adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Evolution of the CSM in the reference models RSG_A1_B1 (frames (a)–(f) in the upper panel) and MEE_A8 (lower panel); see Table 2 for details of the models. The frames in each panel illustrate the geometry and density distribution of the CSM at the labeled times. The isosurface delineates material with a particle number density n > 104 cm−3; the color indicates the density value (color legend provided on the right). In frame (f), the star at the center indicates the position of the SN explosion and the arrows denote the outflow velocity during the He star phase.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: As in Figure 10 but for the MEE models listed in Table 2.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Upper panels: X-ray lightcurve in the [0.5, 100] keV band synthesized from the RSG models compared with the observed lightcurve of SN 2014C. The lightcurves derived from the different RSG models are compared on the left. The reference model RSG_A1_B1 is also shown on the right with the contributions to emission from the shocked plasma from the nebula (dashed line) and the shocked ejecta (dotted line). Lower panels: corresponding to the upper panels, the plots show the evolution of average X-ray emission-weighted electron temperature.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: The 2D cross sections in the (x, z) plane show the spatial density distribution (in a logarithmic scale) of the SNR at the labeled times from RSG (upper panels) and MEE (lower panels) models. The symmetry axis of the bipolar blast wave aligns with the z-axis.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Comparison of actual (red symbols) and synthetic (blue symbols) spectra of SN 2014C collected with Chandra (upper panels) and NuSTAR (lower panels) at the labeled times. The synthetic spectra have been derived from model MEE_A8 at epochs close to those of observations, assuming an exposure time of 30 ks for Chandra and 50 ks for NuSTAR. The synthetic ideal spectra (black lines) and the contributions from different plasma components are also reported: shocked CSM (green) shocked ejecta (without the contribution of Fe; light blue) and shocked pure-Fe ejecta (magenta).
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Upper panels: X-ray lightcurves in the [0.5, 100] keV band, synthesized from model TOY_T50_D6.8, are shown for the entire emitting plasma (left panel), the shocked CSM (center panel), and the shocked ejecta (right panel). The figure compares simulation results at three different resolutions: low resolution (2563 grid points; yellow line), medium resolution (5123 grid points; red line), and high resolution (10243 grid points; magenta line). In the left panel, these results are compared with the observed lightcurve of SN 2014C, as obtained with Chandra and NuSTAR (blue and green symbols; D. Brethauer et al. 2022; B. P. Thomas et al. 2022). Lower panels: corresponding to the upper panels, these plots show the evolution of the average X-ray emission-weighted electron temperature.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Comparison between the Chandra and NuSTAR images and corresponding source regions in epoch 5. The Chandra 2.″5 radius extraction circle is marked in cyan, whereas the NuSTAR one with a radius of 60″ is marked in white. Left panel: Chandra 0.5–8 keV image. Right panel: NuSTAR 3–20 keV image. Note that the NuSTAR circle encloses the emission from other sources in the host galaxy.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Spectra as in Figure 16 but restricted to the [5, 10] keV band to show the details of the Fe Kα line.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Chandra (red data points) and NuSTAR (blue data points) spectra collected at the labeled times together with the VAPEC+VNEI models (green and magenta curves) resulting from the spectral fitting (see Section 5.4 and Appendix B).
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: As in Figure 16 for all Chandra observations.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Masses of the shocked plasma components contributing to the observed X-ray emission from SN 2014C, as derived from model MEE_A8: shocked CSM (solid line), shocked ejecta (dashed line), and shocked pure-Fe ejecta (dotted line).
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Synthetic X-ray emission map from model MEE_A8 in the [0.1–10] keV band at day 1310 as it would be captured by Chandra if SN 2014C were located at a distance of 600 pc.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: As in Figure 16 for all NuSTAR observations.
Paper: Observations of the Crustal Mini-magnetopause Reconnection at Mars
Authors: Xinzhi Qiu, Yiqun Yu, Jing Wang, Lihui Chai, Fan Gong, Longhui Liu, Jinbin Cao
Figure caption: The overview of the event on the dayside of Mars, occurring between 19:15:00 UT and 20:10:00 UT on 2016 October 26. (a) The MAVEN orbit projected onto the surface of Mars in geographic coordinates, overlaid with crustal magnetic fields (A. Morschhauser et al. 2014). The black star marks the subsolar point at 19:26:00 UT, the dashed line represents the spacecraft’s trajectory, the red solid line represents the crossing of the mini-magnetosphere, and the black solid line represents the crossing of the induced magnetosphere. (b) The magnitude and the three components of the observed magnetic field in the MSO coordinate. (c) The shape parameters for electrons moving toward (red) and away from (pink) the planet, respectively. (d) Ion energy spectrum by SWIA. (e) Ion energy spectrum by STATIC. (f) Ion mass spectrum by STATIC. (g) Electron energy spectrum by SWEA. (h) Thermal pressure (P th), magnetic field pressure (P B), and plasma beta value. Black and red dashed frames show observations of the induced magnetosphere and the mini-magnetosphere.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Graphic displaying an example aerosol’s Mie properties. Top-left panel: refractive index lab data as it varies with wavelength. The effective extinction cross section σ ext,eff (top-right panel), single-scattering albedo ω (bottom-left panel) and asymmetry parameter g (bottom-right panel) as they vary with mean particle size and wavelength. As a particle gets larger, σ ext,eff grows by orders of magnitude and particles preferentially forward-scatter incident radiation (ω ∼ 1, g ∼ 1). We note that the precomputed aerosol database for retrievals (Table 1) only spans mean particle size from 0.001 to 10 μm; however, the forward model algorithm can compute any mean particle size. Users can run forward models with their own refractive indices that will compute radiative properties “on-the-fly” and run an algorithm to include their own species into the precomputed aerosol database for retrievals. Similar plots are available for every aerosol in Table 1, see the “aerosol_database.pdf” on Zenodo (Section 6.1) or POSEIDON's Opacity Database (https://poseidon-retrievals.readthedocs.io/en/latest/content/opacity_database.html).
Paper: Observations of the Crustal Mini-magnetopause Reconnection at Mars
Authors: Xinzhi Qiu, Yiqun Yu, Jing Wang, Lihui Chai, Fan Gong, Longhui Liu, Jinbin Cao
Figure caption: (a) L, M, and N components of magnetic fields in the LMN coordinates. (b) The density of H+ (black), O+ (blue), and ﹩{{\rm{O}}}_{2}^{+}﹩ (red). (c)–(e) Velocity of H+ (e), O+ (f), and ﹩{{\rm{O}}}_{2}^{+}﹩ in the LMN coordinates. (f) Ion mass spectrum. (g)–(i) The energy spectra of H+ (e), O+ (f), and ﹩{{\rm{O}}}_{2}^{+}﹩, respectively. The two red dashed vertical lines indicate the mini-magnetopause (reconnection region) in the time interval of 19:24:05–19:26:35 UT and the two black dashed lines denote the upstream and downstream time of the Walén test.
Paper: Observations of the Crustal Mini-magnetopause Reconnection at Mars
Authors: Xinzhi Qiu, Yiqun Yu, Jing Wang, Lihui Chai, Fan Gong, Longhui Liu, Jinbin Cao
Figure caption: (a)–(b) The spacecraft’s trajectory in the MSO coordinate system. The solid and dashed black lines represent the empirical locations of the bow shock and magnetic pile-up boundary, respectively (J. G. Trotignon et al. 2006). The blue dashed lines represent the MAVEN’s trajectory and the red dashed line represents crossing the mini-magnetopause. (c) The schematic illustration of the reconnection. The blue lines with arrows represent the draped field lines, the red line with arrows represents the closed field lines, and the red and blue gradient line with arrows represents the open field lines. The dark-red line indicates the position of Mars. The green line represents the orbit of MAVEN (when viewed perpendicular to the paper surface, it is above Mars). The black arrow denotes the outflow jet, while the black cross represents the X line of magnetic reconnection. The deep blue signs of “⨂” and “⊙” represent the positive and the negative ΔB  M .
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Assumed particle size distribution (in log radii) for a given mean particle size r  m . Dots represent specific particle sizes that are computed, with an overdensity near the mean particle size.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: As in Figure 17 for all Chandra observations.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: As in Figure 17 for all NuSTAR observations.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Atmospheric retrievals on HST and Spitzer emission data of HD 189733 b. Retrieved spectra display median retrieved spectra (solid lines), with 1σ and 2σ confidence intervals (dark and light shaded regions). Top panels: retrieval results for a clear atmosphere, displaying results for both emission and emission + reflection retrievals. All retrievals include thermal multiple scattering. The left-hand panel is zoomed on HST data and shows that reflection is necessary to fit the STIS data. The right-hand panel shows full retrieved emission spectra. Middle panels: retrieval results for a gray aerosol model with an opaque cloud and parameterized haze. The retrieval does not prefer an opaque cloud deck, but does utilize the absorptive haze to shape the reflection spectrum. Bottom panels: retrieved atmospheric thermal structures (left-hand panel) and posteriors for equilibrium temperature and gas-phase volume mixing ratios of CO2, H2O, and Na + (0.1 K). Top row represents retrievals with just emission, bottom row represents retrievals with emission + reflection. A clear atmosphere is sufficient to fit the data, with no preference for an absorptive cloud deck or haze. Retrieved posteriors are consistent between emission and emission + reflection retrievals with the exception of alkalis, which are constrained due to the short-wavelength reflection spectra. A full list of retrieved parameters can be seen in Table 9.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Top panel: graphic displaying the two main Mie aerosol models introduced to POSEIDON. The fuzzy deck is modeled with an opaque cloud deck with a “fuzzy” cloud top of aerosols. The slab is modeled with a cloud-top pressure, cloud width, and constant mixing ratio for aerosols in the cloud. Both are parameterized with mean particle radius. Bottom panels: example transmission spectra utilizing the two aerosol models are shown. There are a myriad of other aerosol models that are built from these two models, e.g., opaque deck + slab(s), fuzzy deck + slab(s), uniform mixing ratio with pressure (uniform X), and opaque deck + uniform X. For more a more in-depth look at aerosol models and their effect on spectra, see the “Clouds in Transmission Spectroscopy” tutorial in Forward Model Tutorials (https://poseidon-retrievals.readthedocs.io/en/latest/content/forward_model_tutorials.html).
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Atmospheric retrievals on HST and Spitzer transmission data of HD 189733 b, with retrieved offsets applied to the WFC3 data. Retrieved spectra display median retrieved spectra (solid lines), with 1σ and 2σ confidence intervals (dark and light shaded regions). Top panel: retrieval results for a clear atmosphere (aqua) and an atmosphere with a parameterized gray cloud and haze (gray). Middle panel: retrieval results for silicate aerosol species, namely enstatite (MgSiO3, blue) and crystalline quartz (SiO2, yellow). Note the silicate absorption features at 9.6 μm (MgSiO3) and 8.5 μm (SiO2). Bottom panels: retrieved posteriors for atmospheric isothermal temperature, gas-phase volume mixing ratios of CO2, H2O, and K. Retrievals with a parameterized cloud retrieve a supersolar H2O abundance and do not constrain K, while retrievals with Mie-scattering aerosols retrieve subsolar H2O and K abundances. Subsequent rows display retrieved posteriors for the slab-top pressure in log space log P top,slab, width of the slab in log-pressure space ﹩{\rm{\Delta }}\mathrm{log}﹩                      P, mean particle size log r m, and constant aerosol mixing ratio in the slab. Aerosols are needed to fit the 0.3–1 μm slope. Both silicate aerosol species retrieve a high-altitude, thin, low-density (∼−11) slab composed of submicron particles (∼0.1 μm).
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Same as Figure 9, but highlighting the emission + reflection retrieval results for enstatite (MgSiO3) clouds. Top panels: retrieval results for the slab model, with and without fractional cloud coverage as a free parameter. Middle panels: retrieval results for the uniform mixing ratio model, with and without fractional cloud coverage as a free parameter. Bottom panels: retrieved temperature structure of each model. The top row of posteriors is consistent with the results displayed in Figure 9. The bottom row shows retrieved aerosol properties, in particular the mean particle size log r m, and constant aerosol mixing ratio in the cloud for all four clouds models, the slab-top pressure log P top,slab for the two slab models, and the fractional cloud coverage percentage f cloud for the patchy aerosol models. We find that all retrievals fit for a minimal-density aerosol abundance, consistent with the aerosol-free clear model. A full list of retrieved parameters can be seen in Table 9.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Showcasing each aerosol in the precomputed database by performing retrievals fitting for only the short-wavelength slope and WFC3 data and extending to longer wavelengths to show aerosol identifying absorption features. Plots display 1σ regions and are ordered from most hot aerosols (super hot) to coldest (ices), with the last two panels showcasing photochemical products. Most aerosols have infrared absorption features, especially aerosol species found in hot Jupiters (super-hot to silica class) and ices. Many clouds found in T-Y dwarf temperature regimes, as well as many soots and hazes, do not have features readily available via current space-based telescopes. We note that from the slope alone, TiO2 (anatase) provides the best fit (see Figure 15 in the Appendix). Aerosol opacity plots are available for every aerosol in Table 1, see the “aerosol_database.pdf” on Zenodo (Section 6.1) or POSEIDON's Opacity Database (https://poseidon-retrievals.readthedocs.io/en/latest/content/opacity_database.html).
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Emission + reflection retrieval results for cloud-free atmospheres assuming different P–T profiles. Top panels: showcasing the results for the dayside Guillot profile (which was featured in Figures 9 and 10) and the same profile with a larger prior on the infrared opacity (log κ IR) and gamma (γ). With a larger prior, the P–T profile fits for a deep, steep adiabat. Middle panels: showcasing results for two six-parameter P–T profiles, specifically the M. R. Line et al. (2013) and N. Madhusudhan & S. Seager (2009) parameterizations. Bottom panels: showcasing results for two flexible P–T profiles, specifically the slope profile (which assumes a negative temperature gradient) from A. A. A. Piette & N. Madhusudhan (2020) and the knot-fitting profile (which assumes a penalty (σ  s ) on the second derivative) from S. Pelletier et al. (2021). We showcase both a strict penalty on the second derivative (150) as well a relaxed penalty (550) to showcase the effect of the penalization. All P–T profiles, with the exception of the nonphysical Pelletier 550 profile, share a negative temperature gradient from 10 (1600 K) to 0.1 bars (1200 K) that is driving the water and carbon dioxide absorption features in the spectra. The retrieved parameters for gas-phase species are consistent, with the exception of a bimodal carbon dioxide abundance in the Madhu, slope, and Pelletier profiles, which can allow for upper-atmospheric temperature gradients. Retrieved P–T parameters can be seen in Table 13.