adsabs/AstroCLIMB huggingface dataset:
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Overview of the X-ray QPO detected in 1ES 1927+654. (A) Long-term NICER light curves in energy ranges of 0.3–2 keV (blue circles) and 2–10 keV (red circles) beginning 2 months after the optical outburst (M. Masterson et al. 2025). The epoch of the QPO detected by XMM-Newton is shaded in gray. The timing of the millihertz QPO detections suggests a possible association with the formation of the jet, as inferred from radio observations (S. Laha et al. 2025; E. T. Meyer et al. 2025). (B) Evolution of the QPO frequency over time. The purple stars indicate significant detections of the QPO (>6σ), while the gray circles denote marginal detections (<6σ). The presented QPO frequency and corresponding 1σ error bars are obtained from the PSD fitting with an additional Lorentzian. (C) Normalized phase-folded light curves (QPO waveforms) of the ∼1.67 mHz QPO (obsID 0915390701) across multiple energy bands, referenced to the 2–10 keV QPO phase. Data points with error bars are unbinned waveforms, while solid lines are best-fit sinusoidal functions. The data are plotted over two QPO cycles by repeating the pattern. The vertical dashed lines indicate the peak phases of the QPO waveforms obtained from sinusoidal fittings.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Soft-lag amplitude versus black hole mass and soft-lag frequency versus black hole mass trends. The data points with error bars represent the observational results of the millihertz QPO in 1ES 1927+654. The best-fit linear models (in log–log space) for the correlations observed in multiple radio-quiet AGNs (RQ-AGNs; B. De Marco et al. 2013), along with the combined 1σ error on the slope and normalization, are overlaid as the continuous and dashed lines. The plots of the models and the corresponding 1σ confidence intervals are directly taken from public work (B. De Marco et al. 2013). The dotted lines in the left panel represent the light-crossing times at 1Rg, 2Rg, and 6Rg as a function of black hole mass. The plotted soft-lag frequency of 1ES 1927+654 is set to the observed QPO frequency.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: QPO light curves and corresponding PSDs derived from VME analysis. (A) Extracted QPO light curves using the VME method. The orange lines show results obtained with the optimal α values determined from Figure B1 (Approach 1). The blue lines represent results from the posterior distributions derived through the Bayesian approach (Approach 2). The black lines indicate the original XMM-Newton 2–10 keV light curves. (B) PSDs corresponding to the extracted QPO light curves. The colors of the curves match those in panel (A). The original PSDs are shown in black, while the gray curves represent the total PSD model (consisting of L2, C0, and PVME components) plotted from the posterior distributions of the Bayesian approach.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Spectral properties of the QPO in 1ES 1927+654. (A) Comparison of QPO spectra with time-averaged energy spectra. The individual model components are indicated by different line styles and colors. The QPO spectra and their corresponding fit models are scaled by a factor of 10 for better comparison. (B) Variability of the spectral index and hardness ratio over the QPO cycle. The hardness ratio is defined as the flux ratio between the 2–10 keV and 0.3–2 keV energy bands. The phase-folded QPO light curve in 2–10 keV is plotted in each panel as a gray dashed line for reference.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Relationship between PSD FWHM of the extracted QPO mode and the VME α parameter. The horizontal dashed lines represent the FWHM values obtained from the PSD modeling of the millihertz QPO with a Lorentzian function. In the VME analysis, the FWHM decreases monotonically with increasing α, allowing us to estimate reasonable α values for the two observations of 9078 and 6895, respectively.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Posterior probability distributions for parameters derived from Bayesian modeling to estimate the VME parameter α for two observations. (A) Distributions corresponding to the observation with the 1.67 mHz QPO. (B) Distributions corresponding to the observation with the 2.21 mHz QPO.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Phase-folded QPO light curves in three representative energy bands, fitted with a sinusoidal model. The data points with error bars represent the observed count rates in each time bin; the solid lines indicate the best-fit sinusoidal models. The vertical dashed lines mark the best-fit peak phases of the QPO waveform.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Spectral properties of the millihertz QPO from a Monte Carlo simulation analysis using the MONK code. The top panels present the time-averaged (black stars), representative phase-resolved (colored dots), and QPO (blue triangles, scaled by relevant factors for better comparison) spectra with modulations in the accretion rate ﹩\dot{m}﹩, coronal optical depth τ, and corona temperature kTe, respectively, while the lower panels present the corresponding modulations in parameters during the QPO cycle, where F0.3−10 keV represents flux in the energy range of 0.3–10 keV in units of 10−11erg s−1 cm−2, and HR represents the hardness ratio (defined as the flux ratio between the 2–10 keV and 0.3–2 keV energy bands). (A) Spectral properties with modulation in ﹩\dot{m}﹩. (B) Spectral properties with modulation in τ. (C) Spectral properties with modulation in kTe.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Joint fitting of the time-averaged energy spectrum and the QPO rms–energy and lag–energy spectra for the 1.67 mHz QPO observation (obsID 0915390701). In the middle and right panels, the solid green lines represent the best-fitting model with VKOMPTHDK. Bottom panels: residuals.
Paper: Revealing an Oscillating and Contracting Compact Corona near the Event Horizon of the Supermassive Black Hole in 1ES 1927+654
Authors: Qing-Cang Shui, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Yu-Peng Chen, Long Ji, Ling-Da Kong, Liang Zhang, Jing-Qiang Peng, Peng-Ju Wang
Figure caption: Variability of spectral parameters over the millihertz QPO cycle derived from phase-resolved spectral analysis. From top to bottom, the panels show: the spectral index (Γ), blackbody temperature (kT), unabsorbed model fluxes (in units of 10−11 erg s−1 cm−2) for the energy ranges 0.3–2 keV and 2–10 keV, and hardness ratio (flux ratio between these two bands). The phase-folded QPO light curve in the 2–10 keV energy band is plotted in each panel as a gray dashed line for reference.
Paper: A Close Look at the Closest Nitrogen-loud Active Galaxy Akn 564
Authors: Chenwei Yang, Bo Liu, Peng Jiang, Xiheng Shi, Yipeng Zhou, Yaqi Zhao, Xingyu Zhou, Xiang Pan, Hongyan Zhou
Figure caption: Line-ratio abundance diagnostics for multiple galaxy regions of Akn 564 and comparison with other objects. (a) BLR diagnostics employ ratios robust from cospatial emission (solid; from H02), supplemented by metal-to-helium ratios (dashed) that provide reliable abundance scales for Akn 564, where key parameters (ionizing continuum, ionization parameter, and density) are well constrained. (b) Diagnostics for the NLR region. In addition to the commonly used [O III] and [N II] lines, we have included line ratios related to [S III]. (c) Diagnostics for the H II region, using the same color scheme as panel (b). (d) Comparison of abundance constraints from the BLR, NLR, and H II regions with other objects. Note that the x-axis range is broader here to encompass all comparison objects. Data for local Seyfert 2 galaxies were obtained from O. L. Dors et al. (2024), while H II region measurements in the nearby spiral galaxy NGC 3184 come from D. A. Berg et al. (2020). Nitrogen-enriched objects across cosmic time include the local blue compact galaxy HS 0837+4717 at z = 0.042 (S. Pustilnik et al. 2004) and high-redshift “extreme N-emitters” such as GS3073 at z = 5.55 (X. Ji et al. 2024), CEERS-1019 at z = 8.68 (R. Marques-Chaves et al. 2024), and GN-z11 at z = 10.6 (P. Senchyna et al. 2024).
Paper: A Close Look at the Closest Nitrogen-loud Active Galaxy Akn 564
Authors: Chenwei Yang, Bo Liu, Peng Jiang, Xiheng Shi, Yipeng Zhou, Yaqi Zhao, Xingyu Zhou, Xiang Pan, Hongyan Zhou
Figure caption: DESI spectra of Akn 564 with the blue spectrum from the nucleus (designated “Core”) and the green and red spectra from two distinct regions within the galactic disk, designated “AP1” (the brighter one to the east) and “AP2” (the fainter one to the northwest), respectively. The Core spectrum exhibits features typical of a NLS1 galaxy, whereas the AP1 and AP2 spectra are dominated by emission-line signatures characteristic of star-forming regions. The left inset panel shows a DESI image of Akn 564 with the positions of the three spectroscopic apertures overlaid. AP1 and AP2 are located at projected distances of 11﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 (5.4 kpc) and 11﹩\mathop{.}\limits^{\unicode{x02033}}﹩6 (5.6 kpc) from the Core, respectively. The right inset panel shows the location of the line ratios measured from all three spectra on the BPT diagram.
Paper: A Close Look at the Closest Nitrogen-loud Active Galaxy Akn 564
Authors: Chenwei Yang, Bo Liu, Peng Jiang, Xiheng Shi, Yipeng Zhou, Yaqi Zhao, Xingyu Zhou, Xiang Pan, Hongyan Zhou
Figure caption: The HST UV spectrum of Akn 564 (blue) is compared to the composite spectrum of 293 nitrogen-loud quasars (light blue; L. Jiang et al. 2008). Akn 564 shows significantly stronger [N III] λ1750 and [N IV] λ1486 emission than this composite. For broader reference, the SDSS mean quasar spectrum (gray; D. E. Vanden Berk et al. 2001) is also included, on which the [N III] λ1750 and [N IV] λ1486 emission lines are barely detected. Key emission lines are labeled at the top. In addition to the nitrogen enhancement, the Akn 564 spectrum displays systematically narrower line widths compared to both templates. The Akn 564 spectrum is an average of multiple HST exposures, and the comparison templates have been vertically scaled.
Paper: A Close Look at the Closest Nitrogen-loud Active Galaxy Akn 564
Authors: Chenwei Yang, Bo Liu, Peng Jiang, Xiheng Shi, Yipeng Zhou, Yaqi Zhao, Xingyu Zhou, Xiang Pan, Hongyan Zhou
Figure caption: UV and optical spectral lines for Akn 564 (blue), overlaid with the sum of the best-fit models (dashed red). Individual line components (thin colored lines) and their center wavelengths (vertical dashed gray lines) are also displayed. BELs were fitted with Lorentzian profiles, while NELs were fitted with Gaussian profiles. For BELs affected by BALs (Lyα, [N v], [C IV], and [Si IV] + [O IV] blended), the absorption troughs were masked during fitting.
Paper: A Close Look at the Closest Nitrogen-loud Active Galaxy Akn 564
Authors: Chenwei Yang, Bo Liu, Peng Jiang, Xiheng Shi, Yipeng Zhou, Yaqi Zhao, Xingyu Zhou, Xiang Pan, Hongyan Zhou
Figure caption: Comparison of the line intensities calculated by the CLOUDY slab model to the observed line intensities, normalized by He II λ1640. The black dashed line represents a 1:1 ratio. The CLOUDY slab model calculations were performed using best estimated parameters, with values provided in Section 4.1.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Same model as in Figure 7 but applied in the FEROS, HARPS, and ESPRESSO RV time series. The left panel shows the full model to the RVs. The middle panel shows the phased signal for TIC 118798035 c after removing the contribution of the other planets. The right panel shows the phased model signal TIC 118798035 d after removing the contribution of the other planets. The signal of TIC 118798035 b is too small and practically unconstrained; thus, is not shown. The bottom panels show the RV model residuals. The error bars include the jitter obtained from the analysis presented in Section 3.4.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: TESS light curves of TIC 118798035 from sectors 13, 39, 66, and 93, from top to bottom. Regions around transits of candidates b, c, and d are marked in red, blue, and green, respectively. We also plot the model for the out-of-transit variations computed with the Gaussian process described in Section 3.3.2.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: GLS periodogram generated from the FEROS, HARPS, and ESPRESSO RVs of TIC 118798035. The horizontal lines correspond to the 10% and 1% false-alarm probabilities. The red and blue dashed vertical lines mark the orbital periods of candidates b and c, respectively. The green dashed vertical lines mark the possible period aliases of TIC 118798035 d based on TESS photometry.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Same as in Figure 4 but for the bisector spans, FWHM, and S-index. Here the green dashed line corresponds to the orbital period of TIC 118798035 d constrained by the RVs and HATPI light curve.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: TTV time series and best-fit model of TIC 118798035 b, c, and d. The bottom panels show the TTV model residuals.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: TESS and ground-based transits of TIC 118798035 b centered on the transit time predicted from a linear ephemeris. The transit model generated by juliet is also plotted for each transit.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Same as Figure 2 but for TIC 118798035 c.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Same as Figure 2 but for TIC 118798035 d.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Relative planet bulk metallicities as a function of the planet mass for the TIC 118798035 system (black circles) and the solar system (Neptune, Uranus, Jupiter; red circles). We also show the empirical relation found by Y. Chachan et al. (2025).
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Orbital evolution of the TIC 118798035 system for an extent of 1000 yr for the best-fit (maximum −lnL) sample from the MCMC posteriors. Top panels, from left to right: evolution of the planetary semimajor axes, eccentricities, and inclinations, where TIC 118798035 b is shown with blue, TIC 118798035 c with red, and TIC 118798035 d with green. Bottom panels, from left to right: evolution of the period ratio between the inner pair Pc/Pb, the outer pair Pd/Pc, and the libration of the apsidal angle Δωc−d in aligned configuration around 0∘.
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Systems containing two or more transiting planets with a radius larger than 0.5 RJ. The size of the circles scales up with the planet radius. Planets with masses measured with a precision better than 20% have blue borders. The circles are color-coded by transmission spectroscopy metric (TSM).
Paper: A Compact Multiplanet System of Three Transiting Giant Planets around TIC 118798035
Authors: Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, Néstor Espinoza, Felipe I. Rojas, Marcelo Tala Pinto, Matías I. Jones, Daniel Thorngren, Lorena Acuña, Jan Eberhardt, Yared Reinarz, Helem Salinas, Michaela Vítková, Juan I. Espinoza-Retamal, Gaspar Bakos, Attila  Bódi, Gavin Boyle, Zoltán Csubry, Joel Hartman, Anthony Keyes, Vincent Suc, Geert Jan Talens
Figure caption: Posterior probability distributions from the joint TTV and RV MCMC modeling of TIC 118798035. The median values of the fitted and derived parameters are indicated by red lines that create the shape of a plus sign. Black contours mark the 1σ, 2σ, and 3σ confidence intervals of the distributions.
Paper: A Carbon-rich Atmosphere on a Windy Pulsar Planet
Authors: Michael Zhang, Maya Beleznay, Timothy D. Brandt, Roger W. Romani, Peter Gao, Hayley Beltz, Matthew Bailes, Matthew C. Nixon, Jacob L. Bean, Thaddeus D. Komacek, Brandon P. Coy, Guangwei Fu, Rafael Luque, Daniel J. Reardon, Emma Carli, Ryan M. Shannon, Jonathan J. Fortney, Anjali A. A. Piette, M. Coleman Miller, Jean-Michel Desert
Figure caption: Temperature structure from 3D GCMs. Here, we show maps of the time-averaged temperature and streamlines at two isobars (left) and equatorial temperature–pressure profiles (right) for two different heat deposition cases. The subpulsar point is indicated with a star. The isobaric projections correspond to roughly 20 mbar (the top row of the maps)—shown by the blue substellar marker and dashed line in the T–P profiles—and 2 bar (the bottom row of the maps)—corresponding to the purple dashed line and marker from our GCMs with a bespoke heating scheme given heat depositions centered at 3 bar and 0.3 bar. The combination of a rapid rotation rate and deep heating results in the circulation pattern. Specifically, we find westward-shifted midlatitude hot regions at the 2 bar pressure level for both cases of heat deposition. However, at 20 mbar, the model with more shallow heating shows a different temperature structure that is more symmetric and unlikely to produce a westward offset. In the more deeply heated 3 bar case, the hot region being centered at negative longitudes implies a flux peak after phase 0.5, as observed.