adsabs/AstroCLIMB huggingface dataset:
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Average low S/N bias of cflux (red points) and least-squares fit to Equation (8) (gray solid line). The effective detection threshold of crowdsource obtained from the fit is shown (vertical gray-dashed line). Fit residuals are shown in the bottom panel.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Comparison of DECaPS2 and PS1 catalogs on a low-extinction calibration field at (ℓ, b, Δθ) = (236°, −14°, 3°), where Δθ is the angular radius of the circular field. The color scale is in log-density, and each panel has its own normalization (light, white, low; dark, blue, high density). Lines indicate quartiles in the y-axis per x-axis bin with 25% and 75% in black and 50% (the median) in green. Outlier robust center (median) and scatter (σ IQR) metrics are shown for stars between 15th and 17th mag.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Top: histogram of imaging depth assuming 5.85σ-detection limit for each photometric CCD image included in the DECaPS2 catalog, separated by band. Dashed vertical line indicates the median. Bottom: median bias for recovered injected sources that are unblended as a function of magnitude, again separated by band. Horizontal dashed line indicates −169 mmag bias, which is the bias at which only 50% of sources with that magnitude would be detected.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Median angular distance (NSide = 512) between source location in DECaPS2 and the crossmatched source location in Gaia eDR3. This figure employs a cut requiring that sources be brighter than 19th magnitude in g band and be detected three times (total, regardless of band).
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Same as Figure 14 except comparing cflux- flux within the DECaPS2 catalog.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Spatial variation of the effective detection threshold s  d  in i band, which tracks source density. The average value of s  d  obtained from the fit in Figure 17 is indicated on the color bar by a green line.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Scatter plot of sources not flagged by the CP as saturated when the saturation threshold was set too low. The plot shows the ﹩{\hat{\chi }}_{r}^{2}﹩ as a function of the estimated source flux (in instrumental magnitudes). There is a sharp linear increase in the ﹩{\mathrm{log}}_{10}({\hat{\chi }}_{r}^{2})﹩ at the brightest magnitudes (<−15), indicative of sources at or near saturation being poorly modeled by the average PSF. The three brightest unflagged sources are shown as red triangles, and a set of 100 bright, but unsaturated, reference sources is shown as green squares. This example is for an i-band image taken by CCD S26.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Left: histogram (2D) of the position errors for recovering injected sources. Color scale shows log density (light, white, low; dark, blue, high). Center: same as left, but with linear density and focused on the central peak. Right: histogram (2D) of the distance error between the recovered and injected source locations as a function of the brightness of the injected source. Color scale shows log density (light, white, low; dark, blue, high).
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Histogram showing the runtime of an exposure vs. the number of sources found in that exposure for crowdsource (top) and CLOUDCOVERR.JL (bottom) processing of DECaPS2. The color scale is in log-density, and each panel has its own normalization (light, white, low; dark, blue, high density).
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: The FWHM for sources from crowdsource as a function of position on the focal plane of a typical g-band exposure. The median g-band FWHM reported for the whole survey is indicated on the color bar by a green line. The sky orientation shown for the focal plane is north up, west right.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Representative crowded bulge region (ℓ, b) = (3, −3.5) of an r-band image comparing the crowdsource model (top), original image (middle), and the resulting residuals (bottom). All panels are in ADU and on the same, highly stretched linear scale. Pixels masked by the CP, and thus not used in the crowdsource fit, are shown in gray.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Median offset between DECaPS2-PS1 in r band for stars between between 15th–17th mag, as defined using the color transform between the PS1 and DECaPS filter systems, which was derived using the calibration field at (R.A., decl.) = (100°, −27°).
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Histogram of the seeing per CCD for photometric DECaPS observations, separated by band. The tick mark above each band label indicates the median of the distribution for that band.
Paper: NEOWISE Variability of the New Gaia Herbig Ae/Be and Classical Be Stars—Variability Sample and Statistical Analysis
Authors: Ying Mei, Shi-Ming Song, Jun-Ting Liu, Lucas J. Hyland, Xi Chen
Figure caption: Left panel: the distributions of the differences between maximum and minimum magnitudes in W2 band (ΔW2) vs. the stochasticity (SD/σ of W2 flux densities) for all the variable sources selected by the criteria in Section 2.3. SD is the standard deviation of flux densities, and σ is the mean flux density uncertainty of a given light curve in the W2 band. Colors represent different three sample categories: blue for PMS, green for uncertain, red for CBE. The region dominated by the AGB stars in our samples is marked with a box. Right panel: comparison of the 2D density distributions between our PMS sample (blue counters) and Park et al. (2021) sample (red counters).
Paper: NEOWISE Variability of the New Gaia Herbig Ae/Be and Classical Be Stars—Variability Sample and Statistical Analysis
Authors: Ying Mei, Shi-Ming Song, Jun-Ting Liu, Lucas J. Hyland, Xi Chen
Figure caption: Representative light curves of W2 variability. Left panel shows the example light curves of linear(+) and linear(-). Middle panel shows example light curves of periodic and curved variables (sin and sin + linear). Stochastic variable examples are given in right panel, with upper to lower corresponding to burst, drop, and irregular light curves, respectively. The red dashed line represents the median magnitude, and the criteria for burst and drop are indicated by the dashed green lines. The burst and drop events are marked by red circles.
Paper: NEOWISE Variability of the New Gaia Herbig Ae/Be and Classical Be Stars—Variability Sample and Statistical Analysis
Authors: Ying Mei, Shi-Ming Song, Jun-Ting Liu, Lucas J. Hyland, Xi Chen
Figure caption: The cross-comparisons of cumulative distributions of the W1–W2 color (left) and W4 luminosity (right) for different types of variables in different sample categories. Upper two panels: the comparisons of the overall PMS (solid curves) and the PMS with HAeBe stars excluded (dashed curves). Middle two panels: the comparisons between HAeBe stars (solid curves) and sources in uncertain class (dashed curves). Lower panel: the comparisons between sources in the uncertain (dashed curves) and CBe categories (solid curves). Different colors represent different variable types in each panel.
Paper: NEOWISE Variability of the New Gaia Herbig Ae/Be and Classical Be Stars—Variability Sample and Statistical Analysis
Authors: Ying Mei, Shi-Ming Song, Jun-Ting Liu, Lucas J. Hyland, Xi Chen
Figure caption: Comparisons of cumulative distributions of the variability parameters (period and fractional amplitude) for the line, curved, and periodic variables in different sample categories. Upper panel: comparison of the variability periods derived from sin (dashed curves) or sin+linear (solid curves) curve fitting. Lower panel: comparison of the fractional amplitudes of the variability derived from sin (dashed curves) or sin+linear (solid curves) curve fitting.
Paper: NEOWISE Variability of the New Gaia Herbig Ae/Be and Classical Be Stars—Variability Sample and Statistical Analysis
Authors: Ying Mei, Shi-Ming Song, Jun-Ting Liu, Lucas J. Hyland, Xi Chen
Figure caption: Histogram distributions of Stetson indices of sources in PMS, CBe, and uncertain categories. The dashed lines marks the criterion threshold (larger than 20) for identifying variable sources.
Paper: NEOWISE Variability of the New Gaia Herbig Ae/Be and Classical Be Stars—Variability Sample and Statistical Analysis
Authors: Ying Mei, Shi-Ming Song, Jun-Ting Liu, Lucas J. Hyland, Xi Chen
Figure caption: Comparison of cumulative distributions of the periodic variability parameters (fractional amplitude and period), IR color, and W4-band luminosity between the AGBs and other PMS objects excluding AGBs. The AGBs are shown with solid curves, and PMS objects excluding AGBs are shown with dashed curves in these cumulative distributions.
Paper: NEOWISE Variability of the New Gaia Herbig Ae/Be and Classical Be Stars—Variability Sample and Statistical Analysis
Authors: Ying Mei, Shi-Ming Song, Jun-Ting Liu, Lucas J. Hyland, Xi Chen
Figure caption: Distributions of SED slope α for different samples.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Convergence of the Sedov–Taylor blast wave with respect to the analytic solution. Default parameters: N = 1003 resolution, N ppl = 256 particles per leaf, f  l  = 2 limiter level. Top: varying resolution; middle: varying limiter; bottom: varying leaf size. The dashed lines in the top panel show the best-fit power law N  α  of the L1-norm for each particle property, with exponents given in the legend; the results exhibit the expected linear (N −1) convergence. The middle and bottom panels measure the L1-norm ratio compared to a simulation with global time stepping at resolution N = 1003; the measurements indicate our default parameter values for f  l  and N ppl are conservatively selected.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Results of the Sedov–Taylor blast wave problem. Left: particle distribution at time t target ≃ 0.402 in a slice of thickness 2/N, colored by the specific energy u for four different resolution runs. The point size is scaled with the particle mass. Right: radial profiles of density, specific energy, pressure and radial velocity, obtained using the median value for each of the 60 bins across a domain r ∈ [0.2, 1.0]. The simulations converge to the analytic solution (black line) at the target time.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Density field at time t = 2.0 for the Kelvin–Helmholtz instability test measured on the xy-plane for N = 643, 1283, and 2563 particles. At the lowest resolution, the vortices are barely resolved, leading to over-diffusion of the primary instability. With increasing resolution, fluid mixing is more prevalent, capturing the roll-up of the primary vortices, in addition to secondary instabilities becoming visible.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: The time evolution of the y-mode amplitude and the maximum kinetic energy along the y-axis of the Kelvin–Helmholtz instability. In addition to the three HACC-simulations of N = 643, 1283, and 2563 particles, we include the high-resolution result by McNally et al. (2012). The simulations approach this reference with improving resolution, as the vortices and turbulence are increasingly refined.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Results of the 3D Sod shock-tube test run at t = 0.15 with 1D resolutions of N  x  = 50 + 25, 100 + 50, and 200 + 100 particles across a [0, 1) domain, evenly replicated along the remaining dimensions. The simulations converge to the analytic prediction (black line). Although the panels include all particles, no scatter is visible at each x-coordinate, demonstrating that the 1D solution is well maintained.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Radial profiles for density, pressure, specific energy, and radial velocity at time t = 0.77 for the Evrard collapse problem with resolutions N = 643, 1003, and 2003 particles. The solid line shows the results from the 1D PPM calculation by Steinmetz & Mueller (1993). The simulations converge well with increasing resolution.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: L1-norm convergence of the density, energy, pressure, entropy, and velocity to the analytic solution of the Sod shock-tube problem with increasing resolution. The dashed lines show the best-fit power law N  α , with exponents given in the legend. Appropriately, the state-variables converge roughly linearly (N −1), as expected for a shock test.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Evolution of the kinetic, thermal, and gravitational energy for the Evrard collapse problem. Initially, gravitational potential energy is converted to kinetic infall energy, which in turn is shock-heated into thermal energy. As in Figure 7, CRK-HACC convergences nicely to the 1D PPM results of Steinmetz & Mueller (1993).
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: Comparison of the RL relation with and without the correction for evolution in redshift of luminosities, as shown in the right and left panels, respectively. Points are marked with different colors according to their redshift, as depicted in the pictures, and the red line represents the best-fit linear RL relation.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: Behavior of the k parameter in the parameter spaces {Ω M , Ω k } (panels (a) and (b)) and {Ω M , w} (panels (c) and (d)) for both UV (left panels) and X-rays (right panels). (a) Behavior of the k parameter in the parameter space {Ω M , Ω k } for UV. The dashed black line shows the “no Big Bang” constraint (see Section 4.1 and Equation (8)). (b) Behavior of the k parameter in the parameter space {Ω M ,  Ω k } for X-rays. The dashed black line shows the “no Big Bang” constraint (see Section 4.1 and Equation (8)). (c) The behavior of the k parameter in the parameter space {Ω M ,  w} for UV. The region under the thick white line corresponds to the scenario of ﹩H^{\prime} (z){| }_{z=0}\leqslant 0﹩, while the region above the following line corresponds to ﹩H^{\prime} (z){| }_{z=0}\gt 0﹩. (d) The behavior of the k parameter in the parameter space {Ω M ,  w} for X-rays. The region under the thick white line corresponds to the scenario of ﹩H^{\prime} (z){| }_{z=0}\leqslant 0﹩, while the region above the following line corresponds to ﹩H^{\prime} (z){| }_{z=0}\gt 0﹩.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: We mark with a thick, black line the values of ﹩{k}_{{L}_{{\rm{X}}}}﹩ and ﹩{k}_{{L}_{\mathrm{UV}}}﹩ computed for the Ω M  = 0.3, Ω k  = 0, and w = −1 together with 1σ, 2σ, and 3σ error bars marked with red, orange, and green dashed lines, respectively. (a) Behavior of k-parameter for the correction of L UV in relation to Ω k  for a nonflat ΛCDM model with Ω M  = 0.3. (b) Behavior of k-parameter for the correction of L X in relation to Ω k  for a nonflat ΛCDM model with Ω M  = 0.3. (c) Behavior of k-parameter for L UV in relation to w for a flat wCDM model with Ω M  = 0.3. (d) Behavior of k-parameter for L X in relation to w for a flat wCDM model with Ω M  = 0.3.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: Comparison between the values of H 0 obtained in all of our analyses. Beside each point, we report both the corresponding data set and methodology used for the computation and the z-score z  s  with respect to the H 0 value obtained from the CMB, defined as ﹩{z}_{s}=\tfrac{| {H}_{0,\mathrm{CMB}}-{H}_{0}| }{\sqrt{{\sigma }_{{H}_{0},\mathrm{CMB}}^{2}+{\sigma }_{{H}_{0}}^{2}}}﹩, where H 0 refers to the value obtained from our fit. The two vertical dashed gray lines with the corresponding dashed light-gray lines are the reference points of CMB and SNe Ia measurements with their 1σ uncertainties. The points marked with “⧫” correspond to the cases in which the analyses do not converge for one or more parameters.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: X-ray luminosity (in logarithmic units) vs. (1 + z). The solid purple curve shows the truncation due to the flux limit, which is here assumed to be ﹩{F}_{\mathrm{lim}}=6\times {10}^{-33}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{\mathrm{Hz}}^{-1}﹩ (Dainotti et al. 2022a). The rank ﹩{{ \mathcal R }}_{i}﹩ of the point of luminosity L  i  at redshift z  i  is the number of points in the rectangle within black lines, with points under the purple curve being discarded. This figure is computed under the assumption of a flat ΛCDM model with Ω M  = 0.3.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: Corner plots obtained under the assumption of the wCDM model.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: Corner plots obtained under the assumption of the flat ΛCDM model using noncalibrated QSOs alone.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: Corner plots obtained under the assumption of the flat ΛCDM model.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: The results of the 100 looped fits of the H 0-parameter for all cases with calibrated QSOs. H 0 is in units of km s−1 Mpc−1.
Paper: A Bias-free Cosmological Analysis with Quasars Alleviating H 0 Tension
Authors: Aleksander Łukasz Lenart, Giada Bargiacchi, Maria Giovanna Dainotti, Shigehiro Nagataki, Salvatore Capozziello
Figure caption: Corner plots obtained under the assumption of the nonflat ΛCDM model.