adsabs/AstroCLIMB huggingface dataset:
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Top panel: relative RV curves (red) for the Be+sdO binary system HD 113120. The zero orbital phase is defined as the epoch when the Be star reaches superior conjunction in its orbit. The RVs of the Be star measured from the CHIRON Hα profiles are labeled with black dots, and the RVs of the sdO companion star obtained from the prior studies using FUV spectroscopy from IUE (Wang et al. 2018) and HST (Wang et al. 2021) are shown in green and blue, respectively. Systemic velocities for each stellar component obtained from the orbital fits were subtracted from individual measurements for the purposes of this plot. Bottom panel: measured RVs minus the calculated values obtained from the orbital fits. The zero residuals are shown as the red dotted line. The typical error of the measured Be RVs is ∼0.5 km s−1, which is too small to be shown in the figure.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Relative RV curves for the Be binary HD 137387, plotted in the same format as Figure 2. The RVs of the Be star were measured from the He I λ5875 profiles using the cross-correlation technique.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The He I λ5875 profile observed on the night of HJD 2,458,496 (black) and the coadded mean spectrum (green) for HD 137387. The relative RV (2.2 ± 3.3 km s−1; shown as the tick mark) was measured from the peak position of the CCF that was calculated by cross-correlating the observed spectrum with the mean spectrum of all 46 observations.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The Hα profile observed on the night of HJD 2,458,536 for HD 152478. The RV measured from the broad wings using the bisector technique is shown as the tick mark.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Relative RV curve (red) for the Be star HD 157832 from the Hα measurements (black) shown in the same format as Figure 2.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Relative RV curves for the Be binary HD 152478, plotted in the same format as Figure 2. The RVs of the Be star were measured from the Hα profiles using the bisector technique. The sdO RVs are collected from prior studies by Wang et al. (2018, 2021).
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The Hα profile of HD 157832 observed on the night of HJD 2,458,541. The RV measured from the broad wings using the bisector technique is shown as the tick mark.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The Hα profile of HD 157042 observed on the night of HJD 2,458,538. The RV measured from the broad wings using the bisector technique is shown as the tick mark.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Relative RV curves for HD 157042 in the same format as Figure 2.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Spectra of the sdO components from Doppler tomography reconstructions of the CHIRON spectroscopy (solid lines) that were made using the preliminary double-lined orbital velocity solutions. There is no double-lined orbit for HD 157832, so we assumed a reflex motion of the companion for a mass ratio of M 2/M 1 = 0.1 and then plotted the reconstructed spectrum for a supposed flux contribution of f 2/(f 1 + f 2) = 0.018. The TLUSTY model spectra predicted from analysis of the HST ultraviolet spectra (Wang et al. 2021) are overplotted as dotted lines. The reconstructed and model spectra are shown with vertical offsets of 0.04, 0.03, 0.02, and 0.01 for HD 113120, HD 137387, HD 152478, and HD 157042, respectively, for ease of comparison. The reconstructed spectra reveal the presence of the expected He II λ4686 line in all but the case of HD 157832.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The Hα profiles that were omitted in the orbital fit for HD 157832. The RVs measured from the seven spectra displayed a significant deviation from the derived orbital fit, and these spectra showed a steep drop in intensity in the blue wing of the peak profile. These include observations made on the nights of HJD 2,458,635 (green), HJD 2,458,637 (brown), HJD 2,458,638 (red), HJD 2,458,650 (cyan), HJD 2,458,653 (magenta), HJD 2,458,664 (orange), and HJD 2,458,667 (blue). The spectrum observed on the night of HJD 2,458,625 with a measured RV in accord with the orbital solution is plotted in black for comparison.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: (a) Hα variations of HD 152478. The red peak dominated at the beginning of the observing campaign (black; HJD 2,458,536). The profile gradually decreased in strength (green, HJD 2,458,916; blue, HJD 2,459,294). The red and violet emission peaks reached a comparable and lower strength toward the end of the observations (red; HJD 2,459,416). (b) Temporal evolution of the Hα equivalent width (integrated over 6552–6577 Å).
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Left: Hα profiles of HD 157832 plotted as a function of the orbital phase and Doppler shift. The continuum of each profile is aligned with the orbital phase in the top panel, and the flux scale relative to the continuum is indicated by the vertical bar in the upper right corner. A gray-scale version of the profiles appears in the bottom panel, in which the brightness scales with emission flux above the continuum. The arrows indicating the orbital phases of the observations are marked along the right ordinate. Right: Hβ profiles plotted in the same format as the left panel but for different flux scaling.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The RV curves of HD 113120 for Hβ (panel (a)), Fe II λ5276, 5316 (panel (b); all line features were measured together in the same echelle spectral order using the CCF approach), Fe II λ λ 5316, 5362 (panel (c); all line features were measured together in the same echelle spectral order), and Fe II λ8451 (panel (d)), plotted for phases from the ephemeris reported in Table 3.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Emission profile variations of HD 113120 for Hα (left) and Hβ (right). This subsample is arranged with vertical offsets that increase with time.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: (a) The Hα profiles of HD 157042 displayed a gradual weakening throughout the observing campaign. Observations made on the nights of HJD 2,458,538, 2,458,716, 2,458,909, and 2,459,414 are plotted in black, green, blue, and red, respectively. (b) Temporal variations of the Hα equivalent width (integrated over the range 6551–6574 Å).
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The Hα variations of HD 137387. Panel (a) shows the growth of new emission on short and long timescales with offsets of +0.3 and +0.6 in normalized flux. Panel (b) shows the time evolution of the equivalent width W  λ  (summed over the wavelength range from 6552 to 6578 Å).
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Measured RVs from the Hα profiles of HD 113120. Long-term variations resulted in shifts appearing in the measured RVs obtained after HJD 2,458,800 (black). Corrected RVs are shown in blue.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The RV plots of the Be star HD 157832 measured from He I and metallic lines, plotted from the ephemeris reported in Table 7. The relative RVs of these profiles were determined from the peak location of the calculated CCFs of observed spectra with the coadded mean spectrum of the associated profile, except in the case of the Fe II λ6456 and Ca II λ λ8542, 8600 profiles, in which the RVs were measured from the CCF wings using the bisector technique. Panel (a): RVs for He I λ4921 (black). Velocities were measured for both the He I λ5015 and Fe II λ5020 profiles together in the same echelle spectral order (blue). Panel (b): RVs for Fe II λ5197 (black), λ5234 (blue), λ λ5276, 5284 (green), and λ6456 (purple). Panel (c): RVs for O I λ8446. Panel (d): RVs for Ca II λ λ8542, 8600.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: The RV curves from Hβ for the Be binary systems HD 152478 (panel (a)), HD 157042 (panel (b)), and HD 157832 (panel (c)). The relative RVs of the Be stars HD 152478 and HD 157042 were determined from the peak locations of the CCFs constructed by cross-correlating the observed spectra with the coadded mean Hβ profile. Alternatively, the absolute Hβ velocities of HD 157832 were measured directly from the wings using the bisector technique from Shafter et al. (1986). The phases are obtained from the ephemeris reported in Table 5 for HD 152478 (Table 6 for HD 157042 and Table 7 for HD 157832).
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Time plot of W  λ  for Hβ (panel (a)), He I (panel (b)), and Ca II λ8542 (panel (c)) for HD 137387. Measured W  λ  values for He I λ4921 (black), λ5015 (green), λ5875 (blue), λ6678 (red), and λ7065 (cyan) are shown in panel (b).
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Time plot of W  λ  measured for Hα (panel (a)), Hβ (panel (b)), He I λ6678 (panel (c)), and He I λ7065 (panel (d)) for HD 113120.
Paper: Confirmation of Color-dependent Centroid Shift Measured After 1.8 Years with HST
Authors: Aparna Bhattacharya, David P. Bennett, Jean Philippe Beaulieu, Ian A. Bond, Naoki Koshimoto, Jessica R. Lu, Joshua W. Blackman, Clément Ranc, Aikaterini Vandorou, Sean K. Terry, Jean Baptiste Marquette, Andrew A. Cole, Akihiko Fukui
Figure caption: Panel (A): A 3″ section of the stack image of 16 Keck K-band images, taken with the narrow camera, with the yellow square indicating the target. Panel (B): A close-up of the target object. The source and lens positions are obtained from the best fit dual star PSF model. Panel (C): The residual image after subtracting the best fit single star PSF model. The residual shows a clear indication of the presence of an additional star East of the target. Panel (D): The residual image after subtracting the best fit dual star PSF model. This shows a smooth residual, confirming the second star at separation of ∼54 mas. (C) and (D) use the same photometry scale.
Paper: Confirmation of Color-dependent Centroid Shift Measured After 1.8 Years with HST
Authors: Aparna Bhattacharya, David P. Bennett, Jean Philippe Beaulieu, Ian A. Bond, Naoki Koshimoto, Jessica R. Lu, Joshua W. Blackman, Clément Ranc, Aikaterini Vandorou, Sean K. Terry, Jean Baptiste Marquette, Andrew A. Cole, Akihiko Fukui
Figure caption: The Bayesian posterior probability distributions for the planetary companion mass, host mass, their separation, and the distance to the lens system are shown with the light-curve + HST constraints in blue (based on Bennett et al. 2006) and the constraints from our Keck follow-up observations in red. The central 68.3% of the distributions are shaded in darker colors (dark red and dark blue) and the remaining central 95.4% of the distributions are shaded in lighter colors. The vertical black line marks the median of the probability distribution of the respective parameters. The older results are smoother because they assume Gaussian uncertainties on the microlens model parameters, while new results include the full parameter distributions from the MCMC. This comparison shows the consistency of the 2018 mass measurement results from Keck to the 2005 mass measurement results with HST centroid shift measurements.
Paper: To Be or Not to Be: Alicante-8, a Cluster or Not?
Authors: Randa Asa'd, V. D. Ivanov, I. Negueruela, J. M John, A. Gonneau, M. Rejkuba
Figure caption: VLT/X-shooter J-band spectra of the targets analyzed in this work. Numbers as in Negueruela et al. (2010).
Paper: To Be or Not to Be: Alicante-8, a Cluster or Not?
Authors: Randa Asa'd, V. D. Ivanov, I. Negueruela, J. M John, A. Gonneau, M. Rejkuba
Figure caption: VLT/X-shooter H-band spectra of the targets analyzed in this work. Numbers as in Negueruela et al. (2010).
Paper: To Be or Not to Be: Alicante-8, a Cluster or Not?
Authors: Randa Asa'd, V. D. Ivanov, I. Negueruela, J. M John, A. Gonneau, M. Rejkuba
Figure caption: Proper motions of stars in a ﹩3^{\prime} ﹩ circle around the nominal center of Alicante-8. Stars S1–S8 are marked as large orange circles. The blue circles represent objects with redder than typical colors (see text for details), i.e., the population to which the candidate members must be compared. We note that they are more tightly concentrated than the general population, but our objects are clearly divergent.
Paper: To Be or Not to Be: Alicante-8, a Cluster or Not?
Authors: Randa Asa'd, V. D. Ivanov, I. Negueruela, J. M John, A. Gonneau, M. Rejkuba
Figure caption: Luminosity classification of the targets in the field of Alicante-8 (red dots). RSGs, RGB stars, and asymptotic giant branch (AGB) stars from the sample of Rayner et al. (2009) are shown. The dotted lines indicate the borders of the RSG loci, defined by Messineo et al. (2021). The spectral indices used on the axes are shown in Figures 2–4. See text for more details.
Paper: To Be or Not to Be: Alicante-8, a Cluster or Not?
Authors: Randa Asa'd, V. D. Ivanov, I. Negueruela, J. M John, A. Gonneau, M. Rejkuba
Figure caption: Two Micron All Sky Survey (2MASS) K S-band finding chart for the Alicante-8 candidate member stars from Negueruela et al. (2010). It is a linearly scaled 2MASS K S-band image with a field of view of ∼7′ × 7′, centered at (R.A., decl.) ∼ (18:34:50, −07:13:30). North is up and east is left.
Paper: To Be or Not to Be: Alicante-8, a Cluster or Not?
Authors: Randa Asa'd, V. D. Ivanov, I. Negueruela, J. M John, A. Gonneau, M. Rejkuba
Figure caption: VLT/X-shooter K-band spectra of the targets analyzed in this work. Numbers as in Negueruela et al. (2010).
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The two complementary decompositions of a hypothetical data matrix with one column for each frame. The matrix can be decomposed into left singular vectors, shown here as v 1, v 2,…,v  n , or into right singular vectors as u 1,…,u  n . An interpretation of the left singular vectors, with the same number of entries as a single vector of pixels from an image, as eigenimages of the pixel-to-pixel covariance, is shown in the lower left. An analogous interpretation for the right singular vectors is as eigen time series from which each pixel’s time series can be composed, as shown on the right.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Single example frame after background subtraction, scaled to show structure. Bad pixels are cyan, the science PSFs and the cold stop diffraction spikes are outlined in blue, negative artifacts from amplifier crosstalk at a predictable separation from the star are shown in green, and other stray light artifacts that can move over the course of the observation are highlighted in orange. (Adapted from Long et al. 2018.)
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Radial profiles of the “top” (upper) and “bottom” (lower) vAPP PSFs (see Figure 3) taken from median-combined data of Sirius and o Gruis, normalized to 1.0 at ρ = 0″. The o Gruis data allowed us to estimate the brightness of Sirius by fitting the wings of the PSF, and were used as an unsaturated PSF template when injecting fake planets.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The first row shows the “top” vAPP median PSF, with saturated Sirius data on the left and o Gruis data on the right. The second row shows the “bottom” PSFs. They have been scaled to relative units such that the peak of the unsaturated data is 1.0, and the saturated data are scaled to match the radial profiles in the unsaturated regions (see Figure 2).
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Behavior of optimized median S/N = 5 contrast at each radius value with increasing number of optimization iterations, comparing PCAT to our implementation of KLIP. Both algorithms were optimized using the same Bayesian optimization procedure, with the median S/N = 5 contrast shown after 10 iterations as a dotted line, after 100 as a dashed line, and after 200 as a solid line.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Median S/N = 5 contrast vs. separation for three different levels of coadding. Within 4 λ/D, the median contrast degrades with temporal downsampling by coadding. This relationship turns over, and by 5 λ/D the 10:1 downsampled data cube actually provides better contrast.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Median S/N = 5 contrast vs. separation shown at 10, 20, 30, 40, 50, 100, and 200 iterations of hyperparameter exploration by the Bayesian optimization algorithm. The Bayesian optimization procedure rapidly converges to near-optimal parameters.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: Correspondence of [3.95] absolute magnitudes to masses assuming A  B  = 0.5. Main panel: the relationship between magnitude and mass is plotted at an age of 242 Myr and several different equilibrium temperatures to illustrate its dependence on T eq. The T eq = 685 K line corresponds to the relationship at the smallest separation probed at the IWA. The dashed line indicates the median absolute-magnitude value of the contrast floor across all focal plane locations. The apparent discontinuity around 12 M J is where the relationship becomes double valued as deuterium burning begins, and we take the lower value of the two. Lower panel: histogram of S/N = 5 detection levels reached at the probe locations shown in Figure 9 in 0.25 mag bins. Right panel: histogram of probe locations reaching particular mass sensitivity limits in 1 M J bins.
Paper: Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
Authors: Joseph D. Long, Jared R. Males, Sebastiaan Y. Haffert, Logan Pearce, Mark S. Marley, Katie M. Morzinski, Laird M. Close, Gilles P. P. L. Otten, Frans Snik, Matthew A. Kenworthy, Christoph U. Keller, Philip Hinz, John D. Monnier, Alycia Weinberger, Volker Tolls
Figure caption: The pattern of saturated pixels in each complementary half of the gvAPP-180 PSF, combined with the field rotation, leads to a varying number of frames from the original science data contributing to the value of each final pixel. This picture shows the result of rotating the data masks (set to 1.0 where data are kept) and summing along the time axis to visualize this effect. The overlaid points represent locations at which we injected and recovered a planet signal to calibrate our contrast limits.