adsabs/AstroCLIMB huggingface dataset:
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: The pyKLIP reduced 2393 2 s images of the 2022 April data set. The pyKLIP parameters are 10 KLIP modes removed, movement = 0, high-pass filtered at 5.3 pix, and 1.3 hr of total integration (frames stacked into 39× 120 s images that are fed into pyKLIP with 96° of rotation). The green circles (r = 13 mas continuum; r = 20 mas Hα and ASDI) have identical centers in all images and are centered on the predicted planet orbital location from the orbit of J. J. Wang et al. (2021). Following D. Mawet et al. (2014), the SNR of the ASDI b detection is 5.3, while c is weakly detected at just SNR ∼ 2.2. This image is 762.75 × 454.3 mas, and North is up, and East is left in these, and all following, images.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Summary of all of the data sets with the parameters from Figures 2, 3, and 4. Note how much better c has been detected in 2023 and 2024, vs. 2022. We get this “contrast boost” in 2023–2024 by: use of the narrow Δλ = 1 nm Hα filter (which passes all of the Hα planet light but minimizes starlight), better AO correction, better read noise, and better removal of the non-common-path errors. This all results in the Hα Strehl improving from 9% in 2022 to 20% in 2023 and still further to 26% in 2024.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Possible scattered light off the PDS 70 b CPD. Here we see in an 0.94 × 0.″94 two-color image that the continuum image from 2023 (shown in blue) shows a strong scattered light feature centered on the Hα emission from PDS 70 b (shown in pink). We see that the Hα emission of b is that of a point source. We note that the slight elongation in the radial direction of the Hα emission is typical of a point source with some self-subtraction with the pyKLIP reduction. This pink point source subtracts very well with a forward-modeled planet, as noted in the photometry Section.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Here we see that the continuum image from Figure 5 (shown in blue) shows a strong elongation that is roughly consistent with the circumplanetary dust detected by O. O. Balsalobre-Ruza et al. (2023) with ALMA at 855 μm (yellow contours). Note that we have superimposed these contours at the peak of b’s emission, assuming the 855 μm dust is orbiting around PDS 70 A with b.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Here we see the 3.5 hr PSF of PDS 70 A at Hα of the 2023 March data set. The units are the log10 of the photons minute−1 pixel−1 on a median stack of 219× 60 s images; the x-axis is in 0.″0059 pixels. There is no smoothing or block averaging applied. We show the positions of the peak pixel locations of the b and c planets with the correct contrasts. This image is very helpful in that it shows how pyKLIP is clearly needed to detect the planets because they are ∼3× below the noise floor of the PSF. However, we have 219× 60 s images, and so pyKLIP can easily trace and remove the lower orders in the PSF and through ADI clearly detect both the b and c planets. At the locations of b (155 mas), the stellar photons are about equal to those from the residual read noise, bias, and CIC residuals. By the position of c (206 mas), the flux is more dominated by read noise, bias, and CIC noise residuals, which are independent of light from the star, as the PSF starts to flatten out. This plot is also very useful, as it shows that we expect ∼2.6 Hα photon minute−1 pix−1 from the center planet b pixels and ∼1.8 Hα photon minute−1 pix−1 from planet c (these are very faint signals). Inset: we show a log stretch of the PSF with a 18.5 pix high-pass filter (this leads to a slight dip around the central star, but helps highlight compact speckles), but very little flux is removed from the core of the PSF (or the planet) with a 18.5 pix high-pass filter. This slightly negative dip around the PSF core is completely removed by the pipeline during the radial profile subtraction step. The two green circles trace the circles that the b and c planets traced out as they moved 137° along these circles during the observations as the sky parallactic angle rotated.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: The calculated Hα line fluxes of planets b and c, assuming no extinction (A R = A p = 0 mag) from the last two columns of Table 4. The main plot covers 7 yr of observations and has a large Y-axis upper limit to accommodate the 2017 February archival MagAO image recovery of c (K. B. Follette et al. 2023). Even though the errors are large, it appears that both c and b may have been much brighter at Hα around 6–7 yr ago. Then, from 2018 April to 2022 April, planet b was roughly constant at ∼11 × 10−16 erg s−1 cm−2 (see inset for zoom in), but then from 2023 March onward, b dramatically faded to just ∼2–3 × 10−16 erg s−1 cm−2. Planet c’s line flux has been roughly constant since 2018 April at ∼5 × 10−16 erg s−1 cm−2. Yet, we see evidence that c’s flux is changing with a slight (but significant) 2.3× increase from 2023 to 2024. The green points are the magnitudes of PDS 70 A that we observed in the continuum filter and converted to r′. This variability of PDS 70 A in the continuum was accounted for and calibrated out of our MagAO-X line fluxes in this work. These data suggest that b is generally fading at Hα but c has recently brightened and now surpasses b.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: ASDI contrast curves (ASDIcontrastHα  vs. Separation) from 2022 (3σ) and 5σ for 2023 and 2024 (1 pix = 0.″0059). Left panel: we show the 3σ contrast curve for the 2023 data set with a movement of 0 with 10 KLIP modes after pyKLIP reduction of our 39× 120 s images. We also plot the actual detections of planets b (contrast of 2.8 × 10−4; and c (0.9 × 10−4), which were detected at SNR = 5.3 and SNR = 2.2, respectively. See the right-hand panel image in Figure 2 to see the image for which this curve was generated. Middle panel: the 5σ ASDI 2023 data reduction of 219× 60 s images with pyKLIP (movement 0; 10 modes; see right panel of Figure 3). We also show the detections of planets b (contrast of 4.75 × 10−4) and c (contrast of 4.25 × 10−4) detected at SNR = 10.4 and SNR = 13.1, respectively. Note that even though the ASDI Hα flux of b was 4.6× fainter in 2023, the contrasts are larger (easier to detect) than in 2022 because we switched from the 8 nm wide Hα filter in 2022 to the much narrower 1 nm filter in 2023. So even if raw ASDIcontrastHα  were only marginally increased in 2023, our sensitivity to lower Hα line fluxes was increased by ∼8× by our “contrast boost” by using the narrower 1 nm filter and better Strehl. Right panel: here we show the 2024 data set with b at ASDIcontrastHα  = 4.7 × 10−4 at SNR = 4.3 and c with ASDIcontrastHα  = 6.2 × 10−4 and SNR = 12.3; this is based on the image in Figure 4.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Left panel: a composite image of the outer 1.48 × 1.″40 ASDI field with a classical ADI reduction around PDS 70 lacks any obvious Hα emission point sources besides c and b. The inner dark hole has a ∼10× suppressed stretch and is 0.″227 in radius. We did detect one marginally significant (∼3σ) source (CC2 at sep = 0.″348 PA = 184.°0) that seemed to be present in all of the reductions in the 2022 and 2023 data sets. The outer ellipse is the rough position of the ALMA dust-free cavity (r = 76 au), and the faint dashed blue line is the possible coplanar orbit for CC2 (r ∼ 57 au). Right panel: same field with a single uniform stretch, CC2's ASDI contrast is ∼7.5 × 10−5 at ∼3σ. Each of the sources as bright as CC2 were found to be strong continuum sources as well, only CC2 was the only outer source (other than b and c) significantly detected in Hα but not continuum. Unfortunately, CC2 was not detected in the 2024 data set, casting doubt on its existence.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Left panel: the radiative transfer scattered light model of J. Szulágyi & A. Garufi (2021) showed that for a 10 M jup protoplanet at 20 au, one would expect a CPD diameter of ∼6.6 au (2 Hill Sphere radii) reproduced from Figure A1 of J. Szulágyi & A. Garufi (2021). Right panel: the observed dust distribution (continuum filter) in 2023 around b is in reasonably good agreement with the predicted scattered light model of a CPD. The CPD has a diameter of ∼5 au and is brightest on the edge facing into the starlight with the back and center of the flared CPD possibly in shadow.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: The upper panels show the original 2024 ASD image. The upper-right panel shows the same data set after BKA forward modeling of negative fake planets added on top of the real planets. When the astrometry and photometry of the fake planets matches the flux, then the positions of both planets are zero. This verifies that the fake planets are correct in flux, allowing the ASDIcontrastHα  to be directly measured. In the bottom panels, we inserted a “ring of fake planets” all at the ASDIcontrastHα  of b (left) and c (right) to estimate the residual noise in the final ASDI images at the radii of the planets.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Here we see a full Gaussian propagation of 10,000 random draws of errors with Equation (4) of observed uncertainties of the r′ flux of PDS 70 A and those of the measured ASDI contrasts of b and EMgains. It is fit (black Gaussian lines) quite well by a (3.64 ± 0.87) × 10−16 erg s−1 cm−2 Hα line flux for b (red; top) and by (4.77 ± 0.43) × 10−16 erg s−1 cm−2 for c (blue; bottom). The c–b flux difference is (1.13 ± 0.97) × 10−16 erg s−1 cm−2; hence, c is ∼1.2σ brighter than b in 2024. This implies that there is a ∼12% chance that b is actually brighter than c (despite how clearly c looks significantly brighter than b in our 2024 data; hence, errors are perhaps too large). Regardless of the possibility that these errors are perhaps slight overestimates, we adopt these errors throughout this study.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Shown here are the ASDI data sets from Figure 6 with a deep stretch to depict the inner disk area near the star (small light-green circle in center). There is only one object inside the orbit of b that could be consistent with a plausible orbit around PDS 70. This r ∼ 5.6 au orbit is highlighted by the larger green circle at all epochs. Note that the very bright object “CC3” in the 2023 and 2024 ASDI images track this orbit (large green circle). The object is at 41 mas and PA = 305° in 2023 and rotates clockwise (as expected) to 49 mas and PA = 295° in 2024. This object is not detected well in the lower-quality 2022 data set. Object CC3 could be a bright clump in the inner disk.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Similar to Figure 10, but for the 2024 data set. The 2024 observed dust distribution around b is in reasonably good agreement with the scattered light radiative models of J. Szulágyi & A. Garufi (2021), where the size of the CPD diameter is estimated at ∼9 au. The back and center of the flared CPD may be in shadow from the brightly illuminated front side edge.
Paper: A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Authors: Lisa Dang, Taylor J. Bell, Ying (Zoe) Shu, Nicolas B. Cowan, Jacob L. Bean, Drake Deming, Eliza M.-R. Kempton, Megan Weiner Mansfield, Emily Rauscher, Vivien Parmentier, Alexandra Rochon, Kevin B. Stevenson, Mark Swain, Laura Kreidberg, Tiffany Kataria, Jean-Michel Désert, Robert Zellem, Jonathan J. Fortney, Nikole K. Lewis, Michael Line, Caroline Morley, Adam Showman
Figure caption: Trends in T day, T night, phase amplitudes and phase offsets against irradiation temperature, orbital period, planet’s radius, stellar temperature, and planet’s mass. The color of the data point represents the irradiation temperature of the planet. The best-fit linear relationship between each pair of parameters is plotted in gray. The Pearson correlation coefficient (PCC) for each pair of independent parameters and measured quantities is noted in each panel, and the background color of each panel is scaled with the corresponding Pearson coefficient with the most opaque panel corresponding to a strong correlation. For irradiation temperature and planet masses, we have adjusted the axis limits in to focus on the densest parameter spaces, as such the highly irradiated and massive planets do not appear on the plot.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: The purpose of this plot is to “bound” ﹩{\dot{{M}}}_{{\rm{p}}}﹩ and give a rough order of magnitude of the mass accretion rate of both these protoplanets. We also note from Section 6.2 that these values assume M p b = 4 M Jup and M p c = 2 M Jup and R p = 1.3 R Jup for both b and c. There is also ∼2× uncertainty in these adopted planet parameters, but as is clear from Equation (7), ﹩{\dot{{M}}}_{{\rm{p}}}﹩ varies linearly with R p/M p and so the values in Figure D1 could be off by ∼1–4× due to errors in our planetary mass and radius estimates. Hence, all we can say for certain is that the order of magnitude is ﹩{\dot{{M}}}_{{\rm{p}}}﹩ ∼ 10−13 M Sun yr−1 for both planets, where any of the values between the solid and dotted lines in Figure D1 are possible.
Paper: A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Authors: Lisa Dang, Taylor J. Bell, Ying (Zoe) Shu, Nicolas B. Cowan, Jacob L. Bean, Drake Deming, Eliza M.-R. Kempton, Megan Weiner Mansfield, Emily Rauscher, Vivien Parmentier, Alexandra Rochon, Kevin B. Stevenson, Mark Swain, Laura Kreidberg, Tiffany Kataria, Jean-Michel Désert, Robert Zellem, Jonathan J. Fortney, Nikole K. Lewis, Michael Line, Caroline Morley, Adam Showman
Figure caption: Summary of the analysis of a Spitzer phase curve with SPCA. Top left: example of the raw photometry output from SPCA. Top right: preferred detrended phase curve of WASP-77Ab. Bottom: a comprehensive overview of all SPCA fits of the 4.5 μm full-orbit phase curve of WASP-77Ab. Each subplot displays the best-fit astrophysical model compared to the corrected Spitzer photometry with different detector models. Each column indicates the detector model used where Poly# means a 2D polynomial of order #, PLD Ord# indicates the PLD order, and 3 × 3 or 5 × 5 indicates the pixel stamp size used for PLD. The rows indicate the phase variation model used (sinusoid of order 1 or 2) and whether the detector model also included a linear model with PSF width (σ  x , σ  y ) as inputs. The ΔBIC from the preferred solution of each fit is indicated in each box, and the opacity of the background of each box reflects fit preference (darker is better). The dayside and nightside temperatures inferred from each fit are displayed.
Paper: A Comprehensive Analysis of Spitzer 4.5 μm Phase Curves of Hot Jupiters
Authors: Lisa Dang, Taylor J. Bell, Ying (Zoe) Shu, Nicolas B. Cowan, Jacob L. Bean, Drake Deming, Eliza M.-R. Kempton, Megan Weiner Mansfield, Emily Rauscher, Vivien Parmentier, Alexandra Rochon, Kevin B. Stevenson, Mark Swain, Laura Kreidberg, Tiffany Kataria, Jean-Michel Désert, Robert Zellem, Jonathan J. Fortney, Nikole K. Lewis, Michael Line, Caroline Morley, Adam Showman
Figure caption: Schematic view of second-order effects beyond radiative forcing that could complicate the interpretation of phase curves for close-in exoplanets. These multifactor effects motivate the large sample of phase curves used in this population study, with irradiation temperatures, equilibrium temperatures, and orbital periods shown in the bottom panel. The gray points represent the known hot Jupiter population obtained from the NASA Exoplanet Archive, while the colored points represent our sample targets.