adsabs/AstroCLIMB huggingface dataset:
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: A sample fringe fit of J0117+8928 phase-calibrated by J054236.1+495107 to extract the nondispersive residual delay arising from an incorrect baseline vector. Left: log-likelihood vs. differential ionosphere density ΔTEC and delay τ, normalized to its maximum value and with color scale saturated to ±5σ. Right: cross-correlation visibility phases with Y × Y polarization in open red circles and X × X in open blue triangles. We apply τ and ΔTEC corrections corresponding to the maximum likelihood to the phase and plot the original fit and the residuals.
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: SEFD of each input. Color indicates a specific input number. Inputs 0–63 are all X polarization, and 64–127 are Y polarization. The solid black line shows the median over inputs within each polarization. The dashed black line marks the SEFD of beamformed baseband data.
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: Amplitude and phase of the gain for a single input on several days. These are all computed from Cygnus A transits. The persistent RFI mask (see Section 3.2) was applied to the data starting on 2023 June 7, with the effect of removing some of the noisier structure visible on 2023 June 6. Gains are largely stable over many weeks.
Paper: CHIME/FRB Outriggers: KKO Station System and Commissioning Results
Authors: Adam E. Lanman, Shion Andrew, Mattias Lazda, Vishwangi Shah, Mandana Amiri, Arvind Balasubramanian, Kevin Bandura, P. J. Boyle, Charanjot Brar, Mark Carlson, Jean-François Cliche, Nina Gusinskaia, Ian T. Hendricksen, J. F. Kaczmarek, Tom Landecker, Calvin Leung, Ryan Mckinven, Juan Mena-Parra, Nikola Milutinovic, Kenzie Nimmo, Aaron B. Pearlman, Andre Renard, Mubdi Rahman, J. Richard Shaw, Seth R. Siegel, Rick J. Smegal, Tomas Cassanelli, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Mark Halpern, Hans Hopkins, Victoria M. Kaspi, Kholoud Khairy, Kiyoshi W. Masui, Bradley W. Meyers, Daniele Michilli, Emily Petroff, Tristan Pinsonneault-Marotte, Ziggy Pleunis, Masoud Rafiei-Ravandi, Kaitlyn Shin, Kendrick Smith, Keith Vanderlinde, Tarik J. Zegmott
Figure caption: North–south position of the dual-polarization feeds. The top panel shows the north–south position of the feeds as a function of feed number. The first 64 feeds are the Y-polarization feeds, and the next 64 feeds are the X-polarization feeds. The bottom panel shows the residual when the measured position is compared to the design position.
Paper: SCExAO/CHARIS Multiwavelength High-contrast Imaging of the BD+45°598 Debris Disk
Authors: Maria Vincent, Kellen Lawson, Thayne Currie, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Vincent Deo, Sébastien Vievard
Figure caption: Corner plot showing the optimization of the disk model to the ADI-ALOCI result. The star and triangle symbols show the best model DE converged at in the off-diagonal and diagonal panels respectively. The diagonal panels show the solution as a function of ﹩{\chi }_{\nu }^{2}﹩. The off-diagonal panels display the solutions as a function of two of the parameters. Each point in the subplots represents a single sample, colored according to its ﹩{\chi }_{\nu }^{2}﹩ score that ranges from ﹩{\chi }_{\nu ,{\min }}^{2}﹩ to ﹩{\chi }_{\nu ,{\min }}^{2}+10\cdot \sqrt{2/\nu }﹩. The dotted black line in the diagonal panels mark the threshold for acceptable solutions.
Paper: SCExAO/CHARIS Multiwavelength High-contrast Imaging of the BD+45°598 Debris Disk
Authors: Maria Vincent, Kellen Lawson, Thayne Currie, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Vincent Deo, Sébastien Vievard
Figure caption: Range of values for minimum grain size assuming a grain composition of standard astronomical silicates derived using agglomerated debris particle calculations from Arnold et al. (2022). The solid lines correspond to the variation of disk color as a function of minimum grain size derived from the input models, and the markers (with error bars) are the minimum grain size values derived from the disk color measured in the data corrected for self subtraction. The gray line marks the blowout size for the star, which is approximately 0.45 μm.
Paper: SCExAO/CHARIS Multiwavelength High-contrast Imaging of the BD+45°598 Debris Disk
Authors: Maria Vincent, Kellen Lawson, Thayne Currie, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Vincent Deo, Sébastien Vievard
Figure caption: The disk intensity relative to the stellar flux as a function of wavelength for radii ≥0.″7. The orange line shows the measured spectrum and the maroon line shows the best fit scattered-light model prior to PSF convolution and forward modeling. In the models used here, the disk geometry is kept fixed, while the disk brightness varies as function of wavelength. The blue line shows the model after passing through the same image processing steps as applied to the data.
Paper: SCExAO/CHARIS Multiwavelength High-contrast Imaging of the BD+45°598 Debris Disk
Authors: Maria Vincent, Kellen Lawson, Thayne Currie, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Vincent Deo, Sébastien Vievard
Figure caption: The disk intensity relative to the stellar flux as a function of wavelength for radii 0.″7 to 1.″0. In the models used here, the disk geometry is kept fixed, while the disk brightness varies as function of radius. The disk brightness from the data plotted here has been corrected for self subtraction, and is measured in apertures of width 0.″05, starting from 0.″7 as indicated by the x-coordinate of the data points, and height 0.″05.
Paper: SCExAO/CHARIS Multiwavelength High-contrast Imaging of the BD+45°598 Debris Disk
Authors: Maria Vincent, Kellen Lawson, Thayne Currie, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Vincent Deo, Sébastien Vievard
Figure caption: Corner plot showing the optimization of the disk model to the ADI-ALOCI result of the slices of the image cube corresponding to λ = 1.93, 2.0, and 2.07 μm.
Paper: SCExAO/CHARIS Multiwavelength High-contrast Imaging of the BD+45°598 Debris Disk
Authors: Maria Vincent, Kellen Lawson, Thayne Currie, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Vincent Deo, Sébastien Vievard
Figure caption: The contrast curve curve for point sources at different wavelengths. The 5σ limit on the intensity relative to the central star is plotted as a function of the stellocentric angular separation in arcseconds and stellocentric separation in au.
Paper: SCExAO/CHARIS Multiwavelength High-contrast Imaging of the BD+45°598 Debris Disk
Authors: Maria Vincent, Kellen Lawson, Thayne Currie, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Vincent Deo, Sébastien Vievard
Figure caption: Top: comparison of surface brightness the east and west sides of the disk spine. The east side is brighter than the west. Bottom: ratio of the east and west sides, which ascertains that there is no notable brightness asymmetry in the disk.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Removal of the background flux in NIRSpec rate maps, in particular the diffuse background created by charge transfer from the very highly saturated stellar PSF core. This illustrates a single column of the NRS1 detector (index 300 of jw01414004001_02101_00001_nrs1_rate.fits). The region of the detector corresponding to illuminated IFU slice data is masked. The spline continuum model (“Best-fit model”) is fit to the “Background pixels” only and then subtracted from the data (“Corrected data”). Note the two panels above show the same data but with the Y-axis ranges different by a factor of 100×. The resulting image is shown in Figure 24.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Modeling the correlation of the noise for the RDI spectrum of HD 19467 B shown in Figure 3. Left: empirical correlation profile in black and model fit to this profile in orange. Middle: double Gaussian model for the correlated component of the empirical profile. Right: model for the uncorrelated noise component, which is only nonzero in the first two pixels; note the scaling on the x-axis.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Proof of concept for the atmospheric characterization of HD 19467 B using the detector FM and an RDI-based prior on the speckle fluxes. We use the BT-Settl model grid (Allard et al. 2003). (Left) Natural logarithm of the marginalized posterior of the effective temperature and surface gravity for a single dither position. (Right) Best-fit effective temperature for each detector image and each dither position in the observing sequence.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: NIRSpec IFU rate map before and after background subtraction for jw01414004001_02101_00001_nrs1_rate.fits. Both vertical striping from 1/f noise and the diffuse signal excess extending away from the very saturated stellar PSF core are effectively removed.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: RDI prior for the speckle intensity in different rows of the NIRSpec detector. Each panel is similar to the top panel of Figure 11, but the 1σ speckle intensity prior is represented as the shaded gray region. The row numbers match those in Figure 10. Only rows intersecting the companion trace on the detector were chosen to highlight the deviations of the continuum caused by the companion signal.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Best-fit BT-Settl model (Allard et al. 2003) derived from the FM with RDI priors (FM+RDI) compared to the RDI-extracted spectrum. The model was fitted directly to the detector images (NRS1 and NRS2 separately) so the difference between the model and the RDI spectrum is not the residuals of a fit.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Revised companion detection sensitivity of the NIRCam coronographic data originally presented in Greenbaum et al. (2023). The 5σdetection limits are defined in terms of the companion-to-star flux ratio in different NIRCam photometric filters. The crosses indicate the flux ratio of HD 19467 B in the various filters.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Radial velocity measurements of HD 19467 B for individual exposures. At the time of writing, systematics in the NIRSpec wavelength solution has not been characterized or calibrated at this level of precision, which could explain the discrepancy between the NRS1 and NRS2 detectors.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Simulated companion injection and recovery test for the FM in Section 4. The recovered fluxes are consistent with the original simulated companion showing no significant signs of self or oversubtraction in the algorithm.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Definition of the model covariance. Top: large-scale 2D correlation model (﹩{{\rm{\Psi }}}_{\mathrm{large},{l}_{2}-{l}_{1}}﹩) and the outer product of the large-scale errors (﹩{\sigma }_{\mathrm{large},{l}_{1}}{\sigma }_{\mathrm{large},{l}_{2}}﹩). Bottom: small-scale 2D correlation model (﹩{{\rm{\Psi }}}_{\mathrm{small},{l}_{2}-{l}_{1}}﹩) and outer product of the small-scale errors (﹩{\sigma }_{\mathrm{small},{l}_{1}}{\sigma }_{\mathrm{small},{l}_{2}}﹩). The small-scale correlation matrix only shows a 50 x 50 pixel area so that the fine structure along the diagonal is visible. The final covariance is shown in Figure 28.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Final covariance matrix and its inverse. The logarithmic scale is used on the left to show fine structure but cannot used on the right due to negative values in the inverse. The code to generate these matrices is available in the Github repository dedicated to this work.
Paper: JWST-TST High Contrast: Achieving Direct Spectroscopy of Faint Substellar Companions Next to Bright Stars with the NIRSpec Integral Field Unit
Authors: Jean-Baptiste Ruffio, Marshall D. Perrin, Kielan K. W. Hoch, Jens Kammerer, Quinn M. Konopacky, Laurent Pueyo, Alex Madurowicz, Emily Rickman, Christopher A. Theissen, Shubh Agrawal, Alexandra Z. Greenbaum, Brittany E. Miles, Travis S. Barman, William O. Balmer, Jorge Llop-Sayson, Julien H. Girard, Isabel Rebollido, Rémi Soummer, Natalie H. Allen, Jay Anderson, Charles A. Beichman, Andrea Bellini, Geoffrey Bryden, Néstor Espinoza, Ana Glidden, Jingcheng Huang, Nikole K. Lewis, Mattia Libralato, Dana R. Louie, Sangmo Tony Sohn, Sara Seager, Roeland P. van der Marel, Hannah R. Wakeford, Laura L. Watkins, Marie Ygouf, C. Matt Mountain
Figure caption: Visual verification of the model covariance. Left: 10 examples of residual speckle spectra used to calculate the empirical profile of the correlation. Right: samples of residual speckles generated by querying the model covariance matrix for comparison.
Paper: SuperBIT Superpressure Flight Instrument Overview and Performance: Near-diffraction-limited Astronomical Imaging from the Stratosphere
Authors: Ajay S. Gill, Steven J. Benton, Christopher J. Damaren, Spencer W. Everett, Aurelien A. Fraisse, John W. Hartley, David Harvey, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Richard Massey, Jacqueline E. McCleary, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, L. Javier Romualdez, Jürgen Schmoll, Mohamed M. Shaaban, Ellen L. Sirks, Georgios N. Vassilakis, André Z. Vitorelli
Figure caption: The PSF FWHM distribution for different bands from the galaxy cluster images. The PSF was modeled using the PSFEx modeling software (Bertin 2011).