adsabs/AstroCLIMB huggingface dataset:
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Time evolution of atmospheric pressure with variations in mantle carbon concentration (C conc) for models assuming an otherwise Earth-like core. An Earth-like initial carbon concentration of 0.011 wt% (not shown) results in an atmospheric mass-loss rate always greater than the outgassing rate, so no atmosphere can build up. Models with greater carbon inventories than found on Earth build up temporary secondary atmospheres that are nonetheless lost within 4 Gyr. Even with orders of magnitude greater initial carbon inventory than Earth, GJ 1252b would have no significant remaining atmosphere, due to its prodigious atmospheric-loss rate.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Predicted IRAC2 4.5 μm eclipse depths (colored shading) from our suite of atmospheric models for atmospheres dominated by N2; each model has a single dominant, active IR absorber of either CO (top) or CH4 (bottom). The contour lines indicate the level of agreement with our eclipse measurement of ﹩{149}_{-32}^{+25}﹩, with darker regions being more consistent with our data. Thick atmospheres with P surf ≳ 10 bar are disfavored by all modeled mixing ratios.(The data used to create this figure are available.)
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Simulated eclipse spectra of GJ 1252b from our suite of no-atmosphere models for different types of solid, unmelted surface mineralogies (lines; from Hu et al. 2012) compared to our measured depth and uncertainty (red circle with error bars). Squares show the values obtained by averaging the models over the IRAC2 bandpass (dotted line). All but the granitoid and feldspathic models are consistent with our measurement at ≤2σ.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Spitzer 4.5 μm photometry and secondary eclipse fit (top) and residuals to the fit (bottom). The photometry is shown after detrending for systematic effects, combining the photometry from all 10 eclipse visits, and binning down to a two-minute cadence. The measured depth is ﹩{149}_{-32}^{+25}﹩ ppm.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Same as Figure 4, but for atmospheres dominated by O2 and with active IR absorbers of CO2 (top), SO2 (middle), and H2O (bottom). Thick atmospheres (P surf ≳ 10 bar) with mixing ratios of ≳ 10−4 are disfavored in all cases.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Joint posterior distributions of eclipse depth and time of eclipse center from the analysis plotted in Figure 2. The eclipse depth exhibits no covariance with the eclipse timing, despite the latter’s long tail toward high values.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Folded and binned two-sector TESS lightcurve (blue points) with the median model plotted in black. Residuals (data minus model) are shown in the lower panel.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Spitzer 4.5 μm lightcurves for our joint analysis of all eclipse visits. In each triptych, the top panel shows the raw Spitzer photometry (black circles) vs. the PLD model (red points); the middle panel shows the systematics-corrected photometry (black circles) vs. the best-fit eclipse model (red line); the bottom panel shows the residuals. Although we performed our analysis without binning the data, the data are binned here by a factor of 16 for plotting purposes. Figure 2 shows the stacked average of all 10 eclipses.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: The dispersions of the binned residuals (solid black line) to the 4.5 μm lightcurves show limited evidence for correlated noise. The dashed lines show the expectations for wholly uncorrelated errors, which scale as N −1/2.
Paper: GJ 1252b: A Hot Terrestrial Super-Earth with No Atmosphere
Authors: Ian J. M. Crossfield, Matej Malik, Michelle L. Hill, Stephen R. Kane, Bradford Foley, Alex S. Polanski, David Coria, Jonathan Brande, Yanzhe Zhang, Katherine Wienke, Laura Kreidberg, Nicolas B. Cowan, Diana Dragomir, Varoujan Gorjian, Thomas Mikal-Evans, Björn Benneke, Jessie L. Christiansen, Drake Deming, Farisa Y. Morales
Figure caption: Same as Figure 10, but for the final four Spitzer eclipse visits.
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Constraints on the direction of the heliocentric relative lens-source proper motion derived from OGLE photometric data (gray and black contours) and HST astrometric data (blue and red lines). Contours represent 39.3%, 86.5%, and 98.9% confidence regions. Solid and dashed lines correspond to the best-fit direction and its 1σ error bar, respectively.
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Microlensing parallax π E,N  − π E,E  contours derived using subsets of the OGLE data. Left panel: old reductions. Right panel: new reductions. Both the direction and magnitude of the microlensing parallax vector measured using old reductions when restrict to the excellent seeing data (θ FWHM < 4) are systematically shifted. This behavior is no longer present in the new reductions (right panel). The contours represent 68.3% and 95.5% confidence regions.
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Microlensing parallax π E,N  − π E,E  contours. Black contours are derived using only photometric OGLE data. Red and blue contours are based on a joint OGLE and HST fit using Lam et al. (2022a) and Sahu et al. (2022) astrometric reductions, respectively. Contours presented in the left panels are not corrected for possible systematic errors in the astrometric data. The contours represent 39.3%, 86.5%, and 98.9% confidence regions.
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Upper panel: photometric OGLE light curve of OGLE-2011-BLG-0462 together with a best-fit model to OGLE and HST data from Sahu et al. (2022). The best-fit model based on Lam et al. (2022a) reductions is nearly identical (the difference between these two models is smaller than 1 mmag). Gray data points mark median residuals in bins of 10 days. Lower panel: best-fit model to astrometric data (after subtracting proper motions) reduced by Sahu et al. (2022; blue, left panels) and Lam et al. (2022a; red, right panels). F814W data are marked with circles, F606W data with squares.
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Mean OGLE baseline brightness of OGLE-2011-BLG-0462 as a function of hour angle (upper panel) and seeing (lower; based on 2013–2016 data, new OGLE reductions).
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Fits to the HST photometric data in the F814W (left panel) and F606W (right) filters based on the best-fitting model to the photometric OGLE data only (Section 2). Sahu et al. (2022) and Lam et al. (2022a) photometric reductions are marked with blue and red colors, respectively. Solid (dotted) lines mark best-fitting models with (without) blending. Lower panels show residuals from the best-fitting models without blending.
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Difference between astrometric measurements of OGLE-2011-BLG-0462 taken by Lam et al. (2022a) and Sahu et al. (2022) in F814W (upper panel) and F606W filters (lower panel).
Paper: Systematic Errors as a Source of Mass Discrepancy in Black Hole Microlensing Event OGLE-2011-BLG-0462
Authors: Przemek Mróz, Andrzej Udalski, Andrew Gould
Figure caption: Difference between the F814W and F606W photometric measurements of OGLE-2011-BLG-0462 taken by Lam et al. (2022a) and Sahu et al. (2022). The dashed lines indicate a constant shift of 0.303 ± 0.007 and 0.086 ± 0.010 mag in F814W and F606W, respectively.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: One- and two-dimensional marginalized posteriors for the parameters of each component spin model we consider (see Appendix A.2). These posteriors correspond to the measured distributions of component spin magnitudes and tilts shown above in Figure 5. Some parameters are defined only for a subset of component spin models. The shaded region in the joint μ  χ –σ  χ  posterior is the region excluded by the prior cut on the shape parameters of the spin magnitude Beta distribution; see Appendix A.2. We find that the fraction f spike of black holes comprising a zero-spin subpopulation is consistent with zero. The data also require that at least some spins are misaligned by more than 90° relative to their Newtonian orbital angular momentum; among models that include a variable truncation bound z min on the ﹩\cos \theta ﹩ distribution, this bound is inferred to be confidently ≤ 0, regardless of assumptions about a possible zero-spin subpopulation. Allowing such a truncation bound, meanwhile, significantly impacts constraints on f iso, the fraction of binaries with isotropically oriented spins, as well as σ  t , the width of a preferentially spin-aligned mixture component (see Equation (8)). As seen in Figure 5, the introduction of a truncation bound yields a significantly flatter ﹩p(\cos \theta )﹩ distribution, corresponding here to larger values of f iso and σ  t .
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Inferred distributions of component spin magnitudes (left), spin–orbit tilts (middle), and effective inspiral spins (right) of binary black holes under the various component spin models considered in this paper. Solid black lines denote the median and the 90% credible intervals, while red/green light curves correspond to individual draws from the posterior for each model. Among models that allow for a distinct subpopulation of nonspinning systems (bottom two rows), we infer that the fraction of binaries in such systems is consistent with zero. Meanwhile, we find that the ﹩\cos \theta ﹩ distribution confidently extends to negative values; models that allow for a sharp truncation in the ﹩\cos \theta ﹩ distribution require this truncation to occur at ﹩{z}_{\min }\lt 0﹩. Despite the varying component spin magnitude and tilt distributions recovered by these different models, all yield similar χ eff distributions. For reference, the dashed black curves in the right-hand column show the mean χ eff distribution obtained by direct inference with the BimodalGaussian model of Section 4; all four component spin models give χ eff distributions that are consistent with this result.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Marginalized posterior on the fraction ζ spike of binary black holes comprising a distinct subpopulation with χ eff = 0. The blue curve shows the results obtained through analysis of the binary black holes in GWTC-3 (Abbott et al. 2021d). We find ζ spike to be consistent with zero, indicating no evidence for an excess of zero-spin systems. Nevertheless, p(ζ spike) peaks suggestively at ζ spike ≈ 0.5. We demonstrate that this is not unexpected by repeatedly generating and analyzing mock catalogs of χ eff measurements, drawn from an intrinsically spikeless population described by a simple Gaussian. These catalogs yield posteriors similar to our own, often (and incorrectly) disfavoring ζ spike = 0. As discussed in the main text, this behavior is due to a degeneracy between ζ spike and the inferred mean of the spinning “bulk” population. For reference, the black dashed line shows the posterior on the zero-spin fraction ζ 0 inferred in Roulet et al. (2021), which is qualitatively consistent with both our GWTC-3 measurement and the simulated spikeless measurements.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Posterior on the fraction ζ of binary black holes in which both components have zero spin, as obtained in the simple counting experiment of Section 3. This counting experiment uses only events detected through GWTC-2 (Abbott et al. 2021c) and furthermore only relies on the fully marginalized likelihoods for each binary under spinning (﹩0\leqslant {\chi }_{1},{\chi }_{2}\leqslant {\chi }_{\max }﹩) and nonspinning (χ 1 = χ 2 = 0) priors. Values of ζ ≳ 0.8 are definitively ruled out. Whether or not ζ is consistent with zero, however, depends more sensitively on assumptions regarding the distribution of black hole spin magnitudes. If we assume that black hole spins range uniformly up to ﹩{\chi }_{\max }=1.0﹩, ζ = 0 is disfavored. At the same time, relaxing ﹩{\chi }_{\max }﹩ to slightly smaller values yields posteriors increasingly consistent with zero, which would indicate no distinct subpopulation of nonspinning systems.
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Marginal posterior distribution for χ eff using results from Abbott et al. (2021b) that have no excess of zero-spin events (blue) and results from Galaudage et al. (2021) that imply that ∼50% of binaries have zero spins (red). The solid lines trace the mean distribution inferred by each model while shaded regions denote the 90% credible regions; the light traces trace individual draws from the population posterior under each model. We see that, if a significant fraction of binary black holes are indeed nonspinning, this should be clearly identifiable through their χ eff distribution. This figure is modeled after Figure 5 of Galaudage et al. (2021).
Paper: No Evidence that the Majority of Black Holes in Binaries Have Zero Spin
Authors: Thomas A. Callister, Simona J. Miller, Katerina Chatziioannou, Will M. Farr
Figure caption: Posterior for the first percentile (χ eff,1%) of the χ eff distributions implied by each of our component spin models, as shown in the right-hand column of Figure 5. The median values and 90% credible intervals for χ eff,1% are also reported in Table 1. Each of our component spin models require the binary black hole population to contain spins misaligned by more than 90° relative to their Newtonian orbital angular momentum. Correspondingly, χ eff,1% is inferred to likely (although not necessarily) be negative. The χ eff,1% values recovered here are consistent with the minimum χ eff values measured by Abbott et al. (2021a, 2021b).
Paper: Dynamical Origin for the Collinder 132–Gulliver 21 Stream: A Mixture of Three Comoving Populations with an Age Difference of 250 Myr
Authors: Xiaoying Pang, Yuqian Li, Shih-Yun Tang, Long Wang, Yanshu Wang, Zhao-Yu Li, Danchen Wang, M. B. N. Kouwenhoven, Mario Pasquato
Figure caption: (a) Histogram of the distribution of u-matrix elements. The vertical dashed line denotes the threshold value of u that gives a 10% contamination rate for the identified groups, corresponding to the color patches in the 2D neural network (panel (b)). (b) Neural network generated by SOM. Neurons with a u-threshold corresponding to a 10% contamination rate are shown as colored patches. The transparent pink and orange patches are considered as the top-level structure overall. Solid pink and orange patches are the cores of the secondary hierarchical structures, which correspond to Collinder 132 gp 1 (pink) and group 2 (orange). Other red, green, maroon, purple, and cyan patches correspond to Collinder 132 gp 3, Collinder 132 gp 4, Collinder 132 gp 5, Collinder 132 gp 6, and Gulliver 21 with a contamination rate of 10%, respectively.
Paper: Dynamical Origin for the Collinder 132–Gulliver 21 Stream: A Mixture of Three Comoving Populations with an Age Difference of 250 Myr
Authors: Xiaoying Pang, Yuqian Li, Shih-Yun Tang, Long Wang, Yanshu Wang, Zhao-Yu Li, Danchen Wang, M. B. N. Kouwenhoven, Mario Pasquato
Figure caption: Absolute magnitude CMDs (with M  G  adopting Gaia DR 3 parallaxes) for member stars obtained from Gaia DR 3. The colored circles in each panel represent the corresponding member candidates in each subgroup. Black crosses are field stars that are excluded from further investigation (see Section 3.1). The PARSEC isochrones of the best-fitted age are indicated with the black solid curves, with solar metallicity and estimated A  V . The black dotted curve is an isochrone of 50 Myr, with solar metallicity and AV  = 0.06. The gray dashed curves in panels (f)–(h) are 25 Myr isochrones for comparison.
Paper: Dynamical Origin for the Collinder 132–Gulliver 21 Stream: A Mixture of Three Comoving Populations with an Age Difference of 250 Myr
Authors: Xiaoying Pang, Yuqian Li, Shih-Yun Tang, Long Wang, Yanshu Wang, Zhao-Yu Li, Danchen Wang, M. B. N. Kouwenhoven, Mario Pasquato
Figure caption: (a) Projected spatial distribution of member candidates. Cross-matched members with the Collinder 132 moving group in Kounkel & Covey (2019; KC19) are indicated by the black plus signs. Matched stars with the Theia 86 moving group in KC19 are shown as gray plus signs. (b) The U–V velocity distribution for eight subgroups in the Collinder 132–Gulliver 21 region obtained from this study. Members of these eight subgroups are shown as colored circles. The mean errors of U and V are indicated in the lower left corner. The gray circles in the background are 85 clusters and groups from Pang et al. (2022) for comparison. The S/Ns of RVs constructing velocities U and V are restricted to be greater than 20. The black cross indicates the median position of the open cluster Alessi 62 taken from Pang et al. (2022). Alessi 62 is a dissolving cluster with an age of 692 Myr, which forms a diagonal stripe structure.
Paper: Dynamical Origin for the Collinder 132–Gulliver 21 Stream: A Mixture of Three Comoving Populations with an Age Difference of 250 Myr
Authors: Xiaoying Pang, Yuqian Li, Shih-Yun Tang, Long Wang, Yanshu Wang, Zhao-Yu Li, Danchen Wang, M. B. N. Kouwenhoven, Mario Pasquato
Figure caption: (a) The relative PMs of member candidates. All PM vectors are relative to the median PM of Gulliver 21. The vectors of Gulliver 21 members are thicker and are using different scaling than those for other groups (upper right corner). (b–c) The relative 3D velocity vectors for members, projected onto the X-Y and Y-Z planes. The median motion of Gulliver 21 is taken as the reference. We only show velocity vectors for stars with S/N > 20 in RV, of which the mean error is 5.8 km s−1. The large thick gray arrows represent the mean velocity of each subgroup relative to that of Gulliver 21, whose scaling is indicated in the upper left corner (gray arrow). The gray dashed curve shows the orbit of Gulliver 21, and the orbital direction is indicated with an arrow. The dashed arrows in panels (b) and (c) indicate the direction of the line of sight (LOS). The colors of the vectors in these three panels indicate the directions of the vectors, consistent with the color wheel. The scaling of the vectors is shown in each panel.
Paper: Dynamical Origin for the Collinder 132–Gulliver 21 Stream: A Mixture of Three Comoving Populations with an Age Difference of 250 Myr
Authors: Xiaoying Pang, Yuqian Li, Shih-Yun Tang, Long Wang, Yanshu Wang, Zhao-Yu Li, Danchen Wang, M. B. N. Kouwenhoven, Mario Pasquato
Figure caption: (a–b) Past and future 100 Myr integrated orbits of the eight subgroups in the Collinder 132–Gulliver 21 stream using Galpy. (c) Evolution of the separation between seven subgroups and the oldest population, Gulliver 21. The ±1σ uncertainty interval computed from observational errors in the PM and RV is indicated with the shaded areas. An age of 0 Myr corresponds to the present day. The colored plus signs in the three panels indicate the positions of the corresponding subgroups at the time of birth. The triangles represent the present-day positions, and the filled circles indicate the predicated positions at 100 Myr from the present.