adsabs/AstroCLIMB huggingface dataset:
Paper: KRIOS: A New Basis-expansion N-body Code for Collisional Stellar Dynamics
Authors: Kerwann Tep, Brian T. Cook, Carl L. Rodriguez, Jiya Jolly, Eddie Sawin, Michael S. Petersen, Christoph Gaffud
Figure caption: Impact of the KRIOS parameters on the time required to reach 1 trh, over 128 CPUs, where we used 25 nearest neighbors (NNs) for the local density estimates (the impact of the number of NNs on runtime is negligible compared to the other parameters) and one sample per dynamical time. Solid lines show timings with basis filtering, while dashed lines show timings without basis filtering. The duration scales linearly with ﹩{n}_{{\rm{\max }}}﹩ (without basis filtering) and almost linearly with N, while basis filtering speeds up force calculation. The effect of filtering sometimes results in the calculation of a single basis element of the SCF expansion thanks to our use of the optimized Z96 basis family.
Paper: KRIOS: A New Basis-expansion N-body Code for Collisional Stellar Dynamics
Authors: Kerwann Tep, Brian T. Cook, Carl L. Rodriguez, Jiya Jolly, Eddie Sawin, Michael S. Petersen, Christoph Gaffud
Figure caption: Evolution of the change in angular momentum (in Hénon units), ∣ΔL∣, ∣ΔLz∣, as in the bottom panel of Figure 10 (nonrotating isotropic cluster), using the radial pairing scheme (dotted lines) and the local-density-pairing scheme (solid lines) for an isotropic Plummer sphere. The latter method yields much better conservation, with an error in the angular momentum about 10 times lower than with the radial pairing method.
Paper: KRIOS: A New Basis-expansion N-body Code for Collisional Stellar Dynamics
Authors: Kerwann Tep, Brian T. Cook, Carl L. Rodriguez, Jiya Jolly, Eddie Sawin, Michael S. Petersen, Christoph Gaffud
Figure caption: Evolution of the SCF 3D local-mass density, ρ(r), for the run shown in Figures 8 and 10. As we near core collapse, density tends to converge toward the r−2.23 behavior in the central region and r−3.5 behavior in the outer region, which is in agreement with K. Takahashi (1995).
Paper: KRIOS: A New Basis-expansion N-body Code for Collisional Stellar Dynamics
Authors: Kerwann Tep, Brian T. Cook, Carl L. Rodriguez, Jiya Jolly, Eddie Sawin, Michael S. Petersen, Christoph Gaffud
Figure caption: Same as in Figure 8, instead starting from an isotropic rotating Plummer sphere with LBD parameter αr = 0.5. As in the nonrotating case, the SCF approach is consistent with measurements made in N-body simulations over the course of the cluster’s relaxation up to the deeper stages of core collapse. Changes in the integrals of motion are once more kept below <1% relative error in energy and ∣δL∣ ≤ 0.03 HU.
Paper: KRIOS: A New Basis-expansion N-body Code for Collisional Stellar Dynamics
Authors: Kerwann Tep, Brian T. Cook, Carl L. Rodriguez, Jiya Jolly, Eddie Sawin, Michael S. Petersen, Christoph Gaffud
Figure caption: Same as Figure 8, but instead starting from a q = −6 tangentially anisotropic cluster. As in the isotropic case, the SCF approach is consistent with measurements made in N-body simulations over the course of the cluster’s relaxation up to the deeper stages of core collapse. Changes in the integrals of motion are kept below <1% relative error in energy and ∣δL∣ ≤ 0.004 HU.
Paper: Using LHASSO-observed Gamma-Ray Bursts to Study the Extragalactic Background Light
Authors: Longhua Qin, Jiancheng Wang, Chuyuan Yang, Quangui Gao, Huaizhen Li, Ju Ma, Weiwei Na, Ao Wang, Xu Zhang, Baoyu Ma, Tingfeng Yi, Zunli Yuan, Chunxia Gu
Figure caption: Left panel: constraints on the EBL as a function of wavelength at z = 0, ranging from 0.1 to 40 μm, compared with various surveys—24 μm and MIPS data from C. Papovich et al. (2004), Lick/Two Micron All Sky Survey from E. L. Wright (2001), DIRBE Wright from E. L. Wright (2004), optical data from Bernstein (R. A. Bernstein et al. 2002), IRTS NIR Matsumoto (T. Matsumoto et al. 2005), 15 μm ISO from D. Elbaz et al. (1999), GAMA–DEVILS–HST from S. Koushan et al. (2021), JWST/NIRCam for R. A. Windhorst et al. (2023), and IPAC data from G. G. Fazio et al. (2004) and R. S. Savage & S. Oliver (2005). Right panel: the derived cosmic emissivity (luminosity density), comparing with data from A. Domínguez et al. (2011) for Dominguez 2011 and A. Saldana-Lopez et al. (2021) for Saldana–Lopez. Final results are taken as the medians of four WCDA-only and two WCDA+KM2A reconstructions.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: 2″ × 2″ cutout images of J0217-0208 (top panel), SXDF-NB1006-2 (middle panel), and J1211-0118 (bottom panel). The leftmost panels display Subaru/HSC Y-band images, while the other four panels show JWST/NIRCam images obtained in this study. The white circles in the JWST cutouts show the point-spread function (PSF) FWHMs. J1211-0118 is resolved into multiple clumps in the JWST/F150W image whose PSF FWHM is ﹩\sim 0\mathop{.}\limits{^{\prime\prime} }07﹩.
Paper: Using LHASSO-observed Gamma-Ray Bursts to Study the Extragalactic Background Light
Authors: Longhua Qin, Jiancheng Wang, Chuyuan Yang, Quangui Gao, Huaizhen Li, Ju Ma, Weiwei Na, Ao Wang, Xu Zhang, Baoyu Ma, Tingfeng Yi, Zunli Yuan, Chunxia Gu
Figure caption: Comparison of the optical depth derived from spectral fitting with the EBL model by A. Saldana-Lopez et al. (2021).
Paper: Using LHASSO-observed Gamma-Ray Bursts to Study the Extragalactic Background Light
Authors: Longhua Qin, Jiancheng Wang, Chuyuan Yang, Quangui Gao, Huaizhen Li, Ju Ma, Weiwei Na, Ao Wang, Xu Zhang, Baoyu Ma, Tingfeng Yi, Zunli Yuan, Chunxia Gu
Figure caption: The best-fitting SEDs of the GRB 221009A under the EBL model of A. Saldana-Lopez et al. (2021).
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Comparison of electron densities measured using the optical line ratio (ne,optical) and the FIR [O III] line (ne,FIR). The red diamonds represent our measurements from the [O III] 52 μm/[O III] 88 μm and [O II] λ3729/[O II] λ3726 ratios for J0217-0208, SXDF-NB1006-2, and J1211-0118. The red open squares show densities measured using the [O III] 88 μm/[O III] λ5007 and [O II] λ3729/[O II] λ3726 ratios for COS-3018555981 (J. Witstok et al. 2022; J. Scholtz et al. 2025) and MACS1149-JD1 (M. Stiavelli et al. 2023; C. Marconcini et al. 2024). The black circles (squares) represent densities of galaxies at z ∼ 0 measured using the [O III] 52 μm/[O III] 88 μm and [S II] λ6716/[S II] λ6731 ([O II] λ3729/[O II] λ3726) ratios in J. Moustakas & R. C. Kennicutt (2006) and J. R. Brauher et al. (2008; those from Y. Chen et al. 2023, 2024 are shown in parentheses). At z ∼ 0, the electron densities measured with the optical line ratios are comparable to those measured with the FIR [O III] line ratio, except for the Seyfert galaxy NGC 1068. At z ∼ 6–9, the FIR-based electron densities are systematically lower than those with the optical line ratios.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: SFRs and stellar masses (M*) of the galaxies analyzed in this study. The red diamonds represent J0217-0208, SXDF-NB1006-2, and J1211-0118, whose stellar masses are estimated in this study. The red open squares represent COS-3018555981 and MACS1149-JD1, which are analyzed in Section 5. Their SFRs and stellar masses are estimated in the literature (J. Scholtz et al. 2025; C. Marconcini et al. 2024). The SFRs are measured from the dust-corrected Hβ luminosities. The blue solid line represents the star formation main sequence at z ∼ 6–7 from L. Clarke et al. (2024), with the shaded region indicating its intrinsic scatter at the high-mass end. The blue dashed line shows the main sequence at z = 7 from J. S. Speagle et al. (2014), shifted by 0.32 dex to match the low-metallicity calibration adopted in L. Clarke et al. (2024).
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Resolved maps of electron density derived from the [O II] λ3729/[O II] λ3726 line ratio. We mask spaxels where the electron density is not reliably estimated, specifically when the ratio of the estimated density to its uncertainty is less than three. The black contours represent arbitrary [O III] λ5007 flux levels. In J0217-0208 and SXDF-NB1006-2, most (>90%) of the pixels show densities higher than 500 and 100 cm−3, respectively, and no significant fraction of pixels with low densities is observed.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: JWST/NIRSpec spectra around the [O II] λλ3726, 3729 emission lines after continuum subtraction. The red dashed lines represent the best-fit Gaussian functions for each emission line, convolved with the line-spread function, while the red solid line shows the total profile. Thanks to the resolution (R ∼ 2700) of the G235H (for J0217-0208 and J1211-0118) and G395H (for SXDF-NB1006-2) gratings, we can measure the [O II] λ3729/[O II] λ3726 line ratio, allowing us to constrain the electron densities of these galaxies.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: ALMA [O III] 52 μm data for J0217-0208 (top panels), SXDF-NB1006-2 (middle panels), and J1211-0118 (bottom panels) obtained in this study. The left-hand panels display the 3″ × 3″ [O III] 52 μm maps, with contours drawn from ±3σ with an interval of 1σ. Positive and negative contours are shown as solid and dashed lines, respectively. The background is the JWST/NIRCam F150W image, and the red ellipse at the lower left corner indicates the synthesized beam sizes of ALMA. The right-hand panels present the continuum-subtracted spectra, with the observed wavelength of the [O III] 52 μm line indicated by the gray dotted line. We clearly detect the [O III] 52 μm line in J0217-0208 at the 6.7σ significance level.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: JWST/NIRSpec IFU data for J0217-0208 (top panels), SXDF-NB1006-2 (middle panels), and J1211-0118 (bottom panels) obtained in this study. The left panels show the 2″ × 2″ [O III] λ5007 map integrated over 300 km s−1. The contours are drawn from ±5σ (±3σ) with an interval of 4σ (1σ) for J0217-0208 and SXDF-NB1006-2 (J1211-0118). The background image is a rest-frame UV (JWST/NIRCam F150W) image. The right panels display the continuum-subtracted spectra, with the observed wavelengths of several emission lines indicated by the gray dotted lines.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: [O III] 52 μm/[O III] 88 μm line ratio as a function of electron density. The brown, purple, blue, cyan, green, and yellow curves represent the line ratios for electron temperatures of Te = 8000, 10,000, 13,000, 16,000, 20,000, and 24,000 K, respectively, calculated using PyNeb. The black dashed curve shows the fit for Te = 13,000 K (Equation (1)).
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: JWST/NIRSpec spectra around the Hγ and [O III] λ4363 emission lines after continuum subtraction. The [O III] λ4363 emission line is detected (tentatively identified) at the 6σ (4σ) significance level in SXDF-NB1006-2 (J0217-0208).
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: SED fitting results for J0217-0208 (top panels), SXDF-NB1006-2 (middle panels), and J1211-0118 (bottom panels). The left-hand panels show the SEDs, where the red circles represent observed magnitudes, and the blue line along with open circles denote the best-fit model SED obtained with PROSPECTOR. The right-hand panels display the star formation history constrained by the SED fitting.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Results of the two-zone model fitting with the low-density and high-density gas for optical and FIR emission lines observed with JWST and ALMA. The left-hand panels show comparisons between the observed and predicted luminosities, with the black circles representing the ratios of them. With a high temperature in the high-density region and a low temperature in the low-density region, the two-zone model can successfully reproduce all of the emission lines from the optical to FIR. The blue and red bars indicate the fractions of the luminosities emitted from the low-density and high-density regions, respectively. The FIR [O III] 88 μm and [O III] 52 μm emission lines primarily arise from low-density regions due to their low critical densities (510 and 3600 cm−3, respectively). The [O III] λ4363 luminosity is dominated by emission from the high-density and high-temperature regions, as its emissivity strongly depends on the electron temperature. The right-hand panels show the constraints on the metallicity (Z) and the O32 ratio from the two-zone model. Data points in the 1σ, 2σ, and 3σ confidence intervals are indicated with the black, gray, and light-gray dots, respectively.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Schematic illustrations of galaxies at z ∼ 0 (left) and z > 6 (right). At z ∼ 0, galaxies are low density on average, and the [O III] and [O II] luminosities are dominated by emission from low-density gas (blue; ne ∼ 10–100 cm−3). At z > 6, we propose two scenarios: (a) clumpy galaxy and (b) AGN. In the clumpy galaxy scenario (a), the optical [O III] and [O II] emission lines ([O III] λλ4959, 5007, [O II] λλ3726, 3729, and [O III] λ4363) are emitted from both the low-density gas (blue) and the high-density gas in clumps (red), and sometimes the [O III] λ4363 luminosity is dominated by emission from the high-density clumps due to its strong sensitivity to the electron temperature. The FIR [O III] emission ([O III] 88 μm and [O III] 52 μm) arises from the low-density gas due to their low critical densities. In the AGN scenario (b), the optical [O III] and [O II] emission originates both from the high-density gas in the AGN narrow-line region and/or outflowing gas around the AGN, and from the low-density gas in the host galaxy. In both scenarios, since the [O II] λλ3726, 3729 emission is contributed by both low-density (ne ∼ 100 cm−3) and high-density (ne ∼ 10,000 cm−3) gas, the electron density measured with the [O II] line ratio at z > 6 (ne ∼ 1000 cm−3) represents an intermediate value between those of the low- and high-density components.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: The bottom panel shows the mass–metallicity relation. The red filled diamonds represent our fiducial metallicities measured with the two-zone model fitting (see Section 5.3) using the emission lines observed with JWST and ALMA. The red open diamonds indicate metallicities measured with the direct-Te method using [O III] λ4363, which fail to reproduce the ALMA FIR [O III] line luminosities (see Section 5.2). As shown in the top panel, metallicities measured with the direct-Te method can be significantly underestimated by up to ∼0.8 dex, compared to those derived from the JWST and ALMA joint analyses. The lines in the bottom panel show the mass–metallicity relations at z ∼ 0 in B. H. Andrews & P. Martini (2013, the black line), at z ∼ 2.3 and 3.3 in R. L. Sanders et al. (2021, the blue and green lines, respectively), and at z ∼ 4–10 in K. Nakajima et al. (2023, the orange dashed line), M. Curti et al. (2024, the orange dotted line), and L. E. Rowland et al. (2025, the orange solid line).
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Comparison of observed and predicted luminosities with the one-zone model for J0217-0208, COS-3018555981, SXDF-NB1006-2, and MACS1149-JD1. The circles represent the ratios of the observed and predicted luminosities. Using the electron density and temperature measured from the optical [O II] λ3729/[O II] λ3726 and [O III] λ4363/[O III] λ5007 line ratios, the one-zone model successfully reproduces the optical emission-line luminosities (the black circles), but it significantly underpredicts the luminosities of the FIR [O III] 88 μm and [O III] 52 μm emission lines (the red circles).
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Relation between metallicity and the [O III] 88 μm/Hβ (left) and [O III] 88 μm/[O III] λ5007 (right) line ratios. The red diamonds show the observed line ratios and metallicities constrained with the two-zone model at z ∼ 6–9 in this study, and the black open squares are results at z ∼ 0 (Y. Chen et al. 2023, 2024). The red curves represent the best-fitting relations presented in Equations (6) and (7).
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Comparison of the mass–metallicity relations with simulations. The red filled diamonds represent our fiducial metallicities measured with the two-zone model fitting (same as Figure 15). We show predictions from cosmological simulations: First Light in blue (Y. Nakazato et al. 2023), Illustris TNG in green (P. Torrey et al. 2019), Astraeus in purple (G. Ucci et al. 2023), FLARES in gray (S. M. Wilkins et al. 2023), and FIRE-2 in brown (A. Marszewski et al. 2024). All predictions are at z = 7, except for the one at z = 6 from Illustris TNG. Our inferred high metallicities in massive galaxies are consistent with the steep slope of the mass–metallicity relations predicted by some simulations.
Paper: JWST and ALMA Joint Analysis with [O II] λλ3726, 3729, [O III] λ4363, [O III] 88 μm, and [O III] 52 μm: Multizone Evolution of Electron Densities at z ∼ 0–14 and its Impact on Metallicity Measurements
Authors: Yuichi Harikane, Ryan L. Sanders, Richard Ellis, Tucker Jones, Masami Ouchi, Nicolas Laporte, Guido Roberts-Borsani, Harley Katz, Kimihiko Nakajima, Yoshiaki Ono, Mansi Gupta
Figure caption: Same as Figure 9, but for the [O III] 88 μm/[O III] λ5007 ratio. This ratio depends on both the electron temperature and density. Therefore, if the temperature is determined from other lines (e.g., [O III] λ4363), we can derive the electron density.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: The relation between torus radius vs. bolometric luminosity in W1 (left) and W2 (right) bands. The torus radii from Y.-J. Chen et al. (2023) and A. K. Mandal et al. (2024) are also shown, noting that the values from the former were not corrected for accretion disk contamination. The best-fit relations for this sample and the one including A. K. Mandal et al.'s (2024) sample are shown with different colors. Note that the sample from Y.-J. Chen et al. (2023) is not included in the best-fit analysis since AD contamination has not been corrected in that case.
Paper: Probing the Dust Torus Radius–Luminosity Relation: A WISE View
Authors: Ashutosh Tomar, Suvendu Rakshit, Amit Kumar Mandal, Shivangi Pandey
Figure caption: Quality assessment through p-valve and maximum cross-correlation coefficient (r﹩{}_{{\rm{\max }}}﹩) color coded by ﹩{{ \mathcal R }}_{\mathrm{Fe}\,\mathrm{II}}﹩ values. The selection criteria are p-valve < 0.2 and r﹩{}_{{\rm{\max }}}﹩ > 0.5, as shown by the horizontal and vertical dashed lines, respectively.