adsabs/AstroCLIMB huggingface dataset:
Paper: Measurements of Magnetic Cloud Expansion through Multiple Spacecraft in Radial Conjunction
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Bin Zhuang, Florian Regnault, Antoinette B. Galvin
Figure caption: The fitting of the MC observed by MESSENGER and STB in the year 2010. MESSENGER: 2010-11-05T16:30:00–2010-11-06T14:00:00; STB: 2010-11-08T03:00:00–2010-11-09T09:00:00. The panels are the same as the first example. There are no V  p  data at the MESSENGER spacecraft.
Paper: Measurements of Magnetic Cloud Expansion through Multiple Spacecraft in Radial Conjunction
Authors: Wenyuan Yu, Nada Al-Haddad, Charles J. Farrugia, Noé Lugaz, Bin Zhuang, Florian Regnault, Antoinette B. Galvin
Figure caption: The fitting of the MC observed by Wind and Juno in the year 2013. Wind: 2013-04-14T16:30:00–2013-04-15T18:00:00; Juno: 2013-04-17T01:30:00–2013-04-18T13:00:00. The panels are the same as the first example. There are no V  p  data at the Juno spacecraft.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: CGM gas properties for two illustrative TNG100 L* halos. Left column is for a star-forming (SF) halo with M vir = 1.2 × 1012 M ⊙, and sSFR = 8.63 × 10−11 yr−1. Right column is for a quenched (Q) halo with M vir = 1.7 × 1012 M ⊙ and sSFR = 1.48 × 10−14 yr−1. Upper row: thermal phase plots for the CGM gas in the density (n H) vs. temperature (T) plane. The horizontal green dashed lines mark the virial temperatures T vir = 4.2 × 105 K (left) and 5.6 × 105 K (right). The red dashed lines are at 0.4 × T vir above which we define any gas as “hot” (see text). The hot gas mass fractions are f hCGM = 0.46 (left) and 0.17 (right). The vertical green dashed lines mark the mean hot CGM gas densities, ﹩{\bar{n}}_{{\rm{H}}}=2.7\times {10}^{-5}﹩ cm−3 (left) and 1.0 × 10−5 cm−3 (right). Second row: volume weighted electron pressure within R vir for all TNG100 particles, cool, intermediate, and hot (solid black curve with 1σ bars), and the hot phase electron pressure alone (solid red curve). The best-fitting PLMs for the hot gas are also plotted (green dashed curves) for which ϕ  T  = 1.1, a  P,th = 1.5, and a  n =1.3 (left), and ϕ  T  = 1.48, a  P,th = 1.7, and a  n =1.4 (right). Third row: volume weighted hydrogen density for all TNG100 particles (solid black curves), hot particles (solid red curves), and the PLM fits for the hot gas (green dashed). Bottom row: mass-weighted gas temperature for all TNG100 particles (solid black curves), hot TNG100 particles (solid red curves), and the PLM fits for which a  T  = a  P,th − a  n  = 0.2 (left) and 0.3 (right). Gas is hot above the red dashed lines. The background blue regions are 2D histograms showing the radially dependent simulation CGM particle values for the pressure, density, and temperature, within the two halos.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: The normalized Compton parameters, y(0.2R vir)/M vir,12 (left panel) and ﹩{Y}_{500}/{M}_{\mathrm{vir},12}^{5/3}﹩ (right panel) as functions of central stellar mass, M *. The gray strips show the predicted ranges for our PLM (see text). The black curves (with 1σ bars) are the medians for our set of TNG100 halos (SF+Q), and using the B. P. Moster et al. (2010) SMHM relation to convert the TNG100 virial masses to stellar masses. The vertically aligned squares (yellow, purple, and turquoise) are the FSM20, FSM20-maximal, and FSM17 predictions, and at the Galactic stellar mass of 6 × 1010 M ⊙ (the Galactic stellar mass departs from the B. P. Moster et al. 2010 relation; see text). The green square is the B+22 stack measurement, and the black filled gold circles are the D+23 data. In the right panel, we include the original P+13 data for massive galaxies and clusters (open black). We also show the three J. C. Hill et al. (2018) model estimates (PL blue, UB red, and CB cyan) for the intrinsic (one-halo) contributions to the P+13 observations.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Spherical Compton pressure integrals, Y 500 (kpc2) or ﹩{\tilde{Y}}_{500}﹩ (arcmin2), normalized by ﹩{M}_{\mathrm{vir},12}^{5/3}﹩, for the FSM20, FSM20-maximal, and FSM17 models (yellow, pink, and turquoise squares), together with the B+22 stack (green square), and D+23 measurements. For the D+23 data, we have used the B. P. Moster et al. (2010) relation to convert stellar mass to virial mass (see text). The dashed green line is for our best-fitting PLM (a  P,th = 2.03, ﹩{\phi }_{T}^{* }=2.39﹩) for the B+22 Compton-y profile in Figure 4. The red triangle is the Y 500 we infer from the recent Y. Zhang et al. (2024) X-ray observations of L* galaxies (see Section 8.1).
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: PLM fit results for our selected TNG100 halos. Left panel: Distribution of PLM pressure and density indices, a  P,th and a  n , for our TNG100 halo sample. The dotted line is for isothermal (a  P,th = a  n ) gas. Dashed is isentropic (a  n  = 3a  P,th/5). Right panel: pressure, density, and temperature indices, a  P,th, a  n , and a  T  =  a  P,th − a  n , (top, middle, and bottom) for SF, Q, and all halos, as functions of M vir.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Compton-y maps and profiles for the same two TNG100 SF and Q halos in Figure 12. Top row: Compton-y maps due to gas entirely within the virial radii indicated by the outer white circles (impact parameter b = 1). The dashed circles are at b 500 ≈ 0.5, and the dotted circles are at b = 0.2. Middle row: The black curves (with 1σ bars) are the radially averaged TNG100 Compton-y-parameter profiles extracted from the above TNG100 maps. The blue curves are Compton-y profiles that also include particles beyond the virial radii and out to 10 Mpc from the halo centers; the dashed green curves are the PLM forms for y(b) (Equation (16)) for the best-fitting PLM parameters shown in Figure 12. Bottom row: the projected TNG100 Y ⊥(b) integrals including gas only within the virial radii (black), out to 10 Mpc (blue), the dashed green curves are the PLM forms for Y ⊥(b) (Equation (22)) for the best-fitting PLM parameters in Figure 12.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: The normalized Compton parameters, y(0.2R vir)/M vir,12 (left panel), and ﹩{Y}_{500,s}/{M}_{\mathrm{vir},12}^{5/3}﹩ (right panel) as functions of halo virial mass. The symbols and curves are for the same quantities as in Figure 16. For the D+23 data, we have used the B. P. Moster et al. (2010) SMHM relation to convert the observed stellar masses to virial masses (see text).
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Spherical Compton pressure integrals, Y 500 (kpc2) or ﹩{\tilde{Y}}_{500}﹩ (arcmin2), normalized by ﹩{M}_{\mathrm{vir},12}^{5/3}﹩ (M vir ≡ 1012 M vir,12) for all of our selected TNG100 halos (black), and for the star-forming (SF, blue) and quenched (Q, red) halos separately. The green square is the B+22 stack measurement.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Cumulative distributions for the CGM gas masses, M <T /M CGM (left panel), and Compton-Y pressure integrals, Y <T /Y vir (right panel), as functions of T/T vir for TNG100 halos with M vir from 1011 to 1014.4 M ⊙. The vertical dashed lines mark the temperatures 0.4 × T vir above which we define the gas as “hot.”
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Left panel: the intrinsic temperature parameter, ϕ  T,TNG, as functions of virial mass, for all (black), SF (blue), and Q (red) halos in our TNG100 sample. Middle panel: the fitted PLM parameters ϕ  T,PLM, for these halos. Right panel: The ratios ϕ  T,PLM/ϕ  T,TNG vs. halo mass. The turquoise and yellow squares are for the FSM17 and FSM20 models (fiducial and maximal).
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Time series of daily data from 2015 January to 2023 September. (a) Count rate C and (b) leader fraction L from four Antarctic NMs, at SP (red), MC (green), JB (blue), and MA (black). (c) Solar wind speed (yellow), (d) B magnitude (blue), and (e) B  x  − B  y  (magenta). There are vertical grid lines every 81 days and minor ticks along the axis every 27 days. Note that for ease of comparison, the SP C data have been shifted downward by 15 s−1 and the SP L data have been shifted upward by 0.091.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Time series of daily data from 2015 March to 2023 September. (a) SP NM count rate (C), reflecting changes in the cosmic-ray flux at rigidities ≳1 GV. (b) SP leader fraction L, a measure of the cosmic-ray spectral index γ. The labels “FD” and “GLE” indicate Forbush decrease and ground-level enhancement events, respectively, in association with solar storms. (c) AMS-02 proton spectral index over the rigidity range 2.97–16.6 GV. The black line is based on measurements from 2015 March 3 to 2019 October 29. The gray shading around the line indicates the uncertainty associated with the fitting process. The magenta line represents the prediction of the spectral index beyond 2019 October 29, based on SP L using Equation (3), i.e., our prediction for what will be found from AMS-02 data when they are made public. The shading around this line represents the corresponding uncertainty.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Map of Antarctica indicating the locations of NMs used in this work (red dots): the South Pole (SP) station at an altitude of 2820 m; and the McMurdo (MC), Jang Bogo (JB), and Mawson (MA) stations near sea level. In each case, the rigidity-dependent response to primary cosmic rays has an atmospheric cutoff (i.e., threshold) at ∼1 GV.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Daily AMS-02 proton spectral index over the rigidity range 2.97–16.6 GV vs. the SP leader fraction L. The black line represents the linear fit to the data. The blue dashed lines, displaced from the black line by 1 standard deviation, illustrate the associated uncertainty when employing L as an estimator of the spectral index.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Normalized daily values of the SP leader fraction (red) and AMS-02 proton spectral index (2.97–16.6 GV; black) from 2015 March 3 to 2019 October 29, when both SP L and AMS-02 proton data were available, confirming that L serves as a proxy of the cosmic-ray proton spectral index.
Paper: Forecasting Solar Energetic Particle Events During Solar Cycles 23 and 24 Using Interpretable Machine Learning
Authors: Spiridon Kasapis, Irina N. Kitiashvili, Paul Kosovich, Alexander G. Kosovichev, Viacheslav M. Sadykov, Patrick O'Keefe, Vincent Wang
Figure caption: Timelines of the total line-of-sight unsigned flux (USFLUXL in Maxwells) and the unsigned flux R near polarity inversion lines (R_VALUE in Maxwells) for the total tracking period of AR 10180 and the day (2002 September 11) during which an SEP occurred (bottom). Underlined (solid green) are the start time (t_start keyword) of the SEP producing (positive) flare of this AR and the data points that the matching algorithm selects for the ML-ready data sets. The process of selecting the data points in the green boxes is referred to as SMARP/SHARP data selection in Figure 2.
Paper: Forecasting Solar Energetic Particle Events During Solar Cycles 23 and 24 Using Interpretable Machine Learning
Authors: Spiridon Kasapis, Irina N. Kitiashvili, Paul Kosovich, Alexander G. Kosovichev, Viacheslav M. Sadykov, Patrick O'Keefe, Vincent Wang
Figure caption: Probability density histograms for the six SHARP/SMARP predictors (Table 1) for the 10 hr window ML-ready data set for the positive (red) and negative (green) events. The red and green curves correspond to the fitted trend lines of the histogram bin values.
Paper: Forecasting Solar Energetic Particle Events During Solar Cycles 23 and 24 Using Interpretable Machine Learning
Authors: Spiridon Kasapis, Irina N. Kitiashvili, Paul Kosovich, Alexander G. Kosovichev, Viacheslav M. Sadykov, Patrick O'Keefe, Vincent Wang
Figure caption: Scheme of a workflow to prepare ML-ready data sets from the SMARP and SHARP (M. G. Bobra et al. 2021; P. A. Kosovich et al. 2024). The arrows depict the previous work (light black, Section 2), the flare and SEP coupling process (black, Section 3), and the SMARP/SHARP data selection (blue, Section 4).
Paper: Forecasting Solar Energetic Particle Events During Solar Cycles 23 and 24 Using Interpretable Machine Learning
Authors: Spiridon Kasapis, Irina N. Kitiashvili, Paul Kosovich, Alexander G. Kosovichev, Viacheslav M. Sadykov, Patrick O'Keefe, Vincent Wang
Figure caption: Probability density distribution of the 3356 positive (green) and 110 negative (red) events in our data set that occurred between 1996 April 4, and 2022 December 30 (SHARP/SMARP data set availability) for the logarithm of flare intensities (left panel) and angular distances to the magnetic foot point of the Earth (right panel).
Paper: Forecasting Solar Energetic Particle Events During Solar Cycles 23 and 24 Using Interpretable Machine Learning
Authors: Spiridon Kasapis, Irina N. Kitiashvili, Paul Kosovich, Alexander G. Kosovichev, Viacheslav M. Sadykov, Patrick O'Keefe, Vincent Wang
Figure caption: Distribution of 100 score values of ACC, TSS, HSS FAR, and F1 (left panel). Each metric is calculated using the entries of the confusion matrix produced in each run, the average over 100 runs (right panel). The values were obtained using the R_VALUE and the ANG_DIST on a logistic regression model and constitute the best SEP prediction the SMARP/SHARP data can achieve. The box range shows the interquartile range, the green line inside is the median value, the whiskers show the results range, and the circles show two outlier values. The samples are obtained using the clean data set, where non-SEP-producing flares in SEP-producing ARs are omitted and used on a balanced training method where positive and negative training and evaluation data sets are of equal size.
Paper: Forecasting Solar Energetic Particle Events During Solar Cycles 23 and 24 Using Interpretable Machine Learning
Authors: Spiridon Kasapis, Irina N. Kitiashvili, Paul Kosovich, Alexander G. Kosovichev, Viacheslav M. Sadykov, Patrick O'Keefe, Vincent Wang
Figure caption: Box plots of the distribution of 100 score values of ACC, TSS, HSS FAR, and F1, for seven decision thresholds τ. The values were obtained using the R_VALUE and the ANG_DIST to train an experimental logistic regression model. The box range shows the interquartile range, the green line inside it shows the median value, the whiskers show the results range, and the circles show two outlier values. These results correspond to the seventh row in Table 5 for τ = 0.5.
Paper: Precise Measurements of TeV Halos around Geminga and Monogem Pulsars with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. de la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, P. Hüntemeyer, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, V. Joshi, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Urea-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Wu, S. Yun-Cárcamo, H. Zhou, C. de León, M. Di Mauro
Figure caption: Radial profile of Geminga (left) and Monogem (right) divided into three energy bins. Top: for energies of 1–17 TeV. Middle: for energies of 17–31 TeV. Bottom: for energies of 31–316 TeV. Radial profiles show no significant change for the three different energy bands.
Paper: Pre-peak Emission in Tidal Disruption Events
Authors: Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-fei Jiang, 燕飞 姜
Figure caption: Gas density (first and second rows) and lab-frame radiation energy density (third and fourth rows) snapshots from RSI50Edd10. The three columns corresponds to t = 21.9, 94.6, and 240.8 hr; the white text labels the time since stream–stream collision. The density ﹩\rho ^{\prime} ﹩ and radiation energy density ﹩{e}_{R}^{\prime} ﹩ are unitless, with the scaling reported in Section 2.2 to convert to physical units. The first and third rows are quantities volume averaged over Δθ ∼ 5° near the θ = π/2 plane, providing a “face-on view.” The second and fourth rows show the volume average from Δϕ ∼ 5° near the ϕ inj plane, providing a “side view.” The white curve in the third row shows the shape of estimated light curve in log scale (Figure 7); the blue circles label the time of the current snapshot.
Paper: Pre-peak Emission in Tidal Disruption Events
Authors: Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-fei Jiang, 燕飞 姜
Figure caption: The first two rows show gas density snapshots from RSI50Edd10 at t = 56.1 hr. The first row is a “face-on” view at the orbital plane; the plotted quantity is averaged over Δθ ∼ 5° near the θ = π/2 plane. The second row is a “side view” that cuts through the gray dashed line in the first row; the plotted quantity is the volume average from Δϕ ∼ 5° near the ϕ = 2.07 plane. The third row is flow speed normalized to speed of light; the black solid lines show the velocity streamlines at this projection. The fourth row shows ﹩{E}_{t}^{{\prime} }﹩ (Equation (9)); a positive value corresponds to unbound gas. The blue crosses label selected sample points to extrapolate ballistic trajectories in Figure 19.
Paper: The Wanderer: Charting WASP-77A b’s Formation and Migration Using a System-wide Inventory of Carbon and Oxygen Abundances
Authors: David R. Coria, Neda Hejazi, Ian J. M. Crossfield, Maleah Rhem
Figure caption: Interpolating the stellar 12C/13C ratio from our high-resolution and high signal-to-noise Keck/HIRES spectrum. On the left, we show our three selected 13CH lines, post-renormalization. We have labeled, in black, some nearby atomic and molecular lines that help us determine the best-fit base model spectrum. Refer to Table 2 for the complete line list. On the right, we zoom in on the χ2 fit windows to better see the separation between model spectra with high and low 12C/13C ratios. We then calculate χ 2 values between the model spectra and the observed spectrum for each target line, and fit the points with a cubic spline. The minimum of the spline represents the best-fit 12C/13C for the individual 13CH line.
Paper: Pre-peak Emission in Tidal Disruption Events
Authors: Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-fei Jiang, 燕飞 姜
Figure caption: The outflow rate (first row), accretion rate (second row), luminosity (third row), and mass-weighted average outflow speed (fourth row) of RSI50Edd10. In the first row, the solid line shows the total mass outflow rate, normalized to ﹩{\dot{M}}_{\mathrm{Edd}}﹩. The dotted line shows the unbound outflow rate. In the third row, the dotted line shows the kinetic luminosity (Equation (10)) carried by the unbound outflow, and the dotted line in the fourth row shows the mass-weighted average outflow speed for unbound gas. The horizontal dashed line labels the escape velocity at the measuring radius.
Paper: Pre-peak Emission in Tidal Disruption Events
Authors: Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-fei Jiang, 燕飞 姜
Figure caption: The integrated ballistic trajectories for black hole mass M BH = 107 M ⊙ (blue), 8 × 106 M ⊙ (orange), and 6 × 106  M ⊙ (red), according to E. Tejeda & S. Rosswog (2013). The filled circles label the stream injection location in each simulation.
Paper: Pre-peak Emission in Tidal Disruption Events
Authors: Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-fei Jiang, 燕飞 姜
Figure caption: The average density (top panel) and average gas temperature (bottom panel) of RSI50Edd10 at t = 240 hr. In the top panel, the solid black line shows average gas density through spherical shells. The purple solid line shows the average gas density through a finite range of θ but excluding the orbital plane, π/32 < ∣θ − π/2∣ < π/8 near π/2. The three vertical dashed lines are tidal radius (also pericenter radius given β = 1.0) r  p , stream–stream collision radius r SI, and injection radius r inj.
Paper: The Wanderer: Charting WASP-77A b’s Formation and Migration Using a System-wide Inventory of Carbon and Oxygen Abundances
Authors: David R. Coria, Neda Hejazi, Ian J. M. Crossfield, Maleah Rhem
Figure caption: Interpolating the stellar 12C/13C ratio from the publicly available, high-resolution, and high signal-to-noise VLT/ESPRESSO spectrum. Similar to Figure 2, we show our selected 13CH lines, post-renormalization on the left. On the right, we show a zoom-in on the χ 2 fit windows and the χ 2 minimization used to determine 12C/13C for individual 13CH lines.
Paper: The Wanderer: Charting WASP-77A b’s Formation and Migration Using a System-wide Inventory of Carbon and Oxygen Abundances
Authors: David R. Coria, Neda Hejazi, Ian J. M. Crossfield, Maleah Rhem
Figure caption: Interpolating the stellar 12C/13C ratio from the publicly available, high-resolution, and high signal-to-noise VLT/ESPRESSO spectrum. Similar to Figure 2, we show our selected 13CH lines, post-renormalization on the left. On the right, we show a zoom-in on the χ2 fit windows and the χ 2 minimization used to determine 12C/13C for individual 13CH lines.