adsabs/AstroCLIMB huggingface dataset:
Paper: FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision
Authors: Thomas C. Abbott, Daniel Amouyal, Bridget C. Andersen, Shion E. Andrew, Kevin Bandura, Mohit Bhardwaj, Kalyani Bhopi, Yash Bhusare, Charanjot Brar, Alice Cai, Tomas Cassanelli, Shami Chatterjee, Jean-François Cliche, Amanda M. Cook, Alice P. Curtin, Evan Davies-Velie, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Nina Gusinskaia, Jason W. T. Hessels, Danté M. Hewitt, Jeff Huang, Naman Jain, Ronniy. C. Joseph, Lordrick Kahinga, Victoria M. Kaspi, Afrasiyab (Afrokk) Khan, Bikash Kharel, Adam E. Lanman, Magnus L'Argent, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Kyle McGregor, Ryan Mckinven, Juan Mena-Parra, Daniele Michilli, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Scott M. Ransom, Gurman Sachdeva, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, David C. Stenning, Haochen Wang, Thomas Boles, Ismaël Cognard, Tammo Jan Dijkema, Alexei V. Filippenko, Marcin P. Gawroński, Wolfgang Herrmann, Charles D. Kilpatrick, Franz Kirsten, Shawn Knabel, Omar S. Ould-Boukattine, Hadrien Paugnat, Weronika Puchalska, William Sheu, Aswin Suresh, Aaron Tohuvavohu, Tommaso Treu, WeiKang Zheng
Figure caption: Multiband radio images of NGC 4141 using the VLA and the uGMRT. The FRB position is indicated by crosshairs, with the 5σ localization ellipse drawn at the center. Contours begin at 3σ and increase by factors of ﹩\sqrt{2}﹩, where σ corresponds to the rms of the residuals. Images are saturated ±5σ. The synthesized beam is indicated in the bottom left of each image by a gray ellipse. Host galaxy emission dominates at low angular resolution and low frequencies, gradually fading as the angular resolution increases.
Paper: FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision
Authors: Thomas C. Abbott, Daniel Amouyal, Bridget C. Andersen, Shion E. Andrew, Kevin Bandura, Mohit Bhardwaj, Kalyani Bhopi, Yash Bhusare, Charanjot Brar, Alice Cai, Tomas Cassanelli, Shami Chatterjee, Jean-François Cliche, Amanda M. Cook, Alice P. Curtin, Evan Davies-Velie, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Nina Gusinskaia, Jason W. T. Hessels, Danté M. Hewitt, Jeff Huang, Naman Jain, Ronniy. C. Joseph, Lordrick Kahinga, Victoria M. Kaspi, Afrasiyab (Afrokk) Khan, Bikash Kharel, Adam E. Lanman, Magnus L'Argent, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Kyle McGregor, Ryan Mckinven, Juan Mena-Parra, Daniele Michilli, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Scott M. Ransom, Gurman Sachdeva, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, David C. Stenning, Haochen Wang, Thomas Boles, Ismaël Cognard, Tammo Jan Dijkema, Alexei V. Filippenko, Marcin P. Gawroński, Wolfgang Herrmann, Charles D. Kilpatrick, Franz Kirsten, Shawn Knabel, Omar S. Ould-Boukattine, Hadrien Paugnat, Weronika Puchalska, William Sheu, Aswin Suresh, Aaron Tohuvavohu, Tommaso Treu, WeiKang Zheng
Figure caption: Best-fit solutions and marginalized errors for the two-screen, two-component model described in the text. Gaussianity in each parameter is consistent with a converged solution with some covariance between parameters indicating that our model is mildly degenerate but mutually constrained.
Paper: FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision
Authors: Thomas C. Abbott, Daniel Amouyal, Bridget C. Andersen, Shion E. Andrew, Kevin Bandura, Mohit Bhardwaj, Kalyani Bhopi, Yash Bhusare, Charanjot Brar, Alice Cai, Tomas Cassanelli, Shami Chatterjee, Jean-François Cliche, Amanda M. Cook, Alice P. Curtin, Evan Davies-Velie, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Nina Gusinskaia, Jason W. T. Hessels, Danté M. Hewitt, Jeff Huang, Naman Jain, Ronniy. C. Joseph, Lordrick Kahinga, Victoria M. Kaspi, Afrasiyab (Afrokk) Khan, Bikash Kharel, Adam E. Lanman, Magnus L'Argent, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Kyle McGregor, Ryan Mckinven, Juan Mena-Parra, Daniele Michilli, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Scott M. Ransom, Gurman Sachdeva, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, David C. Stenning, Haochen Wang, Thomas Boles, Ismaël Cognard, Tammo Jan Dijkema, Alexei V. Filippenko, Marcin P. Gawroński, Wolfgang Herrmann, Charles D. Kilpatrick, Franz Kirsten, Shawn Knabel, Omar S. Ould-Boukattine, Hadrien Paugnat, Weronika Puchalska, William Sheu, Aswin Suresh, Aaron Tohuvavohu, Tommaso Treu, WeiKang Zheng
Figure caption: Comparison of the observed dynamic spectra of FRB 20250316A (left) with the best-fit model (middle) and squared residuals (right).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Results of the injection–recovery analysis with the α Cen AB data. Left column: 2D 5σ flux sensitivity maps for each of the three epochs of observation, and their combined minimum, in sky coordinates (north up, east left). The central region (<0﹩\mathop{.}\limits^{^{\prime\prime} }﹩75, or <1.5 FWHM, radial separations) is masked (poor detectability). The dotted lines correspond to the orientation of the 4QPM transition boundaries (one for each roll in 2025 April). The regions excluded from the injection–recovery analysis in the 2024 August and 2025 February observations due to contamination from α Cen B are labeled. The crosses mark the (ρ, θ) grid points where sensitivity was estimated. A discrete color map is chosen to highlight the different sensitivity zones across the image. Center column: same as the left column but for the S/N = 5 flux sensitivity. Right column: 5σ and S/N = 5 median and minimum flux–contrast curves for each epoch. The median and minimum flux–contrast are both computed over all PAs of injection for a given separation from the 2D sensitivity maps.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Joint PCA-KLIP subtraction of α Cen AB for the 2025 April observations with automatic PC selection. Left column: the de-rotated residual image (north up, east left) after PSF subtraction in three concentric annuli for each roll observation. The MIRI/4QPM transition boundaries are shown as gray shaded regions. Circular apertures are drawn centered on a few visually distinct features in the roll 1 reduction and at the same location in the roll 2 reduction. The features are present in the roll 2 reduction but offset in PA (matching the direction of the V3PA angle change between the two rolls) from their roll 1 location indicating that they are PSF-subtraction artifacts. Right column: S/N map for the reductions shown in the left column. No significant point sources are detected.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Illustrative example of the injection–recovery procedure. Left: the S/N corresponding to a 5σ detection for the radial separations at which synthetic companions are injected. Center: S/N of a synthetic companion injected at a given (example) position as a function of flux. The 5σ and S/N = 5 detection thresholds are marked with horizontal dashed and dashed–dotted lines, respectively. Right: PSF-subtracted images before and after the injection of the model PSF corresponding to a 5σ detection (≈3.5 mJy in this case).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Top panel: the PSF-subtracted image obtained before (left) and after (right) the injection of a negative copy of the best-fit STPSF forward model for S1. The reduction parameters are identical between the two images. The STPSF model injected into the background-subtracted Stage 2 α Cen AB integrations is pictured in the bottom left corner of the right image. The 1.5 FWHM diameter circular aperture where the RSS is minimized is drawn for reference. Bottom panel: marginalized RSS distributions as a function of injected model separation (left), PA (center), and flux (corrected for coronagraph throughput, right). The RSS distributions are well fit by quadratic functions and the minimum corresponds to the forward modeled parameters.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Left: the de-rotated off-axis ϵ Mus reference for α Cen B for the 2024 August observations. It acts as a proxy for and shows the diffraction features expected from α Cen B in vicinity of α Cen A. The locations of the detections of S1 and A1 in 2024 August are marked. Center left: the de-rotated off-axis ϵ Mus reference for α Cen B for the 2025 February observations. The diffraction pattern is nearly identical to that observed in 2024 August. Center right: joint PCA-KLIP reduction of the 2025 February data set with one PC showing the presence of an “A1-like” artifact. Right: joint PCA-KLIP reduction with eight PCs showing that no persistent artifacts are seen at the location of S1 (and A1).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Joint PCA-KLIP subtraction of α Cen AB for the 2025 February observations with automatic PC selection. Left: the de-rotated residual image (north up, east left) after PSF subtraction in three concentric annuli. The MIRI/4QPM transition boundaries are shown as gray shaded regions. Right: S/N map for the reduction shown in the left panel. No significant point sources are detected.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Left: sky motion of S1 (with respect to α Cen A marked with a star symbol), as seen by JWST, assuming it is a stationary background source. The square and triangle symbols mark the expected location of S1 for the 2025 February and April observation dates, respectively. Right: joint PCA-KLIP reductions for the two epochs showing the nondetection of a point source at the expected location for a background object (marked with a cross, top panel). Injection and recovery of a 2.5 mJy STPSF model (bottom panel) confirms the sensitivity of the observations to S1. S1 is not a stationary background object.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Joint PCA-KLIP subtraction of distinct subsets of the α Cen AB science integrations from the 2024 August observations. Reductions performed on the first half, second half, even set, odd set, first frame, and last frame of the integration sequence are shown from top left to bottom right. S1 is consistently detected in all data subsets.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Joint PCA-KLIP reductions for the 2024 August observations where frames at each ϵ Mus dither position are iteratively excluded (one at a time) from the reference library. S1 is detected in all reductions indicating that it is not likely an artifact introduced by the ϵ Mus coronagraphic images.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: PSF-subtracted images (top) and the corresponding extended emission S/N maps (bottom) for the 2025 February observation for three cases: (left) original data, (center) ABA-3 exozodi model injected with a coplanar orientation, and (right) ABA-3 exozodi model injected with an offset orientation. In the image plots, a one FWHM diameter beam is indicated in the bottom left corner with a dotted circle. The aperture that yields the highest S/N (marked by a star in the S/N maps) is shown in the images. For the original data, dotted lines in the S/N map mark the PAs of the 4QPM transition boundaries. For the injected cases, dashed lines mark the PAs of the injected disks.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Same as Figure 21 but for the 2025 April observations. Here, the injected cases shown are the ABA-4 and ABA-3 models, both in the coplanar orientation. In the image showing the original data (top left), a solid circle marks a suspected PSF-subtraction artifact (see the text).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Left column: reduced images showing the recovery of a synthetic STPSF model injected at a separation of 1″ and a PA of 80° in the 2025 February observations. From top to bottom are reductions with a binned reference library, a reference library with all the integrations used and the number of PCs automatically selected, and a reference library with all the integrations used and the number of PCs selected to maximize the S/N of the injected companion, respectively. Right column: same as the left column for injections at a separation of 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩5. Using all the integrations results in a higher S/N recovery of the injected source compared to binning the integrations.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Illustration of how the S/N map is generated for the detection of extended emission. The figure shows an example of a signal region (green) at one PA, along with the corresponding perpendicular annular noise region (purple), using the coplanar asteriod belt analog (ABA) ABA-1 exozodi model injected into the April data. The S/N is calculated by varying the aperture’s PA and length.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: From left to right, joint PCA-KLIP-reduced images for the 2024 August, 2025 February, and 2025 April (roll 1) epoch observations showing the detection of the ∼1 mJy background source KS2 (circled) from P. Kervella et al. (2016).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Left: an “off-the-shelf” Stage 2b F1550C image of the α Cen AB system downloaded from the Mikulski Archive for Space Telescopes (MAST) for the 2024 August observation (no bad-pixel correction). The image is oriented north up and east left. The white stars denote the approximate positions of α Cen B, saturated near the top of the image, and α Cen A in the lower part of the image placed behind the 4QPM. At the edge of the detector, to the west of α Cen A, is a known background source, KS5 (P. Kervella et al. 2016). The color bar is logarithmically scaled in units of MJy sr–1. Right: same as the left image for 2025 February (top) and 2025 April (bottom).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Evolution of S1 and A1 with the number of PCs used in the joint PCA-KLIP subtraction procedure for the 2024 August observations. The left panel corresponds to reductions where joint PCA-KLIP is applied to a single annulus. The right panel corresponds to reductions where joint PCA-KLIP is applied to a single annulus divided into two subsections. Top row: S/N as a function of of the number of PCs for S1 and A1. They are compared to the S/N of the residual speckle noise estimated in one FWHM diameter circular apertures at the same separation as S1 but at different PAs (control region; each semitransparent line corresponds to an aperture at a different PA). Center row: same as the top row but for the aperture-integrated flux as a function of the number of PCs. Bottom row: two representative postprocessed images at PCs marked by stars in the above figures. S1’s signal remains stable across PCs, whereas A1’s signal disappears after a certain number of PCs.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. II. Binary Star Modeling, Planet and Exozodi Search, and Sensitivity Analysis
Authors: Aniket Sanghi, Charles Beichman, Dimitri Mawet, William O. Balmer, Nicolas Godoy, Laurent Pueyo, Anthony Boccaletti, Max Sommer, Alexis Bidot, Elodie Choquet, Pierre Kervella, Pierre-Olivier Lagage, Jarron Leisenring, Jorge Llop-Sayson, Michael Ressler, Kevin Wagner, Mark Wyatt
Figure caption: Results from classical PSF subtraction of α Cen AB for the 2024 August observations. Top panel: the de-rotated residual image (a; north up, east left) and associated S/N map (b) after subtraction of α Cen AB with a linear combination of reference images, using the best-fit c1 and c2 coefficient values. Visually identified point sources, S1 and A1, are circled. The star symbol marks the center of α Cen A. Bottom panel: the left image (c) is the de-rotated α Cen AB science integration before PSF subtraction and the right image (d) is the de-rotated off-axis ϵ Mus reference for α Cen B. The latter acts as a proxy for and shows the diffraction features expected from α Cen B in vicinity of α Cen A. A red circle marks the position of A1, which is colocated with a diffraction feature of α Cen B’s PSF and is likely a residual speckle artifact. A green circle marks the position of S1, which may be associated with an α Cen B diffraction feature but is the only source we confidently redetect in the more robust PCA-KLIP reductions.