adsabs/AstroCLIMB huggingface dataset:
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: Left panel: slices through the beam at the origin, all dishes, at 448 MHz, for the north-polarized inputs. Right panel: slices through the beam for the east-polarized inputs. Beam power data are shown as filled circles with 1σ errors. Open circles indicate data with five or fewer data points, and thus, we do not report statistical errors. Shaded regions for the main beam (﹩\phi \lt \pm 3\mathop{.}\limits^{^\circ }5﹩), first sidelobes (9∘ > ϕ > 13∘), and second sidelobes (22∘ > ϕ > 25∘) indicate the region we average over to provide the standard deviations for the noise values given in the text. Vertical lines are drawn at 12∘ and 25∘, corresponding to the radial lines in Figure 7. The same features present in Figure 7 are also clear here: we have a high-significance measurement of the main beam and first sidelobe region, a detection of power in the second sidelobe region, and are dominated by noise where the signal level is small. The data has not been corrected for the beam of the transmitting antenna, and thus, the first sidelobe is −0.7 dB suppressed and the second sidelobe −2.7 dB suppressed here, as discussed in the text.
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: The top row shows 2D beam measurements in polar coordinates for north-polarized inputs for all four dishes considered in this paper at frequency 448 MHz after processing (see Section 3). The bottom row shows 2D beam measurements for east-polarized inputs. Circles overlaid at 12∘ and 25∘ indicate the approximate locations of the first and second sidelobes. The data are normalized, and shown in logarithmic scale.
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: FWHM values from coadded maps for all inputs as a function of frequency, with values from simulations (black crosses) and values from on-sky TONE measurements included for comparison. The top panel shows the width along the east–west direction for the north-polarized inputs. The second-from-top panel shows the width along the north–south direction for the north-polarized inputs. The third-from-top panel shows the width in the east–west direction for the east-polarized inputs. The bottom panel shows the width in the north–south direction for the east-polarized inputs. Also indicated is the diffraction limit for a uniformly illuminated dish, given as 1.03﹩\frac{c}{\nu D}﹩ for a D = 6 m diameter dish at frequency ν and speed of light c.
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: Each panel shows the beam measured from each of the flights used in this analysis for a single dish and frequency after the per-flight processing performed in Section 3. The cardinal direction “north” is vertical; some flights were oriented north–south and others east–west, and color indicates beam amplitude. The polarization during the flight was either aligned north–south (“N-pol”) or east–west (“E-pol”). The smaller grids target a measurement of the main beam, while the larger grids target a measurement of sidelobes. Additional details on the flights are given in Table 2.
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: Th top row shows the standard deviation per pixel, divided by the value of the pixel, for all north-polarized inputs, shown in polar coordinates. The bottom row shows the standard deviation divided by the value of the pixel, for the east-polarized inputs. Pixels with fewer than five counts have been excluded. The color scale has been inverted compared to Figure 7 to better highlight the regions with lower signal to noise (orange and yellow regions). We find 10% variations in the main beam and first sidelobe regions, and 25% variations in the second sidelobe region.
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: Beam power vs. angle in a single 1D cut through the beam at the origin for frequency 448 MHz and a north-polarized input. The left panel shows a 1D cut through the north–south direction. The right panel shows a 1D cut through the east–west direction. Each flight is shown as a different color after the normalization correction procedure described in Section 3.5. As described, the amplitude correction procedure matches the average signal power in the first sidelobe region. As a result, the main beam flights have good signal in the main beam and the sidelobes, while the brighter sidelobe flights will look flat within the main beam where the signal was saturated.
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: Counts per pixel (“hit map”) after gridding, shown in polar coordinates at 448 MHz. The left panel shows the east-polarized input for Dish 0. The right panel shows the north-polarized input for Dish 0. The hit map is input and frequency dependent. In polar coordinates, counts range from 0–30; typical values are 15. There are fewer east-polarized flights, and so those hit maps are sparser than the north-polarized flight hit maps. We mask pixels with fewer than 5 counts to indicate where the standard deviation cannot be calculated.
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: One-dimensional slice of simulated and measured TONE beams at 450 MHz, (top) for θ = 0, (middle) for θ = 45, and (bottom) for θ = 90. θ = 0 corresponds to north. The data from all dishes are shown in color, and the simulation is shown in black. As discussed in Section 4.5, we have not included the effects of the transmitting antenna beam (which would decrease our measurement of the first sidelobes by 0.7 dB) nor a geometrical projection effect (which would increase the first sidelobes by 0.2 dB).
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: A single transit of the drone through near the center of the beam for Dish 0, north-polarized input from flight 625 at frequency 448 MHz. The colors indicate points in the flight where the background fitting found the signal was on (black), off (purple), or partially on and partially off (peach). Only “on” data are used in the following analysis after background subtraction.
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-left panel: signal amplitude vs. yaw angle at 448 MHz for Dish 0, populated with an HIRAX-style feed. The colors indicate the location of the 360∘ rotation (nominal center, and four locations corresponding to 8 m distances in the four cardinal directions, as described in the text). The markers indicate east-polarized and north-polarized inputs. In this panel, the two polarizations are clearly separated by ∼90∘ for all locations in the beam. Upper-right panel: the same frequency, markers, and colors as the left panel, but for Dish 6, instrumented with a CHIME-style feed. The CHIME data are clearly saturated (a flat line) for most locations, but the ∼90∘ difference between polarizations is still apparent for all locations. Middle-left and middle-right panels: the same as above, but for frequency 772 MHz. The CHIME feed continues to show an orthogonal pattern between the two polarizations; however, the HIRAX input shows that the two polarizations are no longer orthogonal, which is true for all locations. Center panel: phase difference between the east-polarization and north-polarization inputs for three dishes populated with HIRAX feeds, for the location +8 m east. At low frequencies below 600 MHz, the phase difference is 90∘, as expected, but diverges at high frequencies. The gray band indicates ±20∘. Lower panel: the phase difference for Dish 6, instrumented with the CHIME feed. Here, the difference is consistently near 90∘ for all frequencies, as expected. The range in this plot is also shown as the gray band in the HIRAX-style feeds in the plot above. The cause of the high-frequency (10 MHz) ripple is unknown.
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-left panel: map of Dish 0, north-polarized input in copolarization, for flight 618 at frequency 448 MHz. The white circle denotes the approximate FWHM of ﹩7\mathop{.}\limits^{^\circ }5﹩. Upper-right panel: copolarized map of Dish 0, east-polarized input for flight 620. Center-left panel: cross-polarized map, with normalization discussed in the text, for Dish 0, north-polarized input. Center-right panel: cross-polarized map for Dish 0 east-polarized input. Lower-left panel: a slice through the center of the beam, now showing north-polarized inputs from all dishes. The copolarized map is shown as circular markers, and the cross-polarized are crosses. The level of cross-polarized is roughly similar across inputs, and the ±8% error bar (as described in the text) is present for the cross-polarized values. Shaded regions show limits from systematics as discussed in the text, for contributions from misaligned polarization angle and the transmitter cross-polarization. Lower-right panel: same as the lower-left panel but for east-polarized inputs. The north-polarized inputs are clearly not systematics limited; however, the east-polarized cross-polarized is low enough that the −20 dB cross-polarized amplitude from the transmitting antenna may be limiting our measurement.
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: Drone RFI measurements at GBO. Shown in this figure are spectra acquired by the TONE telescope while the drone (with onboard calibration source off) is within 5° of zenith pointing per dish (rose line) and the average maximum and minimum value (rose band). RFI from the drone measured in the test chamber with no external RFI is shown in yellow, with the yellow line indicating the average over many positions and the yellow band showing the max and min of those positions. Finally, the spectrum measured through the TONE antenna shows the ambient RFI at GBO (black). The amplitude is arbitrary, and values have been scaled to show them on the same plot. The emission from the drone while the RF source is off can be accounted for by the combination of ambient RFI and known RFI from the chamber 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: Simulated (left column) and measured (center and right columns) beams for the TONE dishes at four frequencies (from top to bottom: 450, 500, 550, and 600 MHz). The left column shows beams simulated using the CST Studio Suite software. The center and right columns show the measured beams for the polarizations nominally oriented north–south and east–west, respectively. Dashed lines have been drawn at the approximate locations of the first and second sidelobes in the measured data (12∘ and 25∘).
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: Each panel shows the evolution of the beam with frequency for three slices (left to right: θ = 0∘, 45∘, and 90∘) for Dish 0, (top is north-polarized input, bottom is east-polarized input). Gaps are a result of the frequency selection described in Section 3. The beamwidth of the main beam is slightly larger at lower frequencies, and the sidelobes shift outward and widen with it. The amplitude of the first sidelobe is similar across frequencies; the amplitude of the second sidelobe is more variable in both angular location (this is also apparent in Figure 7) and as a function of frequency.
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: Panels show the beam maps from all inputs, at frequency 448 MHz, in 2D Cartesian coordinates. In this gridding, an asymmetry in the dip feature between the main beam and first sidelobe is clearly present in all inputs. Dish 0, north-polarization appears to have a symmetric dip which is circular, while both inputs on Dish 7 and Dish 5 have an asymmetry that is aligned ∼35∘ clockwise from north. Both inputs on Dish 8 have an asymmetry that is aligned ∼45∘ counterclockwise from north.
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: Unintended drone RFI emission as measured in the anechoic chamber at GBO. Total unintended emission meets required limits from MeerKAT (shown in red) except in two regions, where the upper bounds exceeded the requirements.
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: Experimental measurement setup inside GBO anechoic chamber. In the foreground is a standard gain horn. In the background is the drone and payload on a custom nonreflective wooden mount.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: The ZTF r and g band light curves and the period analysis for TIC 198459831. In the top panel we show the r- and g-band light curves. The middle panel shows the same light curves but zooms into the shaded region between 59,400 and 59,500 days. The bottom-left panel shows the LS periodogram over the range of 2–100 days. In the bottom right panel we show the phase-folded light curve, folded at the period with the highest LS power, and overlay the sinusoidal model at this period. We also indicate A, the semiamplitude of the oscillation.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: The measured ZTF periods overlaid on the A. McQuillan et al. (2014) Kepler catalog. In the left panel, the orange crosses (N = 6265) indicate targets which did not pass the cut described in the text, while the blue circles (N = 272) indicate those that did. The horizontal streak of periods at ∼29 days is due to the lunar phase and are treated as systematics. The high-temperature cutoff is due to our threshold of Teff < 5300 K and the increase of sources at Teff < 4000 K is due to the way the TESS CTL is produced where the cool-dwarf list is included (P. S. Muirhead et al. 2018). The right panel is the same as the left panel but zoomed into the region where Teff < 4000 K. We can see that our accepted periods trace out the shape present in A. McQuillan et al. (2014).
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: Our custom-extracted light curve (purple) compared to the PDCSAP (orange) and SAP (green) light curves for Sector 23. The top panel shows the raw, normalized light curves, and the middle panel shows the notch-detrended light curves, using a 0.75 day filtering window, with the transits of TOI 2076 e highlighted in teal and a y offset between the extractions for clarity. The raw and detrended custom light curves show significantly less noise than the PDCSAP light curves. The bottom panel shows the phase-folded light curves binned to 5 minute intervals with a y offset for clarity. The gray dashed lines mark the expected ingress and egress. The custom-extraction light curve shows a clear transit-like shape while the PDCSAP light curve is too noisy to detect the transit. The custom extraction light curve is available in machine readable format as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: Candidate comoving stars to TOI 2076 (red x) and TOI 1807 (orange x). All stars identified with FriendFinder are shown as colored points. Stars identified as a member of Crius 224 from L. Moranta et al. (2022) are marked as a square, and stars identified as a member in the GAPS survey (D. Nardiello et al. 2022; M. Damasso et al. 2024) are outlined in purple. Stars that fall into all three black, dashed lined regions are used in the age analysis. Stars not used in the analysis but identified as candidate members are shown in lower opacity.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: Color–magnitude diagram of likely members of Crius 224 (black circles) including TOI 2076 (red star) compared to isochrones from PARSEC. The green lines are random samples from the MCMC posterior. Circles are colored by their outlier probability (mixture weight). We show 125 Myr (red dashed) and 500 Myr (blue dashed) lines for reference. The lack of pre-main-sequence M dwarfs rules out ages ≲150 Myr, while higher ages are ruled out by the A star HD 153808.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: (Left) TESS light curve binned to 10 minutes intervals and phase-folded (gray points) with the full (unbinned) TESS light curve phase folded and binned to 15 minutes intervals for clarity (purple points). The best-fit transit model is shown as the bright, opaque red line with 25 model fits pulled from the posterior shown as the dark, translucent red lines. The best-fit GP stellar variability model has been removed from the data and transit model. (Right) Representative section of the TESS light curve (gray points) with the best-fit GP model (red line). Transits of TOI 2076 e are highlighted in purple, and transits of TOI 2076 b, c, and d are highlighted in pink, green, and blue, respectively.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: The rotation periods of the candidate comoving stars (purple circles) against color (as a proxy for stellar type). Only the high-quality, high-reliability rotation periods are shown. TOI 2076 is marked as the red x, and TOI 1807 is marked as the orange x. The rotation sequence for Pleiades (green squares; L. M. Rebull et al. 2016) and NGC 3532 (yellow diamonds; D. J. Fritzewski et al. 2021) are shown for reference. The stars comoving with TOI 2076 show a distribution in between Pleiades and NGC 3532, consistent with the derived gyrochronology age.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: Period-radius injection-recovery map for TOI 2076. Blue points indicate recovered signals, while red points mark signals that were not recovered. Only 20% of injected planets are shown for clarity. The background is color coded by the overall completeness in a given bin. The previously known planets in the system are marked as the gold stars, TOI 2076 e is marked as the green star, and candidate TOI 2076 f is marked as the gray circle.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: Young, multiplanet transiting systems found in a stellar cluster or association (left) compared to mature multiplanet systems from Kepler around similar host stars (right). The mature ≥three-planet systems show a higher level of intrasystem uniformity in period and radius space than the young systems. The inclusion of TOI 2076 e pushes the system out of uniformity.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: The Li equivalent widths of the candidate comoving stars against effective temperature (as a proxy for color; purple points). TOI 2076 is shown as the red x, and TOI 1807 is shown as the orange x. The teal region shows the expected distribution for the best-fit age (210 Myr).
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). III. An Inner Super-Earth in TOI 2076
Authors: Madyson G. Barber, Andrew W. Mann, Andrew Vanderburg, Andrew W. Boyle, Ana Isabel Lopez Murillo
Figure caption: The final age estimate distribution (210 ± 20 Myr; solid purple) compared to the age estimates from each method (colored lines).
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Global-median temperature (K) and horizontal wind speeds (m s−1) at 0.008 mbar, or the middle atmosphere, showing the results for a planet around actively flaring stars (gold and red), around a moderately active star (blue), around a quiescent/inactive star (black), and a more energetic star with a lower overall flare rate (orange). Time series' are computed from the 8 yr simulation.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Boxplots of extreme, active, and moderate anomalies for temperature (T in K), nitric oxide (NO, in mol mol−1), and hydroxide (OH, in mol mol−1). Anomalies are computed by subtracting the quiescent temporal field median from the daily medians of the three sets of simulated cases: extreme, moderate, and active boxplots in (a), (c), and (e) are computed for the 1.223 × 10−5 mbar middle atmospheric level, whereas the ones in (b), (d), and (f) represent the 0.008 mbar lower level. Each panel also represents six key regions: equatorial substellar (Eq Sub), equatorial antistellar (Eq Ant), midlatitude substellar (Mid Sub), midlatitude antistellar (Mid Ant) In all panels, at least one of the extreme, moderate, and active anomaly medians significantly differ from one another at the 1% level.