adsabs/AstroCLIMB huggingface dataset:
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: MNI score as a function of the minimum cluster size. The HDBSCAN result is compared against CAMS classification for the ORBIT (solid blue), GEO (dashed red), and LUTAB (dashed–dotted green) vectors. Darker shades correspond to the eom selection method, while lighter shades indicate the leaf method.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Silhouette score as a function of the minimum cluster size. Results are shown for the ORBIT (solid blue), GEO (dashed red), and LUTAB (dashed–dotted green) vectors. Darker shades correspond to the eom selection method, while lighter shades indicate the leaf method. Markers denote the results at minimum cluster size of 100 for each vector: ORBIT (dot), GEO (square), and LUTAB (diamond), with accompanying horizontal lines for reference.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the α-Capricornids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Southern Taurids.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Mean features of the Geminids.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Top: optical speckle imaging and sensitivity curves for the SAI observations, with a medium-band filter centered on 625 nm. Center: optical speckle imaging and sensitivity curves for the Gemini observations; the 562 nm sensitivity is shown in blue, and the 832 nm sensitivity curve is shown in red. Bottom: Near-IR AO imaging and sensitivity curves for the Palomar observations, in a narrowband Kcont filter centered on 2.29 μm. Insets: the central portions of each image.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: The fits to the TESS light curves, with Sector 19 on the left, Sector 59 in the middle, and Sector 86 on the right. Top: the PDCSAP SPOC data, and the best-fit GP detrending model in green. Middle: the detrended data, with the best-fit transit models for TOI-6054b and TOI-6054c plotted in blue and purple, respectively. Bottom: the residuals after subtracting the GP model and the transits.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Left: the best-fit stellar SED for TOI-6054. The data are in black, the best fits to the data are in blue, and the best-fit stellar model is in orange. Error bars on both the data and the fit points are smaller than the points. Right: the stellar evolution track for the best-fit stellar mass is plotted in green, with TOI-6054’s Teff and Lbol,S plotted in black. The end of the main sequence on this track, as defined by the MIST evolutionary phase, is plotted in blue. An arrow is plotted on the track indicating the forward direction in time.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: Top: the RV data are shown vs. time in black, with the best-fit combined RV model shown in green. The RV contribution from TOI-6054b is plotted as a blue dashed line, the contribution from TOI-6054c is plotted as a purple dashed line, and the contribution from the background trend is plotted as a black dotted line. Residuals are plotted below. Lower left: the phase-folded best-fit RV model for TOI-6054b. The data plotted have had the background and TOI-6054c contributions subtracted. Residuals are plotted below. Lower right: the phase-folded best-fit RV model for TOI-6054c. The data plotted have had the background and TOI-6054b contributions subtracted. Residuals are plotted below.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: The transit timing variations (TTVs) between the best-fit transit times and the linear ephemeris. We find that there is no significant evidence to include TTVs in our reported fit results. The top row shows the TTVs of TOI-6054b, while the bottom row shows those of TOI-6054c. The time axis is split into three columns for Sector 19 (left), Sector 59 (middle), and Sector 86 (right) for visual clarity.
Paper: A Pair of Dynamically Interacting Sub-Neptunes around TOI-6054
Authors: Maxwell A. Kroft, Thomas G. Beatty, Ian J. M. Crossfield, Joseph R. Livesey, Juliette Becker, Jacob K. Luhn, Paul Robertson, Allyson Bieryla, David R. Ciardi, Catherine A. Clark, Maria V. Goliguzova, Steve B. Howell, Jack J. Lissauer, Colin Littlefield, Michael B. Lund, Boris S. Safonov, Joseph M. Akana Murphy, Natalie M. Batalha, Malik Bossett, Jonathan Brande, Tansu Daylan, Courtney Dressing, Anna Gagnebin, Daniel Huber, Howard Isaacson, Stephen R. Kane, Laura Kreidberg, David W. Latham, Rafael Luque, Alex S. Polanski, Pranav H. Premnath, Maleah Rhem, Claire J. Rogers, Emma V. Turtelboom
Figure caption: The phase-folded best-fit transit models for the TESS data. The upper two rows are the Sector 19 data and their fit residuals, and the lower two are the Sector 59 and 86 data and their fit residuals. The left column is the TOI-6054b transit model, and the right column is the TOI-6054c transit model. Binned data are plotted in black with error bars for clarity.
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption:                         (a) Two-dimensional density distribution of our analyzed GCs. Each GC, labeled in the top right, contains its surface density distribution colored by σ level on the top row. The contours indicate 1, 2, and 3σ levels. Additionally plotted are the GC orbit (forward/backward orbits are indicated by a solid/dashed gray line) based on MWpotential2014  (J. Bovy 2014), the direction toward the Galactic center (dotted black line), the GC Jacobi radius (green circle), and the Galstreams stream track of any extended structure (cyan line). Stream track labels: I21, R. Ibata et al. (2021); P21, C. G. Palau & J. Miralda-Escudé (2021). (b) Two-dimensional density distribution of our analysis GCs. A continuation of Figure 4. Stream track labels: S20, A. Sollima (2020); I21, R. Ibata et al. (2021).
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption:                         (a) Position angle as a function of radius for our GCs with 2D surface density distributions. Each GC, labeled in the top-right corner, has its radial position angle profile demonstrated by the blue points. Also demonstrated are the forward/backward orbits as solid/dashed gray horizontal lines, and the position angle of the eTidal N-body models is demonstrated by the solid green line, where the shaded region shows the 1σ uncertainties of the measurements. Last, the GC tidal and Jacobi radii are shown through dotted and dashed vertical lines, respectively. (b) Position angle as a function of radius for our GCs with 2D surface density distributions. A continuation of Figure 7.
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption:                         Demonstration of the eTidal GC N-body models (top row) and the Y. Chen et al. (2025) particle spray models in both forward and backward trajectories within the four selected MW potentials: McMillan17  (P. J. McMillan 2017), Cautan20  (M. Cautun et al. 2020), and MWpotential2014  (J. Bovy 2014) both with and without a W. Dehnen (1999) bar, and randomly selected N = 10,000 particles from GEMS (bottom row; S. M. Grondin et al. 2024). The forward trajectory, with its leading tail points, is marked in green, and the backwards trajectory, with its trailing points, is marked in blue. They are overplotted on the 2D density profiles of the four GCs, NGC 1261, NGC 1851, NGC 2808, and NGC 6934 (left to right columns), and the Galstreams stream track is also presented. The density profiles, contours, and Galstreams track are the same as what is presented in Figure 4.
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption: Demonstration of the separation between extended tidal structure that is highly constrained (green), and that which is less constrained (red), designated by σθ as a function of heliocentric distance, R⊙. The pointing direction of the arrows (triangles) indicates whether a GC last passed the pericenter (apocenter) of its orbit. The separation of σθ = 8 is shown by the horizontal dashed line.
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption:                         (a) The same as Figure 4 but with the addition of the conservative selection of stars denoted by the green points. Stream track labels: I21, R. Ibata et al. (2021); P21, C. G. Palau & J. Miralda-Escudé (2021). (b) A continuation of Figure 10. Stream track labels: S20, A. Sollima (2020); I21, R. Ibata et al. (2021).
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption:                         (a) The same as Figure 4, with the addition of eTidals N-body simulations of disrupting GCs, demonstrated with the gray points. Stream track labels: I21, R. Ibata et al. (2021); P21, C. G. Palau & J. Miralda-Escudé (2021). (b) A continuation of Figure 6. Stream track labels: S20, A. Sollima (2020); I21, R. Ibata et al. (2021).
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption: Corner plot of GC parameters used to explore potential predictors of extended structure and its form. Points share colors and triangle orientations with Figure 5. NGC 104 is marked with a cross; NGC 1261, NGC 1851, NGC 2808, and NGC 6934 are circled in black. Parameters, from top to bottom: orbital phase, eccentricity, heliocentric distance, mass-loss fraction, and relaxation time; from left to right: [Fe/H]PGS, orbital phase, eccentricity, heliocentric distance, and mass-loss fraction.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: The TOI-6303b and TOI-6330b phase-folded photometric observations. The TESS phase-folded light curves are shown in subfigures (a) and (b) for Sectors 18 and 58, respectively. The black points show the detrended data and the purple line details the model with a 1σ uncertainty in the translucent-purple region. We show the median uncertainty at −0.07 days. The red models for the TESS light curves indicate a floating dilution term, which is constrained with the data sets in purple.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: Left: An RV time series for TOI-6303 (top) and TOI-6330 (bottom) as observed by HPF. The model best fit is designated by the purple line with a lighter purple indicating the 16%–84% uncertainty. The error bars along the time series model are difficult to see because they are small compared to the y-axis spread. For TOI-6303, the observations with larger error bars are one 15 minutes exposure while the rest are two binned 15 minutes exposures (see Table 2). Right: Phase-folded HPF RVs on best-fit orbital parameters (top: TOI-6303, bottom: TOI-6330). We set the eccentricity and argument of periastron to float. TOI-6303 is consistent with a circular orbit, while TOI-6330 shows an eccentric orbit.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: The TOI-6330 ZTF periodogram with the ZTF-r filter. The teal and blue vertical lines detail the 1 and 28 days periods, respectively. The red highlight shows a peak period at 36.29 days believed to be from stellar activity. The horizontal dashed lines detail the 10%, 5%, and 1% FAPs from bottom to top. The ZTF data is obtained directly from the ZTF database via IRSA.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: The TOI-6303 and TOI-6330 light curves processed using eleanor for TESS Sectors 18 (the top subfigure with an 1800 s exposure time) and 58 (the bottom subfigure with a 200 s exposure time). The top panel of each sector’s light curve is a rotation Gaussian process kernel that is used to remove both astrophysical and instrumental systematics in the light curve labeled RotationTerm from celerite2 (seen in red). The bottom panel is the best-fit Gaussian process-subtracted photometry for the transit of TOI-6303b and TOI-6330b.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: Top: 5σ processed contrast curve for TOI-6330 observed from NESSI in the Sloan z’ and r’ filters. Bottom: 5σ processed contrast curve for TOI-6330 observed from ShaneAO in the Ks-band.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: Top: 5σ processed contrast curve for TOI-6303 observed from NESSI in the Sloan z’ and r’ filters. Bottom: 5σ processed contrast curve for TOI-6303 observed from ShaneAO in the Ks-band.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: Left: TOI-6303b and TOI-6330b (seen in blue with a ring) on a planetary mass vs. stellar mass plot. The red circles designate transiting GEMS, the red triangles indicate RV-only GEMS, the gray circles indicate FGK planetary companions (NASA Exoplanet Archive; R. L. Akeson et al. 2013), and the red squares are true mass-measured RV objects where astrometry is used to break the sini degeneracy (G. Stefansson et al. 2025). The gray region between 4 and 10 MJ indicates a sparse region of planetary discoveries made where there is a transition between two major planetary formation paths, core accretion and GI (K. C. Schlaufman 2018). The dotted line indicates the 13 MJ limit where deuterium burning occurs initiates (A. L. D. Etangs & J. J. Lissauer 2022). Right: The mass ratio vs. stellar mass plot for TOI-6303b and TOI-6330b (seen in blue with a purple ring).
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: Left: The eccentricity vs. semimajor axis over the stellar radius for TOI-6303b and TOI-6330b (seen in blue with a purple ring). The red circles indicate the transiting M-dwarf planetary companions and the gray circles are the FGK transiting companions as used in Figure 7. Both TOI-6303b and TOI-6330b are at similar values for a/R* (26.95 ± 0.79 and 25.55 ﹩{}_{-0.59}^{+0.63}﹩, respectively) but have different eccentricity values (0.02 ± 0.02 and 0.34 ± 0.01). Right: Similar to left plot but evaluating eccentricity vs. mass ratio with their Mp/M* being 1.16% for TOI-6303b and 1.79% for TOI-6330b.
Paper: Searching for GEMS: Two Super-Jupiters Around M Dwarfs that May have Formed via Gravitational Instability
Authors: Andrew Hotnisky, Shubham Kanodia, Jessica Libby-Roberts, Suvrath Mahadevan, Caleb I. Cañas, Arvind F. Gupta, Te Han, Henry A. Kobulnicky, Alexander Larsen, Paul Robertson, Michael Rodruck, Gudmundur Stefansson, William D. Cochran, Megan Delamer, Scott A. Diddams, Rachel B. Fernandes, Samuel Halverson, Leslie Hebb, Andrea S.J. Lin, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab
Figure caption: We show TOI-6303b and TOI-6330b (seen in blue with a purple ring) on in the planet mass–radius plane. The red circles designate transiting GEMS and the gray circles indicate FGK planetary companions. We removed NGTS-1b from this plot due to its large uncertainties on the planetary radius from its grazing transit.
Paper: Drone Beam Mapping of the TONE Radio Dish Array
Authors: Emily R. Kuhn, Will Tyndall, Benjamin R. B. Saliwanchik, Anna Rose Polish, Maile Harris, Laura B. Newburgh
Figure caption: TONE at Green Bank Radio Observatory (GBO). The eight active dishes are marked with X’s, color-coded by whether the dish is instrumented with an HIRAX or CHIME feed. The four dishes used for drone beam mapping are marked with a yellow circle and numbered. The drone takeoff location and “Dish 0” location (which served as the coordinate system origin) are also marked. The inset table provides an alternative description of the dish numbers, input numbers, and feeds used for the measurements.
Paper: Drone Beam Mapping of the TONE Radio Dish Array
Authors: Emily R. Kuhn, Will Tyndall, Benjamin R. B. Saliwanchik, Anna Rose Polish, Maile Harris, Laura B. Newburgh
Figure caption: Upper panel: a rendering of the Matrice 600 Pro, and a photograph of the payload with components indicated (described in more detail in Section 2.1). The payload consists of the calibrator source, a GPS to provide a pulse synchronized to PPS, batteries for the source and components, and the transmission antenna. Lower panel: schematic of transmission signal RF chain.