adsabs/AstroCLIMB huggingface dataset:
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of HD 24040. Top left: K2 and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on K2 or TESS. The rightmost plots highlight the differences between Kepler and TESS training.
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of HD 106315. Top left: K2 and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on K2 or TESS. The rightmost plots highlight the differences between Kepler and TESS training. A dashed black line indicates the orbital period and amplitude of the system's known planet(s).
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of HD 119291. Top left: K2 and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on K2 or TESS. The rightmost plots highlight the differences between Kepler and TESS training.
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of Kepler-37. Top left: Kepler and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on Kepler or TESS. The rightmost plots highlight the differences between Kepler and TESS training. A dashed black line indicates the orbital period and amplitude of the system's known planet(s).
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of HD 31966. Top left: K2 and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on K2 or TESS. The rightmost plots highlight the differences between Kepler and TESS training.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Radial distributions of [N II]/Hα, [S II]/Hα, and [S II]/[N II] line ratios and oxygen abundance as a function of Rgal. The data are organized into 16 bins based on Rgal, and a dashed line connects the median value of each bin. The results of Sample-I and Sample-II are illustrated in the left and right panels, respectively.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Plan view of the disk DIG from the north Galactic pole displaying the projection of the sample points on the Galactic disk. The Galactic center is taken as the origin point, the direction from the Sun to the Galactic center is taken as the polar coordinate starting direction, and the radial unit is in kiloparsecs. We mark the location of the solar system at the Galactocentric distance of 8.34 kpc. Background image credit: NASA/JPL-Caltech/ESO/R. Hurt.
Paper: Diffuse Ionized Gas in the Anticenter of the Milky Way
Authors: Shiming Wen, Wei Zhang, Lin Ma, Yunning Zhao, Man I. Lam, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Guozhen Hu, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: Similar to Figure 7, with the variation plotted as a function of Galactic disk height (z).
Paper: Exoplanet Occurrence Rate with Age for FGK Stars in Kepler
Authors: Maryum Sayeed, Ruth Angus, Travis A. Berger, Yuxi(Lucy) Lu, Jessie L. Christiansen, Daniel Foreman-Mackey, Melissa K. Ness
Figure caption: Planet occurrence rate as a function of isochrone age (blue, dashed line) and gyrochronology age (black, solid line), in groups of stellar mass and metallicity. The text indicates the number of observed planets in each bin. The mass increases from top to bottom, and the metallicity increases from left to right, where the low- and high-mass samples refer to mass ranges of 0.8 − 1.0 M⊙ and 1.0 − 1.2 M⊙, respectively, and low to high metallicity refers to metallicity ranges of −0.5 − 0.0 dex and 0.0 − 0.5 dex, respectively. Based on the slope and p-value (see Table 2), there are no significant trends in bins of mass, metallicity, and age.
Paper: Exoplanet Occurrence Rate with Age for FGK Stars in Kepler
Authors: Maryum Sayeed, Ruth Angus, Travis A. Berger, Yuxi(Lucy) Lu, Jessie L. Christiansen, Daniel Foreman-Mackey, Melissa K. Ness
Figure caption: Planet occurrence rate as a function of isochrone age (blue, dashed line) and gyrochronology age (black, solid line). Left: detection efficiency, Q, per age bin, where the error bars are the standard deviation of Q in each bin. Middle: number of planets per star, where the error bars indicate binomial errors (Equation (10)). Right: occurrence rate of planets per age bin, where the error bars indicate the propagated error (Equation (11)) from the detection efficiency and rate of planets. The text in the middle and right panels indicates the number of observed planets in each bin for stars with isochrone ages (blue) and gyrochronology ages (black); see Table 1 for the number of stars in each bin. We find no significant trend in the exoplanet occurrence rate as a function of age for both samples.
Paper: Exoplanet Occurrence Rate with Age for FGK Stars in Kepler
Authors: Maryum Sayeed, Ruth Angus, Travis A. Berger, Yuxi(Lucy) Lu, Jessie L. Christiansen, Daniel Foreman-Mackey, Melissa K. Ness
Figure caption: Left: stellar sample from B20 and L24 on an H-R diagram before and after quality cuts. Middle: age distribution of isochrone and gyrochronology ages for 2658 stars in both sets. Right: comparison of gyrochronology and isochrone ages with an rms of 1.79 Gyr. The red points show the median isochrone and gyrochronology ages within age bins, where the error bars show the 16th and 84th percentiles of the isochrone age. The yellow line indicates perfect agreement between the two age samples. There is a significant deviation between both ages for overlapping stars; stars with gyrochronology ages are preferentially younger than those with isochrone ages and cover a larger parameter space than isochrone ages.
Paper: Exoplanet Occurrence Rate with Age for FGK Stars in Kepler
Authors: Maryum Sayeed, Ruth Angus, Travis A. Berger, Yuxi(Lucy) Lu, Jessie L. Christiansen, Daniel Foreman-Mackey, Melissa K. Ness
Figure caption: Distribution of stellar isochrone mass (top) and spectroscopic metallicity (bottom) with isochrone (left) and gyrochronology (right) ages, where the color indicates the number of data points in each bin, with equal numbers of bins across the four distributions. These distributions illustrate that the two samples of isochrone and gyrochronology ages span different parameter spaces in mass and metallicity, despite sharing the same stars. It also shows the relationship between mass and metallicity with age, which could bias the trend between the occurrence rate and age.
Paper: Revised Masses for Low-density Planets Orbiting the Disordered M-dwarf System TOI-1266
Authors: Dakotah Tyler, Erik A. Petigura, James Rogers, Jack Lubin, Andreas Seifhart, Jacob L. Bean, Madison Brady, Rafael Luque
Figure caption: Combined RV time series for TOI-1266. The HARPS-N observations from R. Cloutier et al. (2024) are indicated by pink squares. The MAROON-X observations (this work) are blue and red circles for the blue and red arms, respectively. The best Keplerian model for the system is plotted with a solid blue line. The MAROON-X RV's are available in machine readable format.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Revised Masses for Low-density Planets Orbiting the Disordered M-dwarf System TOI-1266
Authors: Dakotah Tyler, Erik A. Petigura, James Rogers, Jack Lubin, Andreas Seifhart, Jacob L. Bean, Madison Brady, Rafael Luque
Figure caption: Generalized Lomb–Scargle periodogram for offset-corrected MAROON-X time series. The known planets periods are indicated with vertical red dashed lines (Pb = 10.89 days) and 18.97 days (Pc = 18.8 days). The candidate planet at 32.2 days is marked with a vertical orange dashed line. The 1% FAP is plotted with the horizontal blue dashed line.
Paper: Exoplanet Occurrence Rate with Age for FGK Stars in Kepler
Authors: Maryum Sayeed, Ruth Angus, Travis A. Berger, Yuxi(Lucy) Lu, Jessie L. Christiansen, Daniel Foreman-Mackey, Melissa K. Ness
Figure caption: Integrated detection efficiency for the full sample of 2658 stars with available isochrone and gyrochronology ages over a grid of orbital period and planet radius. The contours and grid lines are shown for reference.
Paper: SKYSURF. VI. The Impact of Thermal Variations of HST on Background Light Estimates
Authors: Isabel A. McIntyre, Timothy Carleton, Rosalia O'Brien, Rogier A. Windhorst, Sarah Caddy, Seth H. Cohen, Rolf A. Jansen, John MacKenty, Scott J. Kenyon
Figure caption: Schematic of HST Wide Field Camera 3 (WFC3), adapted from J. W. MacKenty et al. (2010). The components of the WFC3 that we focus on for this paper are the pickoff arm, which holds the pickoff mirror, and components near the infrared cold enclosure and filters.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Bottom panels: detected Hilda asteroids during the phase II of CSS operations projected onto the plane of Cartesian folding of eccentricity e vs. perihelion ϖ, namely ﹩e\,\exp (\imath \,\varpi )﹩: (i) the dotted axes (and the numerical values at the abscissa and on the ordinate) are the osculating heliocentric values of e and ϖ as of MJD 60200.0 epoch, and (ii) the dashed axes (with the origin shifted to the forced planetary term) are the proper parameters ep and ϖp. The left panels show H ≤ 15 (bright) Hildas (the size of the symbol indicating the size of the asteroid), and the right panels show H ≥ 16.5 (faint) Hildas. The enveloping gray circle approximately delimits the observed population. The dashed circles with ep = 0.12 and ep = 0.22 specify the annulus, from which data shown at the upper panels is registered. These show the distribution of number of detected Hildas in ϖp using 20∘ bins. Bright Hildas (top and left) are consistent with uniform distribution within that area. Faint Hildas (top and right) have a nonuniform distribution with maximum at ϖp ≃ 60∘ and minimum at ϖp ≃ 240∘. This is due to the shift of the origin by the forced (Jupiter’s) term eforced ≃ 0.08 along the ϖ ≃ 0∘ axis. Small (faint) Hildas can be detected only on large-eccentricity orbits with low-enough perihelion.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Hilda population represented by the 1D distributions of the proper parameters: (i) ap (left panel), (ii) ep (middle panel), and (iii) ﹩\sin {I}_{{\rm{p}}}﹩ (right panel). The location of the principal families, most distinctly featured by peaks of the inclination distribution, is indicted by labels (right panel). Data are shown by the gray histogram with bin size given in Table 8 and used in Sections 4 and 5 to determine properties of bias-corrected Hilda population. The color-coded solid lines illustrate distribution functions Di(pi) for various subpopulations: (i) background population (black line), (ii) Schubart family (red line), (iii) Hilda family (blue line), and (iv) Potomac family (cyan line). The green line is their composite, which, after adjustment of free coefficients in Di(pi) should match the observed data. Since the purpose of this figure is to illustrate the capability of the chosen Di(pi) functions to match the data, their free coefficients were preliminarily guessed here. Their values after optimization of the model to the observations will be given in Section 5.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Detection probability ﹩{ \mathcal P }\left({\boldsymbol{p}};H\right)﹩ for the Hilda asteroid having orbital parameters ap = 3.99 au, ep = 0.155, all sampled values of ﹩\sin {I}_{{\rm{p}}}﹩ (smaller values larger detection probability for a given H), and two values of ϖp = 45∘ (dark gray curves) and 225∘ (light gray curves) as a function of the absolute magnitude H. The left panel shows phase I, and the right panel shows phase II of CSS operations. The color-coded curves are for the approximate inclinations of the major families: (i) red for Schubart, (ii) blue for Hilda, and (iii) cyan for Potomac families. The detection probabilities for ϖp = 225∘ are shifted by up to  ≃0.5 mag in H compared to ϖp = 45∘ values for faint objects in phase II (see also Figure 5 are related discussion). The spread with orbital inclination is small for the phase II data thanks to field-of-view sampling of high ecliptic latitudes (Figure 1). The phase I operations are concentrated more closely to the ecliptic zone; thus, the detection probability falls more rapidly with increasing inclination value. Additionally, even the lowest-inclination probability of phase I is somewhat smaller, and the ϖp trend is less evident due to its considerably shorter time span.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Differential magnitude distribution (left panel; bin width 0.25 mag) and cumulative distribution of the selected Hilda population of 6094 asteroids known as of 2024 January (Section 2). The black line is the total population downloaded from the MPC database; blue shows detections by CSS during the phase I; red shows detections by CSS during the phase II operations. For the sake of reference, the upper abscissa translates the absolute magnitude value to size using a constant geometric albedo pV = 0.055, mean value in the Hilda population reported by T. Grav et al. (2012). This information is relevant to understand what part of the population is being tested in the long-term simulations in Section 6.2.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Population of 6094 Hildas known as of 2024 February projected onto 2D planes of proper parameters: (i) ﹩({a}_{{\rm{p}}},\sin {I}_{{\rm{p}}})﹩ top left, (ii) ﹩({e}_{{\rm{p}}},\sin {I}_{{\rm{p}}})﹩ top right, and (iii) (ap, ep) bottom. The size of the symbol correlates with the size of the asteroid. The statistically significant clusters, prominently concentrated in ﹩\sin {I}_{{\rm{p}}}﹩, are collisional families. The two largest are associated with (153) Hilda (blue star) and (1911) Schubart (red star). The gray line in the bottom panel shows location of the stationary point of the J3/2 mean-motion resonance with Jupiter at Ip = 0∘ (see Appendix B.1).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Population-wise weighted detection probability ﹩\overline{{ \mathcal P }}(H)﹩ computed using Equation (13) (left panel for phase I; right panel for phase II of the CSS operations). Different curves for specific choice of the weighting function w(p): (i) background (green), (ii) Schubart family (red), and (iii) Hilda family (blue). The composite total is the black line. The embedded plots show the behavior of ﹩\overline{{ \mathcal P }}(H)﹩ for the brightest Hildas and two specific values of ϖp = 75∘ (red) and 285∘ (blue). Here the detection probability may again drop from unity due to signal saturation, especially when the asteroid is sensed near perihelion of its orbit (red curve). This problem, and the sky coverage incompleteness, manifest primarily in the CSS phase I due to its short duration. In the twice-as-long phase II, even the bright Hildas may eventually appear to be observable close to the aphelion of their orbit, increasing their apparent magnitude to allow detection.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Detection probability ﹩{ \mathcal P }\left({\boldsymbol{p}};H\right)﹩ for Hilda asteroid having orbital elements ap = 3.99 au, ep = 0.155, ﹩\sin {I}_{{\rm{p}}}=0.05﹩ as a function of ϖp for four values of the absolute magnitude H: (i) 7.5 (cyan curve), (ii) 15.45 (red curve), (iii) 15.95 (blue curve), and (iv) 16.45 (green curve). In the CSS phase II case (right panel), ﹩{ \mathcal P }\left({\boldsymbol{p}};H\right)﹩ for the groups (i) and even (ii)—brightest from the faint group—does not depend on ϖp (or only weakly). Conversely, ﹩{ \mathcal P }\left({\boldsymbol{p}};H\right)﹩ for fainter groups (iii) and (iv) becomes strongly dependent on ϖp. Statistics of the observed Hildas (Figure 5) match the predicted profile with maximum at ϖp ≃ 45∘ and minimum at ϖp ≃ 225∘. The trends in the CSS phase I are affected by field-of-view incomplete coverage of sky and its short duration.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Differential magnitude distribution of the G96 observations (blue for phase I and red for phase II) compared with the best-fitting biased model (black line with a σ interval, based on analysis of 10,000 posterior random samples of the model, depicted by the gray zone). The ordinate normalization corresponds to the magnitude 0.1 mag bins used for the model. The data, originally allocated to 0.2 mag bins, were smeared into the neighboring 0.1 mag wide bins for direct comparison with the model (this also implies that the lowest occupancy is “0.5 body"). The largest detected objects with H < 9 mag (four in both phases I and II) are shown individually by symbols (the model predicts slightly less than one object in this range, but the fit is dominated by H > 9 mag objects).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Number of detections for each unique Hilda in the CSS phase I (left; 2970 bodies) and phase II (right; 4317 bodies) plotted as a function of the absolute magnitude. Each black dot stands for one observed Hilda member. The blue curve is the mean number of detections in a 0.25 wide magnitude bin, and the vertical bars are statistical dispersion within the bin. The black line is the population-wise weighted ﹩\overline{{ \mathcal R }}(H)﹩ prediction from our model. The gray area delimits our simple estimate of a range defining in 0.1-wide bins the minimum to maximum number of detections as a function of H (see the text for more details).