adsabs/AstroCLIMB huggingface dataset:
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Relation between the recovered and planted magnitude of Sgr A*-NIR obtained with star-planting simulations for three example frames in 2022 August 20: two in the ﹩K^{\prime} ﹩ band (left panel), one in the H band (right panel). Sgr A* is confused with S0-38 for this epoch. The median and confidence interval are determined by randomly sampling the magnitude and location of S0-38, from a distribution informed by unconfused observations. Since the confusing source adds to the detected flux, we have m rec ≤ m plant. This flux contribution depends on the PSF: in ﹩K^{\prime} ﹩, the frame with a low Strehl ratio (S ≈ 0.2, i.e., close to the cut; see Appendix B) shows larger deviations of m rec from m plant than the frame with a relatively high Strehl ratio (S ≈ 0.45). Fainter than some magnitude ﹩{m}_{\mathrm{lim}}﹩ (shown in red for the H-band frame), the confusion correction becomes ambiguous since a recovered magnitude m rec would not correspond to a unique m plant value. We note that the curves have been slightly smoothed for the sake of visualization.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Same as the bottom panel of Figure 1, but for the other epochs of our data set (from top to bottom: 2005 July 31, 2019 May 13, 2022 May 25, 2022 August 16, 2022 August 19, and 2022 August 20). We also show the lightcurves before confusion correction (except for 2019 May 13 since Sgr A*-NIR is not confused with any known source). The lightcurves (with flux/magnitude values with uncertainties, before/after confusion correction) are also available as a machine-readable table.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Comparison between the uncertainties added during the confusion correction step and the uncertainties added during the interpolation step, as a function of ﹩K^{\prime} ﹩ magnitude. Interpolation tends to add more uncertainty for brighter points, but as Sgr A*-NIR gets fainter the uncertainty added by confusion correction starts to dominate.
Paper: New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Authors: Hadrien Paugnat, Tuan Do, Abhimat K. Gautam, Gregory D. Martinez, Andrea M. Ghez, Shoko Sakai, Grant C. Weldon, Matthew W. Hosek, Zoë Haggard, Kelly Kosmo O'Neil, Eric E. Becklin, Gunther Witzel, Jessica R. Lu, Keith Matthews
Figure caption: Distribution of normalized leave-one-out errors for the MOGP interpolation (all epochs combined).
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: Top: the multiband light curves of the microlensing event ASASSN-22av, which are well described by the best-fit 2L1S model (black solid line) from the joint VLTI and light-curve analysis. The light curves deviate from the best-fit 1L1S model with finite-source effects (black dashed line) near the peak, as shown with the enlarged view in the inset. We analyze three nights of VLTI GRAVITY observations taken after the peak, and their epochs are marked with the red dashed lines. Middle: the residuals of the best-fit 2L1S model. Bottom: the best-fit 1L1S model shows significant residuals for the ∼10 days around the peak.
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: The observed (black) and fitted (red) synthetic HERMES spectra from GALAH DR4, showing generally good agreement and small residuals (blue) across the entire spectrum. While some individual lines are deviating, the overall fit is well aligned with the observations, whose continuum is suppressed by molecular absorption features across the entire wavelength region of this luminous cool giant star.
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: The source trajectories and light curves of three 2L1S models (“wide A−,” “wide B+,” and “close A−”) taking the microlens parallax and binary orbital motion into account. Left: the upper, middle, and lower subpanels show the caustics (blue) and source trajectories (black curves with arrows) for the “wide A−” (best-fit), “wide B+,” and “close A−” solutions, respectively. In each subpanel, we show the source positions (red circles) and caustics at ﹩\mathrm{HJD}^{\prime} =9300﹩ and 9601, with increased opacity for the latter. The inset of each subpanel displays the source positions and caustics on the three nights of the VLTI GRAVITY observations. Right: the Gaia G-band light curve shows a broad feature at ﹩\mathrm{HJD}^{\prime} \sim 9300﹩, and the three best-fit 2L1S models are shown with solid (wide A−), dashed (wide B+), and dotted (close A−) lines, respectively. The wide solutions can match this feature well, while the “close A−” solution cannot. The sharply peaked spike of the “close A−” solution is induced by the source crossing a planetary caustic due to dramatic orbital motions, but even this finely tuned configuration fails to reproduce the observed feature.
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: Four × two-panel groups showing the closure-phase data and the best-fit microlensing model (“wide A−”) for the eight VLTI GRAVITY exposures obtained over three nights. Within each group, the left subpanel shows the closure-phase data as a function of wavelength, with the best-fit model overplotted as solid lines; the right subpanel shows the caustics (blue), source trajectory (black line with an arrow), and source position (red circle) at the time of the VLTI observation, with the microlensed images displayed as shaded regions and the critical curves as blue dashed lines.
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: The comparisons of α LC derived from light-curve fitting with α VLTI inferred from VLTI data. The colored arcs denote the 1σ range of α LC for the solutions “close A+” (black), “close A−” (red), “close B+” (cyan), “wide A+” (blue), “wide A−” (green), and “wide B+” (yellow), respectively. The shaded regions indicate the 3σ range of α VLTI at Ψ ∼ −100°, −10°, 80°, and 170°. Three solutions (“wide A−,” “wide B+,” and “close A−”) have consistent α LC with α VLTI.
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: The 1σ and 2σ posterior distributions of the microlens parallax vector  π  E = (π E,E, π E,N) from light-curve analysis for the “close A+” (red contours), “close B+” (cyan contours), “wide A−” (green contours), and “wide B+” (yellow contours) solutions, respectively. The shaded regions are the 1σ, 2σ, and 3σ constraints on Φ π  derived from the interferometric data for the local minimum of Ψ ∼ −100°. The light-curve and VLTI constraints are consistent for the “wide A−,” “wide B+,” and “close A−” solutions.
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: The source trajectory (black solid line) and caustics (blue closed curves) for the “wide A−” (top panel), “wide B+” (middle panel), and “close A−” (bottom panel) solutions. The solid dots denote the source positions on the three nights of VLTI GRAVITY observations. The 3σ contours in magenta show the posteriors of the source positions inferred from the interferometric data only, with the geometric parameters (s, q, ρ, θ E, Ψ) held fixed to the values in Table 2.
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: Left: the ﹩{\rm{\Delta }}{\chi }_{\mathrm{tot}}^{2}({\theta }_{{\rm{E}}},{\rm{\Psi }})﹩ map from fitting the VLTI data evaluated at (s, q, ρ) = (3.8, 0.84, 0.044). Areas with Δχ 2 < 30, 120, 270, 480, and Δχ 2 > 480 are color-coded in red, yellow, green, blue, and gray, respectively. There are four local minima around Ψ = (170°, 80°, −10°, −​​​​100°). Right: images and geometry of the four local minima. The four rows from top to bottom correspond to local minima at Ψ = 170° (blue), 80° (black), −10°(green), and −100°(red), respectively. The first three columns show the model images oriented in the east and north directions on the three VLTI nights. The last column shows the source positions (solid dots) on the three VLTI nights and the caustics (black closed curve).
Paper: First Resolution of Microlensed Images of a Binary-lens Event
Authors: Zexuan Wu, Subo Dong, A. Mérand, Christopher S. Kochanek, Przemek Mróz, Jinyi Shangguan, Grant Christie, Thiam-Guan Tan, Thomas Bensby, Joss Bland-Hawthorn, Sven Buder, Frank Eisenhauer, Andrew P. Gould, Janez Kos, Tim Natusch, Sanjib Sharma, Andrzej Udalski, J. Woillez, David A. H. Buckley, I. B. Thompson, Karim Abd El Dayem, Anthony Berdeu, Jean-Philippe Berger, Guillaume Bourdarot, Wolfgang Brandner, Richard I. Davies, Denis Defrère, Catherine Dougados, Antonia Drescher, Andreas Eckart, Maximilian Fabricius, Helmut Feuchtgruber, Natascha M. Förster Schreiber, Paulo Garcia, Reinhard Genzel, Stefan Gillessen, Gernot Heißel, Sebastian Hönig, Mathis Houlle, Pierre Kervella, Laura Kreidberg, Sylvestre Lacour, Olivier Lai, Romain Laugier, Jean-Baptiste Le Bouquin, James Leftley, Bruno Lopez, Dieter Lutz, Felix Mang, Florentin Millour, Miguel Montargès, Hugo Nowacki, Mathias Nowak, Thomas Ott, Thibaut Paumard, Karine Perraut, Guy Perrin, Romain Petrov, Pierre-Olivier Petrucci, Nicolas Pourre, Sebastian Rabien, Diogo C. Ribeiro, Sylvie Robbe-Dubois, Matteo Sadun Bordoni, Daryl Santos, Jonas Sauter, Jules Scigliuto, Taro T. Shimizu, Christian Straubmeier, Eckhard Sturm, Matthias Subroweit, Calvin Sykes, Linda Tacconi, Frédéric Vincent, Felix Widmann
Figure caption: Δχ 2 map for the grid search of 2L1S light-curve models, in the ﹩\mathrm{log}s-\mathrm{log}q﹩ (upper panel) and ﹩\mathrm{log}s-\alpha ﹩ (lower panel) planes. For ﹩\mathrm{log}s\lt 0﹩, there is a perfect degeneracy ﹩(\mathrm{log}q,\alpha )\to (-\mathrm{log}q,\alpha +\pi )﹩, and thus the search is only conducted with ﹩\mathrm{log}q\leqslant 0﹩. The regions with Δχ 2 < 30, 120, 270, 480, and >480 with respect to the best fit are color-coded with red, yellow, green, blue, and light gray, respectively.
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: Panel (a): position of the visible star on the Hertzsprung–Russell diagram for J0606+2132. The gray points are plotted for a comparison, which are from Gaia EDR3 with distances d < 100 pc, G mag between 4 and 18 mag, and Galactic latitudes ∣b∣ > 20. No extinction correction was done for these stars. Panel (b): SED fitting of J0606+2132. The black line is the best model. Panel (c): comparison of flux-calibrated Gaia BP/RP (XP) spectrum (solid black line) and the PHOENIX template (T eff = 10,000 K, ﹩\mathrm{log}\,g=3.5﹩ dex, [Fe/H] = 0; red line). The flux of the template has been normalized to the distance of J0606+2132, taking extinction into account. The dashed line is the combined spectrum of PHOENIX templates of the visible star and a main-sequence star with a mass of 1.34 M ⊙ (T eff = 6600 K, ﹩\mathrm{log}\,g=4.5﹩ dex, [Fe/H] = 0). Panel (d): comparison of the mean LAMOST MRS (black line) and the PHOENIX template (T eff = 10,000 K, ﹩\mathrm{log}\,g=3.5﹩ dex, [Fe/H] = 0, v sin i = 67 km s−1; red line; R ≈ 7500).
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: Left panel: folded RV curve with a period of 2.7735540 days. The phases of the inferior conjunction (ϕ = 0 or 1), quadrature (ϕ = 0.25 and 0.75), and superior conjunction ϕ = 0.5 are marked with vertical gray lines. The RV data are determined from the LAMOST LRS (green dots) and MRS (red dots for S/N r  > 50; gray diamonds for S/N r  < 50). Right panel: PHOEBE fitting (red line) to the normalized LCs from TESS. The blue dashed line represents the maximum flux at ϕ = 0.75, whereas the green dashed line represents the maximum flux at ϕ = 0.25. The asymmetric peaks are caused by Doppler boosting.
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: Left panels: evolutionary tracks of the selected BPASS models in Hertzsprung–Russell diagrams. The orange lines show the time steps where RLOF is occurring in these models. The black stars mark the position of J0606+2132. The blue squares are the models matching the search criteria. Middle panels: evolution of the masses for both components in models. The orange areas represent the evolutionary stages of RLOF. Right panels: evolution of the binary separation and the radii of the visible stars. The orange areas represent the evolutionary stages of RLOF.
Paper: A Massive White Dwarf or Low-mass Neutron Star Discovered by LAMOST
Authors: Xinlin Zhao, Song Wang, Pengfei Wang, Chuanjie Zheng, Haibo Yuan, Jifeng Liu
Figure caption: Period estimation of J0606+2132. Top panel: power spectrum of LS obtained from the TESS and ASAS-SN V- and g-band LCs. Bottom panel: the phase dispersion calculated with the TESS and ASAS-SN V- and g-band LCs. The red line marks the phase-dispersion minimum, corresponding to a period of 2.7735540 days.