adsabs/AstroCLIMB huggingface dataset:
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: For illustration, we show the PSF of a star from a blue-band galaxy cluster image, highlighting imaging quality near the diffraction limit.
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: Absolute QE curve of the SuperBIT sensor, the Sony IMX-455 BSI CMOS sensor (around the QHY600 camera). The QE of the SuperBIT camera (KAI-29052) during the 2019 engineering flight is also shown. The IMX-455 significantly outperforms the KAI-29052 above 375 nm, with a smaller pixel size and a lower read noise compared to the KAI-29052.
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: Histogram of the standard deviation (1σ) of the multi-axis star camera centroids during the 300 s science exposures on the fine image stabilization cameras.
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: Histogram of the standard deviation (1σ) of the guide star centroids on the boresight camera during the 300 s science exposures, highlighting that SuperBIT met the telescope pointing stabilization requirement.
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 centroid behavior on the FSC with the FGS on and off over a 5-minute (300 s) time chunk. The left panel shows the x-axis behavior, the middle panel shows the y-axis behavior, and the right panel shows the combination of the two.
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 SuperBIT optical system, consisting of a modified-Dall–Kirkham f/11 design with a 0.5 m elliptical primary mirror (M1), a spherical secondary mirror (M2), and a three-lens corrector stack to improve off-axis image quality.
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 SuperBIT battery heaters consist of aluminum plates that cover the sides of the batteries. The heater on the plates consists of resistive nichrome wire, which is electrically insulated from the plate with high-temperature polyester tape.
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 bottom of the SuperBIT gondola outer frame showing the installed batteries and the reaction wheel.
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: Extracted delays and TECs for a sample of 53 triggered baseband events from 16 unique pulsars referenced to J0117+8928 from 2023 June through August. Top panel: we plot the residual delay (nanoseconds) as a function of projected sky separation between target and calibrator (degrees) before applying the baseline correction. Only statistical error bars are present, which are clearly underestimated. Middle panel: for the identical set of pulsars, we plot the residual delays after applying the offset correction. We compute the statistical and systematic uncertainties according to the covariance matrix derived in the Appendix. Bottom panel: we plot the extracted TEC values from the fringe fits along with their statistical error bars. We verify that the TEC values extracted before and after applying the correction were identical, confirming that our grid spacing used to carry out the fringe fit was sufficiently fine. The values have a mean and standard deviation of 0.0 ± 0.4 TECu.
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: Left panel: measured offsets of 100 pulses relative to positions obtained with the VLBA as a function of cross-correlation S/N. The points are color-coded by target–calibrator separation, and the rms of the entire sample is 1.″16 (dashed horizontal lines). Right panel: Distribution of offsets for the entire sample (white outlined in black), and offsets after removing sources where the cross-correlation signal could be measured in only half the band.
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: Baseline offset MCMC. Modeling 22 delay measurements using difxcalc11, we run a 150,000-step MCMC to determine the offset from the original position of the KKO GPS clock. The parameter α characterizes the amplitude of systematic errors in the delay measurements (see the Appendix). The log-likelihood is given by Equation (18). No priors are assumed on any of the offset parameters. We assert a Gaussian prior on α with mean 1 ns and width 0.4 ns, motivated by measurements of beam phase at CHIME (see the Appendix for details). The MCMC had a mean acceptance fraction of 55%, and the fit residuals are well behaved.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: TESS photometry of TOI-2015 from Sectors 24 and 51. Blue points are the PDCSAP data, and white points show 2 hr binned data. (A) TESS photometry showing out-of-transit variability. The black curve shows the transit model along with the Gaussian process (GP) quasiperiodic correlated noise model from our juliet fit (black curve). (B) TESS photometry after removing out-of-phase variability as modeled by the GP. Transits of TOI-2015 b are clearly visible. The data behind this figure are available in machine-readable format. In addition to the TESS photometry, it also includes the photometry from the ARC, LCOGT, RBO, and WIRO data sets. The latter can be used to generate other figures in the article.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Out-of-transit photometry from ZTF and TESS. (A)–(F) ZTF photometry and associated generalized Lomb–Scargle periodograms in the z  g , z  r , and z  i  filters. All filters show a peak at 8.7 days (red vertical line). (G)–(J) TESS photometry and associated TESS-SIP plots for Sectors 24 and 51. TESS Sector 24 shows a peak consistent with 8.7 days, whereas Sector 51 shows a peak at 6.3 days. We attribute the latter to low data coverage and large gaps in the TESS data. We adopt a rotation period of 8.7 ± 0.9 days. In panel (I), we also show a zoomed-in view of one of the flares in the TESS photometry.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Seeing-limited imaging. Left: seeing-limited imaging from POSS-1 in the blue filter from the Digital Sky Survey-1 from 1954. Right: seeing-limited imaging obtained with TMMT in the Johnson I filter in 2021 May. The filled yellow circle (7″ radius) denotes the Gaia position of TOI-2015 at the Gaia epoch (2015.5). The white lines show the outline of the TESS aperture. North is up, and east is to the left. The two nearby stars, TIC 368287010 and TIC 368287012, result in a modest dilution of 0.131892 ± 0.001231 in the TESS aperture. No other nearby stars are detected.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: High-contrast imaging of TOI-2015 from (A) WYIN 3.5 m/NESSI speckle imaging, and (B) Lick 3 m/ShaneAO. The curves show azimuthally averaged radial Δ magnitude constraints, in the 562 nm (blue) and 832 nm (red) filters for NESSI, and the J and K  S  band for ShaneAO. The inset images show the corresponding high-contrast images. We see no evidence of nearby companions in either the NESSI or the ShaneAO observations.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Kernel density estimate for a CMD based on Gaia DR3 showing M dwarfs closer than 50 pc. The dashed line shows the upper edge of the Jao Gap (Jao et al. 2018), which is the transition zone between partially and fully convective M dwarfs. TOI-2015 (red star) is below this transition zone, suggesting that it is a fully convective M dwarf.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: A comparison of double Gaussian parameters from the fitted models in Figure 9. With the exception of the outlier σ mp from the PARSEC CMD 3.7 model (see the lack of a local minimum in that model for NGC 4839 in Figure 9) the models produce very similar sets of double Gaussian parameters.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: Double Gaussian fits for the MDFs from Figure 8.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: A comparison of double Gaussian parameters from the 5 stellar models with (lighter boxes) and without (darker boxes) age corrections.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Corner plot for the stable posterior samples from the joint TTV-RV fit assuming the 2:1 period ratio. The figure was created using corner.py (Foreman-Mackey 2016).
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: Forward-modeling results. From left to right: input model—the best fitted synthetic disk which is the input model convolved with the instrumental PSF prior to forward modeling; proc model—the model disk post forward modeling, which yields the synthetic equivalent of the wavelength-collapsed image of the disk after ADI A-LOCI PSF subtraction; data—the wavelength-collapsed, PSF-subtracted image of the disk; data—model—the residual for the data product and the synthetic disk model postprocessing. The minimal structure that remains after subtracting the two disk images suggests our model closely matches 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: A grid of wavelength-collapsed images of the disk following ADI A-LOCI PSF subtraction for different pairs of N  A  and δ FWHM (indicated here as nfwhm) values. N  A =250, δ FWHM = 0.75 has the highest signal to noise ratio along the spine of the disk.
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: A grid of wavelength-collapsed images of the disk following ADI A-LOCI PSF subtraction for different pairs of geom and SVD﹩{}_{\mathrm{lim}}﹩ (indicated here as svd) values. geom = 0.25, SVD﹩{}_{\mathrm{lim}}={10}^{-5}﹩ has the highest signal-to-noise ratio along the spine of the disk.
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: Images of the disk post ADI-ALOCI PSF subtraction for each wavelength channel. The wavelength of each channel is in microns.
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: Images of the disk post ADI-ALOCI PSF subtraction with wavelength channels combined for images within J, H, and K bands.
Paper: Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure
Authors: Beverly J. Smith, Matthew Watson, Mark L. Giroux, Curtis Struck
Figure caption: Left: plot of R(max), the maximum distance out to which we trace spiral arms, vs. R(edge), the edge of the GZ-3D field of view. The small black dots are all of the galaxies in the z < 0.05 GZ-3D sample for which we are able to mark spiral arms. Red open triangles mark the galaxies that we classified as multiarmed. Blue open circles are galaxies classified as grand design. Magenta open diamonds mark galaxies which have R90/R(edge) > 1.2. These are galaxies that are physically large compared to the GZ-3D field of view. The red dotted line is the minimum R(max) possible for galaxies flagged as three-armed. The blue solid line is the minimum R(max) possible for a galaxy defined as grand design by our definition. Right: histograms of the maximum radius out to which we are able to reliably mark spiral arms (i.e., at a threshold = 3) for the multiarmed galaxies (red hatched histogram) and the grand design galaxies (blue).