adsabs/AstroCLIMB huggingface dataset:
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 122 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as low density (LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 156 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated/low density (EI/LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 102 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated/low density (EI/LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 135 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated/low density (EI/LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 100 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated/low density (EI/LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 144 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as low density (LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 119 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 91 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 121 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: The lower (acoustic) limit V 1 and the upper limits—i.e., V 2,+ and V 2,−, based on Equations (17) and (18), respectively—are depicted vs. the negative-over-positive ion density ratio δ. The following parameter values have been adopted: v  b,0 = 0.18, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: The lower (acoustic) limit V 1 and the upper limits—i.e., V 2,+ and V 2,−, based on Equations (17) and (18), respectively—are depicted vs. the negative-over-positive ion density ratio δ for three sets of κ  e,c  and κ  e,h . (a) The variation for κ  e,c  = 2.5 and κ  e,h  = 6, (b) the variation for κ  e,c  = 4 and κ  e,h  = 2.5, and (c) the variation for κ  e,c  = κ  e,h  = 10,000. The following parameter values have been adopted: v  b,0 = 0.18, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, and β = 2.7.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: The variation of the angular frequency ω of linear electrostatic modes with respect to the wavenumber k is shown. The plots have been obtained by solving Equation (5) numerically. The left panel (a) represents the two real roots (ω 1, ω 2) and the real part of the (two) complex roots (ω 3, ω 4) for v  b,0 = 0.18. The right panel (b) depicts the imaginary parts of the two complex roots (ω 3, ω 4) obtained (for the same value, v  b,0 = 0.18). A set of indicative (arbitrary) values of the plasma parameters have been considered: δ = 0.1, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 1) (a) Pseudopotential profiles and (b) phase portrait profiles for δ = 0.05. Curve (i), curve (ii), and curve (iii) correspond to the velocities V = 1.3, V = 1.35, and V = 1.41, respectively. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.05, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2) (a) Potential profiles corresponding to negative-polarity pulses in the preceding Figure 7. (b) Electrostatic potential profile corresponding to positive-polarity pulses in Figure 7. (c) E-field corresponding to negative-polarity pulses in Figure 7. (d) E-field corresponding to positive-polarity pulses in Figure 7. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.34, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2) (a) The pseudopotential (S) profiles and (b) phase portrait profiles are shown for δ = 0.2. Curves (i) and (ii) correspond to V = 1.35 and V = 1.4302, respectively. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.34, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 1) (a) Potential (pulse) profiles and (b) E-field (bipolar pulse) profiles corresponding to solitary wave solutions of the cases depicted in Figure 5. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.05, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: The lower bound (true sound speed) V 1 is shown with respect to v  b,0 for indicative (arbitrary) values of the plasma parameters: q = 1, δ = 0.1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6. The diagram is obtained by solving Equation (15) numerically.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 2) (a) The pseudopotential (S) and (b) phase portrait profiles are shown for δ = 0.3483. Curves (i)–(iii) correspond to V = 1.41, V = 1.440163, and V = 1.443, respectively. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.3483, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 1) (a) The pseudopotential (S) profiles and (b) phase portrait profiles are depicted for δ = 0.34, considering different values of V: curves (i), (ii), and (iii) correspond to V = 1.42, V = 1.438, and V = 1.445, respectively. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.34, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 3) (a) Pseudopotential and (b) phase portrait profiles for δ = 0.38: curves (i), (ii), and (iii) correspond to V = 1.44, 1.4521, and 1.455, respectively. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.38, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 1) The electrostatic potential ϕ (solid line; values on the left vertical axis) and the resulting charge separation Δn (dashed line; values on the right vertical axis) are depicted vs. η (a) for negative-polarity solutions and (b) for positive-polarity solutions. All panels refer to the situation shown in the preceding Figure 9 (note the labels (i)–(iii) and the color code, which match the respective curves in the previous figure). The plasma parameters are chosen as v  b,0 = 0.18, δ = 0.34, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 3) The potential pulse solution ϕ (solid line) and the corresponding total charge density disturbance Δn (dashed line) are depicted, associated with the positive-polarity solutions obtained from the curves depicted in Figure 15. Panels (i)–(iii) correspond to curves (i)–(iii) in Figure 15. (All parameter values are the same as listed in Figure 15.)
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 3) E-field profiles for positive-polarity pulses, associated with the solutions depicted in the preceding Figure 16. Panels (i)–(iii) correspond to curves (i)–(iii) in Figure 15. (All parameter values are the same as listed in Figure 15.)
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 2) Potential profile (solid line) and charge density profile (Δn) (dashed line) for the positive-polarity pulses depicted in Figure 12. Panels (i)–(iii) correspond to curves (i)–(iii) in Figure 12. (The parameter values adopted are listed in that figure.)
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 1) The bipolar E-field excitation resulting from the solutions depicted in Figure 9 is shown (for the same values), i.e., (a) for a series of negative-polarity pulses and (b) for positive-polarity pulses. The remaining plasma parameters are v  b,0 = 0.18, δ = 0.34, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 2) E-field profile for positive-polarity pulses depicted in Figure 12. Panels (a)–(c) correspond to curves (i)–(iii) in Figure 12. (The parameter values adopted are listed in that figure.)
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Left: Hα vs. Paβ flux ratio diagram for HAEs in the Spiderweb protocluster. Yellow and blue circles show the emission-line fluxes of our sample of HAEs with and without spectroscopic redshift, respectively. The solid and dotted lines represent increasing values of nebular extinction AV  (see Section 3.3). The gray shaded area displays the forbidden region where our assumptions of Case B recombination are no longer valid. Right: main sequence diagram. Symbols and colors of the HAE samples follow the same scheme shown in the left panel. The solid line and the gray area display the location of the Main Sequence of star formation from J. S. Speagle et al. (2014). The dotted line marks the boundary of 1 dex below the main sequence.
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Source distribution at 2.12 < z < 2.21 across the Spiderweb protocluster over the JWST/NIRCam F405N image. Magenta circles display the 42 color-selected narrowband PBEs (S24). Big yellow and blue circles respectively depict the known HAEs with and without spectroscopic redshift (J. D. Kurk et al. 2004a, 2004b; Y. Koyama et al. 2013; J. M. Pérez-Martínez et al. 2023; R. Shimakawa et al. 2024a). Green diamonds show additional spectroscopic samples in this field (L. Pentericci et al. 2000; S. Croft et al. 2005; E. Kuiper et al. 2011; B. H. C. Emonts et al. 2018; K.-i. Tadaki et al. 2019; S. Jin et al. 2021). The violet cross marks the position of the Spiderweb radio galaxy (H. J. A. Roettgering et al. 1994).
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 4) (a) The pseudopotential (S) curve and (b) the corresponding phase portrait profile are depicted for δ = 0.42: curve (i), curve (ii), and curve (iii) correspond to V = 1.46, V = 1.4731722, and V = 1.474, respectively, in both panels. Note that the latter two curves do not cross the horizontal axis on the positive side, as the limit dictated by the condition ﹩\phi \lt \tfrac{{(V-{v}_{b,0})}^{2}}{2}={\phi }_{\max ,+}﹩ is attained before they do. The phase-space trajectories are therefore not closed, beyond the DL occurrence shown as curve (ii). The remaining plasma parameters are v  b,0 = 0.18, δ = 0.42, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Gallery depicting the images of the HAEs with spectroscopic redshift quoted in Table B1. Sources are ordered by the ID given in R. Shimakawa et al. (2024a) and organized in two blocks made of five columns, each displaying squared cutouts (4″ × 4″) for each HAE. The cutouts respectively correspond to the SUBARU/MOIRCS NB2071 and Ks filters, the JWST/NIRCam F405N and F410M filters, and a stacked RGB color that combines the JWST/NIRCam F115W, F182M, and F410M broad and medium band filters, roughly matching the rest-frame U, V and J bands. The first cutout column of each block includes a magenta dotted line displaying the size of the aperture used to extract the flux in the four presented filters (see Section 3.2). ID 73 corresponds with the Spiderweb galaxy (G. K. Miley et al. 2006).
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 3) (a) Pseudopotential (S) and (b) phase portrait profiles for δ = 0.5: curves (i), (ii), and (iii) correspond to V =  2.4, 3, and 3.3, respectively. The remaining plasma parameters are v  b,0 = 0.18, δ =  0.5, q = 1, μ = 2.216, ζ = 0.01, ν = 0.99, β = 2.7, κ  e,c  = 4, and κ  e,h  = 6.
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 3) (a) The electrostatic potential and (b) the E-field excitations are depicted for negative-polarity solutions obtained from the curves depicted in Figure 20. (The parameter values adopted here are as listed in Figure 20.)
Paper: Electrostatic Solitary Waves in Electronegative Martian Plasma
Authors: Steffy Sara Varghese, Kuldeep Singh, Frank Verheest, Ioannis Kourakis
Figure caption: (Region R 2, case 4) (a) Electrostatic potential and (b) E-field profiles, representing the positive-polarity solutions obtained for the parameter values considered in Figure 18. (All parameter values are as listed in that figure, for the respective curves.)
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Phase-space diagram. Our spectroscopic sample of HAEs is displayed by circles color-coded according to the nebular attenuation AV . The green diamonds display additional spectroscopically confirmed protocluster members from different sources (e.g., L. Pentericci et al. 2000; S. Croft et al. 2005; E. Kuiper et al. 2011; R. Shimakawa et al. 2015; B. H. C. Emonts et al. 2018; K.-i. Tadaki et al. 2019; S. Jin et al. 2021; J. M. Pérez-Martínez et al. 2023). The shaded gray area represents the virialized region according to the values for M200, R200, and σ cl derived in R. Shimakawa et al. (2014). The dashed line marks the boundary between the accreted and outskirts regions (﹩\eta =({{R}}_{\mathrm{proj}}/{{R}}_{200})\times (\left|{\rm{\Delta }}{v}\right|/{\sigma }_{{\rm{cl}}})=2﹩) of an overdensity as defined by A. G. Noble et al. (2013).
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Nebular dust attenuation (AV ) as a function of local density (Σ5), taking as a reference five neighboring galaxies (left) and the projected clustercentric distance toward the Spiderweb (SW) galaxy. Yellow and blue circles represent our samples of HAEs with and without spectroscopic redshift as in previous figures. We allow for negative values AV  (gray shaded areas) to display those objects whose Hα/Paβ ratios are higher than 17.6 and thus not compatible with the Case B recombination (see Section 4.1).
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Dust attenuation over Hα vs. stellar mass diagram. Symbols and colors from our sample follow the same scheme as in previous figures. Big white diamonds display the median values for our sample within the stellar mass bins ﹩9.4\lt \mathrm{log}\ {{M}}_{* }/{{M}}_{\odot }\lt 10.2﹩ and ﹩10.2\lt \mathrm{log}\ {{M}}_{* }/{{M}}_{\odot }\lt 11.0﹩. Solid lines display the dust attenuation laws from T. Garn & P. N. Best (2010), M. Pannella et al. (2015), and R. J. McLure et al. (2018) renormalized for the G. Chabrier (2003) IMF and the Hα wavelength following a D. Calzetti et al. (2000) extinction law. The green shaded area depicts the 0.3 mag evolution for M. Pannella et al. (2015) relation within their redshift range.
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Gallery depicting the images of the HAEs discarded due to their lack of Paβ emission in Section 3.2 or due to their low S/N (Section 4.1). Sources are ordered by ID in two blocks made of five columns, each displaying squared cutouts (4″ × 4″) for each HAE. Images and symbols follow the same scheme outlined in Figure 2.
Paper: JWST/NIRCam Paβ Narrowband Imaging Reveals Ordinary Dust Extinction for Hα Emitters within the Spiderweb Protocluster at z = 2.16
Authors: Jose Manuel Pérez-Martínez, Helmut Dannerbauer, Yusei Koyama, Pablo G. Pérez-González, Rhythm Shimakawa, Tadayuki Kodama, Yuheng Zhang, Kazuki Daikuhara, Chiara D'Eugenio, Abdurrahman Naufal
Figure caption: Gallery depicting the images of the HAEs without spectroscopic redshift quoted in Table B1. Sources are ordered by ID in two blocks made of five columns, each displaying squared cutouts (4″ × 4″) for each HAE. Images and symbols follow the scheme outlined in Figure 2.
Paper: Revisiting the Chemical Composition of WD 1145+017: Impact of Circumstellar Disk Contamination on Photospheric Abundances
Authors: Érika Le Bourdais, Patrick Dufour, Siyi Xu, 偲艺 许
Figure caption: Illustration summarizing the mechanism leading to the pollution of white dwarfs. Adapted from M. Jura & E. D. Young (2014).
Paper: Revisiting the Chemical Composition of WD 1145+017: Impact of Circumstellar Disk Contamination on Photospheric Abundances
Authors: Érika Le Bourdais, Patrick Dufour, Siyi Xu, 偲艺 许
Figure caption: Photometric measurements in SDSS ugriz bands compared to our best-fit model for WD 1145+017.
Paper: Revisiting the Chemical Composition of WD 1145+017: Impact of Circumstellar Disk Contamination on Photospheric Abundances
Authors: Érika Le Bourdais, Patrick Dufour, Siyi Xu, 偲艺 许
Figure caption: Side view map of the density distribution in the disk model.