adsabs/AstroCLIMB huggingface dataset:
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption:                       ﹩\widehat{{SK}}\,﹩ versus log power for (a) M = 128 and (b) M = 4096. As in the above figures, the center channel is colored blue, the first sidelobe channel in green, and noise in gray. As M rises, the ﹩\widehat{{SK}}\,﹩ values of the weak sidelobes move away from the gray noise more dramatically, leading to cleaner flagging. This data was generated at 20 ksps, which has noticeable sidelobes extending one channel on either side of the center channel. ﹩\widehat{{SK}}\,﹩ thresholds are outlined in red.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Flagging percentages (top) and overflagging percentages (bottom) for single-scale and several multiscale ﹩\widehat{{SK}}\,﹩ shapes compared to the data rate of the RFI signal. These signals are modulated with the BPSK scheme with 100% duty cycle, centered in channel 120, and M = 512.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Waterfall plots of unmitigated and mitigated RFI, for comparing MS-21 ﹩\widehat{{SK}}\,﹩ flagging to the duty cycle of the RFI signal. These signals are modulated with the BPSK scheme with 50% duty cycle, centered at channel 120 and mitigated with M = 512. (a) and (b) Unflagged and flagged 1 ksps signal. (c) and (d) 20 ksps signal. (e) and (f) 100 ksps signal. (g) and (h) 200 ksps signal.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Flagging percentages for various data rates compared to the duty cycle of the RFI signal. Signals with a 1/W FIR cutoff in the symbol smoothing window are shown on the top and 4/W FIR on the bottom. These signals are modulated with the BPSK scheme, M = 512, and mitigated with MS-21 ﹩\widehat{{SK}}﹩.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Flagging percentages comparing data rate to M for several multiscale ﹩\widehat{{SK}}\,﹩ bin shapes. (a) Single-scale ﹩\widehat{{SK}}\,﹩, (b) MS-12, (c) MS-21, (d) MS-42.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: An incoherent stationary astronomical signal that escapes detection by both single-scale and MS-42 ﹩\widehat{{SK}}\,﹩.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: BPSK signal flagging while the carrier frequency is (a) centered on a channel, (b) offset by a quarter channel, and (c) offset by a half channel. In all cases, MS-4X flags at above 90%.
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: APOGEE-derived effective temperature vs. UV color for the selected stars having GALEX photometry. The figure is color-coded by the nominal WD effective temperatures inferred from ATLAS9 (Castelli et al. 1997) and the WD (Koester 2010) grid of synthetic models for a range of temperatures, assuming MS stars as the red companion. The white line shows the initial, simple selection criterion used for the AGGC, chosen to avoid the single-star locus in the upper right corner of the plot.
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: The UV color vs. temperature diagram for WDMS binaries found in the SDSS/SEGUE survey and the galactic and extragalactic symbiotic variables (SySts) reported in Merc et al. (2019; left panel) and chromospherically active stars explored by Boro Saikia et al. (2018) and Martínez-Arnáiz et al. (2010; right panel).
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: The dereddened UV color vs. temperature distribution for confirmed WDs in the SDSS. The red line shows expectations for a blackbody. The blackbody was generated by the synthetic models in the Virtual Observatory facility (VOSA), and the steps in temperature jump from 50 to 1000 K for temperature hotter than 20,000 K; the log scale amplifies this effect.
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: Top panel: the best-fitting SED (black line) for a WDMS binary using GALEX, Gaia, 2MASS, and WISE broadband photometry (black circles). The red line is the best Kurucz model (Castelli et al. 1997) fit for the secondary, while the blue circles/line represent the best-fitting Koester (2010) model for the WD. Bottom panel: WD temperature–radius plane color-coded by the χ 2 value. The blue color indicates the lowest χ 2 value.
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: Left panel: stellar radius logarithmic distribution for the MS and RG star secondaries in solar radii. Most of the MS stars have radius close to 1 R ⊙ (black line). We also have subgiants and giant star secondaries with a large range in radius (red dashed line). We use the APOGEE surface gravity to select MS and RG objects, as indicated in the legend. The distribution shows a group of giants with R ∼ 10 R ⊙, associated with the RC. Right panel: stellar radius distribution for the WD candidates, where the units are in Earth radii for MS (black line) and RG (red dashed line). The vertical black line represents the value R = 25 R ⊕. The number of WDs with R < 3 R ⊕ is much larger for MS than for RG. In the RG distribution most of the WDs have R ∼ 9 R ⊕.
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: The UV color vs. APOGEE-derived temperature diagram for different types of stars as classified by Clementini et al. (2019) or as listed in the SIMBAD database. The solid lines inside the figures represent the “chromospherically active area.” See text for details.
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: The UV color vs. ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ diagram for the Boro Saikia et al. (2018; black circles) and Martínez-Arnáiz et al. (2010; red circles) catalogs. The most active stars tend to have UV colors ﹩{\left(\mathrm{FUV}\mbox{--}\mathrm{NUV}\right)}_{\circ }\lt 4.0.﹩
Paper: White Dwarf Binaries across the H-R Diagram
Authors: Borja Anguiano, Steven R. Majewski, Keivan G. Stassun, Carles Badenes, Christine Mazzola Daher, Don Dixon, Carlos Allende Prieto, Donald P. Schneider, Adrian M. Price-Whelan, Rachael L. Beaton
Figure caption: Histogram of the discrepancies between the temperature and the radius derived in the SDSS spectra and those derived in this work using an SED-fitting procedure. A fit with a simple Gaussian (black line) reveals small offsets in the results coming from the two methods and a dispersion of ∼2200 K for the temperature and ∼0.6 R ⊕ for the WD radius.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: An average periodogram of 7431 CORR, PCA, and RAW light curves for stars with T eff between 8000 and 9000 K that appear to be aperiodic. This highlights the artificially injected periods due to the systematics from TESS, most notably at ∼7 and 14 days, corresponding to 0.5 and 1 orbit of TESS around the Earth. RAW light curves are most susceptible to these systematics but can recover the real periods >7 days most faithfully compared to the literature. CORR light curves are least dominated by systematics, but they largely suppress longer periods in their corrections.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Example of the periodic light curves and the corresponding Lomb–Scargle periodograms of the sources in this work.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: Corner plots showing the posteriors of all parameters from the NS analysis for the three-planet model. The top panel of every column shows the histogram distribution of each parameter. The bottom left cornerplot, from top to bottom and left to right the parameters are: RV offsets of HARPS, FEROS, and HIRES, RV jitters of HARPS, FEROS, and HIRES, K d, P d, e d, K b, P b, e b, K c, P c, and e c. The top right cornerplot shows the posterior distribution of the derived parameters: the semimajor axes a d, a b, and a c, the minimum masses ﹩{m}_{{\rm{d}}}\sin i﹩, ﹩{m}_{{\rm{b}}}\sin i﹩, and ﹩{m}_{{\rm{c}}}\sin i﹩, and the mean longitudes, which are λ b,c,d = ω b,c,d + M db,c,d. The two-dimensional contours indicate the 1, 2, and 3σ confidence levels of the posterior distribution. The red lines mark the position of the median values.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: Top row: the evolution of the semimajor axes a and eccentricities e for HD 33142d (blue), HD 33142b (red), and HD 33142c (green) of a representative stable fit from the posterior distribution. Middle row: the evolution of apsidal angles Δω d−b, Δω d−c, and Δω b−c, which are librating in an antialigned, aligned, and antialigned geometry, respectively. For purposes of providing a clear representation, the plot only shows a 50,000 yr excerpt.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: MLP of the combined RV data from HARPS, HIRES, and FEROS, as well as stellar activity indicators. The horizontal lines correspond to the FAP levels of 10% (dotted line), 1% (dotted–dashed line), and 0.1% (dashed line). The orbital periods of the planets are indicated as vertical dashed blue lines and the estimate for the rotation period by Jofré et al. (2015) is shown as a red dashed line, while the red shaded area denotes its uncertainties (see Table 1).
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption:  N-body simulations of the HD 33142 system, including stellar evolution effects on the orbital evolution, in particular the planetary semimajor axis a (colored lines). Initial conditions from the N-body simulations were adopted from the stable median posterior values presented in Table 3. The evolution of the stellar radius (dashed curve and the underlying gray area) is expressed in astronomical units. The WD phase is off-scale, since the stellar radius at age 3.2 Gyr is only ∼4 × 10−5 au.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: Distribution of 1000 randomly sampled NS posteriors integrated for 1 Myr. The black, two-dimensional contours indicate 1, 2, and 3σ confidence intervals of the whole posterior distribution, and the red contours indicate 1, 2, and 3σ confidence intervals for the stable subsample. Only the mean planetary eccentricities and eccentricity amplitudes for all three planets are shown, which are decisive for the system’s stability and dynamical properties. The median values of the total posterior distribution are marked with green lines.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: Top main panel shows the RV measurement time series from HIRES (green triangles), HARPS (blue circles), and FEROS (red stars) and the best three-planet model for HD 33142 (gray line; Table 3). Top small panel shows the data residuals after applying the best three-planet Keplerian model. The data uncertainties include the RV jitter. The bottom panels show phase-folded representation of the planetary signals. In each case, the orbits of the other two planets were subtracted.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: Distribution of 141 known exoplanets (black points) around giant stars on a diagram of minimum mass vs. orbital period. The planets of the HD 33142 system are indicated as red star symbols. The lines approximate the locations of RV semiamplitudes of 10,100 and 1000 m s−1 for a host star of 1.5 M ⊙.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: Same evolution as in Figure 5 but for the trajectory evolution of HD 33142d, b, and c, as a function of the product of their eccentricity and sine/cosine of their mutual Δω. In all cases, these variables exhibit libration around a fixed point (red dot, centered at [0,0]).
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: Schematics of the MBCM strategy. (a) In MBCM targeted searches, an ETI signal detected by Beam 1 cannot appear in the 6 outermost beams, otherwise it is RFI. (b) An example of permitted signals in MBCM blind searches. (c) An example of forbidden signals in MBCM blind searches. Beams 5, 6, and 17 are arranged in a line; thus an extraterrestrial signal cannot cover them simultaneously.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: A schematic of the FAST multibeam digital backend for the L-band 19 beam receiver. Every two beams share one Roach 2 FPGA board, except for Beam 19. Before processed by Roach 2, the signals in polarization directions X and Y are transmitted and sampled separately. After self-correlation and cross correlation of the data of two polarization directions, the data output by the FPGA for one beam consists of 4 polarization channels: XX, YY, X *Y, and Y *X.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: A signal at 1140.604 MHz detected during our 20 minutes observation toward Kepler-438. This signal is only present in Beam 1, not in any other beam, and is the only signal that satisfies this characteristic in our observations.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: Histograms of hits and events for XX as functions of frequency, drift rate, and S/N. Frequency bands of cataloged interference sources are displayed on the frequency panel. The blue bars show the distributions of the hits detected by all 19 beams. The orange bars show the distributions of the events detected by Beam 1.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: Histograms of hits and events for YY as functions of frequency, drift rate, and S/N.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: Examples of false positives. (a) An event visible in the reference beams. (b) An event invisible in Beam 1. The red dashed lines show the frequencies and drift rates of the hits in Beam 1 fitted by turboSETI.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: 33 observed targets in equatorial and galactic coordinates. The observable sky of FAST is the region between the green curves. Sources with planets in the habitable zones are denoted by blue symbols. Sources in the Earth transit zone are denoted by diamonds.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: The theoretical beam response at 11′.6 from the beam center for uniform illumination and cosine-tapered illumination for the FAST L-band 19 beam receiver.
Paper: Sensitive Multibeam Targeted SETI Observations toward 33 Exoplanet Systems with FAST
Authors: Zhen-Zhao Tao, Hai-Chen Zhao, Tong-Jie Zhang, Vishal Gajjar, Yan Zhu, You-Ling Yue, Hai-Yan Zhang, Wen-Fei Liu, Shi-Yu Li, Jian-Chen Zhang, Cong Liu, Hong-Feng Wang, Ran Duan, Lei Qian, Cheng-Jin Jin, Di Li, Andrew Siemion, Peng Jiang, Dan Werthimer, Jeff Cobb, Eric Korpela, David P. Anderson
Figure caption: The frequency distribution of the 140 events passing visual inspection.