adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Authors: Adina D. Feinstein, Darryl Z. Seligman, Kevin France, Jonathan Gagné, Adam Kowalski
Figure caption: High-level summary of the demographics of flares in our sample. Top: the number of flares identified compared to the number of stars in each nearby young moving group, cluster, or association. A linear relationship is expected. Bottom: distribution of measured TESS energies and equivalent durations of flares in our sample, colored by the probability of the flare as identified with stella. ✎
Paper: Evolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Authors: Adina D. Feinstein, Darryl Z. Seligman, Kevin France, Jonathan Gagné, Adam Kowalski
Figure caption: Comparison fits between the Llamaradas Estelares single-peak model from Tovar Mendoza et al. (2022) and the double-peak flare model from Pietras et al. (2022) for flares with A ≥ 0.4. Top (A): comparison in the χ 2 between the best-fit model for 900 flares. A one-to-one line is plotted in peach to guide the eye. Across this sample of high-amplitude flares, there is good agreement between the fits for these two distinct models. Bottom: comparison in best-fit models for a subset of flares. The best-fit Llamaradas Estelares model is plotted in blue; the best-fit double-peak model is plotted in orange. We highlight examples where the double-peak flare model has the better fit (B), (C), the Llamaradas Estelares flare model has the better fit (D), (E), and where the models perform equally as well (F), (G). We note that there is no correlation between the flare amplitude and the preferred model. ✎
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Left column: average reduced χ 2 as a function of the number of Gaussian parameters (three per Gaussian component:  a   n ,  μ   n , and  σ   n ). The mean ﹩{\chi }_{r}^{2}﹩ as a function of the number of parameters in the IPS-GI field is shown by the gray line. The red dot represents the mean ﹩{\chi }_{r}^{2}﹩ at the N Gauss selected. Middle column: reduced χ 2 map of the total model built with Table 3 parameters, with the position of IPS-GI measurements overlaid in white. Right column: dispersion–velocity probability distribution function weighted by the fraction of total emission of each Gaussian component (as in Marchal et al. 2019, Figure 16).
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Left: Diffuse dust emission at 12 μm from WISE (background) compared with the thermal dust column density (the contours) and polarization (the black pseudo-vectors) at 353 GHz from Planck in the vicinity of fields C2 (top row), C16 (middle row), and C37 (bottom row) marked by the white rectangle in the center. Right: Comparison between the optical polarization (the white pseudo-vectors) and the thermal dust polarization at 353 GHz (the black pseudo-vectors). The orientation of the thermal dust polarization was rotated by 90° so that both Planck polarization and optical polarization pseudo-vectors indicate the orientation of the plane-of-sky magnetic field.
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: H I column density maps per intermediate-latitude IPS-GI field in units of 1021 cm−2. From left to right: ﹩{N}_{{\rm{H}}}^{\mathrm{GASS}}﹩ from H I emission observed with GASS, N H of the total model obtained with ROHSA, ﹩{N}_{{\rm{H}}}^{\mathrm{cnm}}﹩ from the CNM model, ﹩{N}_{{\rm{H}}}^{{\rm{lnm}}}﹩ from the LNM model, ﹩{N}_{{\rm{H}}}^{\mathrm{wnm}}﹩ from the WNM model, and the residuals between the observations (﹩{N}_{{\rm{H}}}^{\mathrm{GASS}}﹩) and the total model from ROHSA (N H). Be aware of the different color scale of the LNM model in field C16.
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Magnetic field strength calculated with the DCF (the circles), ST-DCF (the triangles), and ADF-DCF (the squares) methods as a function of the effective thickness, colored by the total volume density. The red and orange horizontal dashed lines represent our B pos results calculated with ADF-DCF and ST-DCF, respectively. The vertical black dashed–dotted line shows the effective thickness of the cloud obtained with the values of Table 1.
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Magnetic field strength maps in field C2 (left), C16 (middle), and C37 (right). The white pseudo-vectors represent the IPS-GI starlight polarization.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: GLS periodograms of the RV data of TOI-1450 with various signals subtracted. Each panel has a note describing which signals have been subtracted from the data to produce the residual periodogram. The bottom panel shows the window function. A red dashed line corresponding to a FAP of 0.1% is shown on each plot. In addition, vertical dotted lines corresponding to the periods of the fit planets are also included. The red line is the 2.04 days signal, the gold is the ≈3 days signal, the green is the ≈5 days signal, the gray is the ≈15 days signal, and the purple is the 20 days signal.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: A ℓ 1 periodogram of the TOI-1450 RV data. Vertical dotted lines correspond to various periods. The red line is a 2.044 days signal, the gold a 3.44 days signal, the green a 5.06 days signal, the gray a 14.9 days signal, and the purple a 20.1 days signal. The horizontal dashed line corresponds to a 1% FAP.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: Top: the offset-subtracted RV data for TOI-1450A. The MAROON-X red and blue channels are colored accordingly. Middle: the RV data with both the offsets and best-fit GPs subtracted. The best-fitting two-planet Keplerian model is shown in gray. Bottom: the data residuals (subtracting out the offsets, GPs, and best-fit Keplerians).
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: The phase-folded RVs for TOI-1450A b and TOI-1450A c. The offsets, activity, and other planets are subtracted out in each panel to focus on the relevant signal. The MAROON-X red and blue channels are colored accordingly, and binned data are shown in black. The best-fit model is shown in gray.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: GLS periodograms of the signals present in the MAROON-X activity indicators, with outliers due to flares removed and the dLW data normalized to the mean within each run. The dashed gold line indicates the location of a 39 days period. A red dashed line corresponding to a false-alarm probability (FAP) of 1% is also shown.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: Lomb–Scargle periodograms of the ASAS-SN photometry. The red dashed horizontal line corresponds to a 1% false-alarm probability (FAP), and the golden vertical line indicates a 43 days period.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: GLS periodograms of the WASP data. The red dashed horizontal line corresponds to a 1% false-alarm probability (FAP), and the golden vertical span indicates periods from 40 to 47 days. The signal at 1 day is likely related to the nightly sampling and is thus unlikely to be physical.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: The phase-folded transit data for TOI-1450A b, with our best-fit model shown in red. Binned data are shown as black points. Each panel highlights a different data set.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: Time series of the MAROON-X activity indicators.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: Ternary diagram of the composition of TOI-1450A b generated using ManipulatePlanet (Zeng & Sasselov 2013; Zeng et al. 2016). The solid black line indicates the planet composition for a variety of different central pressure values, while the dotted black lines indicate the range of values given the mass and radius errors.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: The mass and radius of TOI-1450Ab (black star) compared to both interior composition models from Zeng et al. (2019; colored dashed lines) and other exoplanets with mass and radius errors <20% from TEPCat (gray points). Earth and Venus are also included for reference.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: The measured equivalent width of the metastable helium line as a function of age for Neptunes (4 ≤ R ⊕ ≤ 6) around K stars (triangles) and M stars (diamonds), and sub-Neptunes (R ⊕ <  4) around K stars (circles) and around G and M stars (squares). The upper limits from our sample are shown for K2-100b (green), V1298 Tau c (orange), and HD 63433b (purple). The He equivalent width for HD 63433b from Zhang et al. (2022) is shown in the open purple square. We also show predicted trends between helium absorption and age from hydrodynamic models (Allan et al. 2024) for 2% (solid black line) and 10% (dashed black line) He abundance. These models are calibrated for a 0.1 M Jup planet orbiting a K-type star at 0.045 au (details in text). Literature helium values are taken from Allart et al. (2018), Gaidos et al. (2023), Kasper et al. (2020), Krishnamurthy et al. (2021), Nortmann et al. (2018), Orell-Miquel et al. (2022, 2023), and Zhang et al. (2021, 2022a, 2023).
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Helium triplet excess absorption predictions (left) and their corresponding mid-transit extinction maps (right), obtained with the model of Allan et al. (2024) as described in Section 4.3. For the excess absorption profiles, solid lines indicate mean phase-averaged (T1–T4) profiles while the shaded region encompasses all phases between first contact and mid-transit. For the extinction maps, the dashed circle marks the stellar disk. The displayed extinction is the sum of the three individual extinctions of each of the triplet lines. A helium to hydrogen number fraction of He/H = 0.1 was assumed for each planet, with He/H = 0.02 also being tested in the case of V1298 Tau c as shown by the gray dashed profile. Additional planetary and stellar parameters listed in Table 1 were used.
Paper:  NotPlaNET: Removing False Positives from Planet Hunters TESS with Machine Learning
Authors: Valentina Tardugno Poleo, Nora Eisner, David W. Hogg
Figure caption: Fraction of planet candidates (top) and true contaminants (bottom) flagged as contaminants as a function of the PC score threshold for the seven validation sectors. For each validation sector, we chose a threshold that maximized the fraction of discarded contaminants while discarding zero planets. We then chose our final threshold (dashed line) by performing a weighted average of each validation sector’s threshold. The weights were assigned as the inverse square of the number of contaminants found in a given sector, allowing for a more conservative cutoff.
Paper:  NotPlaNET: Removing False Positives from Planet Hunters TESS with Machine Learning
Authors: Valentina Tardugno Poleo, Nora Eisner, David W. Hogg
Figure caption: Selected light curve chunks from sector 50. The rightmost column (purple) contains the light curves flagged as contaminants by our model. The leftmost and middle columns (green) contain light curves classified as “keep for further vetting.” The left column shows true planet candidates, while the middle one shows true contaminants that were incorrectly classified as “keep for further vetting.” The y-axis range is displayed in the lower-left corner of each panel, while the lower-right corner displays the TIC ID of the light curve.
Paper:  NotPlaNET: Removing False Positives from Planet Hunters TESS with Machine Learning
Authors: Valentina Tardugno Poleo, Nora Eisner, David W. Hogg
Figure caption: Convolutional block diagram. The block consists of two 1D convolutional layers with the ReLU activation function, layer normalization, and max pooling.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Posterior distributions of retrieved parameters from our 1D p-winds models.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Same as Figure 10, but for V1298 Tau c.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Same as Figure 10, but for HD 63433b.
Paper: Resonant and Ultra-short-period Planet Systems Are at Opposite Ends of the Exoplanet Age Distribution
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Jacob H. Hamer
Figure caption: Model for the self-consistent tidal evolution of a typical USP planet system. We plot as colored lines the semimajor axis (top left), eccentricity (bottom left), stellar rotation period (top right), and difference in stellar obliquity from the initial value of 20° (bottom right) as functions of time in years. Our model uses the system of ODEs presented in Leconte et al. (2010) that solves the coupled tidal evolution of the rotation and revolution of both a planet and its host star. We account for the rotational evolution of the host star due to stellar evolution and winds using a solar-composition, median-rotation M * = 1 M ⊙ stellar model from the rotational stellar evolution grid presented in Amard et al. (2019). We model the median USP planet with R p  =  1.2 R ⊕, 2.0 M ⊕, and ﹩{Q}_{{\rm{p}}}^{\prime} ={10}^{2}﹩. We plot in blue the solution with an assumed stellar tidal quality factor ﹩{Q}_{* }^{\prime} ={10}^{7}﹩ as appropriate for solar-type main-sequence stars (Barker 2020) and a nonzero but unobservable excited eccentricity e = 0.005. Given these parameters, the rotation and revolution of the planet are quickly synchronized and the planetary obliquity is quickly damped (e.g., Leconte et al. 2010). To evaluate whether tidal dissipation in the star could reproduce our observational result, we plot as dark and light green lines models calculated using the same ODE system, but with no eccentricity excitation and smaller ﹩{Q}_{* }^{\prime} ={10}^{6}﹩ (light green) and ﹩{Q}_{* }^{\prime} ={10}^{5}﹩ (dark green). This model corroborates our observational evidence that it takes billions of years and trillions of orbits for a rocky planet to tidally migrate and become a USP planet as a consequence of tidal dissipation inside the planet.
Paper: Resonant and Ultra-short-period Planet Systems Are at Opposite Ends of the Exoplanet Age Distribution
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Jacob H. Hamer
Figure caption: Stellar velocity dispersion as a function of age for the Kepler field. For the sample of subgiants in the Kepler field with ages presented in Xiang & Rix (2022), we first order the sample in age. We then calculate velocity dispersion in consecutive windows of 750 stars and plot the result of these calculations as overlapping dark gray points. We plot as the solid black line a smoothing spline of these data. We plot as the gray polygon the 16th/84th quantile range of the velocity dispersion distribution suggested by bootstrap resampling. We plot as horizontal lines the velocity dispersions of the Hamer & Schlaufman (2024) samples of Kepler-discovered plausibly first- and second-order mean-motion resonant systems as well as the subsample of plausibly first-order resonant systems with an innermost planet affected by tidal dissipation. For comparison, we plot as the light blue horizontal line the velocity dispersion of the complete Hamer & Schlaufman (2024) sample of Kepler-discovered multiple-planet systems. The sample of second-order resonant systems and the subsample of first-order resonant systems with an innermost planet affected by tidal dissipation have characteristic mean ages τ ≲ 2 Gyr. On the other hand, the overall sample of first-order resonant systems has a similar velocity dispersion and therefore age as the complete sample of Kepler-discovered multiple-planet systems. Combined with the Hamer & Schlaufman (2024) observation that the characteristic mean ages of these resonant populations are older than 500 Myr, the implication is that many multiple-planet systems form in mean-motion resonances and diffuse away from resonance over about 1 Gyr.