adsabs/AstroCLIMB huggingface dataset:
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Top panel: metallicities of the Scl dSph members as a function of half-light radius/projected distance. Black points represent median [Fe/H]MAGIC values in bins of 0.5 rh. The black line represents a piecewise fit (inner fit: slope = −0.62 and intercept = −1.08; outer fit: slope = −0.10 and intercept = −1.63). The red line shows the segmented fit performed for the adjusted MAGIC metallicities, brought to the T23 scale. Bottom panel: metallicity gradients obtained in this work, along with previous estimates reported in the literature. We present metallicity gradients from E. N. Kirby et al. (2011, K11), R. Leaman et al. (2013, L13), N. Ho et al. (2015, H15), C. E. Martínez-Vázquez et al. (2016, MV16), S. Taibi et al. (2022, T22), and E. Tolstoy et al. (2023, T23).
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Top panels: median difference between MAGIC and T23 estimates in each bin used to calculate [Fe/H]adjusted, and residual plot after the adjustment of [Fe/H]MAGIC. Vertical bars correspond to the median absolute deviation. The number of stars comprising each bin is indicated. MΔ[Fe/H] indicates the median value. Bottom panel: MDFs for estimated MAGIC metallicities (thin blue line) and adjusted values ([Fe/H]adjusted, thick red line).
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Spatial distribution of Scl dSph members (small dots) and EMP candidates ([Fe/H]MAGIC < −3.0; diamonds) from our MAGIC photometric metallicity data.
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Cumulative distribution functions (CDFs) for the Scl dSph members at different metallicity intervals.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: Schematic diagram of the power spectral density as a function of wavenumber k, illustrating the energy-containing range with a power-law scaling of Ak−1, and an inertial range with a scaling of Bk−p. The wavenumber kc marks the spectral break between the energy-containing and inertial ranges, while kd denotes the spectral break between the inertial and dissipation ranges.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: The top left and right panels illustrate the magnetic Reynolds number and viscosity as functions of distance, with red dots representing near the Kolmogorov range (–1.71 ≤ index ≤ –1.63), and blue dots representing near the IK range (–1.54 ≤ index ≤ –1.46). The bottom left and right panels illustrate the ratios of Reynolds numbers (near Kolmogorov to IK) and viscosity (near Kolmogorov to IK). Vertical lines represent error bars and the dashed lines the fitted curves.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: The left and right panels show the Reynolds number and viscosity as functions of distance for different spectral index intervals. Blue symbols correspond to indices from −1.99 to −1.8, cyan symbols represent indices between −1.8 and −1.61, yellow symbols correspond to indices from −1.61 to −1.41, and red symbols to indices between −1.41 and −1.22.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: The top left and top right panels illustrate the magnetic Reynolds number and magnetic viscosity in the solar wind as a function of distance, with the color bar denoting the magnitude of the solar wind speed. The bottom left and right panels represent the same as in the top panels, but the color bar denotes the spectral indices.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: The inverse injection wavenumber, ﹩{k}_{\mathrm{inj}}^{-1}﹩, (left panel) and the proton gyroradius (right panel) as a function of distance. The color bar denotes the same as in Figure 2.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: PSP and SolO measured solar wind speed (top left), solar wind density (top right), magnitude of the magnetic field (bottom left), and Alfvén velocity (bottom right) as a function of distance. The color bar represents the magnitude of the solar wind speed.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: Fluctuating magnetic energy density (left panel) and the corresponding correlation length (right panel) as a function of distance. The color bar denotes the same as in Figure 2.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: Fluctuating kinetic energy (left panel) and the corresponding correlation length (right panel) as a function of distance. The color bar denotes the same as in Figure 2.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: Spectral indices of the velocity fluctuations in the inertial range as a function of distance from the Sun. The color bar denotes the same as in Figure 2.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: Spectral indices of the magnetic field fluctuations in the inertial range as a function of distance from the Sun. The color bar denotes the same as in Figure 2.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: All 57 systems sorted by ΔBIC between a linear transit timing model and a quadratic transit timing model. Systems with a positive ﹩\dot{P}﹩ are colored blue while systems with a negative ﹩\dot{P}﹩ are colored red. Furthermore, systems that passed the 3σ criterion and had ΔBIC > 10, and therefore show significant evidence of a decrease in orbital period over time, are outlined in orange. Bottom: zoom-in to better display ΔBIC of most systems.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit times in minutes as a function of time in days for CoRoT-2, showing our best-fit linear transit timing model and quadratic transit timing model in red and orange, respectively. The blue circles represent transit times obtained from IW22, the green circles represent transit times obtained from this work, and the red circles are the average transit times obtained from this work for each TESS sector and Kepler quarter. The shaded regions around the red and orange lines are 1σ uncertainties. Additionally, the dotted line represents the default orbital period reported by the NASA Exoplanet Archive.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Top: the SPOC light curve of TrES-3 from TESS Sector 25, with the best-fit transit model overplotted (red line). The time of each transit was fit independently. Bottom left: the light-curve data and transit model phase-folded at the measured orbital period. Bottom right: the residuals of the phase-folded light curve after subtracting the transit model, in parts per million (PPM).
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: The top left and right panels illustrate the kinetic Reynolds number and kinetic viscosity in the solar wind as a function of distance, with the color bar indicating the magnitude of the solar wind speed. The bottom left and right panels represent the same quantities as in the top panels, but the color bar represents the spectral indices.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: The top left and right panels illustrate the kinetic Reynolds number and viscosity near the Kolmogorov and IK scales. The bottom left and right panels illustrate the ratios of Reynolds numbers (near Kolmogorov to IK) and viscosity (near Kolmogorov to IK). Vertical lines represent error bars, and the dashed lines represent the fitted curves. The description of the figure is the same as in Figure 8.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Each individually fit transit for TrES-3. The transits are horizontally aligned based on the sector they were observed in, and stacked in order of time. The y-axis is relative flux.
Paper: Reynolds Number and Viscosity in the Solar Wind
Authors: Laxman Adhikari, Ashutosh Giri, Monika Karki, Prashant Baruwal, Prashrit Baruwal, Rubaiya Khondoker Shikha, Bigyan Mainali, Dessalegn Kenno, Ismita Tasnim, Gary P. Zank, Bingbing Wang, Lucien Treville, Sagar Ghimire
Figure caption: The left and right panels illustrate the kinetic Reynolds number and viscosity corresponding to different spectral index intervals as a function of distance. The description of the figure is the same as in Figure 7.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit time diagram for TrES-5.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Comparison between between our ﹩{Q}_{* }^{{\prime} }﹩ values (circles), our ﹩{Q}_{* }^{{\prime} }﹩ lower limits (red arrows), and theoretical estimates obtained by A. J. Barker (2020; orange crosses) and N. N. Weinberg et al. (2024; blue crosses). Systems with two theoretical estimates from N. N. Weinberg et al. (2024) had high uncertainties in stellar ages or stellar ages in between two models, so we report lower and upper estimates from N. N. Weinberg et al. (2024) for those systems. We highlight systems that show significant evidence of a deviation from a linear ephemeris as closed circles, while remaining systems are shown as open circles. Three A. J. Barker (2020) values are displayed for WASP-12 (two are overlapping at around 2 × 105) because A. J. Barker (2020) calculated ﹩{Q}_{* }^{{\prime} }﹩ for three different stellar models of WASP-12 across different evolutionary states.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit time diagram for WASP-99.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit time diagram for WASP-45.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit time diagram for XO-3 b.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit time diagram for WASP-19.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit time diagram for WASP-4.
Paper: In Search of Decay: An Analysis of Transit Times of Hot Jupiters in Main-sequence and Post-main-sequence Systems
Authors: Noah Sodickson, Samuel Grunblatt
Figure caption: Observed minus calculated transit time diagram for WASP-12.
Paper: The Slow Brightening of WNTR23bzdiq/WTP19aalzlk: Possible Onset of Common Envelope Evolution in an Asymptotic Giant Branch Star?
Authors: Viraj R. Karambelkar, Mansi M. Kasliwal, Kishalay De, Danielle Frostig, Robert Stein, Geoffrey Mo, Nathan P. Lourie, Robert A. Simcoe, Nadejda Blagorodnova
Figure caption: Multiband lightcurve of WNTR23bzdiq. The J-band discovery lightcurve from WINTER is displayed in the inset plot, which shows a slow brightening from 2023 to 2024 relative to the 2014 UKIRT measurement. The full plot shows the optical to MIR photometry spanning 2003–2025. In the optical data available until 2015, the source only shows small amplitude (<0.3 mag) erratic brightness variations. In 2018, it started brightening smoothly, underwent a 1000 day outburst from 2021 to 2023, and has continued rebrightening since. The NEOWISE MIR data show a smooth brightening from 2016 to 2023, following which it declines slightly. Importantly, the MIR fluxes continued to increase even when the optical luminosity faded in 2023. The black vertical lines mark the epochs of the spectroscopic observations.
Paper: The Slow Brightening of WNTR23bzdiq/WTP19aalzlk: Possible Onset of Common Envelope Evolution in an Asymptotic Giant Branch Star?
Authors: Viraj R. Karambelkar, Mansi M. Kasliwal, Kishalay De, Danielle Frostig, Robert Stein, Geoffrey Mo, Nathan P. Lourie, Robert A. Simcoe, Nadejda Blagorodnova
Figure caption: Comparison of properties of WNTR23bzdiq (purple, reference MJD 59500) to the giant star merger OGLE-BLG (blue, MJD 53125) and classical LRNe V838 Mon (red, MJD 52315), V1309 Sco (black, MJD 54725), and M31-LRN-2015 (green, MJD 57044). The phases are plotted relative to MJD = 59500 for WNTR23bzdiq. Top: the classical LRNe are relatively short-lived eruptions with a sharp rise to maximum, while OGLE-BLG shows a slower rise and longer duration than the classical LRNe. WNTR23bzdiq has an even slower rise and longer duration, consistent with its progenitor being more evolved and extended than that of OGLE-BLG. Middle: during their eruptions, all stellar mergers become hotter than their progenitors (indicated by stars) at initial times and then cool rapidly to resemble cold M-type stars. The progenitor of WNTR23bzdiq is an M-type star to begin with, and so it is not expected to show these sharp transitions. The long-term temperature is similar to that reached by OGLE-BLG. Bottom: the LRNe show rapid photospheric and dust shell expansions with velocities of ≈300 km s−1 (black dotted line). In contrast, WNTR23bzdiq and OGLE-BLG show a much slower radius evolution with dust-radius expansion velocities of ≈5 km s−1.
Paper: The Slow Brightening of WNTR23bzdiq/WTP19aalzlk: Possible Onset of Common Envelope Evolution in an Asymptotic Giant Branch Star?
Authors: Viraj R. Karambelkar, Mansi M. Kasliwal, Kishalay De, Danielle Frostig, Robert Stein, Geoffrey Mo, Nathan P. Lourie, Robert A. Simcoe, Nadejda Blagorodnova
Figure caption: Optical-NIR spectra of WNTR23bzdiq (colored) compared to stellar spectral templates (black). The spectra of WNTR23bzdiq resemble those of late M-type giant stars. We find that the NIR spectral type varies from an M8-9 in our earliest spectrum, which was taken at the end of the 2021 outburst (orange), to M7 in the next two spectra (red, purple) taken during the 2024 rebrightening. Additionally, the spectra at the two later epochs have mixed spectral types, where the optical spectra match an M1 spectral type template while the NIR spectra match later M7-type templates. This behavior resembles the Galactic stellar merger V838 Mon. Inset: continuum-normalized optical spectra zoomed in around the Hα line, showing no strong Hα emission.
Paper: The Slow Brightening of WNTR23bzdiq/WTP19aalzlk: Possible Onset of Common Envelope Evolution in an Asymptotic Giant Branch Star?
Authors: Viraj R. Karambelkar, Mansi M. Kasliwal, Kishalay De, Danielle Frostig, Robert Stein, Geoffrey Mo, Nathan P. Lourie, Robert A. Simcoe, Nadejda Blagorodnova
Figure caption: Left: SED of the progenitor star (black dots) together with the range of best-fit PHOENIX+DUSTY models (orange). Our modeling suggests the progenitor has Teff ≈ 3500 K and a total luminosity log_L  =  4.2 L⊙. Right: comparing these progenitor properties (blue star) to MIST stellar evolutionary tracks (colored lines) in the H-R diagram suggests the progenitor is a 7 ± 2 M⊙ star in its early-AGB phase.
Paper: The Slow Brightening of WNTR23bzdiq/WTP19aalzlk: Possible Onset of Common Envelope Evolution in an Asymptotic Giant Branch Star?
Authors: Viraj R. Karambelkar, Mansi M. Kasliwal, Kishalay De, Danielle Frostig, Robert Stein, Geoffrey Mo, Nathan P. Lourie, Robert A. Simcoe, Nadejda Blagorodnova
Figure caption: H-R diagram with the progenitors of classical LRNe (black dots), OGLE-BLG (cyan dot), and WNTR23bzdiq (cyan star) with MIST stellar evolutionary tracks. The stellar tracks are color coded with the expected dust obscurations (AV) from the wind model of M. MacLeod et al. (2022). The progenitor of WNTR23bzdiq is colder than that of any other merger transient, and is the only progenitor on the AGB—potentially providing a unique opportunity to study the outcomes of CEE in an AGB star.
Paper: The Slow Brightening of WNTR23bzdiq/WTP19aalzlk: Possible Onset of Common Envelope Evolution in an Asymptotic Giant Branch Star?
Authors: Viraj R. Karambelkar, Mansi M. Kasliwal, Kishalay De, Danielle Frostig, Robert Stein, Geoffrey Mo, Nathan P. Lourie, Robert A. Simcoe, Nadejda Blagorodnova
Figure caption: WNTR23bzdiq (pink cross) is located in the outskirts of M31, at an angular separation of ≈0.9 deg from its center, corresponding to a distance of ≈12 kpc. Inset: a comparison of a new J-band WINTER image from 2023, an archival J-band UHS reference image from 2014, and the difference image of these two. The position of WNTR23bzdiq is marked by crosshairs. The background image is taken from the Digitized Sky Survey II.
Paper: CMB-S4: Foreground-cleaning Pipeline Comparison for Measuring Primordial Gravitational Waves
Authors: Federico Bianchini, Dominic Beck, W. L. Kimmy Wu, Zeeshan Ahmed, Sebastian Belkner, Julien Carron, Brandon S. Hensley, Clement L. Pryke, Caterina Umiltá
Figure caption: Comparison of B-mode maps and related map products from Pipelines B and C. The first two columns present the cleaned CMB maps from Pipelines B and C, respectively. The central panels display the foreground residuals, calculated as the difference between the cleaned total CMB map and the combined lensing B modes and noise maps after component separation. The two columns on the right illustrate the lensing template and the input lensed CMB maps. Different rows correspond to different foreground models, ranging from Model 0 (top) to Model 2 (bottom). All maps are band-limited to 30 ≤ ℓ ≤ 200 to highlight scales relevant for r inference. With Model 0 (Gaussian foregrounds), the residuals are negligible from both pipelines, as expected. With Model 2, the residuals show spatial variations and differences between methods—reflecting the differences in the assumptions embedded in each foreground-cleaning method. The LT and ΛCDM panels provide a visual confirmation of negligible foreground contaminations in the LTs.
Paper: CMB-S4: Foreground-cleaning Pipeline Comparison for Measuring Primordial Gravitational Waves
Authors: Federico Bianchini, Dominic Beck, W. L. Kimmy Wu, Zeeshan Ahmed, Sebastian Belkner, Julien Carron, Brandon S. Hensley, Clement L. Pryke, Caterina Umiltá
Figure caption: Posterior distributions of the tensor-to-scalar ratio (r) derived from Markov Chain Monte Carlo (MCMC) chains run on PySM3 foreground models. The rows of panels, from top to bottom, display results for Models 3, 4, and 5. The left column corresponds to the r = 0 scenario, while the right column shows results for r = 0.003. In each panel, the colored lines represent the posterior distributions obtained from the three analysis pipelines (A, B, and C). The dotted line represents Pipeline B results without marginalizing over residual foregrounds, typically leading to a larger bias in r. The vertical black dashed line marks the input value of r = 0.003 for reference.