adsabs/AstroCLIMB huggingface dataset:
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: This figure shows the fractional percentage temperature change of the same five clusters from Figures 13 and 14. There is overlap between the free redshift and offset temperatures, suggesting that either method of correction works.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: This figure shows how the gain offset, as obtained by the methods described in Appendix B, varies over the lifetime of NuSTAR. The offset remains consistently around a value of 0.11 keV, suggesting that the issue has continuously existed across all observation cycles.
Paper: NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission
Authors: Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, Niels-Jorgen Westergaard
Figure caption: This figure shows observations conducted in every NuSTAR observation cycle since the first light on 2012 June 28. The first two points are observations of the Bullet Cluster taken pre-cycle 1. The final three points are MACS J0717.5+3745, A2319, and A1795 in that order.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: The total ILC residuals in the MV CMB map. The solid gray line shows the primary CMB TT power spectrum, while the dashed–dotted gray line corresponds to a rough kSZ level of D  ℓ  = 3 μK2. CMB dominates on large scales (ℓ ≲ 4000), while the residual noise and foregrounds are higher than kSZ on small scales. We note that the kSZ S/N for individual modes is always lower than 1 for all experiments.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: The observed foreground-induced lensing biases due to tSZ, kSZ, and CIB when cross-correlating the CMB lensing convergence κ map from S4-Wide with galaxy overdensity δ  g  and shear γ from LSST-Y1. The fiducial maximum CMB multipole is set to ﹩{{\ell }}_{\max }^{T}=3000﹩ except for red the curves, where we set ﹩{{\ell }}_{\max }^{T}=5000﹩. The standard QE (Hu & Okamoto 2002; blue) is significantly affected by tSZ (left panel), while the other estimators are immune to tSZ. The bias form kSZ (middle panel) is the same for all estimators with ﹩{{\ell }}_{\max }^{T}=3000﹩ and small at ≲0.1σ (∼1%–3%) level. The bias from CIB follows the order MH18 QE (green; MH18) > standard QE (blue; Hu & Okamoto 2002) > cross-ILC QE (yellow), but note that the CIB biases are boosted by ×10 for clarity. For all foregrounds, the bias from the cross-ILC is the lowest, and hence we also quantify the bias for ﹩{{\ell }}_{\max }=5000﹩ as well (red curve). As is evident from the red curve, the foreground-induced biases are at a negligible level for cross-ILC QE even for ﹩{{\ell }}_{\max }^{T}=5000﹩. We limit this figure to a single redshift bin z ∈ [0.56, 82] but present the biases for multiple redshift bins in Figure D1.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: The total CIB and tSZ residuals expected in the S4-Wide survey for different ILC combinations. Thin lines are for auto-spectra, and thick lines are for cross-ILC. We note that the residuals in cross-ILC combination (tSZ-free × CIB-free in black) are much lower than kSZ (D  ℓ  = 3 μK2) and hence can be a compelling means of measuring the kSZ power spectrum with future CMB surveys.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: Radio residuals using AGORA expected from S4-Wide for the masking threshold S 150 = 3 mJy (yellow curve) used in this work. They are negative for the cross-ILC tSZ-free × CIB-free combination. We also show the analytical modeling of the radio residuals using Lagache et al. (2020) in the yellow band. The band quantifies the residual power assuming a scatter in the radio spectral index σ(α rad) ∈ [0, 0.35]. For reference, we also show the residuals and the models for multiple masking thresholds: S 150 = 1 mJy in blue, S 150 = 2 mJy in green, and S 150 = 4 mJy in red. The yellow dotted curve near the lower right corner is the residual expected when a radio spectrum α rad = − 0.76 is nulled along with tSZ.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: The ratio of the total CIB + tSZ residual compared to the expected level of kSZ (D  ℓ  = 3 μK2) for the cross-ILC combination tSZ-free × CIB-free from different CMB surveys. In the left panel we show the residuals for the baseline experiments, while the right panel is after the inclusion of HF bands from SPT-3G+ or FYST.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: Marginalized constraints on reionization parameters ﹩{z}_{\mathrm{re}}^{\mathrm{mid}}﹩ and ﹩{\rm{\Delta }}{z}_{\mathrm{re}}﹩ from kSZ power spectrum (dashed–dotted) and large-scale E-mode measurements of ﹩\sigma ({\tau }_{\mathrm{re}})=0.007﹩ from Planck (blue shade) and ﹩\sigma ({\tau }_{\mathrm{re}})=0.002﹩ from LiteBIRD (brown shade) in the left panel. The joint constraints from kSZ and Planck or LiteBIRD are given in the middle or right panels. The kSZ power spectrum does not constrain ﹩{z}_{\mathrm{re}}^{\mathrm{mid}}﹩, and hence it is dominated by the ﹩{\tau }_{\mathrm{re}}﹩ for all experiments. The future surveys can reduce the uncertainty on the duration of reionization ﹩\sigma ({\rm{\Delta }}{z}_{\mathrm{re}})\sim 1.5﹩ (left panel), which is currently unconstrained by Planck. The constraints on ﹩\sigma ({\rm{\Delta }}{z}_{\mathrm{re}})﹩ improve by 2.5–3× when moving from Planck (middle panel) to LiteBIRD (right panels) measurements of ﹩{\tau }_{\mathrm{re}}﹩.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: Total CIB and tSZ residuals from AGORA simulations for two different ILC weights. Solid lines correspond to the case when the AGORA foreground model is used in the covariance matrix to calculate the weights, while the dashed lines use a foreground model based on SPT measurements. The colors correspond to different ILC combinations. The close match between the solid and dashed curves asserts that our baseline approach of using the AGORA foreground model is a valid assumption.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: Left: band power errors for the S4-Wide survey from different ILC techniques. The data points include contribution from CMB, kSZ, residual foregrounds, and noise. As expected, MV returns the least error, while tSZ-free maps have the largest error. The cross-ILC combination tSZ-free × CIB-free is ∼2× worse (better) than MV (tSZ-free). Right: band power errors expected from the cross-ILC technique for different experiments considered in this work. We assume Δ ℓ  = 250 for this figure. From the right panel, it is evident that the cumulative kSZ S/N for all experiments is high.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: Systematic biases in kSZ power spectrum estimation σ sys(A kSZ) due to 5% unmodeled CIB and tSZ residuals in the CMB maps. The bias in the cross-ILC technique is low compared to MV, which is significantly biased. As expected, the bias in MV increases when extending ﹩{{\ell }}_{\max }﹩ in the analysis.
Paper: A Cross-internal Linear Combination Approach to Probe the Secondary CMB Anisotropies: Kinematic Sunyaev–Zel’dovich Effect and CMB Lensing
Authors: Srinivasan Raghunathan, Yuuki Omori
Figure caption: Biases in cosmological parameters due to residual CIB and tSZ signals for the S4-Wide survey. The biases are negligible for both MV and cross-ILC since the constraints are dominated by EE/TE rather than TT.
Paper: IXPE and XMM-Newton Observations of the Soft Gamma Repeater SGR 1806–20
Authors: Roberto Turolla, Roberto Taverna, Gian Luca Israel, Fabio Muleri, Silvia Zane, Matteo Bachetti, Jeremy Heyl, Alessandro Di Marco, Ephraim Gau, Henric Krawczynski, Mason Ng, Andrea Possenti, Juri Poutanen, Luca Baldini, Giorgio Matt, Michela Negro, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Left: joint XMM-Newton 1–12 keV EPIC-pn and MOS light curve folded to the best period inferred from the phase-fitting analysis (see text for details). The colored area marks the 1σ uncertainties on the data points. Right: EPIC-pn (black plus signs and lines), MOS1 (blue plus signs and lines), and MOS2 (red plus signs and lines) spectra of SGR 1806–20 (upper panel), together with the fitting residuals, in units of standard deviation (lower panel), for the BB+PL model discussed in the text. The individual BB and PL components are shown by an orange dashed–dotted and gray dashed line, respectively.
Paper: IXPE and XMM-Newton Observations of the Soft Gamma Repeater SGR 1806–20
Authors: Roberto Turolla, Roberto Taverna, Gian Luca Israel, Fabio Muleri, Silvia Zane, Matteo Bachetti, Jeremy Heyl, Alessandro Di Marco, Ephraim Gau, Henric Krawczynski, Mason Ng, Andrea Possenti, Juri Poutanen, Luca Baldini, Giorgio Matt, Michela Negro, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Contour plot of the IXPE PD and PA in different energy bands. The inner and outer contours mark the regions at the 68.3% and 99% confidence level, respectively. The spectral model is frozen to that obtained from the XMM-Newton observation.
Paper: IXPE and XMM-Newton Observations of the Soft Gamma Repeater SGR 1806–20
Authors: Roberto Turolla, Roberto Taverna, Gian Luca Israel, Fabio Muleri, Silvia Zane, Matteo Bachetti, Jeremy Heyl, Alessandro Di Marco, Ephraim Gau, Henric Krawczynski, Mason Ng, Andrea Possenti, Juri Poutanen, Luca Baldini, Giorgio Matt, Michela Negro, Iván Agudo, Lucio A. Antonelli, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chieng-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgró, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Count rate in the 2–8 keV energy range, summed over the three IXPE DUs, as a function of time for two regions in the field of view, one containing the source and the other only background. Periods in which the background was larger than 50% of the average source rate are identified by vertical white lines and removed by subsequent analyses. The time bin is 5000 and 100 s for the source and background, respectively.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: Results from the fit of a Gaussian function to the cross sections of fine structure observed in the coronal holes. The results are given for the height above the limb in solar radii. In the text, these are discussed as plumes 1, 2, and 3, in descending order. The left-hand plots show the peak intensity, with the posterior mean values for each fit shown as a gray cross, and the vertical length of the cross-arms represents the 94% highest density interval for the posterior. The black solid line is the running average of the means, and the blue line is the average intensity across the coronal hole. The right-hand plots show the Gaussian full width at half maximum (FWHM). The posterior mean values are the blue crosses, and the vertical length of the cross-arms represents the 94% highest density interval for the posterior. The blue solid line is the running average of the posterior means. The pink line shows the expected expansion from the polar coronal hole magnetic field model in Cranmer & van Ballegooijen (2005).
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: The polar region subject to further processing. The top panel displays the Level 4 minsmoothed data. The lower panel shows the unsharp masked Level 5 data, which are generated from a temporal average over 420 s. The white dashed lines show the region where the curves are extracted for visual and Fourier analysis.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: Visual examination of intensity structures. The different curves correspond to the intensity in polar coronal hole across the plumes at a fixed radial distance from the photosphere. The intensity is a spatial and temporal average. For visibility, we have added a constant value to the Level 5 curve (10 DN). It can be observed that the Level 4 and 5 processing steps enhance the fine-scale structures.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: Polar coronal hole observed the 2011 January 30. The panels show the different stages of processing applied to the data. Panel (a) shows the original Level 1 data. Panel (b) shows the deconvolved data (Level 2). Panel (c) shows the noise-gated data (Level 3). The plumes are substantially clearer in the Level 3 data, highlighting the removal of scattered light and significant noise reduction.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: Discrete Fourier transform of Level 3 and 5 curves shown in Figure 3. The vertical dashed–dotted curve marks the approximate position of the spectral break. The dashed line shows a k −1 power law for comparison to the Level 3 data.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: See Figure 6 caption for details. In the text, these are discussed as plumes 4 and 5.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: Probability density of the lifetime of the fine structure in coronal holes.
Paper: The Fine-scale Structure of Polar Coronal Holes
Authors: R. J. Morton, R. Cunningham
Figure caption: Example of a Gaussian fit to a cross-sectional intensity profile. The black crosses are the observed intensity values from the Level 5 data. The blue dots show the posterior means for the intensity, and the peach band corresponds to the 95% highest density interval (HDI).
Paper: The Missing Link: Testing Galactic Chemical Evolution Models with the First Multi-isotopic Abundances in Solar Twin Stars
Authors: David R. Coria, Ian J. M. Crossfield, Joshua Lothringer, Becky Flores, Nikos Prantzos, Richard Freedman
Figure caption: Comparison of our six solar twin 12C/13C and 16O/18O ratios to GCE models (Kobayashi et al. 2011; Romano et al. 2017; Prantzos et al. 2018) and archival solar twin measurements (Botelho et al. 2020).
Paper: The Missing Link: Testing Galactic Chemical Evolution Models with the First Multi-isotopic Abundances in Solar Twin Stars
Authors: David R. Coria, Ian J. M. Crossfield, Joshua Lothringer, Becky Flores, Nikos Prantzos, Richard Freedman
Figure caption: Example of our analysis approach for the infrared solar spectrum from the ACE-FTS Solar Atlas (Hase 2010). Here, we show the six χ 2 values calculated between the solar line profile and each model of varying 13CO and C18O abundances. We fit a parabola to the χ 2 values (≤175) and assign the minimum as the best-fit isotopologue abundance relative to solar. We measure 1.10 ± 0.10 and 1.03 ± 0.42 ×  solar abundances for 13CO and C18O, respectively.
Paper: The Missing Link: Testing Galactic Chemical Evolution Models with the First Multi-isotopic Abundances in Solar Twin Stars
Authors: David R. Coria, Ian J. M. Crossfield, Joshua Lothringer, Becky Flores, Nikos Prantzos, Richard Freedman
Figure caption: Stacked C18O line profiles for our sample. The line profiles represent the weighted average of several M-band C18O lines for the observed stellar spectrum (in blue) and multiple PHOENIX model spectra of varying C18O abundances. We interpolate between these models using χ 2 minimization to determine the stellar C18O abundance relative to solar (χ 2 minimization shown in Figure 4; results shown in Table 3).
Paper: The Missing Link: Testing Galactic Chemical Evolution Models with the First Multi-isotopic Abundances in Solar Twin Stars
Authors: David R. Coria, Ian J. M. Crossfield, Joshua Lothringer, Becky Flores, Nikos Prantzos, Richard Freedman
Figure caption: Stacked 13CO line profiles for our sample. The line profiles represent the weighted average of several M-band 13CO lines for the observed stellar spectrum (in blue) and multiple PHOENIX model spectra of varying 13CO abundances. We interpolate between these models using χ 2 minimization to determine the stellar 13CO abundance relative to solar (see analysis example in Figure 4; results shown in Table 3).
Paper: The Missing Link: Testing Galactic Chemical Evolution Models with the First Multi-isotopic Abundances in Solar Twin Stars
Authors: David R. Coria, Ian J. M. Crossfield, Joshua Lothringer, Becky Flores, Nikos Prantzos, Richard Freedman
Figure caption: Comparing 12C/13C ratio measurements for our solar twin sample with archival measurements (Botelho et al. 2020). The closer measurements from each study are to each other, the closer they lie to the blue dotted line. All solar twin measurements are consistent within the uncertainties except for HIP 42333, for which we report a significantly lower 12C/13C ratio (∼58) than in the previous study (∼94); refer to Section 5.4 for more details.
Paper: The Missing Link: Testing Galactic Chemical Evolution Models with the First Multi-isotopic Abundances in Solar Twin Stars
Authors: David R. Coria, Ian J. M. Crossfield, Joshua Lothringer, Becky Flores, Nikos Prantzos, Richard Freedman
Figure caption: A small section of the normalized spectra for the Sun from the ACE-FTS Solar Atlas (Hase 2010) and our six solar twins from IRTF/iSHELL (Rayner et al. 2016). The spectra have been shifted to the same wavelength frame. The black dotted lines show the location of some 13CO features used in our abundance analysis.