adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Same as Figure 12 plotting our MCMC fits using the BT-Settl08 grid for our continuum-subtracted NIRSpec spectra.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Same as Figure 12 plotting our MCMC fits using the DRIFT-PHOENIX grid for our continuum NIRSpec spectra.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: Six strongly revised orbits. All these pairs were discovered visually. Their WDS codes, discoverer designations, and revised periods are indicated, while periods of the previously computed orbits are given in brackets.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: Six orbits based only on speckle measurements. The WDS codes, discoverer designations, and periods are indicated. Alternative orbits are plotted by dotted lines.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: The accurate speckle-only orbit of 17304−0104 (STF 2173) on the left, with the visual measurements in the nineteenth century overplotted as crosses. Its fragment on the right shows the systematic residuals to the previous orbit (dashed line).
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: The orbit of HR 6100. Accurate positions are plotted as squares, less accurate as crosses (including three nonresolutions arbitrarily placed at 2 mas separation). The dashed circle indicates the diffraction limit of 27 mas. The lower plot shows separation versus time.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: Top row: Three shift-and-add images of HR 6100 suggesting resolutions in the same quadrant (black dots mark the center). The speckle power spectra of the object and the reference star taken in 2021.73 are shown below.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: Speckle DVA images of HR 6100 from the CHARA archive (courtesy B. Mason). The green arrows mark the companion’s location according to the orbit. The darker green arrow with a question mark indicates the published position in 1991.72.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: Orbits of 14453−3609 with periods of 15.9 yr (full line) and 31.8 yr (dash). Two discrepant visual measures are plotted by crosses and connected to the ephemeris positions by dotted lines.
Paper: Orbits of Binary Stars: from Visual Measures to Speckle Interferometry
Authors: Andrei Tokovinin
Figure caption: Three poorly constrained orbits.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: Normalized histogram distributions of the physical properties, including line radius (top left panel), masses (top right panel), surface mass densities (bottom left panel), and GDR (bottom right panel) of the well-defined distance clouds. The red, blue, and green lines represent the parameter distributions for min_npix = 225 (this work), min_npix = 144, and min_npix = 81, respectively. The median and standard deviation are presented in the top corner of every panel in matching colors.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: Left panel: the change of color excess ratios ﹩{E}_{\mathrm{NUV},{G}_{\mathrm{BP}}}﹩/﹩{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}﹩ with ﹩{\rm{\Delta }}{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}^{\mathrm{MC}}﹩. Right panel: the change of color excess ratios ﹩{E}_{\mathrm{NUV},{G}_{\mathrm{BP}}}﹩/﹩{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}﹩ with Galactic plane distance ∣z∣. Red dots are the results of the studied dust clouds, and purple stars are the median color excess ratios of the 0.05 ﹩{\rm{\Delta }}{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}^{\mathrm{MC}}﹩ interval (left panel) and 50 pc Galactic plane distance ∣z∣ interval (right panel). The blue dots in the left panel are the simulation results considering the effective wavelength shift because of T eff and ﹩{\rm{\Delta }}{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}^{\mathrm{MC}}﹩.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The distribution of the distances (d) and their relative uncertainties (σ  d /d). The proportion of clouds with σ  d /d < 5% are presented in the upper right corner of the panel.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The linear fitting for the color excess ﹩{E}_{\mathrm{NUV},{G}_{\mathrm{BP}}}﹩ to ﹩{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}﹩ in cloud 37 and cloud 96. Red and black dots represent sources within and outside the 95% confidence interval, respectively. The black line represents the fitting curve, and the purple shadow represents the 95% confidence interval.
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The relationship between ﹩{\rm{\Delta }}{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}^{\mathrm{MC}}﹩[ and ﹩{\rm{\Delta }}{E}_{\mathrm{NUV},{G}_{\mathrm{BP}}}^{\mathrm{MC}}﹩ (blue plus signs and blue line), as well as ﹩{E}_{{G}_{\mathrm{BP}},{G}_{\mathrm{RP}}}^{0}﹩ and ﹩{E}_{\mathrm{NUV},{G}_{\mathrm{BP}}}^{0}﹩ (red plus signs and red line).
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The distribution of dust clouds is shown in a Cartesian coordinate system, with the color bar indicating the Z-coordinate. The background image displays the contour of the V. Pelgrims et al. (2020) bubble (left panel) and the C. Zucker et al. (2022) bubble (right panel).
Paper: Identification and Distance Measurement of Dust Clouds at High Latitude by a Clustering Hierarchical Algorithm
Authors: Mingxu Sun, 明旭 孙, Biwei Jiang, 碧沩 姜, Helong Guo, 贺龙 郭, Wenyuan Cui, 文元 崔
Figure caption: The comparison of the distances of dust clouds with those derived by E. F. Schlafly et al. (2014), C. Zucker et al. (2019), and M. Sun et al. (2021b). The inset shows the distribution of the differences between our results and theirs.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: An example spectrum from MMT/Hectochelle for a member of Theia 456 (Gaia DR3 191357324369704448) in black, and the corresponding MINESweeper fit to the spectrum in purple. Residuals are shown in the top panel.
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption: The top plot compares μ  α  to μ  δ  (arcsec yr−1), with symbol color encoding photometric classification. The black points with associated numbers are subdwarfs described in Section 6. The bottom plot shows the distribution of the total proper motion of the SMDET sample. Note that objects with calculated proper motions were utilized in the analysis, while all other objects relied on proper motion measurements from CatWISE2020.
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption: (a) The near-infared (0.8–2.4 μm) SpeX spectrum of J1252+5220 (black lines) compared to T4, T5, and T6 spectral standards (orange, maroon, and yellow lines, respectively). (b) Similar sequence comparing ARCoIRIS data for J1603−7320 to T2, T3, and T4 spectral standards. The standard spectra are those defined in A. J. Burgasser et al. (2006b), with data from A. J. Burgasser et al. (2004) and A. J. Burgasser et al. (2006a). All are normalized at the peak of the J bandpass (∼1.3 μm).
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption: Distribution of spectral-type estimates for our SMDET sample. This figure does not include subdwarf candidates discovered in this paper.
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption:  J MKO−W2 vs. estimated distance with associated uncertainties. Symbol color encodes photometric classifications.
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption: Apparent W2 vs. estimated tangential velocity with associated uncertainties. Symbol color encodes photometric classifications.
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption: A color–color diagram illustrating our photo-type spectral-type estimates compared to known spectral types from W. M. J. Best et al. (2018). The starred objects are the 89 with available J MKO out of 110 photo-type spectral estimates from this study.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption:  BV photometry from SD24 presented with VR isochrones, [α/Fe] = 0.0 and [Fe/H] = −0.39. The isochrones have been adjusted for a reddening value E(B − V) = 0.07 and a true distance modulus = 13.12, as derived from astrometry by CG20.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption: VLT spectra in the Li line region for four giant members of NGC 2204, including the apparently rapid rotator W4216 = WOCS4009. For this figure, the spectrum of WOCS4009 has been offset by 0.7 Å to the blue, equivalent to a ∼30 km s−1 offset to align its spectrum with the other three. The vertical cyan line indicates the expected location of the Li line, 9.9 Å to the blue of the Ca 6717 Å line.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption: Comparison of Hydra and Gaia DR3 radial velocities. The cyan line is not a fit, merely an illustration of one-to-one correspondence. A single red filled symbol shows WOCS1002, denoted by Mermilliod & Mayor (2007) as an SB. Possible SBs WOCS1005, WOCS2006, WOCS1003, and WOCS4014 are denoted by magenta open triangles. Two green solid triangles show the positions of WOCS9015 and WOCS8011 while the blue squares represent the remaining comparisons between Hydra and DR3 radial velocities.
Paper: Li Evolution among Stars of Low/Intermediate Mass: the Metal-deficient Open Cluster NGC 2204
Authors: Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Aaron Steinhauer, Qinghui Sun, Bruce A. Twarog
Figure caption: CMD of the preselected sample of 167 stars in NGC 2204. Ultimate membership decisions are reflected by symbol: blue squares for probable members, red triangles for nonmembers.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: HR diagram of sample of one million stars cross-cataloged between Gaia and 2MASS with density contours. The MIST evolutionary track is shown in black for a 1 Gyr, 0.2 dex metallicity star assuming no extinction. KELT-24 is well-described as an F-type star, while KELT-24B is notably bright in comparison to stars of similar color.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Top: spectral energy distribution of the KELT-24 system modeled for two sources. Black points represent the observed photometric measurements, where the horizontal bars represent the effective width of the bandpass. The blue and orange lines are the corresponding model fluxes from the best-fit atmosphere models for our two sources considered. Bottom: flux ratios of KELT-24 to KELT-24B as a function of wavelength. KELT-24B contributes <1% of the total flux at bandpasses narrower than 0.7 μm, but is nearly 10% as bright as KELT-24 in redder bands.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Corner plot from LOFTI accepted trial orbits.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Phase-folded light curves from all KELT-FUN and TESS photometry. Spurious outlier points that deviate more than 2% from the baseline flux are removed here for enhanced clarity.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Snippet from TESS Sector 40 highlighting the single transit (BJD−2457000 ≈ 2415) in the KELT-24 (TIC 349827430) field of view. KELT-24 b can be seen transiting three times (BJD−2457000 ≈ 2406.5,  2412.0,  2417.5).
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Masses and periods of potential planetary counterparts to KELT-24 b that are not restricted by available RVs and photometry. Parameter space restricted by photometric and spectroscopic observations is shown in gray. Our supposed RV sensitivity limit of K = 100 m s−1 is conservative and based on the standard error of our current observations. We place a somewhat arbitrary P = 50 days threshold as a conservative minimum period for an additional body excluded via absence in TESS photometry, but note that slightly misaligned planets with shorter periods cannot be ruled out. The estimated habitable zone (HZ) is shown as the narrow hatched region.
Paper: Trials and Tribulations in the Reanalysis of KELT-24 b: A Case Study for the Importance of Stellar Modeling
Authors: Mark R. Giovinazzi, Bryson Cale, Jason D. Eastman, Joseph E. Rodriguez, Cullen H. Blake, Keivan G. Stassun, Andrew Vanderburg, Michelle Kunimoto, Adam L. Kraus, Joseph Twicken, Thomas G. Beatty, Cayla M. Dedrick, Jonathan Horner, John A. Johnson, Samson A. Johnson, Nate McCrady, Peter Plavchan, David H. Sliski, Maurice L. Wilson, Robert A. Wittenmyer, Jason T. Wright, Marshall C. Johnson, Mark E. Rose, Matthew Cornachione
Figure caption: Independent determination of the RM signal for KELT-24 b using only the in-transit SONG spectra taken with the ThAr cell. The best-fit spin–orbit angle (﹩\lambda =-{1.62}_{-5.56}^{+6.01}\circ ﹩) is consistent with our findings presented in Table 9. The gray regions represent the 1σ, 2σ, and 3σ deviations from our best-fit model. The spurious in-transit RVs from our analysis are simply overlaid to demonstrate agreement, and are not included in the fit here.