adsabs/AstroCLIMB huggingface dataset:
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The parameters extracted from the time-averaged data of the magnetic dipole study (left panel) and the accretion rate study (right panel). The parameters are magnetospheric radius Rm, outflow rate ﹩{\dot{M}}_{{\rm{out}}}﹩, luminosity L (computed in the optically thin region), and the beaming factor, which is shown as 1/b, from top to bottom panels, respectively. The beaming factor is computed at two radii, 250 rg and 500 rg, in the magnetic dipole study, and at 500 rg in the accretion rate study, and the outflow rate and luminosity are computed at radius 100 rg. In the accretion rate study (right), the parameters are shown for two magnetic dipoles; the red x markers and the blue circles denote the magnetic dipoles 3 × 1010 G and 1 × 1010 G, respectively.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Theoretically calculated gamma-ray spectra of the MR-SN model shown in Figure 1, assuming a location of 10 kpc at time t = 10 days postexplosion. Instrument sensitivities are also scaled to 10 days of observing time. The first (top) panel shows the overall spectra and instrument sensitivity limits. The second panel breaks down the total spectrum into the contributions from different nuclear decays: beta minus and the combination of beta plus and ϵ capture. Although the light curve is dominated by 56Ni and 56Co gammas from beta plus decay at this early time, some r-process isotopes, such as 131I, 132I, and 132Te, dominate in a few energy windows. The third and fourth panels indicate prominent lines for each type of decay.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Spectra of the MR-SN at 10 kpc at 100 days postexplosion. At this time, the decays of 56Ni and 56Co are still significant, and the annihilation contribution from para-positronium and ortho-positronium is strong. However, between 0.55 and 0.75 MeV, there is a window for weak r-process isotopes such as 103Ru, 106Rh, 125Sb, and 95Nb. The style is the same as Figure 10, although telescope sensitivities are scaled to 100 days of observation time.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Spectra of the MR-SN at 10 kpc at 6 yr after the explosion. The energy windows for the r-process lines are significantly expanded, and the isotopes 125Sb and 106Rh dominate the region between 0.55 and 0.75 MeV. The contributions from 56Ni and 56Co are significantly reduced at this time due to their relatively short half-lives, and the annihilation contribution primarily stems from positrons produced in the beta plus decay of 44Sc. Telescope sensitivities are scaled to 1 yr of observation time.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Similar to Figure 7, but for Vela SNR. For Vela, we assume that the jet material is not mixed uniformly, so the jet ejecta resides within the angular resolution of the detector. To estimate the reduction in sensitivity in the case where the ejecta are uniformly mixed, we scale the INTEGRAL/SPI line (dashed gray) by the ratio of the angular resolution of the instrument to the angular extent of Vela.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Sketch of the geometric setup used to estimate the positron annihilation signal. The ejecta is represented as a sphere of radius Rmax, shown as the dark purple circle. At a radial coordinate r, we define an auxiliary ℓ-sphere with radius ℓ and elevation angle θ, shown as the magenta circle. The two spheres intersect at the elevation angle θℓ, beyond which positrons would escape the ejecta. The solid angle subtended by the ℓ-sphere for θ < θℓ corresponds to the trajectories of positrons that come to rest and annihilate within the ejecta. This region is illustrated with medium purple shading.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Spectra of the MR-SN at 10 kpc at 100 days after the explosion, similar to the second panel of Figure 11 but with vej = 0.08c.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Similar to Figure 7, but for SN 1987A. The 1.157 MeV 44Sc line previously reported by INTEGRAL in SN 1987A (S. A. Grebenev et al. 2012) is now weaker due to the currently older age of the remnant. The 68 keV and 78 keV lines from 44Ti have been detected by NuSTAR (S. E. Boggs et al. 2015). The 44Sc and 44Ti lines are also expected in neutrino/advection-driven CCSN.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Spectra of the MR-SN at 10 kpc at 10 days after the explosion, similar to the second panel of Figure 10 but with vej = 0.08c.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Spectra of the MR-SN at 10 kpc at 6 yr after the explosion, similar to the second panel of Figure 12 but with vej = 0.08c.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Simulations at the magma ocean–atmosphere interface of K2-18b assuming real versus ideal gas behavior. As in Figure 6, the total hydrogen budget expressed as a fraction of the planet’s mass (Mp) varies from 0.1% to 3%, while other input parameters are fixed: Tsurface = 3000 K, C/H (by mass) = 0.32 (which is ∼100× the solar ratio) and fO2 at ΔIW = −3. Unlike Figure 6, here the x-axis corresponds to the total hydrogen mass fraction of the planet, expressed as a percentage of K2-18b’s mass. The solid lines correspond to the cases assuming real gases and the dashed lines are for cases with ideal gas behavior. (a) Pressures of volatile species in the atmosphere (GPa) and the total atmospheric pressure (gray). (b) C/H (purple, left y-axis) and C/O (teal, right y-axis) in the atmosphere. (c) Solubility of each volatile species (wt%, i.e., fraction of the planet’s mantle mass). (d) Fugacity coefficient (ϕ) of each volatile species. The coefficient for ideal behavior (gray dashed line) is unity for all volatiles.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Cooled atmospheres at 280 K for TRAPPIST-1e, starting with the elemental abundances in the atmosphere for a fully molten mantle and a surface temperature of 1800 K. Points are colored by oxygen fugacity of the initial, high-temperature atmosphere expressed relative to the IW buffer, and sized in proportion to log10 C/H for the fully molten starting state. Condensed inventories of water, graphite, and α-sulfur are normalized by the Earth’s present-day ocean mass (EO). Other scatter plots show the VMR of major species in the atmosphere, total pressure, and molar mass. Density levels indicate areas with high likelihood in the scatter plots, while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare with the cool atmospheres derived from a partially molten mantle in Figure B4.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: For an early TRAPPIST-1e with a fully molten mantle (surface temperature of 1800 K), scatter plots of atmospheric and total C/H, C, H, and S dissolved in the interior relative to the total inventory of the element by mass, pressure, and molar mass. Points are colored by oxygen fugacity expressed relative to the IW buffer and sized in proportion to log10 C/H. Density levels indicate areas with high likelihood in the scatter plots, while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare to a partially molten mantle in Figure B3.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: For an early TRAPPIST-1e with a fully molten mantle (surface temperature of 1800 K), scatter plots of atmospheric molar abundance, total pressure, and molar mass, for N2 and minor species: ClH, S2, H2S, NH3, and Cl2. Points are colored by oxygen fugacity expressed relative to the IW buffer and sized in proportion to log10 C/H. Density levels indicate areas with high likelihood in the scatter plots, while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare to a partially molten mantle in Figure B2.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: For an early TRAPPIST-1e with a fully molten mantle (surface temperature of 1800 K), scatter plots of atmospheric molar abundance, total pressure, and molar mass for major species. Points are colored by oxygen fugacity expressed relative to the IW buffer and sized in proportion to log10 C/H. Density levels indicate areas with high likelihood in the scatter plots, while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare to a partially molten mantle in Figure B1, noting that the extent of the axes for H2O and CH4 is different.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Comparison between the mass fraction of volatile elements in the (a) atmosphere and (b) interior, of K2-18b for real (solid lines) and ideal (dashed lines) gas behavior for hydrogen (blue), carbon (orange), and their sum (gray). In (b), the sum of H+C overlaps with H, since it is the dominant dissolved volatile element in both the real and ideal gas cases. The total hydrogen budget expressed as a fraction of planet’s mass (Mp) varies from 0.1% to 3%, while other input parameters are fixed; Tsurface = 3000 K, C/H (by mass) = 0.32 (which is ∼100× the solar ratio) and fO2 at ΔIW = −3.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: The effect of planetary surface radius and total mass on the atmospheric speciation of K2-18b at the magma ocean–atmosphere interface: Tsurface = 3000 K, the oxygen fugacity is fixed at ΔIW = −3, the total hydrogen mass of the planet is 3% of the planet’s mass, and C/H is 100× solar. (a) Pressures (in GPa) of the gas species assuming real gas EOS (solid lines) and ideal behavior (dashed lines) as a function of the surface radius of the planet which varies from 1.76 to 2.61 R⊕, where the planet mass is constant at 8.63 M⊕. The gray horizontal bar shows typical uncertainties on planetary radius measurements of 5% and 10% for a 2 R⊕ planet. (b) Pressures as a function of planet mass varying from 4 to 9 M⊕, where the planetary surface radius is constant at 1.76 R⊕. The gray horizontal bar shows typical uncertainties on planetary mass measurements of 15 and 30% for a 7 M⊕ planet.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Histogram of log10 C/H in the atmosphere, computed by moles, for a partially molten mantle (10% melt) (Appendix B) and fully molten mantle (main text), both at 1800 K and each based on 10,000 simulations. For reference, the “fully solid” case shows the total C/H imposed as an initial condition that is available to partition between the silicate mantle and atmosphere. Interior dissolution both increases C/H in the atmosphere and broadens its distribution, and for a fully molten mantle there is a long tail to low C/H.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: The PAH map (by Clark et al. 2025, in preparation) here on the left shows the integrated intensity of the 6.2 μm feature (integrated over the 6.12–6.5 μm range after continuum subtraction). A comparison with the CH﹩{}_{3}^{+}﹩ map is shown on the right. Locations marked by A and B represent the two bright spots on the CH﹩{}_{3}^{+}﹩ map. The maps are centered at the central star (R.A. = 17h:13m;44﹩\mathop{.}\limits^{{\rm{s}}}﹩488 ± 0﹩\mathop{.}\limits^{{\rm{s}}}﹩004, decl. = −37°:06﹩{}^{{\prime} }﹩:11﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩76 ± 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩.03) whose position is indicated by the white circle at the center.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Comparison of the integrated surface brightness maps of CH﹩{}_{3}^{+}﹩, H2, and 12CO. (a) 12CO (2–1, 230 GHz, by  (b) Two color composite image: CH﹩{}_{3}^{+}﹩ (red) and 12CO  (cyan). (c) H2 0-0 S5 at 6.908 μm. (d) Two color composite image: CH﹩{}_{3}^{+}﹩ (red) and 12CO (cyan). Locations marked by A and B represent the two bright spots on the CH﹩{}_{3}^{+}﹩ map. The maps are centered at the central star (R.A. = 17h:13m;44﹩\mathop{.}\limits^{{\rm{s}}}﹩488 ± 0﹩\mathop{.}\limits^{{\rm{s}}}﹩004, decl. = −37°:06﹩{}^{{\prime} }﹩:11﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩76 ± 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩03) whose position is indicated by the yellow circle at the center.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Normalized surface brightness profiles of CH﹩{}_{3}^{+}﹩, H2, PAH 6.2 μm (by Clark et al. 2025, in preparation), CO, and HCO+ (by M. Baez et al. 2025, submitted) along the cut. Offset is measured in arcsec from the position of the central star (R.A. = 17h:13m;44﹩\mathop{.}\limits^{{\rm{s}}}﹩488 ± 0﹩\mathop{.}\limits^{{\rm{s}}}﹩004, decl. = −37°:06﹩{}^{{\prime} }﹩:11﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩76 ± 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩03).
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: HCO+ map (by M. Baez et al. 2025, submitted) is shown in blue on the left, and an overlay of the CH﹩{}_{3}^{+}﹩ map is shown in red on the right. Locations marked by A and B represent the two bright spots on the CH﹩{}_{3}^{+}﹩ map. The maps are centered at the central star (R.A. = 17:13:44.488 ± 0.004, decl. = −37:06:11.76 ± 0.03) whose position is indicated by the white circle at the center.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Gaussian fits to the 7.15 band used for the band ratio method to determine the temperature. The integrated surface brightness value at each aperture is listed in Table 1.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Gaussian fits to the 7.2 band used for the band ratio method to determine the temperature. The integrated surface brightness value at each aperture is listed in Table 1.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Integrated surface brightness map of H2 0–0 S(5) line at 6.908 μm. The green boxes and ellipses represent the 25 apertures used to study CH﹩{}_{3}^{+}﹩ emission in detail.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: JWST MIRI spectrum at aperture 1 (in black). The red line provides an example of the continuum adopted to fit the models to the observations.
Paper: Detecting Exoplanets beyond the Local Supercluster through Gravitational Waves with B-DECIGO and DECIGO
Authors: Wen-Long Guo, Li-Ming Zheng, Zhengxiang Li, Zong-Hong Zhu
Figure caption: B-DECIGO: dependence of the minimum detectable planetary mass ﹩{M}_{p}^{{\rm{\min }}}﹩ on the binary chirp mass Mc and component-mass ratio q at DL = 10 kpc (Galactic case). Contours show that higher Mc and more equal masses (q → 1) significantly improve sensitivity, driving ﹩{M}_{p}^{{\rm{\min }}}﹩ down to the super-Earth regime for favorable BNS-like systems.