adsabs/AstroCLIMB huggingface dataset:
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption: Hubble diagram residual (left) and residual histogram (right) in B band for 36 91T/99aa-like SNe Ia (in filled circles) and 87 normal SNe Ia (in open circles) when assuming these two groups have different intrinsic scatters (0.28 mag for 91T/99aa-like, and 0.05 mag for normal SNe Ia). Left: the weighted mean Hubble residuals for 91T-like SNe Ia and normal SNe Ia are 0.03 mag and −0.18 mag, which are also plotted as horizontal lines on the plot (solid line for 91T-like SNe, dashed–dotted line for normal SNe Ia). The dashed line denotes the peculiar velocity effect with v pec = 300 km s−1. Right: Distribution of Hubble residuals. The Gaussian ideograms of each group are also plotted (solid line for 91T/99aa-like, dashed–dotted line for normal SNe Ia). The peak of resulting Gaussian ideograms are 0.01 mag and −0.17 mag for normal SNe Ia and 91T/99aa-like SNe Ia, respectively.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption: Spectra within 2 days of (a) −13 days, (b) −8 days, (c) −4 days, (d) 0 days, and (e) +6 days of our 91T/99aa-like sample. The Si II 6355 ± 5 Å around maximum increases from top to bottom for each panel. SN 1991T, SN 1999aa, and the typical normal Type Ia SN 2004eo are plotted in bold. 91T/99aa-like objects with Δm 15(B) > 1.0 mag are plotted in red. And normal objects in our sample with Δm 15(B) < 0.8 mag are also plotted in dashed gray lines. A vertical gray line at 6150 Å is also plotted to guide the eye.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption: Left: Hubble residual vs. Δm 15(B). Right: Δm 15(B) vs. ﹩{{pEW}}_{{\rm{\max }}}﹩(Si II λλ6355). Open circles indicate objects with zCMB<0.01.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption: Left: histogram of Δm 15 in the B band. Right: histogram of absolute magnitudes at maximum in the B band assuming a constant R  B  = 3.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption:  B-band light curves and fits of normal SNe Ia (in black circles) with Δm 15(B) < 0.8 mag and 91T/99aa-like SNe (in red triangles) with Δm 15(B) > 1.0 mag. Δm 15(B) values are labeled next to each light curve.
Paper: Using 1991T/1999aa-like Type Ia Supernovae as Standardizable Candles
Authors: Jiawen Yang, Lifan Wang, Nicholas Suntzeff, Lei Hu, Lauren Aldoroty, Peter J. Brown, Kevin Krisciunas, Iair Arcavi, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Craig Pellegrino, Stefano Valenti
Figure caption:  B- and V-band light curves for the SNe used in this paper. The light curves have been shifted vertically for better visualization. The gray data points are normal SNe Ia, while the data points of 91T/99aa-like SNe Ia are color-coded by Δm 15(B).
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: A scatter plot of the injected period vs. the recovered period for one CFHT light curve. Each point represents the result of one Kepler (or synthetic) light curve being added to this cluster member’s light curve. Low-amplitude injections are dominated by the existing signal in the data, resulting in the horizontal features on this diagram. Dashed lines represent the 1:1 line for successful recoveries and the most prominent window function effects: half-period aliasing and the Month and Year window peaks (see Section 5.1 for detailed discussion). Additional peaks in the window function align with other trends in this figure but are not plotted to reduce figure crowding (e.g., m = 1, n = ±1, and δ P ∼ 180 would fall between the plotted year-based effect and the 1:1 line).
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: Left panel: the percentage of the time we find a significant (FAP <0.01) rotation signal but the period does not match what we injected into a cluster member’s light curve (to within 10%). Right panel: same as the left panel, but for injections into a field star instead of a cluster member. Many of these light curves, especially those of the cluster members, already have periodic signals in them. Thus, in the case of a low-amplitude injection we often recover what already existed in the data. Since this does not match what was injected, this is marked as a “false positive.” In both panels bins with a white box drawn around them are the ones where over half (i.e., ≥25) of the injected signals are Kepler light curves.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: Top left panel: a replication of the first panel of Figure 7 of Curtis et al. (2020), but with our results and the results of Barnes et al. (2016) added. Top right panel: a subset of the top left panel, zoomed in on the T eff range of the results presented in this paper. Bottom left panel: Same as the top left panel, but now plotted over a 2D histogram of field star rotation periods. Bottom right panel: same as the top right panel, but now plotted over field star rotation periods. In all cases, the colored points are a collection of open clusters that have been used as gyrochronological benchmarks. Benchmarks include the Pleiades (120 Myr; Rebull et al. 2016), Praesepe (670 Myr; Douglas et al. 2017, 2019), NGC 6811 (1 Gyr; Curtis et al. 2019), NGC 752 (1.4 Gyr; Agüeros et al. 2018), NGC 6819/Ruprecht 147 (2.5 Gyr projected forward by Curtis et al./2.7 Gyr; Meibom et al. 2015; Curtis et al. 2020), M67 (4 Gyr; Barnes et al. 2016; this work), and three field stars: α Cen B and 61 Cyg A and B (Table 3 of Curtis et al. 2020, and references therein). Field stars are taken from a collection of literature sources: Kepler (Santos et al. 2019), the PS1 Medium Deep Survey (Kado-Fong et al. 2016), MEarth (Newton et al. 2016, 2018), CARMENES (Díez Alonso et al. 2019), Evryscope (Howard et al. 2020), and the K2SDSS sample (Popinchalk et al. 2021).
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: Left panel: recovered rotation periods for members of the open cluster M67 plotted vs. their color-derived effective temperatures. All points have a low FAP (<1%) for the detected rotation period. Right panel: we fit a polynomial to the sequence by iterative outlier rejection. The larger points are used in the polynomial fit after outlier rejection. The shaded region is the confidence interval of this fit. Red squares are the median values of the data binned in T eff, and the red line is a polynomial fit to these values.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: The rotation period vs. effective temperature of M67 members with our fit to the M67 sequence (solid black). Dashed lines are the result of assuming that our fit to the sequence is the true period in Equation (9), along with m = 1 and n = ± 1. Dotted lines are the same, but with n = ± 2. Left panel: using 29.5 days for δ P Equation (9). Right panel: using 380.8 days for δ P Equation (9). Additionally, the half-period alias of Equation (7) is in solid blue.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: Left panel: the selected subset (from iterative outlier rejection; Section 5) of M67 rotation periods vs. their effective temperatures. The shaded region in gray is the confidence interval of the fit, plotted as a dotted black line. Predictions for the sequence from the empirical models are plotted as colored lines. Right panel: same as the left panel, but with predictions from the theoretical models.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: Mean vertical wavenumber spectra of normalized temperature perturbations divided by N4 at different latitude bins, in the altitude range of 160–200 km (upper panels) and 180–220 km (bottom panels) during northern ((a) and (c)) spring (Ls = 0°–90°) and ((b) and ((d)) summer (Ls = 90°–180°) in MY35. The theoretical spectrum of saturated GWs given by a dashed black line. The different color lines correspond to their respective latitude ranges.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: Mean vertical wavenumber spectra of normalized temperature perturbations divided by N4 in MY33, for the altitude range of 160–200 km, panels (a)–(b), and 180–220 km, panels (c)–(d), as in Figure 4.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: The spatiotemporal coverage of NGIMS data during solar longitudes L s  = 0–180° (northern spring: L s  = 0–90°; northern summer: L s  = 90°–180°). Top to bottom, the panels are MY33 and MY35, respectively. The coverage is shown as a function of (a) altitude and latitude, (b) latitude and longitude, (c) latitude and local time, and (d) latitude and solar longitude. The data coverage in MY35 is shown in the same format in panels (e)–(h).
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: The altitude profiles of (a) CO2 density, (b) estimated temperature (black) and the seventh-order polynomial fit to the data (red), (c) normalized temperature perturbations, and (d) Brunt–Väisälä frequency observed on orbit 1060 in MY33. Panels (e)–(h) are the same, but for orbit 2101 in MY35.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: (a) Time series of sunspot numbers (Sn) for the last 13 yr, with the solid orange line representing the daily average and the blue and red lines indicating the monthly average and monthly smooth average, respectively. (b) Monthly sunspot number (Sn) as a function of solar longitude, with different colored dotted lines indicating the corresponding Martian years.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: Mean vertical wavenumber spectra of normalized temperature perturbations divided by N4 at different longitude bins, in the altitude range of 160–200 km (upper panels) and 180–220 km (bottom panels) in MY35.
Paper: Accelerated Bayesian SED Modeling Using Amortized Neural Posterior Estimation
Authors: ChangHoon Hahn, Peter Melchior
Figure caption: A comparison of the posteriors of the 12 SED model parameters derived from standard MCMC sampling (black) and our SEDFLOW (blue) for an arbitrarily selected NSA galaxy (NSAID = 26; red in Figure 1). The posteriors are in excellent agreement for all of the SED parameters. In the bottom panel, we present the SEDs of the best-fit parameter values from SEDFLOW (blue lines) and the MCMC posteriors (black dotted lines), which are both in good agreement with the observed NSA photometric flux (red dots). Estimating the posterior using MCMC sampling requires ∼10 CPU hr. Even using neural emulators to accelerate the likelihood evaluations, MCMC sampling requires ∼10 CPU minutes. With SEDFLOW, inferring the full posterior takes 1 s per galaxy.
Paper: Accelerated Bayesian SED Modeling Using Amortized Neural Posterior Estimation
Authors: ChangHoon Hahn, Peter Melchior
Figure caption: The distributions of the photometric magnitudes, uncertainties, and redshifts of the NSA galaxies for which SEDFLOW does not produce valid posteriors (blue or orange). These galaxies lie outside the support of the SEDFLOW training data (black), so SEDFLOW cannot accurately estimate their posteriors. We mark the NSA galaxies that have unusually high photometric uncertainties that are not accounted for in our noise model in orange and the galaxies that have photometric colors that cannot be modeled by our SED model in blue.
Paper: Accelerated Bayesian SED Modeling Using Amortized Neural Posterior Estimation
Authors: ChangHoon Hahn, Peter Melchior
Figure caption: SBC plot of the SEDFLOW posteriors for 1000 synthetic test observations. The histograms in each panel represent the distributions of the rank statistics of the true values within the marginalized SEDFLOW posteriors (blue lines) for each SED parameter. For the true posteriors, the rank statistics will have a uniform distribution (black dashed lines). For reference, we include the rank distributions of the MCMC posteriors for a subset of 100 test data (gray dotted lines). The rank statistic distributions of SEDFLOW are nearly uniform for all of the SED parameters. Therefore, SEDFLOW provides unbiased and accurate estimates of the true posteriors.
Paper: Accelerated Bayesian SED Modeling Using Amortized Neural Posterior Estimation
Authors: ChangHoon Hahn, Peter Melchior
Figure caption: P–P plot of the SEDFLOW posteriors for 1000 synthetic test observations, with the known true parameter values. We plot the CDFs of the percentile scores of the true values within the marginalized SEDFLOW posteriors for each SED parameter. For the true posteriors, the percentile scores are uniformly distributed, so the CDF is diagonal (black dashed line). For reference, we include the P–P plot of the posteriors estimated from the MCMC sampling (gray dotted lines). The SEDFLOW posteriors are in excellent agreement with the true posteriors.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Variations of Pearson’s CC between the averaged and shifted H fluxes at different energies (written in the middle column) and the averaged SSN with respect to the averaging window during SC23 (left) and SC24 (right) are shown. The fluxes are shifted based on the calculated lags with respect to the SSN variation. The green dots are Pearson’s CCs when there is no cutoff on the fluxes (as shown in Figure 3 in the main text). The red, black, pink, and blue dots represent Pearson’s CCs obtained in the similar way after putting cutoffs on the fluxes. The threshold values of the fluxes in units of particles/(cm2-s-sr-MeV/n) are written above each subplot.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Variations of the lags between the averaged fluxes and SSN with respect to the averaging window. Panels (a), (c), (e), (g), (i), and (k) show the variations of the lags for H, 4He, 3He, Fe, C, and O, respectively, during SC23. Panels (b), (d), (f), (h), (j), and (l) represent the same during SC24. Energy channels corresponding to H, 4He, and 3He are written on the left side of the left column of the figure. The same corresponding to Fe, C, and O are mentioned on the right of the right column of the figure.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Plots of two year “quiet” time averaged differential directional flux vs. energy for the six elements under consideration. The spectral slopes (m  i ) of the fitted lines for different phases of SC23 and SC24 are also shown in different colors. The MoEs of the spectral index estimations within 95% confidence bounds are written on the left for H, 4He, and 3He and on the right for C, O, and Fe.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Variations of spectral indices of (a) H and (b) 3He and comparative variations of (c) C (red) and O (black) and (d) 4He (red) and Fe (black) with respect to the different phases of the solar cycles starting from the maximum of SC23 up to the minimum of SC24–25. The MoEs corresponding to the 95% confidence interval, in estimating the spectral indices as shown in Figure 6, are set as error bars.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Variations of Pearson’s CC between the averaged and shifted 4He fluxes at different energies (written in the middle column) and the averaged SSN with respect to the averaging window during SC23 (left) and SC24 (right) are shown. The fluxes are shifted based on the calculated lags with respect to the SSN variation. The green dots are Pearson’s CCs when there is no cutoff on the fluxes (as shown in Figure 3 in the main text). The red, black, pink, and blue dots represent Pearson’s CCs obtained in the similar way after putting cutoffs on the fluxes. Threshold values of the fluxes in units of particles/(cm2-s-sr-MeV/n) are written on the left and right of each pair of subplots corresponding to SC23 and SC24, respectively.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar to Figure A5 but for Fe.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar to Figure A2 but for 3He.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar to Figure A4 but for O.
Paper: Differential Behaviors of Suprathermal 4He and Fe Populations in the Interplanetary Medium during Solar Cycle 24
Authors: Bijoy Dalal, D. Chakrabarty, N. Srivastava
Figure caption: Similar to Figure A3 but for C.
Paper: Phase Mixing and the 1/f Spectrum in the Solar Wind
Authors: Norbert Magyar, Tom Van Doorsselaere
Figure caption: 2D noise maps used to generate the transverse density inhomogeneity for the numerical analysis. For the surface Alfvén wave setup, the maximum density is reduced to two in each plot. Left: pink noise (﹩f({k}_{\perp })\sim {k}_{\perp }^{-1}﹩). Center: Kolmogorov noise (﹩f({k}_{\perp })\sim {k}_{\perp }^{-5/3}﹩). Right:  Brownian noise (﹩f({k}_{\perp })\sim {k}_{\perp }^{-2}﹩).
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: The coverage of emission from an exoplanet to Earth (top) and the simplified case for extremely small angle between the line-of-sight direction and the direction of emission (bottom). The area filled with yellow is the location range where an observer on Earth can detect signals from the exoplanet.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: Left: extraterrestrial signal received by a pair of telescopes pointing at the same direction ﹩\hat{s}﹩. The baseline vector  b  points from the jth telescope to the ith telescope. Right: frequency drifts of the signal received by the two telescopes. The different locations of two telescopes cause the geometric delay of the signal.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: Eccentric anomaly is one of the angular parameters defined by a planet orbiting a central star along an elliptic Kepler orbit.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: Pseudosinusoidal relative frequency curves of long-term observations for TRAPPIST-1g, Kepler-438 b, and Proxima Centauri b.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: Conversion between latitude and polar angle.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: The motion of an object on a rotating planet and the simplified case.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: A certain point in a spherical coordinate system, rotating at an angular velocity ω.
Paper: Drift Rates of Narrowband Signals in Long-term SETI Observations for Exoplanets
Authors: Jian-Kang Li, Hai-Chen Zhao, Zhen-Zhao Tao, Tong-Jie Zhang, Sun Xiao-Hui
Figure caption: The orbit of a planet around its host star in a polar coordinate system.
Paper: MEGASIM: Lifetimes and Resonances of Earth Trojan Asteroids—The Death of Primordial ETAs?
Authors: Travis Yeager, Nathan Golovich
Figure caption: Binned ETA ejections over time for the two simulations. Bin widths are 100 kyr. The top panel shows the IAS15 simulation, which was only integrated for 50 Myr. The bottom panel shows the first 50 Myr of the WHfast simulation for comparison.