adsabs/AstroCLIMB huggingface dataset:
Paper: Study of a Red Clump Giant, KIC 11087027, with High Rotation and Strong Infrared Excess—Evidence of Tidal Interaction for High Lithium Abundance
Authors: Raghubar Singh, Anohita Mallick, Bacham E. Reddy, Jeewan C. Pandey, Gang Zhao
Figure caption: (a) Location of KIC11087027 (solid square) in the H-R diagram along with MESA-MIST (Paxton et al. 2011; Dotter 2016) evolutionary tracks for [Fe/H] = −0.55 dex with different masses. Panels (b), (c), and (d) are the spectral synthesis of Li resonance lines at 6707 Å, Li subordinate line at 6103 Å, and CN red line band near 8004 Å, respectively.
Paper: On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A
Authors: Ignacio Magaña Hernandez, Virginia d'Emilio, Soichiro Morisaki, Mohit Bhardwaj, Antonella Palmese
Figure caption: Corner plot showing the marginalized posterior distributions on the total mass m tot, the mass ratio q, and the effective inspiral spin parameter χ eff for GW190425 for both the low-spin (left panel) and high-spin (right panel) priors under the fixed sky location (orange) and fixed position (green) assumptions as described in Section 3. For both cases, we also show the corresponding results from Abbott et al. (2020a) for reference (blue).
Paper: On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A
Authors: Ignacio Magaña Hernandez, Virginia d'Emilio, Soichiro Morisaki, Mohit Bhardwaj, Antonella Palmese
Figure caption: Skymap for GW190425 event, obtained both with high-spin and low-spin priors. The red box shows CHIME’s instantaneous FOV at the time of GW190425. Interpolation was generated with a two-dimensional GP density estimator (contour lines). The location of FRB20190425A’s most probable host galaxy (UGC10667) is annotated for comparison.
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: Pressure P as a function of density n for matter in beta equilibrium based on the new χEFT calculations at N2LO (orange) and N3LO (blue) from Keller et al. (2023; including contributions from electrons and muons) compared to those from Hebeler et al. (2013; dotted gray). We also show the BPS crust EOS (solid black) and the polytropic interpolation of the BPS EOS to the χEFT band (dotted pink). The beginning of the χEFT bands is shown as a gray vertical line at n = 0.5792n 0, and a second vertical line indicates n = 1.1n 0. For simplicity, we only show the BPS EOS to the Hebeler et al. (2013) χEFT matching, but the transitions to the Keller et al. (2023) N2LO and N3LO bands are performed using an identical procedure.
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: Mass–radius prior distributions for the PP model (left panels) and CS model (right panels). The dark (light) blue region and the inner (outer) curves encompass the 68% (95%) credible regions. The top panels compare the priors based on the new χEFT calculations at N2LO (red) and N3LO (blue) from Keller et al. (2023) to those based on the χEFT calculations from Hebeler et al. (2013; dotted black). For the top panels, the χEFT bands are used up to 1.1n 0. In the bottom panels, the prior distributions are shown when using the new χEFT calculations up to 1.5n 0.
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: The same as Figure 2, but for the pressure–energy density prior distributions. The vertical thin lines mark the transition density to the high-density PP and CS extensions.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: SPA basin and SPA compositional anomaly. (a, b) Distribution of FMCs (open circles), Mg-suite (filled circles), and maria and cryptomaria (patches) of SPA and SPACA. The white solid/dashed line represents the boundary of SPACA. (c) Bouguer anomaly of SPA. (d) Bouguer gravity gradient of SPA. (e, f) Comparison between simple and unclassified anomalously shallow craters in Bhabha and Bose regions, likely due to magmatic intrusions.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Potential intrusive materials at the CE-6 landing region. (a) Band II center of Apollo-Oppenheimer region. (b) Band II center of extracted spectra from small, fresh craters. The thick white line represents the boundary of Mg-rich materials. (c) Band I and II centers of extracted spectra and their corresponding lithology. (d) Ejecta thickness of the Chaffee S and White craters to the CE-6 sampling region.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Intrusive magmatism in Apollo basin and its surroundings. (a) Apollo-Oppenheimer region. The white dashed quadrangle and line represent the CE-6 landing region and the boundary of SPACA. (b) Dryden S and T craters. (c) Anders X crater. (d) Hummocky craters to the west of Chaffee S crater. (e) Hummocky crater in the middle of the CE-6 landing region. (f) Tentative Apollo X crater. (g) Tentative Apollo Q crater.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Extensive intrusive magmatism in the Apollo and SPA basins. Various plutonic materials were likely obtained by CE-6, especially Mg-suites from the Chaffee S crater. Widespread Mg-suites exposed by complex craters and impact basins and plutonic materials from sills of FMC and ring dikes may be diffused into CE-6 soils by vertical and lateral mixing. Features are compiled into this figure for depiction. Not all features have the same scale.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Bouguer anomaly and gradient of Apollo-Oppenheimer region. (a) Bouguer anomaly. (b) Bouguer gradient. The dashed circles represent the tentative Apollo X and Apollo Q craters. The thick white line represents the interpreted ring dike encircling the Apollo basin.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: M3 band I center of the Apollo-Oppenheimer region. The thick white line represents the boundary of Mg-rich materials.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Crustal thickness and distribution of lunar FMCs. “CE,” “A,” and “L” represent “Chang’e,” “Apollo,” and “Luna” missions, respectively.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Typical examples of floor-fractured, hummocky, and concentric craters. Poincaré and Schrödinger are the two largest floor-fractured craters within SPA.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Typical examples of ejecta-filled, light plain-filled, and mare-filled craters.
Paper: A Potential Second Shutoff from AT2018fyk: An Updated Orbital Ephemeris of the Surviving Star under the Repeating Partial Tidal Disruption Event Paradigm
Authors: Dheeraj Pasham, E. R. Coughlin, M. Guolo, T. Wevers, C. J. Nixon, Jason T. Hinkle, A. Bandopadhyay
Figure caption: Top: AT2018fyk’s observed 0.3–10.0 keV X-ray luminosity evolution over the past ∼2000 days. The x-axis is in the observer’s frame. Most recent Chandra and Swift data show a drop of >10 from 7 × 1042 to 7 × 1041 over two months. A similar change is also evident in the UV lightcurve (bottom panel). Inverted triangles represent 3σ upper limits. This sudden change can be interpreted as a shutoff, which allows us to refine the orbital period of the star that is repeatedly disrupted to be 1306 ± 47 days. The two shutoff epochs are highlighted with red/vertical bands. The entire X-ray and UV photometry is available at doi:10.5281/zenodo.10913475.
Paper: A Potential Second Shutoff from AT2018fyk: An Updated Orbital Ephemeris of the Surviving Star under the Repeating Partial Tidal Disruption Event Paradigm
Authors: Dheeraj Pasham, E. R. Coughlin, M. Guolo, T. Wevers, C. J. Nixon, Jason T. Hinkle, A. Bandopadhyay
Figure caption: Left: XMM-Newton/EPIC-pn image of AT2018fyk’s field of view on MJD 60102.76 (XMM ObsID 0921510101). The circle centered on AT2018fyk has a radius of 30″, while the arrows pointing north and east are each 30″ in length. Middle: stacked Swift/XRT image of AT2018fyk using data taken between MJDs 60140 and 60200, i.e., the data point around day 1800 between XMM-Newton (pentagon) and Chandra detections (square) in Figure 2 The statistical significance of the detection is 3.7σ. The circle has a radius of 47″, while the directional arrows are 90″ each. Right: stacked Chandra/ACIS X-ray image using data from ObsIDs 28294 and 28972. The circle centered on AT2018fyk has a 4″, radius while the directional arrows are 5″ each.
Paper: Erratum: The Transient Outgassed Atmosphere of 55 Cancri e (2023, ApJL, 956, L20)
Authors: Kevin Heng
Figure caption: Corrected version of top left panel of Figure 2.
Paper: Revealing Gas Inflows Toward the Galactic Central Molecular Zone
Authors: Yang Su, Shiyu Zhang, Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Zhiwei Chen, Xuepeng Chen, Xin Zhou, Lixia Yuan
Figure caption: The upper panel shows the l-v diagram of MWISP 12CO emission in the region [l = 1.°2–4.°0, b ≤ 1.°0] and [l = 4.°0–19.°0, b ≤ −0.°2], while the bottom panel displays the integrated 12CO emission of the entire l-b-v region, overlaid with the gas associated with the whole near dust lane (see Section 3.1). Note that the gas inflows of the large-scale gas structure toward the CMZ are highlighted by the cyan part for the CO emission from the dust lane (i.e., I(CO)/100) and the cyan contours for the corresponding H I emission scaled by ﹩I({\rm{H}}\,{\rm\small{I}})\times \tan (b)﹩. The black ellipses in the upper panel represent the 64 large MC structures (i.e., angular size ﹩\gt 50\ {\mathrm{arcmin}}^{2}﹩ and 2 R MC × v FWHM for the ellipse size; here R MC is the effective radius and v FWHM the mean FWHM) related to the whole near dust lane, and the red rectangles in the bottom panel represent the interesting regions shown in Figure 2.
Paper: Revealing Gas Inflows Toward the Galactic Central Molecular Zone
Authors: Yang Su, Shiyu Zhang, Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Zhiwei Chen, Xuepeng Chen, Xin Zhou, Lixia Yuan
Figure caption: Integrated 12CO emission of three interesting MC structures of the large-scale CO inflows toward the CMZ. Panel (a) shows the arc-like MCs with a sharp edge toward the CMZ in the velocity interval of [192, 202] km s−1 (blue), [203, 216] km s−1 (green), and [222, 237] km s−1 (red). Panel (b) shows the long ballistic-like MCs with the bright head toward the CMZ in the velocity interval of [245, 255] km s−1 (blue), [256, 264] km s−1 (green), and [265, 290] km s−1 (red). Panel (c) shows the MCs located near the end of the CO flows in the velocity interval of [−31, 7] km s−1 (blue), [65, 105] km s−1 (green), and [110, 130] km s−1 (red). The purple circle and the rectangle represent the maser G015.66-00.49 and the ∼0–7 km s−1 filamentary MCs located at the bar end, respectively. The cyan contours are the same as those in Figure 1 for the corresponding H I emission related to the WGL. Note that the blue color in panel (c) roughly traces the near 3 kpc ring emission (see Dame & Thaddeus 2008) or the lateral arm indicated in Figure 3.
Paper: Revealing Gas Inflows Toward the Galactic Central Molecular Zone
Authors: Yang Su, Shiyu Zhang, Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Zhiwei Chen, Xuepeng Chen, Xin Zhou, Lixia Yuan
Figure caption: Schematic representation of the WGL and the lateral arm based on the morphological and kinematic features from the MWISP CO data. In the diagram, the red shaded blocks represent the MCs flowing toward the CMZ, while the blue shaded blocks show the MCs along the near 3 kpc ring (or the lateral arm dragged by the rotation bar). The end of the WGL intersects with the 3 kpc ring structure at a distance of about 5 kpc. The bar plays an extremely important role in driving flows and transporting the reservoir gas at R GC ∼ 3–4 kpc to the CMZ. The red ring represents the CMZ, while the red dots, red stars, and red triangles represent the Sun, the GC, and the bar end, respectively. The direction of the moving gas and the Sun is labeled by the black arrows. Here, the longitude of the near bar end, l, is measured to be about 15°. The inclination angle and the pattern speed of the bar are estimated to be ϕ bar = 23° ± 3° and Ωbar ≲ 32.5 ± 2.5 km s−1 kpc−1 (see the text), respectively.
Paper: On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A
Authors: Ignacio Magaña Hernandez, Virginia d'Emilio, Soichiro Morisaki, Mohit Bhardwaj, Antonella Palmese
Figure caption: Posterior distributions on the total mass m tot for GW190425 from the fixed 3D sky position of UGC10667 parameter estimation results for both low (blue) and high spin (yellow) priors. We also show the estimated prompt collapse threshold mass M threshold posteriors, conditional on EOS constraints from GW170817 (solid black) and with the additional constraint assuming ﹩{M}_{\mathrm{TOV}}^{\max }\geqslant 1.97{M}_{\odot }﹩ (dashed black).
Paper: On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A
Authors: Ignacio Magaña Hernandez, Virginia d'Emilio, Soichiro Morisaki, Mohit Bhardwaj, Antonella Palmese
Figure caption: Marginalized posterior distributions on the luminosity distance D  L  and the inclination angle ι for GW190425 for both the low-spin (left panel) and high-spin (right panel) priors under the fixed sky location (orange) and fixed position (green) assumptions as described in Section 3. For both cases, we also show the results from Abbott et al. (2020a) for reference (blue).
Paper: On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A
Authors: Ignacio Magaña Hernandez, Virginia d'Emilio, Soichiro Morisaki, Mohit Bhardwaj, Antonella Palmese
Figure caption: Marginalized posterior distributions on the primary mass m 1 and the secondary mass m 2 (both in the source frame) for GW190425 for both the low-spin (left panel) and high-spin (right panel) priors under the fixed sky location (orange) and fixed position (green) assumptions as described in Section 3. For both cases, we also show the primary and secondary mass posteriors from Abbott et al. (2020a) for reference (blue).
Paper: On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A
Authors: Ignacio Magaña Hernandez, Virginia d'Emilio, Soichiro Morisaki, Mohit Bhardwaj, Antonella Palmese
Figure caption: Marginalized posterior distributions on the viewing angle θ  v  for GW190425 under the fixed sky location (orange) and fixed position assumptions (green) as described in Section 3. For both cases, we also show the viewing angle posteriors computed using the results of Abbott et al. (2020a) for reference (blue). We show both the low-spin (light lines) and high-spin (solid lines) prior results for completeness.
Paper: Discovery of a Hypervelocity L Subdwarf at the Star/Brown Dwarf Mass Limit
Authors: Adam J. Burgasser, Roman Gerasimov, Kyle Kremer, Hunter Brooks, Efrain Alvarado, Adam C. Schneider, Aaron M. Meisner, Christopher A. Theissen, Emma Softich, Preethi Karpoor, Thomas P. Bickle, Martin Kabatnik, Austin Rothermich, Dan Caselden, J. Davy Kirkpatrick, Jacqueline K. Faherty, Sarah L. Casewell, Marc J. Kuchner
Figure caption: Left: Keck/NIRES spectrum of J1249+3621 smoothed to a resolution of λ/Δλ = 150 (black lines), compared to the L dwarf templates 2MASSW J2130446-084520 (L1, blue dotted–dashed line; data from Bardalez Gagliuffi et al. 2014), 2MASS J17561080+2815238 (sdL1, magenta line; data from Kirkpatrick et al. 2010), and WISE J043535.80+211509.2 (esdL1, red dashed line; data from Luhman & Sheppard 2014). The spectrum of J1249+3621 is normalized at 1.3 μm, and the comparison spectra are normalized to maximize agreement in the 1.0–1.3 μm range. The dwarf and subdwarf comparisons are offset for ease of comparison. Major spectral features are labeled, as are regions of strong telluric absorption at 1.35–1.5 and 1.75–1.85 μm (vertical gray bands). Right: comparison of the smoothed spectrum of J1249+3621 (black lines) to best-fit models (magenta lines) from the Sonora Elf Owl (top; Mukherjee et al. 2024) and SAND (bottom; Alvarado et al. 2024) atmosphere grids. Spectra are scaled to apparent fluxes using the UHS J-band magnitude of J1249+3621, and the models are scaled to minimize ﹩{\chi }_{r}^{2}﹩. Model parameters are listed in the figure captions. Difference spectra (observed minus computed; black line) are compared to the ±1σ uncertainty of the observed flux densities (gray band) in the bottom panels.
Paper: Discovery of a Hypervelocity L Subdwarf at the Star/Brown Dwarf Mass Limit
Authors: Adam J. Burgasser, Roman Gerasimov, Kyle Kremer, Hunter Brooks, Efrain Alvarado, Adam C. Schneider, Aaron M. Meisner, Christopher A. Theissen, Emma Softich, Preethi Karpoor, Thomas P. Bickle, Martin Kabatnik, Austin Rothermich, Dan Caselden, J. Davy Kirkpatrick, Jacqueline K. Faherty, Sarah L. Casewell, Marc J. Kuchner
Figure caption: Projected orbit of J1249+3621 from galpy (Bovy 2015) for 100 initial conditions sampling uncertainties in distance, proper motion, and RV (black lines). The top panels display the forward orbit over 10 Gyr projected onto the Galactic plane on wide (left) and narrow (right) distance scales. The bottom panels display the backward orbit over 150 Myr projected onto the Galactic plane (left) and XZ coordinates (right). The top-left panel shows the present-day positions (magenta crosses) and forward-projected orbits (magenta lines) of 50 satellite galaxies from Fritz et al. (2018), as well as the Milky Way’s virial radius of 180 kpc (dashed blue circle; Sylos Labini et al. 2023). The top-right panel shows the present-day positions of 161 GCs from Vasiliev (2019; magenta circles) and the closest-approach radius of ∼1 kpc from the Galactic center (yellow dashed circle). GCs and their backward-projected orbits (magenta lines) are also shown in the bottom panels.
Paper: Discovery of a Hypervelocity L Subdwarf at the Star/Brown Dwarf Mass Limit
Authors: Adam J. Burgasser, Roman Gerasimov, Kyle Kremer, Hunter Brooks, Efrain Alvarado, Adam C. Schneider, Aaron M. Meisner, Christopher A. Theissen, Emma Softich, Preethi Karpoor, Thomas P. Bickle, Martin Kabatnik, Austin Rothermich, Dan Caselden, J. Davy Kirkpatrick, Jacqueline K. Faherty, Sarah L. Casewell, Marc J. Kuchner
Figure caption: Forward modeling of the Keck/NIRES spectrum of J1249+3621 in the 1.10–1.19 μm (left) and 1.235–1.28 μm (right) spectral regions, both of which contain stellar and telluric absorption features. Each panel displays, from top to bottom, the telluric spectrum in green, the stellar model in blue, the combined model in magenta overlaid on the observed spectrum in black, and the difference spectrum (data model) in black overlaid on the ± 1σ uncertainty band in gray. The reduced χ 2 of each fit is indicated in the text to the right of the plot.
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: Mass–radius posterior distributions for the PP model (left panels) and CS model (right panels) for the “New” scenario. The dark (light) green region and the inner (outer) curves encompass the 68% (95%) credible regions of the N3LO χEFT band. The top panels compare the posteriors based on the new χEFT calculations at N2LO (red line) and N3LO (green bands) from Keller et al. (2023) to those based on the χEFT calculations from Hebeler et al. (2013; dotted black line). For the top panels, the χEFT bands are used up to 1.1n 0. In the bottom panels, the posterior distributions are shown when using the new χEFT calculations up to 1.5n 0. For comparison, we also show the posterior distribution for N3LO used up to 1.1n 0 (dashed blue lines).
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: Prior distributions (lines) and posterior distributions (colored regions) for the pressure at 2n0 (upper panels) and 3n0 (lower panels). Results are shown for the PP model (left panels) and the CS model (right panels) using the χEFT bands at N3LO up to 1.1n 0 (orange) and 1.5n 0 (light blue). The posterior distributions are for the “New” scenario.
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: Correlation between the radius R 2.0 and R 1.4 of a 2.0 M ⊙ and 1.4 M ⊙ neutron star, respectively, for the “New” scenario. Results are shown for the PP model (left panel) and the CS model (right panel) using the χEFT bands at N3LO up to 1.1n 0 (red) and 1.5n 0 (green).