adsabs/AstroCLIMB huggingface dataset:
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: Phase diagrams of OGLE-BLAP-007 (left) and OGLE-BLAP-009 (right), corrected for timing variations using the O − C values from Figure 8. The pulsation phases are calculated using the primary frequency f1 obtained from the Fourier spectra in Figure 7. The other descriptions are the same as those for the right panels of Figure 1.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: Fourier amplitude spectra of OGLE-BLAP-007 (left) and OGLE-BLAP-009 (right) for the KMTNet I-band data, corrected for timing variations. The lower panels display the prewhitening results. A peak near f1 in the lower-right panel is identified as an unresolved frequency.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: O − C residuals (in minutes) for seven BLAP candidates with wide-orbit companions, derived from OGLE data segmented by year. The plot shows periodic variations likely due to the LTT effect, particularly evident for OGLE-BLAP-024.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: Fourier spectra of the O − C residuals for OGLE-BLAP-007 (left) and OGLE-BLAP-009 (right). The other descriptions match those in Figure 5.
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: The differences of the precisions (﹩\sqrt{{\sigma }_{{\rm{\alpha cos\delta }}}^{{\rm{2}}}+{\sigma }_{{\rm{\delta }}}^{{\rm{2}}}}﹩) by using only high-SNR reference stars and by using both high-SNR reference stars and low-SNR reference stars when measuring the same stars via the refined approach. Average of each bin of 1 Gmag is marked as a red circle. Note that, the residuals in R.A. direction have multiplied with cos(decl.).
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: The left panel shows the average precisions (﹩\sqrt{{\sigma }_{{\rm{\alpha cos\delta }}}^{{\rm{2}}}+{\sigma }_{{\rm{\delta }}}^{{\rm{2}}}}﹩) in Gmag bins for the observations via a conventional weighted fourth-order polynomial in blue and the refined approach in red. The right panel shows the difference of the precisions. The enhancement of position precision at the bright end is less significant than the medium-bright stars and the reason might be effects of saturation. The bin size is 0.5 Gmag. Note that, the residuals in R.A. direction have multiplied with cos(decl.).
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: The residuals of the astrometric reduction for Himalia's observations of each night via a weighted fourth-order polynomial (30c), the early version PP technique, and the refined approach (refined PP), which are marked as a black circle, blue circle, and red circle, respectively. Note that the residuals in R.A. direction have multiplied with cos(decl.).
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: All the residuals of the astrometric reduction for Himalia via a weighted fourth-order polynomial (30c), the early version PP technique, and the refined approach (refined PP), which are marked as a black circle, blue cross, and red triangle, respectively. Note that the residuals in R.A. direction have multiplied with cos(decl.).
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: The results of the precisions derived via the early version PP technique (black circle) and the refined approach (red circle) for 2018 November 13 and 2021 January 15, respectively. The average of each bin of 1 Gmag is marked as a blue circle. The dotted line marks the average precision for all the results of each method. Note that the residuals in R.A. direction have multiplied with cos(decl.).
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: The average premium rate of the precision (﹩\overline{{ \mathcal P }}﹩) as a function of the effective FOVs. The blue circles represent the premium rate and the red stars marks the average premium rate of the observation taken with the same CCD. Note that, the residuals in R.A. direction have multiplied with cos(decl.)
Paper: A Refined Astrometric Approach Based on the Precision Premium and its Application to the Jupiter’s Satellite Himalia
Authors: Z. J. Zheng, Q. Y. Peng, F. R. Lin, D. Li
Figure caption: Residual in alt-azimuth coordinate system against (BP − RP)Gaia before and after DCR correction. Note that the results are based on the stars brighter than 16 Gmag.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The fraction of condensed mass composed of major species at radii between 0.5 and 4 au. Vertical bars span between the maximum and minimum of mass fraction for the species measured at 0.5, 1, 2, and 4 au for the respective simulation. Each vertical bar is offset from the center of the species name in the same repeating order (left to right) as the order of the legend (top to bottom). Black tick marks (gray ticks for the black/solar bar) denote the value at 1 au. For example, the bottom of the C/O = 10 line above the species graphite indicates that the minimum condensed mass fraction of graphite at radii of 0.5, 1, 2, and 4 au was about 50%. The top of the line for C/O = 10 shows the maximum was above 90%. Note that only the values associated with the 1 au tick marks can be summed to find the total condensed mass of the shown species. Note that these species are not permanent and will change with later heating and aqueous alteration.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The solid surface density profile with distance from the Sun. The solid surface density for each C/O simulated is normalized to the solid surface density profile of the solar C/O. Recent studies show that C/Os above 1 occur in <0.1% of stars (J. M. Brewer & D. A. Fischer 2016). We include these simulation results for comparison with past studies, like J. C. Bond et al. (2010b).
Paper: The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts
Authors: Ariane Deslières, Charles Cadieux, René Doyon, Étienne Artigau, Neil J. Cook, Clémence Fontanive, Thomas Vandal
Figure caption: Top left: RV time series with, in green, the G. M. Brandt et al. (2021) orbital solution of Gl 229 B. Bottom left: FWHM time series inferred from the LBL dLW activity indicator. The vertical blue dashed line separates the values obtained before and after the optical fibers change in the HARPS instrument. Data points in yellow are those with an SNR lower than 50. Right panels: Lomb–Scargle periodograms of the RVs (top) and FWHM (bottom). The vertical dashed lines represent the reported period of 121.933 days for planet Gl 229 A c (F. Feng et al. 2022; in pink), the reported period of 471 days for planet Gl 229 A b (M. Tuomi et al. 2014; in yellow), the other reported period for planet Gl 229 A b of 579.474 days (F. Feng et al. 2022; in green), and the rotation period of the star (in gray) at 28.9 days. The horizontal black dashed line represents the 99.9% confidence level. The window function is displayed in cyan.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The same figure as Figure 11 except N/Os are varied for each simulation. Vertical bars span between the maximum and minimum mass fraction for the species measured at 0.5, 1, 2, and 4 au for the respective simulation. Black tick marks (gray ticks for the black/solar bar) denote the value at 1 au. Note that these species are not permanent and will change with later heating and aqueous alteration.
Paper: The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts
Authors: Ariane Deslières, Charles Cadieux, René Doyon, Étienne Artigau, Neil J. Cook, Clémence Fontanive, Thomas Vandal
Figure caption: Radial velocity variations of Gl 229 A induced by its BD companion Gl 229 B using the orbital solution from G. M. Brandt et al. (2021). The BD is on an 86,909 days, eccentric (e = 0.851) orbit, inducing a K  ≈  120 m s–1 radial velocity signal. The zoomed-in subpanel displays the RV change during the HARPS measurements time span with, in red, a linear fit.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The same graphic as Figure 3, but here the amount of initial oxygen is held constant at the solar value (i.e., w/Oc) while the initial C/O varies.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The same graphic as Figure 10, but here the C/Os examine the transition in composition around C/O = 0.8. Note that these species are not permanent and will change with later heating and aqueous alteration.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The solid surface density profiles of five select elements in three different simulations, which hold either oxygen or carbon constant: (left) C/O = 1 w/Cc, (middle) C/O = 0.8 w/Oc, and (right) C/O = 1 w/Oc. Compare the corresponding C/O here to the “constant sum” simulations in Figure 4.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: Masked flux maps for each emission line in SN 3, SN 2, and SN 1: Hα, [N II]λ6548, [N II]λ6583, [O III]λ5007, Hβ, [O II]λ3726+[O II]λ3729. The calculated flux maps are masked below a SNR of 3 and a flux cut at 1 × 10−17 erg s−1 cm−2 Å−1. Remaining noisy pixels were removed manually using ds9. In the background, we display the exposure-corrected, background-subtracted, merged Chandra image. The images are aligned to approximately 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩7.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: BPT diagram showing log([N II]λ6583/Hα vs. log([O III]5007/Hβ) in the central region of NGC 1275. The points are color coded by their distance to the AGN at the center of NGC 1275. The cyan arrow represents the upper bound of the brightest pixel in the small northern filament. The AGN is marked by a black star. We overplot the L. Kewley et al. (2001, hereafter K01; purple), K03 (orange), and K06 (blue) diagnostic lines. The region between the K01 and the K03 lines is considered a composite region. Spaxels falling in the composite region are considered to be ionized by multiple types of ionizing sources with a range of characteristic average energy per ionization particle or photon.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: Composite image of the SN 1 (365–385 nm; blue), SN 2 (480–520 nm; green), and SN 3 (651–685; red) filters emission in NGC 1275 obtained with SITELLE on the CFHT. We constrain the image only to cover approximately a quarter of the SITELLE field of view in order to highlight the optical emission nebula.
Paper: Mapping the Filamentary Nebula of NGC 1275 with Multiwavelength SITELLE Observations
Authors: Carter Lee Rhea, Julie Hlavacek-Larrondo, Marie-Lou Gendron-Marsolais, Benjamin Vigneron, Megan Donahue, Auriane Thilloy, Laurie Rousseau-Nepton, Mar Mezcua, Norbert Werner, Jorge Barrera-Ballesteros, Hyunseop Choi, Alastair Edge, Andrew Fabian, G. Mark Voit
Figure caption: Illustrative SN 1 (a), SN 2 (b), and SN 3 (c) spectra (blue) and corresponding fit (purple). The spectrum is integrated from a square region containing 9 pixels (3 x 3 bin) centered at (3:19:49.7, +41:30:45.4) corresponding to the left-hand side of the central region. The x-axis has been shifted by the redshift of NGC 1275. The bottom row shows the SN 1 (d), SN 2 (e), and SN 3 (f) sky emission spectra (orange). Here, the spectrum is integrated from a circular region centered at (3:19:42.4979, +41:32:01.810) with a radius of 9﹩\mathop{.}\limits^{\unicode{x02033}}﹩6.
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: The distributions of frequency, drift rate, and S/N in XX polarization. The frequency bands of cataloged interference sources are displayed on the frequency panel. The dark blue bars indicate the distributions of the hits detected by all 19 beams. The light blue bars indicate the distributions of the events removed the zero drift rate signals and detected by the MBCM blind search mode.
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: Three examples of allowed signals of the MBCM blind search mode. This figure is same as the upper panels of Figure 1 in X.-H. Luan et al. (2023).
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: The distributions of frequency, drift rate, and S/N in YY polarization.
Paper: Precise Parameters from Bayesian Spectral Energy Distribution Fitting Indicate Thermally Driven Mass Loss Likely Driver of Radius Valley
Authors: David Jordan, Inseok Song
Figure caption: Plot of the relative positions of theoretical model predictions from Table 1 (orange diamonds), observational results from Table 2 (blue circles), and this work (green squares) for the slope of the radius valley when viewed as planet radius vs. orbital period (horizontal axis) and planet radius vs. stellar mass (vertical axis) on a log–log scale. Uncertainties are also shown for all observational results including this work. Planet formation processes and their ranges are given by the shaded regions as predicted by the models for each axis.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Top: time-series RV data from Keck-HIRES (black points) and median RV model (blue line). The need to include a long-term trend (dashed black line) in addition to the two planetary Keplerian signals is evident. The χ2 of the RV model to the data (19 data points) with and without the RV jitter term is 15 and 45, respectively. Bottom: individual components of the RV for each planet folded on the best-fit ephemeris such that a phase of zero is the conjunction time (Table 3). The blue lines are the median models and the blue shaded regions are the 68% confidence intervals.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: The stability probability for a system of three 10.5 M⊕ planets with a given eccentricity (as a fraction of the crossing eccentricity) and period ratio accompanied by an outer giant with the properties of Kepler-511 b calculated by SPOCK. The dashed line indicates the rms time-averaged eccentricity of the three planets as a result of their interaction with the outer giant calculated via secular analytical theory.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Bulk metallicity parameter space for Kepler-511 b (y-axis) and Kepler-511 c (x-axis). On both axes, the stellar metallicity is shown with the black triangles. The solid red line (corresponding to the right-side y-axis) shows the time (tacc for Kepler-511 c to accrete its GCR of  ∼1/6.7. Grayed-out regions exclude scenarios whereby Kepler-511 c has tacc < 0.1 Myr, which would require fine-tuning to prevent it from undergoing runaway gas accretion. The allowed regions of parameter space (green) suggest that Kepler-511 c accreted material with a higher metallicity than the host star. The metallicity of the material accreted by Kepler-511 b is likely lower than that of the host star, as the higher metallicity region is unrealistic.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Multiplanet systems with planets that have measurements for both their masses and radii are shown (data from the exoplanet archive). Systems that do not have a single planet with mass ≥95M⊕ or any planet with 17M⊕ <  mass <95M⊕ are grayed out. The Kepler-511 planets are shown with black diamonds. Kepler-511 b is the longest orbital period planet in such a sample. Gas-rich giants (>95M⊕) are typically accompanied by planets that are significantly less massive than Kepler-511 c. Some planets that do have masses similar to Kepler-511 c are typically much larger than it, indicating that they are much more gas-rich compared to Kepler-511 c.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Top: corner plot for the constraints on the semimajor axis (AU), ﹩M{\rm{\sin }}i﹩ (MJup), and eccentricity of the distant companion. The red dashed lines in the eccentricity– semimajor axis 2D histogram mark pericenter values of 1, 5, and 10 au. Bottom: black points mark the RV data with the best-fit model for the two transiting planets subtracted out. The black curve shows the best-fit model to the long-term trend and the red curves correspond to 1000 models from randomly drawn parameters from the posterior.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Top: the SED for Kepler-511 from 2MASS, Gaia, and WISE in red along with the maximum likelihood model from our EXOFASTv2 fit in blue. Bottom: residuals of the fit normalized by the uncertainties in the SED measurements.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Posterior probability distributions for bulk metallicity (Zp) retrievals for Kepler-511 b (left) and Kepler-511 c (right). For Kepler-511 b, the inferred values of Zp do not show significant correlations with the measured planet masses or system age; for Kepler-511 c, mass, and Zp are positively correlated to fit the planet’s observed radius (planet radius increases with mass at a constant metallicity in this planet mass range). By mass, Kepler-511 b and Kepler-511 c are 22% and 87% heavy elements.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Kepler data and the median transit model, folded on the best-fit ephemeris (Table 3), for both Kepler-511 planets. Gray points represent individual frames, and red points are 1 and 0.5 hr bins for Kepler-511 b and Kepler-511 c, respectively. The rms error on the residuals is 414 ppm.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: RealMatch analysis plots for two of our RV spectra (R. Kolbl et al. 2015). We rule out any secondary companions brighter than 1% of the primary’s brightness with an RV separation of ≥±10 km s−1.