adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Planet radius limits for a planet of mass = 0.98 MJ, i.e., the latest mass estimate for ϵ Eridani b (W. Thompson et al. 2025). These curves are computed with E. F. Linder et al. (2019) models and the contrast numbers reported in Figure 4. We use the range of temperatures expected for a Jupiter-like planet in the range of ϵ Eridani’s age.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: The radial MAD values of the individual target-SGD PSF pair subtractions for the epoch 2 subarray observations (shown in Figure 7), used as weights for the final image combination produced for the postprocessing optimized for extended emission. The SGD position #5 subtraction for Obs #52 is highlighted, being a remarkably well aligned pair resulting in minimal residuals.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Contrast curves for the two epochs of observations of δ Eridani, the reference star for PSF subtraction. To obtain these, we used the ϵ Eridani images as PSF references. The sensitivity difference with respect to ϵ Eridani are due to the lack of two rolls and magnitude difference.
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 STIS and IUE FUV spectra of V659 Cen are compared. For the spectrum obtained with the STIS G140L + F25NDQ1, the flux both with and without the correction implied by the earlier standard star spectrum obtained with that filter/grating combination are shown. The flux of 52X0.05 spectrum has been multiplied by 3. For the F25NDQ1 spectrum the 5.5 pixel shift needed to align with the 52X0.05 spectrum is included.
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 flat-fielded image of the G140L spectrum of V659 Cen taken in the 52X0.05 aperture. The green lines show the upper and lower limits of the extraction region used for the 1D spectroscopic extraction. The yellow lines show the location the extraction region would have if it were instead centered on the Cepheid, but there is no evidence of a second star in this image. The most prominent spectral features include multiplets of C III at 1175 Å, (column 95), Lyα (1215 Å, centered near column 165), Si II 1260, 1265, 1304, and 1309 Å, (columns 241, 249, 316, 325), and C II 1335 Å (column 329).
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 second image of V659 Cen that was taken as part of the target acquisition exposure OE2E10PYQ. The Cepheid and spectroscopic binary companion is the brighter upper star; the resolved companion is the lower star. We superimpose a vertical line in green showing our best estimate of the alignment of the 52X0.05 slit during the subsequent spectroscopic exposure.
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 2D flat-field image of the G140L exposure taken with the F25NDQ1 filter. Conventions are the same as in Figure 2. The sharp feature seen near pixel 50 corresponds to the C III multiplet near 1335.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Similar to Figure 5 but for Ca II H blended with Hϵ, Ca II K, and He I 4472 Å instead. The gray background points are the quiescent spectrum, while the foreground-colored points represent the quiescent-subtracted flare-excess emission for the aforementioned lines in each row and at different points in time in each column. Each time column is titled with a position relative to the Hα light curve and the time after the start of the observation period in minutes.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Similar to Figures 5 and 6 for a collection of doublets: N V 1238/42 Å (light blue, topmost row), C II 1134/5 Å (teal, second row), Si IV 1394 Å (dark blue, third row), and Si IV 1403 Å + O IV 1401 Å (purple, fourth row) plotted separately, and C IV 1548/50 Å (green, bottom). The times plotted in each column are single-minute pseudoexposures for minutes 47, 48, 49, 50, 52, 55, and 72 from left to right. The faint gray spectra in the background are the quiescent emission, while the solid step plots in the foreground are the flare-excess spectra after subtracting off the quiescent emission. The flare evolves much more rapidly in the FUV than the optical, with a rise phase that lasts less than 2 minutes from quiescence to peak and the decay is slightly slower but still faster than the optical. The spectra at minute 72 still show a slight flare excess comparable to the original quiescent emission.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: A closer look at the midrise timestamp for Hα (left), Hβ (middle), and Hγ (right) similar to the second column of Figure 5. The gray line in the background of each panel is the quiescent emission line normalized to more easily compare the velocity profiles between the lines. The solid step plots with error bars are the quiescent-subtracted emission from each panel’s corresponding emission line during the rise phase of the flare. The excess Hα emission shows a well-defined narrow component redward of the quiescent emission with a more amorphous and smaller amplitude blue wing. The excess Hβ emission shows both blue and red wing components of comparable magnitude, although the blue wing is slightly more prominent. Finally, the Hγ excess has both blue and red wing components but the blue wing is clearly larger. Another point to note is that the fluxes of the excess Hβ and Hγ are comparable to the excess Hα and to each other, unlike the standard pattern of fluxes decreasing with higher Balmer order present during quiescence.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Similar to Figures 5 and 6, but for the Fraunhofer D lines Na I D1 5895, Na I D2 5890, and He I 5876 Å instead. Because the quiescent emission is in fact a large absorption feature from the Na I doublet, and the three lines are closely spaced, this figure plots the quiescent-subtracted flare-excess flux density against wavelength. Each panel plots vertical lines corresponding to the vacuum wavelengths of each D line, colored cyan, magenta, and maroon for lines D1, D2, and D3, respectively. The points in the spectrum within 200 km s–1 of each D line are colored according to the same pattern.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Light curves of Balmer line flare-excess fluxes on the left, and the flare-excess Balmer decrement (ratio relative to Hβ) on the right. After subtracting off the quiescent emission, the flare-excess fluxes of all the Balmer series peak at similar values, a significant departure from the ratios of the quiescent emission lines, but the decay of each Balmer line is steeper from Hα to Hδ. The Balmer decrements of the quiescent lines are plotted as horizontal gray lines in the right panels and the flare peak decrement is much lower (almost 1 instead of the quiescence’s 4) for Hα and higher for Hγ and Hδ. The Hα flare-excess decrement appears to increase linearly toward the quiescent value while the higher order decrements show a more exponential decay toward their quiescent values. There are error bars on these plots but they are miniscule; the values of the largest error bars are 8.5 × 10−16 erg cm−2 s−1 for the flux panel on the left and 0.12 for the decrement panel on the right.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: The top two panels show the light curves of integrated flux for Hα (brown, top row) and Hγ (red, second row) from the APO spectra, while the bottom three panels plot Lyα (dark blue, third row), Si III 1206 Å (pink, fourth row), and C IV 1548/50 Å (green, bottom row) from the HST spectra. The top of each panel includes the peak time on the left, at 54.7 minutes for the optical and 49 minutes for the FUV, the ratio of peak flux measurement to the initial (varying from 1.3 to 171.3 depending on the line) in the middle, and the ratio of the final flux measurement to the initial on the right (varying from 1.1 to 15.7). Each panel has an independent y-scale because of the dynamic range of peak fluxes depending on the line. Note that the FUV lines peak and decay almost entirely within the rise phase of the optical lines, both optical and FUV lines show both a primary and secondary bump, the secondary bump of the optical takes place while Hubble is unable to observe, and the secondary bumps of the FUV happen during the optical peaks.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Similar to Figure 10 and the rightmost column of Figure 5, this figure is a closer look at a timestamp during the decay phase for Hα (left), Hβ (middle left), Hγ (middle right), and Hδ (right). The gray line in the background of each panel is the (normalized for legibility) quiescent emission line and the solid step plots with error bars are the quiescent-subtracted emission from each panel’s corresponding emission line during the decay phase of the flare. The Hα flare-excess emission is slightly redshifted relative to the quiescent line, while Hβ and Hγ are slightly blueshifted relative to quiescence (pixel widths of 27, 38, 43, and 46 km s−1 for Hα–Hδ respectively). The line profile is dominated by the line-spread function in the line core, but extended wings are still present for at least Hα and Hβ.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Similar to Figure 8 for C III 1175 Å (bluish gray, top row), Si III 1206 Å and Lyα (pink, second row), a blend of Si I – Si III + O I from 1301 to 1310 Å (brown, third row), and He II 1640 Å (teal, bottom row). The evolution of these FUV lines is similarly rapid, but the bottom two panels also highlight a number of flare-brightened lines that are only visible during flare peak.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: Orbit fitting with orvara assuming flat (uniform) companion mass priors. (Left) Predicted orbits with the most likely orbit in black along with 100 randomly selected orbits (color coded by mass) from the MCMC posterior distribution. Blue circles show our data, while empty circles show predicted location per epoch. (Center) Position angle vs. epoch and (right) separation vs. epoch for the selected orbits.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: HIP 99770 b SCExAO/CHARIS detections in the H and K bands on 2023 July 8 and 2023 June 6, respectively. The detected companion is circled, and the centroid of the star is marked by a yellow star.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: Corner plot showing MCMC posterior distributions for the flat prior. Fit using absolute astrometry from HGCA, relative astrometry (from both initial discovery and follow-up), and RV measurements from KPIC courtesy of Y. Zhang et al. (2024). The contours show the 68%  (1σ), 95%  (2σ), and 99%  (3σ) confidence intervals.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: Corner plot showing MCMC posterior distributions for the log-uniform prior. Fit using absolute astrometry from HGCA, relative astrometry (from both initial discovery and follow-up), and RV measurements from KPIC courtesy of Y. Zhang et al. (2024). The contours show the 68%  (1σ), 95%  (2σ), and 99%  (3σ) confidence intervols.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: HIP 99770 b H-band spectra in red from 2023 July 8 and K-band spectra in orange from 2023 June 6 plotted on top of the low-resolution spectra from the original discovery in black from 2021 October 17 and published in T. Currie et al. (2023b).
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: H–R diagr,ams for the binary systems HD 130669, HD 184467, HD 191854, and HD 214222. The positions of the individual stellar components (A and B) are plotted with their respective uncertainties. Evolutionary tracks corresponding to different stellar masses are shown by black lines, while the system’s best-fitting isochrone (age) is indicated by a red dotted line. The zero-age main sequence (ZAMS) is depicted as a thick solid black line. These diagrams were constructed using the evolutionary models to determine the masses and ages of the components based on their effective temperatures and luminosities.
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: Synthetic SED of the binary system HD 191854 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V), with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range (3500–18000 Å).
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: Synthetic SED of the binary system HD 130669 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V), with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range (3500–18000 Å).
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: Synthetic SED of the binary system HD 184467 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V), with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range (3500–18000 Å).
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: Synthetic SED of the binary system HD 21422 constructed using Al-Wardat’s complex method and Kurucz’s ATLAS9 model atmospheres. The total flux (black), flux of component A (blue), and flux of component B (orange) are shown. Overplotted are observed photometric fluxes from 2MASS (J, H), Gaia (BP, RP), and Johnson photometry (B, V), with their respective magnitudes. This comparison validates the consistency between the synthetic model and observed data across a wide wavelength range (3500–18000 Å).
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 N v data from HST-COS (top) and STIS (middle and bottom) roughly spanning the age range presented in this work. From top to bottom, the histogram shows the bolometric flux-normalized N v spectra (tracing transition region formation temperatures ≈1–2 × 105 K) of DS Tuc A (∼40 Myr; red), κ1 Cet (∼650 Myr; orange), and α Cen A (∼5.3 Gyr; gray). The spectra have been velocity-shifted to place N v at its rest wavelength (noted with dashed vertical lines) for comparison, and weak coronal Fe XII is noted with a blue label in κ1 Cet and α Cen A.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The fraction of Earth and Mars mass accreted from beyond the orbital radius r*, as a function of r*. We collected all simulations in model203 (r1 = 0.6 au and r2 = 1.7 au, the 2:1 mass split between the inner and outer sources, no background, strong convergent migration) that produced good matches to the terrestrial planet system (i.e., four good planets as defined in Section 3.1). We then followed the accretion sequence for Earth and Mars and collected all planetesimals that accreted into Earth and Mars, respectively. This accounts for all accretion events, including planetesimals accreting into intermediate-mass protoplanets that then merged into the identified Earth/Mars analogs. The cumulative distribution Earth’s and Mars’ fractional mass budgets, f(r > r*), is plotted here. The black dots represent the results of individual simulations. The red line shows the average. On average, the Earth accreted ≃30% of its mass from the outer reservoir.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: Panel (A): the last giant impact on the Earth in our reference model (model203). We collected all successful simulations and determined the last giant impact on the proto-Earth (as defined in the main text). The triangles show the time of the last giant impact, tgiant, and the impactor-to-target mass ratio, Γ. Panel (B): the mass accreted by the Earth after the last giant impact (a.k.a. late accretion). The gray band shows the HSE-inferred late accretion, 0.25%–1% MEarth, inferred from cosmochemical constraints (A. Morbidelli & B. J. Wood 2015).
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: Earth’s growth in the successful simulations from model213 (panel (A), weaker migration with Σ0 = 1500 g cm−2) and model214 (panel (B), stronger migration with Σ0 = 6000 g cm−2). We collected all successful simulations that produced good analogs to the terrestrial planet system (four planets with good orbits and masses; Section 3.1). In addition, we only used those simulations in which the final mass of the Earth analog was within 10% to the real Earth mass. The accretion sequence of these very good Earth analogs was recalibrated such that the model Earth ended up exactly with 1 MEarth. The vertical dashed line marks the end of the gas disk stage.