adsabs/AstroCLIMB huggingface dataset:
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Broadband and spectroscopic light-curve fits of the NIRSpec G395H transit of TOI-270 b, extracted with exoTEDRF. The top panel is a schematic of TOI-270 b (blue) and d (red) as they transit across the stellar disk at time t = 2460222.265 BJD, illustrating their trajectories (dashed lines) and the 1σ confidence region corresponding to their orbital inclination uncertainties. The broadband light-curve fits (white) are shown for the NRS1 and NRS2 detectors, along with eight systematics-corrected spectroscopic light curves (colored dots) and their best-fit transit models (black lines). The light curves are plotted with a relative flux offset and are binned in time in groups of 75 data points (corresponding to 13.6 minutes bins). The best-fit model transit of TOI-270 d, whose position is indicated by the gray dashed lines, partially overlaps with that of TOI-270 b and is removed from the data and best-fit model for visual clarity. All light curves are well behaved and show Gaussian distributions in their residuals (computed from the nonbinned light curves; right).
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Coupled atmosphere–interior evolution modeling shows that a diversity of atmospheric outcomes are consistent with observational constraints. The PACMAN-P geochemical evolution model (J. Krissansen-Totton et al. 2024) was used to explore plausible evolutionary scenarios for TOI-270 b. This model explicitly couples magma ocean solidification, speciation of C-, H-, O-, and Fe-bearing species, stellar evolution, thermal escape, and radiative-convective climate. Subpanels represent scenarios whereby hydrogen escape causes a transition to an O2–H2O atmosphere (top), an H2O-dominated atmosphere (middle), and a case where an H2-dominated atmosphere is retained (bottom). The internal volatile reservoirs of the planet are not shown.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Position of TOI-270 b relative to the cosmic shoreline. Escape velocity and cumulative XUV irradiation are computed using the scaling of K. J. Zahnle & D. C. Catling (2017) for all known exoplanets with equilibrium temperatures below 1000 K, radii smaller than 1.8 R⊕, and masses measured to higher than 20% precision (data taken from the NASA Exoplanet Archive; R. L. Akeson et al. 2013). The blue dashed line indicates the position of the cosmic shoreline shown in K. J. Zahnle & D. C. Catling (2017), and we add a shaded region corresponding to a factor of 4 uncertainty in XUV irradiation, as in Q. Xue et al. (2024). The solar system telluric planets are shown for comparison, and we also indicate the position of TRAPPIST-1 b (T. P. Greene et al. 2023), TRAPPIST-1 c (S. Zieba et al. 2023), GJ 1132b (Q. Xue et al. 2024), GJ 486 b (M. W. Mansfield et al. 2024), and LTT 1445 Ab (P. Wachiraphan et al. 2025), which have all been found to be consistent with a dark, bare-rock scenario from JWST thermal emission observations. However, some of these targets, such as TRAPPIST-1 c (S. Zieba et al. 2023), remain consistent with a variety of atmospheric scenarios. The two sub-Neptunes of the TOI-270 system, planets c and d, are also shown for comparison with planet b.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Constraints on the water mole fraction and effective surface pressure from the free-chemistry retrieval without TLS. The color represents the normalized posterior probability density from the retrieval assuming no TLS effect, and the full black lines indicate the 1σ, 1.5σ, 2σ, and 3σ confidence intervals. The dashed lines represent those same confidence intervals for the retrieval where we assume as a prior the TLS parameter constraints from the retrieval on TOI-270 d.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: The NIRSpec G395H transmission spectrum of TOI-270 b (black circles, binned at a fixed resolving power of R = 80 for visual clarity) is well fit by either an H2O-rich atmosphere or stellar contamination. The median fit of the atmosphere-only (X + H2O) and bare-rock + TLS retrievals, along with their 1/2σ confidence regions, are shown in blue and orange, respectively. The atmosphere and TLS effect models are similar over the NIRSpec G395H wavelength range, with the difference between these two effects being more easily discernible toward optical wavelengths.
Paper: Possible Evidence for the Presence of Volatiles on the Warm Super-Earth TOI-270 b
Authors: Louis-Philippe Coulombe, Björn Benneke, Joshua Krissansen-Totton, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Michael Radica, Pierre-Alexis Roy, Eva-Maria Ahrer, Charles Cadieux, Yamila Miguel, Hilke E. Schlichting, Elisa Delgado-Mena, Christopher Monaghan, Hanna Adamski, Eshan Raul, Ryan Cloutier, Thaddeus D. Komacek, Jake Taylor, Cyril Gapp, Romain Allart, François Bouchy, Bruno L. Canto Martins, Neil J. Cook, René Doyon, Thomas M. Evans-Soma, Pierre Larue, Alejandro Suárez Mascareño, Joost P. Wardenier
Figure caption: Corner plot of the spot covering fraction and spot contrast from the bare-rock + free TLS retrieval on TOI-270 b (blue), and the atmosphere + free TLS retrieval on TOI-270 d (red). Owing to its larger size, the atmospheric retrieval on TOI-270 d is much more constraining regarding the TLS parameters and is able to rule out significant contamination from the star. Moreover, the range of fspot and ΔTspot values needed for TLS to explain TOI-270 b’s spectrum is significantly disfavored by the constraints from TOI-270 d.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Planetary SED (left) and the corresponding signature in the differential output (right) for an instrument and observation as specified in Table 1. Top: unit SED. The impact of shot noise is visible at the lower wavelengths. Center: blackbody spectrum for Tp = 254 K. Compared to the unit SED, one can clearly see the reduction in signal at the lower wavelengths. Bottom: Earth spectrum. Again, the absorption bands in the atmosphere cause a clear reduction in signal at the corresponding wavelengths. Note that different time-step binning is used than in Figure 4, explaining the different values of the color bar.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Comparison of the 1σ uncertainties of the estimated planetary SED derived from the diagonal terms of Equation (35) for the different scenarios. To ensure comparability, it is assumed here that the correct planet position is known a priori, even for the optimistic unwhitened case. Top: the black dashed line shows the true planetary spectrum, and the shaded areas indicate the uncertainties obtained from averaging over 50 simulated observations. Significant differences are seen below ∼10 μm. Bottom: the 1σ uncertainties of the optimistic whitened, optimistic unwhitened, and pessimistic whitened cases, normalized by the ideal uncertainty. Results for the pessimistic unwhitened scenario are not shown, as the algorithm was not able to converge.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Estimated SED for the optimistic scenario without data whitening (top) and with data whitening (bottom), assuming the true planet position is known a priori. Apart from the larger uncertainties in the non-whitened case, the SED values at shorter wavelengths show prominent systematic errors. These systematics are significantly reduced after the whitening.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Distribution of the test statistics, TED (left two plots) and TNP (right two plots), under the null hypothesis, ﹩{{ \mathcal H }}_{0}﹩, and alternative hypothesis, ﹩{{ \mathcal H }}_{1}﹩, for the optimistic scenario with and without whitening. A PFA = 0.00135 corresponding to a 3σ detection is assumed. The empirical results are calculated for a sample of 500 simulated observations of our target system. The bootstrapped results are sampled from a multivariate normal distribution following the considered instrumental error covariance, Σref.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Illustrative example of the correlation matrix corresponding to the covariance matrix defined in Equation(35), averaged over 100 runs. The color map is capped at ±0.08, to increase the visibility of the smaller features. This pattern is similar to the covariance of the planetary signal as shown in Figure 4 (top).
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Correlations between the estimated planetary SED and sky coordinates. The correlations generally depend on the position of the planet and may look differently in other cases.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Correlation maps of the Earth-like planet around an M star for the ideal (left), optimistic unwhitened (center), and optimistic whitened (right) cases.
Paper: Robust Data Interpretation for Perturbed Nulling Interferometers via Proper Handling of Correlated Errors
Authors: Philipp A. Huber, Felix A. Dannert, Romain Laugier, Taro Matsuo, Loes W. Rutten, Adrian M. Glauser, Sascha P. Quanz
Figure caption: Additional examples of extracted planetary SEDs with corresponding uncertainties for the optimistic unwhitened case, all showing clear systematic errors below ∼10 μm. Variations among the different panels stem from the random instantiations of the instrumental perturbations.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Comparison of the theoretical RV curve with the observation for HY Vir and V1031 Ori (top panels). The red diamonds are the observational data, while the other black symbols are the literature data from C. H. Sandberg Lacy & F. C. Fekel (2011) for HY Vir and from J. Andersen et al. (1990) for V1031 Ori. The middle and bottom panels represent the residuals between the observation and theoretical RV variation for primary (star showing eclipse at deep minimum) and secondary (star showing eclipse at shallow minimum) stars, respectively.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Comparison of the theoretical RV curve with the observations for HD 117476 and 205 Dra (top panels). The middle and bottom panels represent the residuals between the observation and theoretical RV variation for primary (star showing eclipse at deep minimum) and secondary (star showing eclipse at shallow minimum) stars (see also Table 5), respectively.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Chemical abundance distributions of the binary components relative to solar abundance (M. Asplund et al. 2009). The subscripts “p” and “s” represent the primary and secondary components, respectively. Abundances from five or more lines are shown with filled symbols, while open symbols indicate fewer than five lines.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: Top panels: the theoretical binary models (red solid lines) fit to the TESS photometric data of the target systems. Bottom panels: residuals.
Paper: Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip
Authors: Filiz Kahraman Aliçavuş, Fahri Aliçavuş, Zeynep Çelik Orhan, Eda Çelik, Giovanni Catanzaro, Marina Giarrusso
Figure caption: The theoretical composite spectra (red line) fit the observed Hα lines (black lines). The blue and yellow lines represent the theoretical spectra of the primary (star showing eclipse at deep minimum) and secondary (star showing eclipse at shallow minimum) components (see also Table 5) of each eclipsing binary system. The light-green line in the V1031 Ori panel displays the synthetic spectra of third component.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Histogram of height from the Galactic plane for identified MCs (top), plot of height vs. the Galactic longitude (middle), and plot of height vs. galactocentric distance (bottom) in different segments of the Galactic disk. The disk segments are divided at galactocentric distances where the number of MCs reaches a local minimum for the G120 and G50 regions, respectively. MCs in the segments are primarily distributed along the known spiral arms; nevertheless, there are also MCs located in the adjacent inter-arm regions. The segments are named after the spiral arms in them and are labeled in the upper-right corner of the panels. The Local–G50 and Sagittarius–G50 segments are divided by the heliocentric distance, rather than the galactocentric distance, at the minimum number of MCs. The height of the Sun above the Galactic midplane is taken as 15.7 pc (Y. Su et al. 2019; X. Zhou et al. 2023) to fix the position of the Galactic plane. The histograms of the heights from the Galactic plane are weighted by the logarithm of mass, by summing the log(M) of each cloud in each bin. Each bin of the histogram contains at least nine MCs. The histograms are fitted with Gaussian functions, and the results of the Gaussian fit are shown by black dotted lines. The corresponding Gaussian parameters are indicated in the upper-right corner of the top panels. In the middle and bottom panels, each spot represents a sample of nine MCs. Black solid lines indicate the running mean of zgal, and the deep and light gray shaded areas indicate the 1σ and 2σ ranges, respectively. The zgal = 0 plane is shown by the black dotted lines for reference. The red dots mark the same MCs as those indicated by the red crosses in Figure 8.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Systemic velocity vs. the Galactic longitude for identified MCs in the G120 (left) and G50 (right) regions. The sizes of the circles indicate the physical sizes of the MCs (see Table 2). MCs that are not fully resolved (i.e., those with a longitude or latitude span of two pixels) are not shown here. The 10 pc size used as a reference is shown in the lower left corner of the left panel and in the upper left corner of the right panel. The red circles mark the same selected MCs as those indicated by the red crosses in Figure 8. The extensions of the G50 Perseus–Outer inter-arm spurs are indicated by blue solid lines. The approximate locations of the spiral arms resemble those in Figures 3 and 4. Here, the Outer and OSC arms are labeled and more clearly visible. The Perseus arm in the G120 region is labeled as well, which has a relatively large velocity span, from approximately −75 to −30 km s−1. The gray solid line is the same as that shown in Figure 4, which follows the upper velocity limit well.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Kinematic distance of each identified MC in the G120 (left) and G50 (right) regions as a function of systemic velocity. The kinematic distances of the MCs are derived from the Galactic rotation curve of J. Brand & L. Blitz (1993) with the Sun’s galactocentric distance of 8.15 kpc and the circular rotation speed of 236 km s−1 (M. J. Reid et al. 2019). For MCs with positive systemic velocities in the G50 region, based on the rotation curve, one velocity corresponds to two distances, near and far, so we apply a full distance–probability density function method (M. J. Reid et al. 2016, 2019) to calculate the distance instead (see Section 3.3 for details). MCs in the velocity range from −55 to −30 km s−1 in the G120 region are marked as red crosses in the left panel, which are probably located in the Perseus arm spiral shock region. MCs with velocities ranging from −23 to −7 km s−1 and Galactic longitudes ranging from 48° to 53﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 are labeled with red crosses in the right panel, which are in substructures within the inter-arm region between the Perseus and Outer arms, referred to as the G50 Perseus–Outer inter-arm spurs.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Histogram of modified systemic velocities for MCs in different segments of the Galactic disk. The systemic velocity of the MCs is modified by subtracting the baseline of velocity changes with the Galactic longitude for each disk segment, to eliminate the trend of velocity variations along the Galactic longitude. The baseline is obtained from a linear fit of the velocity variation with the Galactic longitude. The disk segments are the same as those identified in Figures 12 and 13, and the names are marked in the upper-right corner of each panel. The histograms are weighted by the logarithm of mass, in the same way as in Figures 12 and 13. The histograms are fitted with Gaussian functions, and the results of the Gaussian fit are shown by black dotted lines. Due to insufficient samples in the Local–G50 and OSC–G50 segments, the center and deviation of the Gaussian functions are determined as the mean and deviation of the modified velocities, respectively, weighted by the logarithm of mass. The corresponding Gaussian parameters are indicated in the upper-right corner of each panel.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Histogram of radius (left) and radius–mass relation (right) for the MWISP clouds, overplotted with those for clouds from other literature catalogs, i.e., GRS (13CO (J = 1–0); J. M. Rathborne et al. 2009; J. Roman-Duval et al. 2009, 2010), COHRS (12CO (J = 3–2); D. Colombo et al. 2019), CHIMPS (13CO and C18O (J = 3–2); A. J. Rigby et al. 2019), and SEDIGISM (13CO (J = 2–1); A. Duarte-Cabral et al. 2021). The radius of the clouds is the HWHM, except for the GRS clouds. The radius of the GRS clouds is the equivalent radius estimated by the emission area, which is larger than the HWHM radius. In the right panel, the density of points for the MWISP sample is shown in a square root scale. The other samples are shown by blue points (GRS), green triangles (SEDIGISM), red plusses (CHIMPS), and brown crosses (COHRS). For better visibility, only two hundred randomly selected clouds from each sample are shown. Linear fits to the radius–mass relationship are performed on the full sample from each catalog. The fitting results are shown by solid lines, and the corresponding linear functions are indicated in the upper-left corner.