adsabs/AstroCLIMB huggingface dataset:
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Comparison of predicted sky brightness at 5000 Å, ﹩{I}_{\mathrm{sky}}^{5000{\rm{A}}}﹩, of the bright-time sky brightness model vs. the observed ﹩{I}_{\mathrm{sky}}^{5000{\rm{A}}}﹩ for a test set of observations. The bright-time sky brightness model is trained using ridge regression on ﹩{I}_{\mathrm{sky}}^{5000{\rm{A}}}﹩ compiled from the exposures in Figure 21. The bright-time sky brightness model shows overall good agreement with observations and, therefore, accurately estimates the sky brightness during bright time.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The distribution of air mass and lunar conditions (illumination, altitude, separation) of DESI SV1 (blue), DESI commissioning (CMX; orange), and BOSS (green) sky spectra used to construct the empirical bright-time sky brightness model. The exposures enable us to construct a model that predicts sky brightness given air mass, Moon illumination, altitude, and separation as input.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: A representative set of contrast curves for a single data set demonstrating the methodology used to choose a “data quality cut”. The colored curves reflect the contrast achieved after discarding varying proportions of the lowest-quality images. In this case, the curves converge after ∼0.″2, but the achieved contrast inside of this radius varies with the proportion of data discarded. Inset images are S/N maps showing three planets injected into raw images at separations of 0.″12, 0.″17, and 0.″22 with no data discarded (top, 0% cut) and with the selected optimal amount of data discarded (bottom, 70% cut). Recovery of the innermost two planets is markedly improved in the lower plot, increasing their recovered S/Ns by ∼2. The outer planet is recovered at equivalent S/N in both reductions, reflective of the converging of the contrast curves at this separation.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Median combinations of the images in each GAPlanetS image sequence, normalized to 1 by dividing by the peak pixel and arranged from brightest to faintest r’ band magnitude. The extreme variability in the PSF between objects and among images of the same object acquired on different nights is apparent in the variable size of the PSFs. The VisAO PSF is highly dependent on weather conditions.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for all HD 169142 epochs. pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle. The locations of candidate companions from previous work are indicated with dashed cyan circles at the literature detection epoch listed in Table 4 (“O07,” Okamoto et al. 2017; “O12–13,” Osorio et al. 2014; “R13,” Reggiani et al. 2014; “B13” and “B14,” Biller et al. 2014; “G15-17A,” “G15-18B,” “G15-18C,” and “G15-18D,” Gratton et al. 2019; “B18,” Bertrang et al. 2020). Yellow “x” symbols indicate locations where apparent companions are introduced into SDI imagery through subtraction of a negative continuum speckle. The most compelling 3σ–4σ point-source candidates are indicated with yellow circles, though there are reasons to be skeptical of each, as detailed in the text.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: KLIP reductions of the H-alpha (left) and continuum (middle left) images for all HD 142527 epochs. KLIP parameters were optimized with pyKLIP-PE based on the recovered signal of false planets injected into the continuum images. The middle right panel shows a conservative SDI reduction created by multiplying the continuum KLIP image by the median Hα/continuum scale factor for the primary star (reported in table 2) and subtracting it from Hα imagery, which should effectively remove scattered light emission and continuum artifacts. The rightmost panel shows the unscaled Hα – continuum reduction, which is most appropriate in regions where no scattered light artifacts are present. The lack of a resolved inner disk component in HD 142527 makes scattered light from circumstellar material of minimal concern; however, there may be some contribution to these signals from a circumsecondary disk.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Post-processed GAPlanetS images for all PDS 70 epochs. KLIP parameters were optimized to maximize the average S/N metric at the locations of the PDS 70 b and c planets in Hα (left-hand panel). Although S/Ns are low at Hα, the parameters selected result in recovery of PDS 70 c in SDI imagery in all three epochs and recovery of PDS 70 b in the 2018 May 3 epoch. The cyan circle labeled “Z20d” marks the location of a third point-source candidate in this system from Zurlo et al. (2020). The cyan “WiPb” and “WiPc” circles mark the predicted location of the planet at the precise epoch of our observations, computed from Wang et al. (2021a). The yellow ellipse marks the inner edge of the known scattered light cavity in this system.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Throughput-corrected 5σ contrast curves of all epochs for continuum false planet optimized pyKLIP reductions of the three previously reported GAPlanetS companion and companion candidate-hosts: HD 142527 (seven epochs), PDS 70 (three epochs), and LkCa 15 (two epochs). Throughput was computed as described in the text, with a correction for the small number of independent noise samples near the star following Mawet et al. (2014). Solid curves indicate regions where throughput-corrected contrast was computed directly. The curves are also projected inward from the innermost throughput measurement to the inner working angle, and this extrapolated region is indicated with a dashed line.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Post-processed GAPlanetS images for all PDS 70 epochs. KLIP parameters were optimized for false planets injected into the continuum channel, resulting in marginal (S/N ∼ 3) recoveries of PDS 70 c in 2017 and on 2018 May 2, but a nonrecovery of PDS 70 b in all epochs. The cyan “WiPb” and “WiPc” circles mark the predicted location of the planet at the precise epoch of our observations, computed using Wang et al. (2021a). The cyan circle labeled “Z20d” marks the location of a third point-source candidate from Zurlo et al. (2020). The yellow ellipse marks the inner edge of the known scattered light cavity in this system.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: KLIP reductions of both LkCa 15 epochs, with parameters optimized by equally weighting all six post-processed image quality metrics across 5 and 20 KL modes for the single false planet injected into the continuum images inside of the control radius (at separation = 0.″1, PA = 0). The locations of candidate companions from the literature are indicated with cyan circles (“S14b,” “S14c,” “S14d,” Sallum et al. 2015; “S16b,” “S16c,” “S16d,” Sallum et al. 2016). The yellow “x” marks a strong negative speckle just outside the control radius in the continuum images, which appears bright in SDI imagery.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Throughput-corrected 5σ contrast curves of all epochs for continuum false planet optimized pyKLIP reductions of the three GAPlanetS targets with reported close (<0.″5) companion candidates in the literature: HD 100546 (two epochs), HD 169142 (four epochs) and SAO 206462 (two epochs). Throughput was computed as described in the text, with a correction for the small number of independent noise samples near the star following Mawet et al. (2014). Solid curves indicate regions where throughput-corrected contrast was computed directly. The curves are also projected inward from the innermost throughput measurement to the inner working angle, and this extrapolated region is indicated with a dashed line.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: The same as Figure 7, except for the most difficult HD 142527 B detection epochs. Here, KLIP parameters have been optimized on the known location of the companion in the Hα images (cyan circle labeled “B”; Balmer et al. 2022), resulting in a recovery of the companion in the 2018 data, but nonrecovery in 2017. The yellow “x” marks a strong negative continuum speckle.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for the single GAPlanetS CS cha epoch. The new candidate companion, CS Cha “c” is apparent to the east of the star in Hα and SDI imagery.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for all three HD 100453 epochs. pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle. The companion HD 100453 B, is clearly visible in the lower left of each image panel, and its locations from Wagner et al. (2018b) and Gonzalez et al. (2020) are marked with cyan circles labeled “W17” and “G19,” respectively. A known background star lies in the upper left-hand corner of each Hα and Continuum image (except in the 2018 May 2 epoch, when it is saturated and therefore not completely removed through SDI subtraction), but is absent in the SDI imagery because it is not actively accreting .
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Wide-field and narrow-field views of the 1:1 scaled ASDI reduction from the highest-contrast epoch for all three GAPlanetS targets with known wide companions (CS Cha B, HD 100453 B) and companion candidates (TW Hya). No clear Hα excess signal is present at the location of the wide TW Hya candidate(s) reported in Ilee et al. (2022; “I16”) or Tsukagoshi et al. (2019; “T17”), nor is it apparent from the known, highly embedded CS Cha B companion (“G17,” Ginski et al. 2018). Hα excess is, however, apparent from the HD 100453 B companion at a location consistent with its reported position in 2019 (Gonzalez et al. 2020; “G19”).
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right) and 1:1 scaled ASDI (right) imagery for both HD 100546 epochs. pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle. The Currie et al. (2015) and Quanz et al. (2013) planet candidate locations at the original detection epochs are marked with dashed cyan circles labeled “C15” and “Q11,” respectively
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for both SAO 206462 epochs. pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle. The Cugno et al. (2019) and Casassus et al. (2021) planet candidate locations at the original detection epoch are marked with dashed dashed cyan circles labeled “C16” and “C19,” respectively.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Throughput-corrected 5σ contrast curves for continuum false planet optimized pyKLIP reductions of all epochs for the four GAPlanetS targets without reported companion candidates in the literature: HD 141569 (five epochs), UX Tau A (one epoch), V4046 Sgr (two epochs), V1247 Ori (two epochs), and PDS 66 (one epoch). Throughput was computed as described in the text, with a correction for the small number of independent noise samples present near the star implemented following Mawet et al. (2014). Solid curves indicate regions where throughput-corrected contrast was computed directly. The curves are also projected inward from the innermost throughput measurement to the inner working angle, and this extrapolation region is indicated with a dashed line.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for both TW Hya epochs. pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle. The Huélamo et al. (2022) point-source candidate (a suspected artifact according to the authors) is marked with a dashed cyan circle labeled “H19.”