adsabs/AstroCLIMB huggingface dataset:
Paper: Constraints on the Spindown of Fully Convective M Dwarfs Using Wide Field Binaries
Authors: Emily K. Pass, David Charbonneau, Jonathan M. Irwin, Jennifer G. Winters
Figure caption: Observed and theoretical K-band magnitudes for the blended light from three Praesepe eclipsing binaries. The dashed line indicates unity. We consider the MLRs of Benedict et al. (2016) and Kraus & Hillenbrand (2007), finding good agreement between Benedict et al. (2016) and observations from 2MASS. The Kraus & Hillenbrand (2007) relation predicts the systems would be brighter than observed by roughly 0.5 mag. For the Benedict et al. (2016) points, we propagate uncertainties in mass, parallax, and 2MASS magnitude, and add in quadrature the reported 0.09 mag rms in the Benedict et al. (2016) MLR.
Paper: Constraints on the Spindown of Fully Convective M Dwarfs Using Wide Field Binaries
Authors: Emily K. Pass, David Charbonneau, Jonathan M. Irwin, Jennifer G. Winters
Figure caption: Comparison between the masses published in Douglas et al. (2017) for presumed single Praesepe M dwarfs using the Kraus & Hillenbrand (2007) MLR and masses we estimate using the Benedict et al. (2016) MLR. The dashed line indicates unity. The outliers are the result of inaccurate distances for a few of the Douglas et al. (2017) estimates, as they adopted the cluster distance for targets where a Hipparcos parallax was unavailable. Our estimates benefit from precise Gaia parallaxes.
Paper: Constraints on the Spindown of Fully Convective M Dwarfs Using Wide Field Binaries
Authors: Emily K. Pass, David Charbonneau, Jonathan M. Irwin, Jennifer G. Winters
Figure caption: Age posteriors for wide, FGK primaries to active, low-mass M dwarfs, based on isochrones and gyrochronology from stardate, lithium abundance aging from BAFFLES, and moving group membership from BANYAN Σ. Six of the 10 stars have posteriors that are consistent with young ( ≤600 Myr) ages, similar to the ages probed by studies of M dwarfs in clusters. Four (GJ 166 A, HD 75302, HD 217142, and HD 183870) are consistent with ages older than 1 Gyr.
Paper: Constraints on the Spindown of Fully Convective M Dwarfs Using Wide Field Binaries
Authors: Emily K. Pass, David Charbonneau, Jonathan M. Irwin, Jennifer G. Winters
Figure caption: Rotation rate evolution of a 0.3 M ⊙ main-sequence star with varying initial rotation rates (defined as the rotation in the immediate post-disk phase), calculated using the model of Garraffo et al. (2018) that considers changing magnetic complexity during spindown.
Paper: Constraints on the Spindown of Fully Convective M Dwarfs Using Wide Field Binaries
Authors: Emily K. Pass, David Charbonneau, Jonathan M. Irwin, Jennifer G. Winters
Figure caption: Rotational modulation of G 232-62, observed in two filters with the Zwicky Transient Facility (ZTF; Masci et al. 2019). In the top panel, we show the photometry publicly available through ZTF DR9. In the bottom panel, we phase the data to a 59 day period. Each year is presented separately for clarity, as the spot pattern evolves over the 4 yr of data.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: BAL outflow velocity as a function of the Eddington ratio for the sample of low-redshift FeLoBALQs. Top: The sample shows the V ∝ L bol/L Edd upper-limit envelope behavior commonly found in BALQs (Laor & Brandt 2002; Ganguly et al. 2007); see text for details. The scatter below the envelope can be characterized by parameter V ledd=1, the velocity any object would have if L bol/L Edd = 1 (see text for details). Bottom left: An anticorrelation between the force multiplier and V ledd=1 indicates that the scatter in the E1 < 0 objects may be caused by the scatter in FM. Bottom right: A correlation of R/R  S  with V ledd=1 suggests that the scatter in the E1 > 0 objects may be caused by the scatter in R/R  S .
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Volume filling factor (﹩\mathrm{log}{\rm{\Delta }}R/R﹩) as a function of the ionization parameter (logU) and the location of the outflow (logR). We found a wide range of ﹩\mathrm{log}{\rm{\Delta }}R/R﹩, with the overlapping trough and loitering BALs having higher values of ﹩\mathrm{log}{\rm{\Delta }}R/R﹩. Left panel: ﹩\mathrm{log}{\rm{\Delta }}R/R﹩ increases with logU following the slope of ∼1.5. This tight correlation is expected given the relationship between logU and ﹩\mathrm{log}{N}_{H}﹩ for FeLoBALs (Section 5.3, Choi et al. 2022). One of the main sources of the scatter along the ﹩\mathrm{log}{\rm{\Delta }}R/R﹩ can be ascribed to the range of ﹩\mathrm{log}n﹩ observed in the sample. Right panel: We found a wider range of ﹩\mathrm{log}{\rm{\Delta }}R/R﹩ distribution for the FeLoBALs that are located close to the central black holes. The green (dashed) and blue (dotted–dashed) diagonal lines represent the locations of the constant physical thickness of the BAL winds at ﹩\mathrm{log}{\rm{\Delta }}R=-5﹩ and 0 [pc], respectively. The error bars show 2σ uncertainties, and the gray shaded bars represent the range of the values among the tophat model bins for each BAL.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Comparison of the BAL velocity offset with the [O III] properties. Note that negative BAL velocities denote outflows. In the left and middle panels, the squares show the column-density weighted velocity, while the left and right triangles show the maximum and minimum speeds, respectively. The size of the square scales with the log of the [O III] equivalent width. Left: There is a correlation between the [O III] velocity offset and the BAL velocity offset (p = 1.9 × 10−4). Middle: There is an anticorrelation between the [O III] velocity width and the BAL velocity offset (p = 2.7 × 10−4). Right: The covering fraction correction factor is anticorrelated with the BAL velocity offset for our sample (p = 7.8 × 10−3) but possibly also for the Xu et al. (2020) sample. Larger velocity offsets may produce line emission that is distributed over a range of wavelengths where it may be blended with the continuum or hidden under strong Fe II emission.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Relationship between the number of clouds required to occult the 2800 Å continuum emission region and the location of the outflow normalized by the dust sublimation radius. The size of the points is scaled with the angle subtended by the continuum emission region as viewed from the location of the outflow. Compact outflows (those with ﹩\mathrm{log}R/{R}_{{\rm{D}}}\lt 2﹩) are segregated by the E1 parameter, with E1 < 0 objects having macroscopic clouds and E1 > 0 objects requiring 100–1000 s of cloudlets to cover the source.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Inferred [O III] luminosity from the SimBAL models as a function of the observed [O III] luminosity. The several objects with more than one outflow component are plotted more than once. The marker color denotes the corresponding E1 parameter and the size of the marker corresponds to the location logR parameter. Left: The predicted values are generally larger than the observed values, potentially implying a smaller emission-line-gas covering fraction than the assumed 10%. Right: The same as the left plot, with the covering fraction correction determined by the regression analysis (see text). The data were plotted using regression results for each of the 48 combinations.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Comparison of the [O III]λ5008 emission profile with the absorption profile for objects with compact outflows (﹩\mathrm{log}R\lt 1﹩ [pc]) and low log covering fraction correction factors (<0.5). Top panel in each frame: [O III]λ5008 profile from the normalized and continuum-subtraction spectrum. Bottom panel in each frame: SimBAL-derived opacity profiles for ground-state Mg II, ground-state Fe II λ2883, and excited-state Fe II λ2757 taken from Figure 13 of Choi et al. 2022.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Covering fraction corrections inferred from the regression analysis necessary to reconcile the observed [O III] emission with that predicted to be emitted by the absorption-line gas. The assumed emission-line covering fraction was 0.1, so a log covering fraction correction value of 1 would imply that a covering fraction of 0.01 would be needed to reconcile the values. The point color represents E1, and the point size represents logR. Left: The multiparameter regression is a function of the E1 parameter and logR and is therefore most accurately represented in 3D. The bow-tie surface shows the inferred errors from the mlinmix_err procedure; the results from all 48 combinations have been plotted. Middle: The results projected onto the E1 parameter plane. Right: The results projected onto the logR plane.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: XMM-Newton EPIC-PN contours (white) overplotted on Chandra-b (left) and the Hubble Space Telescope (center) observation of NGC 7479. The right panel shows the NuSTAR-1 observation. In the figure, the other X-ray sources in the galaxy are also highlighted: the ultraluminous X-ray source (ULX; cyan), the star-forming region (SFR) (orange), the supernova SN 2009jf (yellow), the supernova remnant of SN 1990u (red), and the central engine (magenta). The regions showed in the figure are for display only and do not correspond to the ones used for the spectral extraction.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Comparison between C2N (left) and OTFMAP (right) observations of NGC 1068 at 89 μm. First row: Herschel observations at 70 μm (color scale) of NGC 1068 within an FOV of 500 × 500 arcsec2 with overlaid C2N (left) and OTFMAP (right) configurations. For C2N, on-axis (white) and off-axis (yellow) positions with the FOV of HAWC+ at 89 μm are shown. For OTFMAP, the Lissajous curve (white solid line) of one scan is shown. Second row: HAWC+ total flux observations for C2N and OTFMAP within the same FOV as above. Contours start at 32σ  I  and increase in steps of 2 n  σ, where n = 5, 5.5, 6,... and σ  I  = 0.3 mJy arcsec−2. The beam size is shown as a red circle in the lower left corner. Third row: same as above within an FOV of 120 × 120 arcsec2. Polarization measurements (white lines) are shown for P/σ  P  ≥ 3, PI/σ PI ≥ 3, P < 30%, and I/σ  I  ≥ 50. A 5% polarization measurement is shown at the bottom right. Fourth row: HAWC+ polarized flux observations (color scale) within the same FOV and polarization as above. Contours start at 3σ PI and increase in steps of 1σ PI, where σ PI = 0.46 mJy arcsec−2.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Fluxes uncorrected and corrected owing to PWV variations during observations of M83. Measured fluxes (left column) are fit with a polynomial function of order 3 (black solid line) for flights F0735 (top) and F0736 (bottom). Corrected fluxes (left column) by the normalized fit to the mean flux of flight F731 are shown.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Active galactic nuclei. Shown are Centaurus A at 89 μm; Circinus at 53, 89, and 214 μm; NGC 1068 at 53 and 89 μm; and NGC 1097 at 89 and 154 μm. Also shown is total intensity (color scale) in logarithmic scale with contours increasing in steps of 2 n  σ, with n = 5, 5.5, 6,.... The measurements of polarization fraction (white lines) are shown with constant length to display the B-field orientations. Only measurements of polarization fraction with P/σ  P  ≥ 3 and I/σ  I  ≥ 80 were selected. A physical scale (black line) of 0.5, 1.0, or 2.0 kpc and the beam size (red circle) are shown.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Starburst galaxies. Shown are M82 at 53, 89, 154, and 214 μm; NGC 2146 at 53, 89, 154, and 214 μm; and NGC 253 at 89 and 154 μm. Total intensity (color scale) is shown in logarithmic scale with contours increasing in steps of 2 n  σ, with n = 5, 5.5, 6,.... The measurements of polarization fraction (white lines) are shown with constant length to display the B-field orientations. Only measurements of polarization fraction with P/σ  P  ≥ 3 and I/σ  I  ≥ 80 were selected. A physical scale (black line) of 1.0 kpc and the beam size (red circle) are shown.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Spiral galaxies. M51, M83, NGC 3627, NGC 4736, NGC 6946, and NGC 7331 at 154 μm and NGC 4826 at 89 μm are shown. Total intensity (color scale) is shown in logarithmic scale with contours increasing in steps of 2 n  σ, with n = 5, 5.5, 6,.... The measurements of polarization fraction (white lines) are shown with constant length to display the B-field orientations. Only measurements of polarization fraction with P/σ  P  ≥ 3 and I/σ  I  ≥ 80 were selected. A physical scale (black line) of 1.0 kpc and the beam size (red circle) are shown.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Sensitivity comparison between C2N (red) and OTFMAP (blue) observations of NGC 1068 at 89 μm. Histograms of the total intensity (top left), polarized intensity (top right), standard deviations of the total flux (middle left), and polarized flux (middle right) are shown. The median and 1σ uncertainty of the distribution of the standard deviations are shown in the middle panels. The polarization fraction (bottom left) and polarization angle (bottom right) for C2N and OTFMAP observations are shown. A 1:1 line (black dashed line) is shown.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: IP for the C2N and OTFMAP observing modes at all bands. IP for the C2N (circles), OTFMAP (stars), and polarization skydips (squares) for bands A (blue), C (red), D (orange), and E (gray) are shown. Definitions and details of the estimation of the IP are described in Sections 2.5 and 3.3.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Flux variation as a function of time and aircraft altitude for NGC 6946 at 154 μm. Top panel: measured peak fluxes of the scans per HWP PA and ﹩{ \mathcal R }﹩ and ﹩{ \mathcal T }﹩ arrays. Middle panel: PWV-corrected fluxes using the fits shown in Figure 13. The mean (black solid line) and 2σ uncertainty (black dotted line) are shown. Bottom panel: aircraft altitude at the time of data acquisition.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Fluxes uncorrected and corrected by a linear fit due to PWV variations during observations of NGC 6946. Measured fluxes (left column) are fit with a linear function (black solid line) for flights F0683 (top), F0689 (middle), and F0690 (bottom). Corrected fluxes (right column) by the normalized fit to the mean flux of flights F684 and F685 are shown.
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: (Top plot) Ratio of each element from interplanetary CMEs divided by proton density, X/HCME, and normalized by the solar wind, X/HSW, for plasma where C/HCME:C/H SW  >  Fe/HCME:Fe/HSW (black diamonds) and vice versa (red diamonds) organized by mass. The bottom plot is the same for isolated prominences within CMEs as identified in Lepri & Zurbuchen (2010) and Lepri & Rivera (2021).
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: Example of two CMEs as indicated by the solid (start) and dashed (end) vertical lines. The multi-panel shows data from ACE/SWICS, ACE/SWEPAM, and ACE/MAG ranging between days of year 110 and 130. Panel (a) shows the ratio of each element as X/H:X/HSW as described in the text. Panels (b)–(d) show the relative abundances of C, O, and Fe, respectively. Panel (e)–(g) show the proton temperature, velocity, and density, respectively. Panel (h) shows the magnetic field magnitude and RTN components.
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: (Top) Plot of the normalized counts of CME periods across different Fe absolute abundances compared to the solar wind, as log10 Fe/H:Fe/HSW and 〈Q Fe〉. The color bar indicates counts normalized to the peak of the distributions of 2 hr integrated measurements of CMEs between 1998 and 2011.
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: 2D histogram of CME plasma of 〈QFe〉 = 9–17 and log10 Fe/H:Fe/HSW. The color bar indicates the value of elemental density, X, divided by the proton density normalized to its solar wind value as log10X/H:X/HSW. The error bars are the standard deviation of the points.
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: Plots of log10 X/H:X/HSW across 〈QFe〉 for each Fe/H:Fe/HSW bin in Figure 2. The legend indicates the value for each log10 Fe/H:Fe/HSW bin. The error bars are the standard deviation of the points.
Paper: Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks
Authors: Sayantan Auddy, Ramit Dey, Min-Kai Lin, Daniel Carrera, Jacob B. Simon
Figure caption: The upper panel shows the normalized dust surface density distributions of disks with different initial conditions and for different planet masses at 3000P 0. The disk parameters are indicated at the top right of each plot, together with the planet mass at the bottom right. The lower panel shows the radial profiles of the azimuthally averaged surface densities at the beginning of the simulation (Σd0; the dashed black lines) and at the end of the simulation after the gap is formed (Σd; the solid red lines). The horizontal arrow marks the dust gap width. The gap width is the distance between the inner and outer edge of the gap (the vertical dotted lines) where Σd(R) reaches 50% of the initial surface density Σd0. The crosses indicate the minimum surface density Σdmin.