adsabs/AstroCLIMB huggingface dataset:
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Example correlations between bisector shape summary statistic and anomalous, granulation-induced velocity shift for a synthetic Fe I 5434 Å time series. Left: Time-averaged line bisector (opaque blue curve) and bisector variations (transparent blue curves). The amplitude of the bisector variations are exaggerated 50× for visual effect. The regions bound by the horizontal dashed lines and dotted lines represent the v  t  and v  b  regions used in the calculation of BIS, respectively. Middle: correlation between BIS and apparent RV excursion with best-fit relation. Each point corresponds to one snapshot of the synthetic time series. Right: same as middle panel, but for bisector amplitude a  b .
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Panel (a): Synthesis accuracy for the GRASS GPU implementation assessed against the CPU implementation fiducial. Spectra synthesized at double precision on a CPU and at both single and double precision on a GPU are shown in the top panel. Residuals for each of the GPU precisions are shown in the middle and bottom panels. Marginal distributions of the residuals are shown at the right of the middle and bottom panels. Note the differences in y-axis scales between each panel. Compared to the double-precision synthesis, which is accurate to several parts in 1015, single-precision synthesis is only accurate to a few parts in 103 as the result of catastrophic cancellation in repeated interpolation calculations. This effect is most pronounced closer to the line core, where many repeated interpolations and in-place multiplications are performed, compared to the line wings and continuum. Because flux errors at the level of 1 × 10−3 propagate to velocity errors of order ∼several centimeters per second, we strongly advise against the use of the single-precision GPU implementation of GRASS. Panel (b): GRASS performance by implementation architecture. GPU benchmarks were performed with an NVIDIA Tesla V100S GPU. For these benchmarks, the size of the synthesized spectrum (i.e., number of lines) was varied, with the number of time steps fixed at N  t  = 50, and the number of latitude slices fixed at N  ϕ  = 197. Even for smaller problem sizes, the GPU implementation outperforms the CPU implementation because of the large overhead incurred by computing the necessary geometrical parameters and weights (see Appendix A.2) on the CPU. The double-precision GPU implementation achieves a factor of ≳100 speed-up for larger problem sizes. Owing the large loss in accuracy in the Float32 implementation (see Figure 9), we do not recommend use of single-precision synthesis with GRASS.
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Tiling (left-hand plot) and subtiling (right-hand plot) of an example stellar surface viewed at slight inclination. In both plots, the tiles and subtiles are drawn artificially large for illustrative clarity. The coloring indicates the fractional weight of each tile normalized to the largest weight value; individual weights are given by the product of the limb darkening and projected area of the tile. The stellar equator and the 0° and 90° meridians are overplotted as white dashed lines. Left: the stellar surface is divided into tiles according to the prescription developed by Vogt et al. (1987). The number of latitudinal slices (and consequently the total number of tiles) is set such that the average tile area corresponds to the average angular size of the input observations, as described in Appendix A.2. Right: zoom-in on the tile highlighted by the blue border in the left-hand plot, with example subtiling. Because the grid resolution dictated by the angular size of the input observations would normally introduce discretization errors in the rotation velocity, limb darkening, and projected tile area computations, these quantities are calculated at the centers of subtiles within each larger tile (indicated by the black dots). As in Cegla et al. (2019), the subtiles are spaced evenly in stellar latitude and longitude within each larger tile.
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Percent improvement in rms RV for a subset of the simulations described in Section 4.3.1 and shown in Figure 5. Combinations of SNR and number of binned lines denoted with a “-” showed no significant improvement in rms RV; none of the three lowest-resolution simulations (R ∼ 98,000, R ∼ 120,000, and R ∼ 137,000) achieved significant improvements in rms RV for any combination of SNR and number of binned lines and so are not shown. It is plausible that ESPRESSO in UHR mode and PEPSI could demonstrate a retrieval (and correction of) convective variability for a bright star if enough similarly varying lines could be identified and binned, as discussed in Section 4.3.2.
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Example Voigt fits to observed line profile (left-hand subplot) and resulting input data. The bisector (middle subplot) is measured directly from the observed line profile, whereas the width as a function of intensity (right-hand subplot) is measured from the best-fit Voigt wings above ∼88% of the continuum flux in this example.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: Reference star TA performance for the SW (top) and LW (bottom) observations. The dots are color-coded by dither position and show the measured offsets between the reference star and science target observation (first roll), while the crosses show the commanded and expected offsets in the case of a perfect TA. The TA performance is good for the SW channel, but worse than expected for the LW channel (see Section 2.2.2 for details). The plots show the F210M and F335M data sets; all other filters in the same NIRCam detector channels show similar performance.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: JWST/NIRCam coronagraphy images of the β Pic system. The six rows show the six observed filters and the three columns show the pre-KLIP images (non-PSF-subtracted; left), the post-KLIP images (PSF-subtracted; middle), and the post-KLIP and high-pass-filtered images (high-pass filter size of 3 pixels; right). The host star is located at the origin. All images are shown in the same linear color stretch. The small insets in the middle and right columns show a zoom-in on the giant planet β Pic b in a different color stretch that aims to highlight the planet PSF.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: 5σ contrast limits (top) and companion mass limits (bottom) measured from the PSF-subtracted JWST/NIRCam coronagraphy images of the β Pic system. The left panels show the ADI+RDI limits for all six observed filters; the right panels compare the three employed KLIP PSF subtraction techniques (ADI+RDI, ADI, and RDI) for the F444W wideband filter. All curves were computed from high-pass-filtered images to remove the flux of the edge-on debris disk around β Pic as much as possible. The solid lines show the limits away from the disk midplane and the transparent lines show the limits in the disk midplane. The companion mass limits were computed using ATMO + BEX hot-start evolutionary models and assuming an age of 18.5 Myr and a distance of 19.44 pc for β Pic. The masses of the gas and ice giants in the solar system are shown for reference (planet symbol sizes are not to scale, and planet projected separations are five times the true separations from the Sun).
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: JWST/NIRCam KLIP (top) and MCRDI (bottom) photometry of the giant planet β Pic b in red, plotted together with other photometry and spectra and a DRIFT-PHOENIX model atmosphere of β Pic b from the literature. The filled symbols show the data and the open symbols show the values predicted by the best-fitting model atmosphere. The model atmosphere was fitted to the literature data only (and not the new NIRCam data), and its parameters are printed at the top of the middle panel. The residuals between the data and the model atmosphere are shown in the bottom panel and the filter transmission curves are shown in the top panel.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: JWST/NIRCam color–magnitude diagram (left) and color–color diagram (right) showing Sonora Bobcat and AMES-Dusty isochrones for an 18.5 Myr old companion in blue and orange, respectively. The giant planet β Pic b is shown by a red star and two other substellar companions that have already been observed with JWST spectroscopy are shown by pink stars. The dashed gray line shows a blackbody and the dashed blue and orange lines show the isochrones for a 100 Myr old companion for reference.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: JWST/NIRCam astrometry of the giant planet β Pic b plotted together with the GRAVITY data points and the inferred orbits of both β Pic planets from Lacour et al. (2021). The blue point in the inset shows the expected position of β Pic b at the time of the JWST observations. Due to the large (systematic) uncertainties if compared to the GRAVITY measurements, the NIRCam astrometry does not provide improved constraints on the orbital parameters of β Pic b.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: JWST/NIRCam color–magnitude diagrams showing an ATMO + BEX hot-start evolutionary track for an 18.5 Myr old bound companion in blue. The point-like background source identified in the NIRCam data of β Pic and the giant planet β Pic b are shown by an orange and a red star. The dashed and transparent blue line shows an ATMO + BEX cold-start evolutionary track for reference.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: PSF-subtracted JWST/NIRCam (left) and MIRI (right) images of the β Pic system (arbitrary color stretch). Five background sources were identified based on their NIRCam colors or morphology whose positions are highlighted in both images with red circles. The orange circles in the NIRCam image show the source positions rotated by the telescope roll angle, where negative ADI residuals are visible. BG4 appears to be the only source which is also visible in the MIRI image. The MIRI image was adapted from Rebollido et al. (2024).
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: Forward modeling of β Pic b’s PSF in the KLIP approach. The six rows show the six observed filters and the three columns show the KLIP-subtracted images (left), the best-fit forward-model planet PSFs (middle), and the residuals between the two (right). The position of the host star β Pic is indicated with a black star.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: MCRDI modeling of β Pic b. The six rows show the six observed filters and the three columns show the host star PSF- and disk-model-subtracted images (left), the best-fit planet PSF models (middle), and the residuals between the two (right). The position of the host star β Pic is indicated with a black star. F250M and F300M are particularly affected by spatial undersampling and the PSF subtraction has higher residuals for these filters.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: Best-fit model atmospheres from the BT-Settl (top), DRIFT-PHOENIX (middle), and Exo-REM (bottom) grids fitted to the JWST/NIRCam photometry of the giant planet β Pic b alone (light gray) and together with existing data from the literature (dark gray).
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: Recovered companion fluxes as a function of the high-pass filter size from fake companion injection and recovery tests using the ADI+RDI (solid lines), ADI (dashed lines), and RDI (dotted lines) techniques. The injected fluxes (ground truth) are shown by a horizontal solid line. The fake companion was injected at the same angular separation as β Pic b, but on the opposite side of the star.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: Comparison of β Pic b’s inferred luminosity and radius with NGPPS (Emsenhuber et al. 2021). The left panel shows the bolometric luminosity, with the orange area highlighting the combined constraints from the SED fits (all six models in Table 6). The right panel shows the radius, with the constraints from the three model atmosphere grids highlighted separately. The samples from NGPPS were selected from NG73 (i.e., one planetary embryo per simulated system) at an age of 20 Myr. The gray area shows the dynamical mass of β Pic b, indicating a discrepancy with the bulk constraints from the SED.
Paper: JWST-TST High Contrast: JWST/NIRCam Observations of the Young Giant Planet β Pic b
Authors: Jens Kammerer, Kellen Lawson, Marshall D. Perrin, Isabel Rebollido, Christopher C. Stark, Tomas Stolker, Julien H. Girard, Laurent Pueyo, William O. Balmer, Kadin Worthen, Christine Chen, Roeland P. van der Marel, Nikole K. Lewis, Kimberly Ward-Duong, Jeff A. Valenti, Mark Clampin, C. Matt Mountain
Figure caption: Model atmosphere parameter posterior distributions for the BT-Settl (top), DRIFT-PHOENIX (middle), and Exo-REM (bottom) grids fitted to the JWST/NIRCam photometry of the giant planet β Pic b alone (orange) and together with existing data from the literature (blue). The markers with horizontal error bars above the histograms show the 16th, 50th, and 84th percentiles of the distribution.
Paper: In Search of Infall Motion in Molecular Clumps. V. HCO+ (1–0) and HCN (1–0) Observations toward 210 Infall Candidates
Authors: Shuling Yu, Zhibo Jiang, Zhiwei Chen, Yang Yang, Haoran Feng
Figure caption: The distributions of gas kinetic temperature, infall velocity, and mass infall rate. The red and blue dashed lines in the four figures represent the median values of the double-peaked and the peak-shoulder sources, respectively.
Paper: In Search of Infall Motion in Molecular Clumps. V. HCO+ (1–0) and HCN (1–0) Observations toward 210 Infall Candidates
Authors: Shuling Yu, Zhibo Jiang, Zhiwei Chen, Yang Yang, Haoran Feng
Figure caption: The left panel shows a positive correlation between infall velocity and free-fall velocity, with a gray dashed line representing the linear regression fit. Meanwhile, the right panel displays a positive correlation between mass infall rate and H2 column density.
Paper: In Search of Infall Motion in Molecular Clumps. V. HCO+ (1–0) and HCN (1–0) Observations toward 210 Infall Candidates
Authors: Shuling Yu, Zhibo Jiang, Zhiwei Chen, Yang Yang, Haoran Feng
Figure caption: Effect of different density index α on spectral line profile in the RATRAN model. The vertical dashed line represents the system velocity.
Paper: In Search of Infall Motion in Molecular Clumps. V. HCO+ (1–0) and HCN (1–0) Observations toward 210 Infall Candidates
Authors: Shuling Yu, Zhibo Jiang, Zhiwei Chen, Yang Yang, Haoran Feng
Figure caption: Relationship between the envelope mass and infall velocity/mass infall rate.
Paper: Exoplanet Aeronomy: A Case Study of WASP-69 b’s Variable Thermosphere
Authors: W. Garrett Levine, Shreyas Vissapragada, Adina D. Feinstein, George W. King, Aleck Hernandez, Lía Corrales, Michael Greklek-McKeon, Heather A. Knutson
Figure caption: Summary of comparative aeronomy between the terrestrial thermosphere and WASP-69 b. Left: time series of solar activity indicator (top panel) and terrestrial thermospheric conditions (bottom panel) from 1960 to 2020. Numbers on the top panel label the solar cycles by their numbers. Right: analogous plots for the WASP-69 system. The top panel shows stellar activity proxied by X-ray flux observed at Earth, and the bottom panel shows WASP-69 b’s thermospheric conditions as traced in metastable HeI from Section 3.3. Multiepoch, multiwavelength campaigns are necessary to extend the well-developed field of solar system aeronomy to the exoplanets.
Paper: Exoplanet Aeronomy: A Case Study of WASP-69 b’s Variable Thermosphere
Authors: W. Garrett Levine, Shreyas Vissapragada, Adina D. Feinstein, George W. King, Aleck Hernandez, Lía Corrales, Michael Greklek-McKeon, Heather A. Knutson
Figure caption: Results from joint fitting WIRC night 1 (blue), WIRC night 2 (red), and TESS (gray) data. Panel (a) shows the phase-folded light curves for all three time series. Individual points and their uncertainties are shown with small markers, and Palomar/WIRC data binned to 10 minute intervals are shown with larger markers. Best-fit light-curve models are shown as solid lines. Panels (b), (c), and (d) show the residuals for the WIRC night 1, WIRC night 2, and TESS time series, respectively.
Paper: Exoplanet Aeronomy: A Case Study of WASP-69 b’s Variable Thermosphere
Authors: W. Garrett Levine, Shreyas Vissapragada, Adina D. Feinstein, George W. King, Aleck Hernandez, Lía Corrales, Michael Greklek-McKeon, Heather A. Knutson
Figure caption: Gaussian FWHM of WASP-69's PSF plotted vs. orbital phase during the WIRC science imaging sequence for night 1 (blue line) and night 2 (red line). Normalized radial seeing profiles were constructed and fitted with a Gaussian using photutils (Bradley et al. 2023). Although the night 2 PSF varied more than the night 1 PSF, both time series were stable over the observations.
Paper: Exoplanet Aeronomy: A Case Study of WASP-69 b’s Variable Thermosphere
Authors: W. Garrett Levine, Shreyas Vissapragada, Adina D. Feinstein, George W. King, Aleck Hernandez, Lía Corrales, Michael Greklek-McKeon, Heather A. Knutson
Figure caption: Allan deviation plots for each detrended WIRC light curve in the joint fitting with both time series and TESS data. The top and bottom panels show results from the detrended night 1 and night 2 light curves, respectively. Colored lines with error bars denote the rms error of the binned residuals for each light curve. The solid black lines denote the expected noise from purely Poisson statistics, and the dotted line shows the photon noise scaled up to the rms error of the binned residuals.
Paper: Exoplanet Aeronomy: A Case Study of WASP-69 b’s Variable Thermosphere
Authors: W. Garrett Levine, Shreyas Vissapragada, Adina D. Feinstein, George W. King, Aleck Hernandez, Lía Corrales, Michael Greklek-McKeon, Heather A. Knutson
Figure caption: Photometry of WASP-69 from TESS Sector 55. The lightest gray points are the PDCSAP flux that were downloaded from MAST, and the magenta line shows the best-fit spline from Keplerspline. Detrended flux, obtained by dividing the PDCSAP flux by the spline, is shown with two colors. Dark gray dots are detrended points far from the observed transits that are removed by the mask. Black dots are detrended points that are included by the mask. Upward-pointing arrows indicate expected transit midpoints from orbital parameters published by Kokori et al. (2022).