adsabs/AstroCLIMB huggingface dataset:
Paper: Investigating the Potential of LS 5039 as a Triple System Using Fermi-LAT Data
Authors: Lujun Zeng, Mengqing Zhang, Chongyang Ren, Pengfei Zhang, Jingzhi Yan
Figure caption: LSP power spectra (black histogram) derived from the 0.1–500.0 GeV AP light curve of 4FGL J1826.2−1450. Left panel: the three periodicities, P H, P orb, and P L, are in close proximity. The gray dashed–dotted line marks the location of the 53.4 day precession period of the Fermi-LAT orbit. Right panel: LSP power spectrum zoomed in the left. The green dotted and pink dashed lines indicate the signals of P H and P L, respectively. The horizontal red dashed and blue dashed–dotted lines stand for 5σ and 7σ confidence levels, respectively. HESS results drawn from Figures 2 and 3 of F. Aharonian et al. (2006) are shown in the inset plot.
Paper: Investigating the Potential of LS 5039 as a Triple System Using Fermi-LAT Data
Authors: Lujun Zeng, Mengqing Zhang, Chongyang Ren, Pengfei Zhang, Jingzhi Yan
Figure caption: LSP power spectra for 4FGL J1827.4−1445 (black histogram) and 4FGL J1829.4−1500c (orange histogram). The vertical green and pink arrows show the positions of the two signals of P H and P L. The gray dashed–dotted line is the precession period of the Fermi-LAT orbit, and the red dashed line is the 5σ confidence level.
Paper: Investigating the Potential of LS 5039 as a Triple System Using Fermi-LAT Data
Authors: Lujun Zeng, Mengqing Zhang, Chongyang Ren, Pengfei Zhang, Jingzhi Yan
Figure caption: LS 5039’s energy-dependent LSP power spectra, where the black, red, and green histograms stand for the spectra constructed with the 0.1–0.3, 0.3–1.0, and 1.0–500.0 GeV AP light curves, respectively. As in Figure 2, the red dashed and blue dashed–dotted lines are the 5σ and 7σ confidence levels.
Paper: Investigating the Potential of LS 5039 as a Triple System Using Fermi-LAT Data
Authors: Lujun Zeng, Mengqing Zhang, Chongyang Ren, Pengfei Zhang, Jingzhi Yan
Figure caption: Phase-resolved light curves derived from the 0.1–500.0 GeV Fermi-LAT events, folded over the periods P H (top panel) and P L (bottom panel). Both panels share the same y-axis label.
Paper: Dynamics Around Supermassive Black Holes: Extreme-mass-ratio Inspirals as Gravitational-wave Sources
Authors: Barak Rom, Itai Linial, Karamveer Kaur, Re'em Sari
Figure caption: Orbital dynamics in the (r, r  p ) phase space, where r is the semimajor axis and r  p  is the periapsis. The dashed black line distinguishes between the two-body-scattering-dominated region and the GW-dominated one (Equation (7)); above it, the scattering leads to a diffusion dominantly in the r  p -direction (as encapsulated by the shaded vertical blue funnel), while below it, GW emission efficiently shrinks and circularizes the orbit (along the horizontal shaded funnel). The red dashed–dotted line marks the mostly bound orbit, with r  p  = 4R  s , and the yellow dashed–dotted line represents the critical semimajor axis R  c , (Equation (8)), separating EMRI progenitors (with r ≲ R  c ) and plunge progenitors (with r ≳ R  c ). The gray lines demonstrate examples of trajectories leading to an EMRI or a plunge, according to their initial semimajor axis.
Paper: Dynamics Around Supermassive Black Holes: Extreme-mass-ratio Inspirals as Gravitational-wave Sources
Authors: Barak Rom, Itai Linial, Karamveer Kaur, Re'em Sari
Figure caption: Steady-state distributions of the sBHs (blue lines) and the stars (yellow lines), as given by Equations (15) and (19). We consider an SMBH with M BH = 4 × 106 M ⊙ and sBH number fractions f • = 10−3 (solid lines) and f • = 10−4 (dashed lines), as defined in Equation (11). We plot n(r) × r 3/2, which corresponds to the commonly used phase-space density, f(E). The star distribution extends from R  h  to the tidal radius, R  t  (Equation (18)), while the sBHs can reach R ISCO = 3R  s .
Paper: Dynamics Around Supermassive Black Holes: Extreme-mass-ratio Inspirals as Gravitational-wave Sources
Authors: Barak Rom, Itai Linial, Karamveer Kaur, Re'em Sari
Figure caption: Characteristic strain of EMRIs as a function of the observed frequency. The black line is the LISA sensitivity curve (T. Robson et al. 2019) and the colored lines present contours of the observed source numbers, between 1 and 105, in a logarithmic frequency bin. The dashed lines present an analytical estimation at z ≪ 1 (Equation (40)), scaling as f 1/60 at low frequencies and f −19/60 at high frequencies. The color bar presents the source-frame SMBH mass that corresponds to the average redshift of the observed sources. The purple dotted line depicts the average SMBH mass M 〈z〉 = 105 M ⊙.
Paper: Dynamics Around Supermassive Black Holes: Extreme-mass-ratio Inspirals as Gravitational-wave Sources
Authors: Barak Rom, Itai Linial, Karamveer Kaur, Re'em Sari
Figure caption: A realization of the observed EMRIs; each black line represents an EMRI, chosen according to the distribution given in Equation (35), assuming an observation time T LISA = 4 yr. As in Figure 5, the black thick line is the LISA sensitivity curve and the colored lines present contours of the observed source numbers. The color bar presents the average redshift of the observed sources. The white line corresponds to the GWB (Equation (41)), assuming a limit of one source per four frequency bins, δ f = 1/T LISA. Roughly 2 × 103 resolvable sources lie above the red line, which depicts the ﹩{\left.\mathrm{SNR}\right|}_{\mathrm{th}}=20﹩ threshold.
Paper: Dynamics Around Supermassive Black Holes: Extreme-mass-ratio Inspirals as Gravitational-wave Sources
Authors: Barak Rom, Itai Linial, Karamveer Kaur, Re'em Sari
Figure caption: EMRI eccentricity probability density function at the mostly bound orbit. The blue line corresponds to the case where the sBH number fraction is larger than the critical value, ﹩{{\rm{f}}}_{\bullet }\geqslant {f}_{\bullet }^{c}﹩, where the distribution is independent of the specific value of f •, and peaks at e ≃ 0.08. The red line exhibits an example of the complementary case, ﹩{{\rm{f}}}_{\bullet }={10}^{-5}\lt {f}_{\bullet }^{c}﹩, where the distribution peaks at e  I  ≃ 0.04 (as given by Equation (29)) and falls steeply, as ﹩p(e\gtrsim {e}_{I})\mathop{\propto }\limits_{\sim }{e}^{-49/19}﹩. In both cases, the distributions satisfy p(e ≪ 1) ∝ e 5/19.
Paper: Dynamics Around Supermassive Black Holes: Extreme-mass-ratio Inspirals as Gravitational-wave Sources
Authors: Barak Rom, Itai Linial, Karamveer Kaur, Re'em Sari
Figure caption: EMRI-to-plunge ratio as a function of the sBH number fraction, assuming sBHs of mass m • = 10M ⊙ (blue line) and m • = 30M ⊙ (red line), as calculated from Equations (20) and (21). The dashed–dotted lines mark the critical number density, ﹩{f}_{\bullet }^{c}﹩ (Equation (12)), for each sBH mass, with respective colors, and the dashed lines present the ratio in the limiting cases of scarce (﹩{{\rm{f}}}_{\bullet }\ll {f}_{\bullet }^{c}﹩) and abundant (﹩{{\rm{f}}}_{\bullet }\gg {f}_{\bullet }^{c}﹩) sBH populations (Equations (22) and (23)), respectively.
Paper: Astrophysical Properties of the Sirius Binary System Modeled with MESA
Authors: Momin Y. Khan, Barbara G. Castanheira
Figure caption: H-R diagram for the evolutionary tracks of Sirius A for a high metallicity of [Fe/H] = 0.4 (or Z = 0.034) determined by T. M. Sitnova et al. (2018) (blue line), solar metallicity (orange line), and another model with supersolar of Z = 0.015 estimated from C. R. Cowley et al. (2016) (green line), in comparison to the observed luminosity and T eff. None of the high metallicity models is in agreement with the current position of Sirius A in the H-R diagram.
Paper: Astrophysical Properties of the Sirius Binary System Modeled with MESA
Authors: Momin Y. Khan, Barbara G. Castanheira
Figure caption: H-R diagram for the evolutionary tracks calculated with MESA for Sirius A. We have used different initial metallicities from Z = 0.0115 (yellow line, top left) to 0.0150 (dark red, bottom right), in steps of 0.0005. Compared to the observed luminosity and determinations of T eff, our best fit is a subsolar metallicity of ﹩Z=0.0124{\pm }_{0.00077}^{0.00073}﹩.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption:  L [C II]/L CO(1−0) plotted vs. f AGN (left), L [N II]205 μm/L [C II] (middle), and [O III] 88 μm-to-[N II] 122 μm flux ratio. Arrows in the middle and right panels, respectively, indicate the upper and lower limits of the x-axis. The solid lines are linear fits to the data. The correlation coefficient and probability of the null hypothesis are also given in each panel.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption: CO(1−0) line luminosity plotted against [C II] line luminosity. Red and green symbols show (U)LIRGs and normal galaxies, respectively. Open diamonds are early-type galaxies from R. C. Lapham et al. (2017), plus signs represent local main-sequence galaxies from G. Accurso et al. (2017b), asterisks demonstrate Lyman-break analogs at z ∼ 0.2 from A. Contursi et al. (2017), crosses and squares respectively display local (U)LIRGs from T. Díaz-Santos et al. (2017) and D. Farrah et al. (2013), stars are the H-ATLAS star-forming sources at z ∼ 0.02–0.2 from E. Ibar et al. (2015), circles show z ∼ 0.3 (U)LIRGs from G. E. Magdis et al. (2014), triangles and bowties are high-redshift (z > 1) sources, including (U)LIRGs, QSOs and SMGs, respectively observed in CO(1−0) (S. Malhotra et al. 2001; C. L. Carilli & F. Walter 2013; G. E. Magdis et al. 2014; T. D. Rawle et al. 2014; S. Malhotra et al. 2017; Z.-Y. Zhang et al. 2018b; T. K. D. Leung et al. 2019; D. A. Riechers et al. 2020), and in CO(2−1) (C. L. Carilli & F. Walter 2013; C. Ferkinhoff et al. 2014; M. T. Huynh et al. 2014; R. Pavesi et al. 2018, 2019; D. A. Riechers et al. 2020; D. J. M. Cunningham et al. 2020). The fitted trends are annotated with corresponding correlation coefficients (ρ) and probability of a null hypothesis (p) and are plotted as red solid, green dotted, and black dashed lines for (U)LIRGs, normal galaxies, and the whole sample, respectively.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption: Comparison of the distribution of the [C II]-to-CO luminosity ratios for various samples. Top: The whole sample (black), (U)LIRGs (red), and normal galaxies (green), with the result of a Gaussian fit to the data superposed. The number of members and mean L [C II]/L CO(1−0) ratio and scatter from the Gaussian fit for each sample are also labeled with corresponding colors. Middle: ETGs (green solid line), MS galaxies (green dashed–dotted line), local (red solid line), z ∼ 0.2–0.3 (red dotted line), and z > 1 (red dashed line) (U)LIRGs. Bottom: Galaxy-integrated results of our whole sample (black solid line), Galactic H II regions and extragalactic starburst nuclei (G. J. Stacey et al. 1991; blue dashed line), and Galactic GMCs and nonstarburst nuclei/regions (G. J. Stacey et al. 1991; D. Fadda et al. 2021; blue solid line). The arrows in the middle and bottom panels indicate the corresponding mean values.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption: [C II]-to-CO luminosity ratio plotted versus metallicity for dwarf (D. Cormier et al. 2015; M. Grossi et al. 2016; S. C. Madden et al. 2020; R. Minchin et al. 2022) and massive galaxies. QSOs and AGNs are excluded from the plot. For comparison, the overplotted lines show α CO as a function of metallicity from Wolfire et al. (2010, purple dashed line), Accurso et al. (2017b, black dotted line), and Madden et al. (2020, red solid line), assuming a constant α [C II] of 34.9 M ⊙/L ⊙.
Paper: Astrophysical Properties of the Sirius Binary System Modeled with MESA
Authors: Momin Y. Khan, Barbara G. Castanheira
Figure caption: Comparison between models and the observations of Sirius B in L–T eff plane. The best model (yellow star) was found by the minimization of the normalized luminosity, spectroscopic T eff, and astrometric mass (not displayed in this plot). The models are for the calculated metallicity (red dots) and upper and lower limits (blue and green dots, respectively. The spread of the models becomes large for progenitor masses over 6.2 M ⊙.
Paper: Astrophysical Properties of the Sirius Binary System Modeled with MESA
Authors: Momin Y. Khan, Barbara G. Castanheira
Figure caption: Comparison between models and the observations of Sirius B in L–M plane. Just as before, the best model (yellow star) was found by the minimization of the normalized luminosity, spectroscopic T eff, and astrometric mass. This plot highlights that smaller initial masses of Sirius B do not fit the spectroscopic parameters very well. With this, we can put a lower limit on acceptable progenitor masses.
Paper: Astrophysical Properties of the Sirius Binary System Modeled with MESA
Authors: Momin Y. Khan, Barbara G. Castanheira
Figure caption: Comparison between models and the observations of Sirius B in M–T eff plane. Despite there being many models that fall into the range of acceptable temperature, the mass is so well constrained that it limits the possible solutions.
Paper: Astrophysical Properties of the Sirius Binary System Modeled with MESA
Authors: Momin Y. Khan, Barbara G. Castanheira
Figure caption: H-R Diagram for Sirius B for the best-fit metallicity, including the upper and lower bounds, for a progenitor mass of 6.0 M ⊙. The white dwarf cooling track agrees with the current placement of Sirius B on the luminosity temperature plane.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Panels (i.c), (ii.c), and (iii.c) show the mixing ratio of CH4, CO, and NH3, respectively, at 1 mbar pressure level and solar metallicity, for a range of equilibrium temperatures. The dashed, dotted–dashed, and dotted lines are the mixing ratios for ﹩{\mathrm{log}}_{10}({K}_{{zz}})﹩ = 8, 10, and 12, respectively, for T int = 150 K (green lines) and T int = 450 K (blue lines). The solid lines are the thermochemical equilibrium mixing ratio. In panel (i.a), the solid black lines are the thermal profile for a range of equilibrium temperatures and T int = 150 K, while the solid red lines are the contours of the thermochemical equilibrium abundance of CH4. The dashed, dotted–dashed, and dotted lines are the quenched curves for ﹩{\mathrm{log}}_{10}({K}_{{zz}})﹩ = 8, 10, and 12, respectively (see Figure 9 of V. Soni & K. Acharyya 2023a for quenched curves). Panel (i.b) is the same as panel (i.a), but for T int = 450 K. Panels (ii.a) and (ii.b) are the same as panels (i.a) and (i.b), respectively, but for CO. Panels (iii.a) and (iii.b) are the same as panels (i.a) and (i.b), respectively, but for NH3.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption:  L [C II]/L CO(1−0) plotted against sSFR/sSFRMS. The solid purple line shows the relationship obtained with the locfit function using all data points, while the dashed line displays the relationship estimated by excluding the two apparent outliers (i.e., two ETGs with Δ(MS) < − 1 and ﹩\mathrm{log}({L}_{[{\rm{C}}\,{\rm\small{II}}]}/{L}_{\mathrm{CO}})\gt 3.7﹩). The correlation coefficient and probability of the null hypothesis, computed separately for ﹩\mathrm{log}(\mathrm{sSFR}/{\mathrm{sSFR}}_{{MS}})\leqslant 0﹩ and ﹩\mathrm{log}(\mathrm{sSFR}/{\mathrm{sSFR}}_{{MS}})\gt 0﹩, are also given in the plot.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption: Distributions of L [C II]/L CO(1−0) from the “WK2020” (left; M. W. Pound & M. G. Wolfire 2023) and “KOSMA-tau” (right; M. Röllig et al. 2013; M. Röllig & V. Ossenkopf-Okada 2022) PDR model sets (Z = Z ⊙ and ζ CR = 2 × 10−16 s−1), overlaid with the Gaussian fitting results. The black, red, and green colors show the results of models having G 0/n = 10−2 − 102, 10−1.5 − 101.5, and 10−1 − 101 cm3, respectively.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption: Infrared luminosity surface density ΣIR plotted vs. L [C II]/L IR (top), L CO(1−0)/L IR (middle) and L [C II]/L CO(1−0) (bottom). All the plots span 2.5 dex vertically for direct comparison. In each panel, arrows indicate lower limits of the x-axis, and the solid line shows the relation computed using the locfit.censor function. The correlation coefficient and probability of the null hypothesis are also given in the bottom panel for the L [C II]/L CO(1−0)-ΣIR relation.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The transit depth excess due to vertical mixing in the exoplanet atmosphere from our 1D chemical kinetics model run (T equi = 500–2000 K; T int = 150, 250, 350, 450, and 550 K; ﹩{\mathrm{log}}_{10}({K}_{{zz}})﹩ = 9; surface gravity = 1000 cm s−2). The color contours from blue to red represent the transit depth excess due to CH4 (panels (a)–(e)) and NH3 (panels (f)–(j)). The white-to-black colormesh plots in all the panels represent the total transit depth excess.
Paper: Ionized Carbon in Galaxies: The [C II] 158 μm Line as a Total Molecular Gas Mass Tracer Revisited
Authors: Yinghe Zhao, 应和 赵, Jiamin Liu, Zhi-Yu Zhang, Thomas G. Bisbas
Figure caption: Distribution of L [C II]/L CO(1−0) from S. C. Madden et al. (2020) PDR model sets (Z = 0.05 − 1 Z ⊙, G 0 = 101.25 − 104.06, and n = 101 − 104 cm−3), overlaid with the Gaussian fitting results. The black, red, and green colors show the results of models having A  V  = 6.5 − 10, 7 − 9, and 7.5 − 8.5 (all with mean A  V  ∼ 8), respectively.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The mass mixing ratios for a test exoplanet (model B in the Appendix: ﹩{\mathrm{log}}_{10}(g/\mathrm{cm}\ {{\rm{s}}}^{-2})﹩ = 3, ﹩{\mathrm{log}}_{10}({K}_{{zz}}/{\mathrm{cm}}^{2}\ {{\rm{s}}}^{-1})﹩ = 9, [M/H] = 0, internal temperature = 200 K, and equilibrium temperature = 1000 K). The solid lines are the output of the 1D chemical kinetics model, and the dashed lines are the output of the disequilibrium model function.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Block diagram of the QLR. The model calculates the output spectrum for an input planet spectrum and its parameters. The parameter estimation method (PyMultiNest) is used to find the parameter distribution and calculate the best-fit parameters for the input spectrum. The blue boxes are the steps that are done by petitRADTRANS, and the green boxes are the steps carried out by our disequilibrium model function.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The retrieved values of [M/H], K  zz , and T int for different values of metallicity and equilibrium temperature with ﹩{\mathrm{log}}_{10}({K}_{{zz}})=9﹩, T int = 200 K, and g = 1000 cm s−2. The rows from top to bottom correspond to metallicity values of −1, −0.4, 0.2, 0.8, and 2. The blue horizontal lines show the true values of the parameters.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Left column: the top panel shows the vertical volume mixing ratio for A1 (thermochemical equilibrium abundance) and A2 (disequilibrium abundance) in solid and dashed lines, respectively. The bottom panel shows the transmission spectra for A1 and A2 in solid blue and red lines, respectively. Right column: similar to the left column, but for B1 and B2.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The retrieved values of [M/H], K  zz , and T int for different values of eddy diffusion coefficient and equilibrium temperature with T int = 200 K, g = 1000 cm s−2, and solar metallicity. The rows from top to bottom correspond to ﹩{\mathrm{log}}_{10}({K}_{{zz}})﹩ values of 4, 6, 8, 10, and 12. The blue horizontal lines show the true values of the parameters.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The best-fit model transit spectrum generated from the CCR (panels (a)–(d)) and QLR (panels (e)–(h)) models for the cases A1 (first row), A2 (second row), B1 (third row), and B2 (fourth row) for the synthetic JWST observation of the respective model run.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The solid blue line shows the rebinned transit spectrum of A1 (top left panel), A2 (top right panel), B1 (bottom left panel), and B2 (bottom right panel). The filled red circles show the simulated JWST observed spectrum, and the black vertical lines are the associated errors. The three solid horizontal colored lines (yellow, brown, and green) show the wavelength coverage of the labeled JWST instrument.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The retrieved values of [M/H], K  zz , and T int for different values of surface gravity and equilibrium temperature with ﹩{\mathrm{log}}_{10}({K}_{{zz}})=9﹩, T int = 200 K, and solar metallicity. The rows from top to bottom correspond to surface gravity values of 3, 10, 30, 100, and 300 m s−2. The blue horizontal lines show the true values of the parameters.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The corner plot (posterior distribution) of the parameters retrieved for the model run from CCR. Top left: A1; bottom left: A2; top right: B1; bottom right: B2. T  i  is the internal temperature, and T eq is the equilibrium temperature.
Paper: Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The corner plot (posterior distribution) of the parameters retrieved for the model run from QLR. Top left: A1; bottom left: A2; top right: B1; bottom right: B2. T  i  is the internal temperature, and T eq is the equilibrium temperature.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Variation of the scale height h  z  and vertical scale parameter z 0 = 2h  z  with inclination i obtained from different inclination angles of the gSd model of the GalMer database. Left panel: values of h  z  derived using the 2D method. Right panel: values of z 0 obtained using the 1D method compared to those from the Galfit 2D method (solid blue line). The ensuing relation can be used to correct for inclination for results from both the 1D and 2D methods for galaxies of inclination 80° ≤ i ≤ 90°.
Paper: On the Stellar Disk Vertical Scale Height of Edge-on Galaxies from S4G
Authors: Notahiana Ranaivoharimina, T. Randriamampandry, Jing Wang, K. Menéndez-Delmestre, T. S. Gonçalves
Figure caption: Top panels: uncleaned image of the galaxy UGC 09977 as seen in the 3.6 μm band. Bottom panels: background-subtracted, cleaned, and rotated image of the above panels. A mask has also been applied to eliminate remaining foreground stars. Images on the left are scaled linearly; those on the right show log-scaled maps. All images are in units of MJy sr−1.