adsabs/AstroCLIMB huggingface dataset:
Paper: On the Decline of Star Formation during the Evolution of Galaxies
Authors: Adelheid Teklu, Rolf-Peter Kudritzki, Klaus Dolag, Rhea-Silvia Remus, Lucas Kimmig
Figure caption: The fraction of cold gas resolution elements with a given density for the highest mass bin, where the different colors and lines represent the different look-back times. The dashed line represents the threshold for star formation. Toward lower look-back times the peak shifts from high to low density, lying below the SF threshold at later times.
Paper: On the Decline of Star Formation during the Evolution of Galaxies
Authors: Adelheid Teklu, Rolf-Peter Kudritzki, Klaus Dolag, Rhea-Silvia Remus, Lucas Kimmig
Figure caption: The mean number of cold gas (top), star-forming (middle) resolution elements, and the fraction of star-forming to cold gas resolution elements (bottom) in each radial bin for the galaxies in the highest mass bin, where the different colors and lines represent the different look-back times.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The distributions of four parameters, including ﹩{G}_{\mathrm{pre}}-G﹩, ﹩\mathrm{log}({bp}\_{rp}\_{excess})﹩, ﹩\mathrm{log}({pos}\_{err})﹩, and ﹩\mathrm{log}({astrometric}\_{excess}\_{noise})﹩, which is written as ﹩\mathrm{log}({excess}\_{noise})﹩ in the fourth column. In the top panel, we plot the LAMOST stars with 2D histograms, while the LAMOST galaxies are plotted with green dots and the M31 GCs with orange diamonds. In the bottom panel, we plot the predicted point sources (P ext < 0.5) with 2D histograms and the predicted extended sources (P ext > 0.5) with red dots. We also plot the GC candidates with the dark cyan diamonds.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The candidates, the known GCs, and the galaxies in our 1562 visually checked sources are plotted in the P GC–D plane. In the middle panel, the triangles represent the candidates, with the different colors indicating their different types. The red squares show the distribution of the known GCs. The blue squares show the distribution of the known galaxies, which is also confirmed by our visual inspections. All of these sources get a P GC higher than 0.25. We use the visually checked galaxies here, because only 116 simbad-labeled galaxies have P GC > 0.25, even though we obtained over 4000 of them in total with P GC < 0.25. Thus, the galaxies used in this figure are the galaxies that are most likely recognized as GCs by our Clf2. The top panel shows the distance distribution of the known GCs and galaxies, while the right panel shows the distribution of P GC. The height of the histogram means the fraction of the sample in each bin. The colors of the bars in both the top and right panels refer to the same sample as the squares in the middle panel.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: Top: the Pan-STARRS g magnitude distributions of the different samples mentioned in Section 4.2. The blue and orange lines represent the LAMOST stars and LAMOST galaxies, respectively. The green and red lines represent the predicted point sources (P ext < 0.5) and extended sources (P ext > 0.5), respectively. Bottom: the color g − r distributions of the same four different samples in the top panel.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The spatial distribution of the candidates. Known GCs are depicted as gray dots, while triangles represent different types of candidates. The dark red dotted lines show circles with radii of 100 and 150 kpc, centered at coordinate (0, 0), which stand for the center of M31. The black ellipse indicates the disk of M31, also centered at (0, 0), with a major axis of 2°. Here, we adopt a major axis position angle of 38°, with an inclination angle of 78° (Wang et al. 2019). The irregular green dashed–dotted lines show the large-scale structures of M31 (copied from Figure 12 of McConnachie et al. 2018). Some GC candidates fall in several structures, which are listed in Table 12. The names of the structures are indicated in the upper right corner of the figure.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: Top: the contamination fraction varies with the cut of ﹩{G}_{\mathrm{pre}}-G﹩ in the predicted sample. The blue line shows the completeness with the left y-axis, while the red line shows the contamination fraction with the right y-axis. Bottom: the completeness of the extended sources varies with the cut of ﹩\mathrm{log}({bp}\_{rp}\_{excess})﹩. The blue line and the red line have the same meanings as in the top panel.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The blue histogram is the P ext distribution of the predicted extended sources (P ext > 0.5). The orange histogram shows a small number of the predicted extended sources, with ﹩{log}\_{bp}\_{rp}\_{excess}\lt 0.4﹩ and P ext > 0.5.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: PAndAS g-band images of the 50 candidates newly identified in this work. The size of each panel is 54 × 54 pixels, which is ﹩10.1\times 10.1\,{\mathrm{arcsec}}^{2}﹩. At the top left of each panel, we write the ID and type of the source. The position (J2000) of the source is shown at the bottom of the panel.
Paper: Searching for New Globular Clusters in M31 with Gaia EDR3
Authors: Yilun Wang, Haibo Yuan, Bingqiu Chen, Xinlei Chen, Hao Wu, Zexi Niu, Song Huang, Jifeng Liu
Figure caption: The distribution of the candidates (triangles) in the color–magnitude plane, together with the known GCs and known galaxies. The 2D histogram shows the distribution of known galaxies, which are labeled as “Galaxy” in simbad with P ext > 0.5. The gray dots are the known GCs.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: The density of detections in the MADGICS (this work, left) and Gaia 							(Schultheis et al. 2023, right) 8621 Å DIB catalog as a function of the DIB 							width (σ DIB) and its central wavelength (λ DIB). The color scale indicates density, where darker colors 							indicate more detections, and is a common logarithmic stretch for both 							catalogs. The (λ DIB, σ DIB) cuts imposed in defining the Gaia HQ sample are shown as 							a gray box, inside of which the HQ sample is shown. Outside of that box, 							the Gaia catalog is shown with only the stellar S/N, DIB S/N, and 							GSP-Spec flag cuts imposed. Guidelines for the central wavelength of the 							DIB and stellar lines are labeled and color coded between the plots. 							Stellar lines in magenta indicate lines not included or not well 							calibrated in the GSP-Spec line list, and the Gaia DIB detections 							preferentially cluster at those wavelengths, especially at low σ DIB. Because the MADGICS catalog inference marginalizes over 							a data-driven stellar model, it is free from detectable contamination 							from these stellar lines and provides a more robust characterization of 							the DIB properties.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Projections of the 4D DIB radial velocity map in (left) angular 									(ℓ, b) and (right) Cartesian (X, Y) Galactic 								coordinates. The inverse-variance weighted mean of ﹩{v}_{\mathrm{DIB}}^{\mathrm{LSR}}﹩  is shown in color, averaging over dimensions not 								shown.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Weighted least-squares linear fit of EWDIB vs. extinction to 							the background star as measured by Bayestar19 (Green et al. 2019) in the range 0 							< A  V  < 1. The color scale indicates EWDIB 							inverse-variance weighted number density, where darker colors indicate 							more (confident) detections and a log normalization has been applied. 							Scatter points represent inverse-variance weighted mean EWDIB 							for each Av bin.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Projections of the 3D DIB EW map in (left) angular (ℓ, b) and (right) Cartesian 								(X, Y) 							Galactic coordinates. The inverse-variance weighted mean of 								EWDIB is shown in color, averaging over dimensions not 							shown.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: (Top) The covariance matrix of high stellar S/N and low-dust spectra 								used as MADGICS prior for the stellar component. (Middle) Third 								eigenvector of the stellar covariance matrix. (Bottom) Zoom-in of 								the third eigenvector near the DIB feature. Guidelines for the 								central wavelength of the DIB and stellar lines are labeled and 								color coded. A higher-resolution solar spectrum from Kurucz et al. 									(1984) is 								plotted in orange for reference.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Histogram (2D) illustrating the correlation between the ﹩{v}_{\mathrm{DIB}}^{\mathrm{LSR}}﹩ and intensity-weighted velocity of the nearest CO 								component in the Dame et al. (2001) CO map. The color scale 								indicates density, where darker colors indicate more detections and 								a logarithmic stretch has been applied.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Scatter plot of ﹩{v}_{\mathrm{DIB}}^{\mathrm{LSR}}﹩ for DIB detections with DIB S/N >5.5 overlaid 								on longitude–velocity diagram of CO emission from Dame et al. (2001), integrated 								over b (color bar, top). Scatter 								points are colored by the distance to the background star (color 								bar, right).
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Histograms (2D) in the space of GSP-Spec stellar parameters for all 							(left) and training (middle) spectra. (Right) The overall “goodness of 							fit,” measured by how close χ 2/dof is to 1, is shown. Each pixel is the median of ﹩{\mathrm{log}}_{10}({\chi }^{2}﹩/dof), which is zero in the ideal case.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Scatter plot showing residuals after fitting λ LSR vs. ﹩{\ell }^{\prime} ﹩ and d where the 								color shows the weighting of each point in the fit. Only detections 								such that ﹩| {\ell }^{\prime} | \lt 10^\circ ﹩, ∣b∣ < 10°, and 									d < 3 kpc are shown. Our 								derived rest-frame wavelength of λ rest = 8623.14 ± 0.087 Å is bluer than Schultheis et al. 									(2023), but 								our updated value is validated in Figure 8 by comparison with CO gas 								velocities.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Histograms (2D) showing projections of the MADGICS catalog in the space 							of moment-0, moment-1, moment-2, and DIB S/N. The color scale indicates 							density, where darker colors indicate more detections, and each panel 							has its own logarithmic stretch.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Example MADGICS decomposition of Gaia RVS spectrum under a star + 								residual (red) and star + DIB×star + residual model (black).
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Residual components, sorted by stellar S/N, divided by the stellar 							component, and averaged over 32 adjacent spectra. The bottom panel shows 							the value of stellar S/N along the sorted axis.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: The median of the DIB width σ DIB as a function of the DIB S/N and the extinction along the 							line of sight in the Bayestar19 3D dust map (Green et al. 2019). The weak 							correlation could be due to the presence of multiple cloud components at 							different velocities along the line of sight and/or the presence of 							velocity structure within individual clouds.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Histograms (2D) for DIB models as a function of EWDIB, λ DIB, σ DIB, and stellar S/N in the columns, left to right 							respectively. The λ DIB is reported relative to the reference center of the 							MADGICS parameter grid. Positive EWDIB indicates absorption. 							The rows show this distribution for (top) the total χ 2 per degree of freedom of the component fit, the negative 							change in χ 2 as a result of adding the DIB component before (middle) and 							after (bottom) imposing cuts on ﹩{\chi }_{\mathrm{tot}}^{2}/\mathrm{dof}﹩. Guidelines indicate cuts imposed in each space. The 							color scale indicates density, where darker colors indicate more 							detections, and each panel has its own logarithmic stretch.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Histograms illustrating the bias of DIB detections relative to reported 							uncertainties (Z-scores) for injection tests where ground truth is 							known. Histograms are a function of injected EWDIB, injected 								λ DIB, injected σ DIB, stellar S/N and DIB S/N in the rows, and show the bias 							in the recovered quantities EWDIB, λ DIB, σ DIB in the columns (left to right). The λ DIB is reported relative to the reference center of the 							MADGICS parameter grid. The color scale indicates density, where darker 							colors indicate more detections, and each panel has its own logarithmic 							stretch. Dashed guidelines provide a reference for 0 and ±1σ. Solid lines indicate the center (red) and 							spread (white) of the Z-score distribution.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: The density of detections in the MADGICS (left) and Gaia (right) 8623Å 							DIB catalog as a function of λ DIB and σ DIB, removing cuts imposed on the goodness of fit of the 							model to the overall spectrum. This removes the second block of cuts in 							Table 1 for both 							catalogs. The Gaia catalog shown is the full DIB sample, including DIB 							detections in the public Gaia DR3 DIB catalog that were identified on 							spectra that are not public. The color scale indicates density, where 							darker colors indicate more detections, and is a relative logarithmic 							stretch for both catalogs, with the maximum rescaled by relative catalog 							sizes. Guidelines for the central wavelength of the DIB and stellar 							lines are labeled and color coded between the plots.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Median change in EWDIB as a function of EWDIB and 							DIB S/N after including dustier lines of sight in the training data for 							the stellar covariance. Green indicates >25% of detections not found, 							gray indicates detections not found with the clean stellar covariance, 							and dark gray indicates no injection tests present. The guideline 							(magenta, dashed) indicates the detection cut on the estimated DIB S/N 							imposed in making the MADGICS catalog.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: (Top) Cumulative counts of MADGICS DIB detections as a function of DIB 							S/N. (Bottom) 2D histogram of MADGICS DIB detections as a function of 							DIB and stellar S/N. The color scale indicates density, where darker 							colors indicate more sources, and is a logarithmic stretch. A guideline 							is shown at stellar S/N 70, which is the cutoff imposed by the Gaia DIB 							catalog.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Histogram (2D) illustrating the correlation between the ﹩{v}_{\mathrm{DIB}}^{\mathrm{LSR}}﹩ and intensity-weighted velocity of CO over all 							velocity channels in the Dame et al. (2001) CO map. The color scale indicates 							density, where darker colors indicate more detections and a logarithmic 							stretch has been applied.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: (Top) Histogram of public Gaia RVS sources with respect to stellar S/N. 							(Bottom) 2D histogram of public Gaia RVS sources with respect to stellar 							S/N and the mean normalized flux in the RVS spectrum. The color scale 							indicates density, where darker colors indicate more sources, and is a 							logarithmic stretch. A guideline is shown at stellar S/N 70, which is 							the cutoff imposed by the Gaia DIB catalog.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: The density of public RVS spectra on the sky (left, HEALPix grid at 							NSide=64) and projected onto the Galactic plane in Cartesian coordinates 							(right).
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Fractional detection bias determined by injection tests for 								EWDIB (top) and σ DIB (bottom) as a function of the true DIB S/N and true 								σ DIB.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: (Top) Velocity shift in the stellar rest frame as measured from the 							MADGICS residuals by comparing the magnitude a fit of a Lorentzian 							derivative to a Lorentzian fit of the stellar component of the spectra. 							(Bottom) Measurements of the average shift in the core of the Ca triplet 							lines using Lorentzian fits to Gaia data alone. Zero velocity reference 							arbitrarily chosen to be the (stellar S/N, ﹩\mathrm{log}g﹩) ≈(150, 2) bin. A comparison shows MADGICS residuals 							are sensitive enough to show small velocity shifts below the reported 							precision in Gaia radial velocities that are present in the data 							themselves.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Estimated true positive (TP) and false positive (FP) rates as a function 							of DIB S/N cut using the injection tests and stellar training set, 							respectively (solid lines). Estimated TP and FP rates using a broader 							set of low reddening injection tests/spectra are shown in dotted–dashed 							lines. Vertical guideline illustrates the value chosen in this work 							(gray, dashed).
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Estimated completeness of DIB catalog as a function of EWDIB 							and σ DIB based on quality cuts on injection tests.
Paper: Measuring the 8621 A Diffuse Interstellar Band in Gaia DR3 RVS Spectra: Obtaining a Clean Catalog by Marginalizing over Stellar Types
Authors: Andrew K. Saydjari, Ana Sofía M. Uzsoy, Catherine Zucker, J. E. G. Peek, Douglas P. Finkbeiner
Figure caption: Posteriors for pixels within either the DIB component C DIB or stellar component C stellar. Covariance between pixels spanning the two 							components is shown as the cross terms C DIB,stellar and C stellar,DIB.