adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Quasiperiodic Pulsations in Solar and Stellar Flares with a Neural Network
Authors: Sergey A. Belov, Dmitrii Y. Kolotkov, Valery M. Nakariakov, Anne-Marie Broomhall
Figure caption: The graphical interface of the browser application for the FCN-based QPP detection in the flare lightcurve data.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Linkage between master sources, stacked observation detections, and per-observation detections in CSC 2. Master sources and stacked observation detections are linked uniquely when the stacked observation detection is associated with a single master source, whereas they are linked ambiguously if the stacked observation detection can be associated with more than one master source. A nondetection linkage implies that no source was detected at the location of a known master source in the associated stacked observation. Source detection is performed at the stacked observation detections level. In this example, master source I is linked uniquely to stacked observation detection A and linked ambiguously to stacked observation detection B. Per-observation (individual observation) detections 1 and 2 will contribute to master source I source properties, whereas per-observation detection 3 will provide a photometric upper limit at the epoch of that observation. Master source II is linked uniquely to stacked observation detections C and D, linked ambiguously to stacked observation detection B, and has a nondetection linkage to stacked observation detection E. Per-observation detections 4, 5, 6, and 7 will contribute to master source II’s source properties, and per-observation detection 3 will provide a photometric upper limit at the epoch of that observation. Since no source was detected at the location of stacked observation detection E, per-observation detection 8 is defined to be a local PSF-sized region that will be used to compute a photometric upper limit at the epoch of that observation. For more information on linkage, see the details in the description of the Master Source/Stacked Observation Detection Associations table in the text. The algorithm used to match stacked observation detections to identify master sources is described in Section 3.9.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Example detect, valid, and likely stacks for six candidate detections (“A”–“F”) identified in a stack of three observations (ObsIDs 1–3) shown in red, blue, and green, respectively. The field edges are shown by the solid lines while the dashed lines identify the pixel mask edges. Pixels that fall outside of the pixel mask are considered invalid. The light curves for each candidate detection are shown beneath the respective ObsID labels. Candidate detection “A” is valid in all three observations, but because the source is bright only in ObsID 2 the likely stack for that detection only includes ObsID 2. Detection “B” is only valid in ObsID 1 because it falls outside the field of view of the other observations in the stack. Detection “C” falls within the field of view but off the pixel mask for ObsID 2, and so that observation is excluded from the valid stack. Detection “D” is a bright source that is saturated in ObsIDs 1 and 2; the readout streaks emanating from the source in these ObsIDs are marked invalid by the pixel mask, although the pixel mask streak cutouts are broken around the bright source itself. Detection “E” falls on the pixel mask streak cutout for the bright source “D” in ObsID 2 and so that observation is excluded from the detection’s valid stack; since the source is only bright in ObsID 1, only that observation is included in the likely stack. Finally, detection “F” falls outside the pixel masks (but within the fields of view) for all three observations, and so the corresponding valid stack is empty; this detection will not be present in the catalog.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: The upper panels show CSC 2.0 detections in stack acisfJ0956451p284947_001, which includes a single observation, color coded by master source significance (left) and master source broadband flux (right). The corresponding plots for the modified stack in CSC 2.1, acisfJ0956451p284947_002, which includes five observations, are shown in the lower panels. While the gain in the total number of detections is clearly evident, some detections present in CSC 2.0, for example at approximately (α, δ) = (149.42, 28.79), are no longer detected in CSC 2.1. This is due to the detection thresholds (see Section 3.7.2) changing as a result of the newly added observations.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: High-level flow of the catalog-processing steps. The references identify the relevant sections of the text that describe the methods and algorithms used.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Voronoi tessellation of a region containing both source and background events. Voronoi polygons with areas α < α thresh (blue) are identified with sources. Merging Voronoi source polygons yields nonconvex source polygons (red).
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Sky coverage of release 2.1 of the CSC. The ordinate value is the total sky area included in the CSC that is sensitive to point sources with fluxes in any energy band at least as large as the corresponding value on the abscissa.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Distribution of CSC release 2.1 master sources on the sky, in Galactic coordinates.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Robust photometric and variability parameters vs. redshift for 0.298 million Gaia CRF quasars. The black dots connected with step lines are the median values for each bin of the sample sorted by z. The orange dots show the 0.16–0.84 quantile dispersion limits corresponding to ±1σ interval. Left: median G BP−G RP color. Middle: Spearman’s correlation ρ(G, BP−RP). Right: Spearman’s correlation ρ(BP, RP).
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Empirical dependence of Spearman’s correlation coefficients ρ(G, BP − RP) on variability amplitude smad(﹩\hat{G}﹩) (left panel) and ρ(BP, RP) on the median (BP−RP) color (right panel) for the brighter subset of Gaia CRF3 with ﹩\hat{G}\lt 19.6﹩ mag. The black dots connected by a step line show the median values for each bin of sorted data. The orange dots show the 0.159 and 0.841 quantiles of the values for each bin, which correspond to the ±1σ width of the sample distribution.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Gaia DR3 light curve of the extreme-flaring FSRQ blazar QSO J2232+1143 = IERS B2230+114, which is also part of the ICRF3. The filtered measurements that have been accepted in this analysis are shown with black dots. The quality flags in Gaia discard a genuine flare event around MJD = 57750, when the source was brighter than G = 12 mag. Blue circles represent the discarded Gaia measurements with noisyFlag=1. Ground-based photometric measurements from (Liodakis et al. 2019) in the R band are shown with magenta dots.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Histograms of robust variability parameters in G for the ICRF3 subset of Gaia CRF3. Left panel: dispersion of measured magnitudes smad ﹩(\hat{G})﹩. The red curve is copied and renormalized from Figure 1 to facilitate visual comparison with the general sample. Right panel: normalized dispersion of measured magnitudes ﹩\hat{Z}﹩.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Gaia DR3 light curves in G magnitude of two sources from the MVO sample with the highest Spearman’s correlation value 0.9996.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Robust photometric and variability parameters vs. redshift for 0.298 million Gaia CRF quasars. The black dots connected with step lines are the median values for each bin of the sample sorted by z. The orange dots show the 0.16–0.84 quantile dispersion limits corresponding to the ±1σ interval. Left: variability amplitude in G magnitude. Middle: variability amplitude in G RP magnitude. Right: variability amplitude in G BP−G RP color.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Histograms of Spearman’s correlation coefficients ρ(G, BP − RP) (left panel) and ρ(BP, RP) (right panel) for the brighter subset of Gaia CRF3 with ﹩\hat{G}\lt 19.6﹩ mag.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Left panel: Distribution of [Mn/Fe] vs. [Cr/Fe] for our sample stars and stars from the literature, including I. U. Roederer et al. (2014b), R. Ezzeddine et al. (2020), and D. Yong et al. (2013), shown as a density plot. The darker colors indicate a higher density of points in the parameter space; lighter colors indicate a lower density of points. The symbols are the same as in previous figures. Right panel: Trend for Δα = (([Ca/Fe] + [Si/Fe] + [Ti/Fe])/3 − [Mg/Fe]), as a function of [Mg/Fe]. Our sample stars are color coded by metallicity (see color bar at right). The sample of metal-poor halo stars from JINAbase (A. Abohalima & A. Frebel 2018), which includes I. U. Roederer et al. (2014b), R. Ezzeddine et al. (2020), and D. Yong et al. (2013), are shown with gray dots. The theoretical yields of CCSNe and HNe are from K. Nomoto et al. (2013).
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Distribution of the odd-Z light elements Na and Al, as a function of metallicity, [Fe/H]. The red stars denote the LTE abundances of the stars in this study; filled downward-black triangles represent the derived upper limits. The individual elements are marked on the panels. The sample of stars from JINABASE (A. Abohalima & A. Frebel 2018), including D. Yong et al. (2013), I. U. Roederer et al. (2014b), C. M. Sakari et al. (2018), and R. Ezzeddine et al. (2020), are shown with gray dots. The Mg-poor VMP stars, and the globular cluster escapee are marked in blue and green, respectively. Typical error bars are indicated at the bottom right in each panel.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Distribution of carbon, as a function of metallicity, [Fe/H]. The red stars denote the abundances of the stars in this study. The sample of stars from JINABASE (A. Abohalima & A. Frebel 2018), including D. Yong et al. (2013), I. U. Roederer et al. (2014b), C. M. Sakari et al. (2018), T. T. Hansen et al. (2018), R. Ezzeddine et al. (2020), and E. M. Holmbeck et al. (2020), are shown with gray dots. The blue-dashed line indicates the level above which stars are considered to be CEMP stars. The Mg-poor VMP stars, and the globular cluster escapee are marked in blue and green, respectively. Typical error bars are indicated at the bottom right in the panel.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Example spectral synthesis for the region of the molecular CH G-band. The red line shows the best-fit synthetic spectrum to the data (black dots). The blue and green lines mark deviations by ±0.25 dex. The black line corresponds to the absence of carbon.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Distribution of the Fe-peak elements formed by incomplete Si burning, as a function of metallicity, [Fe/H]. The symbols are the same as in Figure 6. Typical error bars are indicated at the bottom right in each panel.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Distribution of the α-elements Mg, Si, Ca, and Ti, as a function of metallicity, [Fe/H]. The symbols and sources of literature data are the same as in Figure 7. Typical error bars are indicated at the bottom right in each panel.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Distribution of the neutron-capture element abundances for Sr, Ba, and Eu, and the ratio [Sr/Ba], as a function of metallicity, [Fe/H]. The symbols are the same as in Figure 6. The error bars are indicated at the bottom right in each panel. The red- and blue-dashed lines represent the limit for the r-II stars at [Eu/Fe] = +0.7, and r-I stars at [Eu/Fe] = +0.3, respectively.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Example spectral syntheses for lines of key r-process elements Sr, Ba, and Eu for 2MASS J02462013−1518418, 2MASS J06321853+3547202, and 2MASS J09143307+231544, which are r-II, r-I, and EMP stars, respectively. The red line indicates the best-fit synthetic spectrum; blue and green lines mark deviations by ±0.20 dex. The black line corresponds to the absence of the given element.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Comparison of the derived abundances for 2MASS J02462013-1518418 from this study marked in red, and compared to the derived abundances from T. T. Hansen et al. (2018) and C. M. Sakari et al. (2018) in green and blue, respectively.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Number of candidate detections per detection bundle for CSC 2.0 observation stacks. Approximately ∼96.1% of the detection bundles include only a single candidate detection, and ∼99.97% of the detection bundles include five or fewer candidate detections.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Histogram of the total radial astrometric correction relative to the Gaia-CRF3 reference frame for all observations included in CSC 2.1, computed by combining the individual observation relative astrometry corrections with the stack absolute astrometry corrections. The short-dashed red histogram reflects the distribution for which the observation stack absolute astrometry corrections were computed from matches with the Gaia reference catalog that were modified by human review (i.e., man_astrom_flag = TRUE). The long-dashed blue histogram identifies cases where no observation stack absolute astrometric correction could be computed due to a lack of reliable X-ray source—Gaia optical source matches.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: MPDFs for ACIS the broad band's energy flux in seven observations contributing to master source 2CXO J004152.6–092213. The green, blue, and red curves represent the MPDFs for observations included in the three identified flux-ordered Bayesian Blocks. The flux-ordered block with the longest exposure time includes the observations in green. The black curve is the master source “best-estimate” MPDF, which combines data from all observations included in that block. The observations included in the remaining blocks shown in blue and red are photometric upper limits and so have exponential MPDFs.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Left: Chandra Level 2 event file for ObsID 6204, smoothed with a Gaussian kernel with a radius of 3 pixels. Right: DTFE background image for the same region constructed using the approach described. The background image contains a bright readout streak and the polygon containing the galaxy has been filled in with a relatively high uniform surface brightness. Both images are gray scale, showing pixel values in the range 0.001 (white) to 5 counts (black) on a logarithmic scale.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Left: source detection efficiency estimated from ACIS observations with exposure times ∼10 (red), 61 (green), and 122 ks (blue) as a function of the broad band's energy flux, for detections with off-axis angles ﹩\theta \leqslant 6^{\prime} ﹩. Typical error bars are indicated for each curve. Right: same, except for detections with off-axis angles ﹩\theta \gt 6^{\prime} ﹩.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: The function ﹩{ \mathcal L }+\mathrm{ln}(\gamma (B+n,B))﹩ varies smoothly with n and has a single root that can be easily determined numerically. Example plots of ﹩{ \mathcal L }+\mathrm{ln}(\gamma (B+n,B))﹩ as a function of source counts n are shown for two representative values of B and ﹩{ \mathcal L }﹩.