adsabs/AstroCLIMB huggingface dataset:
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: Distribution of the recovered S/N as a function of drift rate (0–1 Hz s−1 only) for a process that imitates the BL pipeline. Only the central region within ±0.15 Hz s−1 (blue lines) is free of Doppler smearing. The recovered S/N values are lower than the injected values because of Doppler smearing that worsens at larger drift rates, as quantified by smaller dechirping efficiencies at larger drift rates. Dechirping calculations for a BL-like process had predicted a drop in S/N to about ∼62% of nominal for df/dt = 0.25 Hz s−1, ∼31% for df/dt = 0.5 Hz s−1, and ∼16% for df/dt = 1 Hz s−1 (Margot et al. 2021), which are roughly consistent with what is observed.
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: Expected frequency drifts from monochromatic (f  t  = 1.42 GHz) transmitters experiencing spin and orbital accelerations in various settings. The solid lines represent the maximum drift rates corresponding to Project Cyclops, Breakthrough Listen (BL), and UCLA SETI searches. This figure is adapted from Sheikh et al. (2019) and reduces the drift rates sampled by BL by a factor of ∼7 to correct an error in the original figure.
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: Left: dynamic spectra showing the ON-OFF-ON scans corresponding to MLc3 as detected by the UCLA SETI pipeline. The detection of the signal in the OFF scan indicates that the signal can be immediately identified as RFI. Center: same data for MLc4, which was identified by the UCLA SETI pipeline as a candidate worthy of visual inspection. Right: same data for MLc5, which was identified by the UCLA SETI pipeline as a candidate worthy of visual inspection.
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: Distributions of the recovered S/Ns (left) and drift rates (right) for a process that imitates the BL pipeline, i.e., incoherent averaging of the spectra with N INC_SUMS = 51 followed by signal detection with turboSETI.
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: Distributions of the injected signals and signals recovered by the UCLA SETI pipeline as a function of frequency. Blue bands indicate the operating bands of GPS and GLONASS satellites, where recovery rates are markedly lower. Frequencies corresponding to a notch filter at the GBT (1.2–1.3412 GHz) are excluded.
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: Search volume characteristics of select surveys. The DFM (left) does not account for pipeline efficiency nor frequency drift rate coverage, but the MDFM (right) does.
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: Distributions of starting frequencies (left) and drift rates (right) of 10,000 artificial, linear FM “chirp” signals injected in voltage data. Frequencies corresponding to a notch filter at the GBT (1.2–1.3412 GHz) are excluded.
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: Distributions of the recovered S/Ns (left) and drift rates (right) for the UCLA SETI pipeline.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Two examples of simulated planetary microlensing light curves (dotted cyan curves), and the corresponding single microlensing events (setting q = 0; dashed green curves). In each panel, the raw and denoised data are represented with pink and blue colors, respectively. The best-performing wavelet for denoising and the used planetary lensing parameters are shown at the top of panels. Two given values for ﹩{\mathrm{log}}_{10}[\mathrm{STD}(\mathrm{mag})]﹩ correspond to raw and denoised data, respectively.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Same as Figure 1, but with four different cadence values: 15 min (top-left panel), 1 hr (top-right panel), 2 hr (bottom-left panel), and 4 hr (bottom-right panel).
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Similar to Figure 4, but for these two events, planetary like deviations appear in the denoised data (blue), whereas these deviations are not discernible in raw data (pink). The planetary like deviations are located at times 8225 and 8290 days in the left- and right-hand panels, respectively.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Examples of denoised data due to four real microlensing events found by the OGLE group. The OGLE name of each event, the best-performing wavelet, and the values of ﹩{\chi }_{n}^{2}﹩ for raw and denoised data (respectively) are mentioned at the top of each plot. The best-fit single microlensing light curves (as characterized in the OGLE page) are shown with dashed green curves.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Left panel: similar to Figure 1, by considering a 2 hr cadence for simulated data. Right panel: the 3D wavelet map resulting from CWTs with the wavelet cgau2.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Similar to Figure 4, but in the denoised data of these two events intrinsic pulsations of source stars appear. These pulsations are not discernible in the raw data.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: The 3D wavelet maps resulting from CWTs for the two OGLE events shown in Figure 7, with emergent planetary like signatures in their denoised data.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: The normalized distributions of ﹩{\chi }_{n}^{2}s﹩ for raw (pink) and denoised (blue) data for 100 OGLE microlensing events.
Paper: Wavelet Transforms of Microlensing Data: Denoising, Extracting Intrinsic Pulsations, and Planetary Signals
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: The scatter plot of ΔSTD(mag); (improvements in STD of the data due to DWT denoising) vs. the baseline magnitude of the source stars for simulated planetary and single microlensing events.
Paper: Free-floating Planet Mass Function from MOA-II 9 yr Survey toward the Galactic Bulge
Authors: Takahiro Sumi, Naoki Koshimoto, David P. Bennett, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Integrated detection efficiencies for events with u 0 < ρ and a significant FS signal as a function of θ E for all sources (orange line) and giant sources with I  s,0 < 16 mag (blue line) from MOA (Koshimoto et al. 2023) and FSPL events from KMTNet (green line; Gould et al. 2022). I  s,0 < 16 mag is the limiting magnitude used by Gould et al. (2022). This is similar to the ﹩{\tilde{\epsilon }}_{\mathrm{FS}}({\theta }_{{\rm{E}}};{\rm{\Gamma }})﹩ shown in Figure 8 of Koshimoto et al. (2023), except that Koshimoto et al. (2023) do not include the u 0 < ρ condition. These are only for the comparison to Gould et al. (2022) and not used for our analysis.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: Binary identification via the CMD. The Pleiades cluster is shown as an example. (a) Best-fitted isochrone for the Pleiades (red curve). The region enclosed by the solid curve demarcates the single-star boundary defined in this work, whereas the dotted curve identifies the binary region. The right boundary of the solid polygon is the binary isochrone of q = 0.4, which is the boundary that we use to separate single and binary stars. The upper limit of the solid boundary is M  G  = 4 mag and the lower limit is 0.5M ⊙ (M  G  = 9 − 10 mag). Members of the Pleiades are overplotted (gray circles). (b) Stars within the solid curve boundary are selected as single stars and are highlighted as blue dots. Binary stars (orange dots) are stars located within the binary boundary (dashed curves). (c) A zoom-in on the binary selection region. The green dots in the background are artificial stars produced via Monte Carlo simulations based on the photometric uncertainty (see the error estimation in Section 3.2 for details).
Paper: Understanding the Capability of Future Direct-imaging Observations to Quantify Atmospheric Chemical Effects of Stellar Proton Events
Authors: Georgios P. Afentakis, Kyla Mullaney, Howard Chen, John Blalack, Jade Checlair, Dorian S. Abbot
Figure caption: Time series of the proton fluence (stellar flares, top), global-mean NO2 column (middle,black), NO2 column at the antistellar point (middle, red), NO2 column at the substellar point (middle, blue), and S/N of NO2 including clouds in the calculation (bottom, blue) and excluding clouds (bottom, black) for an Earth-sized, oxygen-rich planet orbiting a K star that is 2 pc from Earth and observed at a phase of 45°.
Paper: Understanding the Capability of Future Direct-imaging Observations to Quantify Atmospheric Chemical Effects of Stellar Proton Events
Authors: Georgios P. Afentakis, Kyla Mullaney, Howard Chen, John Blalack, Jade Checlair, Dorian S. Abbot
Figure caption: NO2 vertical profile from Kopparapu et al. (2021) and our O2-rich G-star planet (left). Signal-to-noise ratio (S/N) for a detection of NO2 for both models assuming a LOIVOIR-type telescope with a 15 m diameter and only considering UV data, as in Kopparapu et al. (2021; right).
Paper: Free-floating Planet Mass Function from MOA-II 9 yr Survey toward the Galactic Bulge
Authors: Takahiro Sumi, Naoki Koshimoto, David P. Bennett, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: The observed timescale t E distribution passing criteria CR2 from the 9 yr MOA-II survey. The 1σ error bars and upper limits are based on the Poisson distribution. The red line indicates the best-fit single-lens model for all populations. The blue dotted line represents the known populations of stars, BDs, and stellar remnants, and the green dashed line represents the planetary-mass population.
Paper: Free-floating Planet Mass Function from MOA-II 9 yr Survey toward the Galactic Bulge
Authors: Takahiro Sumi, Naoki Koshimoto, David P. Bennett, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: IMF of the best-fit PL model for CR2. The red line indicates the best fit for all populations. The blue dotted line and green dashed line show the IMFs for the stellar and BD population and for the planetary-mass population, respectively. The shaded areas indicate 1σ error. The gray dashed line and the shaded area indicate the best fit and 1σ range of the bound planet MF by Suzuki et al. (2016) via microlens. The pink shaded area indicates 1σ uncertainty for the broken power-law FFP model.