adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: The fraction of submillimeter sources (S 870 ≥ 0.5 mJy) with optical counterparts (i ≤ 26 mag) in 2D bins of redshift and stellar mass for the field (left), protocluster outskirts (middle), and protocluster cores (right). At fixed redshift and stellar mass, the fraction of SMGs that have optical counterparts does not exhibit a strong dependence on the environment. However, massive galaxies are generally more difficult to detect in both wavelengths simultaneously, i.e., more-massive SMGs are less likely to have optical counterparts than lower-mass SMGs.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: The median obscured SFR fraction (f obs ≡ SFR IR /SFR ≥ 0.5) vs. stellar mass. The different curves show the relation for seven redshift bins from z ∼ 0.2 to z ∼ 4.5. The gray dashed line marks our definition of dust-obscured galaxies (an obscured SFR fraction of greater than 50%). On average, the obscured SFR fraction increases with stellar mass. At fixed stellar mass, the obscured SFR fraction is higher at higher redshifts, but the variation with redshift is subdominant to that with stellar mass.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: Similar to Figure 10, but for dust-to-stellar mass ratio. For all redshifts and protocluster types, the distributions are similar for the three different environments. They peak at the expected value of ∼0.01. There is a tail to low dust-to-stellar mass ratio that is slightly more enhanced in protocluster cores, but these excess dust-poor sources constitute a small fraction of the population.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: Similar to Figure 10, but for ﹩{v}_{\max }﹩ (as a proxy for dark matter halo mass). Protocluster cores exhibit flatter ﹩{v}_{\max }﹩ distributions than both protocluster outskirts and the field. The difference is greatest for Coma-type protoclusters and increases with decreasing redshift.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: PDs and PAs as functions of the observed frequency ν for Model I1 at T = 0.3(<T j), 1( ∼ T j), and ﹩3(\sim {T}_{{\nu }_{m}})\,\mathrm{days}﹩. The circle points and square points indicate ν m and ν c, respectively.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: PDs and PAs as functions of time T for Models I1, A1, I2, A2, and O at the frequencies ν opt (purple lines) and ν radio (orange lines) during T = 0.1–4.0 days. Realizations (1)–(10) are the calculation results for different realizations of turbulent magnetic field from Figures 3, 4, 8, 9, and 10. The top and bottom panels represent the PD curves and the PA curves, respectively.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Same as Figure 3, but for Model O.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Same as Figure 3, but for Model A2.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Same as Figure 11, but for Model A1.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 5-1
Authors: V. P. Shyam Prakash, Vivek K. Agrawal
Figure caption: The hardness–intensity diagram (HID) of the source GX 5-1 plotted using data from LAXPC20 with hard color computed using the count rates in 8–20 keV divided by that in 3–8 keV and intensity represented by the total counts in 3–20 keV. Boxes represent the regions considered for segment-based spectral and timing analysis.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 5-1
Authors: V. P. Shyam Prakash, Vivek K. Agrawal
Figure caption: SXT image of the source in the 0.7–7 keV energy band. The annular region used to extract the source counts to generate light curves and spectra is also shown.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Same as Figure 11, but for Model O.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: First row: volume-averaged radial extent of jet material centered on the black hole particle coordinates (solid lines), with shaded areas representing ±1 standard deviation. Second row: volume-averaged Mach number of the shocked cells within the jet material, with shaded areas indicating the range from minimum to maximum values. Third row: Volume fraction of the shocked jet material relative to the total jet-material volume. The figure’s upper and lower panel sets correspond to the mass ratios R = 1:5 and R = 1:2, respectively, both with an impact parameter of θ = 20°.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Upper panel: evolution of the volume-weighted mean Mach number inside the central region (r < 5 Mpc) of the main cluster for both mass ratios and impact parameters. Lower panel: mass-weighted entropy radial profiles as a function of time. The profiles are computed with a sphere with radius 1 Mpc. The markers indicate the initial profile of the central cluster. We only show two representative cases where the jet direction is initialized in the x-direction.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Timescales of synchrotron + IC losses (solid lines), Coulomb losses (dashed lines), and super-Alfvènic turbulent (re)acceleration (blue dotted–dashed lines) as a function of momentum. We show the R = 1:5 (upper panel) and R = 1:2 (lower panel) cases with θ = 20°, the jet initialized at t jet,0 = 50 Myr and in the x-direction. The losses lines are colored according to the evolution after the launching time. The acceleration times computed with Equation (12) for different values of ψ are shown in the horizontal shaded areas. The extent of each shaded area corresponds to the minimum and maximum estimated t acc throughout the simulation.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Same as Figure 3 but for the runs with θ = 10°.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Acceleration and cooling time ratio, t acc/t cool (first, third, fifth, and seventh rows), and volume fraction where t acc/t cool < 1 (second, fourth, sixth and eighth rows) as a function of time for all our simulations at a fixed momentum value of 5 × 103 m  e  c (where electrons in a μG magnetic field will contribute to the ∼100 MHz emission). Similar to Figure 3, each column shows the evolution for runs with different initial jet ignition times, t jet,0. We only show runs with an initial jet direction in the x-direction. Larger line widths and smaller opacity lines refer to a smaller parameter value ψ. The horizontal gray (coral) solid lines are a reference for t acc/t cool = 1 (50% of the volume fraction).
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Thin CR pressure slices through the center of the main cluster. We overplot the Mach number contours. The upper panels show in blue the Mach number distribution of the whole shock that is crossing the CR jet material and in purple the Mach number distribution corresponding to the region that overlaps with the CR material. The magnetic field vectors are weighted with B 2 ρ CR.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Volume average of the turbulent energy flux per unit volume for solenoidal (purple) and compressive (pink) modes as a function of time. We show the evolution for the R = 1:2 (solid line) and R = 1:5 (dashed line) runs with θ = 20°, t jet,0 = 50 Myr and the jet orientation initialized in the x-direction. The dashed–dotted lines show the flux computed with the solenoidal and compressive turbulent velocities using the Helmholtz–Hodge decomposition method for the R = 1:2 run.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: A 2D histogram of the magnetic field and density weighted by the CR pressure. The insets correspond to projection maps of the CR pressure (left-hand inset) and magnetic field strength (right-hand inset). The dotted white line shows the expected scaling based on adiabatic compression.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: CR pressure contour maps of runs R = 1:5, t jet,0 = 50 Myr with θ = 20° (left-hand column) and θ = 10° (right-hand column) at τ = 1.77 Gyr. Each row shows morphological differences depending on the initial direction of the jet.
Paper: Cosmic Censorship in Sgr A* and M87*: Observationally Excluding Naked Singularities
Authors: Avery E. Broderick, Kiana Salehi
Figure caption: Excluded region (blue) in the γ–Q parameter space of the 4D EGBQ naked singularity spacetime. The black region in the lower left shows parameter values for which the 4D EGBQ metric describes a black hole. The dotted red line shows the approximation in Equation (D5). Note that the axes are logarithmic.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: Left: smoothed Chandra 0.3–3 keV image of NGC 5728 binned at 1/4 of the native ACIS-S pixel. Contours from CO(2–1) emission from ALMA (V. Ramakrishnan et al. 2019) are shown in white. Red sectors represent the regions used for spectrum extraction. Right: merged X-ray spectrum of the star-forming ring in NGC 5728. The extraction regions used are shown in the left panel, and the data are binned at 5 counts per bin. We show the best-fit spectral model in orange and residuals on the bottom panel.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: First: RGB composite image of NGC 5728. HST F160W image is shown in red, 0.3–1.5 keV soft X-ray emission is shown in green, and 1.5–3 keV soft X-ray emission is shown in blue. Second: as in the first panel, but HST F438W image shown in red. Third: as in the first two panels, but Hα+[N II] emission from MUSE in red. Fourth: smoothed 0.3–3 keV Chandra image, with contours from Hα+[N II] contours from MUSE in white.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption:  V − H color map of NGC 5728 constructed using archival HST F438W (V-band) and F160W (H-band) images. Regions with high extinction have large V − H values and appear darker on the map. The color scale shows the V − H (mag) values. We also show the position of the 3 regions as in Figure 3, the CO (2–1) contours from ALMA in red, and the H2 contours from SINFONI in cyan.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: Left: Chandra ACIS-S images of NGC 5728 in the 0.3–3 keV band. This image is binned at 1/8 of the native ACIS-S pixel and is adaptively smoothed with a 2–15 pixel scale, 9 counts under kernel, and 30 iterations. Overlaid are the 1.3 mm contours from ALMA (in black), CO contours from ALMA (in red), and warm molecular H2 contours from SINFONI (in green). Center and right: soft and hard ratio maps, respectively, as in Figure 3, overlaid with H2 contours from SINFONI in red and CO contours from ALMA in black.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: Chandra ACIS-S images of NGC 5728 in the specified energy bands. These are binned at 1/8 of the native ACIS-S pixel and are adaptively smoothed with a 2–15 pixel scale, 9 counts under kernel, and 30 iterations. Overlaid in green are the H2 contours from SINFONI. We also mark the regions of enhanced X-ray emission A, B, and C, as in Figure 2, and an additional region of enhanced emission as a yellow circle.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: X-ray spectra of the two bright point sources detected near the star-forming ring in the Chandra FOV of NGC 5728. The best-fit power-law model is shown for NGC 5728 X-1, and the best-fit thermal model is shown for NGC 5728 X-2. Residuals are shown on the bottom panels.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Optical light curves and corrections for stellar contamination. (a): ASAS-3, ASAS-4, and ASAS-SN data, after cross-calibration procedures described in the text. Seasonal average for 2011 includes the few measurements from 2010 and 2012. (b) Light curve after the correction process illustrated in panels (c)–(e). (c): SkyMapper g-band image (linear scaling) with Proxima removed (green ellipse) and three obscured sources added back using data from an observation when Proxima was at a different location. (d): Image from panel (c) convolved with the ASAS 23″-FWHM PSF. Pairs of dashed circles show the FWHM for ASAS (red) and ASAS-SN (blue) at Proxima’s position for the first (left) and last (right) observations in each data set. Solid circles in the upper left show sizes of ASAS and ASAS-SN brightness extraction regions. (e): Model results for stellar contamination of Proxima, with solid lines denoting observation intervals for both data sets.
Paper: Detection of the Temperature Dependence of the White Dwarf Mass–Radius Relation with Gravitational Redshifts
Authors: Nicole R. Crumpler, Vedant Chandra, Nadia L. Zakamska, Gautham Adamane Pallathadka, Stefan Arseneau, Nicola Gentile Fusillo, J. J. Hermes, Carles Badenes, Priyanka Chakraborty, Boris T. Gänsicke, Stephen P. Schmidt
Figure caption: The difference in measured gravitational redshifts between the cool and warm subsamples of the combined catalog for redshifts measured by binning at the peak radius (top) and peak surface gravity (bottom) for one run of the bias correction simulation. Our measured gravitational redshifts for the cool and warm samples, including bias corrections and mean radius or surface gravity corrections, are shown in red and blue, respectively. The mean redshift for the cool and warm samples computed by binning in radius is 22.0 ± 1.3 and 32.7 ± 1.0 km s−1, respectively. The mean redshift for the cool and warm samples computed by binning in surface gravity is 24.2 ± 1.3 and 30.7 ± 1.2 km s−1, respectively. The LSR and asymmetric drift-corrected radial velocities in the peak bin for the cool and warm samples are shown in the red and blue histograms, respectively.
Paper: Detection of the Temperature Dependence of the White Dwarf Mass–Radius Relation with Gravitational Redshifts
Authors: Nicole R. Crumpler, Vedant Chandra, Nadia L. Zakamska, Gautham Adamane Pallathadka, Stefan Arseneau, Nicola Gentile Fusillo, J. J. Hermes, Carles Badenes, Priyanka Chakraborty, Boris T. Gänsicke, Stephen P. Schmidt
Figure caption: Same as Figure 2 but divided by temperature. We show our measurements using the combined catalog divided into a cool WD subsample (<11,000 K) in red and a warm WD subsample (>16,000 K) in blue. We find that cool WDs have smaller gravitational redshifts than warm WDs at a given radius or surface gravity, in line with our expectations from theory.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Concatenated Swift X-ray light curves. Time bins average ∼400 s but vary so time axes are not exact. Dotted horizontal lines mark each epoch’s 10th and 60th percentile rates (see Figure 3). Vertical orange bars denote periods of overlap with Chandra HRC observations (see Figure 5). Epochs 6 and 7 were not included in further analysis because of their short exposures and high proportion of flaring.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: X-ray light curves for XMM pn (epochs 5X and 13X) and Chandra HRC (epochs 8C, 12Ca, and 12 Cb) observations. Dotted horizontal lines mark quiescent rate limits. Vertical orange bars denote periods of overlap with Swift observations (see Figure 2), allowing for flux normalizations. The first overlap was not used for normalization, because it was during a flaring period.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: XRT and UVOT/W1 rate distributions for each epoch, with vertical lines marking the 10th–60th percentile range used for calculating average quiescent rates. UVOT rates are scaled down by a factor of 4 in the plot.
Paper: Detection of the Temperature Dependence of the White Dwarf Mass–Radius Relation with Gravitational Redshifts
Authors: Nicole R. Crumpler, Vedant Chandra, Nadia L. Zakamska, Gautham Adamane Pallathadka, Stefan Arseneau, Nicola Gentile Fusillo, J. J. Hermes, Carles Badenes, Priyanka Chakraborty, Boris T. Gänsicke, Stephen P. Schmidt
Figure caption: The distribution of measured radii (top) and surface gravities (bottom) for the cool (red) and warm (blue) subsamples of the combined catalog. The red and blue vertical lines correspond to the weighted means of the cool and warm distributions, respectively. The mean radius for the cool and warm samples is 0.01250 ± 0.00007 and 0.01304 ± 0.00008 R ⊙, respectively. The mean surface gravity for the cool and warm samples is 7.958 ± 0.005 and 7.918 ± 0.004 dex, respectively.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Sherpa fits to quiescent X-ray data from epochs 8 and 12 (near cycle minimum and maximum, respectively) with three components at fixed temperatures corresponding to active regions, active region cores, and subdued flaring regions. Note the large difference in high-temperature emission between the two epochs.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Optical data (with corrections for stellar contamination) and GPR fit showing rotational modulation, with the dates of Swift observations marked by gray shading. The dotted curve is from a sliding boxcar average of the GPR fit over the rotation period; subtraction of the dotted curve yields the rotational “residuals” used to study correlation with X-ray and UV variations (see Figure 8).
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Residual rates for UV/W1 (left) and XRT (center) vs. residual optical intensities for the GPR fit (excluding AOs 6 and 7). Upper limits on vertical axes are 95th percentiles. Solid black lines show least-squares fits to data within the 10th–60th percentiles (bounded by dotted lines) and only when an optical measurement was made within 21 days of a Swift measurement (black points). Cyan lines show 1σ uncertainties on the fits. Right panels show binned rates using only the black points, with and without adjustments for rotational modulation derived from the fits. Dotted vertical lines mark the 10th and 60th rate percentiles after adjustments for rotational modulation.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Cycle fits for optical, X-ray, and UV data. Optical brightness scale is inverted to aid comparison with the anticorrelated X-ray and UV intensities. X-ray and UV data were fitted simultaneously, with uncertainties adjusted to provide equal statistical weight. UV/X-ray period agreement with the optical data is much improved if the first (∼2010) data points are raised to match peak values near the ∼2018 maximum (see text). XMM and Chandra HRC data points are not used for fitting.