adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for the Sources of Excess Extragalactic Dispersion of FRBs
Authors: Sunil Simha, Khee-Gan Lee, J. Xavier Prochaska, Ilya S. Khrykin, Yuxin Huang, Nicolas Tejos, Lachlan Marnoch, Metin Ata, Lucas Bernales, Shivani Bhandari, Jeff Cooke, Adam T. Deller, Stuart D. Ryder, Jielai Zhang
Figure caption: Cumulative estimate of 〈DMhalos〉 as a function of the maximum halo mass that can contribute to DMhalos. 〈DMhalos〉 is computed assuming the HMF corresponding to our adopted cosmology (McClintock et al. 2019), integrated to the given maximum M halo from the same minimum M halo = 1010.3  M ⊙. The halo gas model has the same modified NFW profile described previously, extending to one virial radius with 75% of the halo baryons in the hot, ionized phase.
Paper: False-positive Self-lensing Events: TESS Observing Asteroid-crossing Events in Disguise
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Liam J. Neeley, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: The binned light curve of TIC 1008555 displaying a large symmetric pulse during which the stellar brightness appears to increase by 3.3%.
Paper: Transport Equation of Kappa Distributions in the Heliosphere
Authors: G. Livadiotis, D. J. McComas
Figure caption: Scheme explaining the transitions of the expanding solar wind in the heliosphere. When entropy increases (e.g., due to combining the plasma with other less organized plasmas or particle systems), it shifts the system toward classical thermal equilibrium (κ → ∞ ) (Eq), where the kappa values are likely within the near-equilibrium region (defined by κ > 2.5; red arrow). However, when entropy decreases (e.g., due to the exchange of the plasma ions with other more organized ion populations, such as the highly-organized newly born PUIs), it shifts the system away from the classical thermal equilibrium and closer to the anti-equilibrium stationary state (κ → 3/2) (aEq), where the kappa values are likely within the far-equilibrium region (defined by κ < 2.5; blue arrow). The interaction of the highly ordered motion of newly formed PUIs increases the ordering of space plasmas, thus decreases their entropy, and eventually, drives them away from the classical thermal equilibrium. Therefore, the inner heliosphere, with comparatively fewer PUIs resides in near-equilibrium stationary states, while the outer heliosphere and inner heliosheath reside in states far from equilibrium (adapted from Livadiotis & McComas 2011a.)
Paper: Transport Equation of Kappa Distributions in the Heliosphere
Authors: G. Livadiotis, D. J. McComas
Figure caption: The radial profile of the kappa parameter of the solar wind protons (left panel) plotted for both pickup proton dimensionalities D pui = 2 (black) and 1 (red), as well as for polytropic index (i) fixed and equal to the adiabatic value (dash) and (ii) given by the modeled polytropic index γ(R) (solid). The plot shows that the kappa decreases with increasing the heliocentric distance as the solar wind expands in the heliosphere, ending at its outer limits near the heliosheath, where the four lines provide kappa values mostly within the interval 1.5 < κ < 2.5, the far-equilibrium region. This coincides with the histogram of kappa values (right panel) characterizing the whole sky-map of the inner heliosheath (Livadiotis et al. 2022).
Paper: False-positive Self-lensing Events: TESS Observing Asteroid-crossing Events in Disguise
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Liam J. Neeley, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: Light curves of the four asteroid-crossing events (black points) with our self-lensing model (orange curve) fitted using EMCEE. The thickness of each curve represents the 95% confidence interval.
Paper: Transport Equation of Kappa Distributions in the Heliosphere
Authors: G. Livadiotis, D. J. McComas
Figure caption: Radial profile of the polytropic index of the solar wind in the heliosphere (upper panels) for (a) a constantly adiabatic expansion, and (b) according to the model in Equation (22). The corresponding kappa (middle panels) is plotted in terms of the heliocentric distance R (radial profile) and (lower panels) in terms of the dimensionality of the newly born pickup protons D pui.
Paper: Transport Equation of Kappa Distributions in the Heliosphere
Authors: G. Livadiotis, D. J. McComas
Figure caption: Scheme showing the drop in entropy caused by the exchange of a PUI with a kappa-distributed plasma proton in a timescale τ. The low dimensionality D pui < 3 of the newly born PUI, which was exchanged with a 3D kappa-distributed plasma proton, causes the plasma entropy to decrease. After the exchange, the newly born PUI will continue to evolve, but the effect on the entropy of the whole plasma system has already been achieved.
Paper: Transport Equation of Kappa Distributions in the Heliosphere
Authors: G. Livadiotis, D. J. McComas
Figure caption: Radial evolution of the kappa distribution of particle energy in the heliosphere, plotted for heliocentric distance R = 1 au (blue), 10 au (green), and 100 au (red), and for the dimensionality of the newly born pickup protons, which is D pui = 1. (Note that the kinetic energy is expressed in the heliospheric inertial frame.)
Paper: False-positive Self-lensing Events: TESS Observing Asteroid-crossing Events in Disguise
Authors: Nicholas M. Sorabella, Silas G. T. Laycock, Liam J. Neeley, Dimitris M. Christodoulou, Sayantan Bhattacharya
Figure caption: Asteroid 1590 Tsiolkovskaja (circled in red) passing in front of TIC 1008555 over the course of 10 hr.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: Top: the distribution of best-fit parameter values for the 1T (red), 2T (green), and T+IC (blue) models using the 1000 realizations of the background (as described in Section A.2) for A2146. The parameters shown represent the temperatures of each model and the IC norm. Bottom: the distribution of the difference in C-stat values (Δ C) between the T+IC and 2T models from fits using the 1000 realizations of the background. The 2T model is preferred in all iterations for describing the NuSTAR-observed spectra over the T+IC model, with the latter not having any realization favoring it over the 2T model. Therefore, we conclude that the data clearly disfavor the addition of a nonthermal component.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: Top: the distribution of best-fit parameter values for the 1T (red), 2T (green), and T+IC (blue) models using the 1000 realizations of the background (as described in Section A.2) for A665. The parameters shown represent the temperatures of each model and the IC norm. Bottom: the distribution of the difference in C-stat values (Δ C) between the T+IC and 2T models from fits using the 1000 realizations of the background. The 2T model is preferred in all iterations for describing the NuSTAR-observed spectra over the T+IC model, with the latter not having any realization favoring it over the 2T model. Therefore, we conclude that the data clearly disfavor the addition of a nonthermal component.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: This figure shows the 20–80 keV nonthermal flux for six clusters as measured by NuSTAR (blue), Beppo-SAX(red), Chandra (black), RXTE (green), Suzaku+XMM-Newton (purple), NuSTAR+XMM-Newton (magenta), and Swift (orange). Results for A2163 (star) are taken from Feretti et al. (2001); Million & Allen (2009); Rojas Bolivar et al. (2021), and Rephaeli et al. (2006). The A665(downward triangle) flux is also from Million & Allen (2009). The Bullet Cluster (square) measurements are from Wik et al. (2014) and Ajello et al. (2010). Coma Cluster (diamond) results are taken from Rephaeli & Gruber (2002), Fusco-Femiano et al. (2004), Wik et al. (2009), Gastaldello et al. (2015), and Wik et al. (2011). A523 (circle) results are from Cova et al. (2019). All data points are plotted with the NuSTAR measured temperature, although some have been slightly shifted for clarity.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: A false color (faint to bright represented by black to blue to green to yellow to red to white) combined (A+B) log scaled images from 4–25 keV, smoothed by a Gaussian kernel with σ = 3 pix, and stretched to show features in the outer parts of the FOV. The source regions from which spectra were extracted are shown as black circles. Superimposed in blue are radio contours obtained from Vacca et al. (2010) for A665 and Hlavacek-Larrondo et al. (2018) for A2146. For A665, we display the total intensity radio contours at 1.4 GHz (combined VLA data in C and D configurations). For A2146, we display low-resolution 1–2 GHz contours. Top (left to right): A665 (OBSID: 70201002002) and A665 (OBSID: 70201003002) Bottom: A2146.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: Global fits to the A665 (upper panels) and A2146 spectra (lower panels) with 1T (left panels), 2T (middle panels), and T+IC (right panels) models. For the A665 spectra, black indicates FPMA and red indicates FPMB for OBSID 0201002002, whereas for OBSID 0201002002, FPMA and FPMB are indicated by green and orange, respectively. For the A2146 spectra, black indicates FPMA and red indicates FPMB. For both A665 and A2146, crosses show the data and the background is denoted with asterisks. The dashed curves correspond to the model components to visualize their contributions to the composite model. For plotting purposes, adjacent bins are grouped to ensure a detection significance of at least 10σ, with maximum 20 bins.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: False color images of FPMA (left panels) and FPMB (right panels) for both observations of A665 (OBSID 70201002002 on top, OBSID 70201003002 on bottom). Overlaid are the nuskybgd regions used to extract background spectra from each of the four detectors. Note that we did not use a region in DET2 as the cluster’s emission is largely present there without much room to make a good enough region to capture background emission. We also used an exclusion region around the cluster to remove emission leaking into our regions. Background fits can be seen in Appendix A.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: A665 (OBSID 70201002002 on the left and OBSID 70201003002 in the middle) and A2146 (right) in different energy bands. In each panel; top left: 3–8 keV; top right: 8–15 keV; bottom left: 15–30 keV; bottom right: 30–40 keV. Each image has been background subtracted and exposure corrected. They are presented in a log scale from 0 counts s−1 pix−1 (in black) to 20+ counts s−1 pix−1 (in white) and smoothed by a Gaussian kernel with σ = 3 pix. There are fewer cluster counts present in the higher energy images and there are no obvious morphological changes with respect to the lower energy images, which are dominated by thermal photons.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: Filtered light curves for FPMA (top panel) and FPMB (bottom panel) telescopes following the process described in Section 2.1. The light curves have been filtered in the 50–160 keV energy range to eliminate SAA background contributions as well as the 1.6–20 keV range to remove solar activity background contributions. The set of light curves are in order from left to right as A665 (OBSID: 70201002002), A665 (OBSID: 70201003002), and A2146 (OBSID: 70401001002).
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: False color images of FPMA (left panel) and FPMB (right panel) for A2146. Overlaid are the nuskybgd regions used to extract background spectra from each of the four detectors. Background fits can be seen in Appendix A.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: Biases due to tSZ (left panel), kSZ (middle panel), and CIB (right panel) in CMB lensing cross-correlations similar to Figure 7 but extended to other experiments and more redshift bins. See text for more details.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: The spatial analysis of synthetic coronal emission. The left-hand image shows the density distribution through a coronal slab, which follows an isotropic 1/k scaling law. The color scale has been clipped to the given values. The right-hand panel shows the analysis of the one-dimensional emergent intensity that is calculated from the coronal slab. The Fourier spectra of the original and smoothed emergent intensity are displayed, along with a curve indicating the slope of a 1/k power law.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: Estimate of image noise to signal level as function of distance from Sun center for the deconvolved (Level 2), noise-gated (Level 3), and unsharp mask averaged data (Level 5).
Paper: Energy Budget in the Solar Corona
Authors: Daniele Telloni, Marco Romoli, Marco Velli, Gary P. Zank, Laxman Adhikari, Lingling Zhao, Cooper Downs, Jasper S. Halekas, Jaye L. Verniero, Michael D. McManus, Chen Shi, Aleksandr Burtovoi, Roberto Susino, Daniele Spadaro, Alessandro Liberatore, Ester Antonucci, Yara De Leo, Lucia Abbo, Federica Frassati, Giovanna Jerse, Federico Landini, Gianalfredo Nicolini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Vincenzo Andretta, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Stuart D. Bale, Justin C. Kasper
Figure caption: Coronal radial trends in the Metis FOV of (a) plasma mass density, (b) bulk-flow (black) and Alfvén (red) speed, (c) magnetic field strength, (d) outward-propagating Alfvén wave energy, (e) proton (black) and electron (red) temperature, and (f) temperature anisotropy. Dashed curves in (e) and (f) are for profiles obtained in the CGL adiabatic limit. The green dot denotes the PSP-measured reference point for each extrapolated profile.
Paper: Energy Budget in the Solar Corona
Authors: Daniele Telloni, Marco Romoli, Marco Velli, Gary P. Zank, Laxman Adhikari, Lingling Zhao, Cooper Downs, Jasper S. Halekas, Jaye L. Verniero, Michael D. McManus, Chen Shi, Aleksandr Burtovoi, Roberto Susino, Daniele Spadaro, Alessandro Liberatore, Ester Antonucci, Yara De Leo, Lucia Abbo, Federica Frassati, Giovanna Jerse, Federico Landini, Gianalfredo Nicolini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Vincenzo Andretta, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Stuart D. Bale, Justin C. Kasper
Figure caption: Contributions (a) and fractions (b) of the total energy flux (black), coming from the kinetic energy flux (red), enthalpy flux (green), gravitational (cyan) and electric (blue) potential energy fluxes, Alfvén wave energy flux (yellow), and heat flux (gray). Shaded areas with the same color code indicate the confidence interval for fluxes estimated under different assumptions for coronal quantities (see text for details); the adiabatic approximation is marked by dashed lines.
Paper: Energy Budget in the Solar Corona
Authors: Daniele Telloni, Marco Romoli, Marco Velli, Gary P. Zank, Laxman Adhikari, Lingling Zhao, Cooper Downs, Jasper S. Halekas, Jaye L. Verniero, Michael D. McManus, Chen Shi, Aleksandr Burtovoi, Roberto Susino, Daniele Spadaro, Alessandro Liberatore, Ester Antonucci, Yara De Leo, Lucia Abbo, Federica Frassati, Giovanna Jerse, Federico Landini, Gianalfredo Nicolini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Vincenzo Andretta, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Stuart D. Bale, Justin C. Kasper
Figure caption: Overview of PSP measurements as the spacecraft entered the POS observed by Metis: (a) bulk-flow and Alfvén speeds (U and U A, in black and red, respectively), (b) magnetic field intensity B, (c) proton and QTN electron number densities (n  p  and n  e , in black and red, respectively), (d) proton and QTN electron temperatures (T  p  and T  e , in black and red, respectively), (e) temperature anisotropy T ⊥p /T ∥p , and (f) heat flux Q.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: A segment of the TESS light curve (BJD 2,649,647–2,649,648), where the secondary minima deviate from phase 0.5.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: Panel (a): Max I and Max II change relationship diagram, A ∼ G represent seven different stages. Panel (b): Min I and Min II change relationship diagram. Panel (c): Max I–Min I and Max II–Min change relationship diagram. Panel (d): O-C diagram of TESS after removing sine and parabolic trends.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: Upper panel: the O-C diagram of NY Boo. Middle panel: O-C diagram after subtracting the parabolic variation. Bottom panel: final residuals after subtracting parabolic and periodic variations. The red dots refer to the eclipse times obtained from TESS.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: Panel (a): Max I vs. Max II correlation diagram with a Pearson correlation coefficient of –0.87. Panel (b): Min I vs. Min II correlation diagram with a Pearson correlation coefficient of –0.93. Panel (c): Max I–Min I vs. Max II–Min II correlation diagram with a Pearson correlation coefficient of –0.93. Panel (d): Correlation diagram between O-C values of primary and secondary eclipses with a Pearson correlation coefficient of –0.87.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: CCF profile of part of the spectrum. The solid black line indicates the CCF profile. The red dashed line represents the double Gaussian fit. The blue and pink dashed lines denote individual Gaussian components.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: Two examples of LAMOST and SDSS normalized spectra.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: Left Panel: ASAS-SN photometric data in V band. Right panel: convert to one phase and fit the light minima phase with a parabola.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: The normalized light curves of all the sectors.
Paper: NY Bootes: An Active Deep and Low-mass-ratio Contact Binary with a Cool Companion in a Hierarchical Triple System
Authors: Fangbin Meng, Liying Zhu, Shengbang Qian, Nianping Liu, Linjia Li, Azizbek Matekov
Figure caption: The TESS phase-flux diagram that varied with time.
Paper: Evolution of Nonparametric Morphology of Galaxies in the JWST CEERS Field at z ≃ 0.8–3.0
Authors: Yao Yao, Jie Song, Xu Kong, Guanwen Fang, Hong-Xin Zhang, Xinkai Chen
Figure caption: The C–A and G–M 20 diagrams at rest-frame ∼570 and ∼1000 nm. The first column represents the values that have been matched to the F200W PSF, and the other columns represent the values that have been matched to the F444W PSF. The red, green, and blue crosses present the mean values and 1σ quantiles of the z = 0.8–1.3, 1.3–2.0, and 2.0–3.0 bins, respectively. The sloped lines on the C–A diagrams are the boundaries between LTGs and intermediate galaxies, defined by Bershady et al. (2000), and the horizontal lines are used to divide mergers and LTGs at A = 0.35, defined by Conselice (2003). The classification of galaxies on the G–M 20 diagrams is based on Lotz et al. (2008a). The solid orange lines (G = 0.14M 20 + 0.80) show the boundaries between LTGs and ETGs, and the blue lines (G = −0.14M 20 + 0.33) divide mergers and nonmergers. The dashed orange lines are the boundaries between LTGs and ETGs described by Equation (1), which have corrected the λ rf-dependent morphology biases.