adsabs/AstroCLIMB huggingface dataset:
Paper: Origins of Hot Jupiters from the Stellar Obliquity Distribution
Authors: Malena Rice, Songhu Wang, and Gregory Laughlin
Figure caption: Damping evolution for a sample primordial ∣λ∣ distribution. The initial obliquity model is comprised of 20% stellar Kozai–Lidov systems, 40% planet Kozai–Lidov systems, 10% secular chaos systems, and 30% planet–planet scattering systems. Planets are initialized with the same distribution of semimajor axis, planet mass, age, and stellar Teff as the current set of cool stars with e = 0 planets and measured λ.
Paper: Origins of Hot Jupiters from the Stellar Obliquity Distribution
Authors: Malena Rice, Songhu Wang, and Gregory Laughlin
Figure caption: Cumulative sums as a function of orbital period P (top) and orbital separation a/R* (bottom), for comparison with the eccentricity cumulative sum in Figure 1.
Paper: Turbulence in the Sub-Alfvénic Solar Wind
Authors: G. P. Zank, L.-L. Zhao, L. Adhikri, D. Telloni, J. C. Kasper, M. Stevens, A. Rahmati, and S. D. Bale
Figure caption: Overview of the first sub-Alfvénic interval, located between the dashed vertical lines, and the adjacent super-Alfvénic intervals observed by PSP during encounter 8, showing (top to bottom) the radial BR, transverse BT, and normal BN magnetic fields and intensity ∣B∣; the angle θBU between the relative flow velocity U0 (i.e., the relative velocity between the solar wind flow and the spacecraft velocity vectors) and magnetic field vectors; the proton np (black) and electron number density ne (red); the radial component of the plasma speed VR measured in the inertial RTN frame; the Alfvénic Mach number of the radial flow MA = VR/VA; and the plasma beta βp. The bottom three colored panels, in descending order, show frequency spectrograms of the normalized magnetic helicity σm, normalized cross-helicity σc, and normalized residual energy σr.
Paper: Turbulence in the Sub-Alfvénic Solar Wind
Authors: G. P. Zank, L.-L. Zhao, L. Adhikri, D. Telloni, J. C. Kasper, M. Stevens, A. Rahmati, and S. D. Bale
Figure caption: Trace spectra of the Elsässer variables z± calculated in 5 hr intervals for the sub-Alfvénic region (left panel) and a neighboring super-Alfvénic region (right panel). The sub-Alfvénic region is delineated by the two vertical dashed lines shown in Figure 1. The 5 hr interval just after the sub-Alfvénic region is selected as representative of the super-Alfvénic region. The solid green and cyan lines are predicted theoretical spectra, the dashed f−1 curve is to guide the eye, and ft identifies the transition frequency (see text for details). The dashed–dotted vertical line separates the f−1 and the f−1.5 sections of the z+ spectra.
Paper: Turbulence in the Sub-Alfvénic Solar Wind
Authors: G. P. Zank, L.-L. Zhao, L. Adhikri, D. Telloni, J. C. Kasper, M. Stevens, A. Rahmati, and S. D. Bale
Figure caption: The PSDs for the fluctuating density variance in the sub- and super-Alfvénic regions corresponding to those used for Figure 2. The LFR electron density from FIELDS has been used. The fitted frequency range for both intervals ranges from 5 × 10−4 to 1 × 10−2 Hz.
Paper: Turbulence in the Sub-Alfvénic Solar Wind
Authors: G. P. Zank, L.-L. Zhao, L. Adhikri, D. Telloni, J. C. Kasper, M. Stevens, A. Rahmati, and S. D. Bale
Figure caption: The PSDs for magnetic fluctuations in the parallel (blue) and transverse (orange) directions for the sub-Alfvénic (left panel) and super-Alfvénic (right) regions. The total trace spectrum (green) effectively overlays the transverse fluctuations. Pink and blue lines are fitted to the data over the frequency range 2 × 10−3–0.2 Hz to estimate the spectral indices of the incompressible and compressible magnetic field PSDs.
Paper: AGC 226178 and NGVS 3543: Two Deceptive Dwarfs toward Virgo
Authors: Michael G. Jones, David J. Sand, Michele Bellazzini, Kristine Spekkens, John M. Cannon, Burçin Mutlu-Pakdil, Ananthan Karunakaran, Giacomo Beccari, Laura Magrini, Giovanni Cresci, John L. Inoue, Jackson Fuson, Elizabeth A. K. Adams, Giuseppina Battaglia, Paul Bennet, Denija Crnojević, Nelson Caldwell, Puragra Guhathakurta, Martha P. Haynes, Ricardo R. Muñoz, Anil Seth, Jay Strader, Elisa Toloba, and Dennis Zaritsky
Figure caption: Left: false-color F606W+F814W image of the AGC 226178 and NGVS 3543 system. The cyan dashed–dotted ellipse encircles NGVS 3543 out to the half-light radius (Junais et al. 2021, their Table 2), and the green dashed ellipse and circles show AGC 226178. Top middle: CMD of NGVS 3543 constructed from the stars within two half-light radii (i.e., four times the area of the cyan dashed–dotted ellipse). The dashed line indicates the 90% completeness limit, and the dotted line is the 50% limit. The error bars along the edge indicate typical uncertainties in the photometry as a function of F814W magnitude. Top right: CMD of a blank sky region of equal area on the opposite side of the ACS field of view. Bottom middle: CMD of AGC 226178 constructed from the stars within the green dashed ellipse and circles. The error bars along the edge indicate typical uncertainties in the photometry. No background CMD is included; however, the area of AGC 226178 is ∼30% of NGVS 3543, and only ∼seven points in the CMD are expected to be background. Bottom right: repeated CMD of AGC 226178 with stellar population isochrones overlaid for a variety of different ages (assuming the distance to Virgo). Note that the completeness limits in the lower and upper CMDs are the same but appear different due to the different ranges of F814W magnitudes plotted.
Paper: AGC 226178 and NGVS 3543: Two Deceptive Dwarfs toward Virgo
Authors: Michael G. Jones, David J. Sand, Michele Bellazzini, Kristine Spekkens, John M. Cannon, Burçin Mutlu-Pakdil, Ananthan Karunakaran, Giacomo Beccari, Laura Magrini, Giovanni Cresci, John L. Inoue, Jackson Fuson, Elizabeth A. K. Adams, Giuseppina Battaglia, Paul Bennet, Denija Crnojević, Nelson Caldwell, Puragra Guhathakurta, Martha P. Haynes, Ricardo R. Muñoz, Anil Seth, Jay Strader, Elisa Toloba, and Dennis Zaritsky
Figure caption: Top left: contours of integrated H I emission (moment zero map) from the VLA observations of AGC 226178 overlaid on a DECaLS g-band image. The contour levels are −3σ, 3σ, 6σ, 12σ, 24σ, and 48σ, where 3σ corresponds to 1.6 × 1019 cm−2 or, equivalently, 0.13 M⊙ pc−2 (both over 20 km s−1). The beam is shown by the black ellipse in the bottom left corner (56″ × 45″). Top right: GALEX NUV+FUV composite image showing a smaller field of view containing AGC 226178 and NGVS 3543. The red contours show Hα emission mapped by MUSE (contour levels are 5, 15, 45, and 135 × 10−20 erg s−1 cm−2). Object AGC 226178 is detected strongly in both GALEX bands and Hα; NGVS 3543 is ∼1′ to the north and only weakly detected in GALEX. Bottom left: VLA H I contours overlaid on a DECaLS r-band image showing a wide field, including several nearby galaxies that AGC 226178 may have interacted with (contours at the same levels as in the top left panel). The thin black square shows the field of view of the top left panel. Galaxies with H I detections are labeled in blue, those without H I are in red, and those with no redshift measurement are in black. Bottom right: ALFALFA H I integrated emission contours overlaid on the same optical image. The thin black square shows the field of view of the top right panel. The significance of the contour levels is the same, but in this case, 3σ corresponds to 2.8 × 1018 cm−2 or, equivalently, 0.02 M⊙ pc−2 (both over 20 km s−1). The beam is shown by the black ellipse in the bottom left corner (3.′8 × 3.′5). In this case, the H I emission of VCC 2037 has been excluded to avoid confusion.
Paper: AGC 226178 and NGVS 3543: Two Deceptive Dwarfs toward Virgo
Authors: Michael G. Jones, David J. Sand, Michele Bellazzini, Kristine Spekkens, John M. Cannon, Burçin Mutlu-Pakdil, Ananthan Karunakaran, Giacomo Beccari, Laura Magrini, Giovanni Cresci, John L. Inoue, Jackson Fuson, Elizabeth A. K. Adams, Giuseppina Battaglia, Paul Bennet, Denija Crnojević, Nelson Caldwell, Puragra Guhathakurta, Martha P. Haynes, Ricardo R. Muñoz, Anil Seth, Jay Strader, Elisa Toloba, and Dennis Zaritsky
Figure caption: Left: DECaLS grz image showing a linear position–velocity slice (cyan dashed line) that intersects with AGC 226178 and VCC 2034. Here AGC 226178 is not visible on this scale, but its location is marked with an arrow. Middle: position–velocity slice from the ALFALFA data cube along the line in the left panel. A region 3.8′ wide (centered on the line) was collapsed to form this slice, as this corresponds to the resolution of the ALFALFA data. The contours are drawn at 2.4, 4.8, and 7.2 mJy beam–1, approximately 1σ (red), 2σ (orange), and 3σ (yellow), respectively. Object AGC 226178 is the bright clump at upper left (∼1580 km s−1), and VCC 2034 is at lower right (∼1500 km s−1). Object VCC 2037 does not appear in the slice, as it is well below the velocity range plotted. Right: same position–velocity slice but from the VLA tapered data cube. A width of 1.′8 is used for the slice in this case, again roughly corresponding to the resolution of the data. For clarity, the same contour levels are used as in the middle panel; however, in this case, they correspond to approximately 1.1σ and 2.2σ.
Paper: AGC 226178 and NGVS 3543: Two Deceptive Dwarfs toward Virgo
Authors: Michael G. Jones, David J. Sand, Michele Bellazzini, Kristine Spekkens, John M. Cannon, Burçin Mutlu-Pakdil, Ananthan Karunakaran, Giacomo Beccari, Laura Magrini, Giovanni Cresci, John L. Inoue, Jackson Fuson, Elizabeth A. K. Adams, Giuseppina Battaglia, Paul Bennet, Denija Crnojević, Nelson Caldwell, Puragra Guhathakurta, Martha P. Haynes, Ricardo R. Muñoz, Anil Seth, Jay Strader, Elisa Toloba, and Dennis Zaritsky
Figure caption: Observed luminosity function of stars in the NGVS 3543 CMD (Figure 1, top middle). The red dashed line indicates where the TRGB would occur (Jang & Lee 2017) for an RGB population with F606W − F814W = 1 and a fiducial distance of 10 Mpc, and the purple dashed–dotted line corresponds to if NGVS 3543 were at 16.5 Mpc (in Virgo), rather than 10 Mpc. The gray dashed line indicates the 90% completeness limit (at F606W − F814W = 1), and the gray dotted line is the 50% limit.
Paper: A New Magnetic Parameter of Active Regions Distinguishing Large Eruptive and Confined Solar Flares
Authors: Ting Li, Xudong Sun, Yijun Hou, Anqin Chen, Shuhong Yang, and Jun Zhang
Figure caption: Four examples of two eruptive and two confined flares showing SDO/AIA 1600 Å images (left), SDO/HMI photospheric magnetograms Bz (middle), and derived vertical electric current density Jz maps (right). From top to bottom: eruptive X2.1-class flare in AR 11283, eruptive M6.5-class flare in AR 12371, confined X3.1-class flare in AR 12192, and confined M6.1-class flare in AR 12222. AIA 1600 Å images were remapped with CEA projection. Orange and black contours outline the FPIL mask regions within which the mean characteristic twist parameter (αFPIL) in Figure 2 was calculated.
Paper: A New Magnetic Parameter of Active Regions Distinguishing Large Eruptive and Confined Solar Flares
Authors: Ting Li, Xudong Sun, Yijun Hou, Anqin Chen, Shuhong Yang, and Jun Zhang
Figure caption: Scatterplots of mean characteristic twist parameter αFPIL vs. total unsigned magnetic flux ΦAR and flare peak X-ray flux FSXR vs. αFPIL/ΦAR. Blue (red) circles are eruptive (confined) flares. Two vertical green lines in panel (a) correspond to ΦAR of 3.5 × 1022 Mx and 1.0 × 1023 Mx, respectively. The horizontal black line in panel (a) refers to αFPIL of 0.07 Mm−1. The vertical black line in panel (b) denotes αFPIL/ΦAR of 2.2 × 10−24 Mm−1 Mx−1.
Paper: A New Magnetic Parameter of Active Regions Distinguishing Large Eruptive and Confined Solar Flares
Authors: Ting Li, Xudong Sun, Yijun Hou, Anqin Chen, Shuhong Yang, and Jun Zhang
Figure caption: Maps of photospheric free magnetic energy density ρfree and magnetic shear angle Ψ of four examples (from top to bottom: eruptive X2.1-class flare in AR 11283, eruptive M6.5-class flare in AR 12371, confined X3.1-class flare in AR 12192, and confined M6.1-class flare in AR 12222). The white and green contours are the magnetic fields Bz at ± 800 G levels. Mean characteristic twist parameter αHFED and mean shear angle ΨHFED in Figure 4 are calculated within the areas of ρfree > 4.0 × 104 erg cm−3.
Paper: A New Magnetic Parameter of Active Regions Distinguishing Large Eruptive and Confined Solar Flares
Authors: Ting Li, Xudong Sun, Yijun Hou, Anqin Chen, Shuhong Yang, and Jun Zhang
Figure caption: Similar to Figure 2, but for mean characteristic twist parameter αHFED and mean shear angle ΨHFED within the HFED region. Blue (red) circles are eruptive (confined) flares. The horizontal dotted line in panel (a) corresponds to αHFED of 0.1 Mm−1. The vertical dashed–dotted line in panel (b) refers to αHFED/ΦAR of 3.2 × 10−24 Mm−1 Mx−1. The horizontal dotted line in panel (c) denotes ΨHFED of 60°. The vertical dashed–dotted line in panel (d) corresponds to ΨHFED/ΦAR of 1.°0 × 10−21 Mx−1.
Paper: Different Formation Scenarios for Counterrotating Stellar Disks in Nearby Galaxies
Authors: Min Bao, Yanmei Chen, Pengpei Zhu, Yong Shi, Dmitry Bizyaev, Ling Zhu, Meng Yang, Minje Beom, Joel R. Brownstein, and Richard R. Lane
Figure caption: (a) Specific star formation rate as a function of stellar mass. The black and gray dotted lines separate galaxies into BC (blue), RS (red), and GV in between them (green). (b), (c), (d), (e) The difference in kinematic position angles between the stellar and gas components along the radius (black dashed lines), as well as the stellar and gas velocity fields for Types 1a, 1b, 2a, and 2b CRDs. The black and gray solid lines mark the stellar and gas kinematic major axes. The stellar velocity dispersion fields for Types 2a and 2b are also displayed in panels (d) and (e). The black contours indicate the σ peaks along the stellar major axes.
Paper: Different Formation Scenarios for Counterrotating Stellar Disks in Nearby Galaxies
Authors: Min Bao, Yanmei Chen, Pengpei Zhu, Yong Shi, Dmitry Bizyaev, Ling Zhu, Meng Yang, Minje Beom, Joel R. Brownstein, and Richard R. Lane
Figure caption: (a) The relative contributions of Types 1a and 1b. Blue, green, and red histograms represent the BC, GV, and RS galaxies. The dark-colored dashed-line histograms show the fractions of Type 1a (the gas disk corotating with the inner stellar disk). The light-colored dashed-line histograms show the fractions of Type 1b (the gas disk corotating with the outer stellar disk). (b) The relative contributions of Types 2a and 2b. Blue, green, and red histograms represent BC, GV, and RS galaxies. The dark-colored solid-line histograms show the fractions of Type 2a (star–gas corotators). The light-colored solid-line histograms show the fractions of Type 2b (star–gas counterrotators). The percentage of each type is marked on top of the histogram.
Paper: Different Formation Scenarios for Counterrotating Stellar Disks in Nearby Galaxies
Authors: Min Bao, Yanmei Chen, Pengpei Zhu, Yong Shi, Dmitry Bizyaev, Ling Zhu, Meng Yang, Minje Beom, Joel R. Brownstein, and Richard R. Lane
Figure caption: Dn4000 radial gradients in different types of CRDs. Blue, green, and red correspond to the BC, GV, and RS galaxies. (a), (b), and (c) The dark-colored squares mark the median values of Dn4000 in each radial bin of Type 1a. The light-colored squares mark the median values of Dn4000 in each radial bin of Type 1b. (d), (e), and (f) The dark-colored circles mark the median values of Dn4000 in each radial bin of Type 2a. The light-colored circles mark the median values of Dn4000 in each radial bin of Type 2b. The error bars show the 40th to 60th percentiles of the distribution.
Paper: Different Formation Scenarios for Counterrotating Stellar Disks in Nearby Galaxies
Authors: Min Bao, Yanmei Chen, Pengpei Zhu, Yong Shi, Dmitry Bizyaev, Ling Zhu, Meng Yang, Minje Beom, Joel R. Brownstein, and Richard R. Lane
Figure caption: Formation scenarios of counterrotating stellar disks in the nearby galaxies with regularly rotating ionized gas disks.
Paper: Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe: Characterization of Turbulence, Anisotropy, Intermittency, and Switchback
Authors: R. Bandyopadhyay, W. H. Matthaeus, D. J. McComas, R. Chhiber, A. V. Usmanov, J. Huang, R. Livi, D. E. Larson, J. C. Kasper, A. W. Case, M. Stevens, P. Whittlesey, O. M. Romeo, S. D. Bale, J. W. Bonnell, T. Dudok de Wit, K. Goetz, P. R. Harvey, R. J. MacDowall, D. M. Malaspina, and M. Pulupa
Figure caption: An overview of plasma parameters surrounding the sub-Alfvénic intervals observed by PSP near its eighth (left) and ninth (right) perihelion. The panels from top show Alfvén Mach number MA = VR/VA where VA is the Alfvén speed (see text), radial component of solar wind proton velocity VR, electron number density Ne, radial component and magnitude of magnetic field B, and heliocentric distance in units of solar radii. A cyan line is drawn at MA = 1 in the top panels for visual ease. The dashed red lines indicate the sub-Alfvénic periods.
Paper: Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe: Characterization of Turbulence, Anisotropy, Intermittency, and Switchback
Authors: R. Bandyopadhyay, W. H. Matthaeus, D. J. McComas, R. Chhiber, A. V. Usmanov, J. Huang, R. Livi, D. E. Larson, J. C. Kasper, A. W. Case, M. Stevens, P. Whittlesey, O. M. Romeo, S. D. Bale, J. W. Bonnell, T. Dudok de Wit, K. Goetz, P. R. Harvey, R. J. MacDowall, D. M. Malaspina, and M. Pulupa
Figure caption: Probability distribution function (PDF) of magnetic-field turbulence amplitude in the sub-Alfvénic solar wind and the neighboring super-Alfvénic solar wind intervals observed by PSP (see Figure 1 and the text in Section 3).
Paper: Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe: Characterization of Turbulence, Anisotropy, Intermittency, and Switchback
Authors: R. Bandyopadhyay, W. H. Matthaeus, D. J. McComas, R. Chhiber, A. V. Usmanov, J. Huang, R. Livi, D. E. Larson, J. C. Kasper, A. W. Case, M. Stevens, P. Whittlesey, O. M. Romeo, S. D. Bale, J. W. Bonnell, T. Dudok de Wit, K. Goetz, P. R. Harvey, R. J. MacDowall, D. M. Malaspina, and M. Pulupa
Figure caption: Distribution of variance anisotropy in sub-Alfvénic and the neighboring super-Alfvénic solar wind intervals observed by PSP near perihelion 8 and 9 (see Figure 1 and the text in Section 3). The vertical line indicates the value Ab = 2, which corresponds to isotropic distribution.
Paper: Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe: Characterization of Turbulence, Anisotropy, Intermittency, and Switchback
Authors: R. Bandyopadhyay, W. H. Matthaeus, D. J. McComas, R. Chhiber, A. V. Usmanov, J. Huang, R. Livi, D. E. Larson, J. C. Kasper, A. W. Case, M. Stevens, P. Whittlesey, O. M. Romeo, S. D. Bale, J. W. Bonnell, T. Dudok de Wit, K. Goetz, P. R. Harvey, R. J. MacDowall, D. M. Malaspina, and M. Pulupa
Figure caption: Histogram of PVI in the sub-Alfvénic and the neighboring super-Alfvénic periods near perihelia 8 and 9 (see Figure 1 and Section 3). PVI values larger than 2.5 (vertical line) represent intermittent structures.
Paper: Sub-Alfvénic Solar Wind Observed by the Parker Solar Probe: Characterization of Turbulence, Anisotropy, Intermittency, and Switchback
Authors: R. Bandyopadhyay, W. H. Matthaeus, D. J. McComas, R. Chhiber, A. V. Usmanov, J. Huang, R. Livi, D. E. Larson, J. C. Kasper, A. W. Case, M. Stevens, P. Whittlesey, O. M. Romeo, S. D. Bale, J. W. Bonnell, T. Dudok de Wit, K. Goetz, P. R. Harvey, R. J. MacDowall, D. M. Malaspina, and M. Pulupa
Figure caption: Histogram of switchback parameter (Z) in the sub-Alfvenic solar wind and the neighboring super-Alfvénic solar wind intervals observed by PSP (see Figure 1 and the text in Section 3). The vertical line indicates the value Z = 1/2, which corresponds to a polarity-reversed magnetic field. Higher Z values represent stronger switchback.
Paper: The Aligned Orbit of WASP-148b, the Only Known Hot Jupiter with a nearby Warm Jupiter Companion, from NEID and HIRES
Authors: Xian-Yu Wang, Malena Rice, Songhu Wang, Bonan Pu, Gudmundur Stefánsson, Suvrath Mahadevan, Brandon Radzom, Steven Giacalone, Zhen-Yu Wu, Thomas M. Esposito, Paul A. Dalba, Arin Avsar, Bradford Holden, Brian Skiff, Tom Polakis, Kevin Voeller, Sarah E. Logsdon, Jessica Klusmeyer, Heidi Schweiker, Dong-Hong Wu, Corey Beard, Fei Dai, Jack Lubin, Lauren M. Weiss, Chad F. Bender, Cullen H. Blake, Courtney D. Dressing, Samuel Halverson, Fred Hearty, Andrew W. Howard, Daniel Huber, Howard Isaacson, James A. G. Jackman, Joe Llama, Michael W. McElwain, Jayadev Rajagopal, Arpita Roy, Paul Robertson, Christian Schwab, Evgenya L. Shkolnik, Jason T. Wright, Gregory Laughlin
Figure caption: Upper panel: stellar sky-projected obliquities (λ) derived from R-M measurements or Doppler tomography for 112 exoplanet systems, shown as a function of the host star’s effective temperature (T eff). The isolated-hot-Jupiter systems are shown as yellow circles, while compact multi-planet systems are represented by blue diamonds. The vertical red dashed line indicates T eff = 6250  K. Lower panel: the probability distribution for the number of the misaligned systems among 12 randomly selected isolated-hot-Jupiter systems, shown for each of our three test cases. In each panel, the dashed red line represents only one misaligned system, K2-290A, among 12 compact multi-planet systems. Singles with weak tides include systems with low-mass planets, wide-separation systems, or systems around hot stars.
Paper: The Aligned Orbit of WASP-148b, the Only Known Hot Jupiter with a nearby Warm Jupiter Companion, from NEID and HIRES
Authors: Xian-Yu Wang, Malena Rice, Songhu Wang, Bonan Pu, Gudmundur Stefánsson, Suvrath Mahadevan, Brandon Radzom, Steven Giacalone, Zhen-Yu Wu, Thomas M. Esposito, Paul A. Dalba, Arin Avsar, Bradford Holden, Brian Skiff, Tom Polakis, Kevin Voeller, Sarah E. Logsdon, Jessica Klusmeyer, Heidi Schweiker, Dong-Hong Wu, Corey Beard, Fei Dai, Jack Lubin, Lauren M. Weiss, Chad F. Bender, Cullen H. Blake, Courtney D. Dressing, Samuel Halverson, Fred Hearty, Andrew W. Howard, Daniel Huber, Howard Isaacson, James A. G. Jackman, Joe Llama, Michael W. McElwain, Jayadev Rajagopal, Arpita Roy, Paul Robertson, Christian Schwab, Evgenya L. Shkolnik, Jason T. Wright, Gregory Laughlin
Figure caption: Compact multi-planet systems with observed λ constraints, ordered by stellar temperature. For each system, λ is shown, together with uncertainties, relative to the net angular momentum plane of the orbits. This plane is determined from those planets with measured spin–orbit angles in each system. A vertical upward spin axis indicates λ = 0°. The planets with spin–orbit angle constraints are shown in black, while all other planets are shown in gray. The planetary masses in the TOI-942 and V1298 Tau systems were estimated based on their photometric radii using the Chen & Kipping (2017) mass–radius relation.