adsabs/AstroCLIMB huggingface dataset:
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: Pictured above is our color–color diagram of (Pan − STARRS1 r  − MDWHα ) vs. (Pan − STARRS1 r  − Pan − STARRS1 i ). We observe a stellar locus in the plane, with an extended feature to the right that roughly aligns with the synthetic giant sequence (solid blue line) provided by the IGAPS survey. The solid and dotted red lines are also synthetic sequences used and provided by IGAPS, which assists us in visualizing our calibration; we calibrate to the IGAPS stellar locus, which sits between the solid blue/red and dotted red lines (Figure 8 in M. Monguió et al. 2020).
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: A mosaic of the full DR0 region, with areas of interest labeled and/or zoomed in (see Figure 1 for the coordinate range). The Orion Complex occupies the center area, which includes Barnard’s Loop and the Orion Nebula. In the left portion, we see the Rosette Nebula and the Christmas Tree Cluster (NGC 2264) along the Galactic plane. The Eridanus Loop is also partially present. Contrast stretching has been applied to the mosaic to highlight the diffuse Hα emission, though the magnified images of the Orion Nebula (MDW field 2253) and NGC 2264 (MDW field 0368) have been specially adjusted and do not follow the color bar.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: Examples of spiral arms. (a) Two flocculent galaxies: SDSS J122051.70+610237.3 and SDSS J224158.02-004711.5. (b) Two multiple-arm galaxies: SDSS J151320.27+063704.9 and SDSS J113223.25+545858.7. (c) Two grand-design galaxies: SDSS J102126.42+381747.3 and SDSS J092651.03+233037.9.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: A comparison between directly coadding images (left) and mosaicking after performing background corrections, as discussed in Section 4.3 (right). On the left, we see prominent overlaps due to the difference in background levels between fields. Once we correct for the varying background, the output mosaic is more uniform.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: The blueprint of the MDW Survey’s 130GTX refractor with modifications included.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: Pictured is our refractor setup for the northern half of the MDW Survey of our two AstroPhysics 130GTX refractors with Paramount MX+ mounts. Note that we use a Paramount L-350 mount in the southern half of our survey, carried out at ObsTech Observatario El Sauce.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: An FLI ProLine CCD used in the MDW Survey, with a 3 nm Astrodon Hα filter installed directly in front of it.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: Velocity distributions of stars in spatial bins. We show here local four panels as an example; all panels for our total sample are shown in Figure A1. The x and y spatial ranges in kiloparsec covered by each panel are denoted at the top and left of the figure. The contour represents wavelet transformation coefficients, and the colored dots represent selected member stars of each moving group. The concentric ellipses show the velocity range used to select the background sample for each moving group. The color used for each moving group is listed in Table 1, column (7).
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: The metallicity distribution in the (V  R , V  ϕ ) coordinate. The x and y spatial ranges in kiloparsec covered by each panel are denoted at the top and left. The color bar on the right indicates the color corresponding to [Fe/H] values for all panels. The ellipses approximately represent the velocity range covered by each moving group. The colors used for ellipses are listed in Table 1, column (7).
Paper: BSN: The First Photometric Study of 10 Contact Binary Systems from the Northern and Southern Hemispheres
Authors: Atila Poro, Kai Li, Raul Michel, Angel Castro, Eduardo Fernández Lajús, Li-Heng Wang, Jean-François Coliac, Yasemin Aladağ, Ailar Alizadehsabegh, Fahri Alicavus
Figure caption: Sum of the squared residuals as a function of the mass ratio. The zoomed part is shown with an arrow.
Paper: BSN: The First Photometric Study of 10 Contact Binary Systems from the Northern and Southern Hemispheres
Authors: Atila Poro, Kai Li, Raul Michel, Angel Castro, Eduardo Fernández Lajús, Li-Heng Wang, Jean-François Coliac, Yasemin Aladağ, Ailar Alizadehsabegh, Fahri Alicavus
Figure caption: The O − C diagrams of the target binary systems.
Paper: BSN: The First Photometric Study of 10 Contact Binary Systems from the Northern and Southern Hemispheres
Authors: Atila Poro, Kai Li, Raul Michel, Angel Castro, Eduardo Fernández Lajús, Li-Heng Wang, Jean-François Coliac, Yasemin Aladağ, Ailar Alizadehsabegh, Fahri Alicavus
Figure caption: The position of the target systems in different diagrams of the parameter relationships.
Paper: BSN: The First Photometric Study of 10 Contact Binary Systems from the Northern and Southern Hemispheres
Authors: Atila Poro, Kai Li, Raul Michel, Angel Castro, Eduardo Fernández Lajús, Li-Heng Wang, Jean-François Coliac, Yasemin Aladağ, Ailar Alizadehsabegh, Fahri Alicavus
Figure caption: The black dots show the observed light curves of the systems, and the synthetic light curves were generated using the light-curve solutions. From top to bottom, the filters are B, V, R  c , I  c , and TESS, as shown by the colors. The B, V, R  c , and I  c  photometry is available as the data behind the figure for all 10 systems.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: BSN: The First Photometric Study of 10 Contact Binary Systems from the Northern and Southern Hemispheres
Authors: Atila Poro, Kai Li, Raul Michel, Angel Castro, Eduardo Fernández Lajús, Li-Heng Wang, Jean-François Coliac, Yasemin Aladağ, Ailar Alizadehsabegh, Fahri Alicavus
Figure caption: Comparing mass ratio results utilizing spectroscopic (q sp) and photometric (q ph) data for available samples.
Paper: BSN: The First Photometric Study of 10 Contact Binary Systems from the Northern and Southern Hemispheres
Authors: Atila Poro, Kai Li, Raul Michel, Angel Castro, Eduardo Fernández Lajús, Li-Heng Wang, Jean-François Coliac, Yasemin Aladağ, Ailar Alizadehsabegh, Fahri Alicavus
Figure caption: A photometric light curve of V0801 And and first to third derivatives (top to bottom panels, respectively) as an example1 of a process for systems. The units of the panels on the vertical axis from top to bottom are W m−2, 10 W m−2 day−1, 102 W m−2 day−2, and 104 W m−2 day−3, respectively.
Paper: BSN: The First Photometric Study of 10 Contact Binary Systems from the Northern and Southern Hemispheres
Authors: Atila Poro, Kai Li, Raul Michel, Angel Castro, Eduardo Fernández Lajús, Li-Heng Wang, Jean-François Coliac, Yasemin Aladağ, Ailar Alizadehsabegh, Fahri Alicavus
Figure caption: 3D view of stars in the binary systems. The color represents the effective temperature variations on the star’s surface.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: Metallicity comparison with the background sample. The title of each panel shows the name of the moving group. The dots with error bars represent mean values with uncertainties of Δ[Fe/H] of different y positions at a given x position. The error bars are obtained through the jackknife analysis. Δ[Fe/H] is defined as the median [Fe/H] of member stars minus the median [Fe/H] of the corresponding background star sample within an (x, y) spatial bin.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: Velocity distributions of stars in spatial bins for the total sample. These subplots are similar to those in Figure 1 but for all spatial bins.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: Comparison of velocity distributions of moving groups, open clusters, and young associations. Ellipses are moving groups. The colors used for ellipses are listed in Table 1, column (7). Red circles are open clusters, while stars are young associations. The x and y spatial ranges in kiloparsec covered by each panel are denoted at the top and left.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: The same as Figure 2 but for age. The color bar at the top of each panel indicates the color corresponding to the age values.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: The same as Figure 5 but for α abundance.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: The same as Figure 5 but for age.
Paper: Moving Groups in the Solar Neighborhood with Gaia, APOGEE, GALAH, and LAMOST: Dynamical Effects Gather Gas and the Ensuing Star Formation Plays an Important Role in Shaping the Stellar Velocity Distributions
Authors: Xilong Liang, Suk-Jin Yoon, Jingkun Zhao
Figure caption: The same as Figure 2 but for α abundance. The color bar at the top of each panel indicates the color corresponding to the [α/Fe] values.
Paper: Revisiting the Relationship Between Rocky Exoplanet and Stellar Compositions: Reduced Evidence for a Super-Mercury Population
Authors: Casey L. Brinkman, Alex S. Polanski, Daniel Huber, Lauren M. Weiss, Diana Valencia, Mykhaylo Plotnykov
Figure caption: Core mass fraction (CMF) of rocky exoplanets vs. equivalent CMF (see Section 4.2) for their host stars, shaded by planet radius. The CMFs for five solar system bodies are shown at the equivalent CMF of the Sun (from top to bottom: Mercury, Earth, Venus, Mars, and the Moon). The dotted black line shows the one-to-one correspondence of CMFs in stars and planets, which is where planets would fall if they inherited the exact Fe/Mg ratio from their host star. Our linear best-fit models are shown in indigo (ordinary least squares, OLS) and green (orthogonal distance regression, ODR) with 1σ confidence intervals on each.
Paper: Revisiting the Relationship Between Rocky Exoplanet and Stellar Compositions: Reduced Evidence for a Super-Mercury Population
Authors: Casey L. Brinkman, Alex S. Polanski, Daniel Huber, Lauren M. Weiss, Diana Valencia, Mykhaylo Plotnykov
Figure caption: Left: planet CMF and stellar-equivalent “CMF” for 22 planets (21 host stars) as published in V. Adibekyan et al. (2021, A21). Center: same as left, but using SuperEarth to calculate host-star and planet CMF with planet mass and radius values (along with host-star abundances) from A21. Right: our KeckSpec sample of 20 planets using planet mass and radius, along with stellar abundances, presented in this work and using SuperEarth to calculate host-star and planet CMF. The pink line in each plot is the best-fit slope and 1σ uncertainties from A21, and the green dotted line is the one-to-one line where stars and planets have the same composition.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Panel (a): posterior distribution of sky-projected spin–orbit angle for HD 118203 b, obtained from RM effect modeling with stellar oscillations. Panel (b): posterior distribution of stellar inclination (in orange) vs. an isotropic distribution. The stellar inclination ranges from 0°–180° to account for scenarios where the stellar axis may point either toward (<90°) or away (>90°) from the observer. The red dashed lines correspond to 1σ significance. Panel (c): posterior distribution of cosine of true spin–orbit angle for HD 118203 b. Panel (d): true spin–orbit angle distribution for HD 118203 b. The blue dashed lines correspond to 2σ significance.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Panel (a): TESS SPOC light curves phase-folded to the best-fit orbital period of HD 118203 b. The pink points present the TESS data binned every 15 minutes, and the red line shows the best-fit transit model. Panel (b): the out-of-transit RVs from ELODIE (green) and HIRES (orange) phase-folded to the best-fit orbital period of HD 118203 b. The red line depicts the best-fit RV model. The linear baseline has been removed. Panel (c): the in-transit RVs from KPF in blue and the combined RM and GP model in red. Panel (d): KPF data and RM model after removing the contribution from oscillations. Panel (e): KPF data and SHO GP model after removing RM effect. Panel (f): the residuals of the fit.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Lomb–Scargle periodograms of the KPF RV residuals from RM fitting without oscillation. The solid gray and orange lines represent the original and smoothed periodograms (filter width = 340 μHz). The blue dashed line indicates the predicted frequency at maximum power, ﹩{\nu }_{\max }﹩, derived using scaling relations ﹩\tfrac{g}{{g}_{\odot }}=\tfrac{{\nu }_{\max }}{{\nu }_{\odot }}\tfrac{{T}_{\mathrm{eff}}}{{T}_{\mathrm{eff},\odot }}﹩. The values for the star’s surface gravity g and effective temperature T eff were taken from J. Pepper et al. (2020).
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Panels (a)–(d): TESS light curves of HD 118203 obtained in Sectors 15, 16, 22, 49, and 76 with the modulation model at a period of 23.091 days. Panel (e): the Lomb–Scargle periodogram of the detrended TESS light curves of HD 118203 using SIP (C. Hedges et al. 2020). The highest peak in the periodogram is located at 23.091 days. The red dashed line shows the Gaussian fit to the peak to determine the uncertainty of rotation period.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Top panel: mass vs. semimajor axis of detected companions to hot Jupiters. Red circles are stellar companions from H. Ngo et al. (2016), and orange circles are giant planet companions from H. A. Knutson et al. (2014), M. L. Bryan et al. (2016), and L. J. Rosenthal et al. (2021). The orange line represents the limit for a companion to overcoming GR precession at a close-in orbit of 6.13 days. The blue lines represent the limit for a companion overcoming GR precession at 0.3 au, 1 au, and 4 au, respectively. Bottom panel: eccentricity vs. semimajor axis of confirmed planets with mass larger than 0.8M J within 1 au, based on data from the NASA Exoplanet Archive as of 2024 June. The orange region indicates the trajectory associated with high-eccentricity tidal migration, where tidal dissipation within the planet reduces its orbital energy while keeping constant angular momentum. The final semimajor axis range is set between 0.02 and 0.1 au, representing the upper and lower limits.
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Panel (a): sketch showing the orbital geometry for the mutual inclination between HD 118203 b&c. The observer is looking down from the z-axis. The x–y plane is the plane of the sky, and the star is centered on the origin. The orbital inclination of a planet is defined as the angle between the planet orbital axis and line-of-sight direction (z-axis). The mutual inclination is the angle between the orbital axes of the two planets. Panel (b): for a transiting planet with orbital inclination I 1 = 90° without knowing the longitude of acceding node, its orbital axis could fall anywhere along the sky plane (orange). For a planet with an orbital inclination I 2 ≠ 90° without knowing the longitude of acceding node, its orbital axis falls on the surface of a cone (blue) with a vertex angle equals to the orbital inclination (toward observer, I 2 < 90°) or π-orbital inclination (away from observer, I 2 > 90°).
Paper: A Testbed for Tidal Migration: The 3D Architecture of an Eccentric Hot Jupiter HD 118203 b Accompanied by a Possibly Aligned Outer Giant Planet
Authors: Jingwen Zhang, 婧雯 张, Daniel Huber, Lauren M. Weiss, Jerry W. Xuan, Jennifer A. Burt, Fei Dai, Nicholas Saunders, Erik A. Petigura, Ryan A. Rubenzahl, Joshua N. Winn, Sharon X. Wang, Judah Van Zandt, Max Brodheim, Zachary R. Claytor, Ian Crossfield, William Deich, Benjamin J. Fulton, Steven R. Gibson, Samuel Halverson, Grant M. Hill, Bradford Holden, Aaron Householder, Andrew W. Howard, Howard Isaacson, Stephen Kaye, Kyle Lanclos, Russ R. Laher, 嶺亞 良主, Jack Lubin, Joel Payne, Arpita Roy, Christian Schwab, Abby P. Shaum, Josh Walawender, Edward Wishnow, Sherry Yeh
Figure caption: Panel (a): orbital inclination of HD 118203 c (I  c , blue), compared with that of HD 118203 b (I  b , red) and the line-of-sight stellar inclination (i *, orange). Zero degrees corresponds to the line of sight. The stellar inclination ranges from 0°–180° to account for scenarios where the stellar axis may point either toward (<90°) or away (>90°) from the observer. Panel (b): distribution of HD 118203 b and c mutual inclination projected in line-of-sight direction. Panel (c): distribution of spin–orbit angle of HD 118203 c projected in line-of-sight direction.