adsabs/AstroCLIMB huggingface dataset:
Paper: MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3 
Authors: Ben Forrest, Gillian Wilson, Adam Muzzin, Danilo Marchesini, M. C. Cooper, Z. Cemile Marsan, Marianna Annunziatella, Ian McConachie, Kumail Zaidi, Percy Gomez, Stephanie M. Urbano Stawinski, Wenjun Chang, Gabriella de Lucia, Francesco La Barbera, Lori Lubin, Julie Nantais, Theodore Peña, Paolo Saracco, Jason Surace, Mauro Stefanon
Figure caption: Observed K-band spectra for XMM-VID1-2075 from NIRES (red) and MOSFIRE (blue). Spectra are binned to ∼3 Å in the rest frame. Errors are represented by the shaded regions at the bottom, and the Hβ and Hγ absorption features at z = 3.45 are labeled.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: Model T(P) profile, chemical and dynamical timescales, and chemistry for a brown dwarf with T eff 700 K and log(g) = 4.5 is shown in the top panels whereas the same properties for a brown dwarf with T eff 700 K and log(g) = 5.25 is shown in the bottom panels. The T(P) profiles of the two brown dwarfs are shown in the left panels—one with a single deep convective zone, and the other with a deep “sandwiched” radiative zone between two deep convective zones. The middle panels show the comparison between the mixing timescale (black) and the chemical timescales of different gases like CO and NH3 as a function of pressure for each of the T(P) profiles shown in the left panels. The right panels show the volume mixing ratios of various molecules as a function of pressure for each atmosphere. The main point here is that gases can be quenched in a deeper “sandwiched” radiative zone in some brown dwarfs, where mixing timescales can be orders of magnitude larger than in convective zones.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The top panel shows the equilibrium chemistry abundance of CO at pressures where T = T eff in our T eff vs. gravity grid of chemical equilibrium models. The second, third, and fourth panels depict the quenched CO abundance within the T eff vs. gravity parameter space in our disequilibrium chemistry models. The second, third, and fourth panels correspond to models with radiative zone K  zz  values of “Moses,” “Moses × 100,” and “Moses/100,” respectively, while the convective zone mixing length L was fixed at the scale height H. Models where CO was quenched at the radiative zone are marked with black hatches. CO was quenched at a convective zone in the rest of the models. Models with radiative zone CO quenching show much smaller CO abundance compared to models with convective zone quenching.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The left panel shows the T(P) profile of a brown dwarf with T eff of 700 K and log(g) of 4.5. The dashed line is the T(P) profile when chemical equilibrium is assumed, whereas the solid line shows the T(P) profile for disequilibrium chemistry. The convective zones are shown with darker and thicker lines. The right panel shows the wavelength-dependent absorptivity of the different atmospheric layers for both the cases. The absorptivity is given by 1-e−τ . The absorptivity for the equilibrium chemistry model is shown with the dashed lines whereas that for the disequilibrium chemistry model is shown by the solid lines. The local normalized blackbody spectrum is also shown for each layer by the dashed and solid lines for equilibrium and disequilibrium chemistry models, respectively. The blue horizontal line for each layer shows the absorptivity corresponding to τ = 1. The main point here is that opacity changes lead to large (∼100 K) differences in T(P) profiles between chemical equilibrium and disequilibrium models.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The appearance of the second radiative zone in the T eff vs. log(g) parameter space in our grid is shown. The colors show the values of the quantity log10(P bot/Ptop), where P bot and P top are the pressures at the bottom and top of the sandwiched radiative zone, respectively. The top panel shows this for the case of equilibrium chemistry. The subsequent panels show the presence of the second radiative zone if different strengths of K  zz  are chosen, keeping the convective zone mixing length fixed at H. Dark blue indicates no second convective zone at depth.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption:  M-band thermal emission spectra across a range of T eff between 400 and 1000 K with steps of 100 K are shown in each panel. log (g) = 5.0 is on the left and 5.5 is on the right. The colors are representative of the T eff. The models shown in the top-left and -right panels assume the convective mixing length L to be H, whereas the models shown in the bottom-left and -right panels assume L = 0.1 × H. The three line styles show different radiative zone K  zz  parameterizations, including Moses (solid), Moses/100 (dashed), and Moses × 100 (dashed–dotted lines). If quenching occurs in a convective zone, the three spectra are plotted atop each other. The shaded region shows the wavelength range where CO is the most important absorber.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: Appearance of the second radiative zone in the T eff vs. log(g) parameter space in our grid is shown. The colors show the value of the quantity log10(P bot/Ptop) where P bot and P top are the pressures at the bottom and top of the sandwiched radiative zone, respectively. The top panel shows this for the case of equilibrium chemistry. The subsequent panels show the presence of the second radiative zone if different strengths of K  zz  are chosen, keeping the convective zone mixing length fixed at 0.1 × H. Dark blue indicates no second convective zone at depth.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The same as Figure 7 but for quenching of CO2. Given the different t chem for CO2, compared to CO, the quench levels are entirely different.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The same as Figure 7 except with the mixing length in convective zones fixed at 0.1 × H. In these models, CO is mostly quenched in a radiative zone.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The same as Figure 8 but for quenching of NH3. Given the different t chem for NH3, compared to CO, the quench levels are entirely different.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: Simulated data from JWST instruments are shown for one of our model brown dwarfs with T eff of 700 K. The three colors in the simulated data correspond to models with different radiative zone K  zz . The top-left panel shows the simulated NIRSpec spectra of a log (g) = 5.5 object with an exposure time of 10 minutes, while the bottom-left panel shows a zoomed version of the top-left panel to emphasize how JWST NIRSpec M-band observations can clearly distinguish between different K  zz  in the radiative zones for these T-dwarfs. The top-right panel shows the NIRSpec simulated data for a brown dwarf with T eff of 700 K and log(g) of 4.5. The two colors represent different K  zz  in the convective zone but the same K  zz  in the radiative zone. The bottom-right panel shows MIRI LRS simulated data for the same models shown in the top-right panels. To compare the differences between the simulated data from different models to the typical JWST noise, the ratio of the flux differences (δF) between various models and the simulated JWST noise (N) is shown below each of these panels. This shows that both convective and radiative zone K  zz  can be constrained with JWST.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The best-fit quench K  zz  of CO for each object is shown as a function of their best-fit T eff with the red crosses. The median best-fit quench K  zz  vs. T eff inferred by Miles et al. (2020) with lower-gravity models are shown with the faded red crosses. The inferred quench K  zz  for NH3, CO2, HCN, and PH3 from the best-fit models for each object are also shown as a function of their best-fit T eff. The black points show the theoretically maximum K  zz  allowed from mixing length theory for these best-fit models.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption:  H-band thermal emission spectra of models from our grid are shown in the top-left and -right panels, whereas the bottom-left and -right panels show the K-band emission spectra. Models with log(g) = 5 and different T eff between 400 and 1000 K are shown in each panel. From bottom to top, spectra for T eff values of 425, 700, 850, 900, and 1000 K are shown in all of the panels. The top-left panel shows the thermal emission spectra of models that have convective mixing length set at H but have different K  zz  parameterizations like Moses, Moses/100, and Moses × 100, which are represented by different line types in the panels (solid, dashed, and dashed–dotted lines). The top-right panel shows the same but for models with convective mixing length set at 0.1 × H. The bottom-left and -right panels show the sensitivity of the K-band spectrum to radiative zone K  zz  when L = H and L = 0.1 × H, respectively. The shaded region shows the wavelength range where CH4 is the most important absorber.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: Thermal emission spectra of brown dwarfs between 3 and 3.5 μm are shown in the top-left and -right panels. Emission spectra of the same models in the L band are shown in the bottom-left and -right panels. Models with log(g) = 5 and different T eff between 400 and 1000 K are shown in each panel. From bottom to top, spectra for T eff values of 425, 700, 850, 900, and 1000 K are shown in all of the panels. The top-left panel shows the emission spectra of models that have convective mixing length set at H but have different K  zz  parameterizations like Moses, Moses/100, and Moses × 100, which are represented by different line types in the panels (solid, dashed, and dashed–dotted lines). The top-right panel shows the same but for models with convective mixing length set at 0.1 × H. The bottom-left and -right panels show the sensitivity of the L-band spectrum to radiative zone K  zz  when L = H and L = 0.1 × H, respectively. The shaded region shows the wavelength range where CH4 is the most important absorber.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The top-left panel shows the observed M-band spectra of Gl 570D with red points, the 1–2.5 μm observations of Gl 570D with black points, and the Spitzer IRS measurements with brown points. The flux values sampled by the top 131 models with the smallest G  k  parameter after fitting the M-band spectra only are shown by the shaded blue region. The top-right panel shows the best-fit model obtained by fitting the M-band spectra, the 1–2.5 μm data, and the Spitzer 5–14 μm data for Gl 570D. The bottom-left panel shows a comparison of the best-fit model with the M-band spectra only. The three bottom-right panels show, respectively, the T(P) profile of the best-fit model, the t mix and t chem of different quenched species as a function of pressure, and the rightmost panel shows the volume mixing ratios of CO, CH4, NH3, H2O, CO2, and PH3.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: Color–magnitude diagrams (CMDs) of observed brown dwarfs in different filters are shown with overplotted equilibrium and disequilibrium chemistry model tracks with different strengths of convective and radiative zone vertical mixing. The top row shows the J vs. J-H where the models with a convective zone mixing length of H and different radiative zone K  zz  are shown with various red line types. Models with a convective zone mixing length of 0.1 × H and different radiative zone K  zz  are shown with various blue line types, and the equilibrium chemistry models are shown by the dashed black lines. Each column shows the same data, but the model tracks with different values of log(g). The second row shows the L′ vs. L′-M′ whereas the third row shows the W1 vs. W1-W2.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The top-left panel shows the observed M-band spectra of 2M 0415 with red points, the 1–2.5 μm observations of 2M 0415 with black points, and the Spitzer IRS measurements with brown points. The flux values sampled by the top 101 models with the smallest G  k  parameter after fitting the M-band spectra only are shown by the shaded blue region. The top-right panel shows the best-fit model obtained by fitting the M-band spectra, the 1–2.5 μm data, and the Spitzer 5–14 μm data for 2M 0415. The bottom-left panel shows a comparison of the best-fit model with the M-band spectra only. The three bottom-right panels show, respectively, the T(P) profile of the best-fit model, the t mix and t chem of different quenched species as a function of pressure, and the rightmost panel shows the volume mixing ratios of CO, CH4, NH3, H2O, CO2, and PH3.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The left panel shows a heat map of the χ 2 value calculated using model photometry and observed photometry (Miles et al. 2020) in various infrared bands as a function of model T eff and log(g) for WISE 0313. The left panel indicates models where radiative K  zz  is fixed at Moses, and the convective mixing length is H. The middle and right panels also show the χ 2 heat maps using models with radiative K  zz  of Moses/100 and Moses × 100, respectively. The best-fit T eff is near 550 K.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The best-fit atmospheric models and their comparison with the data are shown. Each row corresponds to a different object. The leftmost column shows the best-fit M-band spectra along with the observed data from Miles et al. (2020). The second column from the left shows the best-fit T(P) profile for these objects from the grid of models presented in this paper. The third column shows the best-fit mixing timescale in blue along with the chemical timescale for CO in red as a function of pressure. The volume mixing ratios of various atmospheric gases are shown in the fourth column for each object.
Paper: Cosmic-Ray Convection–Diffusion Anisotropy
Authors: Yiran Zhang, Siming Liu, Dejin Wu
Figure caption: Comparison of the quadrupole anisotropy reported by CR observations and that calculated with the 1D shear model of Equation (11) assuming a full-sky R.A. projection, where ﹩\nu =\left(2.7+3.1\right)/2﹩. The colored pair of numbers represents ﹩\left[\partial \mathrm{ln}\kappa /\partial \mathrm{ln}p,\kappa \left(\mathrm{TeV}\right)\left|{S}_{{zz}}\right|{\cos }^{2}{\delta }_{2}/\left({10}^{29}\ {\mathrm{Myr}}^{-1}\,{\mathrm{cm}}^{2}\,{{\rm{s}}}^{-1}\right)\right]﹩. Long-dashed lines indicate limiting cases in which the shear anisotropy and A 2 data can overlap. The yellow short-dashed and cyan solid lines show the fit to the A 2 data below 5 TeV and above 200 TeV, respectively. The data are from Milagro (Abdo et al. 2009), ARGO-YBJ (Bartoli et al. 2015), EAS-TOP (Aglietta et al. 2009), IceCube/Top (Abbasi et al. 2010, 2012; Aartsen et al. 2013), AGASA (Hayashida et al. 1999), Auger (Abreu et al. 2012; Aab et al. 2018), and Auger+TA (Aab et al. 2014).
Paper: Cosmic-Ray Convection–Diffusion Anisotropy
Authors: Yiran Zhang, Siming Liu, Dejin Wu
Figure caption: Comparison of the dipole anisotropy in R.A. reported by CR observations and that calculated with the inertial effect of Equation (7) assuming a full-sky R.A. projection, where ﹩\nu =\left(2.7+3.1\right)/2﹩. The colored pair of numbers represents ﹩\left[\partial \mathrm{ln}\kappa /\partial \mathrm{ln}p,\kappa \left(\mathrm{TeV}\right)a\cos {\delta }_{1}/\left({10}^{29}\ {\mathrm{cm}}^{2}\mu {\rm{m}}\,{{\rm{s}}}^{-3}\right)\right]﹩. Long-dashed lines indicate limiting cases in which the inertial anisotropy and A 1 data can overlap. The yellow short-dashed and cyan solid lines show the fit to data below 5 TeV and in 200 TeV–50 PeV, respectively. The data are from underground muon detectors (UG-μ data in Amenomori et al. 2005), Milagro (Abdo et al. 2009), ARGO-YBJ (Bartoli et al. 2015, 2018), Tibet-ASγ (Amenomori et al. 2005, 2017), EAS-TOP (Aglietta et al. 1995, 1996, 2009), IceCube/Top (Abbasi et al. 2010, 2012; Aartsen et al. 2013, 2016), KASCADE-Grande (Apel et al. 2019), AGASA (Hayashida et al. 1999), Auger (Aab et al. 2020), and TA (Telescope Array; Abbasi et al. 2020).
Paper: Cosmic-Ray Convection–Diffusion Anisotropy
Authors: Yiran Zhang, Siming Liu, Dejin Wu
Figure caption: Left: equatorial sky map of the CR anisotropic intensity (relative to the isotropic part) induced by the Galactic differential rotation with the Oort shear rate of Equation (19), where ﹩\nu =\left(3.2+2.6\right)/2﹩, κ/k = 1033 cm2 s−1. The white solid curve shows the Galactic disk. The Galactic rectangular frame is indicated with red crosses (north Galactic pole: NGP). Blue dots mark directions of peaks of the R.A. projected intensity, with ϕ 2 ≈ 28°. Right: most similar intensity profile to the left-hand panel, derived with reconstructed Q  ij  in Aab et al. (2018), where the parameters used are given in Table 1.
Paper: Cosmic-Ray Convection–Diffusion Anisotropy
Authors: Yiran Zhang, Siming Liu, Dejin Wu
Figure caption: Schematic view of the simple extension. Left: fluid deformation in a time of τ( ≪ 1/S). The blue dashed-line square is the projection of an isotropic (3D) fluid element on the x–z plane. The red solid-line rectangle shows the element after constant-volume lengthening along ﹩\hat{{\boldsymbol{z}}}﹩. Right: contours of particle momentum–space distributions (with p  y  = 0) corresponding to deformation states in the left-hand panel, where ν = 1, ﹩{{ \mathcal A }}_{2}=0.3﹩. Green dashed arrows represent shear-restoring forces on a particle.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The top panel shows the equilibrium chemistry abundance of PH3 at pressures where T(P) = T eff in our T eff vs. gravity grid of chemical equilibrium models. The second, third, and fourth panels depict PH3 abundance within the T eff vs. gravity parameter space in our disequilibrium chemistry models. The second, third, and fourth panels correspond to models with radiative zone K  zz  values of “Moses,” “Moses × 100,” and “Moses/100,” respectively, while the convective zone mixing length L was fixed at the scale height H. Models where PH3 was quenched in a radiative zone are marked with black hatches. PH3 was quenched at a convective zone in the rest of the models.
Paper: Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
Authors: Sagnick Mukherjee, Jonathan J. Fortney, Natasha E. Batalha, Theodora Karalidi, Mark S. Marley, Channon Visscher, Brittany E. Miles, Andrew J. I. Skemer
Figure caption: The effect of PH3 quenching on the spectra has been shown by comparison with disequilibrium chemistry model spectra, where PH3 is not quenched. Models with different T eff values ranging from 400–1000 K, with a step of 100 K, are shown from bottom to top. All of these models have log(g) = 5.
Paper: Cosmic-Ray Convection–Diffusion Anisotropy
Authors: Yiran Zhang, Siming Liu, Dejin Wu
Figure caption: Schematic view of the inertial dipole anisotropy, where ν = 1, ﹩{{ \mathcal A }}_{1}=0.3﹩. The red solid curve is an isoline of the anisotropic distribution of particles in the momentum space in the a–p plane. The anisotropy can be relaxed in a time of τ(≪ v/a) due to the inertial force, which is shown with the green thick dashed arrow, to produce an isotropic distribution whose contour is the blue dashed circle.
Paper: Cross-scale Correlations in Imbalanced Solar Wind Turbulence: Parker Solar Probe Observations
Authors: G. Q. Zhao, R. Meyrand, H. Q. Feng, D. J. Wu, J. C. Kasper
Figure caption: CCs against the plasma beta (β  p ) with a bin of 0.3. The top panels are for CCs of σ  c  with PI  and V  p . The middle and bottom panels are for CCs of σ  m  with σ  c , PI , T  p , and V  p .