adsabs/AstroCLIMB huggingface dataset:
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: Changes of the angular radius of the predicted starspot.
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: Periodograms associated to the TESS data. Red-dashed lines represent multiplies of orbital frequency.
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: The best-fit convective velocity profiles within the patches of star occulted by KELT-18 b as a function of center-to-limb position (left) and time (right). The v conv for models with DR are consistent with zero, i.e., the DR models are primarily fit by extreme DR. The velocity contribution from DR alone is shown by the dashed red line, which plots the difference between the DR-only and SB-only models. Residuals (data minus model) to the SB-only model are plotted in black in both panels; these points represent the amount of local RV that must be coming from either DR or CLVs and are shown as a representation of what the DR and/or CLV components of the other models are effectively fitting.
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: The time series of CCFloc measured with KPF. The top panel shows each 1D CCFloc, with out-of-transit observations colored gray and in-transit observations colored according to the timestamp. The bottom panel displays the same data as a 2D heatmap with time relative to mid transit on the y-axis. The color scale in this case encodes the flux. The shadow of KELT-18 b, if it were aligned, is traced by the gray dashed lines. Black rows correspond to gaps in the time series; the narrow hourly bands correspond to etalon calibration images and the large band near +1.8 hr is when the tip/tilt guiding system failed.
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: On-sky geometry of the KELT-18 system. KELT-18 and KELT-18 b (and its orbit) are drawn to scale in size and relative orientation. The black arrow denotes the normal to KELT-18 b’s orbital plane, and the gray arrow denotes the rotation axis of KELT-18; the angle between these in 3D space is the stellar obliquity, ψ, while λ is the sky projection of this angle (i.e., the angle on this page) and is independent of the stellar inclination. The separation between KELT-18 and KELT-18 B is not to scale and is drawn at an arbitrary orientation on-sky. KELT-18 is colored according to its rotational velocity profile (with no differential rotation), and lines of latitude/longitude are drawn to illustrate the orientation of the pole (i ⋆ = 30°). The angle between the binary star position vector ( r , blue arrow) and relative proper motion ( v , red arrow), γ, is labeled.
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: Analysis of the rotation period using TESS photometry. The top three panels show the 1 hr binned TESS photometry described in Section 2.1. The fourth panel displays a Lomb–Scargle periodogram. We marked the 0.707 day period from M17 with a red dashed line, KELT-18's orbital period with a gray dashed line, and the maximum peak with a blue dashed line. The bottom panel shows all TESS data points (same color coding per sector as above) phase folded to the period with maximum power. Black squares show the phased data evenly binned with bin size 0.05.
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: The extracted local RVs and the best-fit RRM models (SB = solid body, DR = differential rotation, CLV = center-to-limb variations as a linear (lin) or quadratic (quad) effect in 〈μ〉). The solid lines are the MAP model while the shaded regions cover the 16th–84th percentile of posterior distribution of models. The bottom panel compares the residuals between the data and the MAP fit for each model.
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: The posterior distributions for all RRM parameters. The models with DR are colored red, while SB models are colored blue, and models with no, linear, or quadratic CLVs are given progressively darker colors. All models generally agree on the value of λ, while models with DR tend toward extreme values of α at near-polar i ⋆. This degeneracy arises because of the tight prior on ﹩{v}_{\mathrm{eq}}\sin {i}_{\star }﹩ (second column), which all models are confined to.
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: Periodograms, following the same methodology used to produce the periodogram in Figure 1, for each individual TESS sector. The primary peak near 5 days in the overall periodogram only appears in the individual sectors 15, 23, and 48. Other sectors show different peak structures. As in Figure 1, the 0.707 day period from M17 is denoted by the red dashed line, KELT-18's orbital period is denoted by the gray dashed line, and the maximum peak is marked by a blue dashed line. The black dotted line gives the maximum peak in the overall periodogram (i.e., the blue line in Figure 1).
Paper: KPF Confirms a Polar Orbit for KELT-18 b
Authors: Ryan A. Rubenzahl, Fei Dai, Samuel Halverson, Andrew W. Howard, Aaron Householder, Benjamin Fulton, Aida Behmard, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Chris Smith, Guðmundur Stefánsson, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Edward Wishnow
Figure caption: The contrast (top), equivalent width (middle), and FWHM (bottom) of CCFloc as a function of the flux-weighted center-to-limb position 〈μ〉. The color scale is the same used in Figure 2 based on the observation timestamps (purple = ingress, green = mid transit, yellow = egress).
Paper: The Correlation Between Dust and Gas Contents in Molecular Clouds
Authors: Rui-Zhi Li, Bing-Qiu Chen, Guang-Xing Li, Bo-Ting Wang, Hao-Ming Ren, Qi-Ning Guo
Figure caption: CO brightness temperature maps for Cloud 378 at various v LSR. The black, cyan, and yellow polygons denote CO emission significance at 3σ, 6σ, and 9σ, respectively. The lines in the color bar indicate the CO emission at different levels. The red polygon highlights the dust contour boundary of the cloud as identified by B. Q. Chen et al. (2020b). The method for calculating the dust contour threshold, ﹩{A}_{V}^{\min }﹩, is described in Section 2.1.
Paper: The Correlation Between Dust and Gas Contents in Molecular Clouds
Authors: Rui-Zhi Li, Bing-Qiu Chen, Guang-Xing Li, Bo-Ting Wang, Hao-Ming Ren, Qi-Ning Guo
Figure caption: CO brightness temperature maps for Cloud 221, analogous to Figure 1.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Maximum effective temperature of the smaller star if the DTARPS-S candidate (left) were an unequal-mass EB system and if the TOI systems with follow-up (right) were unequal-mass EB systems. Each bar of the histogram is colored to show the labels. Gray represents previously identified FPs, red represents Confirmed Planets from the NASA Exoplanet Archive, and gold represents previously identified planetary candidates. Those newly identified are colored by their disposition level: Level 1 (green) and Level 2 (blue) DTARPS-S candidates, or Galactic Plane list (purple). The temperature of an M3 dwarf is marked by the dashed black and yellow line in each histogram.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Distribution of the ratio of the semimajor axis to the stellar-host radius for DTARPS-S candidate USPs (in gray, omitting Confirmed Planets) and our DTARPS-S candidate xUSPs (in purple, omitting Confirmed Planets). For comparison the a/R ⋆ distribution for USP exoplanets in the NASA Exoplanet Archive with radii > 1.8 R ⊕ is shown by the red dashed histogram.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Distributions of absolute distance from the Galactic plane (left) and Galactic vertical action (right) for the DTARPS-S hot-Neptune candidates and the Kepler confirmed hot Neptunes. The DTARPS-S hot-Neptune Candidates include hot-Neptune candidates from the Galactic Plane catalog. The Confirmed Planets from Kepler are plotted in gray. DTARPS-S candidates are colored by their disposition level. The two distributions are superimposed on top of each other to ease comparison between the two populations.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Relative frequency of the effective temperature of the stellar-host star for Kepler Confirmed Planets (purple) and Confirmed Planets in the TOI list (gray) normalized by the sample size for each population. The DTARPS-S Catalog Candidates are marked by the dashed red histogram. The difference between the median effective temperature for the Kepler planets is only 150 K lower than the median effective temperature of the Confirmed Planets in the TOI list.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Predicted radial-velocity semimajor amplitude as a function of the transmission signal-to-noise metric for the JWST NIRISS instrument. The red line shows the suggested limit for high-priority atmospheric transmission spectroscopy (E. M. R. Kempton et al. 2018). The color of the points indicates the disposition and the shape indicates the category of the DTARPS-S candidates.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Period–radius plot for DTARPS-S candidates around M dwarfs (T eff < 3870 K). The light-gray points are the Confirmed Planets from the NASA Exoplanet Archive. DTARPS-S candidates are colored by their disposition level with symbols representing their novelty.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Period–radius plot of DTARPS-S USP candidates. The xUSP region corresponding to periods of less than 12 hr is highlighted in purple. The light-gray points are some of the Confirmed Planets that transit from the NASA Exoplanet Archive. The color of the DTARPS-S candidate points indicate their DTARPS-S disposition level and the shape of the point indicates any previous identification.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Histogram of the TESS T magnitude of the candidates with hosts around M dwarfs. Only newly identified DTARPS-S candidates and previously identified planetary candidates are included in the histogram. The number of newly identified DTARPS-S candidates in each column is labeled above it.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Distribution of planet radii for high-priority transmission spectroscopy DTARPS-S candidates. Each bar is colored by the DTARPS-S disposition of the candidates. The number of newly identified DTARPS-S candidates is given for each bar.
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Schematic diagram of all relevant angles related to a planet obliquity. (a) Cartoon diagram showing that planet obliquity is the angle between the planet orbit normal and planet spin vector in 3D. (b) An orbit-oriented coordinate system with the orbit normal along the Z-axis. (c) An observer-oriented coordinate system with observer along the ﹩X^{\prime} ﹩-axis, and the line of nodes along the ﹩Y^{\prime} ﹩-axis. These two coordinate systems are related by a 90° − i  o  rotation along the ﹩Y=Y^{\prime} ﹩-axis. These diagrams were inspired by D. C. Fabrycky & J. N. Winn (2009) and J. Dong & D. Foreman-Mackey (2023).
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Schematic diagram of three angular momentum vectors in the VHS system in 2D (left) and 3D (right). Left: LOS inclinations for the spin axis of VHS 1256 b (i  p ), the orbit normal of VHS 1256 b (i  o ), and the orbit normal of the host binary VHS 1256 AB (i AB) are shown relative to an observer on the left. Right: here we highlight the true 3D mutual inclinations between angular momentum vectors. Specifically ψ o−p is the planet obliquity, and ψ AB−p (ψ AB−o) is the mutual inclination between the binary orbital plane and planet spin axis (planet orbit normal). Note that all orbits are eccentric, and not to scale.
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Top panel: normalized posterior distribution for the planet obliquity ψ o−p, using a randomly oriented prior (black), which is uniform in ﹩\cos \psi ﹩. The observer-oriented and orbit-oriented methods show agreement. Bottom panel: same as the top panel, but with a different prior (black). This prior is a Fisher distribution that peaks at 25°, which is chosen to roughly match solar system planet obliquities (from small to large: Earth, Mars, Saturn, and Neptune). Mercury, Venus, Jupiter, and Uranus are excluded as they have planet obliquities near 0°, 90°, and 180°, preventing a simple unimodal prior. In the subsequent analysis, we choose to use the posterior from the upper panel.
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Top panel: normalized posterior distribution for the orbit–orbit mutual inclination ψ AB−o. Bottom panel: normalized posterior distribution for the 3D angle between the binary orbit and planet spin axis ψ AB−p. These distributions are compared to a randomly oriented prior (black), which is uniform in ﹩\cos \psi ﹩.
Paper: Leaning Sideways: VHS 1256−1257 b is a Super-Jupiter with a Uranus-like Obliquity
Authors: Michael Poon, Marta L. Bryan, Hanno Rein, Caroline V. Morley, Gregory Mace, Yifan Zhou, Brendan P. Bowler
Figure caption: Posterior distributions for the LOS projected mutual inclinations. These are lower limits on the true 3D mutual inclinations ψ o−p, ψ AB−o, and ψ AB−p. These distributions are compared to a randomly oriented projected inclination distribution (black), where i  o , i  p , and i AB have all been drawn from uniform distributions in ﹩\cos i﹩.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Histograms of frequencies, drift rates, and S/Ns, and bandwidths of all detected hits and events in the GC and GP survey. These plots indicate that the majority of hits and events in our survey (a) are located in frequency regions of known RFI, e.g., 4 GHz, (b) are consistent with terrestrial RFI due to their zero drift rate, (c) approximately follow an inverse power law with respect to detected S/N, and (d) are clustered at a signal bandwidth of seven frequency bins, or about 20 Hz.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Histogram of diagnostic statistics of detected hits and events throughout all GC and GP observations, compared to the synthetic distributions. Histograms are normalized to integral 1 to directly compare empirical probability densities. There is some overlap between the observed and simulated distributions, with events appearing marginally closer to the simulated distributions, but they are statistically distinct.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Histograms of diagnostic statistics computed using N = 1000 realizations of synthetic scintillated intensity time series embedded in chi-squared radiometer noise. The synthetic observations had Δf = 2.79 Hz, Δt = 2.51 s, and τ = 600 s, matching the observations taken in this study. The signals were generated with a bandwidth of eight frequency bins (about 22 Hz) and S/N = 33. Noisy intensity time series were extracted from the synthetic observations and used to compute each diagnostic statistic.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Monte Carlo–sampled scintillation timescales for the north Galactic pole, (l, b) = (0°, 90°), at the C band with N = 104. The dashed line indicates the median timescale, and the dotted lines indicate the first and third quartiles. As expected, compared to a pointing near the GC (Figure 1), the expected timescales are significantly longer.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Sky map of the fraction of Monte Carlo–sampled scintillation timescales with 10 s ≤ Δt  d  ≤ 100 s, with resolution Δl = Δb = 0.°25. Contours for 25%, 50%, and 75% coverage are shown. The blue dots show the GP targets for this survey, where the light blue dots indicate sight lines that pass through regions of enhanced free electron density.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Examples of signals found from the de-Doppler search that passed the algorithmic event filter, but failed manual inspection. Each primary signal appears continuously or with the same morphology in both the ON and OFF scans, indicating that all of the signals are RFI.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Sky map of the first, second, and third quartiles for scintillation timescale Δt  d , with resolution Δl = Δb = 0.°25. Contours are plotted in each panel for timescales of 10, 30, 60, and 100 s. Notice that the 10 s contour in Q1 and the 100 s contour in Q3 bound the majority of the region within 2° of the GP.