adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Lomb-Scargle periodogram of the detrended NEID observations of HD 35833. We use the same frequency limits as in Figure 5 for ease of comparison. We also show the frequency of maximum power for the oscillation signal as detected in TESS Cycles 1 (blue, dotted) and 4 (purple, dashed) and as predicted by scaling relations (red) as vertical lines, as well as the 10%, 5%, and 1% false alarm levels (calculated via the false_alarm_level() method of the astropy.timeseries.LombScargle class) as horizontal lines (black, dotted–dashed). For comparison, we show periodograms for a set of simulated oscillation time series with the same sampling and photon noise properties as the NEID observations (background colored lines).
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: RV RMS as a function of integration time for NEID observations of HD 35833. We show the total observed RMS (red points), the photon noise as calculated from the information content of the spectra (black dashed line), the RMS of the decomposed oscillation (black dotted–dashed line) and granulation (black dotted line) signals, and the sum of the three sources of RV “noise” (blue solid line). The shape of the oscillation signal is consistent with predictions from the Chaplin et al. (2019) model.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Detrended NEID RV time series for HD 35833 (top) and residuals (bottom). The individual oscillation and granulation signals, separated using the GP decomposition method described in Section 4.3.1, are shown as black dashed (oscillation) and dotted (granulation) lines. The sum of these signals is shown as a solid blue line. The residual signal is calculated by interpolating the oscillation and granulation signals to the observation time stamps and subtracting these from the detrended RVs.(The data used to create this figure are available.)
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: TESS FFI cutout used for PLD detrending of the HD 35833 Sector 32 light curve. The stellar aperture is shown in red and the background aperture is shown in gray.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Ca II H & K S-index measurements for HD 35833 from Lick observations (Isaacson & Fischer 2010). The median value of 0.16 shows that activity-induced suppression cannot explain the observed p-mode oscillation amplitudes.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: NEID RV measurements for HD 35833. RVs are calculated using a modified version of the SERVAL template-matching algorithm applied to 1D extracted spectra from the NEID DRP, with low S/N outliers removed.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The transfer function for a sequence of six exposures separated by nonzero readout time.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The transfer function for a single finite exposure.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Ca II H & K S-index measurements for HD 35833 from the NEID time series.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Alignment of the spectrometer optics. (a) Pinhole focus. The shear plate fringes are parallel to the fiducial line, indicating that the pinhole is at the focus of the collimator. (b) Collimator tilt. The collimator has been tilted to center the collimated beam on the grating. (c) Grating tilt. The grating has been tilted to properly align the red and blue dispersed beams on the focus mirrors. (d) Feedthrough micrometers for tilting the focus mirrors. (e) Focus mirror tilt. Each focus mirror has been tilted to center the pinhole image vertically and properly align the passbands horizontally. (f) Grating rotation. The grating has been clocked so that the broadband image of the pinhole is approximately horizontal in both channels. (g) Slit rotation. The slit has been clocked so that the atmospheric absorption features are approximately vertical in both channels. (h) Cold alignment. Screenshot from the IR visualization software during in-flight alignment of the focus mirrors. The lower panel shows the 3 μm spectral × spatial image and the upper panel a spectral cross section of the image. Spectral alignment is achieved when photospheric absorption features in the measured spectrum (1) overlap with those in the library spectrum (2). Spatial alignment is achieved when light from the slit is centered vertically in the detector, resulting in a dark band at the top (3) and bottom (4).
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Input options for spectrometer alignment. The focusing optics are fed by either two visible lasers or a broadband IR lamp. The focusing optics image the object (microscope objective spot or IR-illuminated field stop) onto the slit through the vacuum chamber window (bottom right).
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Aligning the telescope to the spectrometer. (a) Diagram of components. The theodolite was used to align tip, tilt, and focus, while the IR collimator was used to check centration. (b) Slit-jaw image of the theodolite crosshair. The green plus sign marks the center of the slit, 40″ from the center of the theodolite crosshair. The slit and theodolite crosshair are both in focus. (c) Slit-jaw image of a concentric circle target from the IR collimator. (d) 4 μm IR image of the concentric circle target. The intensity is uniform over the length of the slit, confirming that the telescope pupil is centered on the spectrometer mirrors.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Thermal background reduction. Left: top-down view of the AIR-Spec vacuum chamber before it was blackened to reduce stray light. The spectrometer optics and IR camera are labeled. Liquid nitrogen enters through the LN2 fill port, and nitrogen gas is released through the vent. Copper straps connect the optics to the floor, which is the top of the liquid nitrogen Dewar. Inset: detail of the collimator mount and cooling strap. To maximize stability, each optic is mounted to the warm chamber wall with G10, a thermally isolating fiberglass composite. A thermally conducting copper strap attaches the optic to the cold spectrometer floor. Inner and outer wall guards block radiation from the warm chamber wall. Right: effect of cooling the instrument.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Left: ray-trace of the AIR-Spec telescope and spectrometer, including the layout of emission lines on the infrared detector. Different ray colors indicate different wavelengths. Right: ray-trace of the slit-jaw camera optics. Different ray colors indicate different field angles.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Telescope alignment. Left: optical setup, including the Zygo interferometer, retro ball, AIR-Spec telescope, and retro flat (Zygo Corporation 2015). Middle: aligning the secondary mirror. The retro ball is off-axis, allowing the Zygo laser beam to pass through the system. The secondary is tilted and focused by shimming with washers at the three points indicated. Right: double-pass wave front for the final telescope alignment, after zeroing tip and tilt. The phase variations are due to a combination of defocus and the λ/20 rms surfaces of the primary and secondary.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Maps and histograms of spatial nonuniformity across the detector. The left and middle panels show the offset and gain needed to perform a two-point nonuniformity correction at every pixel. The right panel shows the gain standard deviation in each local 9 × 9 pixel neighborhood.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Image stabilization system block diagram (left) and performance (right). The rms jitter for each 60 ms exposure is plotted in black. The 2-pixel Nyquist limit is the red line. A total of 92% of exposures have jitter below the Nyquist limit.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Slit-jaw camera and associated optics.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Measuring plate scale. The slit-jaw camera plate scale and slit length are calculated experimentally by fitting the limb of the solar disk to measure its diameter (panel (a)). The plate scale is 2.″26 pixel−1, and the slit length is 1.55 R ⊙. The IR camera plate scale is computed by comparing simultaneous observations of the partial eclipse in the slit-jaw camera (panel (b)) and IR camera (panel (c)). The IR camera has a plate scale of 2.″31 pixel−1, 2% larger than the slit-jaw camera.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Measured and modeled throughput.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Modeling wavelength drift/jitter as a linear combination of attitude and time. Measurements and fit for (a) the 3 μm channel and (b) the 4 μm channel. The shaded regions are the 95% prediction intervals. Fit residuals for (c) the 3 μm channel and (d) the 4 μm channel.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Power spectral density of the mean row in the 4 μm channel (top). Fringes with a period of 14 pixels (170 μm) appear as a peak at 6 mm−1. The notch filter (bottom) attenuates frequencies between 5 and 7 mm−1, removing the fringes.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Checking the inverse-modeled throughput. The black line is AIR-Spec data, converted from DN (1 DN = 3.25 e−) to photons s−1. The red line shows the photospheric library spectrum after multiplication by the inverse-modeled throughput.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: PSF FWHM across the detector. The dotted lines represent 95% confidence intervals.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Illustration of data from one of the five eclipse observations. The data set consists of three 3D arrays from the slit-jaw camera and both channels of the IR camera.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Measuring PSF.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: AIR-Spec on board GV HIAPER. The instrument is installed on the floor on the port side of the cabin toward the front of the plane. The image stabilization system, telescope, spectrometer, and slit-jaw camera are mounted on a vibration-isolated optical bench (1). Light enters through a small viewport (2) on the upper starboard side of the fuselage and is reflected into the telescope by a fast-steering mirror (3). The optical bench is translated fore–aft and left–right (4) and the mirror rotated about two axes (5) to facilitate alignment of the Sun, window, mirror, and telescope. The spectrometer optics are contained in a vacuum chamber (6) and cooled with liquid nitrogen (7).
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Predicted spectrum of M1 lines at 1.1 R ⊙ (Judge 1998). Black circles are intensity values for collisional de-excitation only; straight lines include radiative contributions. The smooth baseline is the coronal continuum produced by Thomson scattering by free electrons. Lines outlined in red were measured by AIR-Spec during the 2017 eclipse.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: IR image processing: geometric correction, image registration, and fringe removal. The 3.°5 angle between the slit and the grating grooves shears spectral and spatial features with respect to the detector (panel (a)). After geometric correction, the spectral and spatial axes are aligned with the detector axes in both channels (panel (b)). Due to pointing jitter, the lunar limb crosses the slit at a different place in each frame (panel (c)). The high-contrast limb is used to detect the jitter, and each frame is shifted an integer number of pixels to align with the others (panel (d)). In the 4 μm channel, interference fringes obscure the emission lines (panel (e)). The fringes are removed using a notch filter at the fringe frequency (panel (f)).
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Eclipse flight and operations. The GV flight path is shown in blue, the totality center line is marked by red dashes, and the totality swath appears in light red. The start time of each operation is noted with respect to second contact (C2) at 18:22 UTC. (1) Takeoff from Chattanooga, C2–130 minutes. (2) Enter holding pattern, C2–80 minutes. (3) Begin dry ice, C2–30 minutes. (4) Acquire the Sun, C2–20 minutes. (5) Set wavelength range, C2–10 minutes. (6) Collect darks, C2–2 minutes. (7) Observe totality, C2–0 minutes. (8) Collect darks, C2+4 minutes. (9) Collect calibration data, C2+10 minutes. (10) Land in Chattanooga, C2+45 minutes.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Fit parameters for the time evolution of the dark background. (a) Initial intensity in DN. (b) Rate of change in DN minute–1. (c) Sine wave amplitude in DN. (d) Sine wave phase in radians.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Slit-jaw image registration. By matching features in (a) AIR-Spec and (b) AIA 193, the slit-jaw frames are rotated to orient solar north up. Moon center is found by fitting the lunar limb to a circle (panel (c)). Each frame is shifted horizontally and vertically to place Moon center in the same location.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Alignment of the image stabilization system to the telescope. (a) Fiber-optic gyroscope to telescope. (b) Fast-steering mirror to gyroscope and telescope. (c) Fast-steering mirror adjustments.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Defective pixels. Histograms are used to identify outliers in (a) initial intensity, (b) rate, (c) acceleration, and (d) goodness of fit. Good pixels lie between the black vertical lines. (e) Defective pixel map. Bad pixels are shown in white and make up 2% of the array.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Overview of total eclipse observations. Slit positions superimposed on slit-jaw image (left) and average IR spectra at each slit position (right). Red triangles mark the spectral artifacts.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Gaussian fits to the coronal lines in position 3 (east limb active region). The measurements were averaged in time and over the 21 pixels (49″) nearest the lunar limb, corresponding to an average radius of 1.05 R ⊙.
Paper: The Airborne Infrared Spectrometer: Development, Characterization, and the 2017 August 21 Eclipse Observation
Authors: Jenna E. Samra, Vanessa Marquez, Peter Cheimets, Edward E. DeLuca, Leon Golub, James W. Hannigan, Chad A. Madsen, Advik Vira, Arn Adams
Figure caption: Behavior of the dark background at 60 ms exposure time. (a) Dark frame at the end of totality. (b) 6-minute time series of the spatial average.
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Same as Figure 8.