adsabs/AstroCLIMB huggingface dataset:
Paper: KMT-2018-BLG-0029Lb and OGLE-2019-BLG-0960Lb: Mass Measurements for Two Super-Earth Microlensing Planets
Authors: Keming Zhang, 可名 张, Sean K. Terry, Joshua S. Bloom, B. Scott Gaudi, Jessica R. Lu
Figure caption: Constraints on the lens mass and distance for the two lens systems. KMT-2018-BLG-0029L: Results for the u0 < 0 (top left) and u0 > 0 (bottom left) microlensing parallax models. OGLE-2019-BLG-0960L: Results for the s > 1 (top right) and s < 1 models (bottom right), each combining u0 > 0 and u0 < 0 microlensing parallax solutions. In each panel, the shaded regions represent the 68% confidence intervals of the mass–distance relationships for the lens system as derived from parallax constraints from ground (πE, blue) and Spitzer (gray; only shown for KB180029), the angular Einstein radius (θE, green), and the observed Ks-band lens flux (red). For OB190960, the Spitzer parallax is shown as the black curve to the upper right, as no uncertainties were reported in the original analysis. The median posterior values for the lens mass and distance are shown as the black dot with the error bar indicating the nominal 68% confidence intervals. The gray dashed lines (without shade) indicate the 68% confidence interval of partial extinction as a function of distance, with the vertical span of each panel corresponding to 0% (bottom edge) to 100% (top edge) of the total extinction experienced by the source star.
Paper: KMT-2018-BLG-0029Lb and OGLE-2019-BLG-0960Lb: Mass Measurements for Two Super-Earth Microlensing Planets
Authors: Keming Zhang, 可名 张, Sean K. Terry, Joshua S. Bloom, B. Scott Gaudi, Jessica R. Lu
Figure caption: Illustration of a four-fold degeneracy for the Earth–Roman satellite parallax shown at the epoch when the source crosses the star–planet axis for Roman (green dot), assumed to be the time of planetary anomaly. The Earth-based source location is shown as the blue dot. Due to the inner–outer degeneracy, there are four possible configurations (±Δx0; ±u0) with the identical Earth–Roman difference in the timing and duration of the planet anomaly. Within each scenario, the solid arrow indicates the source offset vector (Δu = u⊕ − uRoman), which lie along the on-sky projected Roman–Earth separation and whose magnitudes are proportional to the lens-source relative parallax. The vertical dashed arrow shows its projection perpendicular to the star–planet axis, which is informed by the anomaly time delay. Shifting the Earth-based source position along the horizontal dashed line does not change the time delay.
Paper: KMT-2018-BLG-0029Lb and OGLE-2019-BLG-0960Lb: Mass Measurements for Two Super-Earth Microlensing Planets
Authors: Keming Zhang, 可名 张, Sean K. Terry, Joshua S. Bloom, B. Scott Gaudi, Jessica R. Lu
Figure caption: Keck NIRC2-LGS images of the two events. North is up and East is to the left. The green and red boxes indicate the target and comparison stars, respectively. Insets show zoomed-in views of each star, including the original image and the residuals following PSF subtraction, which are shown on the identical flux scale to facilitate comparison. The gray dotted circles in the residual images show the predicted lens-source separation.
Paper: KMT-2018-BLG-0029Lb and OGLE-2019-BLG-0960Lb: Mass Measurements for Two Super-Earth Microlensing Planets
Authors: Keming Zhang, 可名 张, Sean K. Terry, Joshua S. Bloom, B. Scott Gaudi, Jessica R. Lu
Figure caption: Illustration of KMT-2018-BLG-0029 in the lens plane, where the planet is shown to perturb the major image from two possible locations, marked by the red and blue open circles. The Einstein radius is shown as a dashed circle. The trajectories of the source star, major image, and minor image are shown below their respective labels, with the direction of the trajectories indicated by the arrows. Note that the axes are rotated 90° with respect to Figure 1.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: TESS photometry across sectors 25, 51, 52, and 79, with the best-fit model shown in blue.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: Top Left: TOI-7149 b (green square) in a mass–radius plane alongside other transiting M-dwarf planets (colored by equilibrium temperature). The GEMS discovered by the Searching for GEMS survey are circled in blue. We also include planets around FGK stars in the background, along with density contours for 0.3, 1, 3 g cm−3  (NASA Exoplanet Archive 2025). Top Right: The insolation-radius plane is shown for the same sample of planets. Bottom: Bulk planetary density vs. stellar mass, color coded by insolation flux. Warm Jupiters orbiting FGK dwarfs receiving <160 S⊕ (Teq ∼ 1000 K) flux are shown in solid color, with hot Jupiters in the background (red circles). TOI-7149 is one of the lowest mass stars hosting a transiting giant planet.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: Photometric observations for TOI-7149 b phase-folded to the best-fit orbital period; each data set is separated by 0.25. The black points show the detrended data, while the model is shown as a solid, colored line along with the 1σ confidence intervals as translucent bands. We include the representative median statistical uncertainty at x = 0.1. Ground-based observations are used to measure the transit depth and ephemeris. The TESS data set (red models) is used to refine the ephemeris, with a floating dilution term, which is constrained using the ground-based photometry (blue models).
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: Left: Time series RVs of TOI-7149 with HPF data shown in green, and the best-fitting model derived from the joint fit to the photometry and RVs plotted in blue. The model includes the 16%–84% confidence interval in lighter blue, as well as the RV trend detailed in Table 3. The bottom panel shows the residuals after subtracting the model from the data. Right: HPF RV observations phase-folded to the best-fit orbital period from the joint fit described in Section 4. Instrument error bars are shown in green, while RV jitter added in quadrature is shown in the background on each point in gray.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: We show a Gaia CMD for the 200 pc sample from the Searching for GEMS survey with a Gaussian kernel density estimation, which is darker in regions with more stars. The upright violet triangles indicate GEMS within 200 pc, whereas the inverted green ones have distances >200 pc. The red dot shows TOI-7149, which is the one of the coldest and reddest M-dwarfs to host one of these GEMS. We also overplot the PARSEC isochrones for a 5 Gyr system at +0.5, 0 and −0.5 dex metallicity (A. Bressan et al. 2012; Y. Chen et al. 2014). The white strip and black arrows indicate the upper edge of the convective transition between partially and fully convective M-dwarfs (W.-C. Jao et al. 2018). The full extent of the CMD is shown on the left, whereas on the right we zoom into the region near the transition zone to show other similar stars to TOI-7149.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: The 3D f(ρ, Sp, M*) distribution conditioned on different stellar masses and Sp = 50 S⊕ (the median insolation flux for transiting GEMS), to estimate the 1D distribution for f(ρ∣Sp = 50 S⊕, M*). In other words, these plots show the probability distribution of bulk densities of transiting giant planets at 50 S⊕ across different stellar masses (shown in different colors). The left plot shows the distribution for all the giant planets in our sample. The middle and right plots show similar distributions after excluding planets >4 MJ and >2 MJ from the sample. Takeway: We find that when excluding super-Jupiters (>2 MJ), the bulk density of transiting warm Jupiters (∼50 S⊕) does not show a strong dependence on host-star mass.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: The gray bar shows the 1σ radius measurement along with age estimates >1 Gyr. The different color cooling tracks generated from planetsynth assume the minimum atmospheric metallicity of solar (1.2%) and different bulk metallicities. Takeaway: The measured radius for TOI-7149 b is inconsistent with theoretical model predictions, thereby suggesting that it is inflated.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: Top: GLS of the HPF RVs in blue, with the dashed vertical line showing the planetary orbital period. The horizontal lines are the 10%, 1%, and 0.1% false alarm probability levels. There is a peak in the RV periodogram, corresponding to the orbital period, that is significant at the <0.1% level. Middle: GLS of the residuals obtained after subtracting the best-fit model do not display any significant peaks. Bottom: Window function of the HPF RVs showing the characteristic 1.0 day peak indicative of observing cadence at HET.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: Overlaying the tglc 3 × 3 pixel aperture for all sectors (red) on a 11 × 11 TESS pixel footprint for all sectors. The blue grid is the 11 × 11 footprint for Sector 79. TOI-7149 is shown as a red star. Stars with ∣ΔGRP∣ < 4 contained in the footprint are colored by their ΔGRP mag, showing the crowded field. The background image is from ZTF zi around 2018.5 (F. J. Masci et al. 2019).
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: 5σ contrast curve for TOI-7149 observed from NESSI in the Sloan ﹩{r}^{{\prime} }﹩filter and ﹩{z}^{{\prime} }﹩filter showing no bright companions within 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 from the host star. The ﹩{z}^{{\prime} }﹩ image is shown as an inset 1″ across.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: Simulated emission spectrum of TOI-7149 b, also showing the instrument bandpasses for JWST NIRSpec and MIRI, along with ARIEL.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: A 2D analysis showing the expectation value for f(ρ∣M*) as well as bootstrapped uncertainties. Similar to Figure 12, we see that the sample of warm Jupiters <160 S⊕ (blue; Teq ∼ 1000 K) have bulk densities that appear to show a stellar mass dependency. This disappears when considering a sample of planets below <2 MJ (green), suggesting different formation or evolution mechanisms across these two subsamples with contrasting stellar mass dependence. In pink, we also show the super-Jupiters >2 MJ. The large bootstrap uncertainty in this for the M-dwarfs (<0.6M⊙ ) is driven by the number of super-Jupiters around M-dwarfs (<5). Since the relative number of super-Jupiters to Jupiters increases with increasing stellar mass (Figure 7), the bulk density of the combined sample (blue curve) shows a stellar mass dependence, whereas intrinsically the <2 MJ do not.
Paper: Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Andrea S.J. Lin, Henry A. Kobulnicky, Ian Karfs, Alexina Birkholz, Andrew Monson, Arvind F. Gupta, Mark Everett, Michael Rodruck, Rowen I. Glusman, Te Han, William D. Cochran, Chad F. Bender, Scott A. Diddams, Daniel Krolikowski, Samuel Halverson, Jessica Libby-Roberts, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gud̃mundur Stefánsson
Figure caption: The expectation values for the planetary bulk density as a function of stellar mass for warm Jupiters (50 S⊕), with the shaded regions representing the 16th–84th percentile uncertainty from bootstrapping the samples. The dashed horizontals line show the density of Jupiter and Saturn for reference. We do not display the stellar masses above the Kraft break due to a potential observational bias related to v sin i and measuring planet masses with RVs. Takeaway: For warm Jupiters unaffected by anomalous inflation (D. P. Thorngren & J. J. Fortney 2018), the giant planet bulk densities offer a probe into their heavy-element content, and appear to be independent of host-star mass when super-Jupiters are excluded.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The J − K distribution for M31. The smallest squares represent the initial pixel unit, and the irregular polygon including multiple pixel units of the same color denotes one final bin with about 300 stars by the Voronoi binning methods. In total, there are 1832 bins.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: Distribution of J − K for a galactocentric radius of 0–24 kpc in M31. The top panel is for no-extinction data. The first four points are fitted to get the red straight line, and the red dotted line is fitted to the open red circles. The black bar represents the dispersion. There are two bumps at 11.5 and 14.5 kpc. The color plus sign is the dust ring position given in different works. The bottom panel is for half-extinction data.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The same as Figure 2, but for M33 and there are 263 bins.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: Distribution of dust rings in M31. Red and green represent the position of the 14.5 kpc dust ring and the 11.5 kpc dust ring, respectively. The black dots are the distribution of Sample-R-M31.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The J − K vs. K diagram of M31 and M33 member stars. The dashed line indicates the area used to determine the color and brightness of TRGB. The black dots indicate the TRGB positions derived in Section 4.1.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: J − K gradient for the north and south regions in M33. Red represents the north, and green represents the south. Black dots are within 2σ.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The variation of the J − K with RGC from the galactic center in M31. The red line is fitted to the red points, and the blue line to the blue points.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: J − K gradient for the east and west regions in M33. Green represents the east and red represents the west.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption:  ﹩\overline{E(B-V)}﹩ calculated for bins of absorber redshift. Bins are 0.04 units wide and the results are plotted for associated (voff  <  3500 km s−1) and intervening (voff  >  3500 km s−1) absorption systems, as well as for the sample of control QSOs.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption:  ﹩\overline{E(B-V)}﹩ calculated for bins of W﹩{}_{0}^{\lambda 2796}﹩. Bins are 0.2 Å wide and the results are plotted for both associated (voff  <  3500 km s−1) and intervening (voff  > 3500 km s−1) systems.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption: Visualization of our extinction-fitting process. Top: an example QSO spectrum with an absorber plotted alongside the blue QSO template, both shifted into the rest frame of the absorption system. Masked regions, including the edges of the spectrum as well as the emission and absorption lines, are shown in gray. Note that the template spectrum has been scaled arbitrarily. Bottom: The result of the fitting process, showing that the reddened template with E(B − V) = 0.114 is a good fit to the unmasked data from the top panel.