adsabs/AstroCLIMB huggingface dataset:
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: BD-17 0063: results of the joint Gaia–Doppler fit, assuming the companion is dark. Left: Doppler data as a function of time and folded time, with residuals. Red curves show the maximum a posteriori probability (MAP) model. Right: The two top panels compare the parameters of the joint model with those from Gaia alone. The first panel shows the Thiele–Innes coefficients; open symbols are the Gaia-only values and red points are from the MAP model. The second panel shows the Z-score (“number of sigma”) between the Gaia-only and best-fit parameters. The lower-right panel shows the orbital geometry according to the MAP model, with black representing the portion on the “near side” of the sky plane and gray representing the “far side.” The origin is the location of the center of mass, the white circle marks the pericenter position, and the red arrow conveys the direction of motion.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 114762: results of jointly fitting the Doppler and astrometric data. Same format as Figure 1, except that the model curve is not shown in the upper-left panel because the plotted time range spans too many cycles for the details to be visible. In the radial-velocity plots, the blue, yellow, and green points are from the Coude spectrograph on the Harlan J. Smith telescope (Cochran et al. 1991), the Lick/Hamilton spectrograph (Kane et al. 2011), and Keck/HIRES (Rosenthal et al. 2021), respectively.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HR 810: results of jointly fitting the Doppler and astrometric data. Same format as Figure 1. The results should be viewed skeptically; see the text for details.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 81040: results of the joint Gaia–Doppler fit, assuming the companion is dark. Same format as Figure 1. In the radial-velocity plots, the filled symbols are from ELODIE and the open symbols are from HIRES.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 132406: results of jointly fitting the Doppler data and Gaia two-body orbital solution, assuming the companion is dark. Same format as Figure 1. In the radial-velocity plots, the filled symbols are from ELODIE, and the open symbols are from SOPHIE.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HIP 66074: results of jointly fitting the Doppler data and Gaia two-body orbital solution. Same format as Figure 1.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 175167: results of jointly fitting the Doppler and astrometric data. Same format as Figure 1.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 111232: Doppler data and the best-fit model, including a single planet and an ad hoc quadratic function of time representing the effects of other bodies.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: BD-17 0063.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: Planet mass vs. period for all planets with known masses and periods. The dashed black lines show the boundaries of the Neptune desert from (Mazeh et al. 2016), the black triangles show M-star planets, the blue circles show all stellar hosts, and the red star shows TOI-674 b. We also show several other similar planets to TOI-674 b on the plot. The total planet sample has been significantly expanded since Mazeh et al. (2016), and the original sharply pointed boundary may in fact have a much more gradual limit near 100.5 days. Planet mass and period data taken from the Exoplanet Archive (NASA Exoplanet Science Institute 2020).
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: The broadband data for the first transit of TOI-674 b. Top: the raw transit data, with the systematics and transit model. Middle: the detrended transit data and light-curve model. Bottom: the white-light-curve residuals.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HIP 66074.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 175167.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 114762.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 132406.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HD 81040.
Paper: Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Joshua N. Winn
Figure caption: HR 810.
Paper: Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset
Authors: Samson J. Mercier, Lisa Dang, Alexander Gass, Nicolas B. Cowan, Taylor J. Bell
Figure caption: Spitzer/IRAC 4.5 μm phase curve of 55 Cancri e ∣Top left: Phase-folded, instrument-detrended Spitzer data and our best-fit models. The solid gray line corresponds to our unconstrained analysis where we do not assume that the phase curve is planetary in nature and therefore do not impose a strictly positive phase curve. In our legend, we use the abbreviation FREE for this unconstrained analysis. The red and blue points correspond to decorrelated photometric data for all AORs and, like in Figure 1, we separate them into two groups and distinguish them with different colors. The gray points are the decorrelated photometric data for our unconstrained analysis. For the constrained and unconstrained analyses, the decorrelated photometric data were binned within each AOR by an extra factor of 75 and 150, respectively. Bottom left: the residuals for our fiducial, constrained model. Top right: The solid black line is our best-fit model using BLISS mapping, same as in the top left plot, and the solid gold line is the best-fit model from D16b. The points represent the decorrelated photometric data for all eight AORs and, like in Figure 1, we separate them into two groups and distinguish them with different colors. These decorrelated photometric data were binned across all AORs by an extra factor of 165. Bottom right: corresponding residuals for our best-fit model. The error bars in each plot are the error on the mean within each bin. We have also added vertical lines for the phase offset obtained with our constrained and unconstrained analyses, and by D16b. Neither our constrained or unconstrained fit match that of D16b, despite using the same raw data detrended with BLISS mapping. The constrained fit is our preferred model; it exhibits a large dayside flux, a negligible offset, and small nightside flux.
Paper: Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset
Authors: Samson J. Mercier, Lisa Dang, Alexander Gass, Nicolas B. Cowan, Taylor J. Bell
Figure caption: Centroid position and raw photometric data. Plotted on the left is the centroid position on the IRAC detector and on the right is the phase-folded raw photometry obtained from SPCA. In both plots, the 8 AORs are separated into two groups: the red group represents the phase range −0.1–0.4 and the blue group represents the phase range 0.4–0.9. The solid black lines on the left plot show the pixel edges. The gray bands in the right plot correspond to the transit (0 phase) and eclipse (0.5 phase) of 55 Cancri e. The black dashed vertical line represents the phase offset obtained by D16b. Note that the offset lines up with the suture point of the two AOR groups around 0.4 orbital phase.
Paper: Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset
Authors: Samson J. Mercier, Lisa Dang, Alexander Gass, Nicolas B. Cowan, Taylor J. Bell
Figure caption: Dayside and nightside brightness temperatures plotted against irradiation temperature, for all circular exoplanets with published 4.5 μm phase curves. Values plotted as gray circles are from Bell et al. (2021), while gray triangles, squares and diamonds are from Crossfield et al. (2020), Zhang et al. (2018), and May et al. (2021), respectively. The gold and black values for 55 Cnc e are from D16b and this work, respectively. In the top plot, the dotted gray line represents the equilibrium temperature while the solid gray line represents the irradiation temperature. The extremely hot dayside brightness temperature for 55 Cnc e is qualitatively consistent with a temperature inversion and 4.5 μm emission due to SiO.
Paper: Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset
Authors: Samson J. Mercier, Lisa Dang, Alexander Gass, Nicolas B. Cowan, Taylor J. Bell
Figure caption: Binned residuals rms plotted against bin size. The expected decrease in white noise is shown as a solid red line. The solid black line indicates the photometric residual rms computed for different bin sizes N binned. The lighter shaded area around the photometric residual rms is the uncertainty that the MC3 package computed (Cubillos et al. 2017). The vertical gray dashed and dashed–dotted lines represent the number of bins contained in the duration of an occultation ingress/egress and in the duration of the entire transit/eclipse.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Performances of the three shear measurement methods (FQ, KSB, re-Gaussianization) for different values of Q. The dashed lines indicate the input shear values, and the shaded region represents the upper and lower 1% bound of input shear values. Each data point shows the recovered shear value using four images (separated by 45° to remove the shape noise and the anisotropic shear responsivity) of one mock galaxy generated by Galsim. No noise is added. In each panel, we include the results for the Gaussian and Moffat PSF in blue and red, respectively. The solid curves connecting the hexagon points are included to show the averages of the scatter points.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: The multiplicative bias as a function of Q for different galaxy sizes. The two panels show the results for the Gaussian and Moffat PSF respectively. In each panel, the red, green, and blue lines are from galaxies of small, middle, and large sizes, respectively. The parameter f is the ratio between the postseeing FWHM of the galaxy and that of the PSF. The solid and dashed–dotted lines are the results of m 1 and m 2 respectively. The shaded region represents the requirement on m (± 2 ∗ 10−3) by the Stage IV surveys.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Performance of FQ for four types of PSFs: Gaussian, Moffat, Airy disk, and CSST i band. The blue data points and light gray regions are similarly defined as in Figure 3. The dark gray regions show the 2∗10−3 bound around the input shear value. The red data points with error bars are the ensemble averages of the shear value, which indicate the level of systematic bias in the presence of the pixelation effect. The galaxies used in producing this figure are all generated using random walks of point sources.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Similar to Figure 3, but for the g 2 component.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: The blue line in each panel shows the PSF power spectrum for Q = 2, and the orange dashed line is the PSF power for Q > > 2, i.e., without the aliasing power.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Simulated oversampled PSF profiles for the g/r/i bands of CSST (in logarithmic scale, not with real pixel size).
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Similar to Figure 5, but for the g 2 component.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Undersampled (left) and oversampled (right) images for the same galaxy.
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: The eclipse timing (O–C) diagram of EW Boo with the terms of LITE ephemeris. In the top panel, the solid curve represents the τ 3 orbit. The bottom panel shows the residuals from the complete ephemeris.
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: The four spectral absorption lines of the primary component. The black dots and red solid lines represent the disentangling spectrum obtained by the FDBINARY code and the synthetic spectrum at 8560 K and 90 km s−1, respectively.
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: The HR diagram for EW Boo (star symbols) and other semidetached EBs with a δ Sct component (circles; Kahraman Alicavus et al. 2017). The primary and secondary components for EW Boo are marked as the open and filled symbols, respectively. The blue and red lines represent the theoretical edges of the δ Sct instability strip (Rolland et al. 2002; Soydugan et al. 2006a). The black solid and dotted lines denote the ZAMS and TAMS lines (Girardi et al. 2000).
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: The black circles represent the observed TESS data (top) and their corresponding residuals (bottom). The red synthetic curve in the top panel was obtained from Model 2 in Table 3.
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: The upper panel shows the time domain residuals of light curves subtracting binary effects. The lower panel shows a short section of the residuals in the inset box of the upper panel. The synthetic curve was computed from the 127 frequency fit to the data.
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: Amplitude spectrum before (upper panel) and after (bottom panel) prewhitening from the PERIOD04 program. The red solid line in the bottom panel is four times the local noise spectrum, which was calculated for the grids on 3 day−1.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: TiO γ bands and the corresponding Stokes parameters Q and U in the optical spectrum of VY CMa.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: ScO bands in emission and the corresponding Stokes parameters Q and U in the optical spectrum of VY CMa.
Paper: High-resolution Linear Spectropolarimetry of Red Supergiant VY CMa: Identification of Atomic and Molecular Features
Authors: Dinh-V-Trung, N. T. T. Bao, P. M. Tien, B. V. Hai, P. H. Minh, L. H. Khiem
Figure caption: TiO γ′ bands and the corresponding Stokes parameters Q and U in the optical spectrum of VY CMa.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Median-combined original (left) and primary-subtracted (middle) images of the Epoch 2020 observations, and extracted spectra of VHS 1256 b (right) at maximum and minimum brightness. In the left panel, from top to bottom, the three brightest spectral traces are VHS 1256 AB (the host binary), VHS 1256 b (the substellar companion), and a background star (2MASS J12560179–1257390). The VHS 1256 b trace is moderately contaminated by the primary PSF. We mitigate the contamination by subtracting an empirically derived PSF model, and the primary-subtraction result is shown in the middle panel. The right panel shows the extracted spectra of VHS 1256 b at its brightest (blue) and faintest (yellow) phases. Their relative difference and the uncertainty are shown as a black line and a gray shaded region in the bottom subplot of the right panel.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Fitting the multiple-sinusoidal model to the broadband light curve. The left panel highlights the excellent agreement between the observed broadband light curve (blue dots) and the best-fitting model (black solid line). Individual model components (the three sine waves and the linear trend) are shown as color dashed lines. In the right panel, we isolate these components to illustrate their importance to the good fit. The top, middle, and bottom panels feature the linear slope, Waves 1+2 and Wave 3, respectively. In each panel, model components other than the one being highlighted are subtracted from both the observed and model light curves. The middle-right panel demonstrates the combined effect of two sine waves that have best-fitting periods of 18.8 and 15.1 hr. In this panel, individual waves are plotted in the dashed lines, and their sum is in the solid red line.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Results of the Lomb–Scargle periodograms analysis. The periodogram of the observed light curve (with the linear trend removed) is shown in all three panels as blue solid lines. In the top panel, the gray solid line marks the periodogram of the observing-window function. The middle panel includes two periodograms derived from the evenly sampled best-fitting model, with time ranges of 42 hr (orange) and 210 hr (magenta). In the bottom panel, the green shaded region shows the periodogram of the best-fitting model sampled in the same way as observations. The range of the region reflects fitting uncertainties. Due to the irregular sampling window, peak locations in the periodograms do not match the results obtained by fitting Equation (1) (black vertical lines).
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Combined light curves of VHS 1256 b in the 2018 and 2020 epochs. In four representative bands: G141 broad band (top panel), F127M (centered at 1.27 μm, sampling the continuum on the blue side of the water band; bottom left panel), F139M (centered at 1.39 μm, sampling the water band; bottom middle panel), and F153M (centered at 1.53 μm, sampling the continuum on the red side of the water band; bottom right panel). The Epoch 2018 light curves are plotted as squares, and the Epoch 2020 light curves are shown as circles. The light curves are normalized by the minimum flux measured in each band. The reference flux values are indicated at the bottom right corners. The right axis of the top panel marks the broadband flux density in erg s−1 cm−2 μm−1. The x-axes are broken to fit the two epochs of data.(The data used to create this figure are available.)
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Heavily stretched grism images of VHS 1256 b showing the contaminating sources in the Epoch 2018 (left) and Epoch 2020 (right) observations. The orange solid contours mark a flux level at 1% of the image maximum, highlighting the position of VHS 1256 AB. The primary binary’s extended PSF is the major contaminating source in the flux measurements of VHS 1256 b. The orange dashed contours show the position of the cross talk systematics caused by the intense illumination from VHS 1256 AB. The cross talk signal is at a symmetric location relative to the PSF of VHS 1256 AB with respect to the x-axis and has a negative flux. The blue rectangles mark the positions of spectral traces of faint background sources.