adsabs/AstroCLIMB huggingface dataset:
Paper: The HI Mass Function of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The M HI –M  B  relation at z ≈ 1. The red points show our measurements of the average HI mass in the three M  B  subsamples. The blue curve and blue shaded region show, respectively, the best fit to the measurements and the 1σ confidence interval. The black dashed line indicates the “mean” M HI –M  B  relation at z ≈ 0 (Dénes et al. 2014). It is clear that our measurements of the average HI mass in the three M  B  subsamples are consistent with the M HI –M  B  relation at z ≈ 0, indicating that the relation has not evolved between z ≈ 1 and z ≈ 0. We emphasize that the figure shows the “mean” M HI –M  B  relation at both z ≈ 1 and z ≈ 0 (see Section 3): we have used the measured scatter of 0.26 dex in the M HI –M  B  relation at z ≈ 0 (Dénes et al. 2014) and Equation (2) to obtain the mean M HI –M  B  relation at z ≈ 0.
Paper: The HI Mass Function of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: (A) The HIMF of star-forming galaxies at z ≈ 1. The blue curve shows our measurement of the HIMF at z ≈ 1, obtained by combining the GMRT-CATz1 measurement of the M HI –M  B  relation with the B-band luminosity function at z ≈ 1 from the ALHAMBRA survey (López-Sanjuan et al. 2017); the shaded region shows the 68% confidence interval on the HIMF. (B) The number density of galaxies at z ≈ 1 with HI mass greater than M HI  (﹩{n}_{\gt {M}_{{\rm{H}}\,{\rm\small{I}}}}﹩), obtained by integrating the HIMF of panel (A) from M HI  to ∞, is shown in blue, with the 68% confidence interval indicated by the blue shaded region. The dashed curve in both panels shows the same quantities at z ≈ 0 from Jones et al. (2018). The figure shows that the number density of galaxies with M HI  > 1010 M ⊙ is far larger at z ≈ 1 than at z ≈ 0.
Paper: The HI Mass Function of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The ratio of the number density of galaxies at z ≈ 1 to that at z ≈ 0 as a function of the assumed scatter in the M HI –M  B  relation at z ≈ 1, for galaxies with HI masses >1010 M ⊙ (blue curve) and >5 × 1010 M ⊙ (orange curve). For each curve, the shaded region indicates the ≈68 % confidence interval. The open circles indicate the ratio for an assumed scatter of 0.26 dex, the value measured in the local Universe (Dénes et al. 2014). The figure shows that the number density of galaxies with M HI  > 1010 M ⊙ at z ≈ 1 is a factor of  ≈4–5 higher than that at z ≈ 0, independent of the assumed scatter in the M HI –M  B  relation. However, the same ratio for galaxies with M HI  > 5 × 1010 M ⊙ is seen clearly to be sensitive to the assumed scatter in the relation.
Paper: The HI Mass Function of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The average HI 21 cm emission signal from star-forming galaxies in different M  B  subsamples at z ≈ 1. The top panels show the stacked HI 21 cm emission spectra, at a velocity resolution of 90 km s−1, for galaxies in the three M  B  subsamples, bright (left panel), intermediate (middle panel), and faint (right panel). The dashed curve in each panel shows the ±1σ error on the stacked HI 21 cm spectrum. The bottom panels show the average HI 21 cm emission images of the same galaxies in the three M  B  subsamples, obtained by integrating the HI 21 cm emission over the central velocity channels (=180 km s−1 to +180 km s−1) of the stacked spectral cubes. The circle at the bottom left of each panel shows the 90 kpc spatial resolution of the images. The contour levels are at −3.0σ (dashed), +3.0σ, and +4.0σ significance; note that there are no −3σ features in the images. The average HI 21 cm emission signals from all three subsamples are seen to be clearly detected in both the spectra and the images.
Paper: The HI Mass Function of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The redshift distributions of the galaxies in the three M  B  subsamples, shown in blue. The distributions have been normalized by the total number of subcubes in each subsample. The HI 21 cm subcubes of each M  B  subsample were assigned weights such that the effective redshift distribution of each subsample is identical to the redshift distribution of the faint M  B  subsample (orange histograms). The number of galaxies in each subsample is indicated in each panel, with the number of HI 21 cm subcubes shown in parentheses.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Spectral resolution as a function of the wavelength coverage allowed by the NIRSpec + MIRI data. The observed data are represented by the black lines. The five models are depicted by the colored lines: ATMO in green, Exo-REM in blue, Sonora in yellow, BT-Settl in red, and DRIFT-PHOENIX in purple. For the models, the spectral resolution has been calculated assuming a Nyquist sampling rate.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Estimation of the T eff (left panel) and log(g) (right panel) using the full SED during the fit (dashed colored line) and using the spectral windows (colored dots). The size of the dots indicates the sensitivity of each spectral window to each parameter. If the sensitivity is too low to be represented by a dot, a colored cross is used. Each panel corresponds to a different model, with the parameter range indicated by the filled colored area. The final value and error extracted from these results are shown by the solid gray line and gray area, respectively. The dotted black lines represent the value estimated by Dupuy et al. (2023), who interpolated the evolutionary model from Saumon & Marley (2008) assuming the bolometric luminosity and age of VHS 1256 b. The two solutions they have found are given.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Same as Figure 3 but for the adiabatic index γ (left) and the sedimentation factor f sed (right).
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b
Authors: Simon Petrus, Niall Whiteford, Polychronis Patapis, Beth A. Biller, Andrew Skemer, Sasha Hinkley, Genaro Suárez, Paulina Palma-Bifani, Caroline V. Morley, Pascal Tremblin, Benjamin Charnay, Johanna M. Vos, Jason J. Wang, Jordan M. Stone, Mickaël Bonnefoy, Gaël Chauvin, Brittany E. Miles, Aarynn L. Carter, Anna Lueber, Christiane Helling, Ben J. Sutlieff, Markus Janson, Eileen C. Gonzales, Kielan K. W. Hoch, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Thomas Henning, Dean C. Hines, Callie E. Hood, Alex R. Howe, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Minjae Kim, Daniel Kitzmann, Adam L. Kraus, Masayuki Kuzuhara, Pierre-Olivier Lagage, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Jarron M. Leisenring, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Bruce Macintosh, Mathilde Mâlin, Elena Manjavacas, Sebastián Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Maxwell A. Millar-Blanchaer, Paul Mollière, Sarah E. Moran, Sagnick Mukherjee, Eric Pantin, Marshall D. Perrin, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Shrishmoy Ray, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Steph Sallum, Matthias Samland, Benjamin Sargent, Joshua E. Schlieder, Karl R. Stapelfeldt, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Malavika Vasist, Arthur Vigan, Kevin Wagner, Kimberly Ward-Duong, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Alice Zurlo, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou
Figure caption: Same as Figure 3 but for the [M/H] (left) and the C/O (right). The dotted black lines represent the solar values 0.0 and 0.55 for [M/H] and C/O, respectively.
Paper: Dramatic Drop in the X-Ray Polarization of Swift J1727.8–1613 in the Soft Spectral State
Authors: Jiří Svoboda, Michal Dovčiak, James F. Steiner, Philip Kaaret, Jakub Podgorný, Juri Poutanen, Alexandra Veledina, Fabio Muleri, Roberto Taverna, Henric Krawczynski, Maïmouna Brigitte, Sudeb Ranjan Datta, Stefano Bianchi, Teo Muñoz-Darias, Michela Negro, Nicole Rodriguez Cavero, Noel Castro Segura, Niek Bollemeijer, Javier A. García, Adam Ingram, Giorgio Matt, Edward Nathan, Martin C. Weisskopf, Diego Altamirano, Luca Baldini, Fiamma Capitanio, Elise Egron, Razieh Emami, Kun Hu, Lorenzo Marra, Guglielmo Mastroserio, Pierre-Olivier Petrucci, Ajay Ratheesh, Paolo Soffitta, Francesco Tombesi, Yi-Jung Yang, Yuexin Zhang
Figure caption: Evolution of Swift J1727.8–1613 on the hardness–intensity diagram spanning from 2023 August 24 to 2024 February 23. The plot shows the ratio of the photon flux between the 4–10 and 2–4 keV bands against the photon flux in the 2–20 keV range, as determined from the MAXI “on-demand” archive with a default 3 day time bin. The black stars, labeled 1–5, denote the initial five observations by IXPE that are described in Ingram et al. (2023) and Veledina et al. (2023). The red triangles (labeled 6 and 7) indicate the location in the diagram corresponding to the new IXPE observations examined in this study, showing Swift J1727.8–1613 still in the soft state.
Paper: Dramatic Drop in the X-Ray Polarization of Swift J1727.8–1613 in the Soft Spectral State
Authors: Jiří Svoboda, Michal Dovčiak, James F. Steiner, Philip Kaaret, Jakub Podgorný, Juri Poutanen, Alexandra Veledina, Fabio Muleri, Roberto Taverna, Henric Krawczynski, Maïmouna Brigitte, Sudeb Ranjan Datta, Stefano Bianchi, Teo Muñoz-Darias, Michela Negro, Nicole Rodriguez Cavero, Noel Castro Segura, Niek Bollemeijer, Javier A. García, Adam Ingram, Giorgio Matt, Edward Nathan, Martin C. Weisskopf, Diego Altamirano, Luca Baldini, Fiamma Capitanio, Elise Egron, Razieh Emami, Kun Hu, Lorenzo Marra, Guglielmo Mastroserio, Pierre-Olivier Petrucci, Ajay Ratheesh, Paolo Soffitta, Francesco Tombesi, Yi-Jung Yang, Yuexin Zhang
Figure caption: Light curve between 2 and 8 keV of the two IXPE observations, showing the decreasing count rate (upper panel) and roughly steady hardness (lower panel) within measurement uncertainties during the observations. The time bin in both panels is 1 ks; hardness is defined as the ratio of the counting rate in the 4–8 keV and 2–4 keV energy ranges.
Paper: Dramatic Drop in the X-Ray Polarization of Swift J1727.8–1613 in the Soft Spectral State
Authors: Jiří Svoboda, Michal Dovčiak, James F. Steiner, Philip Kaaret, Jakub Podgorný, Juri Poutanen, Alexandra Veledina, Fabio Muleri, Roberto Taverna, Henric Krawczynski, Maïmouna Brigitte, Sudeb Ranjan Datta, Stefano Bianchi, Teo Muñoz-Darias, Michela Negro, Nicole Rodriguez Cavero, Noel Castro Segura, Niek Bollemeijer, Javier A. García, Adam Ingram, Giorgio Matt, Edward Nathan, Martin C. Weisskopf, Diego Altamirano, Luca Baldini, Fiamma Capitanio, Elise Egron, Razieh Emami, Kun Hu, Lorenzo Marra, Guglielmo Mastroserio, Pierre-Olivier Petrucci, Ajay Ratheesh, Paolo Soffitta, Francesco Tombesi, Yi-Jung Yang, Yuexin Zhang
Figure caption: Spectral fit of NICER (black), NuSTAR (FPMA in red, FPMB in green), and IXPE (orange, blue, and violet) data. The upper panel shows the data counts, and the lower one shows data residuals from the best-fit model.
Paper: Dramatic Drop in the X-Ray Polarization of Swift J1727.8–1613 in the Soft Spectral State
Authors: Jiří Svoboda, Michal Dovčiak, James F. Steiner, Philip Kaaret, Jakub Podgorný, Juri Poutanen, Alexandra Veledina, Fabio Muleri, Roberto Taverna, Henric Krawczynski, Maïmouna Brigitte, Sudeb Ranjan Datta, Stefano Bianchi, Teo Muñoz-Darias, Michela Negro, Nicole Rodriguez Cavero, Noel Castro Segura, Niek Bollemeijer, Javier A. García, Adam Ingram, Giorgio Matt, Edward Nathan, Martin C. Weisskopf, Diego Altamirano, Luca Baldini, Fiamma Capitanio, Elise Egron, Razieh Emami, Kun Hu, Lorenzo Marra, Guglielmo Mastroserio, Pierre-Olivier Petrucci, Ajay Ratheesh, Paolo Soffitta, Francesco Tombesi, Yi-Jung Yang, Yuexin Zhang
Figure caption: Dependence of the PD on inclination. The red lines correspond to the models of Comptonization in the flat static hot flow with the seed photons either being internal synchrotron (solid line) or from the outer truncated disk (dotted line), corresponding to the models B and C in Poutanen et al. (2023), respectively. The blue lines are for the same models but for the hot flow outflowing with velocity v = 0.4c. The horizontal orange strip marks the observed PD of 4% during the hard state. The inclinations in the range ∼25°–35° are consistent with this PD. The black dashed line is the classical result for the electron-scattering dominated semi-infinite atmosphere (Chandrasekhar 1960; Sobolev 1963) that could correspond to the soft state. The horizontal cyan strip marks the allowed range of the PD during the soft state for the PA perpendicular to that of the hard state (i.e., corresponding to the negative PD).
Paper: Dramatic Drop in the X-Ray Polarization of Swift J1727.8–1613 in the Soft Spectral State
Authors: Jiří Svoboda, Michal Dovčiak, James F. Steiner, Philip Kaaret, Jakub Podgorný, Juri Poutanen, Alexandra Veledina, Fabio Muleri, Roberto Taverna, Henric Krawczynski, Maïmouna Brigitte, Sudeb Ranjan Datta, Stefano Bianchi, Teo Muñoz-Darias, Michela Negro, Nicole Rodriguez Cavero, Noel Castro Segura, Niek Bollemeijer, Javier A. García, Adam Ingram, Giorgio Matt, Edward Nathan, Martin C. Weisskopf, Diego Altamirano, Luca Baldini, Fiamma Capitanio, Elise Egron, Razieh Emami, Kun Hu, Lorenzo Marra, Guglielmo Mastroserio, Pierre-Olivier Petrucci, Ajay Ratheesh, Paolo Soffitta, Francesco Tombesi, Yi-Jung Yang, Yuexin Zhang
Figure caption: Contour plot of the PD vs. PA derived from the final spectral fit with applied polconst on the best-fit model to fit the Q and U spectra. The contours show 1σ (red), 2σ (green), and 3σ (blue) confidence levels. The best-fit values are marked with a black plus sign.
Paper: Dramatic Drop in the X-Ray Polarization of Swift J1727.8–1613 in the Soft Spectral State
Authors: Jiří Svoboda, Michal Dovčiak, James F. Steiner, Philip Kaaret, Jakub Podgorný, Juri Poutanen, Alexandra Veledina, Fabio Muleri, Roberto Taverna, Henric Krawczynski, Maïmouna Brigitte, Sudeb Ranjan Datta, Stefano Bianchi, Teo Muñoz-Darias, Michela Negro, Nicole Rodriguez Cavero, Noel Castro Segura, Niek Bollemeijer, Javier A. García, Adam Ingram, Giorgio Matt, Edward Nathan, Martin C. Weisskopf, Diego Altamirano, Luca Baldini, Fiamma Capitanio, Elise Egron, Razieh Emami, Kun Hu, Lorenzo Marra, Guglielmo Mastroserio, Pierre-Olivier Petrucci, Ajay Ratheesh, Paolo Soffitta, Francesco Tombesi, Yi-Jung Yang, Yuexin Zhang
Figure caption: Modeling PD and PA with relativistic accretion disk model kynbbrr for different black hole spin values, a = 0 (violet), a = 0.87 (green), and a = 0.998 (orange), considering albedo A = 0 (dashed lines) and A = 1 (solid lines). Values for inclinations of 20°, 40°, and 60° are denoted by bullets. Corresponding upper limits for inclination are taken from the intersections with the 3σ contour line. The black bullet shows the case of a = 0.87 and inclination i = 40°, corresponding to the best-fit spectral results, and it is very close to the best-fit values of PD and PA from the IXPE data (denoted by a black plus sign).
Paper: Dramatic Drop in the X-Ray Polarization of Swift J1727.8–1613 in the Soft Spectral State
Authors: Jiří Svoboda, Michal Dovčiak, James F. Steiner, Philip Kaaret, Jakub Podgorný, Juri Poutanen, Alexandra Veledina, Fabio Muleri, Roberto Taverna, Henric Krawczynski, Maïmouna Brigitte, Sudeb Ranjan Datta, Stefano Bianchi, Teo Muñoz-Darias, Michela Negro, Nicole Rodriguez Cavero, Noel Castro Segura, Niek Bollemeijer, Javier A. García, Adam Ingram, Giorgio Matt, Edward Nathan, Martin C. Weisskopf, Diego Altamirano, Luca Baldini, Fiamma Capitanio, Elise Egron, Razieh Emami, Kun Hu, Lorenzo Marra, Guglielmo Mastroserio, Pierre-Olivier Petrucci, Ajay Ratheesh, Paolo Soffitta, Francesco Tombesi, Yi-Jung Yang, Yuexin Zhang
Figure caption: Measured 2–8 keV average PD in all IXPE observations vs. the spectral hardness defined as the flux ratio between the 4–8 and 2–4 keV energy bands measured by IXPE. The new observations 6 and 7 combined (marked in red) are plotted as an upper limit calculated at the 99% confidence level.