adsabs/AstroCLIMB huggingface dataset:
Paper: A Maximum Likelihood Calibration of the Tip of the Red Giant Branch Luminosity from High Latitude Field Giants Using Gaia Early Data Release 3 Parallaxes
Authors: Siyang Li, Stefano Casertano, Adam G. Riess
Figure caption: Probability distribution of absolute magnitude for the best-fit model for the two values that bracket the expected range of β listed in the text. The black histograms show the absolute magnitude probability distribution, marginalized in distance and summed over all the stars in the sample, i.e., the most likely distribution of their absolute magnitudes. The red lines show the corresponding model or idealized LFs. The small blips on either side of the break are a result of the approximation used in drawing this figure, and can be ignored. The results shown here do not yet account for the empirical relationship between the color and luminosity of the TRGB, which we determine to be ∼0.05 mag between the observed and a fiducial, blue TRGB. See Section 3.3 for further details.
Paper: A Maximum Likelihood Calibration of the Tip of the Red Giant Branch Luminosity from High Latitude Field Giants Using Gaia Early Data Release 3 Parallaxes
Authors: Siyang Li, Stefano Casertano, Adam G. Riess
Figure caption: Gaia parallax offset residuals measured externally by sources compiled by Lindegren (2021). The fit for the 10 < G < 13 mag range is represented by the red shaded region where ±5 μas to the fit has been added for clarity. The offsets in the plot are from Bhardwaj et al. (2021), Fabricius et al. (2021), Huang et al. (2021), Ren et al. (2021), Riess et al. (2021a), Stassun & Torres (2021), Vasiliev & Baumgardt (2021), and Zinn (2021).
Paper: A Maximum Likelihood Calibration of the Tip of the Red Giant Branch Luminosity from High Latitude Field Giants Using Gaia Early Data Release 3 Parallaxes
Authors: Siyang Li, Stefano Casertano, Adam G. Riess
Figure caption: Histograms for the final data set after all selection cuts. In clockwise order from the top left: (1) I-band apparent magnitudes, (2) parallax, (3) Gaia G-band magnitudes, (4) Galactic latitude, (5) extinction using the Schlafly & Finkbeiner (2011) dust maps and NASA/IPAC extinction tool, (6) Gaia B  p  − R  p  color, (7) fractional parallax error, and (8) I-band apparent magnitude error. The abrupt cutoffs for 3, 4, and 6 are due to the initial Gaia selection cuts.
Paper: A Maximum Likelihood Calibration of the Tip of the Red Giant Branch Luminosity from High Latitude Field Giants Using Gaia Early Data Release 3 Parallaxes
Authors: Siyang Li, Stefano Casertano, Adam G. Riess
Figure caption: Apparent G-band magnitudes and parallaxes for each star remaining after the initial cut (black), Gaia EDR3/APASS DR9 crossmatch (blue), and final sample (red). These selections are applied sequentially, so the black sample also includes the red and blue points, and the blue sample includes the red points. The upper group of stars contains main-sequence stars that are cut out by the series of selections.
Paper: A Maximum Likelihood Calibration of the Tip of the Red Giant Branch Luminosity from High Latitude Field Giants Using Gaia Early Data Release 3 Parallaxes
Authors: Siyang Li, Stefano Casertano, Adam G. Riess
Figure caption: Plot showing a comparison of TRGB zero-point calibrations since 2017 separated by the galaxy. The right blue dashed vertical line represents the midpoint TRGB value of −3.91 mag found here. The left red dashed vertical line shows the weighted average of the four measures from Freedman 2021 of ﹩{M}_{F814W}^{\mathrm{TRGB}}=-4.043\pm 0.025﹩ mag. Changing their value by 0.05 mag would change the derived value of H 0 from 69.8–71.4 km s−1 Mpc −1.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Energy transfer coefficients A 1 (top), A 2 (middle), and A 3 (bottom) against e in for a parabolic encounter with i mut = 0° (black), 90° (red), and 180° (blue). Dots plotted with the same color represent ∼ 104 snapshots from the simulated trajectories corresponding to those shown in Figure 14 for (r p,out/a in, e out, i mut) = (2.8, 0.4, 0°), (3.8, 0.4, 90°), and (2.2, 0.92, 180°). The curves labeled ZKL show the trajectory along e in = e in(i mut) from Equation (22). Note that the sequences of dots in each panel may look like solid curves, indicating they reproduce well the expected relation between i mut and e in.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Normalized disruption time T d/P in distributions for the triples in terms of x. The magenta, blue, and black dots correspond to q 23 = 5.0, 1.0, and 0.5, respectively. The top, middle, and bottom panels show the results for prograde, orthogonal, and retrograde cases, respectively. The left and right panels show the cases for q 21 = 1.0, and 0.1, respectively. The solid and dotted curves denote the corresponding MK20 RW model estimation for e out = 0.04 and 0.96, which are the lower and upper limit eccentricities in the simulations, respectively. The dashed lines represent the best-fit empirical models.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Examples of evolution of hierarchical triples for q 21 = 1 and q 23 = 5. The initial orbital parameters are (r p,out/a in, e out, i mut) = (2.8, 0.4, 0°; magenta in the left panels), (3.0, 0.4, 0°; green in the left panels), (3.8, 0.4, 90°; magenta in the middle panels), (4.0, 0.4, 90°; green in the middle panels), (2.2, 0.92, 180°; magenta in the right panels), and (2.8, 0.92, 180°; green in the right panels).
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: The disruption timescale distributions of triples for various phase angles (M out, ω out) (top), and the corresponding histograms (bottom). We adopt the same values for the other initial orbital parameters as panels (a), (b), and (c) in Figure 6. The dashed vertical lines are from our empirical best-fit models in Figure 12. Note that T d/P in < 102 and T d/P in > 106 are assigned the same colors as 102 and 106, respectively.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: The best-fit values of the proportional factor K(i mut, q 21, q 23) in Equation (16) corresponding to Figures 8–10. The quoted error bars represent the 1σ confidence range. For reference, the values of the MA01 model are plotted as the black squares.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Histograms of the disruption timescales for various initial phase angles (M out, ω out), corresponding to coplanar prograde (top), orthogonal (middle), and coplanar retrograde (bottom) triples with q 21 = 1, q 23 = 5, and e out = 0.7. The dashed vertical lines are from our empirical best-fit models in Figure 12.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Normalized disruption timescale (T d/P in) distribution for the coplanar prograde and equal-mass triple against x for q 21 = 1, q 23 = 5, and e out = 0.7. For reference, the best-fit empirical model from Figure 12 is plotted as the dashed line.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Dependence of the ejection rate of three bodies on q 23. Red, blue, and black bars represent the ejection of the primary, secondary, and tertiary body, respectively. The top, middle, and bottom panels show prograde, orthogonal, and retrograde cases, respectively. In each set of panels, the upper and lower plots correspond to q 21 = 1.0 and 0.1, respectively.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: The best-fit values for S with their 1σ confidence range.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Orbital configuration of a triple system consisting of an inner binary and a tertiary. The origin of the reference frame is set to be the barycenter of the inner binary, instead of the triple.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: The disruption time T d/P in dependence on e out − r p,out/a in plane for the coplanar prograde (i mut = 0°) and equal-mass (q 21 = 1) inner binary case with q 23 = 5. The disruption timescales evaluated from simulations are indicated according to the side color scales. Magenta and black curves represent the MA01 dynamical stability criterion and the MK20 model predictions, respectively. The region where the inner and outer orbits of the system cross (r p,out/a in < 1) is shaded in green. Cross symbols indicate the triples that remain stable until t int = 109 P in, while circle-cross symbols define the boundary of triples that disrupt before 109 P in.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Normalized disruption timescales T d/P in to the tiny change of the input value of the inner orbital period P in for coplanar prograde triples with q 21 = 1 and q 23 = 5. The top, middle, and bottom panels correspond to (r p,out/a in, e out) = (2.0, 0.84), (2.6, 0.44), and (2.6, 0.88), respectively. In the left and right panels, the 15th and fourth digits of the initial values of P in are modified, respectively.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Disruption timescales of coplanar prograde triples T d/P in. The left and right panels correspond to q 21 = 1 and 0.1, while the top, center, and bottom panels are for q 23 = 0.5, 1, and 5, respectively.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Same as Figure 8 but for coplanar retrograde triples.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Same as Figure 3 but for coplanar retrograde triples (i mut = 180°).
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Ratio of the normalized disruption timescales for individual triples (q 21 = 1 and q 23 = 5) of P in = 103 and 104 days against those of P in = 103 days (left), and their corresponding probability density function (right).
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Schematic illustrations of triple systems for very different q 21 and q 23 regimes. Red, blue, and black filled circles correspond to the primary, secondary, and tertiary, respectively. Note that a triple with q 23 < 1 indicates that its tertiary is more massive than the secondary.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Same as Figure 8 but for initially orthogonal triples.
Paper: Dynamical Disruption Timescales and Chaotic Behavior of Hierarchical Triple Systems
Authors: Toshinori Hayashi, 利憲 林, Alessandro A. Trani, Yasushi Suto, 靖 須藤
Figure caption: Same as Figure 3 but for initially orthogonal triples (i mut = 90°).
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Lensed source 5 in RXJ1347 from Zitrin et al. (2015). The overlaid blue contours in the top two panels show the predicted shape of the lensed source based on the positions of the lensed components 5.1, 5.2, and 5.3 and their magnifications of 17.7, 2.2, and 18.2, respectively. The positions of the lensed components are shown with red squares in all four panels. Note that we applied a 0.″4 astrometric correction in R.A. to the Zitrin et al. (2015) coordinates to match them to the HST image. This correction was used in all four panels. (Upper left panel) The SCUBA-2 850 μm image with the predicted SCUBA-2 850 μm shape overlaid. In order to match the observed 850 μm flux, we need a demagnified value of 0.4 mJy for the source. All three lensed components are blended at the SCUBA-2 850 μm FWHM. (Upper right panel) The SCUBA-2 450 μm image with the predicted SCUBA-2 450 μm shape overlaid. In order to match the observed 450 μm flux, we need a demagnified value of 0.66 mJy for the source. All three lensed components are still blended at the SCUBA-2 450 μm FWHM. Note that the dark region around the source in the SCUBA-2 images is a result of the Mexican hat-shape filter matching. (Lower left panel) The ALMA 1.2 mm image of the source from ALMA program 2018.1.00035.L (PI: K. Kohno). (Lower right panel) The CLASH F160W image of the source.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Lensed source 5 in MACSJ0717 from Zitrin et al. (2009). The overlaid blue contours in three of the four panels show the predicted shape of the lensed source based on the positions of images 5.1, 5.2, and 5.3 and their magnifications of 6.8, 7.5, 3.0, respectively. (Upper left panel) The SCUBA-2 850 μm image with the predicted SCUBA-2 850 μm shape overlaid. In order to match the observed 850 μm flux, we need a demagnified flux of 0.42 mJy for the source. The positions of the lensed components are shown with red squares. The 5.1 and 5.2 images are marginally blended at the SCUBA-2 850 μm FWHM. (Upper right panel) The 450 μm image with the predicted SCUBA-2 450 μm shape overlaid. The 5.1 and 5.2 images are resolved, but neither is detected. (Lower left panel) The ALMA 870 μm field containing the 5.2 image with the predicted SCUBA-2 850 μm shape overlaid. The 5.1 image is off the top of the ALMA field. (Lower right panel) A blow-up of the central region of the ALMA field, with the overlaid white contours showing the HFF F160W image. The large white square shows the position of the 5.2 image. The ALMA image shows two peaks, one associated with the brightest position of 5.2 and a second associated with a fainter region to the south.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: (Upper three panels) ALMA observations in A370. The left panel shows the targeted fields at 870 μm, each with a radius of 9″. The white circles in all panels show our detected sources from these targeted observations. The circles are of arbitrary size but roughly match this ALMA field-of-view. The center panel shows the mosaicked 1.2 mm image from ALMA programs #2013.1.00999.S and #2015.1.01425.S (PI: F. Bauer; González-López et al. 2017), while the right panel shows that from ALMA program #2018.1.00035.L (PI: K. Kohno). The mosaicked images are taken from the Japanese Virtual Observatory (JVO) archive. There are no additional detected sources in the mosaics. (Lower three panels) SCUBA-2 450 μm image (left), HerMES 100 μm image (center), and BUFFALO F160W image.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: (Upper three panels) ALMA observations in MACSJ1149. The left panel shows our targeted fields at 870 μm, each with a radius of 9″. The white circles in all panels show our detected sources from these targeted observations. The circles are of arbitrary size but roughly match this ALMA field of view. The center panel shows the mosaicked 1.2 mm image from ALMA programs #2013.1.00999.S and #2015.1.01425.S (PI: F. Bauer; González-López et al. 2017), while the right panel shows that from ALMA program #2018.1.00035.L (PI: K. Kohno). The mosaicked images are taken from the JVO archive. There are no additional detected sources in the mosaics. (Lower three panels) SCUBA-2 450 μm image (left), HLS 100 μm image (center), and BUFFALO HST F160W image.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: (Upper two panels) ALMA observations in MACSJ0717. The left panel shows the targeted fields at 870 μm from our program and from ALMA program #2017.1.00091.S (PI: A. Pope) as circular fields with a radius of 9″, as well as the targeted fields at 1.2 mm from ALMA program #2016.1.00293 (PI: A. Pope) as square fields. The white circles in all panels show the detected sources in either band from these targeted observations. The circles are of arbitrary size but roughly match this ALMA field of -view. The right panel shows the mosaicked 1.2 mm observations from ALMA programs #2013.1.00999.S and #2015.1.01425.S (PI: F. Bauer; González-López et al. 2017). There are no additional detected sources in the mosaics. (Lower three panels) SCUBA-2 450 μm image (left), HLS 100 μm image (center), and BUFFALO HST F160W image.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Representative SCUBA-2 (left) 850 μm and (right) 450 μm images of the cluster MACSJ1149 showing the central ﹩4\buildrel{\,\prime}\over{.} 5﹩ radius region. (The images for all 10 clusters are shown in the Appendix.) The white circles show the >4σ 850 μm selected sample, including a confusion noise of 0.33 mJy. The green contours on the 450 μm image show the Zitrin (2021) lens model for z = 2 at magnifications (moving inward) of 1.4, 2, and 4.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Redshift vs. observed F160W magnitude. The red squares show A370, blue MACSJ1149, green MACSJ0717, and black the remaining cluster fields. The active galactic nucleus (AGN) in A370 is marked with a larger open square. The black diamonds and triangles show the CDF-S and CDF-N fields, respectively. In all fields, solid symbols show speczs and open symbols show photzs. The horizontal lines show the redshifts of two of the clusters (A370 in red and MACSJ1149 in blue).
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Hubble Space Telescope (HST) Frontier Fields (HFF) F160W image of the giant arc in A370. The red contour shows our 850 μm SCUBA-2 observation of the arc, and the green contour shows the Herschel/PACS 100 μm image (Rawle et al. 2016). The image is 40″ on a side.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: HST three-color (red: BUFFALO/HFF F160W; green: HFF F814W; blue: HFF F606W) images of the A370 sources with ALMA emission overlaid (green contours: 2, 4, 6, 8, 10, and 12σ; beam size is also shown in the lower left corner of each image).
Paper: On the Convergence of the Milky Way and M31 Kinematics from Cosmological Simulations
Authors: J. E. Forero-Romero, D. Sierra-Porta
Figure caption: Median tangential (left) and radial (right) speeds of M31 relative to the MW as a function of the inverse simulation box size. All the simulations listed in Table 1 are included in this figure.
Paper: On the Convergence of the Milky Way and M31 Kinematics from Cosmological Simulations
Authors: J. E. Forero-Romero, D. Sierra-Porta
Figure caption: Cumulative distribution for the tangential and radial speeds of M31 relative to the MW. Only pairs from AbacusBase (the simulation with the largest box size) are included in this figure.
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: The M 0 (top row) and M 1 (bottom row) model components integrated over the zYJH bandpasses. The new SALT3-NIR model is shown in red, while the SALT2-Extended model (previously used for SALT2 simulations in the NIR) is shown in blue.
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: Color law (top) and color scatter (bottom) for SALT3 (black) and SALT3-NIR (red). The dashed region of the SALT3 curve corresponds to the linear regime (color law) or no constraint (color scatter). The same regions are depicted by gray shading for SALT3-NIR. The dust law from Fitzpatrick (1999; green dashed–dotted, R  V  = 3.1) is shown in the top panel for comparison.