adsabs/AstroCLIMB huggingface dataset:
Paper: PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). I. The Ubiquity of Fe I Emission and Inversions in Ultrahot Jupiter Atmospheres
Authors: Sydney Petz, Marshall C. Johnson, Anusha Pai Asnodkar, Alison Duck, Ji Wang, 吉 王, Ilya Ilyin, Klaus G. Strassmeier
Figure caption: Surface gravity as a function of equilibrium temperature of HJs listed in Table 4. Circle, square, and diamond symbols represent planets observed in high resolution, low resolution, and both, respectively. The orange, purple, and blue shaded regions indicate regions of parameter space proposed by T. G. Beatty et al. (2017b) to host planets with inverted or isothermal, ambiguous, and monotonically decreasing P-T profiles, respectively. Note that T. G. Beatty et al. (2017b) cast these in terms of the dayside brightness temperature TB, which is a measured quantity not equal to the theoretical quantity Teq, which we use; however, their relation has only a weak dependence on temperature so the difference should be small. The yellow and teal dashed lines show the boundary found by V. Parmentier et al. (2018) for the presence of TiO and H−, respectively; these species should be present above and to the right of these lines.
Paper: PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). I. The Ubiquity of Fe I Emission and Inversions in Ultrahot Jupiter Atmospheres
Authors: Sydney Petz, Marshall C. Johnson, Anusha Pai Asnodkar, Alison Duck, Ji Wang, 吉 王, Ilya Ilyin, Klaus G. Strassmeier
Figure caption: Top: same as Figure 6, except showing contours of P-T profile slope derived from the GCM suite of A. Roth et al. (2024a). The black dashed line shows the point at which an isothermal P-T profile is expected, while successively more blue-green (red) colors show successively more strongly decreasing (inverted) P-T profiles. The A. Roth et al. (2024a) GCM grid only covers a limited range of Teq–gP space as compared to the observed planets. The solid black lines show our best-fit boundary between inverted and noninverted regimes using a temperature only fit and a temperature and surface gravity fit with a 1σ shaded uncertainty. Bottom: expected volume mixing ratios at a pressure level of 10−2 bar (approximately the pressure level at which the inversions may occur; Figure 2) of several proposed inversion agents as a function of planetary equilibrium temperature, as calculated with FastChemCond.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Planet-to-star flux ratio as a function of orbital phase from the same model as Figure 9. At apastron the spectra show many species in absorption (colored bars) and as the planet progresses toward periastron only the CO feature remains (in emission) with water providing the bulk of the increase in flux from a blackbody due to being in emission.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Temperature as a function of pressure over orbital phase from a 1D timestepping cloud-free atmospheric model generated using EGP+. Due to the presence of TiO and VO in the model atmosphere, at periastron the temperature of the upper atmosphere rises rapidly causing an inversion.
Paper: PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). I. The Ubiquity of Fe I Emission and Inversions in Ultrahot Jupiter Atmospheres
Authors: Sydney Petz, Marshall C. Johnson, Anusha Pai Asnodkar, Alison Duck, Ji Wang, 吉 王, Ilya Ilyin, Klaus G. Strassmeier
Figure caption: Pressure–temperature profiles for TOI-1431 b and TOI-1518 b adopted in this work, shown in red and blue, respectively. The horizontal dashed lines and bands show, in the same per-planet colors, the estimated pressure of peak of the contribution function and 68% contribution range for the Fe I emission spectrum, as calculated by petitRADTRANS. We emphasize that these are estimated P-T profiles produced by a manual grid search to maximize SNR and not robust measurements of the profiles.
Paper: PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). I. The Ubiquity of Fe I Emission and Inversions in Ultrahot Jupiter Atmospheres
Authors: Sydney Petz, Marshall C. Johnson, Anusha Pai Asnodkar, Alison Duck, Ji Wang, 吉 王, Ilya Ilyin, Klaus G. Strassmeier
Figure caption: Left: Phase coverage of the observations used in this work. The solid inner circle shows the stellar surface, while the middle and outer circles show the orbits of TOI-1518 b and TOI-1431 b, respectively, to scale. The observer is off the bottom of the page, and the vertical dashed lines show the line of sight, such that transit occurs in the lower intersection of the dashed lines and planetary orbits, and the secondary eclipse in the upper intersection. The planets orbit counter-clockwise. The colored points show the portions of the orbit where we obtained data. Right: signal-to-noise ratio of our observations as a function of orbital phase. The PEPSI red and blue arms are shown as the solid and dotted lines, respectively. The SNR values shown are, for each spectrum, the 95th quantile per-pixel signal-to-noise ratios.
Paper: PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). I. The Ubiquity of Fe I Emission and Inversions in Ultrahot Jupiter Atmospheres
Authors: Sydney Petz, Marshall C. Johnson, Anusha Pai Asnodkar, Alison Duck, Ji Wang, 吉 王, Ilya Ilyin, Klaus G. Strassmeier
Figure caption: Shifted and combined CCFs for TOI-1518 b for Ni I (top row), Fe II (middle row), and Mg I (bottom row) for only the 2023 November 6 observations (left column) and for the combined data sets (right column). The data for Fe II use both PEPSI arms, while those for Ni I and Mg I use only the red arm. The detection strengths decrease in the combined data, perhaps indicating a changing signal strength between the two data sets. See the main text for further discussion.
Paper: PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). I. The Ubiquity of Fe I Emission and Inversions in Ultrahot Jupiter Atmospheres
Authors: Sydney Petz, Marshall C. Johnson, Anusha Pai Asnodkar, Alison Duck, Ji Wang, 吉 王, Ilya Ilyin, Klaus G. Strassmeier
Figure caption: Shifted and combined CCFs for TOI-1518 b for Fe I (top), and Cr I (bottom row). For the bottom row, the left plot shows only the data from 2023 November 6, while the right plot shows both nights. These plots combine the PEPSI red and blue arms.
Paper: PEPSI Investigation, Retrieval, and Atlas of Numerous Giant Atmospheres (PIRANGA). I. The Ubiquity of Fe I Emission and Inversions in Ultrahot Jupiter Atmospheres
Authors: Sydney Petz, Marshall C. Johnson, Anusha Pai Asnodkar, Alison Duck, Ji Wang, 吉 王, Ilya Ilyin, Klaus G. Strassmeier
Figure caption: CCFs for TOI-1431 b, after being shifted into the planetary rest frame assuming a range of values of the planetary RV semiamplitude KP and combined. Fe I is shown on the left and Cr I on the right.
Paper: A Heliocentric-orbiting Objects Processing System (HOPS) for the Wide Field Survey Telescope: Architecture, Processing Workflow, and Preliminary Results
Authors: Shao-Han Wang, Bing-Xue Fu, Jun-Qiang Lu, LuLu Fan, Min-Xuan Cai, Ze-Lin Xu, Xu Kong, Haibin Zhao, Bin Li, Ya-Ting Liu, Qing-feng Zhu, Xu Zhou, Zhen Wan, Jingquan Cheng, Ji-an Jiang, Feng Li, Ming Liang, Hao Liu, Wentao Luo, Zheng Lou, Hairen Wang, Jian Wang, Tinggui Wang, Yongquan Xue, Hongfei Zhang, Wen Zhao
Figure caption: Orbital elements distribution of various types of 38,474 known asteroids observed by WFST, marked with different symbols. Left: the distribution of eccentricity vs. semimajor axis, with a gray line indicating the orbital elements where q (perihelion distance) equals 1.3 au. Right: the distribution of inclination vs. semimajor axis.
Paper: A Heliocentric-orbiting Objects Processing System (HOPS) for the Wide Field Survey Telescope: Architecture, Processing Workflow, and Preliminary Results
Authors: Shao-Han Wang, Bing-Xue Fu, Jun-Qiang Lu, LuLu Fan, Min-Xuan Cai, Ze-Lin Xu, Xu Kong, Haibin Zhao, Bin Li, Ya-Ting Liu, Qing-feng Zhu, Xu Zhou, Zhen Wan, Jingquan Cheng, Ji-an Jiang, Feng Li, Ming Liang, Hao Liu, Wentao Luo, Zheng Lou, Hairen Wang, Jian Wang, Tinggui Wang, Yongquan Xue, Hongfei Zhang, Wen Zhao
Figure caption: Completeness and run times of HOPS in single-night processing. Top: the number of findable SSOs and completeness of HOPS over dates. The gray line is 95.0% completeness. Bottom: run time of the HelioLinC3D’s make_tracklets (red dot) and the entire HOPS over dates (blue diamond).
Paper: A Heliocentric-orbiting Objects Processing System (HOPS) for the Wide Field Survey Telescope: Architecture, Processing Workflow, and Preliminary Results
Authors: Shao-Han Wang, Bing-Xue Fu, Jun-Qiang Lu, LuLu Fan, Min-Xuan Cai, Ze-Lin Xu, Xu Kong, Haibin Zhao, Bin Li, Ya-Ting Liu, Qing-feng Zhu, Xu Zhou, Zhen Wan, Jingquan Cheng, Ji-an Jiang, Feng Li, Ming Liang, Hao Liu, Wentao Luo, Zheng Lou, Hairen Wang, Jian Wang, Tinggui Wang, Yongquan Xue, Hongfei Zhang, Wen Zhao
Figure caption: Orbital elements distribution of various types of SSO candidates initial reported by WFST, marked with different symbols. Left: the distribution of eccentricity vs. semimajor axis, with a gray line indicating the orbital elements where q (perihelion distance) equals 1.3 au. Right: the distribution of inclination vs. semimajor axis.
Paper: A Heliocentric-orbiting Objects Processing System (HOPS) for the Wide Field Survey Telescope: Architecture, Processing Workflow, and Preliminary Results
Authors: Shao-Han Wang, Bing-Xue Fu, Jun-Qiang Lu, LuLu Fan, Min-Xuan Cai, Ze-Lin Xu, Xu Kong, Haibin Zhao, Bin Li, Ya-Ting Liu, Qing-feng Zhu, Xu Zhou, Zhen Wan, Jingquan Cheng, Ji-an Jiang, Feng Li, Ming Liang, Hao Liu, Wentao Luo, Zheng Lou, Hairen Wang, Jian Wang, Tinggui Wang, Yongquan Xue, Hongfei Zhang, Wen Zhao
Figure caption: Completeness and run times of HOPS in multinight processing. Top: the number of findable SSOs and the completeness of HOPS over dates. The gray line is 90.0% completeness. Bottom: run times of the HelioLinC3D over dates.
Paper: A Heliocentric-orbiting Objects Processing System (HOPS) for the Wide Field Survey Telescope: Architecture, Processing Workflow, and Preliminary Results
Authors: Shao-Han Wang, Bing-Xue Fu, Jun-Qiang Lu, LuLu Fan, Min-Xuan Cai, Ze-Lin Xu, Xu Kong, Haibin Zhao, Bin Li, Ya-Ting Liu, Qing-feng Zhu, Xu Zhou, Zhen Wan, Jingquan Cheng, Ji-an Jiang, Feng Li, Ming Liang, Hao Liu, Wentao Luo, Zheng Lou, Hairen Wang, Jian Wang, Tinggui Wang, Yongquan Xue, Hongfei Zhang, Wen Zhao
Figure caption: Overview of HOPS architecture. Data processing proceeds in the direction of the arrows shown in the figure.
Paper: A Heliocentric-orbiting Objects Processing System (HOPS) for the Wide Field Survey Telescope: Architecture, Processing Workflow, and Preliminary Results
Authors: Shao-Han Wang, Bing-Xue Fu, Jun-Qiang Lu, LuLu Fan, Min-Xuan Cai, Ze-Lin Xu, Xu Kong, Haibin Zhao, Bin Li, Ya-Ting Liu, Qing-feng Zhu, Xu Zhou, Zhen Wan, Jingquan Cheng, Ji-an Jiang, Feng Li, Ming Liang, Hao Liu, Wentao Luo, Zheng Lou, Hairen Wang, Jian Wang, Tinggui Wang, Yongquan Xue, Hongfei Zhang, Wen Zhao
Figure caption: Some example cutouts of true and false sources. The top row shows true sources and the bottom row shows false sources.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Plots of the best-fit dilution coefficient for the high-Ia population. Panel (A): distribution of best-fit Δ values. Panel (B): distribution of Δ with stellar age. Panel (C): average Δ in [Fe/Mg] vs. [Mg/H]. Panel (D): average Δ in ﹩{Z}_{{\rm{\max }}}﹩ vs. Rguide. Panel (E): average Δ in age vs. Rguide. In panels (D) and (E), bins with fewer than 20 stars have been excluded.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Fractional contribution of each eigenvector (EV) to each element for the PCA decomposition in ﹩{Z}_{{\rm{\max }}}﹩ vs. Rguide (left) and the PCA decomposition in age vs. Rguide (right).
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Average residual maps of the fiducial model (left) and dilution model (right) for the high-Ia population in age vs. Rguide for a subset of elements that experience the greatest reduction in their residual amplitudes under the dilution model.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Linear (Na/H) vs. (Fe/H) for three bins of [Mg/H]. In each panel, stars are colored by their age. We plot the KPM-predicted abundances in gray to show the model linearity.
Paper: Many Elements Matter: Detailed Abundance Patterns Reveal Star Formation and Enrichment Differences among Milky Way Structural Components
Authors: Emily J. Griffith, David W. Hogg, Sten Hasselquist, James W. Johnson, Adrian Price-Whelan, Tawny Sit, Alexander Stone-Martinez, David H. Weinberg
Figure caption: Maps of the average ﹩\mathrm{log}(g)﹩ (top), Teff (middle), and RV (bottom) in ﹩{Z}_{{\rm{\max }}}﹩ vs. Rguide (left) and age vs. Rguide (right). Bins with fewer than 20 stars have been excluded.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Eccentricity vs. semimajor axis for all confirmed transiting planets between 6 and 20 Earth radii. Colored circles are planets with measured spin–orbit angles. Blue circles are defined as “aligned” with spin–orbit angles of less than 30° and red circles are defined as “misaligned” with spin–orbit angles greater than 30°. The gray region illustrates planets that are likely undergoing high-eccentricity tidal migration. The upper and lower limits of the track are set by the Roche limit and the tidal circularization timescale (J. Dong et al. 2021). TOI-2005 b sits on the lower edge of the migration track. The dotted-dashed line presents the theoretical upper limit of eccentricities as a result of planet–planet scattering, assuming a planet with a mass of 0.5 MJup and a radius of 2 RJup, for illustrative purpose (C. Petrovich et al. 2014). Data were compiled from the NASA Exoplanet Archive as of 2024 October 30. Stellar obliquity measurements were obtained from E. Knudstrup et al. (2024)'s Table B2 with recent updates.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Radial velocity observations phase folded to the ephemeris. Section 2.2 details the radial velocities observations. Over-plotted are 500 realizations of the converged models from the global modeling, illustrating the set of velocity orbits allowed by the transit and radial velocity observations, illustrating the constraint placed on eccentricity by the joint model. The 3σ radial velocity semiamplitude of 1320 m s−1  provided a 3σ upper mass limit on the companion of 6.4MJup.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Per-sector normalized TESS PDCSAP lightcurves for TOI-2005. The target star was observed over four TESS sectors. The observing cadence was 1800 s in Sectors 9 and 10, 600 s in Sector 36, and 200 s in Sector 63. Unfortunately, during Sectors 10 and 36 the transit occurred in the gap in the lightcurve during data download. Predicted transits are marked with vertical dashed green lines.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: MIKE Doppler spectroscopic results from 2023 February 27. The color scale represents the fractional variation in the spectral line profile. Each plot shows the planetary signal after the average rotational profile is subtracted (top), the best-fit model (middle), and the residuals after subtracting the planetary signal (bottom).
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Correlations between eccentricity and key parameters that affect its posterior distribution, including the argument of periastron Ω, stellar mass and radius, and transit inclination. The 1σ and 2σ regions are marked by the red 2D histograms. We note a bimodality in the stellar radius as the posterior overlaps between the main sequence and subgiant branches.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Ground-based and TESS lightcurves normalized and offset relatively in flux and phased in time to the best-fit ephemeris. The best-fit model is shown in black.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: Spectral energy distribution of the target star TOI-2005. Magnitudes from Gaia G, Bp, Rp, Tycho B, V, 2MASS J, H, Ks, and WISE W1, W2, W3, and W4 are included in the global modeling of the system and are shown in dark blue.
Paper: TOI-2005b: An Eccentric Warm Jupiter in Spin-orbit Alignment
Authors: Allyson Bieryla, Jiayin Dong, George Zhou, Jason D. Eastman, L. C. Mayorga, David W. Latham, Brad Carter, Chelsea X. Huang, Samuel N. Quinn, Karen A. Collins, Lyu Abe, Yuri Beletsky, Rafael Brahm, Knicole D. Colón, Zahra Essack, Tristan Guillot, Thomas Henning, Melissa J. Hobson, Keith Horne, Jon M. Jenkins, Matías I. Jones, Andrés Jordán, David Osip, George R. Ricker, Joseph E. Rodriguez, Jack Schulte, Richard P. Schwarz, Sara Seager, Avi Shporer, Olga Suarez, Thiam-Guan Tan, Eric B. Ting, Amaury Triaud, Andrew Vanderburg, Jesus Noel Villaseñor, Noah Vowell, Cristilyn N. Watkins, Joshua N. Winn, Carl Ziegler
Figure caption: 5σ detection sensitivity and speckle autocorrelation functions of TOI-2005 from the 4.1 m SOAR. We find no companions to TOI-2005 within 3″ in these high-resolution imaging observations.