adsabs/AstroCLIMB huggingface dataset:
Paper: MEGASIM: Lifetimes and Resonances of Earth Trojan Asteroids—The Death of Primordial ETAs?
Authors: Travis Yeager, Nathan Golovich
Figure caption: Panel (a) IAS15 (thick gray) and WHfast (thin black) simulation fraction of ETAs remaining over time. The IAS15 stops at 50 Myr and the WHfast simulation continues to 1 Gyr. Panel (b) is the absolute value of the difference between the two curves in panel (a). For reference, the initial population of ETAs in both simulations is 11.2 million.
Paper: MEGASIM: Lifetimes and Resonances of Earth Trojan Asteroids—The Death of Primordial ETAs?
Authors: Travis Yeager, Nathan Golovich
Figure caption: The initialization of the WHfast simulation with all 11.2 million initial ETAs shown as a heatmap. The Sun, Mercury, Venus, Earth, and Mars are represented as the orange, gray, green, blue, and red dots. The circles are provided for reference and do not represent the exact orbits of the planets.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: Reaction mechanism for the addition of ·OH onto c-C3H2. Highlighted connections indicate the most energetically likely formation route.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: Reaction mechanism for the addition of ·F onto c-C3H2. Highlighted connections indicate the most energetically likely formation route.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: Frontier MOs of intermediate I2a for the formation of c-C3HOH and c-C3HF.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: The three highest-occupied MOs of c-C3HNCO.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: The two highest-occupied MOs of c-C3HCN.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: The three highest-occupied MOs of c-C3HCHO.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: The three highest-occupied MOs of ·NCO.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: Frontier MOs of intermediate I2b for the formation of c-C3HOH and c-C3HF. For brevity, the lower-energy intermediate is taken for the c-C3H2(OH) structure.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: Reaction mechanism for the addition of ·NH2 onto c-C3H2. Highlighted connections indicate the most energetically likely formation route.
Paper: Response of Electric Field in Terrestrial Magnetosphere to Interplanetary Shock
Authors: Dianjun Zhang, Wenlong Liu, Junfeng Du, Yiqun Yu, Xinlin Li, Theodore E Sarris, Jinbin Cao
Figure caption: Comparison between simulated and theoretically estimated onset time, peak time, and rising time of electric field impulses. (a) and (b) Comparison between simulated onset time (red), peak time (orange) of electric field impulses, theoretically estimated fast-mode wave arrival time (blue), and compression-related flow arrival time (green) for L = 5 and L = 6 respectively. (c) and (d) Comparison between simulated (red) and theoretically estimated (blue) rising time for L = 5 and L = 6 respectively.
Paper: Response of Electric Field in Terrestrial Magnetosphere to Interplanetary Shock
Authors: Dianjun Zhang, Wenlong Liu, Junfeng Du, Yiqun Yu, Xinlin Li, Theodore E Sarris, Jinbin Cao
Figure caption: Overview of the IPS event on 2015 March 17. (a) Solar wind measurements by Wind spacecraft. (b) Orbital information of Van Allen Probes spacecraft. (c) Van Allen Probes observations and SWMF simulation results. From top to bottom, geomagnetic index SYM-H, observed magnetic field magnitude, simulated magnetic field magnitude, observed electric field y component, and simulated electric field y component are plotted.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption: Light curves of Las Cumbres Observatory 91T/99aa-like SNe in natural systems. Light-curve fits for ﹩{BVg}^{\prime} r^{\prime} i^{\prime} ﹩ bands using FPCA (He et al. 2018) are shown as dashed lines overlaid on top of their corresponding data points. For completeness, we also plot U and R photometry when available, though for those two filters, we did not correct for color terms. For SNe with data from non–Las Cumbres observing programs, they are included in the figure for comparison, with the sources of the data shown in the insert legends at the upper-right corner of each panel. The relevant references are Stahl 2019: Stahl et al. (2019), Foley 2018: Foley et al. (2018), and TNT: Tsinghua-NAOC Telescope.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption: Examples of K-correction calculation for SN 2016gcl (left) and SN 2019vrq (right). The red data points are the K-correction values measured from the mangled Hsiao template. The black line is the FPCA fit to the red data points. The shaded region is the error of the FPCA fit. And the black crosses are the adopted K-correction values derived from the fitted FPCA curve. By fitting a smooth curve to the measured K-correction, we cannot only get the error estimates but also the K-correction values of the epochs when colors to which the spectra need to be mangled to match are not available (one example is the purple diamond on the left panel).
Paper: Response of Electric Field in Terrestrial Magnetosphere to Interplanetary Shock
Authors: Dianjun Zhang, Wenlong Liu, Junfeng Du, Yiqun Yu, Xinlin Li, Theodore E Sarris, Jinbin Cao
Figure caption: Three different types of Ey temporal profiles in the magnetosphere. (a)–(c) Examples of three different types of Ey profiles in simulation results, and (d) spatial distribution of the three different types in the equatorial plane. Ey profiles are plotted in solid lines with positive for duskward direction. Ea profiles are plotted in dashed lines with positive for westward direction for comparison.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption: Observed ﹩{B}_{\max }-{V}_{\max }﹩ (MW extinction and K-corrected) vs. Δm 15(B). Extinction can only cause ﹩{B}_{\max }-{V}_{\max }﹩ to increase in value, thus the lower envelope (plotted as a black solid line) can be used as an extinction-free curve to correct for host extinction (Section 2.5). 91T/99aa-like data points are plotted in green squares, and historical 91T/99aa-like data points are plotted in purple diamonds. Normal SNe Ia are plotted in gray triangles.
Paper: LensingETC: A Tool to Optimize Multifilter Imaging Campaigns of Galaxy-scale Strong Lensing Systems
Authors: Anowar J. Shajib, Karl Glazebrook, Tania Barone, Geraint F. Lewis, Tucker Jones, Kim-Vy H. Tran, Elizabeth Buckley-Geer, Thomas E. Collett, Joshua Frieman, Colin Jacobs
Figure caption: Top row: HST legacy imaging of spiral galaxies from the Galaxy Zoo catalog. Bottom row: Reconstruction of the light distribution based on a basis set of shapelets (i.e., 2D Gauss–Hermite polynomial) with maximum polynomial order ﹩{n}_{\max }=50﹩. The shapelet-based reconstructions are rescaled to the same characteristic size.
Paper: LensingETC: A Tool to Optimize Multifilter Imaging Campaigns of Galaxy-scale Strong Lensing Systems
Authors: Anowar J. Shajib, Karl Glazebrook, Tania Barone, Geraint F. Lewis, Tucker Jones, Kim-Vy H. Tran, Elizabeth Buckley-Geer, Thomas E. Collett, Joshua Frieman, Colin Jacobs
Figure caption: Throughput of the F200LP (emerald line) and F140W (orange line) filters of the HST WFC3. The spectral energy distributions of a star-forming galaxy (blue line) at z = 2 and an elliptical galaxy (red line) at z = 0.5 are also illustrated with arbitrary amplitude scaling. Each of the two adopted filters maximizes the relative contribution from either the deflector or the source galaxy to the total light.
Paper: LensingETC: A Tool to Optimize Multifilter Imaging Campaigns of Galaxy-scale Strong Lensing Systems
Authors: Anowar J. Shajib, Karl Glazebrook, Tania Barone, Geraint F. Lewis, Tucker Jones, Kim-Vy H. Tran, Elizabeth Buckley-Geer, Thomas E. Collett, Joshua Frieman, Colin Jacobs
Figure caption: Distribution of photometric redshifts of the 699 spiral and disky galaxies selected from the Galaxy Zoo catalog.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar as Figure A11 but for Fe.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Variations of the lag between the averaged and shifted H fluxes at different energies (mentioned in between the subplots) and the averaged SSN with respect to the averaging window during SC23 (left) and SC24 (right) are shown. The fluxes are shifted based on the calculated lags with respect to the SSN variation. The green dots are the lags when there is no cutoff on the fluxes (as shown in Figure 4 in the main text). The red, black, pink, and blue dots represent Pearson’s CCs obtained in the similar way after putting cutoffs on the fluxes. The threshold values of the fluxes in units of particles/(cm2-s-sr-MeV/n) are written above each subplot.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: Products of cyclopropenylidene hydrogen-substitution with various radicals. Energetics of reaction are listed in Table 1. Table 2 lists their names and chemical formulae.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: Reaction mechanism for the addition of ·CN onto c-C3H2. Highlighted connections indicate the most energetically likely formation route.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar as Figure A7 but for 4He. Also, the legends are shown adjacent to the subplots.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar as Figure A8 but for 3He. Energy channels are mentioned inside the subplots.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar as Figure A10 but for O.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar as Figure A9 but for C.
Paper: A Generative Model for Quasar Spectra
Authors: Anna–Christina Eilers, David W. Hogg, Bernhard Schölkopf, Daniel Foreman-Mackey, Frederick B. Davies, Jan–Torge Schindler
Figure caption: Cross-validation of the GPLVM with Q = 16 latent dimensions. Predicted compared to measured black hole masses for all quasars in our data set, colored by the SNR of the single-epoch quasar spectrum. Note that we use only two labels for the quasars here (i.e., L = 2), namely black hole mass and bolometric luminosity.
Paper: A Generative Model for Quasar Spectra
Authors: Anna–Christina Eilers, David W. Hogg, Bernhard Schölkopf, Daniel Foreman-Mackey, Frederick B. Davies, Jan–Torge Schindler
Figure caption: Spectral dependencies on various quasar properties; that is, black hole mass (top), bolometric luminosity (middle), and redshift (bottom). The inset panel shows the expected spectral changes due to the Baldwin effect.
Paper: A Generative Model for Quasar Spectra
Authors: Anna–Christina Eilers, David W. Hogg, Bernhard Schölkopf, Daniel Foreman-Mackey, Frederick B. Davies, Jan–Torge Schindler
Figure caption: Predictions of missing spectral regions. In each panel, we use the spectral region indicated by the yellow-shaded regions to determine the latent representation of the new unseen quasar spectrum shown in black (see Section 3.1). The red curves show the predicted spectra derived from the set of latent parameters. As expected, the precision of the spectral prediction increases when a larger fraction of the spectrum is used to determine the latent parameters, whereas the prediction approaches the mean of the training-set spectra shown in gray if only a small fraction of the spectral coverage is provided as input.
Paper: A Generative Model for Quasar Spectra
Authors: Anna–Christina Eilers, David W. Hogg, Bernhard Schölkopf, Daniel Foreman-Mackey, Frederick B. Davies, Jan–Torge Schindler
Figure caption: Quasar spectra in our data set taken with COS/HST and STIS/HST. The light gray spectra show the original data, while the black curves show the input data re-binned to a common wavelength grid and after fitting a spline and sigma-clipping to remove absorption lines. The red-dashed curve shows the power-law fit to each spectrum, which is used to normalize all spectra to unity at approximately 2500 Å.
Paper: The Formation of Monosubstituted Cyclopropenylidene Derivatives in the Interstellar Medium via Neutral–Neutral Reaction Pathways
Authors: Athena R. Flint, Ryan C. Fortenberry
Figure caption: The SOMO of ·CN.
Paper: A Generative Model for Quasar Spectra
Authors: Anna–Christina Eilers, David W. Hogg, Bernhard Schölkopf, Daniel Foreman-Mackey, Frederick B. Davies, Jan–Torge Schindler
Figure caption: Back hole masses and bolometric luminosities colored by redshift of 31 quasars in our data sample, which have reliable black hole mass measurements based on the RM technique.
Paper: A Generative Model for Quasar Spectra
Authors: Anna–Christina Eilers, David W. Hogg, Bernhard Schölkopf, Daniel Foreman-Mackey, Frederick B. Davies, Jan–Torge Schindler
Figure caption: Visualization of the latent space. We show the locations of the quasars in five latent dimensions, which show the strongest gradient with black hole mass based on the Pearson correlation coefficient.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Chirp mass (left panels), mass ratio (middle panels), and dimensionless black hole spin (right panels) for the populations of MRR (orange) and non-MRR (blue) detectable binary black holes for all 560 model realizations. Three realizations, “K123”, “O312”, and “T231” (see Github) are highlighted with a dotted, dashed–dotted, and dotted curve, respectively. The bottom panels show probability distribution functions (PDFs), except for the black hole spins where we show cumulative distribution functions (CDFs) for visualization purposes. The two top rows show the fraction of expected detectable MRR (f_MRR) and non-MRR (f_nonMRR) binaries. The PDFs are normalized such that for each model realization the MRR and non-MRR PDFs sum up to one to show the relative normalization. https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure3_and_Figure5_BBH_properties_MRR_and_nonMRR_Distribution_plots/super_MRR_split_panel.pdf https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure3_and_Figure5_BBH_properties_MRR_and_nonMRR_Distribution_plots/Make_Figure_3_and_5_Distribution_Plots.ipynb.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Examples of a binary system in our fiducial model realization that undergoes MRR evolved at low metallicity (Z ≈ 0.001; top panel) and solar metallicity (Z ≈ 0.0142; bottom panel). Each panel shows the evolution of the initially more massive (m A) and less massive (m B) star as a function of time. Both systems undergo MRR during the first mass transfer episode after approximately 4 Myr into their evolution (as indicated by the gray vertical bar). Transitions to different evolutionary stages are labeled using the acronyms: HG for a Hertzsprung gap star, HeMS for a helium main-sequence star, HeHG for a helium HG star, and BH for a black hole. More examples are provided on GitHub. https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure1_individual_MRR_systems_detailed_evolution/detailedPlots/Figure_1_MRR.pdf https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure1_individual_MRR_systems_detailed_evolution/Individual_System_Evolution_and_MRR_Statistics.ipynb.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Fraction of MRRs among all binary black hole mergers (black) expected in the astrophysical (redshift 0; top panel) and gravitational-wave detectable (lower panel) populations for our 560 model realizations. The fraction of MRR binary black holes that go through the “classic common envelope” (blue), “only stable mass transfer ”(magenta), and “other” (gray) channels are shown (see Section 2.4). We connect models using the same star formation rate density ﹩{ \mathcal S }(Z,z)﹩ with a line for visual purposes only. The vast majority of binaries in the “other” channel in our simulations are systems that experienced a mass transfer phase initiated by a main-sequence donor (case A mass transfer). https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure2_MRR_Rates_For_All_Models/RelativeMRRrates_Combined.pdf https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure2_MRR_Rates_For_All_Models/MRR_Rates_Intrinsic_and_Detectable_summary.ipynb.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Fraction of the astrophysical (left panel) and detectable (right panel) binary black hole merger population where one of the black holes has a nonnegligible spin magnitude (χ i > 0.05) plotted against the percentage of systems in which the more massive (m 1) or less massive (m 2) black hole is spinning. Each marker style corresponds to one of our 20 stellar evolution variations for the combination with 28 cosmic star formation history models (see Github). Five stellar evolution variations are highlighted. Part of the 90% credible interval range of 0.25–0.71 for the fraction of binary black hole mergers with nonnegligible spin from Galaudage et al. (2021) is shown with a gray bar. https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure4_spinning_BBH_Rates/Rate_MRR_spins_panels_spin_threshold_0.05.pdf https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure4_spinning_BBH_Rates/Plot_fraction_spinning_BBHs.ipynb.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Fraction of binary black hole systems that match the inferred 90% credible contours that are MRR (vs. non-MRR) for the gravitational-wave events from GWTC-1, GWTC-2, and GWTC-3. Arrows indicate the observations that are discussed in the text. Three realizations, “K123”, “O312”, and “T231” (see Github) are highlighted with a cross, vertical line, and diamond marker, respectively. https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure6_GW_Ratio_MRR_vs_non_MRR/Rate_allGWs_MRR.pdf https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure6_GW_Ratio_MRR_vs_non_MRR/fraction_MRR_for_GW_CI.ipynb.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Total mass and mass ratio for MRR (left panel) and non-MRR (right panel) binary black holes in all our combined 560 model realizations. We draw from each model realization 100 binary black holes between the combined MRR and non-MRR populations and show these with a darker hue to visualize the density of points. The 90% credible contours for six gravitational-wave events that are discussed in the text are also shown. https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure_7_and_8_and_9_and_10_Discussion_2D_slices/Mtot_vs_q_all_models_all_pointsallNonMRR.png https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure_7_and_8_and_9_and_10_Discussion_2D_slices/Make_2D_scatter_Distributions.ipynb.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Chirp mass (left panels) and mass ratio (right panels) distributions split up in the subset of systems where the more massive black hole has nonnegligible spin (χ 1 > 0.05; MRR) vs. where the less massive black hole has nonnegligible spin (χ 2 > 0.05; non-MRR). The panels and labels are the same as in Figure 3, but a top panel is added showing the overall fraction of binary black holes with one spinning component (χ i > 0.05). https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure3_and_Figure5_BBH_properties_MRR_and_nonMRR_Distribution_plots/super_spins_split_2.pdf https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure3_and_Figure5_BBH_properties_MRR_and_nonMRR_Distribution_plots/Make_Figure_3_and_5_Distribution_Plots.ipynb.
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Same as Figure 7 but for the chirp mass and effective spin. https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure_7_and_8_and_9_and_10_Discussion_2D_slices/ChiEff_vs_q_all_models_all_pointsallNonMRR.png https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure_7_and_8_and_9_and_10_Discussion_2D_slices/Make_2D_scatter_Distributions.ipynb.