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Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: The effect of surface gravity, cloud thickness, and metallicity on spectra. All models have T eff = 1500 K. The left panels show the broad near-infrared spectra, while the right panels zoom in to the gravity-sensitive features within J band. In the right panels we plot the center value (log g = 4.5; f sed = 4; [M/H] = 0.0) in gray behind each spectrum. The top panels show the effect of surface gravity for models with solar metallicity and f sed = 3; spectral features that have been identified to empirically correlate with surface gravity are labeled. The middle panels show the effect of cloud sedimentation efficiency for models with solar metallicity and log g = 4.5. The bottom panels show the effect of metallicity for models with log g = 4.5 and f sed = 4.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Thermal evolution models for cloud-free and hybrid models at solar metallicity. Each line represents a different mass evolution model; the adjacent number indicates the mass in Jupiter masses. Cloud-free models are shown with dashed lines, and hybrid models are shown with solid lines. The clouds in the hybrid models clear at 1300 K, changing the evolution. Atmospheres cool slightly faster until the transition and then stall at ∼1200 K when the clouds clear, remaining slightly warmer than the cloud-free models of the same age.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Thermal evolution models for cloud-free and hybrid models at solar metallicity. The same models are shown as in Figure 14. Cloud-free models are shown with dashed lines, and hybrid models are shown with solid lines. Radius vs. age (top panel) shows that objects shrink as they age, from 1.5–2.5 R J at 3 Myr to 0.75–1 R J at 10 Gyr. log g vs. age (middle panel) shows that objects increase in surface gravity as they age, typically by roughly 0.5 dex. Luminosity vs. age (bottom panel) looks similar to T eff vs. age and shows that an object's luminosity evolution is shaped by the emergence and disappearance of clouds.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Sonora Diamondback model spectra in Y and J bands (0.9–1.35 μm). Models are shown for a range of T eff from 2400 (top left) to 900 K (bottom right). All models shown have log g = 5.0. Cloudy (f sed = 4) spectra are shown as colored lines; cloud-free models are shown as gray lines for each T eff. Key molecular features are labeled. Models are smoothed to a constant resolution of λ/Δλ = 2000.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Sonora Diamondback model spectra in the thermal infrared (5.5–15 μm). Models are shown for a range of T eff from 2400 (top left) to 900 K (bottom right). All models shown have log g = 5.0. Cloudy (f sed = 4) spectra are shown as colored lines; cloud-free models are shown as gray lines for each T eff. Key molecular features are labeled. The silicate feature from small silicate particles is not seen in our spectra (see Section 4.3) but would be a broad feature at 9–10 μm. Models are smoothed to a constant resolution of λ/Δλ = 600.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Sonora Diamondback model spectra in the mid-infrared (3–5.2 μm). Models are shown for a range of T eff from 2400 (top left) to 900 K (bottom right). All models shown have log g = 5.0. Cloudy (f sed = 4) spectra are shown as colored lines; cloud-free models are shown as gray lines for each T eff. Key molecular features are labeled. Models are smoothed to a constant resolution of λ/Δλ = 1500.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Temperature evolution for cloud-free and hybrid models at solar metallicity. Cloud-free models are shown with solid lines; hybrid models are shown with dashed lines; hybrid-grav models are shown with dotted lines. The clouds in the hybrid models clear at 1300 K, while in the hybrid-grav models they clear at 1000–1400 K (dependent on surface gravity). The top panel shows temperature vs. age. The lower two panels show the temperature difference between the hybrid and hybrid-grav models and the cloud-free models. Clouds can change the effective temperature at a given age by 100–200 K.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Sonora Diamondback model spectra in the near-infrared. Models are shown for a range of T eff from 2400 (top left) to 900 K (bottom right). All models shown have log g = 5.0. Cloudy (f sed = 4) spectra are shown as colored lines; cloud-free models are shown as gray lines for each T eff. Key molecular features are labeled. Models are smoothed to a constant resolution of λ/Δλ = 400.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Sonora Diamondback model spectra in the red optical. Models are shown for a range of T eff from 2400 (top left) to 900 K (bottom right). All models shown have log g = 5.0. Cloudy (f sed = 4) spectra are shown as colored lines; cloud-free models are shown as gray lines for each T eff. Key molecular features are labeled. Models are smoothed to a constant resolution of λ/Δλ = 1000.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Near-infrared CMD, illustrating the effect of metallicity and surface gravity. In both panels, blue lines show cloud-free models and red lines show cloudy models. Markers along the lines indicate 100 K intervals, from 900 to 2400 K; every 300 K, we plot a dotted line of equal temperature to guide the eye. The gray circles show the photometry of field brown dwarfs; the orange stars show the photometry of “young” brown dwarfs (see text); blue triangles show subdwarfs. Unresolved binaries are not plotted. Top: solar-metallicity models are shown with solid lines, while −0.5 and +0.5 are shown with dashed–dotted and dotted lines, respectively. For cloud-free atmospheres, lower-metallicity models are always bluer in near-infrared colors for a given temperature. For cloudy models, lower-metallicity models are typically bluer, with some more complex behavior as the clouds thicken and sink below the near-infrared photosphere. Bottom: models are shown for three surface gravities: log g = 5.5 (dashed lines), log g = 4.5 (solid lines), and log g = 3.5 (dotted lines). Lower-gravity objects are larger and more luminous (moving up on the CMD), and typically somewhat redder, though the behavior at cooler temperatures shows additional complexity.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: The deuterium-burning limits of our models compared to prior modeling efforts. The Diamondback models are shown as circles and labeled as “nc” (cloud-free evolution) or “hybrid” (hybrid evolution). Filled markers denote 50% of D burned in 10 Gyr; open circles denote 90% of D burning in 10 Gyr. Diamondback models are compared to D. Saumon & M. S. Marley (2008) models (diamonds), where “nc” indicates cloud-free models and “f2” indicates cloudy models. D. S. Spiegel et al. (2011) limits are shown as squares, with both Y = 0.25 (their default model) and Y = 0.28 shown. We note that the deuterium-burning limit can be substantially lower than the canonical 13 M J limit.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: CMDs illustrating the effect of clouds. Cloud-free models are blue, and cloudy models are purple and red. The gray circles show the photometry of field brown dwarfs; the orange stars show the photometry of “young” brown dwarfs (see text); the blue triangles show subdwarfs. Unresolved binaries are not plotted. All models shown have log g = 5.0. No single set of models accurately captures the observed photometry of all brown dwarfs, but in general cloudy models fit the photometry of L dwarfs more accurately, while cloud-free models fit the photometry of T dwarfs more accurately.
Paper: The Sonora Substellar Atmosphere Models. III. Diamondback: Atmospheric Properties, Spectra, and Evolution for Warm Cloudy Substellar Objects
Authors: Caroline V. Morley, Sagnick Mukherjee, Mark S. Marley, Jonathan J. Fortney, Channon Visscher, Roxana Lupu, Ehsan Gharib-Nezhad, Daniel Thorngren, Richard Freedman, Natasha Batalha
Figure caption: Temperature evolution for hybrid models at three metallicities. Solar-metallicity models are shown with solid lines; [M/H] = +0.5 models are shown with dashed lines; [M/H] = −0.5 models are shown with dotted lines. The top panel shows temperature vs. age. The lower two panels show the temperature difference between the [M/H] = +0.5 and [M/H] = −0.5 models and solar-metallicity models. Metallicity can change the effective temperature at a given age by 100–200 K.
Paper: Merging Signatures in an Offset Lyman Continuum Emitter at Redshift 3.8
Authors: Fang-Ting Yuan, Zhen-Ya Zheng, Chunyan Jiang, Shuairu Zhu, Ruqiu Lin, Cheng Cheng
Figure caption: Physical properties of CDFS-6664's two components. (a) Effective radii of C1 (orange) and C2 (blue) extracted by GALFIT based on the JWST F182M image. The model and residual images are shown on the lower left of the image. (b) SEDs and best-fitting models of the two components C1 (orange) and C2 (blue). The models can fit the SEDs well, with a goodness of fit χ 2 < 2. (c) Probability density distributions for physical parameters derived from SED fitting for C1 (orange) and C2 (blue). C1 and C2 are consistent with a major merger system with a stellar mass ratio M *,C1/M *,C2 of 3.5. C2 has a bluer ultraviolet slope and younger stellar populations than C1. (d) Star formation rates of C1 and C2 compared to the main sequence of star-forming galaxies at redshift ∼4. The shaded area indicates the 3σ uncertainty. C1 and C2 lie significantly above the main sequence, indicating that starbursts may be triggered by merging.
Paper: Merging Signatures in an Offset Lyman Continuum Emitter at Redshift 3.8
Authors: Fang-Ting Yuan, Zhen-Ya Zheng, Chunyan Jiang, Shuairu Zhu, Ruqiu Lin, Cheng Cheng
Figure caption: Multiwavelength images of the LyC emitter, CDFS-6664 (z = 3.797). Contours of the fluxes in LyC (blue, 3σ, 4σ, and 5σ), HST F606W (orange, 2σ, 5σ, 15σ, and 30σ), and JWST F182M (red dashed, 2σ, 5σ, 30σ, and 60σ) are also displayed. (a) Smoothed image of LyC emission in HST F336W band (rest frame 650–770 Å). (b) Two components (C1 and C2) of CDFS-6664 in HST F606W band image (rest frame 1300 Å). C1 and C2 show comparable fluxes and sizes. (c) Two components (C1 and C2) in JWST F182M band image (rest frame 3800 Å). C2 becomes significantly fainter than C1, indicating that C2 is the bluer component. The LyC emission is at the side of C2, implying a connection between C2 and LyC. According to the positions of stars in the field of CDFS-6664, these multiwavelength frames are aligned with a precision of less than 0.″1.
Paper: An Edge-on Regular Disk Galaxy at z = 5.289
Authors: Haojing Yan, Bangzheng Sun, Chenxiaoji Ling
Figure caption: Image stamps of Dz5289 (3″ × 3″ in size). The bands are as labeled. The F606W, F814W, and F125W images are from the HST CANDELS program, while all others are from the NIRCam observations of the JWST CEERS program. The color image uses F606W + F814W + F115W + F125W + F150W as blue, F200W + F277W as green, and F356W + F410M + F444W as red. As the white line indicates, the galaxy extends at least 1.″0 along its long axis.
Paper: Merging Signatures in an Offset Lyman Continuum Emitter at Redshift 3.8
Authors: Fang-Ting Yuan, Zhen-Ya Zheng, Chunyan Jiang, Shuairu Zhu, Ruqiu Lin, Cheng Cheng
Figure caption: GALFIT results for JWST F182M image of CDFS-6664 in 2″ × 2″ boxes. All the images are normalized to the maximum of the observed F182M image. (a) Results of fitting with one Sérsic component. The image cannot be fitted well, with prominent structures left in the residual image. (b) Results of fitting with two Sérsic components and a PSF. The quality of the fitting is improved with this model.
Paper: Merging Signatures in an Offset Lyman Continuum Emitter at Redshift 3.8
Authors: Fang-Ting Yuan, Zhen-Ya Zheng, Chunyan Jiang, Shuairu Zhu, Ruqiu Lin, Cheng Cheng
Figure caption: GALFIT decomposition for image of CDFS-6664 in each band based on the model derived from the JWST F182M image. (a–j) The left is the observed image, the middle is the best model image by GALFIT, and the right is the residual image. The residual images show that the models can fit images in each band well.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Derived quantities vs. time for the 10–antiparallel–﹩{N}_{\phi }^{\mathrm{high}}﹩simulation. From top: mass accretion rate onto the star; open, closed, and disk-connected magnetic flux in units of the total stellar flux ψ tot; EM jet power L jet in units of the isolated-pulsar wind power L 0; magnetospheric radius r m, with a horizontal line for the corotation radius r co; and flux-opening efficiency factor ζ, derived both from the jet power and the open flux.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Poloidal slices of the mass density and logarithmically spaced contours of the poloidal flux function (i.e., A  ϕ ) of the azimuthally averaged magnetic field at t ∼ 10,500 r g/c, for each combination of the stellar magnetic moment and star–disk field orientation. The initial field orientation becomes progressively less important as μ increases (or, equivalently, as the accretion rate decreases).
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Poloidal (x–z) and equatorial (x–y) slices of the high-resolution μ = 10 simulation, 10–antiparallel–﹩{N}_{\phi }^{\mathrm{high}}﹩, at t = 11,560 r g/c. The color represents the mass density ρ, while blue line segments indicate the direction of the in-plane component of the magnetic field. The star’s light cylinder R LC and corotation radius r co are marked by solid and dashed gray lines, respectively. Several interchange streams can be seen spiraling inward from the magnetospheric boundary at r m ∼ 6.5 r g.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: EM jet power as a function of time for the four magnetic moment values. Color indicates the relative orientation of the stellar and torus magnetic field in the initial conditions: red for parallel, blue for antiparallel. Thin dotted lines indicate the two μ = 10 high-ϕ-resolution simulations.
Paper: An Edge-on Regular Disk Galaxy at z = 5.289
Authors: Haojing Yan, Bangzheng Sun, Chenxiaoji Ling
Figure caption: Fitted template spectrum (black curve) superposed on the SED (red symbols) in four fitting runs using different tools as labeled. The black squares are the synthesized magnitudes from these template spectra. The corresponding χ 2 values are also noted. For EAZY-py, the spectrum is that of the best-fit template. For CIGALE, BAGPIPES, and PROSPECTOR, it is the 50th percentile posterior spectrum. The evolution of SFR (as a function of time; 50th percentile posterior value) is available for the latter three runs, which is shown in the inset in each of these three panels. The shaded area in that of the BAGPIPES run indicates the 16th–84th percentile range.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: Schematic illustration of the accretion flow following the optical outburst of 1ES 1927+654, using the example SED from 2018 December 12. The upper panel gives our interpretation of the super-Eddington accretion flow, which consists of three distinct regimes: (1) an outer truncated disk in thermal equilibrium, depicted as a thin red disk with a vertical color gradient and truncated at radius R tr; (2) an inner overheated disk where advection becomes significant, represented in green without a vertical color gradient, whose photosphere size is denoted by R ph that extends to the inner edge R in from the BH; and (3) an X-ray corona, depicted as the blue component above the inner part of the disk, with radial size R cor. The three components contribute to the main observed SED, as indicated by the red, green, and blue arrows pointing to the spectral components in the lower panel. The outer thin disk is optically thick with a high effective optical depth τ eff and emits multicolor blackbody radiation, manifesting as the big blue bump. The inner disk, with a low τ eff, is overheated due to strong advection and electron-scattering effects, and it emits blackbody radiation at soft X-ray energies with a temperature determined by its photosphere. The corona upscatters the seed photons from the disk and contributes to the Comptonized emission in the hard X-ray band. In addition, relativistic reflection from the inner overheated disk can result in a broad 1 keV feature, which can be phenomenologically modeled with a broad Gaussian component (M. Masterson et al. 2022). These four components effectively describe the observed SED, as demonstrated in the lower panel. The error bars display the simultaneous data as observed (gray) and as corrected for reddening and absorption from the Las Cumbres Observatory (red), Swift (green), XMM-Newton (blue), and NuSTAR (purple). The intrinsic SED model (black curve) comprises a multicolor thin disk (red), a blackbody (green), Comptonization emission (blue), and a phenomenological Gaussian feature (cyan), which are modeled with diskbb, bbody, nthComp, and Gauss in XSPEC.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The dimensionless mass accretion rate (﹩\dot{M}﹩) as a function of the disk mass surface density (Σ), designated as the ﹩\dot{M}-{\rm{\Sigma }}﹩                      S-curve. The color of the circles represents the time since the outburst (2017 December 23), from the beginning (green) to the end (red), where the orange one denotes t ≈ 650 days. The red star shows the value in 2011 May, before the outburst. The blue curves depict the ﹩\dot{M}-{\rm{\Sigma }}﹩ relationship at different radii predicted by the slim accretion disk solution of M. A. Abramowicz et al. (1988). The dashed line indicates ﹩\dot{M}\propto {\rm{\Sigma }}﹩, as anticipated from the advection-dominated slim disk solution, while the dotted line represents ﹩\dot{M}\propto {{\rm{\Sigma }}}^{-1}﹩, as expected from a radiation-pressure-dominated thin accretion disk. The two arrows indicate the direction of movement of 1ES 1927+654 along the slim disk and thin disk branches of the S-curve before and after t = 650 days, respectively.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: Evolution of BH mass accretion rate as a function of time since the optical outburst on 2017 December 23 (t), calculated from the equation set in Section 2.1. The trend is modeled with a power-law decline expressed as ﹩\dot{M}\propto {t}^{-1.53}﹩ (Equation (11) and Table 3), whose best-fit model and 1σ uncertainty are shown by the red curve and red shaded region. The red star and red dashed line mark the preoutburst value calculated from the 2011 observation in R. Li et al. (2024). The dotted line marks the Eddington accretion rate for ﹩{M}_{\mathrm{BH}}={1.38}_{-0.66}^{+1.25}\times {10}^{6}\,{M}_{\odot }﹩ (R. Li et al. 2022).