adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: The CHIME/FRB detection of FRB 20211229A (left) and best-fit, N = 6 model determined by fitburst. The best-fit model was optimized against raw CHIME/FRB data, though each panel shows data that are downsampled along the frequency axis to 256 channels. All parameters except for {δ = −4, ϵ = −2, τ  r  = 0 ms} were simultaneously fitted using an initial guess described in Section 4.4.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: The two-dimensional posterior probability density function (PDF, blue shading) and marginalized PDFs (blue curves in outer panels) of {DM, τ  r } for FRB 20210124B. The inner-to-outermost red contours contain 68.3%, 95.4%, and 99.5% of all probability density, respectively. In the marginalized PDF panels, the red lines denote the median value (solid) and 68.3% credible interval (dashed) derived directly from the PDF. The vertical gray lines denote the same measures but instead determined from computation of the exact-Hessian matrix as described in Appendix B. The overlap of these statistics indicates that the exact-Hessian method yields robust measures of uncertainty and covariance.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: Derived Gaussian SEDs from best-fit fitburst models of FRB 20200928B using the RPL SED, where each fit used a different value of ν  r . While all models yielded statistically consistent fits, the choice in ν  r  ultimately impacts the accuracy in translating between RPL and Gaussian parameters for reasons described in Section 5.5.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: The CHIME/FRB detection of FRB 20210124B (left), optimized scatter-broadened model determined by fitburst (middle), and the corresponding residuals (right). The best-fit model was optimized against raw CHIME/FRB data, though each panel shows data that are downsampled along the frequency axis to 256 channels. All parameters except for {δ = −4, ϵ = −2} were simultaneously fitted using an initial guess described in Section 4.3.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: Measurements of σ when using different frequency/time upsampling factors to model FRB 20200722B. Each point and uncertainty in this figure corresponds to a best-fit estimate of σ made with fitburst for a specific amount of time/frequency upsampling of input data while simultaneously optimizing all other morphological parameters, based on the method described in Section 2.4. The significant differences in σ and its statistical uncertainty indicate the presence of dispersion smearing in FRB 20200722B.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: The coherently dedispersed CHIME/Pulsar observation of PSR J2108+4504 on MJD 59438 and best-fit model determined by fitburst, whose results were first published by Andersen et al. (2023). fitburst can adequately account for wrapping of signal in rotational phase, which is important for pulsars with large duty cycle and/or significant scatter broadening as seen above.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: The CHIME/FRB detection of FRB 20230702B (left). The middle panels corresponds to residuals obtained when fitting a “full,” N = 1 fitburst model as described in Section 2. The rightmost panel shows residuals for the same data and model, but computed using the amplitude-independent modeling procedure described in Section 3.1.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: S/N for FRBs published in the first CHIME/FRB catalog, with S/N from best-fit fitburst models derived using the method discussed in Section 5.4. Over 95% of all fitburst models yield an S/N greater than the value derived by the real-time CHIME/FRB detection pipeline.
Paper: Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst 
Authors: E. Fonseca, Z. Pleunis, D. Breitman, K. R. Sand, B. Kharel, P. J. Boyle, C. Brar, U. Giri, V. M. Kaspi, K. W. Masui, B. W. Meyers, C. Patel, P. Scholz, K. Smith
Figure caption: The correlation matrix of the best-fit model for FRB 20210124B (right) presented in Figure 5.
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: Visual comparisons of the solar coronal magnetic field structure between the MAS simulation results and AI-generated during CR 2194 at 2.04, 12.63, 25.40, and 30.51 solar radii, respectively. Left column: synoptic map of the photospheric magnetic field. Middle column: the magnetic field maps from the MAS simulation model. Right column: AI-generated ones.
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: Comparisons of the solar coronal radial velocity map between the MAS simulation results and AI-generated ones on CR 2178 at 2.04, 12.63, 25.40, and 30.51 solar radii, respectively. Left column: synoptic map of the photospheric magnetic field. Middle column: the radial velocity maps from the MAS simulation model. Right column: AI-generated ones.
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: The flowchart of the Pix2PixCC model and the loss functions.
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: Comparisons of the MAS simulation results and AI-generated ones along the equator (0° latitude) during CRs 2174 and 2220 at 21.30 solar radii. The first column shows the MAS simulation results. The second column displays the corresponding AI-generated results for the magnetic field, radial velocity, and temperature, the third column shows the values of three parameters at 0° latitude of CRs 2174 and 2220, respectively, and the fourth column represents the 2D histograms.
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: Two examples of comparisons of the MAS simulation results, which include the magnetic field, radial velocity, and temperature map plus AI-generated ones of the parameters along the equator (0° latitude) on CRs 2174 and 2220 at 2.6 solar radii. Left to right: MAS simulation results, AI-generated ones, the values of the three parameters at 0° latitude of CRs 2174 and 2220, and the 2D histograms, respectively.
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: Comparisons between the MAS simulation results and AI-generated ones at a distance of 21.30 solar radii during a solar minimum period. From left to right the figure shows the MAS simulation results (left), AI-generated ones (middle), and the 2D histograms between the target and AI-generated ones (right) on CR 2224 (2019 December 10).
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: Comparisons between the MAS simulation results and AI-generated ones at 21.30 solar radii during a solar maximum period. From left to right the figure shows the MAS simulation results, AI-generated ones, and the 2D histograms between the target and AI-generated ones during CR 2170 (2015 November 28).
Paper: Near-real-time 3D Reconstruction of the Solar Coronal Parameters Based on the Magnetohydrodynamic Algorithm outside a Sphere Using Deep Learning
Authors: Sumiaya Rahman, Hyun-Jin Jeong, Ashraf Siddique, Yong-Jae Moon, Bendict Lawrance
Figure caption: Comparison of solar coronal temperature maps between the MAS simulation results and AI-generated ones during CR 2220. Each column is the same as in Figures 2 and 3.
Paper: Jet Mechanism and γ-Ray-emitting Region for Fermi Flat-spectrum Radio Quasars with Broad-line Emissions
Authors: Lixia Zhang, Xiaobiao Chen, Shihui He, Wenwen Nie, Wentao Tang, Jiawei Huang, Guohai Chen, Junhui Fan
Figure caption: In the left panel, the black hole mass (﹩\mathrm{log}{(M/{M}_{\odot })}_{\mathrm{con}}﹩) is calculated by the traditional virial technique with continuum luminosity. In the right panel, the black hole mass (﹩\mathrm{log}{(M/{M}_{\odot })}_{\mathrm{BLR}}﹩) is calculated solely by emission-line parameters. The maximal jet power as a function of the black hole mass. The blue-dashed line is the maximal jet power ﹩{P}_{\mathrm{jet}}^{\mathrm{BZ}}﹩ extracted from a rapidly spinning black hole. The green-dashed line is the maximal jet power ﹩{P}_{\mathrm{jet}}^{\mathrm{BP}}﹩ extracted from the accretion disk. The red-dashed line is the maximal jet power ﹩{P}_{\mathrm{jet}}^{\mathrm{Hybrid}}﹩ in the hybrid model. Solid blue circles: LSP FSRQs; Solid black squares: ISP FSRQs; solid red star: HSP FSRQ; solid orange circles: LSP FSRQs from C24; solid orange squares: ISP FSRQs from C24.
Paper: Jet Mechanism and γ-Ray-emitting Region for Fermi Flat-spectrum Radio Quasars with Broad-line Emissions
Authors: Lixia Zhang, Xiaobiao Chen, Shihui He, Wenwen Nie, Wentao Tang, Jiawei Huang, Guohai Chen, Junhui Fan
Figure caption: Left panel: distribution of the γ-ray dissipation region R  γ : the green-dashed histogram is for the R em from Fan et al. (2023), the blue-dashed histogram is for the minimum R  γ , the red-dashed histogram is for the maximum R  γ . Right panel: Location of γ-ray dissipation region R  γ  from the central black hole as a function of the disk luminosity: the blue circles are minimum ﹩\mathrm{log}{R}_{\gamma }﹩, the red circles are maximum ﹩\mathrm{log}{R}_{\gamma }﹩, and the black circles are the ﹩\mathrm{log}{R}_{\mathrm{em}}﹩, the solid blue line and solid red line represent the BLR distance (﹩\mathrm{log}{R}_{\mathrm{BLR}}﹩) and the DT distance (﹩\mathrm{log}{R}_{\mathrm{DT}}﹩).
Paper: Jet Mechanism and γ-Ray-emitting Region for Fermi Flat-spectrum Radio Quasars with Broad-line Emissions
Authors: Lixia Zhang, Xiaobiao Chen, Shihui He, Wenwen Nie, Wentao Tang, Jiawei Huang, Guohai Chen, Junhui Fan
Figure caption: The distributions of physical parameters: (a) the peak Lorentz factor; (b) the Doppler factor; (c) the magnetic field strength in units of gauss; (d) the radius of the emission region in units of centimeters; (e) the normalization for electron energy distribution; (f) the external photon energy density; (g) the power in the form of Poynting flux in units of ergs per second; (h) the power in the form of electrons in units of ergs per second; (i) the power in the form of protons in units of ergs per second; (j) the power in the form of radiation in units of ergs per second; (k) the total jet power in units of ergs per second.
Paper: Jet Mechanism and γ-Ray-emitting Region for Fermi Flat-spectrum Radio Quasars with Broad-line Emissions
Authors: Lixia Zhang, Xiaobiao Chen, Shihui He, Wenwen Nie, Wentao Tang, Jiawei Huang, Guohai Chen, Junhui Fan
Figure caption: The optical spectra from LAMOST of 4FGL J0018.8+2611 (left) and 4FGL J0112.8+3208 (right), which are modeled with PyQSOFit. The black line shows the original spectral data, the orange line models the continuum, and the cyan line plots the optical and UV Fe II templates, as shown in the main graph. The red and green lines represent the broad and narrow components of the emission line, and the blue line is the sum of all the emission components, the Gaussian fitting of the emission lines of O II, Hβ, and Hα are shown in the corresponding three subgraphs.
Paper: Jet Mechanism and γ-Ray-emitting Region for Fermi Flat-spectrum Radio Quasars with Broad-line Emissions
Authors: Lixia Zhang, Xiaobiao Chen, Shihui He, Wenwen Nie, Wentao Tang, Jiawei Huang, Guohai Chen, Junhui Fan
Figure caption: The IC peak luminosity as a function of the synchrotron peak luminosity, the solid blue circles are LSP FSRQs, the solid black squares are ISP FSRQs, and one solid red star is the HSP FSRQ. The green-dashed line is a linear fit to the ﹩\mathrm{log}L({\nu }_{\mathrm{IC}}^{{\rm{p}}})﹩ vs. ﹩\mathrm{log}L({\nu }_{\mathrm{sy}}^{{\rm{p}}})﹩ for the whole sample with the fit parameters.
Paper: Image Synthesis for Solar Flare Prediction
Authors: Elad Amar, Ohad Ben-Shahar
Figure caption: Comparison of the F1-score and the TSS as a function of the number of synthetic images used. Both metrics exhibit higher values when using the optimized synthetic images.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Left: the results of our work (red shapes) relative to noncontroversial planets listed on the NASA Exoplanet Archive (accessed 2023 November 26) with precisely measured radii, orbital periods, and masses greater than 0.1 M J. The red points occupy a scarcely populated region at long orbital periods. Right: the results of our work (red shapes) relative to noncontroversial planets listed on the NASA Exoplanet Archive (accessed 2023 November 26) with precisely measured radii and masses, and with orbital periods greater than 50 days. Masses have been restricted to greater than 0.1 M J. Most of the planets characterized here fall in line with the broad trend of increasing radius with mass until degeneracy pressure dominates in the core of the giant planet. However, Kepler-111 c and Kepler-849 b appear to be overly dense and possibly identify a new category of heavy metal Jovian planets.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Lomb–Scargle periodograms of the RVs of all systems except for TOI-2180. The red lines identify the periodicity of the transiting giant planet in each of these systems, excluding KIC 5951458, which we argue is spurious. The black triangles show the period with the maximum power in the periodogram. For each of the systems for which we make new mass measurements, these periodicities align.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: RVs and best-fit model for TOI-2180. The Keplerlian signal for TOI-2180 b is shown in panel (c). The orbit of the outer companion that was initially identified by Dalba et al. (2022a) is nearly resolved (panel (d)). The minimum mass of the outer companion is within the planetary regime.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: RVs and best-fit model for KIC 5951458. Only the final RV is new to this paper. The Keplerian signal is consistent with the conjunction time of the single transit observed by Kepler. We conclude that KIC 5951458 b is actually an M dwarf companion.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Posterior probability distributions resulting from the bulk metallicity estimation described in Section 3.3 for Kepler-111 c (top left), Kepler-553 c (top right), Kepler-849 b (bottom left), and PH-2 b (bottom right). Convergence of the model is achieved in all cases, and high precision is achieved on all of the Z  P  values owing to relatively tight constraints on stellar age produced by the EXOFASTv2 fits.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Transits and model of TOI-2180 b, including various cadences as observed by TESS. Each transit is shown to demonstrate the convergence of the TTV model. In the rightmost column, all data have been folded on the maximum likelihood transit ephemeris.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: RVs and best-fit model for Kepler-1513. The red points are bins of 0.08 in phase. Only a weak signal at the ephemeris of the transiting planet is detected, and it relies on a high eccentricity, which may be artificial. Therefore, only an upper limit on planet mass is reported here.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Lomb–Scargle periodogram of the residuals between the TOI-2180 RVs and the best-fit model. No significant periodicity is detected. The dashed line denotes a false alarm probability of 1%.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. IV. Long-term Doppler Spectroscopy for 11 Stars Thought to Host Cool Giant Exoplanets
Authors: Paul A. Dalba, Stephen R. Kane, Howard Isaacson, Benjamin Fulton, Andrew W. Howard, Edward W. Schwieterman, Daniel P. Thorngren, Jonathan Fortney, Noah Vowell, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Molly Kosiarek, Jack Lubin, Andrew W. Mayo, Teo Močnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Diana Dragomir, David Kipping, Matthew J. Payne, Arpita Roy, Alex Teachey, Steven Villanueva
Figure caption: Transit-timing variations for TOI-2180 b.