adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Same as Figure 7, but for the KeplerCam and LCO data from 2020 February 17 and 2021 November 13, respectively.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Calculated CCF of the IRD spectrum of TOI-1696 taken on 2021 January 30 at the orbital phase 0.247, to the template spectrum of GJ699, exhibiting a single peak with width 9.2 k m s−1. The dashed line shows the autocorrelation function of the GJ699 spectrum as a reference.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Posteriors of the planet-to-star radius ratio (R  P /R ⋆) in each bandpass (left) and impact parameter (right) from the joint fit to the TESS data and the ground-based data shown in Figures 7, 8, and 9; the gray shaded region in the right panel represents the uniform prior used in the fit, while the blue histogram is the posterior.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Phase-folded RVs with Keplerian models corresponding to the 1σ, 2σ, and 3σ mass upper limits. The gray points with the error bars show the errors estimated from the data-processing method described in Section 2.8. The error bars in orange show the original errors + jitter term value of 62 m s−1 (added in quadrature) from the best-fit RV model (orange line, best M  p  = 12.3M ⊕).
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Same as Figure 7, but for the MuSCAT (M1) data from 2021 July 28.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Planetary equilibrium temperature vs. radius for TOI-1696 b and other planets with Rp < 10R ⊕, with the host stars having T eff < 3800K and H < 11mag. The point size represents the calculated TSM values. Data points with a planet name beside them are those with a higher TSM values than the target.
Paper: TOI-1696: A Nearby M4 Dwarf with a 3 R ⊕ Planet in the Neptunian Desert
Authors: Mayuko Mori, John H. Livingston, Jerome de Leon, Norio Narita, Teruyuki Hirano, Akihiko Fukui, Karen A. Collins, Naho Fujita, Yasunori Hori, Hiroyuki Tako Ishikawa, Kiyoe Kawauchi, Keivan G. Stassun, Noriharu Watanabe, Steven Giacalone, Rebecca Gore, Ashley Schroeder, Courtney D. Dressing, Allyson Bieryla, Eric L. N. Jensen, Bob Massey, Avi Shporer, Masayuki Kuzuhara, David Charbonneau, David R. Ciardi, John P. Doty, Emma Esparza-Borges, Hiroki Harakawa, Klaus Hodapp, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Jon M. Jenkins, Taiki Kagetani, Tadahiro Kimura, Takanori Kodama, Takayuki Kotani, Vigneshwaran Krishnamurthy, Tomoyuki Kudo, Seiya Kurita, Takashi Kurokawa, Nobuhiko Kusakabe, David W. Latham, Brian McLean, Felipe Murgas, Jun Nishikawa, Taku Nishiumi, Masashi Omiya, Hugh P. Osborn, Enric Palle, Hannu Parviainen, George R. Ricker, Sara Seager, Takuma Serizawa, Huan-Yu Teng, Yuka Terada, Joseph D. Twicken, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn, Yujie Zou, Motohide Tamura
Figure caption: Phase-folded TESS light curve after removing the best-fit GP noise model, with the best-fit transit model (blue) from our joint analysis of the TESS and ground-based light curves.
Paper: Uncertainty in Grain Size Estimations of Volatiles on Trans-Neptunian Objects and Kuiper Belt Objects
Authors: A. Emran, V. F. Chevrier
Figure caption: Grain sizes determined from the Hapke slab (left column) and ISM (right column) using spectra calculated using the Mie model at different particle radii of 1, 10, 100, 1000 μm for pure CH4 ice at 39 K (top row), α-N2:CH4 at 35 K (middle row), and β-N2:CH4 at 38 K (bottom row). The resulting grain sizes are normalized to the input grain sizes. The plots were smoothened using the Savitzky–Golay filter (Savitzky & Golay 1964).
Paper: Uncertainty in Grain Size Estimations of Volatiles on Trans-Neptunian Objects and Kuiper Belt Objects
Authors: A. Emran, V. F. Chevrier
Figure caption: Plot of the single scattering albedo against absorption coefficient for pure CH4 ice particle at 39 K (left column), α -N2:CH4 particle at 35 K (middle column), and β -N2:CH4 particle at 38 K (right column). The subplots show the distribution of w at grain radii at 1 μm (upper row), 10 μm (2nd row), 100 μm (3rd row), and 1000 μm (bottom row). In all subplots, the scattering albedo from the Mie calculation (blue), ISM (yellow), and Hapke slab (green). The Mie calculation follows two different paths due to the Rayleigh scattering effect at lower grain-size particles.
Paper: Uncertainty in Grain Size Estimations of Volatiles on Trans-Neptunian Objects and Kuiper Belt Objects
Authors: A. Emran, V. F. Chevrier
Figure caption: Absorption coefficient of pure CH4 ice at 39 K (a), CH4 saturated with α-N2 ice at 35 K (b), and CH4 saturated with β- N2 ice at 38 K (c). Pure CH4 has an absorption coefficient peak at 3.3 μm. The absorption coefficient is much higher over the wavelength around 3.3 μm at 38 K compared to 35 K for CH4 saturated with N2 ices.
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Left: combined absolute magnitude distribution for the L4 swarm of the known Trojan asteroids taken from the MPC catalog (green squares) and those from the HSC observation by Yoshida & Terai (2017, green circles) scaled at H  V  = 14.0 mag. The V − r color was assumed to be 0.25 mag (Szabó et al. 2007) in converting the HSC r-band magnitudes into the V-band magnitudes. Corresponding diameters for the assumed albedo of 0.05 (Romanishin & Tegler 2018) are also shown at the upper horizontal axis. Note that Yoshida & Terai (2017) assumed an albedo of 0.07 based on Grav et al. (2012), while we used 0.05 for both swarms based on the above more recent work. Right: same as the left panel but for the L5 swarm. The HSC data (red circles) in this case are those obtained by the present work, and are scaled so that their best-fit single-slope power-law distribution (dashed line; see also Figure 6) matches the MPC data (magenta squares) at H  V  = 14.0 mag (see text).
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Cumulative absolute magnitude distribution for the 87 unbiased L5 Jupiter Trojans obtained from our survey (red dots with error bars). Note that the cumulative numbers are corrected using the detection efficiency as shown in Equation (9). Corresponding diameters for the assumed albedo of 0.05 (Romanishin & Tegler 2018) are also shown at the upper horizontal axis. Best-fit single-slope power-law distribution is shown with the dashed line.
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Left: the relationship between the true generated heliocentric distances of synthetic Trojans and the values of the heliocentric distance estimated from their apparent motion under the same observation conditions as our survey. The systematic deviation between the two values is due to the assumption of circular orbits in the estimation from apparent motions. The solid line represents the best fit to the estimated values given by Equation (1). Right: the relationship between the generated heliocentric distances and reestimated values. The latter was obtained by removing the systematic deviation using Equation (1).
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Absolute magnitudes with error bars as a function of heliocentric distance for the 187 Trojan asteroids for which photometric measurements were successfully performed. The dashed lines shows the limiting apparent magnitude of 24.1 mag. The solid lines represent the boundaries we set to select our unbiased sample, i.e., R = 5.5 au and H  r  = 17.0.
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Distribution of apparent velocities of detected Jupiter Trojans (red dots) and Hildas (green dots) along ecliptic longitude and latitude. The background map shows the distribution of apparent velocities of synthetic Trojans and Hildas, respectively, generated by a Monte Carlo method based on the orbital distribution of known asteroids in each population. The three dashed lines show boundaries used to distinguish detected objects for each population.
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Postevent distribution of sampling by MCMC for our unbiased L5 Jupiter Trojans. The red solid lines in the one-dimensional histograms show the best-fit values, and the orange dashed lines represent the resulting confidence intervals. Each blue point in the two-dimensional histograms and the contours show the results of sampling for each step and their distributions, respectively.
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Combined absolute magnitude distribution for the L4 (squares) and L5 (circles) swarms normalized by their values at H  V  = 17.0 mag.
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Relationship between the derived heliocentric distances and orbital inclinations together with their histograms for the detected 189 Trojan asteroids. Random errors for the obtained heliocentric distances and orbital inclinations are 0.18 au and 1.°5, respectively.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Comparison between phase (top row) and amplitude variations (bottom row) in HAT-P-7 b’s phase curve when we detrend the data using a basis spline with different knot spacings. The dashed gray diagonal lines in each plot show a one-to-one slope, while the solid black line shows the slope from a fit accommodating the error bars in both axes. The fitted slope and uncertainty appears on the top left of each plot. For aggressive splines with knot spacings shorter than the duration of one HAT-P-7 b orbit (left column), the phase-curve amplitude was significantly attenuated, and the resulting small signal resulted in highly uncertain measurements of the phase of peak brightness. Knot spacings greater than or equal to one planet orbit (right column) generally were consistent. We chose to use a spacing of one knot per orbit for our analysis to give our spline the most flexibility possible without attenuating the signal.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Comparison between phase (top row) and amplitude (bottom row) variations for the sine at the planet’s orbital period for our baseline model with three sinusoids compared with models including only one one (left column) or two (right column) sinusoids in the phase-curve model. We note that all of the measurements plotted show the phase (ϕ) and amplitude (a) of the sine at the planet’s orbital period—the only differences between the measurements are the number of additional sinusoid terms in the model. The dashed gray diagonal lines in each plot show a one-to-one slope, while the solid black line shows the slope from a fit accommodating the error bars in both axes. The fitted slope and uncertainty appears on the top left of each plot. The inclusion of more harmonics in our model did not cause significant change in our results for the phase and amplitude of the sine at the planet’s orbital period. In order to maintain consistency with the methods of Armstrong et al. (2016), we used a model including three sinusoids for our analysis.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Measurements of the phase (top) and amplitude (bottom) of HAT-P-7 b’s phase curve over time. The vertical dotted lines show where the Kepler light curve is broken into quarters. The reduced χ 2, or χ 2 per degree of freedom, is shown in the upper left of each plot. Although there are no clear patterns in the time evolution of the phase and amplitude of HAT-P-7 b’s phase curve, we find that there may be statistically significant variability based on a χ 2 test.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Phase (left) and amplitude (right) variations resulting from flattening the Kepler light curve using the Sanchis-Ojeda et al. (2013)-inspired filtering vs. the basis-spline method. The dashed gray diagonal lines in each plot show a one-to-one slope, while the solid black line shows the slope from a fit accommodating the error bars in both axes. The fitted slope and uncertainty appears on the top left of each plot. Both methods yield consistent measurements of the phase-curve amplitude, but the Sanchis-Ojeda et al. (2013)-inspired filtering results in smaller variations in the planet’s orbital phase. It is unclear whether the smaller phase variations from the Sanchis-Ojeda et al. (2013)-inspired method are due to better removal of systematic trends or attenuation of real phase variations, so to avoid removing potentially real variability we chose to use a basis spline to detrend the Kepler data for our analysis.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Comparison between phase-offset variations (left) and amplitude variations (right) resulting from the use of Kepler data processed via Simple Aperature Photometry (SAP) vs. Pre-search Conditioning Simple Aperature Photometry (PDCSAP). The dashed gray diagonal lines in both panels show a one-to-one slope, while the solid black line shows the slope from a fit accommodating the error bars in both axes. The fitted slope and uncertainty appears on the top left of each plot. Our analysis shows some minor systematic differences between phases and amplitudes we measure from SAP and PDCSAP data, but qualitatively, the results are similar. We chose to use PDCSAP data for our analysis, to ensure that our result did not depend on possible systematics present in the SAP data.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Overview of our analysis. Top: the full Kepler light curve of HAT-P-7, split into 60 consecutive bins of 10 orbits of HAT-P-7 b, each shown as a different color/stripe. The transits of HAT-P-7 b are so frequent that they blend together in this panel. Middle: close-up view of about 70 days of Kepler data. In this panel, the transits of HAT-P-7 b appear as a regular comb of dips (except for gaps in Kepler’s observations). Bottom: an example planetary phase curve, shown alongside a schematic showing the relative position of the star and planet at several points in the orbit. We analyze each segment of 10 planet orbits (shown as different colors in the top two panels) to model a phase curve similar to that shown here.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: An example phase-curve fit. The green points show about 10 phase-folded orbits of Kepler data (excluding the transit and secondary eclipses), while the blue lines show the models corresponding to 100 draws from our MCMC posterior probability distributions of our sinusoidal model fit to the data. We perform a similar fit every 10 orbits observed by Kepler to detect any variations in the phase curve over time.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The five statistics to characterize the radius valley morphology (i.e., C valley, A valley, ﹩{R}_{\mathrm{valley}}^{+}﹩, ﹩{R}_{\mathrm{valley}}^{-}﹩, and f NP) as functions of kinematic age t (Gyr). In Section 4.1, we rescale the planet radii to eliminate the influence of stellar mass and planetary orbital period on the boundary of radius valley. The results with rescaling radii are plotted as open circles and shifted to the right to avoid overlapping.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The five statistics to characterize the radius valley morphology (i.e., C valley, A valley, ﹩{R}_{\mathrm{valley}}^{+}﹩, ﹩{R}_{\mathrm{valley}}^{-}﹩, and f NP) as functions of [Fe/H]. In Section 4.1, we rescale the planet radii to eliminate the influence of stellar mass and planetary orbital period on the boundary of radius valley. The results with rescaling radii are plotted as open circles and shifted to the right to avoid overlapping.