adsabs/AstroCLIMB huggingface dataset:
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. III. Aperture Masking Interferometric Observations of the Star HIP 65426 at 3.8 μm
Authors: Shrishmoy Ray, Steph Sallum, Sasha Hinkley, Anand Sivaramkrishnan, Rachel Cooper, Jens Kammerer, Alexandra Z. Greebaum, Deeparshi Thatte, Tomas Stolker, Cecilia Lazzoni, Andrei Tokovinin, Matthew de Furio, Samuel Factor, Michael Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo, B. A. Sargent, Christopher A. Theissen, Elena Manjavacas, Anna Lueber, Daniel Kitzmann, Ben J. Sutlieff, Sarah K. Betti
Figure caption: Each purple segment represents a “frame,” which is the same as a “group” in this mode and is the smallest unit of exposure. An “integration” is comprised of a number of groups (three, in this case) and represents the total number of photons collected in a contiguous sequence. After each integration, the detector resets and executes the next integration, to collect photons. The total exposure of an observation is the collection of “n” such integrations.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. III. Aperture Masking Interferometric Observations of the Star HIP 65426 at 3.8 μm
Authors: Shrishmoy Ray, Steph Sallum, Sasha Hinkley, Anand Sivaramkrishnan, Rachel Cooper, Jens Kammerer, Alexandra Z. Greebaum, Deeparshi Thatte, Tomas Stolker, Cecilia Lazzoni, Andrei Tokovinin, Matthew de Furio, Samuel Factor, Michael Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo, B. A. Sargent, Christopher A. Theissen, Elena Manjavacas, Anna Lueber, Daniel Kitzmann, Ben J. Sutlieff, Sarah K. Betti
Figure caption: The calibrated closure phases and the corresponding best fits for the injected companion signals. The test numbers are color-coded according to Figure 5, at the bottom right of each plot. The ΔmF430M and separation values for each injection are also provided at the top left for each plot.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. III. Aperture Masking Interferometric Observations of the Star HIP 65426 at 3.8 μm
Authors: Shrishmoy Ray, Steph Sallum, Sasha Hinkley, Anand Sivaramkrishnan, Rachel Cooper, Jens Kammerer, Alexandra Z. Greebaum, Deeparshi Thatte, Tomas Stolker, Cecilia Lazzoni, Andrei Tokovinin, Matthew de Furio, Samuel Factor, Michael Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo, B. A. Sargent, Christopher A. Theissen, Elena Manjavacas, Anna Lueber, Daniel Kitzmann, Ben J. Sutlieff, Sarah K. Betti
Figure caption: The calibrated squared visibilities and the corresponding best fits for the injected companion signals. The test numbers are color-coded according to Figure 5, at the bottom right of each plot. The ΔmF430M and separation values for each injection are also provided at the top left for each plot.
Paper: TOI-6324 b: An Earth-mass Ultra-short-period Planet Transiting a Nearby M Dwarf
Authors: Rena A. Lee, Fei Dai, Andrew W. Howard, Samuel Halverson, Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Benjamin J. Fulton, Guđmundur Stefánsson, Jack Lubin, Howard Isaacson, Casey L. Brinkman, Nicholas Saunders, Daniel Hey, Daniel Huber, Lauren M. Weiss, Leslie A. Rogers, Diana Valencia, Mykhaylo Plotnykov, Kimberly Paragas, Renyu Hu, Te Han, Erik A. Petigura, Ryan Rubenzahl, David R. Ciardi, Aaron Householder, Gregory J. Gilbert, J. M. Joel Ong, Jingwen Zhang, Jacob Luhn, Luke Handley, Corey Beard, Steven Giacalone, Rae Holcomb, Judah Van Zandt, Ashley D. Baker, Max Brodheim, Matt Brown, David Charbonneau, Karen A. Collins, Ian J. M. Crossfield, William Deich, Xavier Dumusque, Steven R. Gibson, Emily Gilbert, Grant M. Hill, Bradford Holden, Jon M. Jenkins, Stephen Kaye, Russ R. Laher, Kyle Lanclos, W. Garett Levine, Joel Payne, Alex S. Polanski, John O'Meara, George R. Ricker, Kodi Rider, Paul Robertson, Arpita Roy, Joshua E. Schlieder, Christian Schwab, Sara Seager, Abby P. Shaum, Martin M. Sirk, Stephanie Striegel, Johanna Teske, John Valliant, Roland Vanderspek, Gautam Vasisht, Josh Walawender, Sharon Xuesong Wang, Joshua N. Winn, Edward Wishnow, Sherry Yeh
Figure caption: Binned and phase-folded SPOC PDC-SAP light curve of TOI-6324 revealing the transit signal of TOI-6324 b, with the best-fit transit model overplotted in blue. The residuals (data minus model) are shown in the bottom panel.
Paper: TOI-6324 b: An Earth-mass Ultra-short-period Planet Transiting a Nearby M Dwarf
Authors: Rena A. Lee, Fei Dai, Andrew W. Howard, Samuel Halverson, Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Benjamin J. Fulton, Guđmundur Stefánsson, Jack Lubin, Howard Isaacson, Casey L. Brinkman, Nicholas Saunders, Daniel Hey, Daniel Huber, Lauren M. Weiss, Leslie A. Rogers, Diana Valencia, Mykhaylo Plotnykov, Kimberly Paragas, Renyu Hu, Te Han, Erik A. Petigura, Ryan Rubenzahl, David R. Ciardi, Aaron Householder, Gregory J. Gilbert, J. M. Joel Ong, Jingwen Zhang, Jacob Luhn, Luke Handley, Corey Beard, Steven Giacalone, Rae Holcomb, Judah Van Zandt, Ashley D. Baker, Max Brodheim, Matt Brown, David Charbonneau, Karen A. Collins, Ian J. M. Crossfield, William Deich, Xavier Dumusque, Steven R. Gibson, Emily Gilbert, Grant M. Hill, Bradford Holden, Jon M. Jenkins, Stephen Kaye, Russ R. Laher, Kyle Lanclos, W. Garett Levine, Joel Payne, Alex S. Polanski, John O'Meara, George R. Ricker, Kodi Rider, Paul Robertson, Arpita Roy, Joshua E. Schlieder, Christian Schwab, Sara Seager, Abby P. Shaum, Martin M. Sirk, Stephanie Striegel, Johanna Teske, John Valliant, Roland Vanderspek, Gautam Vasisht, Josh Walawender, Sharon Xuesong Wang, Joshua N. Winn, Edward Wishnow, Sherry Yeh
Figure caption: NIR AO imaging and sensitivity curve. The black points represent the 5σ detection limit, and the purple region represents the 1σ azimuthal dispersion of the contrast determination. Inset: AO image of TOI-6324 showing no evidence for a close-in companion.
Paper: TOI-6324 b: An Earth-mass Ultra-short-period Planet Transiting a Nearby M Dwarf
Authors: Rena A. Lee, Fei Dai, Andrew W. Howard, Samuel Halverson, Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Benjamin J. Fulton, Guđmundur Stefánsson, Jack Lubin, Howard Isaacson, Casey L. Brinkman, Nicholas Saunders, Daniel Hey, Daniel Huber, Lauren M. Weiss, Leslie A. Rogers, Diana Valencia, Mykhaylo Plotnykov, Kimberly Paragas, Renyu Hu, Te Han, Erik A. Petigura, Ryan Rubenzahl, David R. Ciardi, Aaron Householder, Gregory J. Gilbert, J. M. Joel Ong, Jingwen Zhang, Jacob Luhn, Luke Handley, Corey Beard, Steven Giacalone, Rae Holcomb, Judah Van Zandt, Ashley D. Baker, Max Brodheim, Matt Brown, David Charbonneau, Karen A. Collins, Ian J. M. Crossfield, William Deich, Xavier Dumusque, Steven R. Gibson, Emily Gilbert, Grant M. Hill, Bradford Holden, Jon M. Jenkins, Stephen Kaye, Russ R. Laher, Kyle Lanclos, W. Garett Levine, Joel Payne, Alex S. Polanski, John O'Meara, George R. Ricker, Kodi Rider, Paul Robertson, Arpita Roy, Joshua E. Schlieder, Christian Schwab, Sara Seager, Abby P. Shaum, Martin M. Sirk, Stephanie Striegel, Johanna Teske, John Valliant, Roland Vanderspek, Gautam Vasisht, Josh Walawender, Sharon Xuesong Wang, Joshua N. Winn, Edward Wishnow, Sherry Yeh
Figure caption: (a) Binned and phase-folded TESS light curve of TOI-6324. The pink curve shows the best-fit model without ellipsoidal light variation (ELV) in the phase-curve model, and the blue curve shows the best-fit result that includes the ELV term. The residuals (data minus model) from each model are shown in the bottom panel. (b) Thermal emission (pink dotted line) and reflected light (blue dotted line) in the TESS band as a function of the Bond albedo. The flux ratio (Fp/F⋆) measured in this work is shown as the black line with the associated 1σ confidence shaded in gray. The phase-curve variation observed in the TESS band is likely attributed to a combination of both thermal emission and reflected stellar light (purple dashed line).
Paper: TOI-6324 b: An Earth-mass Ultra-short-period Planet Transiting a Nearby M Dwarf
Authors: Rena A. Lee, Fei Dai, Andrew W. Howard, Samuel Halverson, Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Benjamin J. Fulton, Guđmundur Stefánsson, Jack Lubin, Howard Isaacson, Casey L. Brinkman, Nicholas Saunders, Daniel Hey, Daniel Huber, Lauren M. Weiss, Leslie A. Rogers, Diana Valencia, Mykhaylo Plotnykov, Kimberly Paragas, Renyu Hu, Te Han, Erik A. Petigura, Ryan Rubenzahl, David R. Ciardi, Aaron Householder, Gregory J. Gilbert, J. M. Joel Ong, Jingwen Zhang, Jacob Luhn, Luke Handley, Corey Beard, Steven Giacalone, Rae Holcomb, Judah Van Zandt, Ashley D. Baker, Max Brodheim, Matt Brown, David Charbonneau, Karen A. Collins, Ian J. M. Crossfield, William Deich, Xavier Dumusque, Steven R. Gibson, Emily Gilbert, Grant M. Hill, Bradford Holden, Jon M. Jenkins, Stephen Kaye, Russ R. Laher, Kyle Lanclos, W. Garett Levine, Joel Payne, Alex S. Polanski, John O'Meara, George R. Ricker, Kodi Rider, Paul Robertson, Arpita Roy, Joshua E. Schlieder, Christian Schwab, Sara Seager, Abby P. Shaum, Martin M. Sirk, Stephanie Striegel, Johanna Teske, John Valliant, Roland Vanderspek, Gautam Vasisht, Josh Walawender, Sharon Xuesong Wang, Joshua N. Winn, Edward Wishnow, Sherry Yeh
Figure caption: The radial velocity (RV) variations of TOI-6324 observed with KPF. (a) Time-series RV measurements along with the best-fit radvel Gaussian process (GP) model (blue line) used to remove stellar and instrumental systematics longer than the 6.7 hr orbital period of TOI-6324 b (see Section 4.2). The yellow contour represents the uncertainty of the GP model. Data points have been median-offset by −49.94 m s−1; the raw values are given in Table 2. (b) Residuals (data–GP model). (c) RV variations of TOI-6324 as a function of orbital phase, resulting from our GP model. The red points show RVs binned to 10% of Porb. (d) RV variations of TOI-6324 as a function of orbital phase, resulting from our floating chunk offset (FCO) analysis (see Section 4.3). Data points are colored by observation date. The measured RV semiamplitude from both the GP and FCO analyses are consistent within 1σ (KGP = 2.69 ±  0.51 m s−1 and KFCO = 2.19 ± 1.02 m s−1).
Paper: TOI-6324 b: An Earth-mass Ultra-short-period Planet Transiting a Nearby M Dwarf
Authors: Rena A. Lee, Fei Dai, Andrew W. Howard, Samuel Halverson, Jonathan Gomez Barrientos, Michael Greklek-McKeon, Heather A. Knutson, Benjamin J. Fulton, Guđmundur Stefánsson, Jack Lubin, Howard Isaacson, Casey L. Brinkman, Nicholas Saunders, Daniel Hey, Daniel Huber, Lauren M. Weiss, Leslie A. Rogers, Diana Valencia, Mykhaylo Plotnykov, Kimberly Paragas, Renyu Hu, Te Han, Erik A. Petigura, Ryan Rubenzahl, David R. Ciardi, Aaron Householder, Gregory J. Gilbert, J. M. Joel Ong, Jingwen Zhang, Jacob Luhn, Luke Handley, Corey Beard, Steven Giacalone, Rae Holcomb, Judah Van Zandt, Ashley D. Baker, Max Brodheim, Matt Brown, David Charbonneau, Karen A. Collins, Ian J. M. Crossfield, William Deich, Xavier Dumusque, Steven R. Gibson, Emily Gilbert, Grant M. Hill, Bradford Holden, Jon M. Jenkins, Stephen Kaye, Russ R. Laher, Kyle Lanclos, W. Garett Levine, Joel Payne, Alex S. Polanski, John O'Meara, George R. Ricker, Kodi Rider, Paul Robertson, Arpita Roy, Joshua E. Schlieder, Christian Schwab, Sara Seager, Abby P. Shaum, Martin M. Sirk, Stephanie Striegel, Johanna Teske, John Valliant, Roland Vanderspek, Gautam Vasisht, Josh Walawender, Sharon Xuesong Wang, Joshua N. Winn, Edward Wishnow, Sherry Yeh
Figure caption: Mass–radius diagram of confirmed USPs (dark purple) and other rocky planets <2 R⊕ (light purple). TOI-6324 b is plotted in pink. The magenta-outlined point represents TOI-6324 b in the case that it is tidally distorted by 5%. In the spherical case, CMF﹩{}_{{R}_{\mathrm{tran}}}﹩ = 27% ± 37%, while in the distorted case, CMF﹩{}_{{R}_{\mathrm{vol}}}﹩ = 3% ± 40%.
Paper: Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in Ωm and H0 across Cosmological Probes
Authors: Xianzhe TZ Tang, Dillon Brout, Tanvi Karwal, Chihway Chang, Vivian Miranda, Maria Vincenzi
Figure caption: The figure shows marginalized ΛCDM fits for H0 and Ωm to mock data sets in w0waCDM cosmologies. Simulated w0waCDM sample the public DES24 chains. Left panel: the ΛCDMΩm distributions for various probes {SN, BAO, and CMB}. The gray dashed curve shows the underlying values of Ωm used for these simulations. The three vertical lines represent the observed ΛCDMΩm values for real data for reference: DESI Y1 (DESI Collaboration 2025; blue), DES-SN 5YR (DESI Collaboration 2024; yellow), and Planck18 CMB only (Planck Collaboration 2020; pink). Right panel: the ΛCDMH0 distributions for BAO and CMB probes. The gray dashed curve shows the w0waCDMH0 values used to simulate the mocks. SNe are not shown here because DES-like SNe are not sensitive to H0 by themselves but require an external calibration. Right panel inset: the corresponding ΔH0 distribution, quantifying the difference between H0 results from BAO and CMB data sets at each step in the chains. The shaded region represents the 68% credible interval. The red dashed line indicates the observed ΔH0 between DESI Y1 BAO and Planck18 CMB under ΛCDM. Our observed difference between the simulated w0waCDM maximum likelihood H0 and the “observed” mock-BAO ΛCDM maximum likelihood H0 is 1.2 km s−1 Mpc−1.
Paper: Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in Ωm and H0 across Cosmological Probes
Authors: Xianzhe TZ Tang, Dillon Brout, Tanvi Karwal, Chihway Chang, Vivian Miranda, Maria Vincenzi
Figure caption: Comparison between the best-fit ΛCDM cosmology (with Ωm = 0.35 for SNe or Ωm = 0.28 for BAO) and a Planck-like ΛCDM cosmology (Ωm = 0.315) against the DESI+CMB+DESY5SN (DESI Collaboration 2025) best-fit w0waCDM model {w0 = −0.727, wa = −1.05, Ωm = 0.316, H0 = 67.24} with realistic data uncertainties shown for SNe (top) and BAO (bottom). The three panels show residuals in the SN distance modulus μ, the BAO DV/rd, and the BAO FAP vs. redshift z. Error bars (shaded regions) reflect uncertainties in DES-SN 5YR (DESI Collaboration 2024) and DESI Y1 (DESI Collaboration 2025), with binned SN errors using weighted averages of uncertainties in redshift bins of width Δz = 0.15 for illustration. The χ2 values reported indicate goodness of fit for each model (colored curves) relative to the mock data generated in w0waCDM (horizontal dashed), calculated similarly to Equations (3) and (8) (without the normalization term). “Minimized” refers to floating one parameter while fixing others to achieve the lowest χ2. For BAO, when Ωm = 0.315, H0 is “minimized” to 68.8; when H0 = 67.5, Ωm is “minimized” to 0.279. For the SNe, H0 is also “minimized” for both models presented.
Paper: Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in Ωm and H0 across Cosmological Probes
Authors: Xianzhe TZ Tang, Dillon Brout, Tanvi Karwal, Chihway Chang, Vivian Miranda, Maria Vincenzi
Figure caption: Constraints on Ωm and H0 obtained by fitting ΛCDM to mock CMB, BAO, and SN data sets generated in the DESI+DES-SN+Planck (DESI Collaboration 2025) best-fit w0waCDM cosmology {w0 = −0.727, wa = −1.05, Ωm = 0.316, H0 = 67.24}. The contours represent the 68% and 95% confidence regions for each mock data set individually: SNe (yellow), BAO (blue), and CMB (pink). This figure illustrates the Ωm and H0 discrepancies between different probes when fitting ΛCDM to data simulated in a dynamical w0waCDM cosmology.
Paper: Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in Ωm and H0 across Cosmological Probes
Authors: Xianzhe TZ Tang, Dillon Brout, Tanvi Karwal, Chihway Chang, Vivian Miranda, Maria Vincenzi
Figure caption: MCMC results testing the w0waCDM model using mock data combined from different probe-like data sets generated under the ΛCDM model but with different Ωm and H0. The black dashed lines indicate the ΛCDM values (w0 = −1, wa = 0). The purple contour represents the constraints from mock SN (Ωm = 0.353) and BAO (Ωm = 0.295, H0 = 68.5 km s−1 Mpc−1) data. The green contour adds the CMB (Ωm = 0.315, H0 = 67.3 km s−1 Mpc−1) mock data to the previous combination. The gray contour shows the constraints from BAO and CMB mock data. This figure illustrates how discrepancies in the ΛCDM model’s Ωm and H0 among different data sets can lead to signals of dynamical dark energy when analyzed under the w0waCDM model.
Paper: Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in Ωm and H0 across Cosmological Probes
Authors: Xianzhe TZ Tang, Dillon Brout, Tanvi Karwal, Chihway Chang, Vivian Miranda, Maria Vincenzi
Figure caption: Results of the grid-based exploration of the w0wa parameter space that can generate the observed discrepancies in ΛCDMΩm. Blue contours represent grid points where each probe’s fitted ΛCDMΩm values are similar to observed values (which are 0.353 ± 0.017 for SNe, 0.295 ± 0.015 for BAO, and 0.315 ± 0.007 for CMB; DESI Collaboration 2024; DESI Collaboration 2025; Planck Collaboration 2020), with the 1σ and 2σ contours obtained from the likelihood ﹩{{ \mathcal L }}_{\,\rm{joint}\,}^{* }﹩ from Equation (B2). The orange contours show the samples from the DES24 chain (DESI Collaboration 2024). Black dashed lines indicate ΛCDM values (w0 = −1, wa = 0).
Paper: Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in Ωm and H0 across Cosmological Probes
Authors: Xianzhe TZ Tang, Dillon Brout, Tanvi Karwal, Chihway Chang, Vivian Miranda, Maria Vincenzi
Figure caption: Constraints on Ωm and H0 obtained by fitting the ΛCDM model to mock CMB, BAO, and SN data sets generated in the best-fit w0waCDM cosmology (w0 = −0.727, wa = −1.05, Ωm = 0.316, H0 = 67.24 km s−1 Mpc−1), with direct rd calibration. The BAO constraints (dark blue contours) become less circular in the Ωm–H0 plane compared to the case without direct rd calibration (Figure 1, also shown here as the dashed–dotted contours).
Paper: Uniting the Observed Dynamical Dark Energy Preference with the Discrepancies in Ωm and H0 across Cosmological Probes
Authors: Xianzhe TZ Tang, Dillon Brout, Tanvi Karwal, Chihway Chang, Vivian Miranda, Maria Vincenzi
Figure caption: Null test: posterior distributions of Ωm, w0, wa, and H0 from the MCMC analysis of the combined data sets when the input is simulated under the same ΛCDM cosmology. The top two panels (left: SNe, BAO; right: SNe, BAO, CMB) adopt rd derived using Equation (2.5) from the DESI Y1 paper, which has standard early-time physics assumptions, taking a Gaussian prior on Ωbh2 = 0.02218 ± 0.00055, the same as in Equation (2.9) in DESI Collaboration (2025). The bottom two panels (left: SNe, BAO; right: SNe, BAO, CMB) use a Gaussian prior on the sound horizon rd = 147.09 ± 0.26 Mpc. The input values Ωm = 0.30 and H0 = 70 km s−1 Mpc−1 are indicated by blue lines, and the contours represent the 68%, 95%, and 99.7% confidence levels. All posteriors recover the input cosmology within 1σ.