adsabs/AstroCLIMB huggingface dataset:
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: In the top two panels, we show the predicted apparent speed of C1's equivalent receding jet ejection for various inclination angles. In the bottom plot, we show the expected distance traveled downstream by C1's receding jet equivalent, since C1's estimated ejection time.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Same as Figure 19, but for the C2 component.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Montage of all frequencies, stacked across the different epochs. The contour levels are at ﹩{\rm{noise}}\times {\sqrt{2}}^{n}﹩, where n = 2, 4, 6, 8,.... The vectors show the EVPA-corrected electric field directions but are not corrected for Faraday rotation.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Same as Figure 12, but for epoch 12.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Same as Figure 12, but for epoch 4.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Same as Figure 12, but for epoch 5.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Same as Figure 12, but for epoch 6.
Paper: The Subparsec-scale Structure and Evolution of Centaurus A. III. A Multi-epoch Spectral and Polarimetric VLBA Study
Authors: S. Prabu, S. J. Tingay, A. Bahramian, J. C. A. Miller-Jones, C. M. Wood, S. P. O'Sullivan
Figure caption: Same as Figure 12, but for epoch 3.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Comparison among the main asteroid belt’s remaining mass, ephemeris uncertainty, and the Yarkovsky effect for the asteroid (6130) Hutton. (a) Influence of main asteroid belt's remaining mass, ephemeris error, and Yarkovsky effect on the predicted orbit of the asteroid (6130) Hutton. The orbit prediction spans approximately 70 yr. The ordinate depicts the difference when including or excluding the remaining mass. The remaining mass is set at 3.4 × 10–11 M Sun, and two radii of the modeled main belt's remaining mass ring (2.316 and 3.165 au) are tested. This figure also includes the difference caused by the ephemeris error, which is represented by the positional difference of the planets between DE441 and INPOP21a. Furthermore, the position difference caused by excluding and including the Yarkovsky effect is displayed. The unit of the reference Yarkovsky parameter A2 is au · day−2. Three different reference Yarkovsky parameters are tested here. (b) Trajectory of the asteroid (6130) Hutton. The dotted line is the modeled main belt remaining mass ring.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: The observation error caused by different ephemeris or the different radii of the main belt remaining mass ring.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Distribution of the MCAs’ absolute magnitude and observed arc length. The majority of observed MCAs exhibit magnitudes ranging from 18 to 20. Excluding MCAs with an observed arc length less than 10 yr, the majority of the remaining MCAs are observed for approximately 30 yr.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Parameter S as a function of ﹩{{\rm{SNR}}}_{{A}_{2}}﹩ for all MCAs. The orbit determination process is seven-dimensional. The weight for all Gaia’s data along the AL direction is set as its actual observation accuracy.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Residuals for Gaia data using six-dimensional and nine-dimensional differential correctors for the asteroid (101429). (a) The figure illustrates the residuals along the AL and AC directions when including all of Gaia's data for the asteroid (101429). (b) The figure illustrates the residuals along the AL and AC directions when deleting the two data with large residuals in Figure 8(a).
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Relative strength of each force with respect to the Sun’s monopole gravity for the asteroid (6141) Durda. Here SRP means the solar radiation pressure, and J2 represents the main component of Sun's nonspherical perturbation. “GR” stands for general relativity. F Sun in the legend of the ordinate indicates the strength of the Sun’s monopole acceleration.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Position difference of the eight planets and Pluto with respect to the epochs between the DE441 and the INPOP21a ephemerides. The ordinate indicates the difference in the planet’s heliocentric distance.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Comparison of Gaia data residuals between the seven-dimensional and the nine-dimensional differential correctors for all MCAs.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Parameter S as a function of ﹩{{\rm{SNR}}}_{{A}_{2}}﹩ for all MCAs. The orbit determination process is nine-dimensional.
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: SED of AF Leporis b in the context of new GRAVITY observations. The top panel plots our reprocessed SPHERE IFS (small circles) and IRDIS (squares) spectrophotometry (see Section 2.2), Keck/NIRC2 Lp photometry from K. Franson et al. (2023a, 2024; large circle), and JWST/NIRCam F444W photometry from K. Franson et al. (2024; hexagon), alongside the GRAVITY spectrum from this work (line). The bottom left panel plots the GRAVITY spectrum as error bars with uncertainties corresponding to the square root of the diagonal of the covariance matrix. The spectrum is dominated by methane absorption from 2.2 to 2.4 μm; there is correlated noise lurking beneath the prominent molecular absorption features. The bottom right panel plots the empirical covariance matrix of the GRAVITY spectrum, in terms of the maximum value of the matrix, with a log stretch in order to illustrate the small but nonzero off-axis correlation terms. These are accounted for in all the spectral analyses in this paper. The new SPHERE and GRAVITY spectra are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: Two-body orbits fit to the observations of the AF Lep system. (a) Sky-projected relative astrometry of AF Lep b (blue scatter points) and fit orbits (lines, color-coded by eccentricity). The new high-precision VLTI/GRAVITY relative astrometry constrains the eccentricity and inclination of the orbit and, when coupled with the long time baseline of the VLT/NACO recovery (M. J. Bonse et al. 2024), results in a well-known, circular orbit. (b) Keck/HIRES RV measurements of AF Lep A and the best-fitting orbits. The available RVs do not constrain the orbit fit, and there remain two degenerate solutions for the argument of periastron (ω) and longitude of ascending node (Ω). (c) Projected separation vs. time for each orbit, and relative astrometry. There is larger scatter between single mirror instruments, but these are consistent within 1σ with the best-fitting circular orbits that are driven by the GRAVITY astrometry. (d) Likewise, for the position angle vs. time for each orbit and the relative astrometry. (e, f) The proper motions in R.A. and decl. for AF Lep A (blue scatter points) and the reflex motion due to the orbit of AF Lep b (colored lines).
Paper: VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity
Authors: William O. Balmer, Kyle Franson, Antoine Chomez, Laurent Pueyo, Tomas Stolker, Sylvestre Lacour, Mathias Nowak, Evert Nasedkin, Markus J. Bonse, Daniel Thorngren, Paulina Palma-Bifani, Paul Mollière, Jason J. Wang, Zhoujian Zhang, Amanda Chavez, Jens Kammerer, Sarah Blunt, Brendan P. Bowler, Mickael Bonnefoy, Wolfgang Brandner, Benjamin Charnay, Gael Chauvin, Th. Henning, A.-M. Lagrange, Nicolas Pourré, Emily Rickman, Robert De Rosa, Arthur Vigan, Thomas Winterhalder
Figure caption: Detections of AF Lep b within the VLTI/GRAVITY fiber field of view. Each panel visualizes the ﹩{z}_{\mathrm{red}}={\rm{\Delta }}{\chi }_{\mathrm{red}}^{2}﹩ calculated for various positions (ΔR.A. and Δdecl. in milliarcseconds, i.e., the displacement with respect to the measured position of the host star AF Lep A), fitting the interferometric observables with a polynomial model of the transmission and stellar halo contribution and a coherent point source with the spectral signature of a T dwarf. Each epoch is presented chronologically, left to right: 2023 November 2, 2023 November 24, and 2023 December 24. The dashed black circle indicates the effective fiber field of view, ∼60 mas. The origin is the placement of the science fiber on-sky for a given observation, a prediction based on the previous available orbit fit. The strongest peak in the χ 2 map reveals the position of the companion, with lower likelihood peaks surrounding this central peak. The shape and distribution of the likelihood depend on the u-v plane coverage of the observations.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: The comparison of the S parameter between different weight rules for Gaia’s data along the AL direction. The S 7d and S 7d,0.1 represent the S value when setting the weight of Gaia’s data along the AL direction to be its real precision and 0.″1, respectively.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Parameter S as a function of ﹩{{\rm{SNR}}}_{{A}_{2}}﹩ for all MCAs. The orbit determination process is seven-dimensional. The weight for all Gaia’s data along the AL direction is set to be 0.″1.
Paper: Precise Orbit Determination of Mars-crossing Asteroids
Authors: Xin Liu, Xi-Yun Hou, Jun Yao, Shanhong Liu, Roberto Armellin, Qingbo Gan, Zhitao Yang
Figure caption: Statistics of maximum observation difference between the orbit integrated with a ring model and the orbit integrated with a 1000-asteroid model.
Paper: Finite-lens Effect on Self-lensing in Detached White Dwarfs-main Sequence Binary Systems
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: For three orbital periods T = 10, 100, and 300 days (from left to right), maps of ﹩{\mathrm{log}}_{10}[{R}_{\mathrm{WD}}/{R}_{1}]﹩, ﹩{ \mathcal O }\times 100﹩, and ΔA m × 100 over the 2D space ﹩{M}_{\mathrm{WD}}({M}_{\odot })\mbox{-}{\mathrm{log}}_{10}[{M}_{\star }({M}_{\odot })]﹩ are displayed from top to bottom. The black curves show the contour lines for each map. Three animations from the maps of ﹩{\mathrm{log}}_{10}[{R}_{\mathrm{WD}}/{R}_{1}]﹩ (https://iutbox.iut.ac.ir/index.php/s/gmxLytwMJWN84ni), ﹩{ \mathcal O }\times 100﹩ (https://iutbox.iut.ac.ir/index.php/s/QDJ8sfbbTdgiTKT), and ΔA m × 100 (https://iutbox.iut.ac.ir/index.php/s/tezLS7jKiHCzMiW) vs. orbital period are available.
Paper: Finite-lens Effect on Self-lensing in Detached White Dwarfs-main Sequence Binary Systems
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: The three top panels show the images formed during the self-lensing of a MS star by its WD companion at three different times. Three bottom panels represent their corresponding residual maps between the projected brightnesses of the images and the source star itself. The white, black, and red (dashed) circles display the edges of the source star, the lens object, and the Einstein radius. The axes are normalized to the source radius projected on the lens plane R ⋆,p. Two animations from the image maps (https://iutbox.iut.ac.ir/index.php/s/mgoqo9YikR2W2se) and residual maps (https://iutbox.iut.ac.ir/index.php/s/BQ2CC3LfqBbgSpL) while the MS star is passing behind the compact object vs. time are available.
Paper: Finite-lens Effect on Self-lensing in Detached White Dwarfs-main Sequence Binary Systems
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: These two plots represent R WD/R E (left panel) and ρ ⋆ (right panel) vs. orbital period T (in days) for different detached binary systems including WDs and MS stars. Here, for detached binary systems three different values for the WDs’ mass, M WD(M ☉) = 0.2, 0.6, and 1.3 (different line styles), and seven types of MS stars with different masses (different colored curves) are considered. The horizontal dark red line in the left panel shows R WD = R E.
Paper: Finite-lens Effect on Self-lensing in Detached White Dwarfs-main Sequence Binary Systems
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Examples of stellar light curves due to WDMS binary systems while the source stars are passing behind the compact objects. In these panels, self-lensing curves, obscuration curves due to finite-lens effects, and the overall light curves due to both self-lensing and finite-lens effects are shown by green dashed, red dotted–dashed, and black solid curves, respectively. The relevant parameters are given at the top of panels. The first panel shows the light curve due to the WDMS binary system whose lensing-induced images are represented in Figure 1.
Paper: Finite-lens Effect on Self-lensing in Detached White Dwarfs-main Sequence Binary Systems
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: The average mass of WDs in WDMS binary systems for which ﹩{R}_{\mathrm{WD}}=\sqrt{2}\,{R}_{{\rm{E}}}﹩ (where the self-lensing and occultation effects cancel each other out) vs. orbital period is plotted with a green dashed curve. The low limit on the WDs’ mass specified is based on real observations (i.e., 0.17M ⊙; see, e.g., M. Kilic et al. 2007; L. M. Calcaferro et al. 2018; W. R. Brown et al. 2020) and is represented with a red dotted–dashed line.
Paper: Finite-lens Effect on Self-lensing in Detached White Dwarfs-main Sequence Binary Systems
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: Top panels: maps of the overestimation of the maximum deviation in the normalized source flux while self-lensing (ΔA m) owing to using Equation (7) as compared to their real values extracted by the IRS method. Bottom panels: maps of the width of the self-lensing/occultation light curves (given by Equation (8)) from different edge-on WDMS binary systems by considering three values for the orbital period. An animation (https://iutbox.iut.ac.ir/index.php/s/bb2fy7NEjwGEk2k) from the maps of light-curve width vs. orbital period is available.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Left: comparison of normalized unfolded lines (solid black) and normalized counts lines (dotted red) at different wavelengths. Each line had a width of σ  L  = 0.05 Å, while the detector response width was σ = 0.01 Å. Right: comparison of normalized unfolded line (solid) and normalized counts lines (dotted) for different detector response widths. The response widths used correspond to Chandra’s HEG (black, yellow) and MEG (red, cyan). Both cases used the same line width of σ  L  = 0.02 Å.
Paper: Finite-lens Effect on Self-lensing in Detached White Dwarfs-main Sequence Binary Systems
Authors: Sedighe Sajadian, Hossein Fatheddin
Figure caption: The ranges and the average of possible widths (specified on the left vertical axis) due to different self-lensing/occultation signals from different WDMS binary systems are shown with dotted–dashed and dashed black curves vs. the orbital period, respectively. We assume at least five data points should cover signals so that they can be realized. In that case, the worst cadence vs. the orbital period for realizing these self-lensing/occultation signals is ﹩{\mathrm{Cadence}}_{\max }(\mathrm{minute})=\mathrm{Maximum}\times 12﹩ and is plotted with a magenta solid line as specified on the right vertical axis.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Examples of unfolding local spectral features, e.g., emission lines, across sharp response features. The left column is the observed count rates of a Gaussian line profile, while the right column is the unfolded version. The three lines have the same flux. There is a discontinuity in the effective area at 10 Å.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Error in the unfolding of a power-law continuum observed with a Gaussian response with constant effective area. The power-law index is varied in the left panel while σ = 2 is held constant. The right panel shows σ varies while γ = 2 is held constant.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Example of how unfolding can remove response features. Both panels use a γ = 1 power-law source model. The left panel uses σ = 0.01 Å, while the right uses σ = 0.1 Å. There is a discontinuity in the effective area at 10 Å, seen in the count spectrum (blue), but effectively removed from the unfolded spectrum (orange).
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Left: comparison of normalized unfolded lines (solid black) and normalized counts lines (dotted red) at different wavelengths. Each line had a width of σ  L  = 0.05 Å. Right: comparison of normalized unfolded lines (solid) and normalized count lines (dotted) for different line widths.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Error in the unfolding of a power-law continuum observed with a CCD detector and constant area.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: This combination of 18 XMM/RGS1 observations, nearly 1 Ms exposure of ζ Puppis demonstrates how dropouts in the count spectrum—the prominent dips in the upper panel—which are due to sharp features in the effective area function, are corrected by unfolding (bottom). Statistical error bars are plotted in gray but are hard to see, except in the regions of very low counts. The bottom panel is thus an accurate representation of the intrinsic source spectrum. The errors are not magnified by unfolding but are simply rescaled and have the same fractional uncertainty as in the upper counts spectrum.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Chandra MEG observation of 3C 273 showing of how unfolding can remove features in spectra caused by the detector. The left panel is the counts spectra, while the right panel is the unfolded version. In both panels, the black histogram is the spectrum binned by a constant factor of 10, and the scaled ARF values are in red.
Paper: Unfolding X-Ray Spectral Data: Conditions and Applications
Authors: Sean J. Gunderson, David P. Huenemoerder
Figure caption: Count rate (top) and unfolded (bottom) spectra of π Aqr from Chandra's HETG (black) and NuSTAR (blue). The HETG spectrum is the HEG + MEG plotted on the MEG grid and binned by a constant factor of 10. The NuSTAR spectrum is telescopes A + B plotted on A’s grid and binned by a constant factor of 3.
Paper: The Search for the In-betweeners: How Packed Are TESS Planetary Systems?
Authors: Jonathan Horner, Robert A. Wittenmyer, Stephen R. Kane, Timothy R. Holt
Figure caption: Schematic view of the seven planetary systems studied in this work. In the upper panel, the location on the x-axis shows the orbital semimajor axis of the planets in question, on a linear scale, with the horizontal lines reaching out from the planet showing the range of its orbit from pericenter to apocenter. The size of the marker for each planet gives the observed radius, as presented in the discovery work, while the color of the marker gives the measured mass for the planet. In the case of the planets orbiting HD 63433, no measured mass has been obtained to date, and we therefore plot an estimated mass for the two planets in that system, based on Figure 3 of J. Chen & D. Kipping (2017). In the case of TOI 1670 b, the mass given is an upper limit. The lower panel presents most of the same information (mass, radius, etc.), but shows the separation of the planetary systems in terms of their orbital periods, with the period of the inner planet in each system set to unity. The parent stars are shown sized relative to one another, but not to scale with their planets, and their color in the plot denotes their effective temperatures, T eff.