adsabs/AstroCLIMB huggingface dataset:
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: Detection efficiency of infrared excess for stars whose effective temperatures are between 5000 and 6000 K is shown for W3, W4, and M1 from left to right. The number of infrared excesses as a function of the excess ratio is also presented as histograms with the right y-axis colored in red.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: (Top) Based on Table 3, the distance of the target stars from the solar system for all stars and for those with infrared excess are shown as solid and dashed lines, respectively. The data for W3, W4, and M1 are shown in blue, green, and red, respectively. (Bottom) The excess rates for W3, W4, and M1 as a function of the distance.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: The colors of infrared excesses are presented as diagrams of excess ratios. The squares and triangles represent debris disks identified as infrared excesses in both two or only one wavelength band, respectively. Dashed lines indicate the thresholds of excess ratio set in Section 4.1. The bottom half shows histograms for the blackbody temperature of debris disks whose infrared excesses are identified at two wavelength bands.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: Comparison of the distance limits determined by the sensitivities of the surveys (solid lines) and those determined by the contamination (dashed lines) as a function of the color. The limits for W3, W4, and M1 are shown in blue, green, and red, respectively. The tentative distance thresholds adopted in Section 2 are shown in black lines.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: Distributions of ﹩\bar{\chi }﹩ for stars with effective temperatures between 5000 and 6000 K. In these panels, red vertical lines indicate a threshold to identify infrared excess (﹩\bar{\chi }\gt 3﹩).
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: The left and middle panels represent the color–magnitude diagrams for the stars without infrared excesses and those with excesses, respectively. The thick black lines indicate the ridges of the density distributions. The thin black lines show the MS region discussed in Section 2.4. The right panels show comparisons of the ridges with isochrones from 100 Myr to 5 Gyr and evolutionary tracks of 1.2, 1.5, and 1.8 M ⊙ stars in the zoomed area presented by dashed lines in the left and middle panels.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: The left panel shows differences in effective temperature between the best-fit models and inputs of mock binaries. The right panel presents the reduced chi-square map of the SED fitting for mock binaries.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: The maps for the excess ratios of binary excesses are presented.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: The SED fitting for a mock binary is presented, in which only photometric data with filled symbols are fitted to determine stellar parameters.
Paper: Frequencies of Warm Debris Disks Based on Point Source Catalogs of Spitzer, WISE, and Gaia
Authors: Toshiyuki Mizuki, Munetake Momose, Masataka Aizawa, Hiroshi Kobayashi
Figure caption: The left panel presents the frequencies of debris disks. The right panel shows the ridges on the color–magnitude diagram with respect to the presence of the infrared excesses of W3. The dashed lines represent the frequencies and the ridges, for which binary candidates showing near-infrared excesses are included in the sample.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: TESS PDCSAP 2 minute exposure light curve of GJ 238 plotted in mean-subtracted relative flux (in parts per thousand, or ppt) as a function of time in days. The top panel shows the data in Sectors 1–6 and 8–13, and the bottom panel shows data in Sectors 27–39. Gaps in the data are primarily due to data downloads and intervals of bad data (due to, e.g., momentum dumps and scattered light). The wide gap in the top panel is during a sector when GJ 238 was not observed by TESS.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: The two left panels show the target’s field of view as observed by UKST and processed by the Digitized Sky Survey on 1979 December 21 (leftmost panel) and 1995 January 25 (second panel from the left). The third panel from the left shows the target’s field as observed by Las Cumbres Observatory (LCO) 1 m/Sinistro on 2023 February 1 with the SDSS-r filter. The three left panels show a 2.′5 × 2.′5 field of view centered on the target’s position at epoch 2015.5. The motion of the target, which is the brightest star in the field, is clearly seen. The rightmost panel shows a zoomed-in view of the target and the two stars closest to it on the sky, encircled in green and labeled by their TIC ID. The image is 1.′0 × 1.′0 and the green circles have a 2.″0 radius. In each panel north is up and east is to the left, and the panel’s title provides its source and the fractional year when they were obtained.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Light curves of the two closest stars to the target spanning a predicted transit time, based on observations with LCO 1 m/Sinistro on 2022 November 18, with a Pan-STARRS z s filter (overlapping the TESS band). Both light curves are plotted in relative flux, and shifted from each other along the y-axis for clarity. The seeing during this observation was 2.″6 and a 4.″0 aperture diameter was used to extract the light curves (for comparison, the distance between TIC 737377690 and the target was close to 10″ at the time of observation). The two gray points along the x-axis mark the predicted transit start and end times. The uncertainty on those values is similar to the size of the markers. The brightness difference between the target and TIC 737377690 and TIC 737377689 is about 8.2 mag in the TESS band and 7.9 mag in G (the two nearby stars have similar brightness and color). Given these brightness differences, to explain the transit seen in the TESS data one of the light curves would have to show a 25% deep eclipse. Such deep eclipses can be ruled out.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Archival HARPS RVs of GJ 238, from Trifonov et al. (2020). The left panel shows the RVs as a function of time, in BJD. The center panel also shows the RVs as a function of time in BJD but while zooming in on the groups of RVs obtained during the same observing season. The right panel shows the RVs phase folded on the transit ephemeris.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Left: planet radius vs. equilibrium temperature at the planet’s orbit assuming zero bond albedo and no heat circulation. Right: planet radius vs. host star distance to the Sun in log scale. In both panels, planets with a radius measurement better than 4σ are marked in black, and those which also have their mass measured to better than 4σ are marked in red. GJ 238 b is marked by a purple diamond. Solar system terrestrial planets are marked in blue in the left panel. The figure is based on data from the NASA Exoplanets Archive, downloaded on 2023 December 18.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Speckle imaging of GJ 238. Each panel shows the contrast curve, in magnitude difference, as a function of angular distance from the target in arcseconds, and the speckle auto-correlation function in the inset. Top: speckle imaging obtained at SOAR in the I band, on 2020 February 10. Bottom: speckle imaging obtained with Gemini-South/Zorro, on 2020 March 13, in 562 nm (blue line) and 832 nm (red line and inset).
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Period analysis of WASP times-series photometry. The panels show periodograms of three seasonal data sets (left column panels) and the phase-folded and binned light curve using the putative 44 day rotational period (right column panels). The strongest peak of the 2010–2011 and 2011–2012 seasons periodogram is at 44 days, while for 2008–2009 it is at the 22 day first harmonic. The horizontal dashed lines are the estimated 1% false-alarm levels.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: GJ 238 SED. The red symbols represent the observed photometric measurements, and the horizontal bars represent the effective width of the passbands. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The Gaia spectrophotometry is shown in gray in both the plot and the inset close-up view of the blue end.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Left: GJ 238 b TESS phase-folded and binned transit light curve (in parts per million, ppm) covering an entire orbital period with the transit at phase zero. Right: phase-folded and binned transit light curve zoomed in on the transit phase. The best-fit model is shown with a black solid line. The lower part of the panel shows the residual flux, after subtracting the model from the data, and offset by 400 ppm, marked by the dashed black line.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: A single transit-like feature that appears in the TESS light curve of GJ 238 during Sector 2. The plot shows relative flux, in units of ppt, as a function of time in days (BJD). If this feature is due to a transiting planet then its depth of about 0.6 ppt corresponds to a planet radius of about 3.6 R ⊕, close to the size of Neptune.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Planet radius (linear scale) vs. planet mass (log scale) for known transiting small planets with mass and radius measurements beyond a 4σ significance. GJ 238 b radius is marked by the red horizontal band, whose width corresponds to the ±1σ measured radius uncertainty. The dashed lines are composition models from Zeng et al. (2016), including, from bottom to top, pure iron (100% Fe; dashed purple line), Earth-like composition (32.5% Fe + 67.5% MgSiO3; dashed blue line), and pure rock (100% MgSiO3; dashed brown line). A few of the planets are labeled, where T1 is an abbreviation for TRAPPIST-1. Solar system terrestrial planets are marked in blue, where Earth is labeled by “E,” Venus by “V,” Mars by “Ma,” and Mercury by “Me.” The figure is based on data from the NASA Exoplanets Archive, downloaded on 2023 December 18.
Paper: GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
Authors: Evan Tey, Avi Shporer, Zifan Lin, Keivan G. Stassun, Jack J. Lissauer, Coel Hellier, Karen A. Collins, Kevin I. Collins, Geof Wingham, Howard M. Relles, Franco Mallia, Giovanni Isopi, John F. Kielkopf, Dennis M. Conti, Richard P. Schwarz, Aldo Zapparata, Steven Giacalone, Elise Furlan, Zachary D. Hartman, Steve B. Howell, Nicholas J. Scott, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, David Charbonneau, Zahra Essack, Stephanie Striegel, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Stellar insolation at a planet’s orbit as a function of escape velocity from the planet’s surface, in log–log scale. Based on data from the NASA Exoplanet Archive, downloaded on 2023 May 18. The empirical “cosmic shoreline” and the water vapor greenhouse runaway threshold (Zahnle & Catling 2017) are shown in cyan and yellow, respectively. Planets are categorized into terrestrial planets (magenta), sub-Neptunes (blue), Neptune-like planets (green), and gas giants (yellow) based on radius, see legend. The red line shows the possible range of escape velocities of GJ 238 b. Because only radius, but not mass, is known, the two endpoints represent two extreme interior scenarios—a 100% iron composition and a 100% silicate composition.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: The Hertzsprung–Russell diagram depicts CHES targets, comprising 19 F stars, 24 G stars, and 51 K stars.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Left panel: the relation between ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ and peak-to-peak variations of photometry; the dashed line shows a parabolic fitting. Right panel: same for the relation between ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ and activity level, while the error bars show the uncertainties in the activity level. The blue circles, orange crosses, and green triangles correspond to F, G, and K stars, respectively.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Properties of the fitted mass (left panel) and periods (right panel) vs. true values of 107 Psc, where every point indicates an injected planet. The red solid line indicates equal values, and the green dashed line and the black dashed–dotted line indicate a 30% upper and lower uncertainty level, respectively.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: The standard deviations of astrometric jitter in two directions of all targets from the simulations. The blue circles, orange crosss, and green triangles correspond to F, G, and K stars, respectively. The two histograms shows the jitter distribution of our sample.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: The photocenter jitter due to spots and faculae of HD 103095 during 5 yr, where the blue circles and orange crosses represent the effects of spots and faculae, respectively.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: The mean jitter caused by stellar spots and faculae from the simulations. The error bars indicate the maximum and minimum jitter duration during a 5 yr period.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Left: a histogram of detection efficiency, where the colo rbar shows the mean effective temperature in each bin. Right: the detection efficiency and distance of all targets, where point sizes indicate stellar radius. The blue circles, orange crosses, and green triangles correspond to F, G, and K stars, respectively.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Theoretical and observed rotation periods of 33 stars in our sample, the dashed line denotes the observed periods are equal to theoretical periods. Error bars indicates the period ranges from uncertainties of ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: An example of the temporal and spatial evolution of spots and faculae on the surface of target 107 Psc, which has a cycle period of about 1200 days. The latitude distribution of the stellar magnetic features follows the butterfly diagram during 8 yr, where the circles represent spots and the crosses represent faculae. The color bar shows logarithmic areas of features, in units of MSH.
Paper: Closeby Habitable Exoplanet Survey (CHES). I. Astrometric Noise and Planetary Detection Efficiency Due to Stellar Spots and Faculae
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: The activity level with photometric peak-to-peak variations. The step of activity level is 0.2 and the y-coordinate of each point indicates the mean peak-to-peak variations of 100 simulated lightcurves.