adsabs/AstroCLIMB huggingface dataset:
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Redshift evolution of elliptical and spiral galaxies in (b − g), (u − b) color–color space. Blue solid lines show the observed galaxy color evolution between 0 < z gal < 1.5; small points mark δ z = 0.02 intervals. Large markers are included as a visual aid: blue stars and cyan error bars mark z gal < 0.5, while red squares and magenta error bars mark z gal ≥ 0.6. Error bars are 1σ color uncertainties for galaxies with b-band S/N = 10. Color–color tracks assume exposure times of 3 hr, 1.5 hr, and 3 hr in the b, g, and u bands, respectively. A “clean” color–color space, with low foreground galaxy contamination (no blue stars), suitable for a cluster at z = 0.5, lies below the dashed black line.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Galaxy brightness histograms (top) and redshift distributions (bottom) for the “all galaxies” sample with only an S/N >5 selection criterion. Dotted lines mark the S/N = 10 limiting magnitudes (top) and the median redshift (bottom), respectively, in each filter.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Galaxy brightness distributions shown as normalized histograms of galaxy counts, binned by AB magnitude. Dotted lines mark the S/N = 10 depth. Left panels: all galaxies with S/N > 5 and z > z clust. Right: galaxies that pass lensing analysis selections including z > z clust.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Normalized redshift distributions of the COSMOS 2015 simulation input catalog (red line), the z > 0.3 lensing sample (blue line), and the z > 0.059 lensing sample (cyan line). The two lensing samples have lower mean redshifts (﹩\bar{z}=1.2﹩ and ﹩\bar{z}=1.3﹩) than the COSMOS 2015 catalog (﹩\bar{z}=1.5﹩).
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Normalized galaxy redshift distributions behind a cluster at z = 0.059 (top), z = 0.3 (middle), and z = 0.45. Left panels: all galaxies with S/N > 5 and z gal > z clust. Right: galaxies that pass lensing analysis selections, including z gal > z clust.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Ni I. Left:  the Mantis Network templates injected and cross-correlated with our data. The 2000 K template is shown in blue, and the 2500 K template is shown in orange. The 3000 and 4000 K templates are omitted because there are no lines present at the GRACES wavelength range. Top right:  the 2D cross-correlation map for the template recovered at the highest significance, which in this case is the 2500 K template. The white lines indicate the peak S/N, which is also the velocity at which the template was injected into our data. Bottom right:  slices of the 2D cross-correlation maps for each of the templates, with the 2000 K template shown in blue and the 2500 K template shown in orange, as in the plot on the left. The 2500 K template is recovered at a significance of >5σ, while the 2000 K template is only tentatively recovered.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A tentative detection of K I absorption in WASP-76b’s atmosphere. The plots are as described in the caption of Figure 5. While we do see a peak at 4.4σ at roughly the expected location of the exoplanet’s atmosphere, the noise in the cross-correlation map prevents us from confidently labeling this as a detection. The 3000 K template was used. The K I line at the blue end of the spectrum was excluded due to the low quality of the data (shown in gray).
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A tentative detection of Cr I absorption in WASP-76b’s atmosphere. The plots are as described in the caption of Figure 5. While we do see a peak at 4.0σ at roughly the expected location of the exoplanet’s atmosphere, the noise in the cross-correlation map prevents us from confidently labeling this as a detection. The 3000 K template was used. Six orders at the blue end of the spectrum were excluded from the analysis (indicated in gray), similar to the 1D high-resolution synthetic transmission spectrum and the Fe I model.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Ba II. The plots are as described in the caption of Figure 12, but in this case a 3000 K template is also displayed in green, and a 4000 K template (which resulted in the strongest recovered detection) is displayed in pink.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: A tentative detection of V I absorption in WASP-76b’s atmosphere. The plots are as described in the caption of Figure 5. The 4000 K template was used. Six orders at the blue end of the spectrum were excluded from the analysis (indicated in gray), similar to the 1D high-resolution synthetic transmission spectrum and the Fe I model.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Mg I. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Ti I. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Co I. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Mn I. The plots are as described in the captions of Figures 12 and 13.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: One-dimensional illustration of the origins of resampling noise. The top panel shows three realizations of a 1D Gaussian line profile with different peak locations. Orange circles represent the values recorded after convolution of the line profile with the tophat pixel boundaries (indicated by the vertical grid lines), and the blue squares indicate the values after drizzling to a different sampling scale. In each case, ϕ gives the pixel phase of the Gaussian peak. Bottom-left panel: peak drizzled flux value as a function of the pixel phase of the Gaussian peak. Bottom-right panel: peak drizzled flux as a function of wavelength assuming a pixel phase that varies with wavelength in a manner similar to a typical MRS spectral trace.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: Semiamplitude of resampling artifacts (see Figure 9) in 1D spectra extracted from observations of the bright star 16CygB as a function of wavelength. Dotted/dashed/solid lines, respectively, indicate undithered data, data obtained with a two-point dither, and data obtained with a four-point dither, respectively. Spectra are extracted from single spaxels (cyan lines), apertures with radius 0.5 times the PSF FWHM (orange lines), 1.0 times the PSF FWHM (green lines), 1.5 times the PSF FWHM (pink lines), and 2.0 times the PSF FWHM (black lines). Both dithering and larger aperture radii help reduce the amplitude of resampling artifacts in extracted spectra; the apparent rise in artifact amplitudes at the longest wavelengths is due in part to the increasing noise in the observed spectrum.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: Ratio of the error measured from multiple simulated realizations of constant surface brightness data cubes (σ meas) divided by the error estimated from the cube error array assuming a diagonal covariance matrix (σ diag;  i.e., no covariance between adjacent spaxels). The top panel shows the results as a function of the aperture extraction radius for Channels 1–4 when each channel has a voxel scale as given in Section 3.2. The bottom panel shows similar results when all four channels are built onto a single output cube scale with spatial sampling optimized for Channel 1 and a nonlinear wavelength solution. Solid black plus signs represent the interpolated values at radii 2.0 times the PSF FWHM.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: Simulated (left) and observed (right) effect of resampling noise on extracted MRS spectra from drizzled data cubes. Simulations assumed a flat noiseless spectrum, while observations targeted the bright G3V star 16CygB. Resampling noise imparts large low-frequency modulations in the spectrum, and is mitigated by dithering and use of large extraction apertures.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: MIRI MRS Channel 3B spectrum of standard star 16 CygB, extracted from the single brightest spaxel in a data cube constructed from four dithered exposures. The solid gray and black lines show the result from data cubes constructed using the 3D drizzle and EMSM methods, respectively, while the red line shows the result from the drizzled data cube smoothed with a spatial Gaussian kernel of radius 0.7 spaxels prior to spectral extraction.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: Same as Figure 4 but representing the simplified case in which the spectral dispersion is assumed to be aligned with detector columns and the spatial distortion constant for all wavelengths covered by a given pixel. This assumption reduces the computation of volumetric overlap between red and gray hexahedra to separable 1D and 2D computations.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: MRS multichannel cube wavelength sampling (solid black line), which varies as a function of wavelength to approximately Nyquist-sample the effective spectral resolution at all wavelengths. Colored lines represent the constant linear sampling step used by default for cubes constructed within a single MRS spectral channel.
Paper: A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer
Authors: David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, Bart Vandenbussche
Figure caption: JWST/NIRSpec G140H/F100LP spectrum of G2V star GSPC P330-E. The solid blue line shows the spectrum of the brightest spaxel in a single exposure, and exhibits significant resampling noise compared to the orange spectrum extracted from a 3 spaxel radius region from a cube built from four dithered exposures.
Paper: Alert Classification for the ALeRCE Broker System: The Anomaly Detector
Authors: Manuel Perez-Carrasco, Guillermo Cabrera-Vives, Lorena Hernandez-García, F. Förster, Paula Sanchez-Saez, Alejandra M. Muñoz Arancibia, Javier Arredondo, Nicolás Astorga, Franz E. Bauer, Amelia Bayo, M. Catelan, Raya Dastidar, P. A. Estévez, Paulina Lira, Giuliano Pignata
Figure caption: Light curves for outliers classified as transients by the ALeRCE light-curve classifier. The light curves include data from the ZTF alert stream in the g (green data points) and r (red data points) filters, as well as from ZTF Data Release 6 in the g (gray data points) and r (blue data points) filters. The gray vertical dotted line represents the last time step used to compute the features and assign the anomaly score.
Paper: Alert Classification for the ALeRCE Broker System: The Anomaly Detector
Authors: Manuel Perez-Carrasco, Guillermo Cabrera-Vives, Lorena Hernandez-García, F. Förster, Paula Sanchez-Saez, Alejandra M. Muñoz Arancibia, Javier Arredondo, Nicolás Astorga, Franz E. Bauer, Amelia Bayo, M. Catelan, Raya Dastidar, P. A. Estévez, Paulina Lira, Giuliano Pignata
Figure caption: Light curves for outliers classified as stochastic sources by the ALeRCE light-curve classifier. Color code as in Figure 4.
Paper: Alert Classification for the ALeRCE Broker System: The Anomaly Detector
Authors: Manuel Perez-Carrasco, Guillermo Cabrera-Vives, Lorena Hernandez-García, F. Förster, Paula Sanchez-Saez, Alejandra M. Muñoz Arancibia, Javier Arredondo, Nicolás Astorga, Franz E. Bauer, Amelia Bayo, M. Catelan, Raya Dastidar, P. A. Estévez, Paulina Lira, Giuliano Pignata
Figure caption: Light curve for the outlier source classified as periodic by the ALeRCE light-curve classifier, namely ZTF 19aaxooyz. The left panel shows the original light curve, whereas the right panel shows the folded light curve using a period of 8.071 days. Color code as in Figure 4.
Paper: Alert Classification for the ALeRCE Broker System: The Anomaly Detector
Authors: Manuel Perez-Carrasco, Guillermo Cabrera-Vives, Lorena Hernandez-García, F. Förster, Paula Sanchez-Saez, Alejandra M. Muñoz Arancibia, Javier Arredondo, Nicolás Astorga, Franz E. Bauer, Amelia Bayo, M. Catelan, Raya Dastidar, P. A. Estévez, Paulina Lira, Giuliano Pignata
Figure caption: Proportion of objects in terms of the number of selected outlier objects. Notice that as the number of outlier candidates increases, objects with lower anomaly scores are selected. Therefore, the outlier candidates are plotted in decreasing order. Outliers are represented by blue lines, wrong classes by orange lines, “nothing special” sources by green lines, and sources showing errors in the data by red lines. Left: Transient sources. Center: Stochastic sources. Right: Periodic sources.
Paper: Alert Classification for the ALeRCE Broker System: The Anomaly Detector
Authors: Manuel Perez-Carrasco, Guillermo Cabrera-Vives, Lorena Hernandez-García, F. Förster, Paula Sanchez-Saez, Alejandra M. Muñoz Arancibia, Javier Arredondo, Nicolás Astorga, Franz E. Bauer, Amelia Bayo, M. Catelan, Raya Dastidar, P. A. Estévez, Paulina Lira, Giuliano Pignata
Figure caption: Periodogram for ZTF 19aaxooyz using ZTF alert (left) and ZTF Data Release 6 (right) data. Both periodograms are calculated using P4J (Huijse et al. 2018).
Paper: Alert Classification for the ALeRCE Broker System: The Anomaly Detector
Authors: Manuel Perez-Carrasco, Guillermo Cabrera-Vives, Lorena Hernandez-García, F. Förster, Paula Sanchez-Saez, Alejandra M. Muñoz Arancibia, Javier Arredondo, Nicolás Astorga, Franz E. Bauer, Amelia Bayo, M. Catelan, Raya Dastidar, P. A. Estévez, Paulina Lira, Giuliano Pignata
Figure caption: Methodology for training and evaluation of the anomaly detection algorithms. We split the data into a training set and a test set, composed of 80% and 20% of the data, respectively. The training set is subdivided into transient, stochastic, and periodic data. For each of these classes, we choose each subclass as the outlier class. The outlier class is removed from the training set and added to the test set (TS2). Then, an anomaly detection algorithm is trained using the remaining objects of each of the classes, and is evaluated using TS2.
Paper: Alert Classification for the ALeRCE Broker System: The Anomaly Detector
Authors: Manuel Perez-Carrasco, Guillermo Cabrera-Vives, Lorena Hernandez-García, F. Förster, Paula Sanchez-Saez, Alejandra M. Muñoz Arancibia, Javier Arredondo, Nicolás Astorga, Franz E. Bauer, Amelia Bayo, M. Catelan, Raya Dastidar, P. A. Estévez, Paulina Lira, Giuliano Pignata
Figure caption: Cumulative distribution function of the anomaly scores for the transient, stochastic, and periodic objects. It is important to note that the anomaly score range displayed in each plot corresponds to the score range covered on the respective top-level class.
Paper: The Orbit of Warm Jupiter WASP-106 b is Aligned with its Star
Authors: Jan-Vincent Harre, Alexis M. S. Smith, Teruyuki Hirano, Szilárd Csizmadia, Amaury H. M. J. Triaud, David R. Anderson
Figure caption: Same as Figure 2, but zoomed in on the Rossiter–McLaughlin anomaly.
Paper: The Orbit of Warm Jupiter WASP-106 b is Aligned with its Star
Authors: Jan-Vincent Harre, Alexis M. S. Smith, Teruyuki Hirano, Szilárd Csizmadia, Amaury H. M. J. Triaud, David R. Anderson
Figure caption: Top: RVs and the best-fit model for all of our data sets of WASP-106, showing the Keplerian orbit. The orbital phase is shown on the x-axis, with the radial velocity being shown on the y-axis. The different instruments are marked according to the legend, with “HARPS1” and “HARPS2” describing the first and second observation made with the HARPS spectrograph. The best-fit model is shown as the red curve. Bottom: residuals of our best-fitting model.
Paper: The Orbit of Warm Jupiter WASP-106 b is Aligned with its Star
Authors: Jan-Vincent Harre, Alexis M. S. Smith, Teruyuki Hirano, Szilárd Csizmadia, Amaury H. M. J. Triaud, David R. Anderson
Figure caption: Phase-folded transit for all available TESS sectors. The TESS data is shown as black dots, the rolling median is shown as blue dots, and the final TLCM model is shown in red.
Paper: HST/WFC3 Light Curve Supports a Terrestrial Composition for the Closest Exoplanet to Transit an M Dwarf
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Aurelia Balkanski, Nikole Lewis, Maura Lally, Jacob L. Bean, Ryan Cloutier, Jason D. Eastman
Figure caption: One of our 188 spatial-scan images of the LTT 1445ABC system. Stars appear as rectangles instead of circles in spatial scans, as the light is smeared in the direction of the scan. This technique allows high-SNR observations of bright sources to be obtained without saturating any pixels. Our 380 × 20 px apertures are indicated in white.
Paper: Peculiar Orbital Characteristics of Earth Quasi-Satellite 469219 Kamo‘oalewa: Implications for the Yarkovsky Detection and Orbital Uncertainty Propagation
Authors: Shoucun Hu, Bin Li, Haoxuan Jiang, Gang Bao, Jianghui Ji
Figure caption: The left panel shows the variations of Δλ for the six Earth quasi-satellites over 100 yr with the same initial states. The right panel shows the evolution of the Yarkovsky detection S/N with different observational time spans with simulated optical astrometry for the quasi-satellites. The initial epochs are set to 1950 January 1 for 2013 LX28 and 2000 January 1 for the other five asteroids, to ensure that the 100 yr time spans are within the quasi-satellite periods. The black dashed lines denote those results for Kamo‘oalewa without considering the gravity of Earth. Here A 2 is assumed to be −1.0 × 10−13 au day−2.