adsabs/AstroCLIMB huggingface dataset:
Paper: Balmer Decrement Anomalies in Galaxies at z ∼ 6 Found by JWST Observations: Density-bounded Nebulae or Excited H I Clouds?
Authors: Hiroto Yanagisawa, Masami Ouchi, Kimihiko Nakajima, Hidenobu Yajima, Hiroya Umeda, Shunsuke Baba, Takao Nakagawa, Minami Nakane, Akinori Matsumoto, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Yi Xu, Yechi Zhang
Figure caption: Same as Figure 4 but for RXCJ2248-ID with Gaussian priors for T e and n e.
Paper: Balmer Decrement Anomalies in Galaxies at z ∼ 6 Found by JWST Observations: Density-bounded Nebulae or Excited H I Clouds?
Authors: Hiroto Yanagisawa, Masami Ouchi, Kimihiko Nakajima, Hidenobu Yajima, Hiroya Umeda, Shunsuke Baba, Takao Nakagawa, Minami Nakane, Akinori Matsumoto, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Yi Xu, Yechi Zhang
Figure caption: Probability distributions for GS-NDG-9422 recovered with modified YMCMC. The diagonal panels show the 1D probability distribution for each parameter. The off-diagonal panels present the 2D contours. The blue solid and black dashed lines indicate the median and the 16th and 84th percentiles of the probability distributions, respectively.
Paper: Balmer Decrement Anomalies in Galaxies at z ∼ 6 Found by JWST Observations: Density-bounded Nebulae or Excited H I Clouds?
Authors: Hiroto Yanagisawa, Masami Ouchi, Kimihiko Nakajima, Hidenobu Yajima, Hiroya Umeda, Shunsuke Baba, Takao Nakagawa, Minami Nakane, Akinori Matsumoto, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Yi Xu, Yechi Zhang
Figure caption: Same as Figure 4 but for GS-NDG-9422 with Gaussian priors for T e.
Paper: Balmer Decrement Anomalies in Galaxies at z ∼ 6 Found by JWST Observations: Density-bounded Nebulae or Excited H I Clouds?
Authors: Hiroto Yanagisawa, Masami Ouchi, Kimihiko Nakajima, Hidenobu Yajima, Hiroya Umeda, Shunsuke Baba, Takao Nakagawa, Minami Nakane, Akinori Matsumoto, Yoshiaki Ono, Yuichi Harikane, Yuki Isobe, Yi Xu, Yechi Zhang
Figure caption: Same as Figure 4 but for RXCJ2248-ID.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: Color images of dust continuum obtained with Herschel at 500 μm. The Herschel images are convolved to the TRAO beam size, 46″, which is marked as a pink circle in the lower left corner. Contours indicate the distribution of CN integrated intensities from ﹩3{\sigma }_{\mathrm{CN}}﹩ in steps of ﹩3{\sigma }_{\mathrm{CN}}﹩ where the ﹩{\sigma }_{\mathrm{CN}}﹩ is the uncertainty of CN integrated intensity in a unit of K km s−1 listed in Table 1.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: The spatial distribution of the CN and H2 column densities. A gray image displays the distribution of the H2 column density. The scale bar in each panel indicates the value of the column density. Blue and red contours in each panel delineate the half-maximum levels of CN and H2 column densities, respectively. Cyan squares and orange triangles indicate the peak positions for CN and H2 column densities, respectively. OMC-1 and NGC 2024 show two sets of symbols for local column density peaks for two clumps for each source.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: Maps of CN column density of the target sources. Black contours in each panel delineate a ﹩3{\sigma }_{\mathrm{CN}}﹩ level.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: CN (N = 1 → 0) spectra toward the center positions of the OTF maps for each target (Table 1). In each panel a thin solid line divides the seven hyperfine lines into two groups; one group of three lines with energy level transitions of N = 1 → 0, J = 1/2 → 1/2 and another group of four lines with the transitions of J = 3/2 → 1/2.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: The spatial separations between peak positions in CN and H2 column density distributions for the observing targets, in units of arcsec (left) and parsec (right). The dashed red line in the left panel indicates the TRAO beam size of 46″. A bar for the pixel size of 22″ is shown in the upper-right corner of the left panel. The error bars shown in the right panel are estimated from the distance uncertainties of the target sources listed in Table 1.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: Correlation between column densities of CN and dust toward six target sources. A green line in each panel draws a best-fitting result of both column densities with a function, log N d = a log N CN + b. The correlation coefficient, r, and the fitting parameters, a and b, are given at the upper part of each panel.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: Integrated intensity maps of the sixth CN hyperfine transition toward the target sources. A circle in the lower left corner of each panel shows the beam size (46″) of the TRAO 14 m telescope. The velocity range for the intensity integration for each map is listed in Table 1.
Paper: The Spatial Correlation between CN-line- and Dust-continuum-emitting Regions in High-mass Star-forming Clouds
Authors: Jihye Hwang, Chang Won Lee, Jongsoo Kim, Eun Jung Chung, Kee-Tae Kim
Figure caption: Maps of the H2 column density of the target sources. The column density is estimated by the SED fitting procedure of the Herschel data at four wavelengths. Black contours indicate the ﹩3{\sigma }_{\mathrm{CN}}﹩ level.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: Panels (a)–(c): the mean tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (d)–(f): the area-weighted tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (g)–(i): the latitude-weighted tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (j)–(l): the area- and latitude-weighted tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: Panels (a)–(c): the standard deviation of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (d)–(f): the rms tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (g)–(i): the mean absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The standard deviation of the tilt angles (a), the rms tilt angle (b), and the mean absolute value of the tilt angles (c) vs. the mean tilt angle during the declining phase. The solid lines show the respective linear fits. The correlation coefficients and the probabilities that the correlations are due to chance can be found in each panel. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The standard deviations of the tilt angles (a), the rms tilt angles (b), and the mean absolute values of the tilt angles (c) during the declining phases of SCs 14–21. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The tilt-angle distributions for the declining phases of SCs 14–21. The solid lines show the respective normal fits. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The mean tilt angles during the declining phases of SCs 14–21. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The strengths (a), amplitudes (b), and durations of the ascending phases (c) in SCs 15–22.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: Panels (a)–(c): the area-weighted absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (d)–(f): the latitude-weighted absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (g)–(i): the area- and latitude-weighted absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: Panels (a)–(c): the mean tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (d)–(f): the area-weighted tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (g)–(i): the latitude-weighted tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (j)–(l): the area- and latitude-weighted tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the MW database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: Panels (a)–(c): the area-weighted absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (d)–(f): the latitude-weighted absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (g)–(i): the area- and latitude-weighted absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the MW database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: Panels (a)–(c): the standard deviation of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (d)–(f): the rms tilt angle during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. Panels (g)–(i): the mean absolute value of the tilt angles during the declining phase vs. the strength, amplitude, and duration of the ascending phase of the next SC. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the MW database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The standard deviation of the tilt angles vs. the percentage of weak SGs (a), the percentage of medium SGs (b), the percentage of large SGs (c), the mean area of all SGs (d), the total area of all SGs (e), and the number of all SGs (f) during the declining phase. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The standard deviation of the tilt angles vs. the percentage of weak SGs (a), the percentage of medium SGs (b), the percentage of large SGs (c), the mean area of all SGs (d), the total area of all SGs (e), and the number of all SGs (f) during the declining phase. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the MW database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: 〈∣α∣〉/〈∣λ∣〉 during the declining phase vs. the strength (a), amplitude (b), and duration of the ascending phase (c) of the next SC. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the KK database.
Paper: Relationship between the Tilt Angles of Sunspot Groups and the Properties of the Next Solar Cycle
Authors: P. X. Gao, J. C. Xu
Figure caption: The standard deviation of the tilt angles (a), the rms tilt angle (b), and the mean absolute value of the tilt angles (c) vs. the mean tilt angle during the declining phase. The solid lines show the respective linear fits. The correlation coefficients and probabilities can be found in each panel. These data are derived from the MW database.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Stellar temperature profiles showing locally super-Eddington radiative luminosity due to opacity peaks. Left panels: a M ZAMS = 30 M ⊙, Z = 1 Z ⊙ model with a opacity peak due to both hydrogen and helium ionization transitions. Left panels correspond to time when ﹩\mathrm{log}{T}_{\mathrm{eff}}/{\rm{K}}=3.76﹩, ﹩\mathrm{log}L/{L}_{\odot }=5.45﹩ on the H-R diagram. Right panels: a M ZAMS = 60 M ⊙, Z = 1 Z ⊙ model with an iron opacity peak. Right panels correspond to time when ﹩\mathrm{log}{T}_{\mathrm{eff}}/{\rm{K}}=4.60﹩, ﹩\mathrm{log}L/{L}_{\odot }=5.80﹩ on the H-R diagram. Top panels: Eddington ratios; ratios of radiative (purple) and convective (green) luminosity against Eddington luminosity. Here, radiative luminosity or convective luminosity refer to, respectively, the luminosity carried by radiative diffusion or convection. Unity is shown in a dashed black line, and the critical optical depth is indicated by a dashed red line (see text in Section 3.) Bottom panels: local opacity in each zone throughout the star (purple) and Eddington opacity (dashed black) 4π GcM/L. Only locally super-Eddington radiative luminosity (in green) is considered in our eruptive mass-loss model.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Eruptive mass-loss rates across the H-R diagram. Left column: ξ = 0.1. Right column: ξ = 1.0. Top row: Z = 1 Z ⊙. Bottom row: Z = Z SMC = 0.2 Z ⊙. Gray lines show the evolutionary tracks of stars from the beginning of main sequence until the end of the model run. Models were run at every 1 M ⊙ increments but only selected models are shown here for clarity. Dashed gray lines show two empirical tracks of Quiescent LBVs and LBVs in Outburst for reference. Solid red lines show the Humphreys–Davidson limit for reference. Colored contours show the rate of eruptive mass loss experienced by the star, with legend on the right.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Profiles of luminosity, energy, and opacity as a function of mass above each radius for a M ZAMS = 30 M ⊙, Z = 1 Z ⊙ star. The model chosen corresponds to the time when ﹩\mathrm{log}{T}_{\mathrm{eff}}/{\rm{K}}=3.76﹩, ﹩\mathrm{log}L/{L}_{\odot }=5.45﹩ on the H-R diagram just after the start of core helium burning (center helium mass fraction of 0.98). For all panels, the horizontal axis is defined as M above = M − m(r). The dashed black and red lines, respectively, show τ crit and r mass loss as defined in Equations (1) and (11). The x-intercept of the red dashed line shows the total mass lost (see Equation (10)). Top panel: local radiative, Eddington (Equation (4)), and excess luminosities. Second panel: total excess energy (Equation (7)) and binding energy (Equation (8)). Third panel: local excess energy (Equation (5)). Last panel: local opacity, showing the opacity peak at around M above ≈ 4 × 10−4 M ⊙ due to both hydrogen and helium ionization transitions.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Ratio of total mass loss against wind mass-loss rates across the H-R diagram. Left column: ξ = 0.1. Right column: ξ = 1.0. Top row: Z = 1 Z ⊙. Bottom row: Z = Z SMC = 0.2 Z ⊙. Colored contours here show the ratio between total mass loss and wind mass loss, with legend on the right. Cooler colors (blues) indicate that eruptive mass loss is more dominant over stellar wind. All axes, labels, and other lines follow Figure 6.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Kippenhahn diagram for M ZAMS = 30 M ⊙, Z = 1 Z ⊙ stars. The age x-axis focuses on the time of core He burning. This is the same model shown in Figure 1. Top panel: modeled with stellar wind and eruptive mass loss. Bottom panel: modeled only with stellar wind. Blue contours show the rate of nuclear energy generation, with the color bar on the right.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Evolutionary tracks of M ZAMS = 30 M ⊙, Z = 1 Z ⊙ stars. H-R tracks for wind only (green) and eruptive mass-loss + wind (purple) models. The models marked with “Decin” contain the modification described in Section 3, while those using the old C. de Jager et al. (1988) rates are marked with “de Jager.” From the differing green and purple tracks, eruptive mass loss prevents evolution to RSG phase.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Evolutionary tracks of M ZAMS = 30 M ⊙, Z = 1 Z ⊙ stars. Left panel: H-R tracks for wind only (green) and eruptive mass loss + wind (purple) models. From the differing green and purple tracks, eruptive mass loss prevents evolution to the RSG phase. Right panel: evolutionary tracks sampled to one model every 1000 yr to show where stars are expected to be observed.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: Evolutionary tracks of models with and without eruptive mass loss. Left column: ξ = 0.1. Right column: ξ = 1.0. First row: Z = 1 Z ⊙. Second row: Z = Z SMC = 0.2 Z ⊙. All axes and labels follow Figure 6.
Paper: A Model for Eruptive Mass Loss in Massive Stars
Authors: Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy
Figure caption: mass-loss rate, mass-loss ratio, and effective temperature over time of an M ZAMS = 30 M ⊙ star with ξ = 1.0 and Z = 1 Z ⊙. The middle panel shows the ratio between the mass-loss rate due to eruptive mass loss and the stellar wind mass-loss rate. The dashed black line marks when the ratio is unity.
Paper: Measurements of Magnetic Cloud Expansion through Multiple Spacecraft in Radial Conjunction
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Bin Zhuang, Florian Regnault, Antoinette B. Galvin
Figure caption: Nine MCs observed by multiple spacecraft. (a) MC1 observed by Helios 1 and Voyager 2 in year 1978; (b) MC2 observed by ACE and NEAR in year 2000; (c) MC3 observed by MESSENGER and STB in year 2009; (d) MC4 observed by MESSENGER and STB in year 2010; (e) MC5 observed by MESSENGER and STB in year 2011; (f) MC6 observed by STB and Juno in year 2012; (g) MC7 observed by STA and Juno in year 2012; (h) MC8 observed by Wind and Juno in year 2013; (i) MC9 observed by MESSENGER and ACE in year 2014. The panels in each plot show the total field strength and the components (B  ϕ  and B  z ) in the MVA coordinate system. The x-axis presents the normalized time, in which 0 means the MC start and 1 means the end time.
Paper: Measurements of Magnetic Cloud Expansion through Multiple Spacecraft in Radial Conjunction
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Bin Zhuang, Florian Regnault, Antoinette B. Galvin
Figure caption: The fittings of the MC observed by Helios 1 and Voyager 2 in the year 1978. Helios 1: 1978-03-02T00:00:00–1978-03-03T05:45:00; Voyager 2: 1978-03-07T02:30:00–1978-03-09T04:00:00. The panels are the total  B  (black, observed; red, radial self-similar expansion solution; blue, isotropic self-similar expansion solution; nT), three B components in the RTN coordinate system (nT), and proton velocities (black, observed data; red, linear fitting of V  p ; km s−1).
Paper: Measurements of Magnetic Cloud Expansion through Multiple Spacecraft in Radial Conjunction
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Bin Zhuang, Florian Regnault, Antoinette B. Galvin
Figure caption: The distributions of the magnetic field strength and components with the distance away from the Sun. (a) Distributions of log(B) vs. log(r) of the nine MCs; (b) distributions of log(B  z ) vs. log(r); (c) distributions of log(B  ϕfront) vs. log(r); (d) distributions of log(B  ϕrear) vs. log(r). The black lines are the average of the linear fittings of the nine MCs’ distributions, and the equations are shown in the panels.