adsabs/AstroCLIMB huggingface dataset:
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: KOI 770.01 false positive due to centroid offset. The image shows an example cadence of the pixel data (TPF); highlighted in red is the aperture selected by the Kepler pipeline, the black dot shows the position of the candidate target, and the blue dot shows the position of the neighbor. The light-curve panels show the time-based (middle) and period-folded (right) time series for the Kepler PDCSAP light curve (top), our PSF photometry for the candidate (middle), and the contaminant (bottom) following the same color code as above. KIC or Gaia identifiers, period values, magnitudes, and pair distances are detailed in the panel titles.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Pearson correlation coefficient between light-curve pairs as a function of distance during quarter 5. Light-curve pairs are made of every possible pair of sources within 60″. Higher coefficients mean a significant correlation between light curves. The break in density around 25″ is due to the typical size of a TPF. The high-density feature with r < 0.2 represents the majority of noncorrelated pairs. The bulge feature between 7″ and 20″ and r < 0.3 is due to the typical distance between pairs in a TPF, while the drop in density within 5″ is due to isolated sources in a TPF and the rejection of predicted negative fluxes (see Section 2.6).
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Top: CMD of KBonus sources (black) and a sample of evolved red giant and horizontal branch stars (blue) that show consistently higher CDPP values with respect to the main distribution. Bottom: 6 hr CDPP values as a function of G-band magnitude from the perturbed PSF model. The figure shows sources after removing the abovementioned evolved stars. The distinctive high-density band around ﹩{\mathrm{log}}_{10}({\rm{6h-CDPP}})\sim -3.5﹩ seen in Figure 8 is not present.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Histogram of magnitude contrast as a function distance for pair sources. The left panel shows the density of all the available Gaia sources (G ≤ 19) on the TPFs, which is our input catalog. The right panel shows the density of extracted sources in the KBonus catalog presented in this work. This figure shows the extraction biases discussed in Section 4 in limitations 1, 2, 4, and 7.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: Confirmed exoplanet Kepler-1698 b with an orbital period of 3.85 days. The top panels (red) show Kepler’s PDCSAP light curve, while the bottom panels (black) are the KBonus PSF photometry. The left panels show the light curve in time space, and the right panels show the phase-folded light curve centered in midtransit.
Paper: Kepler Bonus: Light Curves of Kepler Background Sources
Authors: Jorge Martínez-Palomera, Christina Hedges, Jessie Dotson
Figure caption: KOI 909.01 false positive due to centroid offset. Legends are the same as for Figure 14. The contaminant is KIC 8256044, which was labeled as an EB.
Paper: Evidence for Low-level Dynamical Excitation in Near-resonant Exoplanet Systems 
Authors: Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Khalid Barkaoui, Rafael Brahm, Karen A. Collins, Andrés Jordán, Nataliea Lowson, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Kevin I. Collins, Felipe Murgas, Gavin Boyle, Francisco J. Pozuelos, Mathilde Timmermans, Emmanuel Jehin, Michaël Gillon
Figure caption: Photometry obtained from the seven telescopes used within this work. Observations are ordered by the date on which they were taken, with shaded regions signifying the modeled transit durations and solid gray lines denoting the transit midtimes measured for each dataset. The transit models associated with our parameter solution are shown together with the data, and a dotted line marks the linear ephemeris midtransit. The dataset behind this figure is provided in the digital version of this manuscript.(The data used to create this figure are available.)
Paper: Evidence for Low-level Dynamical Excitation in Near-resonant Exoplanet Systems 
Authors: Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Khalid Barkaoui, Rafael Brahm, Karen A. Collins, Andrés Jordán, Nataliea Lowson, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Kevin I. Collins, Felipe Murgas, Gavin Boyle, Francisco J. Pozuelos, Mathilde Timmermans, Emmanuel Jehin, Michaël Gillon
Figure caption: Sky-projected stellar obliquity ∣λ∣ and 3D stellar obliquity ψ for near-resonant systems. The maximum expected level of stellar obliquity excitation in the convergent migration framework is shown in gray. All ψ values have been measured for separate planetary systems, while V1298 Tau and TRAPPIST-1 include two and three separate displayed ∣λ∣ values, respectively.
Paper: Evidence for Low-level Dynamical Excitation in Near-resonant Exoplanet Systems 
Authors: Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Khalid Barkaoui, Rafael Brahm, Karen A. Collins, Andrés Jordán, Nataliea Lowson, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Kevin I. Collins, Felipe Murgas, Gavin Boyle, Francisco J. Pozuelos, Mathilde Timmermans, Emmanuel Jehin, Michaël Gillon
Figure caption: PFS observations of the TOI-2202 b Rossiter–McLaughlin effect from UT 11/4/22, together with the associated uncertainties and best-fitting model (red dashed line). Two thousand Rossiter–McLaughlin model draws from the posterior distribution are shown in gray. Residuals from the best-fitting model are provided in the lower panel.
Paper: Evidence for Low-level Dynamical Excitation in Near-resonant Exoplanet Systems 
Authors: Malena Rice, Xian-Yu Wang, Songhu Wang, Avi Shporer, Khalid Barkaoui, Rafael Brahm, Karen A. Collins, Andrés Jordán, Nataliea Lowson, R. Paul Butler, Jeffrey D. Crane, Stephen Shectman, Johanna K. Teske, David Osip, Kevin I. Collins, Felipe Murgas, Gavin Boyle, Francisco J. Pozuelos, Mathilde Timmermans, Emmanuel Jehin, Michaël Gillon
Figure caption: Period ratios of planet pairs in compact systems (P out/P in ≲ 4) in which at least one planet has a spin–orbit measurement.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: Doppler drift of a narrowband signal in the topocentric observing frame at four different observing epochs. Simulated waterfalls with narrowband signals observed from the Irish LOFAR station toward the direction of TIC 27677846 are shown for different times of the year in blue. The expected sign and direction of change of the relative velocity are labeled at the top of each plot. It is assumed that a hypothetical narrowband ETI signal is transmitted at a constant frequency of 1420 MHz (with zero drift rate). As shown, the same signal is observed at different frequencies and drift rates depending on the sign and direction of change of the relative velocity at different epochs of observations. For instance, in the first panel, the relative velocity is positive and increases with observing time. Therefore, the observing frequency has been shifted to a lower frequency (as described by Equation (3)), and it continues to shift to even lower frequencies with time.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: Cumulative histogram of EIRP limits of this survey across the HBA band. Reference luminosities for three civilization levels emitting 1017, 1013, or 1010 W are shown in blue, red, and green respectively. The percentage of targets where the station is sensitive to the transmission of 1017 W is shown, as a function of frequency across the band. At lower frequencies, sensitivity to 1017 emitters drops off as the T sys rises. The ﹩{\bar{T}}_{\mathrm{sys}}﹩ varies from 1260 K down to 322 K as frequency is increased across the band. Detailed calculations are presented in Appendix B and Table B1.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: Comaprison of our study (highlighted in red) to prior surveys. The plot presents the transmitter rate vs. EIRP, with the gray line indicating the transmitter rate as a function of EIRP. A solid vertical gray line illustrates the energy surplus of a Kardashev Type-I civilization. Additionally, a dotted–dashed gray line depicts the EIRP of the Arecibo planetary radar. The gray thick line shows the slope of the transmitter rate as a function of their EIRP power. Distance used for EIRP calculation is ﹩\bar{d}+{d}_{\sigma }=7009\,\mathrm{ly}﹩.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: Comparison of drifting signals or “hits” detected at both stations seen across the HBA frequency band. Each bin within the data set represents a 1 MHz frequency range and is accompanied by a corresponding percentage indicating its proportion to the overall data set.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: Dynamic spectra (waterfall plots) of detected narrowband signal centered on the detected frequency of detection, showing the two most common cases of coincidence rejection. Case A (left) shows a narrowband signal with a nonzero drift rate detected at I-LOFAR and not LOFAR-SE. Case B (Right) shows the opposite, where a nonzero drift-rate signal is not detected by I-LOFAR but is detected by LOFAR-SE. For a signal to be considered a detection of interest, both sites would have to exhibit nonzero drift-rate signal at the same frequency simultaneously.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption:  iLiSA block diagram, showing how an operator-defined schedule is ingested and is executed in a timely fashion. Data then begins to flow and ends up being ingested by processing pipelines together with associated metadata.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: The fraction of stars that produce narrowband emission (f  n   c ) against the transmitter power of the total target pool. The hashed region (red) shows the constraints this survey places on a value of f  n   c  at 110–190 MHz.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: The top two plots represent narrowband signals detected at both stations in the topocentric frame of reference. The bottom two plots show the same detected narrowband signals detected at both stations but corrected to the barycentric frame of reference. This is illustrated by the newly added drift to signals present after correction.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: A scatter plot of the drift-rate values against detected frequency. The Irish station is shown in pink and the Swedish station is shown in blue.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: These plots depict the expected spectra at their respective barycentric frequencies and the spectra after the correction for barycentric relative velocity. Each plot represents a single spectrum, where the frequency increases from right to left. (a) In the case of +v rel, the first channel of the topocentric spectra is shifted to a higher barycentric frequency compared to the last topocentric spectra channel, which causes an expansion of the spectra. If two consecutive channels move farther away from each other (shown as f 1 and f 2) by more than half the channel width, an additional channel is added in between, which is the summation of these two channels. Extra channels at the edge of the spectra are dropped. (b) In the case of −v rel, the first channel of the topocentric frequency is shifted to a lower barycentric frequency relative to the last topocentric spectra channel, which causes a squeeze in the spectra. If two consecutive frequency channels shift closer to each other by more than half a channel width, these channels are added together and an extra channel is added at the end containing zeros. The bottom spectra in each plot illustrate these expansion and squeeze effects after correction are applied from the code.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: An outline of the post-detection barycentric correction algorithm for an input filterbank file in sigproc format. For this case, the input filterbank file has a descending order in frequency, and v rel represents the relative velocity between the transmitter and observer. The algorithm considers two cases depending on whether the relative velocity is positive or negative, which indicates whether the source is moving away from or toward the observer, respectively. Each of these cases is further divided into two, where the absolute value of the relative velocity can either increase or decrease, requiring the spectra to be shifted to either the higher- or lower-frequency end. For all cases with +v rel, each spectra is expanded, and for −v rel, each spectra is squeezed, as shown in Figure A3. The code then writes each of these spectra into another sigproc filterbank file, which will have each channel frequency closely corrected to the barycentric frame of reference.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: A typical filterbank file stores data in a time and frequency matrix format. Each row represents a sample, while each column represents a frequency channel for a given sample. Time is increasing from bottom to top, while the frequency is increasing from right to left.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: An Aitoff projection of the sky in Galactic coordinates depicts the distribution of survey pointings, with the Galactic disk shaded in gray. Gaia sources are omitted from the plot due to their extremely high source density. Gray dots represent TESS Targets of Interest (ToIs). Those targets observed during our survey are marked with red dots at boresight, with green showing the half-power beamwidth (2.°59).
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: A Hertzsprung–Russell diagram of the 1,631,198  Gaia targets searched for technosignatures in this survey, with a mean distance of 1270  pc. The relative distribution with respect to spectral type is O <0.01%, B—0.4%, A—6.94%, F—11.01%, G—31.56%, K—47.84%, M—2.12%. This is as opposed to the distribution of the general Gaia catalog, which is O, B <0.0001%, A—1.5%, F—18.9%, G—44.4%, K—34.5%, M—0.6%.
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: This figure illustrates one of the boresight pointings directed at a TESS object (highlighted in green), with the LOFAR beam’s full width at half maximum (FWHM) shown in pink. The background image is from the Sloan Digital Sky Survey (SDSS; Albareti et al. 2017).
Paper: A Simultaneous Dual-site Technosignature Search Using International LOFAR Stations
Authors: Owen A. Johnson, Vishal Gajjar, Evan F. Keane, David J. McKenna, Charles Giese, Ben McKeon, Tobia D. Carozzi, Cloe Alcaria, Aoife Brennan, Bryan Brzycki, Steve Croft, Jamie Drew, Richard Elkins, Peter T. Gallagher, Ruth Kelly, Matt Lebofsky, Dave H. E. MacMahon, Joseph McCauley, Imke de Pater, Shauna Rose Raeside, Andrew P. V. Siemion, S. Pete Worden
Figure caption: The LOFAR HBA beam’s sensitivity at 150 MHz changes in relation to the off-axis boresight angle (θ). Furthermore, a plot of the number of filtered Gaia targets within the beam pointing as a function of θ is presented. The ×represents the value for the FWHM of the beam.
Paper: A Search for Technosignatures Around 11,680 Stars with the Green Bank Telescope at 1.15–1.73 GHz
Authors: Jean-Luc Margot, Megan G. Li, Pavlo Pinchuk, Nathan Myhrvold, Larry Lesyna, Lea E. Alcantara, Megan T. Andrakin, Jeth Arunseangroj, Damien S. Baclet, Madison H. Belk, Zerxes R. Bhadha, Nicholas W. Brandis, Robert E. Carey, Harrison P. Cassar, Sai S. Chava, Calvin Chen, James Chen, Kellen T. Cheng, Alessia Cimbri, Benjamin Cloutier, Jordan A. Combitsis, Kelly L. Couvrette, Brandon P. Coy, Kyle W. Davis, Antoine F. Delcayre, Michelle R. Du, Sarah E. Feil, Danning Fu, Travis J. Gilmore, Emery Grahill-Bland, Laura M. Iglesias, Zoe Juneau, Anthony G. Karapetian, George Karfakis, Christopher T. Lambert, Eric A. Lazbin, Jian H. Li, Zhuofu (Chester) Li, Nicholas M. Liskij, Anthony V. Lopilato, Darren J. Lu, Detao Ma, Vedant Mathur, Mary H. Minasyan, Maxwell K. Muller, Mark T. Nasielski, Janice T. Nguyen, Lorraine M. Nicholson, Samantha Niemoeller, Divij Ohri, Atharva U. Padhye, Supreethi V. Penmetcha, Yugantar Prakash, Xinyi (Cindy) Qi, Liam Rindt, Vedant Sahu, Joshua A. Scally, Zefyr Scott, Trevor J. Seddon, Lara-Lynn V. Shohet, Anchal Sinha, Anthony E. Sinigiani, Jiuxu Song, Spencer M. Stice, Nadine M. Tabucol, Andria Uplisashvili, Krishna Vanga, Amaury G. Vazquez, George Vetushko, Valeria Villa, Maria Vincent, Ian J. Waasdorp, Ian B. Wagaman, Amanda Wang, Jade C. Wight, Ella Wong, Natsuko Yamaguchi, Zijin Zhang, Junyang Zhao, Ryan S. Lynch
Figure caption: Upper limits on transmitter prevalence (95% CL) as a function of transmitter duty cycle. The solid blue line shows the limit calculated for GBT observations of 10,230 stars located within 20,000 ly of the Sun, and the analysis with the UCLA SETI pipeline, which has a conservative 94% probability of detecting detectable narrowband technosignatures (see text for detectability requirements). The dashed blue line shows the limit calculated for the subset of stars located within 1 kpc of the Sun. The solid and green orange lines show revisions to previously published limits (see Section 5.3 for correction factors).