adsabs/AstroCLIMB huggingface dataset:
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: Surface density fits to the CO and dust radius in the AS 209 disk for the two cases of matching the dust mass at a gas-to-dust ratio of 100 (blue lines) and for a disk on the cusp of gravitational instability with ﹩{Q}_{\min }=1﹩ (red lines). The points are at the observed dust and CO radii, measured at the 90% cumulative flux threshold, with surface densities determined by Equations (2) and (3), respectively. The solid lines show the surface density profiles (which are thicker at Σgas > 50 g cm−2 where the 1.3 mm continuum is optically thick), and the dashed lines the Toomre Q parameter. The disk masses in each case are given in solar masses in the top right corner. The stellar age and inferred drift times, as derived by the scaling of the surface density at the dust radius, are given in the bottom left corner.
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: Probability density functions of the ratio of drift time to stellar age for the 41 disks in our sample. The blue curve shows case 1 where the disk mass equals 100 times the dust mass and the red curve represents case 2 where a marginally gravitationally stable disk has Toomre Q minimum equal to 1. The functions are determined through kernel density estimation of the points shown at the bottom of the plot, where the symbol size is proportional to the dust mass.
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: The ratio of case 2 drift time to stellar age for different values of the power-law index γ used in the surface density fitting. Shallower profiles have lower central densities and longer drift times. As long as the gas density does not rise very strongly toward the center, γ ≤ 1.2, then the result that the drift times for disks with ﹩{Q}_{\min }=1﹩ are similar to the stellar ages holds.
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: Comparison of disk radii in the dust (left panel) and gas (middle panel), and case 2 drift times (right panel) for cumulative flux thresholds of 68% and 95% vs. the fiducial 90% threshold used in this work. The radii are tightly correlated in both dust and gas and drift times at the 90% and 95% levels, which agree to within 50%.
Paper: First Results from the Dragonfly Ultrawide Survey: The Largest 11 Quenched Diffuse Dwarf Galaxies in 3100 deg2 with Spectroscopic Confirmation
Authors: Zili Shen, William P. Bowman, Pieter van Dokkum, Roberto G. Abraham, Imad Pasha, Michael A. Keim, Qing Liu, Deborah M. Lokhorst, Steven R. Janssens, Seery Chen
Figure caption: Left column: Dragonfly g-band cutouts of each galaxy in our sample. Right column: Keck/KCWI spectra of each galaxy (black line) and the best-fit pPXF model (orange line). Both the data and the model have been deredshifted to the rest frame using the radial velocity listed in each row. We label Balmer lines and the Ca II H and K lines to guide the eye.
Paper: First Results from the Dragonfly Ultrawide Survey: The Largest 11 Quenched Diffuse Dwarf Galaxies in 3100 deg2 with Spectroscopic Confirmation
Authors: Zili Shen, William P. Bowman, Pieter van Dokkum, Roberto G. Abraham, Imad Pasha, Michael A. Keim, Qing Liu, Deborah M. Lokhorst, Steven R. Janssens, Seery Chen
Figure caption: Two examples of injection-recovery tests conducted with pPXF, where the only difference is a 0.1 dex change in the age of the injected templates (white plus signs in each panel). Top panels: a mock galaxy spectrum (black) with noise added (seen in the residuals in green diamonds) to approximate the SNR of the data. The pPXF best fit is overplotted in red. The mock galaxy spectrum is a linear combination of two templates, whose age and metallicity are shown in the middle panel as white plus signs. Middle panels: the weight of each template that went into the pPXF best fit. Bottom panels: the weight distribution summed along the metallicity axis, plotted against linear age. The peak at ∼1 Gyr and at old ages is clearly visible. The input spectra on the left and right are very similar, but the reconstructed metallicity distributions are quite different. We conclude that at the SNR level of our data, only the age distribution can be reliably recovered.
Paper: First Results from the Dragonfly Ultrawide Survey: The Largest 11 Quenched Diffuse Dwarf Galaxies in 3100 deg2 with Spectroscopic Confirmation
Authors: Zili Shen, William P. Bowman, Pieter van Dokkum, Roberto G. Abraham, Imad Pasha, Michael A. Keim, Qing Liu, Deborah M. Lokhorst, Steven R. Janssens, Seery Chen
Figure caption: Left: the apparent effective radius R e vs. the g-band central surface brightness μ 0,g  of each galaxy in our sample (marked by red stars). The hexagons are a density map of UDG candidates from the SMUDGes survey (D. Zaritsky et al. 2023), and the dotted vertical line represents the surface brightness definition of UDGs (﹩{\mu }_{0}(g)\gt 24\,\mathrm{mag}\,{\mathrm{arcsec}}^{-2}﹩). Right: the physical size of each galaxy vs. the g-band absolute magnitude. Red stars represent galaxies in our sample, while the other colored symbols represent other quiescent isolated UDGs in the literature (D. Martínez-Delgado et al. 2016; M. Bellazzini et al. 2017; J. P. Greco et al. 2018). The gray shaded region represents UDGs; the diagonal boundary shows constant 〈μ〉 e  assuming μ 0(g) = 24 and Sérsic n = 1.
Paper: First Results from the Dragonfly Ultrawide Survey: The Largest 11 Quenched Diffuse Dwarf Galaxies in 3100 deg2 with Spectroscopic Confirmation
Authors: Zili Shen, William P. Bowman, Pieter van Dokkum, Roberto G. Abraham, Imad Pasha, Michael A. Keim, Qing Liu, Deborah M. Lokhorst, Steven R. Janssens, Seery Chen
Figure caption: pPXF stellar population fits of KCWI spectra. The galaxies in the left column require one star formation event, while the galaxies in the middle and right columns require multiple star formation events. For each galaxy, the orange line shows the light distribution as a function of template age in a single fit with a relatively high regularization parameter. The black line shows the average distribution from 30 bootstrap resampling trials using a lower regularization parameter.
Paper: First Results from the Dragonfly Ultrawide Survey: The Largest 11 Quenched Diffuse Dwarf Galaxies in 3100 deg2 with Spectroscopic Confirmation
Authors: Zili Shen, William P. Bowman, Pieter van Dokkum, Roberto G. Abraham, Imad Pasha, Michael A. Keim, Qing Liu, Deborah M. Lokhorst, Steven R. Janssens, Seery Chen
Figure caption: Left panel: DFUWS coverage on sky (R.A. and decl.). Each small gray rectangle within the footprint shows the size of one Dragonfly pointing to scale. The solid gray line marks the Galactic plane. Right panel: a zoomed-in view of the survey footprint with black stars showing the location of galaxies presented in this paper. Each galaxy is labeled with its ID number. Colored dots are known groups from the PGC1 catalog (E. Kourkchi & R. B. Tully 2017) with K  s  < 11 mag.
Paper: First Results from the Dragonfly Ultrawide Survey: The Largest 11 Quenched Diffuse Dwarf Galaxies in 3100 deg2 with Spectroscopic Confirmation
Authors: Zili Shen, William P. Bowman, Pieter van Dokkum, Roberto G. Abraham, Imad Pasha, Michael A. Keim, Qing Liu, Deborah M. Lokhorst, Steven R. Janssens, Seery Chen
Figure caption: Legacy cutouts of all DFUWS galaxies in this paper. The white rectangles represent the KCWI FOV and orientation during our 2023 October observing run.
Paper: The Electric Field and Its Impact on the Pitch Angle of Trapped Electrons in a Sub-ion-scale Magnetic Hole
Authors: Z. Z. Chen, T. Y. Wang, Y. Y. Liu, J. Yu, J. Wang, Y. D. Ye, Y. C. Jiang, H. S. Fu, J. Cui, J. B. Cao, R. E. Ergun
Figure caption: Overview of a sub-ion-scale MH in Earth’s magnetosheath. (a)–(e) MMS2 observations of (a) magnetic field strength, (b) magnetic field, (c) ion velocity, (d) DEF of ions, and (e) current density during the interval 08:58:00–09:45:00 UTC. (f)–(k) MMS observations of (f) magnetic field strength, (g) magnetic field B  x , B  y , and B  z  components, (h) electric field E  x , E  y , and E  z  components, (i) ion bulk velocity V  ix , V  iy , and V  iz  components, (j) electron bulk velocity V  ex , V  ey , and V  ez  components, and (k) current density during the interval 09:28:00–09:28:15 UTC. (l)–(w) MMS observations of (l) magnetic field strength, (m) magnetic field B  L  component, (n) magnetic field B  M  component, (o) magnetic field B  N  component, (p) current density, (q) electron velocity V  eL  component, (r) ion velocity V  iL  component, (s) electron velocity V  eM  component, (t) ion velocity V  iM  component, (u) electron velocity V  eN  component, (v) ion velocity V  iN  component, and (w) energy conversion in electron rest frame ( j  · ( E  +  v    e   ×  B )) during the interval 09:28:07.70–09:28:08.08 UTC. (x) 3D magnetic field topology reconstructed by the SOTE method. The data used in panels (a)–(k) are from MMS2. The data used in panels (l)–(x) are from all four satellites.
Paper: The Electric Field and Its Impact on the Pitch Angle of Trapped Electrons in a Sub-ion-scale Magnetic Hole
Authors: Z. Z. Chen, T. Y. Wang, Y. Y. Liu, J. Yu, J. Wang, Y. D. Ye, Y. C. Jiang, H. S. Fu, J. Cui, J. B. Cao, R. E. Ergun
Figure caption: Electric field and its effects on electron PA distributions. (a)–(e) MMS observations of (a) magnetic field B  L  component, (b) electric field E  L  component, (c) electric field E  M  component, (d) electric field E  N  component, and (e) parallel electric field with error bar (gray shaded area). The error bar is from MMS2. (f) A schematic diagram depicting effects of parallel electric field on electron PA distributions. (g)–(i) MMS2 observations of (g) magnetic field B  L  component, (h) electric field E  L  component, and (i) potential. (j)–(n) MMS2 observations of electron PA distributions at energy (j) 126.12 eV, (k) 165.09 eV, (l) 216.11 eV, (m) 282.89 eV, and (n) 370.31 eV. The magenta and black dashed lines in panels (j)–(n) denote the PAs with and without E ∥ effects, respectively.
Paper: The Electric Field and Its Impact on the Pitch Angle of Trapped Electrons in a Sub-ion-scale Magnetic Hole
Authors: Z. Z. Chen, T. Y. Wang, Y. Y. Liu, J. Yu, J. Wang, Y. D. Ye, Y. C. Jiang, H. S. Fu, J. Cui, J. B. Cao, R. E. Ergun
Figure caption: Electron properties in the sub-ion-scale MH. (a)–(d) MMS observations of (a) magnetic field B  L  component, (b) electron number density, (c) perpendicular electron temperature, and (d) parallel electron temperature. ((e)–(h)) Electron PA distributions measured by (e) MMS1, (f) MMS2, (g) MMS3, and (h) MMS4 at energy of 0.1–1.5 keV.
Paper: The Electric Field and Its Impact on the Pitch Angle of Trapped Electrons in a Sub-ion-scale Magnetic Hole
Authors: Z. Z. Chen, T. Y. Wang, Y. Y. Liu, J. Yu, J. Wang, Y. D. Ye, Y. C. Jiang, H. S. Fu, J. Cui, J. B. Cao, R. E. Ergun
Figure caption: Investigation of generalized Ohm’s law and energy conversion. (a) Magnetic field B  L  component. (b)–(d) MMS1 observations of electric field (b) E  L  component, (c) E  M  component, and (d) E  N  component. (e)–(g) MMS2 observations of electric field (e) E  L  component, (f) E  M  component, and (g) E  N  component. (h)–(j) MMS4 observations of electric field (h) E  L  component, (i) E  M  component, and (j) E  N  component. Measured electric field, electron convection term, and electron pressure gradient term are denoted by black, red, and blue curves in panels (b)–(i), respectively. (k) Electron flow vectors v  eMN  on the M − N plane, accompanied by a schematic diagram depicting electron flows, electric field, and energy conversion. (l) Magnetic field B  L  component. (m)–(o) energy conversion in electron rest frame measured by (m) MMS1, (n) MMS2, and (o) MMS4.
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: An illustration of the runaway flux problem when applying current reflection models to BHXRBs. The blue line shows the power-law spectrum adopted by relxillCp, which illuminates the disk. The green line shows the desired (“true”) spectrum corresponding to Compton-scattered emission from a 0.2 keV diskbb component. The red line shows our adopted multiplicative correction applied to the blue curve. This correction curtails the unphysical runaway at low energies and provides a reasonable approximation to the Comptonization spectrum.
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: Autocorrelation lags for Obs 5 MCMC walkers for i and R in. Each colored line shows the behavior of an individual walker. As shown here, the chains have been run to well over 10 times the characteristic autocorrelation length. This is important to ensure the converged chains obtain representative samples of the posterior parameter space with a useful effective sample size. Note how this measure can differ somewhat between different parameters.
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: The spectrum for Obs 5. Top: NICER (blue and green), Swift (purple and cyan: XRT), and NuSTAR (black: FPMA; red: FPMB) sources and associated background spectra (as stars) of MAXI J1813 for a continuum fit of tbabs × nthcomp. Bottom: associated data-to-model ratio plot. The residuals—NuSTAR in particular—show a broad peak around 6.5 keV corresponding to Fe–K fluorescence, an indicator of spectral reflection. We applied a rebinning on NICER and Swift in order to make the Fe–K line more visible with NuSTAR showing a broad small peak. Two GTIs apiece for each of Swift and NICER are included in Obs 5. We fit for spectral differences between GTIs to account for potential variation.
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: Corner plots show MCMC posterior distributions of parameters of interest for Obs 3 (left) and Obs 5 (right). We emphasize on the inner-radius parameter showing a better constrain in Obs 5 although in both cases the 1σ contour is showing a slightly truncated or nontruncation of the disk. In both cases the disk is moderate-to-high ionized and dense.
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: In this figure shows three ratio Chandra specters plot (black full source, red excluding the central pixel, and in green excluding the central pixel and the immediately adjacent pixels up and down) for Obs 5 with a simple model TBabs(simplcut(diskbb)).
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: The lightcurve of MAXI J1813 from the MAXI telescope during the stalled outburst from 2 to 20 keV. MAXI J1813 reaches its peak of luminosity quickly. The vertical solid lines, correspond to each observation (see Table 1). Obs 4 and 5 were not taken strictly simultaneously by each observatory, but were within 1 day. We therefore mark them as two separate lines in each case.
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: Top: Chandra in yellow, jointly with NICER, Swift, and NuSTAR, corresponding to Obs 5. Middle: Chandra data is represented by the color cyan jointly with Swift and NuSTAR. Bottom: Chandra data is represented by the color cyan jointly with Swift and NuSTAR. In all cases, Chandra is consistent with the other instruments.
Paper: Self-consistent Disk-reflection Analysis of the Black Hole Candidate X-Ray Binary MAXI J1813−095 with NICER, Swift, Chandra, and NuSTAR
Authors: Santiago Ubach, James F. Steiner, Jiachen Jiang, Javier García, Riley M. T. Connors, Guglielmo Mastroserio, Ye Feng, John A. Tomsick
Figure caption: The top panels show the Obs 1 and Obs 5 unfolded spectra and the lower panels are the ratio plots of each observation with the best fit. Both spectra show the continuum and the reflection model. The two NICER GTIs shown with the best S/N ratio. For Swift, we used only GTI due to only one was created for the left panel and two for the right panel.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Upper left: Observed low-resolution optical spectra of AT2022lri. The vertical lines mark host galaxy lines and spectral lines common in TDEs. The gray bands mark atmospheric telluric features. Strong telluric features have been masked. Upper right: Zoom-in to the Hα region of the observed spectra in velocity space. The ESI spectrum (δ t = 484.7 days, Section 2.1) is also shown for comparison. Lower left: The translucent lines show host and continuum subtracted spectra, with the overlying black lines showing the same spectra convolved with Gaussian kernels for visual clarity. For the LRIS spectrum at +269.4 days, we use a kernel FWHM of 200 km s−1. Since the Kast spectra are of lower SNR, we use FWHM kernel sizes of 1500 km s−1 (1000 km s−1) on the blue side at λ rest ≲ 6000 Å, and 300 km s−1 (200 km s−1) on the red side for the +210.4 day (+223.9 day) data. Lower right: Zoom-in to the Hα region of the host and continuum subtracted spectra in velocity space. The dashed red lines are Gaussian fits to the line profile.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Results of the GALFITS imaging decomposition for the LS z-band image of AT2022lri’s host galaxy. Upper left: The LS z-band image centered on AT2022lri, with a size of 30″. The shaded region represents a mask for contaminating sources. Upper middle: the model image generated using the best-fit GALFITS parameters detailed in Table 1. Upper right: the error-normalized residual image, obtained after subtracting the best-fit GALFITS model. Lower left: the model image of the bulge component. Lower middle: the model image of the disk component. Lower right: the surface brightness profile of the observed z-band image (black error bars), the bulge model (red), the disk model (blue), and the total GALFITS model (green).
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: UV and optical light curves of AT2022lri. Solid points represent measurements above 3σ, while semitransparent downward triangles show 3σ upper limits. The solid lines are single-temperature Gausssian-rise exponential-decline models in three bands (o ATLAS, g ZTF, and uvw1UVOT) fitted to the first-year data. The ticks along the upper axis marks the epoch of optical spectroscopy (Section 3.4). The inset shows the ATLAS light curve zoomed around time of first detection.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Net Doppler shifts during transmission for the models near 2.2 μm (left) and 1.3 μm (right). For the CO band on the left, we can see the main trend of our active models showing a sharp blueward slope, then flattening out. The drag-free models on the other hand simply become more blueshifted as transit progresses. For the water band, we see different trends between the models in the first half of transit, while all models flatten out during the second half of transit.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Equivalent width for a single CO feature as a function of phase for our models of WASP-76b and WASP-18b. Broad similarities exist in the behavior of this line, but the differences in the temperature profile result in variations between the active and drag-free models as well as between planets.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Line-of-sight velocities for the east and west limbs during ingress, transit, and egress for both the 0 G DG and PF models. The similarities between the models result in near-identical net Doppler shifts during transit.
Paper: Comparative Planetology of Magnetic Effects in Ultrahot Jupiters: Trends in High-resolution Spectroscopy
Authors: Hayley Beltz, Emily Rauscher
Figure caption: Here we show H2O abundance as a function of temperature and pressure. Overplotted are the substellar profiles from our active drag models. Between the models, we can see that the abundance of water can change by orders of magnitude.