: Apache Point Rapid Response Characterization of Primitive Imminent Impactor 2024 RW1
Authors: Carl Ingebretsen, Bryce T. Bolin, Robert Jedicke, Peter Vereš, Christine H. Chen, Carey M. Lisse, Russet McMillan, Torrie Sutherland, Amanda J. Townsend
Figure caption: The path of 2024 RW1 is indicated by the red line while the Earth is represented by a green circle drawn to scale. The black curve is the orbit of the Moon with the location of the Moon at the time of observation indicated by a gray circle (not to scale). The insert shows a zoomed-in view of the path over Earth. The final point of impact at 18.083657°N, 123.002342° E is marked by a black star. The blue star indicates the location where we observed 2024 RW1 before its impact. Both the main plot and insert are in cartesian equatorial coordinates plotted in the YZ plane. The YZ plane has been used in this plot to show the impact location of 2024 RW1 on the Earth’s surface from the reader’s point of view.
Paper: Apache Point Rapid Response Characterization of Primitive Imminent Impactor 2024 RW1
Authors: Carl Ingebretsen, Bryce T. Bolin, Robert Jedicke, Peter Vereš, Christine H. Chen, Carey M. Lisse, Russet McMillan, Torrie Sutherland, Amanda J. Townsend
Figure caption: Reflectance spectrophotometry of 2024 RW1 consisting of g, r, i, and z observations of 2024 RW1 on 2024 September 4 UTC. The λeff locations of the g, r, i, and z filters have been plotted as vertical dashed lines. The data points for the normalized reflectivity of 2024 RW1 have been offset slightly from their location in the wavelength direction. The error bars on the data points correspond to 1σ uncertainty. The spectrum has been normalized to unity at 550 nm, as indicated by the red X. The spectral range of C-, S-, and B-type asteroids from the Bus–DeMeo asteroid taxonomic catalog (F. E. DeMeo et al. 2009) are over-plotted with the B-type spectrum most closely resembling the spectra of 2024 RW1.
Paper: Apache Point Rapid Response Characterization of Primitive Imminent Impactor 2024 RW1
Authors: Carl Ingebretsen, Bryce T. Bolin, Robert Jedicke, Peter Vereš, Christine H. Chen, Carey M. Lisse, Russet McMillan, Torrie Sutherland, Amanda J. Townsend
Figure caption: Top panel: phased r filter lightcurve data of 2024 RW1 using a single-peaked lightcurve period of ∼950 s. Middle panel: Lomb–Scargle periodogram of lightcurve period vs. spectral power (N. R. Lomb 1976) for the r-band images. A peak in the power is located at a single-peaked lightcurve period of 975.9, implying a double-peaked lightcurve of 1951.8 s. Bottom panel: phase dispersion minimization analysis of lightcurve rotation period vs. Θ metric (R. F. Stellingwerf 1978). The Θ metric is minimized at a single-peaked rotation period of 950.4 s implying a double-peaked rotation period of 1900.8 s.
Paper: Apache Point Rapid Response Characterization of Primitive Imminent Impactor 2024 RW1
Authors: Carl Ingebretsen, Bryce T. Bolin, Robert Jedicke, Peter Vereš, Christine H. Chen, Carey M. Lisse, Russet McMillan, Torrie Sutherland, Amanda J. Townsend
Figure caption: Top-left panel: a median-combined stack of 7 × 45 s g filter images of 2024 RW1 encircled in white. Top-right panel: a median-combined stack of 10 × 45 s r filter images of 2024 RW1. Bottom-left panel: a median-combined stack of 6 × 45 s i filter images of 2024 RW1. Bottom-right panel: a median-combined stack of 5 × 45 s z filter images of 2024 RW1. The images were taken with the telescope tracked at the asteroid’s apparent rate of motion. The orientation of each image is indicated by the compass rose. Each image stack is 114″ by 114″.
Paper: Apache Point Rapid Response Characterization of Primitive Imminent Impactor 2024 RW1
Authors: Carl Ingebretsen, Bryce T. Bolin, Robert Jedicke, Peter Vereš, Christine H. Chen, Carey M. Lisse, Russet McMillan, Torrie Sutherland, Amanda J. Townsend
Figure caption: SDSS a* vs. i–z color indices of 2024 RW1 plotted with a* vs. i–z colors of C (blue), S (red) and V (green) type asteroids (Ž. Ivezić et al. 2001; M. Jurić et al. 2002). The colorization scheme of data points as a function of a* and i–z is adapted from Ž. Ivezić et al. (2002). The a* and i–z range of average S, V, and C-type asteroids are shown computed from the average spectra from F. E. DeMeo et al. (2009).
Paper: V659 Cen: System Members Updated
Authors: Nancy Remage Evans, Charles Proffitt, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: Radial velocities of V659 Can. Top left: the pulsational velocity curve as a function of pulsation phase (Ppuls = 5.624 days), color coded by orbital phase (Porb = 5708 days). Top right: fit residuals against BJD, color coded by pulsation phase. Bottom left: the isolated orbital velocity curve as a function of (and color coded by) orbital phase. Bottom right: the isolated orbital velocity as a function of BJD color coded by pulsation phase.
Paper: V659 Cen: System Members Updated
Authors: Nancy Remage Evans, Charles Proffitt, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: Energy distribution V659 Cen Companion B. Left: the difference between the spectrum and the model. Model temperatures (starting from the top) are 14,500, 15,000, 15,500, 15,750, 16,000, 16,250, 16,500, 17,000 K. The x-axis is wavelength in Å, the y-axis is flux difference in erg cm−2 s−1 Å−1, and the models are offset for clarity. Right: the standard deviations from the spectrum–model comparison for V659 Cen as the temperature of the models is changed. Dots are the values of standard deviation and triangles are the parabola fit.
Paper: V659 Cen: System Members Updated
Authors: Nancy Remage Evans, Charles Proffitt, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: Energy distribution comparisons for V659 Cen Companion B. Comparisons are for the spectrum (black) with model atmospheres (red) for a series of temperatures from 14,500 to 17,000 K. The x-axis is wavelength in angstroms; the y-axis is flux in erg cm−2 s−1 Å−1.
Paper: V659 Cen: System Members Updated
Authors: Nancy Remage Evans, Charles Proffitt, Pierre Kervella, Joanna Kuraszkiewicz, H. Moritz Günther, Richard I. Anderson, Alexandre Gallenne, Antoine Mérand, Boris Trahin, Giordano Viviani, Shreeya Shetye
Figure caption: The schematic summary of the members of the V659 Cen system. The components are at the top. Below them is the information about the spectral type. Below that is an estimate of the separation.
Paper: Precise Physical Parameters, Habitability, and Orbital Stability of Sun-like SB2 Systems: HD 130669, HD 184467, HD 191854, and HD 214222
Authors: Ahmad Abushattal, Nikolaos Georgakarakos, Mashhoor A. Al-Wardat, Bilal Algnamat, Hassan B. Haboubi, Deshinta Arrova Dewi, Enas M. Abu-Alrob, Abdallah M. Hussein
Figure caption: A flowchart of the methodology used in this work.
Paper: Precise Physical Parameters, Habitability, and Orbital Stability of Sun-like SB2 Systems: HD 130669, HD 184467, HD 191854, and HD 214222
Authors: Ahmad Abushattal, Nikolaos Georgakarakos, Mashhoor A. Al-Wardat, Bilal Algnamat, Hassan B. Haboubi, Deshinta Arrova Dewi, Enas M. Abu-Alrob, Abdallah M. Hussein
Figure caption: Circumstellar habitable zones for HD 130669, HD 191854, and HD 214222. Blue color: PHZ, yellow color: AHZ, green color: EHZ, red color: uninhabitable area, purple color: areas of dynamical instability. The white line marks the eccentricity of the stellar binary, while the vertical black lines are the borders of the classical habitable zone.
Paper: Precise Physical Parameters, Habitability, and Orbital Stability of Sun-like SB2 Systems: HD 130669, HD 184467, HD 191854, and HD 214222
Authors: Ahmad Abushattal, Nikolaos Georgakarakos, Mashhoor A. Al-Wardat, Bilal Algnamat, Hassan B. Haboubi, Deshinta Arrova Dewi, Enas M. Abu-Alrob, Abdallah M. Hussein
Figure caption: Circumbinary stability curves for the four binary systems HD 130669, HD 184467, HD 191854, and HD 214222. The curves show the critical semimajor axis acr of a stable circumbinary planet as a function of planet eccentricity ep, calculated based on the orbital and stellar parameters of each system.
Paper: On the Detection of Exorings in Reflected Light with JWST NIRCam
Authors: Rachel Bowens-Rubin, Mary Anne Limbach, Sam Hopper, Klaus Subbotina Stephenson, Matson Garza, Leigh N. Fletcher, Matthew Hedman
Figure caption: Minimum instrument contrast needed to detect an exoring system with same area as Saturn rings. Instruments capable of reaching contrasts above that of the black line at a given separation (shaded in green) would be capable of detecting face-on, fully reflective exoring systems with the equivalent area of Saturn’s rings. As such, the black line provides the most optimistic contrast that would be needed to make the detection. Current ground-based instrumentation may be capable of reaching the contrasts required at tight separations (see zoomed plot on right). (a) The approximate AU separation of the superpuff HIP 41378 f is plotted in gray to show an example of an exoplanet theorized to have a ring system. (The separation of HIP 41378 f was calculated using the central values for the period and the stellar mass provided in A. Vanderburg et al. 2016; while the radius of this ring system is not fully known, the predictions in B. Akinsanmi et al. 2020 indicate that this exoring radius would be likely be smaller than that of Saturn’s ring system.) However, large exoring systems are predicted to be rare on tighter orbits due to the gravitational influence of the star. While the contrasts to detect a exoring with the same area as Saturn’s rings on orbits outside of 1 au is out of reach for JWST, the contrast performance of future instrumentation is expected to reach this needed sensitivity when directly imaging the nearest-neighboring systems.
Paper: On the Detection of Exorings in Reflected Light with JWST NIRCam
Authors: Rachel Bowens-Rubin, Mary Anne Limbach, Sam Hopper, Klaus Subbotina Stephenson, Matson Garza, Leigh N. Fletcher, Matthew Hedman
Figure caption: The rings of Saturn and Uranus as imaged by JWST NIRCam. These images provide an empirical example in which the flux of the ring system is comparable to, or even exceeds, that of the planet when observed with NIRCam. The image of Saturn was created using data from JWST GTO 1247. (a) (GTO 1247: https://www.stsci.edu/jwst/science-execution/program-information?id=1247; image credit: NASA, ESA, CSA, Matthew Tiscareno (SETI Institute), Matthew Hedman (University of Idaho), Maryame El Moutamid (Cornell University), Mark Showalter (SETI Institute), Leigh Fletcher (University of Leicester), Heidi Hammel (AURA)). (b) The image of Uranus was created using data from JWST DD 2739. (DD 2739: https://www.stsci.edu/jwst-program-info/program/?program=2739; image credit: Joseph DePasquale (STScI); NASA, ESA, CSA, STScI).
Paper: On the Detection of Exorings in Reflected Light with JWST NIRCam
Authors: Rachel Bowens-Rubin, Mary Anne Limbach, Sam Hopper, Klaus Subbotina Stephenson, Matson Garza, Leigh N. Fletcher, Matthew Hedman
Figure caption: Ring size detectable with JWST. We used the results from the simulations of NIRCam coronagraphy F200W + MASK335R to estimate the smallest ring size detectable for Proxima Centauri and Tau Ceti in the fully reflective case (blue) and the case where the albedo matches that of Saturn’s rings at F200W (green). The estimate is shown to the edge of the SUB320 field of view (5″ radius). The dotted lines represent where the contrast was extrapolated linearly from the final three points of the PanCAKE simulation. While ring systems smaller than 2.8 the radius of Saturn’s rings are not likely to be detectable with JWST through reflected light direct imaging, large-ring systems (tens to thousands of times the size of Saturn’s rings) surrounding planets in nearby systems could be possible to detect using NIRCam coronagraphy.
Paper: On the Detection of Exorings in Reflected Light with JWST NIRCam
Authors: Rachel Bowens-Rubin, Mary Anne Limbach, Sam Hopper, Klaus Subbotina Stephenson, Matson Garza, Leigh N. Fletcher, Matthew Hedman
Figure caption: NIRCam coronagraphy simulations with MASK335R to determine the optimal filter. PanCAKE was used to simulate the contrast achievable with NIRCam coronagraphy. The contrast predictions for the narrow filters (N) are shown with solid lines, the medium filters (M) are shown in the solid-dot, the wide filters (W) are shown in the dashed–dotted, and the extra wide (W2) are shown in dotted. The values of the simulated contrast at 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 are listed in the legend. The filters are ranked in the order of least to most sensitive. The three filters yielding the best sensitivity for both targets were: F182M, F200W, and F210M.
Paper: On the Detection of Exorings in Reflected Light with JWST NIRCam
Authors: Rachel Bowens-Rubin, Mary Anne Limbach, Sam Hopper, Klaus Subbotina Stephenson, Matson Garza, Leigh N. Fletcher, Matthew Hedman
Figure caption: The albedo spectrum of Saturn’s B-ring across the visible and near-infrared. The measurement of the albedo of Saturn’s rings (green) is plotted alongside the wavelength ranges of the JWST NIRCam wideband filters. The filters unavailable for coronagraphy (F070W, F115W, F150W) are shown in dotted lines. The filters availble for coronagraphy (F200W, F277W, F356W and F444W) are plotted with the thick black lines and gray shading. Saturn’s rings show a reasonably high reflectivity at ≲2 μm but drop significantly at longer wavelengths.
Paper: On the Detection of Exorings in Reflected Light with JWST NIRCam
Authors: Rachel Bowens-Rubin, Mary Anne Limbach, Sam Hopper, Klaus Subbotina Stephenson, Matson Garza, Leigh N. Fletcher, Matthew Hedman
Figure caption: NIRCam Contrast Simulations To Determine the Optimal Mask. An example of the PanCAKE contrast simulations are shown for Proxima Centauri with the F200W filter. This example is consistent across both targets and other filters. MASK335R and MASK430R are the best performing masks in simulation.
Paper: A Semiempirical Estimate of Solar Extreme-ultraviolet Evolution from 10 Myr to 10 Gyr
Authors: Kevin France, Girish Duvvuri, Cynthia S. Froning, Alexander Brown, P. Christian Schneider, J. Sebastian Pineda, David Wilson, Allison Youngblood, Vladimir S. Airapetian, Kosuke Namekata, Yuta Notsu, Tristen Sextro
Figure caption: (Top) The 90–360 Å luminosities of each of the stars in our survey as a function of stellar age. Symbols are the same as in Figure 3, with the addition of direct EUV spectral observations from EUVE (integrated over the 90–360 Å bandpass following a correction for interstellar hydrogen and helium absorption; purple filled circles). The bottom plot shows the complete 90–911 Å EUV luminosities (described in Section 3.3). The G-star X-ray history from T. Penz et al. (2008) employed in the cosmic shoreline formulation (H. Lammer et al. 2009; K. J. Zahnle & D. C. Catling 2017) is shown overplotted as the solid green line (approximate uncertainty range shown as the shaded green region). We see that the EUV and X-ray luminosities are comparable for stars at ages ≲1 Gyr, after which the X-rays decline and the EUV luminosity dominates (see also G. W. King & P. J. Wheatley 2021).
Paper: A Semiempirical Estimate of Solar Extreme-ultraviolet Evolution from 10 Myr to 10 Gyr
Authors: Kevin France, Girish Duvvuri, Cynthia S. Froning, Alexander Brown, P. Christian Schneider, J. Sebastian Pineda, David Wilson, Allison Youngblood, Vladimir S. Airapetian, Kosuke Namekata, Yuta Notsu, Tristen Sextro
Figure caption: The fractional (90–360 Å) EUV activity level of solar analogs as a function of time. The data are comprised of pre-main-sequence solar analogs located in the Upper Scorpius star-forming region (orange triangles), the young Suns with available DEM-based synthetic spectra in the literature (dark magenta open squares), and EUV luminosities derived from the N v-based scaling relations developed by (K. France et al. 2018; open black circles). Uncertainties are defined as the rms scatter on the N v-to-EUV scaling relations (factor of ≈1.7) and modeled uncertainty on DEM calculations (≈ 30%–50%; G. M. Duvvuri et al. 2021). The best-fit piecewise evolution model (Equation (3)) is overplotted as the solid, dark cyan line, with best fitting parameters shown in the dark cyan legend text. The 7 Myr Upper Sco star Upper Sco 2MASS J16132929-2311075 (filled red circle) is an outlier; we discuss this star in the Appendix.
Paper: A Semiempirical Estimate of Solar Extreme-ultraviolet Evolution from 10 Myr to 10 Gyr
Authors: Kevin France, Girish Duvvuri, Cynthia S. Froning, Alexander Brown, P. Christian Schneider, J. Sebastian Pineda, David Wilson, Allison Youngblood, Vladimir S. Airapetian, Kosuke Namekata, Yuta Notsu, Tristen Sextro
Figure caption: Representative DEM-based synthetic EUV spectra and direct EUV observations (shown here from 60 to 912 Å) roughly spanning the age range presented in this work. In the top plot, the histogram shows the bolometric flux-normalized EUV spectra of DS Tuc A (∼40 Myr; red), κ1 Cet (∼650 Myr; orange), and the Sun at moderate activity levels (∼4.6 Gyr; gray). The DS Tuc and κ1 Cet synthetic spectra are developed using the formalism described in G. M. Duvvuri et al. (2021), and the solar data are from the Solar Dynamics Observatory-Extreme Ultraviolet Variability Experiment instrument (T. N. Woods et al. 2012). The bottom plot shows the absolute flux of the same spectra, as received at 1 au from the star.
Paper: A Semiempirical Estimate of Solar Extreme-ultraviolet Evolution from 10 Myr to 10 Gyr
Authors: Kevin France, Girish Duvvuri, Cynthia S. Froning, Alexander Brown, P. Christian Schneider, J. Sebastian Pineda, David Wilson, Allison Youngblood, Vladimir S. Airapetian, Kosuke Namekata, Yuta Notsu, Tristen Sextro
Figure caption: A comparison of two pre-main-sequence stars in Upper Sco, Upper Sco 2MASS J16132929-2311075 (age ∼7 Myr, M* ∼ 1.3M⊙; red histogram), and 2MASS J16081474-1908327 (age ∼6 Myr, M* ∼ 1.3M⊙; gray histogram). The “as observed” spectra are normalized by the bolometric fluxes of each star (M. J. Pecaut & E. E. Mamajek 2016); the exposure times are approximately equal for these two observations, but the differences in S/N are obvious. 2MASS J16132929-2311075 displays much larger relative hot gas fractions in N v (left panels; Tform ≈ 1–2 × 105 K) and Fe XXI (right panels; Tform ≈ 107 K). We speculate that 2MASS J16132929-2311075 was observed in the declining phase of a large stellar flare (Figure 8).
Paper: A Semiempirical Estimate of Solar Extreme-ultraviolet Evolution from 10 Myr to 10 Gyr
Authors: Kevin France, Girish Duvvuri, Cynthia S. Froning, Alexander Brown, P. Christian Schneider, J. Sebastian Pineda, David Wilson, Allison Youngblood, Vladimir S. Airapetian, Kosuke Namekata, Yuta Notsu, Tristen Sextro
Figure caption: The top plot shows the 90–360 Å EUV flux at 1 au from the central star. The dark gray curve shows the EUV flux evolution fit from I. Ribas et al. (2005). The 100 Myr–4.6 Gyr region over which I. Ribas et al. had empirical EUV data are encompassed by the shaded gray area. At the bottom, we show the same plot, normalized to the present-day solar value for intermediate activity conditions (F⊙(EUV) = 1.57 erg cm−2 s−1). The green curve shows the best fit to the normalized EUV flux, demonstrating that the relative EUV flux experienced within the habitable zone varies from approximately 100 × to 0.3 × over the Sun’s 10 Myr–10 Gyr lifetime.
Paper: A Semiempirical Estimate of Solar Extreme-ultraviolet Evolution from 10 Myr to 10 Gyr
Authors: Kevin France, Girish Duvvuri, Cynthia S. Froning, Alexander Brown, P. Christian Schneider, J. Sebastian Pineda, David Wilson, Allison Youngblood, Vladimir S. Airapetian, Kosuke Namekata, Yuta Notsu, Tristen Sextro
Figure caption: Emission-line lightcurves of 2MASS J16132929-2311075 in the N v and C II lines. The C II count rates have been divided by two for display. Both lines show a ∼30%–40% flux decrease across a single HST orbit, suggesting that this star was observed in the declining phase of a large stellar flare.
Paper: A Semiempirical Estimate of Solar Extreme-ultraviolet Evolution from 10 Myr to 10 Gyr
Authors: Kevin France, Girish Duvvuri, Cynthia S. Froning, Alexander Brown, P. Christian Schneider, J. Sebastian Pineda, David Wilson, Allison Youngblood, Vladimir S. Airapetian, Kosuke Namekata, Yuta Notsu, Tristen Sextro
Figure caption: Same as Figure 3 (fractional (90–360 Å) EUV activity level of solar analogs as a function of time), but including the comparable early M dwarf EUV activity evolution from J. S. Pineda et al. (2021). The integrated area in the M dwarf EUV history is a factor of ≈10 higher than the solar case.