adsabs/AstroCLIMB huggingface dataset:
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: A migration map for the MDW disk given by Equation (9) with Σ0 = 1700 g cm−2, β1 = − 1, β2 = 0, and α = 10−4. The color scale shows δa/a, where δa is the change of semimajor axis in 1 Myr. The red and blue colors indicate inward and outward migration, respectively. The thin solid line is the zero migration radius. The thick solid line is where −δa = a (strong inward migration), and the dashed line is where δa = a (strong outward migration). The migration speed is given here for t = 0. It is reduced by the ﹩\exp (-t/\tau )﹩ factor for 0 < t ≤ 5 Myr.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: A comparison between the scaling laws of Z. M. Leinhardt & S. T. Stewart (2012) and the smoothed particle hydrodynamics (SPH) simulations of impacts reported in A. Emsenhuber et al. (2020). We considered three different collision setups for this illustration: the (1) target mass mtarget = 0.01 MEarth, projectile mass mprojectile = 0.2 Mtarget, and impact angle θ = 45° (red symbols and lines), (2) mtarget = 0.1 MEarth, mprojectile = 0.35 Mtarget, and θ = 60° (green symbols and lines), and (3) mtarget = 1 MEarth, mprojectile = 0.7 Mtarget, and θ = 75° (blue symbols and lines). The solid lines show the mass of the largest fragment produced by collisions as a fraction of the combined mass, mlargest/(mtarget + mprojectile), as computed from Z. M. Leinhardt & S. T. Stewart (2012). This can be compared to the results of individual SPH simulations reported in Table 1 of A. Emsenhuber et al. (2020), labeled with crosses here. The dashed lines and stars show the same for the second-largest fragment. Abrupt changes of mlargest/(mtarget + mprojectile) occur at the transitions between different fragmentation regimes.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The initial surface densities of gas disks considered in this work and elsewhere. The green lines show profiles given by Equation (8) with α0 = − 0.5 and α0 = − 1.5 (MMSN profile), and Σ0 = 1700 g cm−2. The red line is our MDW disk from Equation (9) with Σ0 = 1700 g cm−2, β1 = −1, and β2 = 0. Our MDW disk is reminiscent of disk “shallow” in J. M. Y. Woo et al. (2024; blue line).
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The orbital histories of outer planets in our instability model. The planets started in the (3:2, 3:2, 2:1, 3:2) resonant chain. The outer disk of planetesimals, not shown here, with the total mass Mdisk = 20 MEarth was placed beyond Neptune. The plot shows the semimajor axes (solid lines), and perihelion and aphelion distances (dashed lines) of each planet’s orbit. The black dashed lines show the semimajor axes of planets in the present solar system. The third ice giant was ejected from the solar system during the instability about 5.8 Myr after the start of the simulation, which is 10.8 Myr after t0 in the time line discussed in Sections 2.2 and 2.3.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The result of 100 successful simulations of the back20 model (the ring at 0.85 au with a 20% background) that produced a good match to all terrestrial planets (as defined in Section 3.1). The black dots show the results of individual simulations with good final planets. The bigger red dots are the real planets. Note that we do not exclude simulations that produced additional bodies with m < 0.05 MEarth in the Mars region (1.2 < a < 1.8 au). Some of these bodies would collide with Mars at t > 200 Myr (these simulations were terminated at 200 Myr).
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The accretion history of planets in one of the best cases from the simulation set back20 (a ring at 0.85 au, 20% background, no gas). Each pair of connected line segments represents one accretion event. The black and red dots are the model and real planets, respectively. The dot size is proportional to planet mass.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The result of 100 successful simulations of the back20 model (the ring at 0.85 au with a 20% background) that produced a good match to all terrestrial planets (as defined in Section 3.1). The black dots show the results of individual simulations with good final planets. The bigger red dots are the real planets.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Amplitude scaling relations derived with spectroscopic Teff from Specmatch (top panels) and isochrone-based Teff from T. A. Berger et al. (2020b; bottom panels). Left: observed amplitude as a function of the expected amplitude derived using Equation (10) without an activity term. The gray points show the expected amplitudes using best-fit parameters from H11, and the blue points show the expected amplitudes with the relation from H11 but with new best-fit parameters, r, s, and t. The dashed line shows the one-to-one relation. The text indicates the best-fit parameters for both distributions. Middle: same as the left panel but including an activity term, colored by the ﹩{\mathrm{log}}\,{R}_{\,{\rm{HK}}\,}^{{\prime} }﹩ index from HIRES. The annotated text indicates the best-fit parameters, and the dashed line shows the one-to-one relation. Right: residuals between observed and predicted amplitudes using the relation and best-fit parameters from H11 (gray circles), the expected amplitudes derived using the H11 relation but re-derived best-fit parameters (gray squares), and the new relation from Equation (10) (the blue circles). The annotated text indicates the mean offset with error and the scatter.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Comparison of radii (top) and masses (bottom) derived with asteroseismic scaling relations (x-axis) and with Gaia measurements (y-axis). Residuals (i.e., ratio between the seismic and Gaia-derived quantities) are shown in the bottom panels. The color-coding denotes the height-to-background ratio, defined as the ratio between the amplitudes of oscillation and background. The text indicates the mean offset and error between the two measurements and the scatter, σ.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Observed amplitude at νmax as a function of frequency of maximum oscillation. Panel A shows the new detections in blue against the overall sample in gray. Panels B–F are colored by stellar properties: metallicity (B), Kp (C), Gaia DR3 RUWE ≥ 1.5 (D), seismic mass (E), and Gaia effective temperature from T. A. Berger et al. (2020b; F).
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Comparison of amplitudes derived in this work to those from D. Huber et al. (2011) for 447 targets in gray. The blue points show the 132 targets for which ﹩{\mathrm{log}}\,{R}_{\,{\rm{HK}}\,}^{{\prime} }﹩ values are available in HIRES. The text indicates the mean offset with error, and scatter in both distributions. The dashed line indicates unity. The bottom panel shows the residual.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Δν vs. νmax for all 765 stars in our catalog, where the 50 new detections are shown in blue squares. The solid, orange line shows the best-fit relation between νmax and Δν. The bottom panel shows the residuals.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Derived stellar masses and radii using Equations (6) and (7) for our sample, including new detections in blue, planet hosts in yellow, and new planet hosts in orange. 70 out of 765 stars are not shown, given no measurement of νmax, Δν, or Teff.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Fractional uncertainty in νmax (top) and Δν (bottom) for 458 overlapping targets in this work (blue) and H11. The dashed lines and text indicate the mean fractional uncertainty for each sample.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Comparison of radii (top) and masses (bottom) derived with asteroseismic scaling relations (x-axis) and Gaia DR3 FLAME measurements (y-axis). Residuals are shown in the bottom panels. The text indicates the mean offset and error between the two measurements and the scatter, σ.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Background divided power spectra for seven Kepler hosts with newly discovered oscillations centered on νmax.
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: (Left) ﹩{\chi }_{\nu }^{2}﹩ vs. spectral type for objects in the Montreal Spectral Library (J. Gagné et al. 2014) when compared to HIP 99770 b H- and K-band spectra. The sources are colored based on their gravity level. The best fitting objects fall in the L4.5 to L9.5 spectral type range. This spectral range is consistent with a temperature of 1300–1600 K. (Right) The best fitting spectra from the Montreal Spectral Library, SIMPJ0956-1447, shown in blue compared to the HIP 99770 b H- and K-band spectra shown in black, with the low-resolution spectra plotted in gray as a reference for shorter wavelengths.
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: (Left) HIP 99770 b H-band spectra (black) compared to the H-band spectra of HR 8799 b (blue), HR 8799c (orange), SIMPJ0956-1447 (magenta), and HD 33632 Ab (green). The low-resolution spectra are plotted in gray and H2O absorption is also marked in black. (Right) HIP 99770 b K-band spectra (black) compared to the K-band spectra of HR 8799 b (light blue: OSIRIS, dark blue: GRAVITY), HR 8799c (orange), HR 8799 d (red), SIMPJ0956-1447 (magenta), and HD 33632 Ab (green). For both plots, the low-resolution spectra are plotted in gray and H2O and CO absorption is also marked in black.
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: (Left) Predicted location of HIP 99770 b from the best-fitting orvara orbits (assuming flat priors on the companion mass) in 2028 January. (Right) Predicted contrast vs. wavelength for HIP 99770 b from the best-fitting Lacy/Burrows models considered in this paper.
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 without RV measurements from KPIC. Fit using only absolute astrometry from HGCA and relative astrometry (from both initial discovery and follow-up). 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: The best fits from four atmospheric models, Lacy/Burrows, BT Settl, Exo-REM, and Sonora, are plotted against the H and K Band data as well as the photometry point in black (far right). The low-resolution data are also plotted in gray for comparison at lower wavelengths but was not used for fitting the models.
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: The 3σ (dashed) and 5σ (solid) Δχ2 contours for the BT Settl, Lacy/Burrows, Exo-REM, and Sonora Diamondback models in temperature/gravity space. Black contours indicate the parameter combination yielding the best-fitting model (red star) from each grid.
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: Correlation matrix Ψi,j for the H (top) and K (bottom) band as a function of spectral chanel λi, λj. The off-diagonal elements are residual spectrally correlated noise.
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: Same as Figure 5 except including the 2023 May VLTI/GRAVITY astrometric point from T. O. Winterhalder et al. (2025).
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: Same as Figure 3 except including the 2023 May VLTI/GRAVITY astrometric point from T. O. Winterhalder et al. (2025).
Paper: The Galactic Bulge Exploration. VI. Gaia Enceladus/Sausage RR Lyrae Stars in the Inner-central Stellar Halo of the Milky Way
Authors: Andrea Kunder, Zdenek Prudil, Antonela Monachesi, Samuel J. Morris, Kathryn Devine, Joanne Hughes, Kevin R. Covey, R. Michael Rich, Elisa A. Tau
Figure caption: Left: the integrals of motion for five dominant accretion events in the Au-18 inner-central halo. The A. Helmi et al. (2018) Lz–E criteria to select GES stars encompasses a large fraction of the GES-18 (peak_mass_ID=205) particles (rectangle region). Middle: the distribution of eccentricity of GES-18 particles as compared to the in situ particles and the other accreted particles in the inner-central halo of Au-18. The eccentricities of the observed halo RRLs with integrals of motion consistent with GES are also shown. GES-18 dominates at high eccentricities; the peak of high eccentricities in our sample of halo RRLs suggest ∼9% of the sample originated from the GES merger. Right: galactocentric radius vs. [Fe/H] metallicity for GES, the other accreted components, the in situ components and the RRLs in the inner-central halo. Only the in situ Au-18 particles exhibit a statistically significant negative metallicity gradient with Galactocentric radius, with a slope of −0.0075 ± 0.0015 dex kpc−1.
Paper: The Galactic Bulge Exploration. VI. Gaia Enceladus/Sausage RR Lyrae Stars in the Inner-central Stellar Halo of the Milky Way
Authors: Andrea Kunder, Zdenek Prudil, Antonela Monachesi, Samuel J. Morris, Kathryn Devine, Joanne Hughes, Kevin R. Covey, R. Michael Rich, Elisa A. Tau
Figure caption: Left: the logarithm of the fraction of the total accreted particles (gray) and GES-18 particles (red) in the inner-central halo from the Au-18 simulation. The fraction of GES-18 merger particles peaks at ∼−1.3 dex, whereas there is a dramatic increase with decreasing metallicity for other accretion events. Middle: the integrals of motion for the Au-18 inner-central halo particles compared to the RRL sample. The A. Helmi et al. (2018) Lz–E criteria to select GES stars is indicated by the dashed line. Right: the fraction of GES-18 particles as compared to the Au-18 accreted particles (top) and the fraction of GES-18 particles as compared to the Au-18 in situ particles (bottom) that fall within the A. Helmi et al. (2018) Lz-E criteria is shown as a function of [Fe/H] metallicity. The fraction of GES-18 particles that falls outside the A. Helmi et al. (2018) Lz-E criteria is shown as a function of [Fe/H] metallicity. In samples of accreted stars, ∼30% of stars in the A. Helmi et al. (2018) Lz-E criteria will belong to GES.
Paper: The Galactic Bulge Exploration. VI. Gaia Enceladus/Sausage RR Lyrae Stars in the Inner-central Stellar Halo of the Milky Way
Authors: Andrea Kunder, Zdenek Prudil, Antonela Monachesi, Samuel J. Morris, Kathryn Devine, Joanne Hughes, Kevin R. Covey, R. Michael Rich, Elisa A. Tau
Figure caption: Left: our sample of RRLs in Galactic coordinates, where the RRLs with orbits consistent with belonging to the inner-central halo (﹩3\,\mathrm{kpc}\lt {z}_{\max }\lt 20\,\mathrm{kpc}﹩) are highlighted. Middle: the inner-central halo sample has a lower [Fe/H] metallicity and also a period distribution more consistent with accretion than the bulge/disk RRLs. Right: our RRL sample z-coordinate plotted with x-coordinate in left-handed Cartesian Galactocentric coordinates. The gray and red dots represent the sample from G. C. Liu et al. (2020) and our sample, respectively.
Paper: The Galactic Bulge Exploration. VI. Gaia Enceladus/Sausage RR Lyrae Stars in the Inner-central Stellar Halo of the Milky Way
Authors: Andrea Kunder, Zdenek Prudil, Antonela Monachesi, Samuel J. Morris, Kathryn Devine, Joanne Hughes, Kevin R. Covey, R. Michael Rich, Elisa A. Tau
Figure caption: Left: the inner Galaxy RRL sample in Lz and energy space. The inner-central halo RRLs are designated with large red circles, whereas the bulge and disk RRLs are shown as small gray circles. The straight lines indicate the criteria used to select GES stars, namely −1500 < Lz < 150 kpc km s−1 and E > −1.8 × 105 km2 s−2. Right: the RRL with Lz and energy values consistent with GES have higher eccentricities and tend to be more metal-poor as compared to other inner-central halo RRLs.
Paper: The Galactic Bulge Exploration. VI. Gaia Enceladus/Sausage RR Lyrae Stars in the Inner-central Stellar Halo of the Milky Way
Authors: Andrea Kunder, Zdenek Prudil, Antonela Monachesi, Samuel J. Morris, Kathryn Devine, Joanne Hughes, Kevin R. Covey, R. Michael Rich, Elisa A. Tau
Figure caption: The fraction of accreted particles with [Fe/H] = −1 as a function of Galactocentric radius from the Au-18 simulation. Although the fraction of accreted particles increases with increasing distance to the Galactic center, the opposite trend is seen for the GES-18 particles.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The radial distribution of terrestrial planetesimals in the successful two-source models tested in this work. To produce correct Mercury, Venus, and Earth, the inner ring of planetesimals must have been radially narrow (σ1 ≲ 0.1 au) and was located at ≃0.4–0.6 au. The outer reservoir of planetesimals beyond ∼1.5 au was the primary source of Mars’ accretion.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Density histograms of AV (left), ﹩{R}_{\widetilde{VI}}﹩ (middle), and α (right) within the overlap of VV 191b with the restrictions as mentioned in Figure 7. The best log-normal fits of AV and ﹩{R}_{\widetilde{VI}}﹩ and a Gaussian fit of α are overlaid in black. The distributions of the dust parameters with an even stricter threshold, AV > 0.25 and S/NF090W ≥ 3, are shown in orange, with their best-fit probability density function (pdf) fits overlaid in gray. The mean and the standard error of the distributions (not the fits) of ﹩{R}_{\widetilde{VI}}﹩ and α are given in Table 2.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Left: map of the power-law index α used to fit the interstellar attenuation law in the NIR. The map is approximated using the linear slope of the log–log equation of the power law through n = 1000 Monte Carlo iterations. Right: the uncertainties of α, Δα. Each uncertainty pixel is the standard error (﹩\sigma /\sqrt{n}﹩) of the mean of the Monte Carlo distributions.