adsabs/AstroCLIMB huggingface dataset:
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Top panel: Host star metallicity as a function of planet mass. Bottom panel: [Mg/Fe] of planet-hosting stars as a function of planet mass. The errors in metallicity and Mg abundances are represented by the standard error of the mean, whereas the errors in planet mass are represented by the standard deviation in each bin.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Toomre diagram for the current sample of planet-hosting stars. The blue and red circles represent the locus of ν pec for the small and giant planet hosts. The area enclosed by inner circles has ∼50% of stars population, while the outer circles capture ∼80% of the population in each category.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Distribution of ν pec and σ tot for the planet-hosting stars obtained from Monte Carlo simulation. The vertical-dashed lines represent the median of the distribution.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Distribution of p-values from the 1,00,000 AD test performed using Monte Carlo method. The black-dashed line represents the p = 0.05, below which two distributions are considered to be statistically different.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Hertzsprung–Russell Diagram for Stars with Determined Ages in this Study. The color bar on the left-hand side indicates the planet mass in units of M  j .
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Comparison of the [Fe/H] values from GAIA GSP-Spec module and the HARPS sample. The black line is the x = y line and the color bar on the right-hand side represents the effective temperature of the star.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Age distribution for a sample of 807 planet-hosting stars from the MIST isochrone models (binned at 1.25 Gyr). The vertical lines represent the median age.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Galactic orbital parameters for the small and giant planet-hosting stars. Top panel: Eccentricity distribution for the planet-hosting stars (binned at 0.1 dex). Bottom panel: Z max distribution for the different populations of exoplanet-hosting stars (binned at 0.1 Kpc). The vertical lines represent the median of the distribution for the small and giant planet hosts.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Planet-mass distribution for the sample with host stars listed in the GAIA archive.
Paper: Detecting and Characterizing Mg II Absorption in DESI Survey Validation Quasar Spectra
Authors: Lucas Napolitano, Agnesh Pandey, Adam D. Myers, Ting-Wen Lan, Abhijeet Anand, Jessica Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Rebecca Canning, Chiara Circosta, Axel De La Macorra, Peter Doel, Sarah Eftekharzadeh, Victoria A. Fawcett, Andreu Font-Ribera, Juan Garcia-Bellido, Satya Gontcho A Gontcho, L. Le Guillou, Julien Guy, Klaus Honscheid, Stephanie Juneau, T. Kisner, Martin Landriau, Aaron M. Meisner, Ramon Miquel, J. Moustakas, Will J. Percival, J. Xavier Prochaska, Michael Schubnell, Gregory Tarlé, B. A. Weaver, Benjamin Weiner, Zhimin Zhou, Hu Zou, Siwei Zou
Figure caption: A visualization of the doublet-detection step of our pipeline. Detected Mg II systems are shown in the gray-outlined boxes and the search limit of our approach is shown by the vertical-black line. Top: A sample spectrum from DESI that features seven separate Mg II absorption systems. The flux and error spectrum coadded at the boundaries of the three DESI spectrographs are shown. Middle: The same spectrum now shown with an applied Gaussian smoothing kernel (blue) and estimated median-filter continuum (green). Bottom: A residual taken from subtracting the median-filter-estimated continuum from the Gaussian-smoothed data. Note that the seven Mg II absorption systems appear as positive lines.
Paper: Detecting and Characterizing Mg II Absorption in DESI Survey Validation Quasar Spectra
Authors: Lucas Napolitano, Agnesh Pandey, Adam D. Myers, Ting-Wen Lan, Abhijeet Anand, Jessica Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Rebecca Canning, Chiara Circosta, Axel De La Macorra, Peter Doel, Sarah Eftekharzadeh, Victoria A. Fawcett, Andreu Font-Ribera, Juan Garcia-Bellido, Satya Gontcho A Gontcho, L. Le Guillou, Julien Guy, Klaus Honscheid, Stephanie Juneau, T. Kisner, Martin Landriau, Aaron M. Meisner, Ramon Miquel, J. Moustakas, Will J. Percival, J. Xavier Prochaska, Michael Schubnell, Gregory Tarlé, B. A. Weaver, Benjamin Weiner, Zhimin Zhou, Hu Zou, Siwei Zou
Figure caption: Nightly coadded QSO spectra grouped by Mg II absorption redshift and TSNR2 value. Bins are colored according to the completeness, i.e., the number of Mg II doublets recovered compared to the number of expected absorbers. Within each bin, the completeness is quoted as P and the number of expected absorbers is quoted as N. Note that, as in Figure 3, the highest bin groups all spectra with a TSNR2 exceeding 140.
Paper: Detecting and Characterizing Mg II Absorption in DESI Survey Validation Quasar Spectra
Authors: Lucas Napolitano, Agnesh Pandey, Adam D. Myers, Ting-Wen Lan, Abhijeet Anand, Jessica Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Rebecca Canning, Chiara Circosta, Axel De La Macorra, Peter Doel, Sarah Eftekharzadeh, Victoria A. Fawcett, Andreu Font-Ribera, Juan Garcia-Bellido, Satya Gontcho A Gontcho, L. Le Guillou, Julien Guy, Klaus Honscheid, Stephanie Juneau, T. Kisner, Martin Landriau, Aaron M. Meisner, Ramon Miquel, J. Moustakas, Will J. Percival, J. Xavier Prochaska, Michael Schubnell, Gregory Tarlé, B. A. Weaver, Benjamin Weiner, Zhimin Zhou, Hu Zou, Siwei Zou
Figure caption: Visualization of Equation (4). The ratios between the widths and amplitudes of the two lines of the Mg II doublet are plotted for all systems in the visually inspected set following the removal of any systems with positive amplitudes. True Mg II systems are shown in blue and false systems are shown in orange. Note that not all points are shown. Top Right-hand Inset: Density plot indicating that the distribution is highly concentrated around [1.1, 1.1].
Paper: Detecting and Characterizing Mg II Absorption in DESI Survey Validation Quasar Spectra
Authors: Lucas Napolitano, Agnesh Pandey, Adam D. Myers, Ting-Wen Lan, Abhijeet Anand, Jessica Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Rebecca Canning, Chiara Circosta, Axel De La Macorra, Peter Doel, Sarah Eftekharzadeh, Victoria A. Fawcett, Andreu Font-Ribera, Juan Garcia-Bellido, Satya Gontcho A Gontcho, L. Le Guillou, Julien Guy, Klaus Honscheid, Stephanie Juneau, T. Kisner, Martin Landriau, Aaron M. Meisner, Ramon Miquel, J. Moustakas, Will J. Percival, J. Xavier Prochaska, Michael Schubnell, Gregory Tarlé, B. A. Weaver, Benjamin Weiner, Zhimin Zhou, Hu Zou, Siwei Zou
Figure caption: Left-hand panel: Heatmap of synthetic absorber recovery results. Decreases in completeness at low values of ﹩{W}_{0}^{\lambda 2796}﹩ as well as at low redshift, and at certain redshifts corresponding to known skylines can clearly be seen. Top Right-hand Panel: Average completeness as a function of ﹩{W}_{0}^{\lambda 2796}﹩ Bottom Right-hand Panel: Average completeness as a function of absorber redshift.
Paper: Detecting and Characterizing Mg II Absorption in DESI Survey Validation Quasar Spectra
Authors: Lucas Napolitano, Agnesh Pandey, Adam D. Myers, Ting-Wen Lan, Abhijeet Anand, Jessica Aguilar, Steven Ahlen, David M. Alexander, David Brooks, Rebecca Canning, Chiara Circosta, Axel De La Macorra, Peter Doel, Sarah Eftekharzadeh, Victoria A. Fawcett, Andreu Font-Ribera, Juan Garcia-Bellido, Satya Gontcho A Gontcho, L. Le Guillou, Julien Guy, Klaus Honscheid, Stephanie Juneau, T. Kisner, Martin Landriau, Aaron M. Meisner, Ramon Miquel, J. Moustakas, Will J. Percival, J. Xavier Prochaska, Michael Schubnell, Gregory Tarlé, B. A. Weaver, Benjamin Weiner, Zhimin Zhou, Hu Zou, Siwei Zou
Figure caption: The population of healpix coadded quasar spectra TSNR2 values. The numbers above/below the blue/orange bars indicate population size. The right-hand bin includes all spectra with TSNR2 > 140.
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: Map of distortion measurements for M15 observations obtained in 2021. Each vector is one measurement of a single star with the base of the arrow at the observed OSIRIS detector pixel coordinate and the arrow amplitude and direction showing the positional differences between OSIRIS positions and Hubble reference stars. Outliers are marked in red and excluded from the distortion fit. Left: distortion measurements produced by the fitting procedure, which minimizes the average distortion across the frame. Right: distortion measurements with a translation applied to set the distortion at the center of the frame to zero, revealing OSIRIS’s distortion pattern.
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: The steps involved in our method to calculate the distortion solution. The observations are iteratively matched to the reference frame to identify the correct four-parameter transformation (steps 2–5), and the reference frame is iteratively updated to remove any residual distortion in it (step 8).
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: The dither pattern of observations in Table 1. Each marker shows the R.A. and decl. of the telescope for a frame, calculated from the header keywords TARGRA+RAOFF and TARGDEC+DECOFF, and given in arcseconds relative to the first observation of the night. The direction of the arrow shows the position angle (PA) of the observation. The color bar corresponds to the frame number of each image on that night. Typically, three frames are taken at each pointing.
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: The 5th-order Legendre polynomial fit to the observed distortion measurements from Figure 6. This Legendre polynomial is used as the final distortion model for the 2021 data.
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: A diagram of the Keck I telescope, showing the optical path through to OSIRIS. The precision calibration unit (PCU) is mounted at the front of the bench. The deformable mirror and the dichroics that split light off to the wavefront sensor and TRICK could potentially be sources of distortion (modified from Figure 1 of Wizinowich et al. 2020).
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: The difference between each higher-order polynomial model (e.g., Figure 7) and the 2nd-order model, for 2021. The colors correspond to the angle of the vector.
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: A reduced and cleaned OSIRIS image of M15 in the Kn3 band from UT 2021 October 24.
Paper: An Optical Distortion Solution for the Keck I OSIRIS Imager
Authors: Matthew S. R. Freeman, Jessica R. Lu, Jim Lyke, Abhimat Gautam, Renate Kupke, Andrea Ghez, Shoko Sakai, Jay Anderson, Andrea Bellini
Figure caption: An example of differential atmospheric refraction (DAR) for one OSIRIS frame from 2021 October 24. DAR produces a compression in the direction of the parallactic angle q.
Paper: Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B
Authors: Ya-Lin Wu, Yu-Chi Cheng, Li-Ching Huang, Brendan P. Bowler, Laird M. Close, Wei-Ling Tseng, Ning Chen, Da-Wei Chen
Figure caption: The FU Tau system and the neighboring field stars. This image was made by stacking all frames in December 6. The Barnard 215 dark cloud (Barnard et al. 1927) obscures many field stars from the central to the lower-right regions. 2MASS J04241447+2506106 is our Hα reference star. North is up and east is left.
Paper: Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B
Authors: Ya-Lin Wu, Yu-Chi Cheng, Li-Ching Huang, Brendan P. Bowler, Laird M. Close, Wei-Ling Tseng, Ning Chen, Da-Wei Chen
Figure caption: Top: the calibrated light curve of 2MASS J04241447+2506106 indicates that it only has 0.3%–0.7% variations at Hα over the course of our observations. Bottom: the ZTF r-band monitoring over 1670 days shows that 2MASS J04241447+2506106 is stable to a 1.4% level.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: Comparison of H I turbulence measures and SFH on a 400 pc scale: Spearman’s correlation coefficient (ρ) vs. log time, or the correlation between a time bin’s star formation rate and the H I turbulence measures. The 1σ errors based on bootstrapping are the blue shaded region. The associated P-value is listed above each point. The subfigures are the correlation between the SFH and the velocity dispersion and energy surface density of (a) and (b) the Gaussian superprofile, (c) and (d) the superprofile’s wings, and (e) and (f) the second moment map. For the H I turbulence measures in (a), (b), (e), and (f), there is an indication of a correlation with the SFR about 70–140 Myr ago, which is highlighted by the gray shaded region. Additionally, we note the indication of a correlation between the SFR 5–10 Myr ago and the turbulence measures of the second moment map (the rightmost time bin).
Paper: OGLE-2016-BLG-1195 AO: Lens, Companion to Lens or Source, or None of the Above?
Authors: Andrew Gould, Yossi Shvartzvald, Jiyuan Zhang, Jennifer C. Yee, Sebastiano Calchi Novati, Weicheng Zang, Eran O. Ofek
Figure caption: Data (colored points) and two representative models of OGLE-2016-BLG-1195, a central-caustic model (black) that was originally found in the discovery papers (Bond et al. 2017; Shvartzvald et al. 2017), and a new resonant-caustic model. The cumulative Δχ 2 function shows that the new resonant model is strongly disfavored, primarily due to its failure to match the anomalous region, 7569.08 – 7569.22. However, rejection of this model would have been less decisive based on the partial data sets in each discovery paper. See also Figure 4.
Paper: OGLE-2016-BLG-1195 AO: Lens, Companion to Lens or Source, or None of the Above?
Authors: Andrew Gould, Yossi Shvartzvald, Jiyuan Zhang, Jennifer C. Yee, Sebastiano Calchi Novati, Weicheng Zang, Eran O. Ofek
Figure caption: Illustration of four models (corresponding to four degenerate solutions for the microlens parallax  π  E), in which the “other star” is assumed to be a companion to the host. The green arrows show the vector motion over 4.12 yr relative to the source (at the origin) for the companion (upper part of diagram) and host (lower part of diagram) for the four solutions, which are labeled sequentially by decreasing π E,N . In all cases, the host is superposed with the source in 2016, while the companion is at the location measured by Vandorou et al. (2023) in 2020.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: Comparing H I turbulence measures and SFH on a 560 pc scale. As in Figure 7, the subfigures are the correlation between the SFH and the velocity dispersion and energy surface density of (a) and (b) the Gaussian superprofile, (c) and (d) the superprofile’s wings, and (e) and (f) the second moment map. For the 560 pc scale, we note a possible correlation between the SFR 5–10 Myr ago and the turbulence measures of the second moment map (the rightmost time bin), and peaks at 100–140 Myr for ΣH I from the Gaussian superprofile and wings. As in Figure 7, the 70–140 Myr time range is highlighted by the gray shaded region.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: Comparing H I turbulence measures and SFH on a 800 pc scale. As in Figure 7, the subfigures are the correlation between the SFH and the velocity dispersion and energy surface density of (a) and (b) the Gaussian superprofile, (c) and (d) the superprofile’s wings, and (e) and (f) the second moment map. For the 800 pc scale the only correlation we note is a possible correlation between the SFR 5–10 Myr ago and the turbulence measures of the second moment map (the rightmost time bin). As in Figure 7, the 70–140 Myr time range is highlighted by the gray shaded region.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: Spearman’s correlation coefficient (ρ) vs. log time, or how correlated the star formation rate at a given time is with the Hα velocity dispersion. The 1σ errors based on bootstrapping are the blue shaded region. The associated P-value is listed above each point. For σ Hα , we find weak evidence of a possible correlation between the velocity dispersion and the SFR in the 10–25 Myr ago bin.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: A representative superprofile for a region in UGC 4305. The black line is the H I flux of the region corrected for rotational broadening and the Gaussian fit is shown in red. The error on the data is shaded gray, while wings of the H I profile are shaded red. The wings represent the high-velocity, low-density gas that a single Gaussian does not fit.
Paper: OGLE-2016-BLG-1195 AO: Lens, Companion to Lens or Source, or None of the Above?
Authors: Andrew Gould, Yossi Shvartzvald, Jiyuan Zhang, Jennifer C. Yee, Sebastiano Calchi Novati, Weicheng Zang, Eran O. Ofek
Figure caption: Results of a “grid search” for solutions in which (s, q) are held fixed on a grid of values, while the remaining five parameters are allowed to vary. The two “central-caustic” solutions that were previously discovered (Bond et al. 2017; Shvartzvald et al. 2017) were recovered, but two additional “resonant-caustic” solutions were also discovered. Full analysis of the combined data set (Table 2) rules out these solutions. The boundaries between the central-caustic and resonant-caustic regimes are indicated by dashed lines.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Histograms of the derived rotation periods for objects with more than 200 detections within Cycle 1. The red histogram describes small objects with H > 15.5, and the blue histogram describes large objects with H < 13.5.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Histogram of the apparent b/a axis ratios for asteroids as suggested by their light-curve amplitudes. The relative lack of spherical objects represented in this plot is due to biases discussed in the text. We find that 5% of the objects have high-amplitude light curves corresponding to b/a mean axis ratios of <0.4.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Histograms of the derived light-curve amplitudes for objects with more than 200 detections within Cycle 1. The red histogram describes the inner main belt at 2 au < a < 2.5 au, and the blue histogram describes the outer main belt at 3 au< a < 3.5 au.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Histograms of the derived light-curve amplitudes for objects with more than 200 detections within Cycle 1. The red histogram describes small objects with H > 15.5, and the blue histogram describes large objects with H < 13.5.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Histogram of the derived amplitudes from Cycle 1 of TESS for 10,470 objects. The amplitudes presented here are uncorrected for the PAA effect.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Histograms of the derived rotation periods for objects with more than 200 detections within Cycle 1. The red histogram describes the inner main belt at 2 au < a < 2.5 au, and the blue histogram describes the outer main belt at 3 au < a < 3.5 au.