adsabs/AstroCLIMB huggingface dataset:
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Throughput-corrected 5σ contrast curves for continuum false planet optimized pyKLIP reductions of all epochs for the three GAPlanetS targets with reported wide (>0.″5) companions or companion candidates in the literature: TW Hya (two epochs), CS Cha (one epoch), and HD 100453 (three epochs). Throughput was computed as described in the text, with a correction for the small number of independent noise samples present near the star implemented following Mawet et al. (2014). Solid curves indicate regions where throughput-corrected contrast was computed directly. The curves are also projected inward from the innermost throughput measurement to the inner working angle, and this extrapolation region is indicated with a dashed line.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: KLIPed data (left) compared to best-fit BKA forward models (middle), ) and the residuals of their subtraction (right). Fits are shown for all companions whose photometry and astrometry could be extracted from Hα and/or Continuum GAPlanetS imagery, except for HD 142527 B, as qualitatively and quantitatively similarfits to the same data are shown in Balmer et al. 2022. Fit statistics are reported in Table 5.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Contrast curves for all GAPlanetS datasets analyzed in this work. These curves were generated following our conservative survey methodology of optimizing on false continuum planets. Curves are colored by the r’-band magnitude of the star. While the specific contrast achieved for a given target varies widely with seeing, it is also a strong function of r’-band magnitude.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for both V4046 Sgr epochs. pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for both V1247 Ori epochs. pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for all five HD 141569 epochs, as well as the combination of the three 2014 epochs (fourth panel) and the two 2015 epochs (seventh panel). pyKLIP reduction parameters (indicated in the text labels to the left of each image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for the single PDS∼66 epoch. pyKLIP reduction parameters (indicated in the text labels to the left of the image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS)—Results from a 6 yr Campaign to Image Accreting Protoplanets
Authors: Katherine B. Follette, Laird M. Close, Jared R. Males, Kimberly Ward-Duong, William O. Balmer, Jéa Adams Redai, Julio Morales, Catherine Sarosi, Beck Dacus, Robert J. De Rosa, Fernando Garcia Toro, Clare Leonard, Bruce Macintosh, Katie M. Morzinski, Wyatt Mullen, Joseph Palmo, Raymond Nzaba Saitoti, Elijah Spiro, Helena Treiber, Kevin Wagner, Jason Wang, 劲飞 王, David Wang, Alex Watson, Alycia J. Weinberger
Figure caption: Final KLIPed Hα (left), Continuum (middle left), stellar Hα/continuum-scaled ASDI (middle right), and 1:1 scaled ASDI (right) imagery for the single UX Tau A epoch. pyKLIP reduction parameters (indicated in the text labels to the left of the image panel) have been optimized for recovery of false continuum planets injected between the IWA and control radius, as described in detail in the text. The AO control radius of the images is indicated with a white dashed circle.
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: Right panel: the Max.I−Max.II evolving with time derived from Kepler data (upper panel) and the LS periodogram of the Max.I−Max.II (lower panel). Left panel: the Max.I−Max.II evolving with time derived from TESS data.
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: The ﹩\mathrm{log}({P}_{\mathrm{cyc}}/{P}_{\mathrm{orb}})﹩ vs. ﹩\mathrm{log}(1/{P}_{\mathrm{orb}})﹩ and a linear fit (black line) for EBs from Table 13 of Pi et al. (2019). EBs with different spectral types are represented by different colors and the CV represents cataclysmic variables.
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: Distributions of host properties. The histograms are shown on a log scale and have been normalized to show the average counts in a single simulation. The 15.9%, 50%, and 84.1% percentiles of each distribution (i.e., the 1σ range) are reported at the top of each panel. Top row: source magnitudes in the F146, r, i, z, and J bands. Magnitudes were calculated using BT-Settl model spectra and were reduced by realistic dust extinction values. The 99.9% percentiles for the r, i, z, and J magnitudes (used in the Besançon simulation described in Section 2.3) are indicated by dashed black lines. Bottom row: distance in parsecs, effective temperature in Kelvin, spectral type, mass in solar masses, and radius in solar radii.
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: An example detection of a planet in our injection and recovery simulation. The host is an M5 dwarf with F146 = 16.5, R  h  = 0.133 R ⊙, M  h  = 0.108 M ⊙, T eff = 2895 K, a distance of 193 pc, and an age of 2.68 Gyr. The planet has a radius of 1.24 R ⊕, an orbital period of 27.0 days, a/R  h = 136, and i = 89.°9. Top: the full simulated light curve, which consists of six, 72 day campaigns, three near the start of the mission and three near the end. Gray points show the 46.8 s photometry evaluated at a 909.6 s cadence, and black points with error bars show the photometry binned over 1.5 hr timescales. The transit model is shown in blue. Middle: the first of the six campaigns. Bottom: the phase-folded data which we use to assess the transit significance. Black points with error bars show the phased photometry binned over 20 points. The transit was recovered in the phased photometry to an S/N of 40 using Equation (5).
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: Properties of the transiting planet hosts and transiting planets detected across our 1000 simulations. As in Figure 5, the distributions are shown on a log scale and were normalized to show the average counts in a single simulation. The 15.9%, 50%, and 84.1% percentiles are reported at the top of each panel. First row: F146-, r-, i-, z-, and J-band magnitudes of hosts with detected transiting planets. Second row: distance in parsecs, T eff in Kelvin, spectral types, masses in M ⊙, and radii in R ⊙ of the hosts with detected transiting planets. Third row: orbital periods, radii in R ⊕, a/R  h , inclinations in degrees, and irradiances in Earth irradiance (G ⊕) of the detected transiting planets. The irradiance distribution includes a shaded area indicating the conservative HZ of Kopparapu et al. (2013). Fourth row: durations in hours, S/N, and number of transits of detected transiting planets.
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: The distribution of the total number of single mid-M and UCD sources with F146 < 21 in the survey fields over 1000 iterations of our simulation, with the scaled space densities shown in blue. This simulation predicts an average of 75,500﹩{}_{-7000}^{+11,800}﹩ single mid-M dwarf and UCD sources in the survey fields (1σ range). Predictions from the Galactic stellar population synthesis models TRILEGAL and Besançon are marked with orange and red vertical lines, respectively (see Section 2.3 for more details).
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: Radii of confirmed (circles) and candidate planets (stars) smaller than 4 R ⊕ vs. effective temperature for hosts with T eff < 3300 K from the Kepler/K2 (orange) and TESS (pink) missions. Detections from a representative iteration of our simulation (with 1347 total detections) are shown in blue. The effective temperature is listed on the bottom axis while the approximate spectral types are given along the top axis. The top panel shows histograms of the number of planet detections as a function of effective temperature for the different missions.
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: Top: distributions of detected planets with radii between 0.5 and 2.5 R ⊕ and orbital periods between 0.5 and 10 days around M3–M5 dwarfs in our simulations. The results using the DC15 planet occurrence rates for early-M dwarfs are shown in blue, and the results using the HU19 enhanced planet occurrence rates for M3–M5 dwarfs are shown in orange. Bottom: cumulative distribution functions for the two distributions shown in the top panel.
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: The theoretical single-search false alarm rate as a function of detection threshold for the Kepler mission from Jenkins et al. (2002; solid blue line). A dashed blue line indicates the desired false positive rate of 1/100,000 for Kepler, which is achieved at a detection threshold of 7.1σ. A dashed orange line shows an estimate for the Roman survey, where a false positive rate of 1/200,000,000 is achieved at a detection threshold of 8.1σ.
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: Local space densities of single M3–T9 dwarfs as a function of effective temperature used in the simulation described in Section 2.2. The top axis is given as a function of spectral type, the values of which were determined using the M dwarf temperature scale of Rajpurohit et al. (2013) for temperatures above 2800 K and the temperature scale for field M6–T9 dwarfs of Faherty et al. (2016) for temperatures below 2800 K. W21 densities are shown in blue and have been converted from a mass scale to a temperature scale using the 10 Gyr isochrone of Baraffe et al. (2015). K21 densities are shown in red. The densities of M6–M9.5 dwarfs are indicated in orange and were assumed to connect the W21 and K21 densities linearly. The linear fit that was used to generate these estimates is shown as a black dashed line. Error bars indicate the 1σ uncertainty on each bin, which were taken to be Poissonian. The 2100–2250 K bin is a lower limit and is indicated with an upward arrow.
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: The on-sky footprint of the Roman survey with archival z-band imagery from Pan-STARRS1 (Chambers et al. 2016). Bad pixels in the Pan-STARRS1 data are colored in white and are used to flag saturated sources, areas without survey coverage, etc. Left: the full survey footprint, covering ∼2 deg2 of the Galactic bulge over seven fields. Field outlines are shown in orange. Middle: a single field, with outlines of the 18 detector pointings shown in orange. Right: one detector within this field. Field pointings were taken from Penny et al. (2019; https://github.com/mtpenny/wfirst-ml-figures).
Paper: Predicting the Yield of Small Transiting Exoplanets around Mid-M and Ultracool Dwarfs in the Nancy Grace Roman Space Telescope Galactic Bulge Time Domain Survey
Authors: Patrick Tamburo, Philip S. Muirhead, Courtney D. Dressing
Figure caption: The standard deviation of normalized photometry in a single 46.8 s exposure in the F146 band, modeled using the parameters listed in Table 1. The F146 = 21 magnitude cutoff and its corresponding ∼1% single-exposure standard deviation are indicated in dashed black lines.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: Detection of test pulsar B0355+54 using blipss. Left: broadband signal detection at known pulsar rotational period, P 0 ≈ 156.37 ms. We obtain our highest matched filtering S/N values (color scale) at radio frequencies where interstellar scintillation best brightens the pulsar emission. The first subharmonic (P ≈ 312.75 ms) and the first two harmonics (P ≈ 78.19,  52.12 ms) of the pulsar rotational frequency are also detected. In addition, we detect the pulsar at rational multiples of P 0 near 5.2 GHz, where the pulsar emission is at its brightest in our band. These include detections at P ≈ 2P 0/3 and P ≈ 3P 0/2. Right: phase-resolved pulsar spectrum revealing pulse dispersion from radio wave propagation through the interstellar medium. Since our search strategy does not assume a dispersion law, blipss can enable discovery of periodic signals with radio frequency drifts that differ from the often assumed cold plasma dispersion law (arrival times ∝ ν −2).
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: A schematic representation of the blipss workflow consisting of three stages. In Stage 1, a sequence of N input filterbank files is processed channel-wise to search for periodic signals. Operations on different input files are parallelizable across multiple cores of a machine. Stage 1 outputs a list of periodicity candidates detected per channel for every input file. In Stage 2, these candidates are assigned N-digit binary codes based on comparisons between on-target and off-target scans. A “1” at entry j of the code (read from left to right) indicates candidate detection in the j-th input filterbank file. Similarly, we use zeros to label candidate non-detections in different files. Finally, in Stage 3, we define filters to select binary codes warranting visual candidate inspection.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: Statistical distribution of F 1 (blue) and F 2 (orange) events detected in our survey. Top left panel: probability density function (PDF) of candidate periods. The period axis from 11–100 s is spanned by 39 bins of width 2.28 s each. Top right panel: PDF of candidate S/N values. The S/N axis from 7 to 9.81 is covered by 39 equal-sized bins. Bottom left panel: scatter of candidates in the radio frequency-period plane. Bottom right panel: scatter of events in the radio frequency vs. matched filtering S/N diagram.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: Transmission energy budget comparison for S/N = 10 detection of three signal morphologies, i.e., steady Hz-wide CW beacons (red), a sequence of individually detectable broadband millisecond pulses (blue), and ∼kHz-wide periodic spectral signals (black). The blue curve and all black curves assume a signal periodicity of 100 s. The blue and solid black curves both presume a pulse duty cycle, δ = 10−5. In contrast, the dashed and dotted black curves correspond to δ = 0.1 and 0.5, respectively. The red line assumes 100% signal dechirping efficiency. Finally, the red line and all black curves reflect numbers for an integration time of 5 minutes.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: Detection of a target periodic spectral signal using blipss. Left: simulated radio frequency-time data containing 64 spectral channels of width 391 kHz each. A periodic pulsed signal has been inserted into the central channel. Right: radio frequency-period (P) diagram showing the detection of a P 0 = 30 s signal in the central spectral channel. The first harmonic (cross) and the first subharmonic (plus) of the fundamental signal frequency (f 0 = 1/P 0) are also detected at P = 15 s and P = 60 s, respectively.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: A simulated candidate detected with 30 s period in all scans of source X, but unseen in scans of source Y. Left panels show periodograms generated from simulated single-channel time-series data. Right panels illustrate phase-time diagrams (bottom subplots) and folded profiles (top subplots) of candidates at the periods highlighted by red vertical dashed lines in their respective left panels. Each row represents a different input data file. Rows {1, 3, 5} and {2, 4, 6} correspond to scans of sources X and Y, respectively.
Paper: A 4–8 GHz Galactic Center Search for Periodic Technosignatures
Authors: Akshay Suresh, Vishal Gajjar, Pranav Nagarajan, Sofia Z. Sheikh, Andrew P. V. Siemion, Matt Lebofsky, David H. E. MacMahon, Danny C. Price, Steve Croft
Figure caption: An F 2 candidate with P ≈ 21.67 s (vertical red dashed line in left panels) detected exclusively in two B04 scans (rows 3 and 5). Phase-time diagrams (bottom subplots of right panels) on rows 3 and 5 trace the candidate origin to the coincident alignment between intermittent RFI instances in our data. In particular, some of the aforementioned RFI are observed close to the start times of different observing scans.