adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Top row (left to right) partial pressure retrieval model N2 and CO posteriors. Bottom row (left to right) VMR adapted partial pressure retrieval model N2 and CO posteriors. Red marginal distributions represent abundances from N2-dominated retrievals and blue distributions represent abundances from CO-dominated retrievals. The gas’ true value lines are overplotted for each retrieval illustrated with the same color as its retrieval. The left column presents N2 abundances for both retrievals with CO abundances shown in the right column. Both models are able to constrain our defined background gas and the trace gas has an abundance ceiling that trades with the background gas.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: True N2-dominated planet-to-star flux ratio spectrum with an assumed S/N = 20 (red) plotted against 1000 randomly sampled retrieved spectra with 95% confidence intervals. The blue spectrum is the median spectrum created from the 1000 plotted model runs that make up our confidence interval.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Gas-only corner plots (other retrieved parameters not shown) of our nominal N2-dominated partial pressure retrieval and the CO-dominated partial pressure retrieval. Gas abundances are represented by their log10 pressure in Pa. (a) Partial pressure gas-only corner plot w/N2 as BG. (b) Partial pressure gas-only corner plot w/CO as BG.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Comparison of the nominal N2-dominated atmosphere and trading off VMRs of CO with N2. The ∼1.6 μm CO absorption feature is needed to distinguish between N2 and CO backgrounds.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Corner plots for our partial pressure retrievals at S/N 10, 20, and 40. All plots are shown with the gas’ log10 VMR values in Pa.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: True CO-dominated atmosphere planet-to-star flux ratio spectrum (red) plotted against 1000 randomly sampled retrieved spectra with 95% confidence intervals (blue area).
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The NIR spectrum of RW Cep made during the dimming event (from APO; shown in black) compared to an archival spectrum associated with normal brightness (from the IRTF Spectral Library; shown in dark gray). A model BT-Dusty spectrum is shown (light gray) with an offset of −0.5 × 10−11 erg s−1 cm−2 Å−1 (see Section 4). All the spectra are rebinned to a resolving power of R = 1000 for ease of comparison.
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The H-band (top left) and K-band (top right) images of RW Cep made using the SQUEEZE algorithm. The color bar at right shows the correspondence between broadband specific intensity (normalized to the brightest pixel) and image color. The lower panels show the corresponding images reconstructed from the same (u, v) sampling of a model image of a limb-darkened star.
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The H-band (left) and K-band (right) images of RW Cep made using the OITOOLS (top), and SURFING (bottom) algorithms based upon fitting the specific intensity within the stellar disk only. The color bar at right shows the correspondence between broadband specific intensity (normalized to the brightest pixel) and image color.
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The NIR spectrum of RW Cep near the CO bandhead made during the dimming event (from APO; shown in black) compared to an archival spectrum associated with normal brightness (from the IRTF Spectral Library; shown in dark gray). Both spectra are rebinned to a resolving power of R = 1000 for ease of comparison. The dotted line in the lower panel shows the difference (new minus archival).
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The SED of RW Cep. The bright state fluxes are indicated by plus signs and triangles, and only the former were used for the fit of the model photospheric spectrum (solid line). The diamonds depict the estimated fluxes during the current faint state (see Table 2), and the dotted line shows the model photospheric fit for the faint state. See Figure 1 from Jones et al. (2023) for the longer wavelength part of the SED.
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The spatial frequency coverage in the (u, v) plane for the H-band (left) and K-band (right) observations. The lower color legends show the corresponding wavelength channels.
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The H-band visibilities (left) and CPs (right) for the telescope pair and triplet MIRC-X observations of RW Cep. The black symbols with vertical error bars are the measurements and the red dots represent the corresponding fits from the SQUEEZE reconstructed images. The lower panels show the residuals from the SQUEEZE fits. The fits from the OITOOLS and SURFING reconstructions yield residuals that are qualitatively similar in appearance.
Paper: The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Narsireddy Anugu, Fabien Baron, Douglas R. Gies, Cyprien Lanthermann, Gail H. Schaefer, Katherine A. Shepard, Theo ten Brummelaar, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Claire L. Davies, Jacob Ennis, Tyler Gardner, Aaron Labdon, Rachael M. Roettenbacher, Benjamin R. Setterholm, Wolfgang Vollmann, Costantino Sigismondi
Figure caption: The K-band visibilities (left) and CPs (right) in the same format as Figure 3.
Paper: The Dependence of Iron-rich Metal-poor Star Occurrence on Galactic Environment Supports an Origin in Thermonuclear Supernova Nucleosynthesis
Authors: Zachary Reeves, Kevin C. Schlaufman, Henrique Reggiani
Figure caption: Occurrence of IRMP stars as a function of metallicity in different environments. For the Milky Way field, dSph, and Magellanic Cloud samples we plot the posterior medians of occurrence as solid lines and the ranges defined by the 16th and 84th percentiles of the occurrence posteriors as transparent polygons. For the globular cluster sample for which we infer an upper limit on iron-rich metal-poor (IRMP) occurrence, we plot the 68th percentile of the posterior as a solid line and the range defined by the 0th and 68th percentiles of the occurrence posterior as a transparent polygon. There is no obvious dependence of IRMP occurrence on metallicity in the Milky Way’s field population, its globular clusters, its classical dSph galaxies, or the Magellanic Clouds.
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: Simulated spectra of the two Proterozoic-Earth-like scenarios considered in this study.
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: Effect of the lower wavelength cutoff of the UV band on the pdf’s of O2 and O3 for the Proterozoic-Earth-like scenario with 1% of modern Earth’s O2. The results of the retrieval do not change appreciably. The constraints are moderately affected as the distributions are broadened. Blue curves correspond to the results shown in Table 2, with the default 0.2 μm UV lower bound.
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: Simulated data and best-fit retrievals for the Proterozoic-Earth-like scenario with 0.1% of modern Earth O2. VIS/UV/NIR spectrum predicted when fitting: VIS data only (blue curve), UV+ VIS data only (orange curve, same as blue curve, except in the UV), VIS + NIR data only (green curve), UV + VIS + NIR data only (red curve, same as green curve, except in the UV).
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: Simulated data and best-fit retrievals for the Proterozoic-Earth-like scenario with 1% of modern Earth O2. VIS/UV/NIR spectrum predicted when fitting: VIS data only (blue curve), UV+ VIS data only (orange curve, same as blue curve, except in the UV), VIS + NIR data only (green curve), UV + VIS + NIR data only (red curve, same as green curve, except in the UV).
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: Absorption features of different gases in the UV wavelength band. In particular, O3, SO2, and H2S absorption features are compared.
Paper: Reflected Spectroscopy of Small Exoplanets. III. Probing the UV Band to Measure Biosignature Gases
Authors: Mario Damiano, Renyu Hu, Bertrand Mennesson
Figure caption: Similar to Figure 4, but for the scenario with 0.1% modern Earth O2.
Paper: Systematically Measuring Ultradiffuse Galaxies (SMUDGes). IV. Ultradiffuse Satellites of Milky Way Analogs
Authors: Hina Goto, Dennis Zaritsky, Ananthan Karunakaran, Richard Donnerstein, David J. Sand
Figure caption: Comparison of the average cumulative satellite luminosity function for local MWAs (data from Bennet et al. 2019 and references thererin; see text) in blue and our measurements for UDG satellites of MWAs in the nearest redshift slice in red. At a given luminosity, over the range of our measurements, UDG satellites are typically about ∼10% of the total number of satellites.
Paper: Systematically Measuring Ultradiffuse Galaxies (SMUDGes). IV. Ultradiffuse Satellites of Milky Way Analogs
Authors: Hina Goto, Dennis Zaritsky, Ananthan Karunakaran, Richard Donnerstein, David J. Sand
Figure caption: UDG satellite luminosity function. We present the number of UDG satellites within 1 magnitude bins as derived from our three redshift slices. The results for the nearest slice (4500 < cz/(km s−1) < 5500) are represented by the black line, while those of the other two slices are represented by blue circles and gray squares, with the squares representing the farthest of the three slices. Horizontal bars represent the bin widths, while vertical error bars are statistical uncertainties. Units for ΔS UDG, are number per MWA per magnitude.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Our nominal N2-dominated model reflectance spectrum compared with spectra generated by swapping atmospheric species abundances with our background N2 abundance (mixing ratio of 0.78). An Earth-like atmospheric composition is assumed, except for the swapped dominant species. (a) Nominal N2-dominated spectrum vs. non-carbon-based atmospheric gas-dominated spectra. (b) Nominal N2-dominated spectrum vs. carbon-based atmospheric gas-dominated spectra.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: The time constants estimated during DD2 and DD8 subjected to different solar ionizing fluxes. The red solid and dashed–dotted lines represent the chemical and diffusion time constants for ﹩{{\rm{O}}}_{2}^{+}﹩, whereas the blue lines represent the same time constants for O+. The black solid line in each panel shows the magnetic diffusion time constant for comparison. The stars and squares indicate the PCE boundaries (the diffusion time constant becoming comparable to the chemical time constant) and the magnetic frozen boundaries (the magnetic diffusion time constant becoming comparable to the ion diffusion time constant), respectively.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: The time constants estimated during DD2 and DD8 subjected to different solar ionizing fluxes. The red solid and dashed–dotted lines represent the ion–neutral and ion–ion collision time constants for ﹩{{\rm{O}}}_{2}^{+}﹩, whereas the blue lines represent the same time constants for O+. The dashed lines show the ion gyroperiods for comparison. The triangles and circles indicate the ion collision boundaries (the ion–ion collision time constant becoming comparable to the ion–neutral collision time constant) and the ion gyration boundaries (the gyroperiod becoming comparable to the ion–ion collision time constant), respectively.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: Similar to Figure 1 but for the local time variations of different time constants (ion chemical and diffusion time constants, magnetic diffusion time constants) based on the estimates made during four DD campaigns: DD8 for the dayside, DD7 for the duskside, DD6 for the nightside, and DD5 for the dawnside. The upper left panel is identical to the right panel of Figure 1.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: Similar to Figure 1 but for the magnetic control of different time constants (ion chemical and diffusion time constants, magnetic diffusion time constants) based on the estimates made for DD8 and DD9, respectively, characterizing the weakly and strongly magnetized regions of Mars. The left panel is identical to the right panel of Figure 1.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: The species-dependent variations of different boundary altitudes discussed in this study, including the PCE boundary (red), the magnetic frozen boundary (blue), the ion collision boundary (green), and the ion gyration boundary (black). The displayed variations are specific for the DD8 campaign, but the variations obtained for the remaining campaigns are comparable.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: Similar to Figure 2 but for the local time variations of different time constants (ion–neutral and ion–ion collision time constants, ion gyroperiods) based on the estimates made during four DD campaigns: DD8 for the dayside, DD7 for the duskside, DD6 for the nightside, and DD5 for the dawnside. The upper left panel is identical to the right panel of Figure 2.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: Similar to Figure 2 but for the magnetic control of different time constants (ion–neutral and ion–ion collision time constants, ion gyroperiods) based on the estimates made for DD8 and DD9, respectively, characterizing the weakly and strongly magnetized regions of Mars. The left panel is identical to the right panel of Figure 2.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: The density profiles of neutrals (solid lines), including CO2, O, CO, and N2, and ions (dashed lines), including ﹩{{\rm{O}}}_{2}^{+}﹩, O+, CO2 +, NO+, and HCO+, averaged over each campaign.
Paper: Characteristic Timescales for the Dayside Martian Ionosphere: Chemistry, Diffusion, and Magnetization
Authors: Yutian Cao, Jun Cui, Wenjun Liang, Xiaoshu Wu, Haoyu Lu
Figure caption: The neutral, ion, and electron temperature profiles averaged over each campaign.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: Posteriors of H 0 derived for four different LOSs (D 1 and D 2) in the MICEcat simulations, and for two different sky areas (1° and 5° opening angle for D 1x  and D 2x , respectively) around those directions. The top, middle, and bottom panels assume a standard deviation on the luminosity distance that is 10%, 20%, and 30% of the luminosity distance, respectively. All the posteriors are the result of combining 200 GW events and assuming galaxy redshift is perfectly known. We do not find a bias. Note that any particular choice of the random seed used for the simulation will lead to fluctuations of the posteriors around the true value. However, by performing several simulations one should find that these fluctuations are compatible with the confidence levels at which the true value is found (see the discussion about PP plots in the text).
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: GW detection probability computed with the toy likelihood model in Equation (22) as a function of the true luminosity distance. The colors indicate various fractional errors on the luminosity distance. The vertical dashed line indicates the detection threshold for the measured luminosity distance, ﹩{\hat{d}}_{L}﹩. We note that the detection probability only reduces to a Heaviside step function in the limit of ﹩{\sigma }_{{d}_{L}}\to 0﹩. If ﹩{\sigma }_{{d}_{L}}\ne 0﹩, a step function on true luminosity distance cannot be used to account for selection effects, else the H 0 posterior may be biased in a way that depends on ﹩{\sigma }_{{d}_{L}}﹩.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: PP plot generated for the Direction 1 considered here and a nominal error on d  L  of 20%–30%. The shaded area shows the 1, 2, and 3σ fluctuations of the PP plot around the ideal case, computed from a binomial distribution with n equal to the number of realizations and p equal to the credible interval level. Our simulations show that we are able to recover the input value of H 0 without incurring any significant bias.