adsabs/AstroCLIMB huggingface dataset:
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: Posteriors of H 0 derived for four different LOSs (D 1 and D 2) in the MICEcat simulations, and for two different sky areas (1° and 5° opening angle for D 1x  and D 2x , respectively) around those directions. The top, middle, and bottom panels assume a standard deviation on the luminosity distance that is 10%, 20%, and 30% of the luminosity distance, respectively. All the posteriors are the result of combining 200 GW events and assume errors on galaxy redshift. We do not notice any significant bias.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: GW likelihood (vertical axis) as a function of the redshift (horizontal axis) for H 0 = 140 km s−1 Mpc−1. The lines show the case of ﹩{\sigma }_{{d}_{L}}/{d}_{L}=20 \% ﹩ (blue line) and ﹩{\sigma }_{{d}_{L}}/{d}_{L}=30 \% ﹩ (orange line). The vertical dashed line indicates z draw.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: Reconstructions of the galaxy density profile p cat(z) for each of the populations considered in the mock data. The blue histograms indicate the true redshift of the galaxies, the orange lines are the reconstructions of the density profile using Equation (13), and the black dashed lines mark the uniform in comoving volume distributions. For the LOSs with small galaxy numbers, we do not fit the redshift interpolant as these are used only in the limit that we perfectly know the redshift (in order to not introduce a bias due to the breaking of the statistical framework).
Paper: Luminosity Outburst Energized by the Collision between the Infalling Streamer and Disk in W51 North
Authors: Yan-Kun Zhang, Xi Chen, Shi-Ming Song, You-Xin Wang
Figure caption: Left-hand panel: the 22.235 GHz H2O maser spots detected toward W51 North with the VLA are shown with white circles, whereas those detected in Imai et al. (2002) using J-Net telescopes are shown with orange squares. In the background, the possible infall and the outflow traced by the SiO J = 5 − 4 line detected with the ALMA are shown in red and blue, corresponding to the velocity ranges of 67 ∼ 132 and −19 ∼ 46 km s−1, respectively. The 1.3 mm continuum is shown in green. Right-hand panel: the zoomed-in view of the H2O maser spots detected in our VLA observations and those in Imai et al. (2002), which are shown with light-colored circles and dark-colored squares, respectively. The reference position in J2000 coordinate is R.A. = 19h23m40.ˢ047, decl. = ﹩+14^\circ {31}^{{\prime} }05\buildrel{\prime\prime}\over{.} 530﹩. The areas of the circles or squares are proportional to the flux density of maser spots on a logarithmic scale and their colors indicate the velocity with respect to the LSR. The dark blue contours showed the 1.3 mm continuum, with the starting, step, and end level to be 0.0025, 0.0025, and 0.0100 Jy beam−1. The ring-like distributed maser spots are indicated by a thick-gray elliptical ring.
Paper: Luminosity Outburst Energized by the Collision between the Infalling Streamer and Disk in W51 North
Authors: Yan-Kun Zhang, Xi Chen, Shi-Ming Song, You-Xin Wang
Figure caption: The integrated intensity (left-hand panels), velocity distribution (middle panels) and velocity dispersion (right-hand panels) maps of the SiO J = 5 − 4 (upper) and HC3N J = 24 − 23 (lower) for the outflow and the infalling streamer detected toward W51 North with the ALMA. In the two left-hand panels, the 1.3 mm continuum is shown in green and the H2O maser spots are shown with light white circles. The LSR velocity ranges for the red- and blue-shifted SiO components are 67–97 and -36–56 km s−1, and those for HC3N are 68–82 and 35–51 km s−1, respectively. In the velocity distribution maps, the outflow and the infalling streamer are denoted with gray and blue boxes, respectively. The arrow shows the position of the mm continuum component ‘CB17’ detected in Tang et al. (2022). Zoomed versions of the infalling streamer are shown in the right-hand corner of the velocity dispersion maps, with the A region in Figure 5 being denoted with red boxes.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption:  H 0 posteriors with 200 GW events for several cases with inconsistent choices in either the simulation of mock data or the statistical framework for the D 15 LOS. The solid, dashed, and dotted lines are obtained with ﹩{\sigma }_{{d}_{L}}/{d}_{L}=10 \% ,20 \% ﹩, and 30%. First panel: GW events are generated by counting twice over the galaxy catalog. Second panel: the detection probability in the analysis is set as a Heaviside step function. Third panel: GW events are drawn from z < 0.3 and this correction is ignored in the analysis. Fourth panel: the luminosity distance dependence of the GW likelihood standard deviation is not properly taken into account in the formalism. Note that for this particular case alone we show D 21, which shows a more dramatic behavior than D 15, at least for the specific random seeds we tested.
Paper: Luminosity Outburst Energized by the Collision between the Infalling Streamer and Disk in W51 North
Authors: Yan-Kun Zhang, Xi Chen, Shi-Ming Song, You-Xin Wang
Figure caption: The integrated intensity maps and the P-V diagrams of the C18O J = 2 − 1 and 13CS J = 5 − 4 lines observed toward W51 North with the ALMA. The left-hand panel presents the integrated intensity maps, with the starting, step, and end levels of the white/blue contours are 4.5/4.5, 0.5/1.5, and 6.5/15.0 Jy beam−1 km s−1 for the C18O/13CS lines. The background is the C18O integrated intensity map. The red points indicate the H2O maser spots detected by the VLA observations, and the yellow arrow shows the same orientation as the major axis of the ring-like structure of the H2O maser spots. The middle and right-hand panels present the P-V diagrams along the yellow arrow direction shown in the left-hand panel, with contour levels starting from 50% in a step of 10% of their peaks (0.7 and 1.0 Jy beam−1 for the C18O and 13CS lines, respectively). The best Kepler rotation models are shown by the dashed curves and are described in Appendix A.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: Comparison between posteriors obtained in the one-galaxy limit, with 200 observed GW sources, computed using the standard approximate likelihood given in Equation (3) or using the full likelihood given in Equation (34). We show results for fractional errors in the EM measurement of the galaxy redshift of δ z/z = 0.3% and 3%, and also the perfect measurement limit δ z/z = 0%.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: PP plots for the one-galaxy analysis, with 200 observed GW sources, comparing the results using the approximate and full likelihoods. We consider the same values of the fractional error in the redshift measurement that were shown in Figure 8.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption:  H 0 posteriors for 200 GW events drawn from a uniform in comoving volume distribution of 106 galaxies. The several lines indicate various fractional errors on d  L  for the GW likelihood model. The absence of clustering significantly weakens the result, rendering it nearly uninformative in the limit of large numbers of galaxies, but does not incur in significant biases.
Paper: The Hitchhiker’s Guide to the Galaxy Catalog Approach for Dark Siren Gravitational-wave Cosmology
Authors: Jonathan R. Gair, Archisman Ghosh, Rachel Gray, Daniel E. Holz, Simone Mastrogiovanni, Suvodip Mukherjee, Antonella Palmese, Nicola Tamanini, Tessa Baker, Freija Beirnaert, Maciej Bilicki, Hsin-Yu Chen, Gergely Dálya, Jose Maria Ezquiaga, Will M. Farr, Maya Fishbach, Juan Garcia-Bellido, Tathagata Ghosh, Hsiang-Yu Huang, Christos Karathanasis, Konstantin Leyde, Ignacio Magaña Hernandez, Johannes Noller, Gregoire Pierra, Peter Raffai, Antonio Enea Romano, Monica Seglar-Arroyo, Danièle A. Steer, Cezary Turski, Maria Paola Vaccaro, Sergio Andrés Vallejo-Peña
Figure caption: PP plot generated for directions 1 and 2 and a nominal error on d  L  of 10%–30%. The shaded area shows the 1, 2, and 3σ fluctuations of the PP plot around the ideal case. Our simulations show that we are able to recover the input value of H 0 without incurring any significant bias.
Paper: Luminosity Outburst Energized by the Collision between the Infalling Streamer and Disk in W51 North
Authors: Yan-Kun Zhang, Xi Chen, Shi-Ming Song, You-Xin Wang
Figure caption: The left-hand panels present the spectra of the H2O maser detected in the four-epoch monitoring with TMRT during January to April 2020. Some velocity components with obvious variability are marked with dashed lines. The two right-hand panels give the spectrum and spatial distribution of the H2O masers detected with the VLA. For the maser spots at the marked velocities in the spectra, they are enclosed with circles in different colors in the maser distribution image in W51 North (lower right-hand panel). The reference position (offset = (0 mas, 0 mas)) in the J2000 coordinate is R.A. = 19h23m40.ˢ047, decl. = ﹩+14^\circ {31}^{{\prime} }05\buildrel{\prime\prime}\over{.} 530﹩. The regions marked with “A,” “B,” and “C” show obvious maser variability from the multi-epoch monitoring with TMRT. Their corresponding velocity ranges are denoted in the maser spectra.
Paper: Luminosity Outburst Energized by the Collision between the Infalling Streamer and Disk in W51 North
Authors: Yan-Kun Zhang, Xi Chen, Shi-Ming Song, You-Xin Wang
Figure caption: Upper left-hand panel: the artist’s conception for the overview structures of W51N, which are extracted from Zapata et al. (2009). Upper right-hand panel: the zoomed-in view of the H2O maser spots in the velocity range of 54∼64 km s−1 detected with our VLA observation overlaid on the radial velocity field of the disk projected onto the sky plane. The reference position (offset = (0 mas, 0 mas)) in J2000 coordinate is R.A. = 19h23m40.ˢ047, decl. = ﹩+14^\circ {31}^{{\prime} }05\buildrel{\prime\prime}\over{.} 530﹩. Lower panel: a carton front view of the kinematic features of W51 North. The infalling streamer is shown in light-red. The modeled disk is shown in gray with different transparencies, which indicate the inner and outer portions of the disk. The rotational and infalling orientations are shown with arrows near to the infalling streamer and the disk, respectively.
Paper: Luminosity Outburst Energized by the Collision between the Infalling Streamer and Disk in W51 North
Authors: Yan-Kun Zhang, Xi Chen, Shi-Ming Song, You-Xin Wang
Figure caption: Left-hand panel: same as the left-hand panel of Figure 1 for the outflow and infalling streamer traced by the SiO detected toward W51 North with the ALMA. Right-hand panel: the P-V diagram for the infalling streamer along the arrow direction shown in the left-hand panel. The contour levels in the P-V diagram start from 50% in steps of 25% of its peak (0.001 Jy beam−1 for the SiO infalling streamer). The best kinematic model for the gravitationally controlled infalling streamer is shown with the dashed curve and is described in Appendix B.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: (a) Median normalized TESS long-cadence light curve for TOI-3984 A derived with eleanor. The solid green line is the best-fitting Gaussian process model used to detrend the light curve. The triangles indicate the observed transits. (b) Same as panel (a) but for short-cadence TESS data. Panels (c) and (d) show the phase-folded light curves for short- and long-cadence TESS data. In panels (c) and (d), the best-fitting model from the joint fit to the photometry and RVs is plotted as a dashed line, while the shaded regions denote the 1σ (darkest), 2σ, and 3σ (lightest) extent of the model posteriors. The modeling of the photometry and RVs is described in detail in Section 4.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: (a) The 11 × 11 TESS target pixel cutout from Sector 51 centered on TOI-3984 A (marked as a star). Stars identified in Gaia DR3 with magnitudes ΔG RP < 4 are marked with diamond stars for reference. (b) Overlay of the region contained in an 11 × 11 pixel grid centered on TOI-3984 A from all sectors (green polygon), the region contained within all SPOC (red polygon) and eleanor (blue polygon) photometric apertures, and other comparably bright stars on a ZTF zi image.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Same as Figure 1 but for TOI-5293 A. (a) The 31 × 31 TESS target pixel cutout centered around TOI-5293 A (marked as a star). Stars identified in Gaia EDR3 having magnitudes ΔG RP < 4 are marked with diamond stars. (b) Overlay of the TESS 11 × 11 pixel subgrid (green polygon), the region contained in the photometric aperture (red polygon), and other comparably bright stars on a ZTF zi image.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Same as Figure 3 but for TOI-5293 A. (a) Median normalized TESS light curve for TOI-5293 A derived with eleanor along with the best-fitting Gaussian process model. The triangles indicate the observed transits. Panels (b)−(g) are the light curves for the TESS, RBO, LCRO, and TMMT plotted with model posteriors (shaded regions) from the joint fit to the photometry and RVs.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Comparison of the TSM from Kempton et al. (2018) for TOI-3984 A and TOI-5293 A to the existing M dwarf gas giant population (P < 10 days and R  p  > 8 R J). TOI-3984 A is the coolest object in this sample and provides an opportunity to characterize the chemistry in a gas giant with T eq < 600 K. TOI-5293 A b overlaps with TOI-3629 b in equilibrium temperature and TSM but is much larger in radius and provides an opportunity to study a temperate gas giant with R > 1 R J. The TSM value for hot Jupiters orbiting Sun-like stars is included for reference. The data were compiled from the NASA Exoplanet Archive on 2023 May 3.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: (a) TOI-3984 A b (star) and TOI-5293 A b (diamond star) on the mass–radius diagram for transiting M dwarf exoplanets with mass measurements and R  p  > 4 R ⊕. All previously known hot Jupiters (P < 10 days and R  P  ≥ 8 R ⊕) transiting M dwarfs are marked as pentagons. (b) TOI-3984 A and TOI-5293 A on an effective temperature–surface gravity diagram. (c) Insolation flux and radius for these planets. The data were compiled from the NASA Exoplanet Archive (Akeson et al. 2013) on 2023 May 3.
Paper: TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Authors: Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrea S. J. Lin, Maria Schutte, Luke Powers, Sinclaire Jones, Andrew Monson, Songhu Wang, Guđmundur Stefánsson, William D. Cochran, Paul Robertson, Suvrath Mahadevan, Adam F. Kowalski, John Wisniewski, Brock A. Parker, Alexander Larsen, Franklin A. L. Chapman, Henry A. Kobulnicky, Arvind F. Gupta, Mark E. Everett, Bryan Edward Penprase, Gregory Zeimann, Corey Beard, Chad F. Bender, Knicole D. Colón, Scott A. Diddams, Connor Fredrick, Samuel Halverson, Joe P. Ninan, Lawrence W. Ramsey, Arpita Roy, Christian Schwab
Figure caption: Panel (a) shows the RVs for TOI-3984 A derived with modified versions of SERVAL. Panel (b) displays the phase-folded RVs plotted with model posteriors and the residuals to the fit. In panels (a) and (b), the dashed line is the best-fitting Keplerian model. The shaded regions denote the 1σ (darkest), 2σ, and 3σ (lightest) extent of the model posteriors. The modeling is described in Section 4.