adsabs/AstroCLIMB huggingface dataset:
Paper: Sudden Polarization Angle Jumps of the Repeating Fast Radio Burst FRB 20201124A
Authors: J. R. Niu, W. Y. Wang, J. C. Jiang, Y. Qu, D. J. Zhou, W. W. Zhu, K. J. Lee, J. L. Han, B. Zhang, D. Li, S. Cao, Z. Y. Fang, Y. Feng, Q. Y. Fu, P. Jiang, W. C. Jing, J. Li, Y. Li, R. Luo, L. Q. Meng, C. C. Miao, X. L. Miao, C. H. Niu, Y. C. Pan, B. J. Wang, F. Y. Wang, H. Z. Wang, P. Wang, Q. Wu, Z. W. Wu, H. Xu, J. W. Xu, L. Xu, M. Y. Xue, Y. P. Yang, M. Yuan, Y. L. Yue, D. Zhao, C. F. Zhang, D. D. Zhang, J. S. Zhang, S. B. Zhang, Y. K. Zhang, Y. H. Zhu
Figure caption: Polarization profiles of FRB 20201124A burst #1. The PA swing and the profile of the 1000–1500 MHz band are shown in panels (a) and (b). The polarization profile and PA of five 100 MHz subbands are displayed separately on the left side of panel (c), (d), (e), (f), and (g). The black curve represents the total intensity I, the red linearly polarized intensity L, and the blue curve circularly polarization V. The value of PA ranges from −90° to 90°. The burst polarization evolves with time and frequency. On the right side of panel (c), (d), (e), (f), and (g), we show how the two-dimensional I, Q, U, and V vary with the horizontal axis (time) and the vertical axis (frequency).
Paper: Sudden Polarization Angle Jumps of the Repeating Fast Radio Burst FRB 20201124A
Authors: J. R. Niu, W. Y. Wang, J. C. Jiang, Y. Qu, D. J. Zhou, W. W. Zhu, K. J. Lee, J. L. Han, B. Zhang, D. Li, S. Cao, Z. Y. Fang, Y. Feng, Q. Y. Fu, P. Jiang, W. C. Jing, J. Li, Y. Li, R. Luo, L. Q. Meng, C. C. Miao, X. L. Miao, C. H. Niu, Y. C. Pan, B. J. Wang, F. Y. Wang, H. Z. Wang, P. Wang, Q. Wu, Z. W. Wu, H. Xu, J. W. Xu, L. Xu, M. Y. Xue, Y. P. Yang, M. Yuan, Y. L. Yue, D. Zhao, C. F. Zhang, D. D. Zhang, J. S. Zhang, S. B. Zhang, Y. K. Zhang, Y. H. Zhu
Figure caption: Observed and simulated Stokes profile FRB 20201124A Burst #1. Burst #1 in frequency bands 1021–1190 MHz with DM of 413.5 pc cm−3 is shown in panel (a). The polarization position angle of the low-frequency double-peak structure exhibits an orthogonal jump phenomenon with a jump angle of 66°. Panel (b) shows the simulated Stokes profile and its corresponding PA swing.
Paper: Sudden Polarization Angle Jumps of the Repeating Fast Radio Burst FRB 20201124A
Authors: J. R. Niu, W. Y. Wang, J. C. Jiang, Y. Qu, D. J. Zhou, W. W. Zhu, K. J. Lee, J. L. Han, B. Zhang, D. Li, S. Cao, Z. Y. Fang, Y. Feng, Q. Y. Fu, P. Jiang, W. C. Jing, J. Li, Y. Li, R. Luo, L. Q. Meng, C. C. Miao, X. L. Miao, C. H. Niu, Y. C. Pan, B. J. Wang, F. Y. Wang, H. Z. Wang, P. Wang, Q. Wu, Z. W. Wu, H. Xu, J. W. Xu, L. Xu, M. Y. Xue, Y. P. Yang, M. Yuan, Y. L. Yue, D. Zhao, C. F. Zhang, D. D. Zhang, J. S. Zhang, S. B. Zhang, Y. K. Zhang, Y. H. Zhu
Figure caption: Burst width and energy distribution of FRB 20201124A in the first and second episodes. We mark the OPM jump bursts in red scatter.
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: Panel (a) shows the DECaLS g-band image of MaNGA target 1-383997, i.e., LEDA 1678924. The detection of optical counterpart of MJ0818+2257 is marked by red ellipse. Panel (b) represents the stellar continuum– and absorption-subtracted observed spectra of LEDA 1678924 (i.e., spiral galaxy) and outlying emission blob (i.e., LSB dwarf galaxy). Panel (b1) shows the zoomed-in view of Hβ [O III]λ4959,5007 emission lines. Similarly, panel (b2) presents the zoomed-in view of [N II]λ6548,6583 and Hα emission lines.
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: Left: the BPT diagram labeled according to the different regions related to star formation (SF), AGN (Seyfert or LINER), and composite (AGN+SF) activities. Spaxels from LEDA 1678924 and MJ0818+2257 are denoted by dots, while the star symbol represents the data point for LEDA 1678982 (see Figures 1(c) and (d)). Right: the color-coded spatially resolved 2D-BPT diagram corresponds to the left figure.
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: The rotation velocity of ionized gas derived using Hα emission line (top left panel). Top right panel represents its zoomed-in view centered on the central velocity of MJ0818+2257. Similarly, bottom left panel shows the velocity dispersion, and bottom right panel represents its zoomed-in view. In each panel, the location of MJ0818+2257 is marked by black dashed ellipse.
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: Panels (a) and (b) show the Hα and [O III]λ5007 emission-line maps, respectively. In the emission-line maps, the outlying emission blob (which we later name as MJ0818+2257) is marked with a red dashed ellipse. Panels (c) and (d) represent the SDSS g-band image overlaid with the Hα (red) and [O III]λ5007 (yellow) emission-line contours, indicating that there is no optical counterpart of the outlying emission blob.
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: The radio continuum contours as shown by green solid lines at different frequencies that include 1.4 GHz (top left), 3 GHz (top right), 4.86 GHz (bottom left), and 8.46 GHz (bottom right) overlaid on optical g-band image from the DECaLS survey. In each panel, the white contours represent the MaNGA [O III]λ5007 emission line at the location of MJ0818+2257 and the spiral galaxy. Here north and east are up and left, respectively.
Paper: How Rare Are TESS Free-floating Planets?
Authors: Hongjing Yang, 弘靖 杨, Weicheng Zang, 伟呈 臧, Tianjun Gan, 天君 干, Renkun Kuang, 仁昆 匡, Andrew Gould, Shude Mao, 淑德 毛
Figure caption: The expected FFP yields of TESS S61 in mass bins. Each mass bin represents 1 dex in mass. On the top of each bin, the sensitivity (red) and the expected number (black) after considering the FFP mass function from Sumi et al. (2023) are labeled. Summing over all mass bins gives the total expected number N FFP,S61 = 1.81 × 10−3.
Paper: How Rare Are TESS Free-floating Planets?
Authors: Hongjing Yang, 弘靖 杨, Weicheng Zang, 伟呈 臧, Tianjun Gan, 天君 干, Renkun Kuang, 仁昆 匡, Andrew Gould, Shude Mao, 淑德 毛
Figure caption: Light curve of a simulated SNR﹩{}_{\mathrm{entire}}\gt 10﹩, but SNReach ∼ 1 FFP event (upper right panels) and MCMC optimization results of the microlensing model fit to it (lower left corner plot). The true (input) values are marked in red. Parameters including u 0, t E, ρ, and q blend are degenerated and are not well constrained.
Paper: How Rare Are TESS Free-floating Planets?
Authors: Hongjing Yang, 弘靖 杨, Weicheng Zang, 伟呈 臧, Tianjun Gan, 天君 干, Renkun Kuang, 仁昆 匡, Andrew Gould, Shude Mao, 淑德 毛
Figure caption: The expected FFP yields of TESS S61 in source distance and stellar radius bins. The bin sizes are ΔD S = 0.1 kpc and ﹩{\rm{\Delta }}\mathrm{log}[{R}_{{\rm{S}}}/{R}_{\odot }]=0.1﹩. The black dashed lines are the contours of the angular stellar radius θ *.
Paper: How Rare Are TESS Free-floating Planets?
Authors: Hongjing Yang, 弘靖 杨, Weicheng Zang, 伟呈 臧, Tianjun Gan, 天君 干, Renkun Kuang, 仁昆 匡, Andrew Gould, Shude Mao, 淑德 毛
Figure caption: The expected FFP yields of TESS S61 in sky region bins. The bin sizes are ΔR.A. = Δdecl. = 1°. The integral over the entire S61 gives N FFP, S61 = 1.81 × 10−3. The dashed line represents the Galactic plane. The “⋆” symbol marks TIC-107150013, the candidate event reported by Kunimoto et al. (2024).
Paper: How Rare Are TESS Free-floating Planets?
Authors: Hongjing Yang, 弘靖 杨, Weicheng Zang, 伟呈 臧, Tianjun Gan, 天君 干, Renkun Kuang, 仁昆 匡, Andrew Gould, Shude Mao, 淑德 毛
Figure caption: The expected FFP yields of TESS S61 as a function of the source magnitude using the proposed new strategy. The shaded region plots the expected yields and the red dashed line is a quadratic fit to its logarithm (see Equation (12)).
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: Left: the observed velocity map for LEDA 1678924 (i.e., spiral galaxy) and LSB dwarf galaxy (i.e., outlying emission blob). Right: their corresponding histogram velocity distributions and their respective systematic velocities are shown by vertical lines.
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: Deep optical r- (left), i- (middle), and z-band (right) images of LEDA 1678924 and LEDA 1678982, taken from the DeCALS survey. In each panel, a dotted ellipse represents the location of MJ0818+2257.
Paper: An Accreting Supermassive Black Hole Buried in a Faint Dwarf Galaxy
Authors: Abhishek Paswan, Mousumi Das, K Rubinur
Figure caption: The observed spectrum at the center of the outlying emission blob (i.e., MJ0818+2257) overlaid with the five SDSS filter bands, showing contaminations of emission-line features with the filter bands.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: Panel (a) and (b): [N II] and [S II] BPT diagrams of MaNGA 9885-9102. The solid and dashed black curves are the empirical maximum starburst line of G. Kauffmann et al. (2003) and L. J. Kewley et al. (2001), respectively. The dashed–dotted black line in the [S II] diagram is the boundary between Seyfert and LINER (L. J. Kewley et al. 2006). The line ratios of spaxels in the upper and lower blob are shown as blue and green small dots, respectively. The big dots with error bars are the line ratios of the total flux of each blob. The gray small dots are the line ratios of other spaxels with the S/N of Hα and Hβ both greater than 5. Gray grids are generated by the photoionization model with the MF87 (W. G. Mathews & G. J. Ferland 1987) incident spectrum, assuming log(N/O) = −1.0 (see Section 3.4). Panel (c) and (d): the observed UV flux of the two blobs compared with the UV flux predicted by the star-forming photoionization model and the diffused AGN photoionization model. The values of σ in the areas are the deviations between the model and the observed fluxes.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: Images of MaNGA 9885-9102. The first column (panel (a) and (d)) shows the maps of Hα flux and equivalent width. The second column (panel (b) and (e)) shows the maps of [O III]λ5007. The third column panel (c) and (f)) shows the images of the DESI z-band and UVOT UVW2 band. The red circles indicate the positions of the upper and lower blobs, and their sizes represent the area of the blobs.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: Left panel: the flux of Hα and the UVOT UVW2 band. Right panel: the flux of [O III]λ5007 and the UVOT UVW2 band. The blue dot is the average of the resampled pixels of the upper blob. The green dot is the average of the resampled pixels of the lower blob. The gray dots are other pixels. The semitransparent gray area represents the scatter of the relationship fitted by gray dots. The darker area is the 1σ int range, while the lighter one is the 3σ int range. The vertical dashed gray line represent the standard deviation of the background of the UVOT UVW2 band.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: The schematic diagram of two type of models for blobs. Panel (a): photoionization model from star formation. Panel (b): photoionization model from AGN.
Paper: Bipolar Blobs as Evidence of Hidden AGN Activities in the Low-mass Galaxies
Authors: Yao Yao, Enci Wang, Zhicheng He, Zheyu Lin, Yu Rong, Hong-Xin Zhang, Xu Kong
Figure caption: The gas-phase metallicity (12 + log(O/H) map of 9885-9102. (a) Derived by the O3N2 calibrator (R. A. Marino et al. 2013). (b) Derived by the N2 calibrator (R. A. Marino et al. 2013).
Paper: Revisiting the Fundamental Metallicity Relation with Observation and Simulation
Authors: Chengyu Ma, Kai Wang, Enci Wang, Yingjie Peng, Haochen Jiang, Haoran Yu, Cheng Jia, Zeyu Chen, Haixin Li, Xu Kong
Figure caption: The MZR (first column) of observed galaxies and its relation to SFR (second column), galaxy size (third column), and two quantities combined (forth column). Here three different gas-phase metallicity estimators are used (N2S2Ha, Dopita et al. 2016; Scal, Pilyugin & Grebel 2016). The red text in each panel shows the standard deviation to the fourth-order fitting curve shown in black dashed line, which is denoted as σ. One can see that σ is decreasing from the left panels to right panels. Particularly, the panels of the third column exhibit lower σ compared to those of the second panel, which indicates that galaxy size is a better predictor of the deviation in the MZR compared to SFR.
Paper: Revisiting the Fundamental Metallicity Relation with Observation and Simulation
Authors: Chengyu Ma, Kai Wang, Enci Wang, Yingjie Peng, Haochen Jiang, Haoran Yu, Cheng Jia, Zeyu Chen, Haixin Li, Xu Kong
Figure caption: The standard deviation of the residual to the fitting curves in Figure 1 for four different gas-phase metallicity estimators. This figure shows that the inclusion of the SFR only reduces σ by ≲4%, but the inclusion of R e can reduce σ by 10%−16%. Besides, including R e alone can obtain a similar performance to including both R e and SFR.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: Left: integrated intensity maps of the SO J = 87 − 76  and SO J = 56 − 45  lines. The colored ellipses on the bottom right indicate the beam sizes. Right: SO emission overlaid in contours over the 233 GHz continuum image by Tsukagoshi et al. (2019). The color contours correspond to [3, 4, 5, 6]σ. The black crosses show the peak position of knots with positional errors.
Paper: Revisiting the Fundamental Metallicity Relation with Observation and Simulation
Authors: Chengyu Ma, Kai Wang, Enci Wang, Yingjie Peng, Haochen Jiang, Haoran Yu, Cheng Jia, Zeyu Chen, Haixin Li, Xu Kong
Figure caption: The evolution of the SFR and gas-phase metallicity for 12 randomly selected star-forming galaxies as a function of lookback time in the TNG50 simulation. For clear presentation, here we show the deviation from the SFMS and the median MZR. This figure clearly shows that the SFR and the gas-phase metallicity are in anticorrelation on the temporal dimension.
Paper: Revisiting the Fundamental Metallicity Relation with Observation and Simulation
Authors: Chengyu Ma, Kai Wang, Enci Wang, Yingjie Peng, Haochen Jiang, Haoran Yu, Cheng Jia, Zeyu Chen, Haixin Li, Xu Kong
Figure caption: The scatter of the metallicity scaling relations in Figure 1 as a function of the values of α and β for the observations and TNG50. In each panel, the magenta triangles show the values of α and β when fitted individually with the other parameter sets to zero, and the blue crosses show the results when fitting jointly.
Paper: Revisiting the Fundamental Metallicity Relation with Observation and Simulation
Authors: Chengyu Ma, Kai Wang, Enci Wang, Yingjie Peng, Haochen Jiang, Haoran Yu, Cheng Jia, Zeyu Chen, Haixin Li, Xu Kong
Figure caption: The redshift evolution of best-fitting α and β in TNG50. The red circles in the upper panel show the best-fitting α when β is forced to be zero, and the magenta squares show the best-fitting β when α is forced to be zero. The blue solid lines and cyan shadow regions in both panels show the best-fitting (α, β) when both the SFR and galaxy size are used to fit the residual of the MZR.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: Matched-filter response of the SO J = 87 − 76 line with the CLEAN mask. The signal is detected with a ∼7σ significance at v LSR ∼ 7.7 km s−1.
Paper: Revisiting the Fundamental Metallicity Relation with Observation and Simulation
Authors: Chengyu Ma, Kai Wang, Enci Wang, Yingjie Peng, Haochen Jiang, Haoran Yu, Cheng Jia, Zeyu Chen, Haixin Li, Xu Kong
Figure caption: The gravitational potential vs. the M */R e for a randomly selected a sample of 100 galaxies. The blue line shows the linear fitting for the two quantities with the correlation coefficient of 0.86, indicating strong correlations between the two.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: SO J = 87 − 76 spectrum at the emission peak. The best-fitted Gaussian is also described by the gray thick line.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: Left: best-fit outflow trajectory is plotted in the orange thick line. The trajectories calculated from the parameters sampled by the posterior distribution are plotted in yellow thin lines. The background color map shows the sum of the two SNR-integrated intensity maps. The white crosses indicate the knot location used for the fitting. Right: outflow trajectories in the spatial velocity domains.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: The best-fit outflow trajectory in the three-dimensional disk coordinate is plotted in the thick red line. The dotted blue line indicates the blueshifted outflow if it exists.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: Channel maps of the SO J = 87 − 76  line (upper row) and SO J = 56 − 45  line (lower row). We normalized the intensity by the noise level. The gray dotted circles indicate the two major dust gaps at 26 and 42 au from the central star. The gray solid lines mark the hand-written CLEAN masks. The gray ellipses in the bottom-left corner show the synthetic beam sizes.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: Time evolution of the trajectories from 80 yr ago to the present time. The black dotted line and star mean the 42 au orbit and central star, respectively. The red point indicates the location of the protoplanet at that time.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: Same as the left panel of Figure 2 but without applying a CLEAN mask.
Paper: Outflow Driven by a Protoplanet Embedded in the TW Hya Disk
Authors: Tomohiro C. Yoshida, Hideko Nomura, Charles J. Law, Richard Teague, Yuhito Shibaike, Kenji Furuya, Takashi Tsukagoshi
Figure caption: Corner plot of our trajectory model fitting. Note that the values and errors in the panel title indicate the median and [16, 84]% percentiles.
Paper: Spectral Variance in a Stochastic Gravitational-wave Background from a Binary Population
Authors: William G. Lamb, Stephen R. Taylor
Figure caption: The characteristic mass ﹩{{ \mathcal M }}_{* }﹩ has a strong effect on the variance of the GWB. We use “Model 3” of SK23, but change ﹩{{ \mathcal M }}_{* }﹩ (and ﹩{\dot{n}}_{0}﹩). Left: the mean ΩGW(f) as a function of frequency for the three submodels, along with the 68% confidence interval (CI) of the GWB (shaded contours). As ﹩{{ \mathcal M }}_{* }﹩ increases, the width of the 68% CI increases. Note that the mean spectrum for ﹩\mathrm{log}{{ \mathcal M }}_{* }=9.00﹩ is outside of the 68% CI at high frequencies. Right: the variance of the GWB as a function of frequency for the three submodels. The markers are the measured variance from 107 realizations. The plotted lines are the analytically computed variance, given by Equation (11), for each model. The measured variance and analytical variance are strongly consistent.
Paper: Spectral Variance in a Stochastic Gravitational-wave Background from a Binary Population
Authors: William G. Lamb, Stephen R. Taylor
Figure caption: Gravitational-wave background from 107 realizations of a binary population described by Model 3 SK23. Left: we plot the mean and median cosmological energy density as a function of GW frequency. The blue contours represent the 68% and 95% confidence intervals of the spectra, and the orange and green lines represent the 99% confidence interval at two selected frequencies. For comparison, we also plot a ∝f 2/3 spectrum as expected from a population of circular SMBHB, inspiraling due to GW emission only. Right: the GWB distribution across 107 realizations for two selected frequencies, noted in the left plot. As frequency increases, the distribution is wider; hence the variance, skewness, and kurtosis increase.
Paper: Spectral Variance in a Stochastic Gravitational-wave Background from a Binary Population
Authors: William G. Lamb, Stephen R. Taylor
Figure caption: Comparing the mean, variance, skewness, and kurtosis of 107 realizations of the GWB as a function of GW frequency for the five models defined in SK23. The gray lines represent the general frequency scaling relation for the given statistic in the case of λ = 11/3, which are ΩGW(f) ∝ f 2/3, Var[ΩGW] ∝ f 5, Skew ∝ f 11/6, and Kurt ∝ f 11/3. For all models, we see strong agreement with the relations found in Table 1.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Top: time series RV data used in our adopted one circular planet + 1D quasiperiodic GP fit, color coded by instrument. The MAROON-X data sets are broken up between the 2020 and 2021 semesters due to interventions in the spectrograph that introduce a zero-point offset. The purple line is the model of planet b’s orbit, the teal line is the GP representing the star’s contribution to the RV signal, and the black line is the planet’s orbit combined with the GP. The light shaded areas show the GP model's 1σ and 2σ credible intervals. Bottom left: RV data phase-folded to the best-fit period of planet b. Bottom right: comparison of the best-fit semiamplitudes from the published literature (blue and red points, depicting the results from B21 and H21, respectively) and the different Pyaneti models we tested on the combined IRD + CARMENES + MAROON-X data set. Models with two planets always assume a circular orbit for planet b and then either a circular or Keplerian orbit for the outer planet. We place Gaussian priors on the outer planet candidate’s period and transit epoch using the reported planet candidate parameters from B21 and H21. All models produce consistent results for the semiamplitude of planet b, but the preferred solution according to comparisons of the AIC is a single circular planet plus a 1D quasiperiodic GP, which is depicted in green.