adsabs/AstroCLIMB huggingface dataset:
Paper: J-PLUS: Beyond Spectroscopy. III. Stellar Parameters and Elemental-abundance Ratios for Five Million Stars from DR3
Authors: Yang Huang, 样 黄, Timothy C. Beers, Kai Xiao, 凯 肖, Haibo Yuan, 海波 苑, Young Sun Lee, Hongrui Gu, 弘睿 顾, Jihye Hong, Jifeng Liu, 继峰 刘, Zhou Fan, 舟 范, Paula Coelho, Patricia Cruz, F. J. Galindo-Guil, Simone Daflon, Fran Jiménez-Esteban, Javier Cenarro, David Cristóbal-Hornillos, Carlos Hernández-Monteagudo, Carlos López-Sanjuan, Antonio Marín-Franch, Mariano Moles, Jesús Varela, Héctor Vázquez Ramió, Jailson Alcaniz, Renato Dupke, Alessandro Ederoclite, Laerte Sodré, Raul E. Angulo
Figure caption: Comparisons of our estimates of T eff (left panel) and log g (right panel) to those from DR9 of the LAMOST low-resolution survey. The blue dashed lines are the one-to-one lines. The overall median offset and standard deviation are marked in the top left corner of each panel. Color bars representing the numbers of stars are provided at the top of each panel.
Paper: J-PLUS: Beyond Spectroscopy. III. Stellar Parameters and Elemental-abundance Ratios for Five Million Stars from DR3
Authors: Yang Huang, 样 黄, Timothy C. Beers, Kai Xiao, 凯 肖, Haibo Yuan, 海波 苑, Young Sun Lee, Hongrui Gu, 弘睿 顾, Jihye Hong, Jifeng Liu, 继峰 刘, Zhou Fan, 舟 范, Paula Coelho, Patricia Cruz, F. J. Galindo-Guil, Simone Daflon, Fran Jiménez-Esteban, Javier Cenarro, David Cristóbal-Hornillos, Carlos Hernández-Monteagudo, Carlos López-Sanjuan, Antonio Marín-Franch, Mariano Moles, Jesús Varela, Héctor Vázquez Ramió, Jailson Alcaniz, Renato Dupke, Alessandro Ederoclite, Laerte Sodré, Raul E. Angulo
Figure caption: Comparisons of the photometric estimates of [C/Fe] (left panel), [Mg/Fe] (middle panel), and [α/Fe] (right panel) to those from Yang et al. (2022), using the approximately 0.5 million stars in common. The blue dashed lines are the one-to-one lines. The overall median offset and standard deviation are marked in the top right corner of each panel. Color bars representing the numbers of stars are provided at the top of each panel.
Paper: J-PLUS: Beyond Spectroscopy. III. Stellar Parameters and Elemental-abundance Ratios for Five Million Stars from DR3
Authors: Yang Huang, 样 黄, Timothy C. Beers, Kai Xiao, 凯 肖, Haibo Yuan, 海波 苑, Young Sun Lee, Hongrui Gu, 弘睿 顾, Jihye Hong, Jifeng Liu, 继峰 刘, Zhou Fan, 舟 范, Paula Coelho, Patricia Cruz, F. J. Galindo-Guil, Simone Daflon, Fran Jiménez-Esteban, Javier Cenarro, David Cristóbal-Hornillos, Carlos Hernández-Monteagudo, Carlos López-Sanjuan, Antonio Marín-Franch, Mariano Moles, Jesús Varela, Héctor Vázquez Ramió, Jailson Alcaniz, Renato Dupke, Alessandro Ederoclite, Laerte Sodré, Raul E. Angulo
Figure caption: Density distributions of the metallicity difference for APOGEE–J-PLUS, as a function of SFD E(B − V). The blue dashed line indicates zero residuals. The blue dots and error bars represent the median and dispersion of the metallicity difference in the individual bins of SFD E(B − V) reddening estimate. No trend of the metallicity difference with SFD E(B − V) is detected. The color bar at the top of represents the numbers of stars.
Paper: J-PLUS: Beyond Spectroscopy. III. Stellar Parameters and Elemental-abundance Ratios for Five Million Stars from DR3
Authors: Yang Huang, 样 黄, Timothy C. Beers, Kai Xiao, 凯 肖, Haibo Yuan, 海波 苑, Young Sun Lee, Hongrui Gu, 弘睿 顾, Jihye Hong, Jifeng Liu, 继峰 刘, Zhou Fan, 舟 范, Paula Coelho, Patricia Cruz, F. J. Galindo-Guil, Simone Daflon, Fran Jiménez-Esteban, Javier Cenarro, David Cristóbal-Hornillos, Carlos Hernández-Monteagudo, Carlos López-Sanjuan, Antonio Marín-Franch, Mariano Moles, Jesús Varela, Héctor Vázquez Ramió, Jailson Alcaniz, Renato Dupke, Alessandro Ederoclite, Laerte Sodré, Raul E. Angulo
Figure caption: Comparisons of the photometric estimates of [Fe/H] with those from Yang et al. (2022, left panel) and those from Galarza et al. (2022, right panel) using around 0.5 million stars in common. The blue dashed lines are the one-to-one lines. The overall median offset and standard deviation are marked in the top left corner of each panel. Color bars representing the numbers of stars are provided at the top of each panel.
Paper: J-PLUS: Beyond Spectroscopy. III. Stellar Parameters and Elemental-abundance Ratios for Five Million Stars from DR3
Authors: Yang Huang, 样 黄, Timothy C. Beers, Kai Xiao, 凯 肖, Haibo Yuan, 海波 苑, Young Sun Lee, Hongrui Gu, 弘睿 顾, Jihye Hong, Jifeng Liu, 继峰 刘, Zhou Fan, 舟 范, Paula Coelho, Patricia Cruz, F. J. Galindo-Guil, Simone Daflon, Fran Jiménez-Esteban, Javier Cenarro, David Cristóbal-Hornillos, Carlos Hernández-Monteagudo, Carlos López-Sanjuan, Antonio Marín-Franch, Mariano Moles, Jesús Varela, Héctor Vázquez Ramió, Jailson Alcaniz, Renato Dupke, Alessandro Ederoclite, Laerte Sodré, Raul E. Angulo
Figure caption: Left panel: the J-PLUS photometric-metallicity distributions for dwarfs (black histogram) and giant stars (red histogram). Right panel: the metallicity distribution functions of stars in the inner halo (red histogram; r < 25 kpc and ∣Z∣ > 5 kpc) and outer halo (blue histogram; r > 25 kpc and ∣Z∣ > 5 kpc) in the J-PLUS giant sample. The red and blue lines represent the best fits for their corresponding MDFs between [Fe/H] = −2.75 and −4.0, with the slopes listed at the bottom of the panel.
Paper: J-PLUS: Beyond Spectroscopy. III. Stellar Parameters and Elemental-abundance Ratios for Five Million Stars from DR3
Authors: Yang Huang, 样 黄, Timothy C. Beers, Kai Xiao, 凯 肖, Haibo Yuan, 海波 苑, Young Sun Lee, Hongrui Gu, 弘睿 顾, Jihye Hong, Jifeng Liu, 继峰 刘, Zhou Fan, 舟 范, Paula Coelho, Patricia Cruz, F. J. Galindo-Guil, Simone Daflon, Fran Jiménez-Esteban, Javier Cenarro, David Cristóbal-Hornillos, Carlos Hernández-Monteagudo, Carlos López-Sanjuan, Antonio Marín-Franch, Mariano Moles, Jesús Varela, Héctor Vázquez Ramió, Jailson Alcaniz, Renato Dupke, Alessandro Ederoclite, Laerte Sodré, Raul E. Angulo
Figure caption: Density distributions of the metallicity differences for J-PLUS–SAGES (top left), J-PLUS–SMSS (top right), J-PLUS–Pristine (bottom left), and J-PLUS–Gaia XP (bottom right), as a function of J-PLUS photometric [C/Fe]. Blue dashed lines indicate the zero residuals in each panel. The overall median offset and standard deviation are marked in the bottom left corner of each panel.
Paper: J-PLUS: Beyond Spectroscopy. III. Stellar Parameters and Elemental-abundance Ratios for Five Million Stars from DR3
Authors: Yang Huang, 样 黄, Timothy C. Beers, Kai Xiao, 凯 肖, Haibo Yuan, 海波 苑, Young Sun Lee, Hongrui Gu, 弘睿 顾, Jihye Hong, Jifeng Liu, 继峰 刘, Zhou Fan, 舟 范, Paula Coelho, Patricia Cruz, F. J. Galindo-Guil, Simone Daflon, Fran Jiménez-Esteban, Javier Cenarro, David Cristóbal-Hornillos, Carlos Hernández-Monteagudo, Carlos López-Sanjuan, Antonio Marín-Franch, Mariano Moles, Jesús Varela, Héctor Vázquez Ramió, Jailson Alcaniz, Renato Dupke, Alessandro Ederoclite, Laerte Sodré, Raul E. Angulo
Figure caption: Left panel: density distribution of stars in the final J-PLUS parameter sample across the sky in equatorial coordinates. The black dashed line marks the Galactic plane. Right panel: magnitude distribution of stars in the final J-PLUS parameter sample in the Gaia G band. The red histogram represents the magnitude distribution for sample stars with flg [Fe/H] ≥ 0.85.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Comparison of low-multipole temperature power spectrum measurements and model fits. The ΛCDM fit to all the Planck TT data is high relative to the ℓ < 30 data, in particular at 20 ≤ ℓ ≤ 22. Applying a multiplicative rescaling factor of 0.9 to this model provides the best match to ℓ < 30 (Δχ 2 = −4.0 with respect to ΛCDM). Lensing does not directly impact ℓ < 30, but varying A  L  allows the ΛCDM parameters to shift and partially improve the fit here (Δχ 2 = −2.3). The Planck ℓ < 30 TT data contribute 0.4σ of the preference for A  L  > 1. Varying Ω k  instead of A  L  slightly improves the fit at ℓ < 20, with Δχ 2 = −2.6. This is due to a suppression of the late-time ISW effect. Using WMAP TT instead of Planck at ℓ < 30 reduces the preference for A  L  > 1 by 0.2σ.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Binned angular power spectrum difference at 217 GHz between ecliptic equatorial and polar regions, showing significant excess power near the ecliptic. The difference can be roughly approximated as an offset in ℓ 2 C  ℓ  (dashed red line), although this shape does not couple significantly to cosmological parameters. The difference in best-fit ΛCDM+A  L  CMB-plus-foreground models contains additional oscillatory structure, tracing the acoustic peaks (blue line). The marginalized A  L  constraints from the two fits are 1.629 ± 0.220 and 1.218 ± 0.192 for the region near the ecliptic and near the ecliptic poles, respectively (Table 3). The masks used correspond to the rightmost and leftmost Mollweide images in Figure 2.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Correlations between A  L  and ΛCDM parameters for single-frequency and multifrequency fits, with the original Planck masks (top row), with the gal60_857 dust mask added at 217 GHz (middle row), and with the more stringent gal40_857 mask added at 217 GHz (bottom row). We show the 2D correlations to highlight that the degeneracy directions differ slightly with frequency and that the multifrequency A  L  constraint is not simply the average of the constraints from the individual frequencies. The preference for higher A  L  values at 217 GHz is reduced with the gal60_857 mask. This downward shift at 217 GHz is inconsistent with a statistical fluctuation (Section 4.2) and indicates some connection between A  L  at 217 GHz and Galactic dust masking. The preference for A  L  > 1 remains at 2.5σ in the multifrequency fit for the gal60_857 mask, but decreases as further 217 GHz masking is applied (to 2.1σ in the bottom row with the gal40_857 mask, or 1.8σ with 217 GHz removed entirely). The 100 and 143 GHz contours are the same in each row, and the lowl and lowE ℓ < 30 likelihoods are included in each case.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Distribution of power spectrum χ 2 values across 500 simulation realizations for five sets of masks used in this work (blue histograms), compared to the expected χ 2 probability density (black lines). The simulated data vector for each realization and set of masks consists of 765 power spectrum bandpowers from 100, 143, 143 × 217, and 217 GHz, matching the analysis of the real Planck data. The χ 2 values are computed against the input CMB-plus-foreground model used to generate the simulations. The first panel shows results from the original Planck plik likelihood masks (with very minor adjustment for additional bad pixels; see Section 2.1). The other panels show results from additional masking described in Sections 3 and 4. The consistency of the histograms with the expected χ 2 distribution tests the improved narrow-kernel approximation for estimating the covariance matrix (Section 2.3.1). The second through fifth panels demonstrate that additional sky masking does not significantly bias the covariance matrix calculation, even for cases where the sky fraction retained after masking is as low as f sky ≃ 0.2 at 217 GHz.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Visualization of Galactic structures outside the plik 217 GHz temperature mask. Top row: the first image shows the full apodized mask. The other images show a selection of maps with the plik 217 GHz mask applied. Pixels with zero weight in the mask are colored gray. The 217 GHz temperature fluctuations outside the mask are dominated by the CMB, with unmasked Galactic structures more visible in the 217 − 143 GHz difference, where the CMB cancels. The 857 GHz Planck data, where the CMB is negligible compared to the dust, and the HI4PI velocity-integrated HI intensity map, show similar structures to the 217 − 143 GHz difference. Bottom row: same as top row, but with additional masking of pixels within 60° of the ecliptic poles. The Galactic signal is visibly anisotropic, with more bright structures visible near the ecliptic (in the bottom left and top right quadrants of the images) than near the ecliptic poles.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Ratio of power from low ecliptic latitudes (masking around the ecliptic poles) to power from high ecliptic latitudes (masking around the ecliptic plane), estimated using 1000 Planck Full Focal Plane (FFP10) simulations at 217 GHz. We interpret the deviation from unity at ℓ > 1500 as a difference in effective Planck beam function on the different sky regions due to beam asymmetries and the scan pattern. As discussed in the text, this shape does not couple significantly to A  L  or other cosmological parameters, and does not explain the shifts in A  L  with ecliptic latitude.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Comparison of original Planck 2018 plik likelihood mask for 217 GHz with our gal60_857 mask constructed using thresholding in 857 GHz intensity. We perform analysis with the combination (product) of the two masks, which retains sky fraction f sky = 0.42, compared to 0.50 for the original plik mask. The additional masked regions, highlighted in the combined-plik mask difference, remove Galactic dust structures on finer angular scales than the 10° smoothing scale used in the plik mask construction, in particular in the lower-left and upper-right portions of the image.
Paper: Revisiting the A  L  Lensing Anomaly in Planck 2018 Temperature Data
Authors: Graeme E. Addison, Charles L. Bennett, Mark Halpern, Gary Hinshaw, Janet L. Weiland
Figure caption: Comparing 217 GHz sky masks for default and aggressive CO line intensity masking thresholds. (a) Binary CO mask removing pixels above 1 KRJ km s−1, as used in the plik mask construction. (b) Our more aggressive CO mask thresholded at 0.1 KRJ km s−1. (c) Original plik 217 GHz mask. (d) plik 217 GHz mask multiplied by more aggressive CO mask. (e) 217 − 143 GHz map difference with masked pixels in plik mask grayed out. (f) 217 − 143 GHz map difference with more aggressive CO mask.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: The selections (solid lines) described in Section 3 of the halo of M82 (left) and eastern tidal stream (center and right) of NGC 3077. Background selections are shown in dashed lines. The axes are in units of kpc, with the origin centered on M82 in the left and NGC 3077 in the center and right. Red Giant Branch stars are shown in red points, and Asymptotic Giant Branch stars in blue. Large tidal bridges can be seen connecting these two galaxies to M81.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: The stellar halo of M82 (large blue point) compared with stellar halos of MW-mass galaxies reported in B. Harmsen et al. (2023) (large red points) and with simulated galaxies from TNG50 having stellar halos similar in size to those of M82 (small blue points) and the MW (small red points). Left: stellar halo mass vs. mean stellar metallicity of M82 and observed MW-mass galaxies. Center: stellar halo mass vs. t 90. Right: stellar halo mean metallicity vs. t 90. The stellar halo mass of M82 was chosen to be three times that of the unbound mass reported in A. Smercina et al. (2020), with the error ranging from one to five times the unbound mass. The TNG50 metallicities in the right panel were found using the green best-fit slope in the left panel.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: Raw (left), background (center), and background-subtracted (right) CMDs for each of the selections shown in Figure 5, with the AGB and TRGB selections shown in the rightmost panel of each. The color bars show the stars/bin in each of the background-subtracted CMDs. Counts in these selections and their corresponding ratios and t 90 are shown in Table 1.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: Two TNG50 analogs of NGC 3077 that have a similar mass, are orbiting around an M81-like host, and exhibit ongoing star formation in their cores. The upper panel shows a t 90 in the tidal tails of roughly 2 Gyr, while the lower exhibits a much older, 8 Gyr old population. The SFH of the NGC 3077 analogs’ centers and analogs’ tails are shown in the histograms on the right.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: The interpolated metallicity map used to determine the [M/H] of our spatial selections. The left, blue line corresponds to the most metal-poor isochrone used to determine metallicity ([M/H] = −2.15), and the right, orange line is the metal-rich ([M/H] = 0.5). The green line connecting the two isochrones is the TRGB in the metallicity range used for our interpolation (−2.15 < [M/H] < 0.5).
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: A timeline showing the star formation timescales in the outskirts of the central galaxies in the M81 group. The starburst timescales for M82 and NGC 3077 (red) are taken from various literature sources (NGC 3077: M. S. Yun 1999, M82: L. J. Smith et al. 2007; D. F. de Mello et al. 2008), which we adopt to be the time at which M82 and NGC 3077 experienced the strongest tidal forces, i.e., when disruption began. The final merger of these three galaxies will occur in 2 Gyr, as estimated by A. Smercina et al. (2020).
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: The raw, background, and background-subtracted CMDs of the selections shown in Figure 11, presented in the same manner as those in Figure 7. The shifted selections are shown in red and blue, and the originals are in cyan and orange. The isochrones are 100 Myr helium-burning populations with various metallicities.
Paper: A Timeline of the M81 Group: Properties of the Extended Structures of M82 and NGC 3077
Authors: Benjamin N. Velguth, Eric F. Bell, Adam Smercina, Paul Price, Katya Gozman, Antonela Monachesi, Richard D'Souza, Jeremy Bailin, Roelof S. de Jong, In Sung Jang, Colin T. Slater
Figure caption: The minor axis and background selections of M81's minor axis, shown in the same manner as those in Figure 5.
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: From top to bottom, Hα/Hβ, Hγ/Hβ, Hδ/Hβ, and τ Lyβ  as a function of thickness of the nebula. The left and right panels correspond to the blackbody temperatures of 20,000 and 40,000 K, respectively. The dashed and solid lines represent the values calculated at n e = 102 and 105 cm−3, respectively. The gray and black lines indicate the values calculated at ﹩\mathrm{log}U=-2﹩ and −1, respectively. τ Lyγ , τ Lyδ , and τ Ly8 are lower than τ Lyβ  by amounts corresponding to the length of the arrows in the bottom-left panel. The orange (red) line and shaded region denote the observed Balmer line ratios and their uncertainties of GS-NDG-9422 (RXCJ2248-ID), respectively. The horizontal lines in the bottom panels denote τ  λ  = 1, above which the line becomes optically thick.
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: Comparisons between the observed Balmer line ratios and theoretical Balmer line ratios including the effects of the optical depths of the Balmer lines. The squares are the same as Figure 1. The black crosses indicate the Case B values for T e = 20,000 K and n e = 103 cm−3. The cyan, blue, and purple lines and circles denote the Balmer line ratios, including the effects of the optical depths with A V = 0, 1, and 3, respectively. The numbers shown beside the circles represent the values of logN 2. The cyan, blue, and purple shaded regions in the left panel indicate the regions that can be reproduced by interstellar shock (J. M. Shull & C. F. McKee 1979) in the case of A V = 0, 1, and 3, 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: Comparisons of the observed and Case B Balmer line ratios. The orange and red squares represent the values of GS-NDG-9422 (A. J. Cameron et al. 2024) and RXCJ2248-ID (M. W. Topping et al. 2024). The gray shaded regions denote the Case B values, where we change the electron temperature from 15,000 to 25,000 K and the electron density from 101 to 105 cm−3. In the right panel, the Case B values of a 3 × 3 grid of T e and n e are shown. The cyan, blue, and magenta points represent the values of T e = 15,000, 20,000, and 25,000 K, respectively. The circles, triangles, and inverted triangles show the values of n e = 101, 103, and 105 cm−3, respectively. The black arrows represent the directions of the effect of the dust extinction and the Balmer decrement anomalies.