adsabs/AstroCLIMB huggingface dataset:
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: Arm M images of the COSMOS field (left panel) comprising fields 1 to 4 (from right to left), and the Lockman field (right panel) fields 5 and 6 (from right to left). Magenta crosses indicate the central pixel coordinates, and cyan crosses represent the requested coordinates. The difference between the requested and actual pointing is within 8′ for all fields.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Dependence of (top) [Ar V] 7.90 μm/[Ar III] 8.99 μm and (bottom) [Ar V] 13.10 μm/[Ne III] 15.56 μm on the ionization parameter (U), as predicted by AGN photoionization models (colored points). Each panel displays model results under specific parameter constraints: (a1 and a2) 12 + log(O/H) = 8.76 and log(P/k) = 7.0; (b1 and b2) log Epeak = −1.49 and log(P/k) = 7.0; and (c1 and c2) log Epeak = −1.49 and 12 + log(O/H) = 8.76, while the gray dashed line represents the best-fit correlation (Equation (1)) derived from all AGN models in Section 3.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: PSF width as a function of drift for the C3 band, shown for flight data (left) and simulated data (right). Each field presents the results using all frames (circles) and skipping the first few frames (squares). The points represent PSF widths at successive intervals throughout the integration, with colors indicating the progression from the start (violet) to the end (red) of the integration. Both data and simulations show a significant increase in PSF width during the initial frames of fields 1 and 5, attributed to unexpected motions observed in the top panel of Figure 22. In field 1, the pointing shifts by approximately 3 pixels, leading to a PSF width increase of about 2 pixels. Similarly, in field 5, the pointing shifts by 5 pixels, resulting in a PSF width increase of approximately 4 pixels. As the pointing stabilizes and drift diminishes, the PSF width decreases after the first few frames. The other fields exhibit only minor changes in PSF width, as the drift between frames is minimal.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Examples of the AGN ionizing spectra calculated by OPTXAGNF for AGN photoionization models with the black hole mass set as 107 M⊙ and the Eddington ratio (i.e., λEdd) ranging from 10−3 to 1. The vertical lines indicate the required ionization energies of marked ions. All AGN ionizing spectra are normalized by the peak flux for illustration. Note that the energy corresponding to the peak flux (i.e., Epeak, in units of keV) increases along with an increase of λEdd and a decrease of black hole mass.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: Ground and flight PSF comparison with stamp size 25 × 25 pixels. Panels show (left to right) closest launch focus PSF, a single isolated star PSF from field 2 in flight, 9× resolution stacked PSF, and encircled energy graph for (top to bottom) arm L, M, and S, respectively. Each overlaid red circle corresponds to the radius that encloses 85% of the energy in the upsampled PSF centered on the weighted average signal center. Images are locally background subtracted and scaled from zero to the 99th percentile of the signal in the stamp.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Dependence of [Ne VI] 7.65 μm/[Ar V] 7.90 μm on the input AGN spectrum peak energy (Epeak, in keV), as predicted by AGN photoionization models (colored points). Each panel displays model results under specific parameter constraints: (a) 12 + log(O/H) = 8.76 and log(P/k) = 7; (b) log U = −2.8 and log(P/k) = 7; and (c) log U = −2.8 and 12 + log(O/H) = 8.76. The dashed lines represent the best-fit correlations (Equations (2)–(5)) derived from all AGN models with the given log U and 12 + log(O/H).
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: Change in PSF width as traced by C1, field 5 line-fit images. The left panel shows a line-fit image using frames 0–1, with a PSF width of 2.76 pixels represented by the red ellipse. The middle panel shows a line-fit image using frames 0–10. The pointing of the experiment shifted, resulting in two bright spots and an increased PSF width of 6.81 pixels. The right panel shows a line-fit image using frames 0–39. At this point, the pointing had been stable for tens of frames, so the PSF width decreases to 3.8 pixels.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: Cumulative histograms of flat-field values at the positions of stars used for calibration in the C1–C6 bands. Since the mean values are consistent with 1 across all bands, the effect of flat-field variations on the calibration is not biasing in our calibration.
Paper: The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light
Authors: Michael Zemcov, James J. Bock, Asantha Cooray, Shuji Matsuura, Dae-Hee Lee, Candice Fazar, Richard M. Feder, Grigory Heaton, Ryo Hashimoto, Phillip Korngut, Toshio Matsumoto, Chi H. Nguyen, Kazuma Noda, Won-Kee Park, Kei Sano, Kohji Takimoto, Toshiaki Arai, Seung-Cheol Bang, Priyadarshini Bangale, Masaki Furutani, Viktor Hristov, Yuya Kawano, Arisa Kida, Tomoya Kojima, Alicia Lanz, Chika Matsumi, Dale Mercado, Shunsuke Nakagawa, Tomoya Nakagawa, Shuta Nakahata, Ryo Ohta, Dorin Patru, Mai Shirahata, Hiroko Suzuki, Aoi Takahashi, Momoko Tamai, Serena Tramm, Kohji Tsumura, Yasuhiro Yamada, Shiang-Yu Wang
Figure caption: The relationship between the catalog flux λFλ × K and the photocurrent ∑ii for each star (blue points). The flux conversion factors are the slope of the fitting (orange lines).
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Diagrams consisting of (a) [Ne VI] 7.65 μm/[Ar V] 7.90 μm vs. [Ar V] 7.90 μm/[Ar III] 8.99 μm and (b) [Ne VI] 7.65 μm/[Fe II] 5.34 μm vs. [Ar V] 7.90 μm/[Fe II] 5.34 μm to distinguish between photoionization models excited by AGN and radiative shocks (i.e., including the shock precursors). Specifically, the red, blue, gray, and green contours (from dark to light covering 0%–30%, 30%–70%, and 70%–100% of the corresponding models involved in this work) represent AGN models with ﹩-2.0\,\leqslant \,{\rm{log}}{E}_{{\rm{peak}}}\,\leqslant \,-0.95﹩ (high Epeak) and ﹩-3.25\,\leqslant \,{\rm{log}}\,{E}_{{\rm{peak}}}\,\leqslant \,-2.25﹩ (low Epeak), and radiative shock models with vs ≥ 500 km s−1 (high vs) and vs ≤ 500 km s−1 (low vs), respectively. The six gray points represent the measurements in Table 2 of the six Seyferts discussed in Section 3.5.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Same as Figure 2 but for low-luminosity AGN. Each panel, if not specifically marked, displays model results under the same parameter constraints as in Figure 2 for log U (i.e., −2.8), 12 + log(O/H) (i.e., 8.76), and log(P/k) (i.e., 7.0), but with a different value of log Epeak (−2.75 here).
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Dependence of [Ar II] 6.99 μm/[Fe II] 5.34 μm on the metallicity (12 + log(O/H)), as predicted by AGN photoionization models (colored points). Each panel displays model results under specific parameter constraints: (a) log Epeak = −1.49 and log(P/k) = 7.0; (b) log U = −2.8 and log(P/k) = 7.0; and (c) log U = −2.8 and log Epeak = −1.49, while the gray dashed line represents the best-fit correlation (Equation (10)) derived from all AGN models with (P/k) ≤ 8.0.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Diagram consisting of [Ar V] 13.10 μm/[Ne III] 15.56 μm vs. [Ar II] 6.99 μm/[Fe II] 5.34 μm to illustrate the contamination effects of shock excitation on emission-line ratio diagnostics in AGN. For AGN model results on the right, different colors, marker sizes, marker types, and edge widths correspond to different log U, log Epeak, 12 + log(O/H), and log(P/k), respectively. For the shock + precursor model results on the left, black solid and gray dashed grids correspond to model results of standard and strong magnetic fields, respectively, where the two gray arrows indicate the trend of model results as metallicity and shock velocity increase, and the red and blue lines mark the lower boundaries.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Dependence of ([Ar III] 8.99 μm + [Ar V] 7.90 μm)/Pfα on the metallicity (12 + log(O/H)), as predicted by AGN photoionization models (colored points). Each panel displays model results under specific parameter constraints: (a) log Epeak = −1.49 and log(P/k) = 7.0; (b) log U = −2.8 and log(P/k) = 7.0; and (c) log U = −2.8 and log Epeak = −1.49. The dashed lines represent the best-fit correlations (Equations (6)–(9)) derived from all AGN models with the given log U and log Epeak.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Examples of the ionization structures at different depths into the ionized clouds, as predicted by AGN photoionization models with the black hole mass set as 107 M⊙ and log λEdd = −0.5. See the lower right of each panel for the values of other input parameters, i.e., log U, log(P/k), and 12 + log(O/H). The colored solid and dashed lines in each panel represent the abundances of different argon and neon ions relative to the total argon or neon abundance, respectively. As a reference, the black solid line in each panel represents the hydrogen ion abundance relative to the total hydrogen abundance. In addition, the gray solid and dashed lines in each panel, as labeled in panel (a3), represent the temperature T and column density (nH) as a function of the number density (NH), respectively (see the two y-axes on the right).
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Dependence of (a1 and a2) [S IV] 10.51 μm/[Ne III] 15.56 μm on the ionization parameter (U); (b1 and b2) [Ne II] 12.81 μm/Pfα on the metallicity (12 + log(O/H)); and (c1 and c2) [Ar III] 8.99 μm/[Ar III] 21.83 μm on the gas pressure (P/k), as predicted by SF photoionization models (colored points). Each panel displays model results under specific parameter constraints: (a1 and b1) log(P/k) = 7.0; (c1 and a2) 12 + log(O/H) = 8.76; and (b2 and c2) log U = −2.8. The gray dashed lines in panels (a1) and (a2) represent the best-fit correlation (Equation (12)) derived from all SF models discussed in this section, while the colored dashed lines in panels (b1) and (b2) represent the best-fit correlations (Equation (13)–(16)) derived from all SF models with the given log U.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Dependence of [Ne V] 14.32 μm/[Ne V] 24.32 μm on the gas pressure (P/k, in units of K cm−3), as predicted by AGN photoionization models (colored points). Each panel displays model results under specific parameter constraints: (a) log Epeak = −1.49 and 12 + log(O/H) = 8.76; (b) log U = −2.8 and 12 + log(O/H) = 8.76; and (c) log U = −2.8 and log Epeak = −1.49, while the gray dashed line represents the best-fit correlation (Equation (10)) derived from all AGN models with log(P/k) ≳ 6.5.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: The ionizing spectra calculated by A. D. Thomas et al. (2018) for the SF photoionization models, where the vertical lines indicate the required ionization energy of marked ions. All ionizing spectra are normalized by the flux at the IP of hydrogen atom (i.e., 13.6 eV).
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: The same as Figure 11, but with added contours for the SF photoionization models discussed in Section 4.2. Measurements for the central ﹩r=0\mathop{.}\limits{^{\prime\prime} }75﹩ regions of six Seyferts represented by the six gray points are taken from L. Zhang et al. (2024b).
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Dependence of (a1 and a2) [Ne III] 15.56 μm/[Ne II] 12.81 μm; (b1 and b2) [Ar III] 8.99 μm/[Ar II] 6.99 μm; and (c1 and c2) [S IV] 10.51 μm/[S III] 18.71 μm on the metallicity (12 + log(O/H)), as predicted by the SF photoionization models (colored points) discussed in Section 4.2. The top and bottom panels display model results under specific constraints on log(P/k) (i.e., 7.0) and log U (i.e., −2.8), respectively.
Paper: Theoretical Diagnostics for the Physical Conditions in Active Galactic Nuclei under the View of JWST
Authors: Lulu Zhang, Ric I. Davies, Chris Packham, Erin K. S. Hicks, Daniel E. Delaney, Miguel Pereira-Santaella, Laura Hermosa Muñoz, Ismael García-Bernete, Claudio Ricci, Dimitra Rigopoulou, Almudena Alonso-Herrero, Martin J. Ward, Enrica Bellocchi, Cristina Ramos Almeida, Francoise Combes, Masatoshi Imanishi, Omaira González-Martín, Tanio Díaz-Santos, Anelise Audibert, Álvaro Labiano, Nancy A. Levenson, Santiago García-Burillo, Lindsay Fuller
Figure caption: Same as Figure 6 but for low-luminosity AGN. Each panel, if not specifically marked, displays model results under the same parameter constraints as in Figure 6 for log U (i.e., −2.8), 12 + log(O/H) (i.e., 8.76), and log(P/k) (i.e., 7.0), but with a different value of log Epeak (−2.75 here).