adsabs/AstroCLIMB huggingface dataset:
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). IV. Surface Gravity Estimation and Giant–Dwarf Separation with the DDO51 Filter
Authors: Qiqian Zhang, Zhou Fan, Gang Zhao, Ying Wu, Wei Wang, Kai Xiao, Hongrui Gu, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Ali Luo, Nan Song, Yujuan Liu, Yaqian Wu
Figure caption: Color–color diagrams constructed from observed magnitudes prior to extinction correction. Each panel shows a DDO51-related color index plotted against the g − i color: (a) usc – DDO51, (b) vSAGES – DDO51, (c) g – DDO51. The points are color-coded by log g, with values taken from the LAMOST DR10 catalog, as indicated by the color bar.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). IV. Surface Gravity Estimation and Giant–Dwarf Separation with the DDO51 Filter
Authors: Qiqian Zhang, Zhou Fan, Gang Zhao, Ying Wu, Wei Wang, Kai Xiao, Hongrui Gu, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Ali Luo, Nan Song, Yujuan Liu, Yaqian Wu
Figure caption: Derived color excesses vs. reference E(B – V) from Bayestar19 for various color indices involving SAGES filters. Color excesses were calculated with intrinsic colors predicted by the XGBoost model using APOGEE parameters. The color scale represents the density of stars in the data sample. The red line in each panel shows the best-fit linear relationship ﹩E({\lambda }_{1}-{\lambda }_{2})={R}_{{\lambda }_{1}-{\lambda }_{2}}\times E(B-V)﹩, with the derived differential extinction coefficient ﹩{R}_{{\lambda }_{1}-{\lambda }_{2}}﹩ indicated in the legend.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). IV. Surface Gravity Estimation and Giant–Dwarf Separation with the DDO51 Filter
Authors: Qiqian Zhang, Zhou Fan, Gang Zhao, Ying Wu, Wei Wang, Kai Xiao, Hongrui Gu, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Ali Luo, Nan Song, Yujuan Liu, Yaqian Wu
Figure caption: Distributions of stellar atmospheric parameters. Top row (APOGEE-Gaia-SAGES data set): (a) Kiel diagram, showing log g vs. Teff, with color density representing the relative number of stars. (b) [Fe/H] distribution histogram. (c) E(B – V) distribution histogram. Bottom row (LAMOST-Gaia-SAGES data set): (d) Kiel diagram, similar to (a). (e) [Fe/H] distribution histogram, similar to (b). (f) E(B – V) distribution histogram, similar to (c).
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). IV. Surface Gravity Estimation and Giant–Dwarf Separation with the DDO51 Filter
Authors: Qiqian Zhang, Zhou Fan, Gang Zhao, Ying Wu, Wei Wang, Kai Xiao, Hongrui Gu, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Ali Luo, Nan Song, Yujuan Liu, Yaqian Wu
Figure caption: Same as Figure 4, but after applying the extinction correction.
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: Low-mass quiescent galaxies in A2744 quench star formation and form most of their mass later than those in a z ∼ 2.5 overdensity. In both panels, squares and triangles show the sample of ﹩{\mathrm{log}}({M}_{\star }/{M}_{\odot })\lt 9﹩ and ﹩{\mathrm{log}}({M}_{\star }/{M}_{\odot })\gt 9﹩ quiescent galaxies from S. E. Cutler et al. (2024) that are associated with the z ∼ 2.5 overdensity behind A2744, respectively. Circles show the A2744 sample (with stars indicating NIRSpec sources). Dashed and dotted lines show semi-analytical model mass growth and sSFR as a function of redshift (Z. Lu et al. 2014) for ﹩{\mathrm{log}}({M}_{\star }/{M}_{\odot })=7.6﹩ and 8.9 (Mh = 3 × 1010h−1 and 1011h−1 M⊙), respectively. The shaded gray region shows the redshift evolution of sSFR from K. E. Whitaker et al. (2014) between ﹩7\lt {\mathrm{log}}({M}_{\star }/{M}_{\odot })\lt 10﹩, normalized to the J. Leja et al. (2022) main sequence at z = 0.308 in order to correct for methodology-dependent systematic offsets. In the top panel, solid lines show projected stellar mass growth as a function of redshift for the NIRSpec sources, while the bottom panel shows the spectrophotometrically modeled SFHs of low-mass quiescent galaxies. The solid lines are colored based on their stellar mass at observation (z = 0.308).
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: Cartoon showing the evolution from a disky low-mass star-forming galaxy to quiescent dwarf spheroids in a cluster environment. At z < 2, the hot ICM in (proto)clusters removes the gas from low-mass star-forming galaxies, leaving a population of predominantly disky low-mass quiescent galaxies with centrally concentrated residual star formation. Further longer-timescale environmental effects (e.g., dynamical stirring, tidal effects) significantly alter the morphology of low-mass quiescent galaxies in the cluster, either via erosion or expansion. These effects, indicated by black arrows, lead to a mixed population of compact dwarf spheroids and UDGs with a large size scatter but a median size similar to local dwarf galaxies. The bottom panels show the axis-ratio distributions of these three stages broken into intrinsic distributions of disky (blue) and spheroidal (red) galaxies.
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: Low-mass quiescent galaxies in A2744 form at lower redshifts compared to those in a z ∼ 2.5 overdensity. Orange stars show the mass-weighted formation redshifts (﹩{\langle {z}_{\star }\rangle }_{M}﹩) of low-mass quiescent cluster galaxies with associated NIRSpec observations,while black points show low-mass quiescent galaxies in the z ∼ 2.5 overdensity behind A2744. Brown contours show the underlying sample of all low-mass quiescent galaxies in A2744. The right axis indicates the corresponding mass-weighted age (﹩{\langle {t}_{\star }\rangle }_{M}﹩) in billions of years (Gyr).
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: Low-mass quiescent galaxies in A2744 have similar axis ratio distributions to old massive quiescent galaxies at 1 < z < 3. Distributions of mass, size, Sérsic index, and axis ratio for low-mass quiescent galaxies in A2744 (gray shaded histogram) and the cosmic noon quiescent galaxies from S. E. Cutler et al. (2024). The cosmic noon sample is separated by median stellar age: 30 < t50 < 100 in blue, 100 < t50 < 500 in purple, and t50 > 500 Myr in red.
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: Low-mass quiescent galaxies in A2744 have exponential-disk-like light profiles, though their larger median axis ratios do not indicate an overall disky population. The sample of low-mass quiescent galaxies are colored by their F200W Sérsic index (left) and axis ratio (right), with large circles indicating the median size in 0.5 dex mass bins. Large numbers show the median Sérsic index and median axis ratio of the bins, respectively. Solid and dashed black lines indicate the best-fit size–mass relations shown in Figure 2; brown contours indicate the 0 < z < 0.5 quiescent field galaxies from S. E. Cutler et al. (2022). Lines of constant effective surface mass density (﹩{{\rm{\Sigma }}}_{{\rm{e}},{{\rm{M}}}_{\star }}﹩) are shown in gray, ranging from ﹩0.1\lt {{\rm{\Sigma }}}_{{\rm{e}},{{\rm{M}}}_{\star }}\lt 1000\,{M}_{\odot }\,{\mathrm{pc}}^{-2}﹩.
Paper: Advanced Weights for IXPE Polarization Analysis
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: The halo representing scattered prompt emission from GRB 221009A with different background removal techniques. From left: all 2–8 keV counts; counts surviving the background cut of A. Di Marco et al. (2023); counts weighted by the photon character 1 − πi this work introduces; radial profiles of the images. Green circles highlight the rings as a visual aid. The stretch, max, and min are identical between all panels. The gray curve in the rightmost panel presents a model of the true radial profile derived from the Swift GRB 221009A observation, accounting for the IXPE PSF and adding a uniform background.
Paper: The Structure and Formation Histories of Low-mass Quiescent Galaxies in the A2744 Cluster Environment
Authors: Sam E. Cutler, John R. Weaver, Katherine E. Whitaker, Jenny E. Greene, David J. Setton, Zach J. Webb, Ayesha Abdullah, Aubrey Medrano, Rachel Bezanson, Gabriel Brammer, Robert Feldmann, Lukas J. Furtak, Karl Glazebrook, Ivo Labbe, Joel Leja, Danilo Marchesini, Tim B. Miller, Ikki Mitsuhashi, Themiya Nanayakkara, Erica J. Nelson, Richard Pan, Sedona H. Price, Katherine A. Suess, Bingjie Wang, 冰洁 王
Figure caption: Younger low-mass quiescent cluster galaxies have lower Sérsic indices and diskier axis-ratio distributions than older sources. Distributions are shown for the mass-weighted age (﹩{\langle {t}_{\star }\rangle }_{M}﹩), size (﹩{R}_{e{,}_{{\rm{SMA}}}}﹩), Sérsic index (n), and axis ratio (q) for the youngest (blue) and oldest (red) quartiles of low-mass quiescent galaxies in A2744.
Paper: Advanced Weights for IXPE Polarization Analysis
Authors: Jack T. Dinsmore, Roger W. Romani
Figure caption: The average CNN particle character plotted vs. Mom track properties for PSR B0540−69. The dotted black and white line represents the mission-standard background cuts. 68% and 95% contours of suspected source and background events are also shown. The CNN identifies similar energy dependence of the particle track properties, but enables the use of more precise weighting methods.
Paper: Stellar Mass Segregation in Dark Matter Halos
Authors: Raphaël Errani, Jorge Peñarrubia, Matthew G. Walker
Figure caption: Stellar mass segregation in N-body realizations of the example systems UMa3/U1 (top), Del1 (center), and Eri1 (bottom). Each system is embedded in a cuspy dark matter halo, with an initial dynamical-to-stellar mass ratio of ϒdyn = 10. Shown are {x, y} projections of snapshots at t/Gyr = 0, 2.5, 5, 7.5, and 10. The axes are expressed in units of the initial half-light radius rh0. Individual high-mass stars are shown as dark gray points, while low-mass stars are shown in blue. The median half-light radii of high-mass and low-mass stars (computed over a sample of N-body realizations, see text) are shown as black and blue circles, respectively. Over a period of 10 Gyr, the half-light radius of the population of low-mass stars expands, while the half-light radius of the high-mass population contracts. Consistent with the relaxation time estimates of Figure 1, the effect is largest for the UMa3/U1 model and smallest for the Eri3 model. Dynamically formed binaries consisting of two high-mass stars are highlighted in red (see Section 4.2). A video supplementing this figure is available in the Appendix.
Paper: Stellar Mass Segregation in Dark Matter Halos
Authors: Raphaël Errani, Jorge Peñarrubia, Matthew G. Walker
Figure caption: The effects of mass segregation on a stellar system are separable from tidal effects. The final ratio of half-light radii between the low-mass and high-mass populations is virtually unaffected by the adiabatic expansion of the stellar component in response to tides. Shown are the evolution of half-light radius and velocity dispersion of the UMa3/U1 model, in isolation (blue and dark gray curves for the low- and high-mass populations, respectively), and for the case of a tidal field that slowly lowers the dark matter mass enclosed within the stellar component (red and light gray curves). Circles, triangles and squares mark simulation times of 0, 5, and 10 Gyr. Black solid curves illustrate the potential landscape at the beginning of the simulation (top curve, “initial”) and after 10 Gyr (bottom curve, “evolved”) for the simulation with tides; see text for details.
Paper: Stellar Mass Segregation in Dark Matter Halos
Authors: Raphaël Errani, Jorge Peñarrubia, Matthew G. Walker
Figure caption: Stellar mass segregation plays a substantial role in the dynamical evolution of systems akin to UMa3/U1 if their dynamical-to-stellar mass ratios ϒdyn are smaller than ∼50. Shown is the median ratio of half-light radii between the populations of low-mass and high-mass stars after 10 Gyr of evolution for different (initial) dynamical-to-stellar mass ratios ϒdyn, computed over all N-body realizations (see text). Error bars span the 16th to 84th percentiles of the underlying distribution.
Paper: Stellar Mass Segregation in Dark Matter Halos
Authors: Raphaël Errani, Jorge Peñarrubia, Matthew G. Walker
Figure caption: As stellar mass segregation progresses, the half-light radius of the low-mass stars expands as the population heats up, whereas the population of high-mass stars contracts and cools down. The same systems are shown as in Figure 2, with an initial dynamical-to-stellar mass ratio of ϒdyn = 10. Thick blue (black) lines show the median time evolution of the low-mass (high-mass) stellar population computed from all N-body realizations (see text), whereas light blue (gray) lines show individual runs. Poisson noise widens the distribution of half-light radii and velocity dispersions, most notably for the case of UMa3/U1 (left) with N⋆ = 50 stars.
Paper: Stellar Mass Segregation in Dark Matter Halos
Authors: Raphaël Errani, Jorge Peñarrubia, Matthew G. Walker
Figure caption: As the population of high-mass stars contracts and cools, the number of dynamically formed binaries consisting of two massive stars increases. At the same time, as the population of low-mass stars expands and heats up, the number of dynamically formed binaries consisting of a massive star and a low-mass star decreases. Shown is the fraction fbin of high-mass stars that are in binary systems relative to the total number of high-mass stars. Simulation results are shown as shaded bands, computed from a sample of 2000 N-body realizations of the UMa3/U1 model. Dashed curves show the model predictions of Equation (9).
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: The eccentricity parameter ﹩\alpha \equiv d\mathrm{ln}f/d\mathrm{ln}\epsilon ﹩ (Equation (5)), as a function of the projected average binary separation, 〈s〉. Note that α = 1 corresponds to the thermal distribution, while α > 1 and α < 1 represent superthermal and subthermal distributions, respectively. (Each colored curve denotes the value of ηH selected to integrate the G3R (Equation (D1)); ηH is the maximum size of the spatial three-body interaction region (defined in Section 3.1) in units of the triple’s Hill radius. Our preferred model, ηH = 0.10 (green), corresponds to a maximum scattering region 10% the local Hill radius within a cluster. Our most lax condition, ηH = 0.22 (light blue), represents a tidal acceleration 1% of the average relative acceleration between bodies.) The solid black line is the set of α values found by H.-C. Hwang et al. (2022b). In the left panel, the colored dashed lines are the “phase-mixed” distributions (Appendix C.1.2). The right panel features the final eccentricity distributions following the “cumulative scatter” prescription (Appendix C.2). Phase mixing imparts only a slight “thermalization,” with the resultant wide binary distributions far more eccentric than what is observed. Rather, by considering dynamical encounters in the field, cumulative scattering imparts a dramatic thermalization, resulting in eccentricities in greater observational agreement with H.-C. Hwang et al. (2022b). Despite the simplicity of our toy model and the uncertainties surrounding Gaia incompleteness, there is good qualitative agreement: wide binaries tend superthermal while tight binaries tend subthermal.
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: Left: Total number of three-body binaries, Nbin, we predict are presently within 100 pc of the Sun. We do not account for any observational incompleteness in our models, aside from limiting our comparison radius. The black solid line shows the total number of Gaia binaries observed within 100 pc (K. El-Badry et al. 2021), only including the Gaia binary candidates assessed to have a <10% probability of being a chance alignment of two unbound stars. The dashed lines are the totals having removed binaries with average separations <103 au. Our models exclude 3BBF under too strong a tidal field within a cluster using the “tidal isolation” parameter, ηH; it sets the maximum allowed tidal acceleration applied by the cluster to the three scattering bodies (Equation (3)); see also Appendix A.1). Color denotes the field evolution prescription, phase mixing (Appendix C.1), and cumulative scatter (Appendix C.2). The CS prescription destroys more binaries because the destruction and scattering rate of binaries tends to increase following each subsequent encounter and is the unconditionally dominant effect when compared to PM. Right: The average number, Nbin, of three-body binaries (3BBs) that survive without undergoing an encounter in a cluster of initial mass Mcl0 until cluster dissolution; this is largely independent of Galactocentric radius. Note that the right panel does not consider binary disruption in the MW disk or the subset of binaries that migrate to the solar neighborhood. A very small fraction of the initial cluster population forms 3BBs that survive until dissolution without undergoing an encounter, with ≲25% clusters emitting a single unperturbed 3BB to the field.
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: These five subfigures are SMA-focused, “1.5D” versions of the contour plots in Figure 4, detailing “where” and “when” 3BBs were assembled before migrating to the solar neighborhood. Color, the extra “0.5th” dimension, distinguishes between different logarithmically spaced bins, i, in SMA of width Δai. The bottom panel of each subfigure displays the cumulative density functions, C(X, ai), of the integration variable X specified on the panels’ horizontal axes, for each bin in SMA. The top panels of each subfigure display the corresponding probability density functions scaled by SMA bin width, ﹩f(X){\rm{\Delta }}{a}_{{\rm{i}}}=\frac{{\partial }^{2}C(X,{a}_{{\rm{i}}})}{\partial X\partial a}{\rm{\Delta }}{a}_{{\rm{i}}}﹩. The integration variables under examination are (a: {r/rh}) the radial cluster location of the 3BBF in terms of the natal cluster’s half-mass radius, (b: ﹩\{\tilde{\tau }\}﹩) the time between cluster formation and the 3BBF as a fraction of the total cluster lifetime, (c: {Mcl}) the mass of the 3BB’s natal cluster at time ﹩\tilde{\tau }﹩, (d: {RG}) the Galactocentric radius of the natal cluster, and (e: {t}﹩\{{t}^{{\prime} }\}﹩) the time at which the 3BB’s natal cluster dissolves, where ﹩{t}^{{\prime} }=12\,\mathrm{Gyr}﹩ is the present day. The widest binaries tend to be born later in time, both in ﹩\tilde{\tau }﹩ and ﹩{t}^{{\prime} }﹩, and farther out, both in r/rh and RG, than tight binaries. Across the entire parameter space, we predict that solar neighborhood 3BBs mostly formed in clusters with masses ﹩{M}_{{\rm{cl}}}(\tilde{\tau })\lt 1{0}^{2}\,{M}_{\odot }﹩, near the point of absolute dissolution of the cluster (﹩\tilde{\tau }\sim 1﹩).
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: The predicted number, Nbin (top), of 3BBs within 100 pc of the Sun and their probability density function (bottom) as a function of 〈s〉, the projected average binary separation (Equation (4)). (Each colored curve is a model realization with a different “tidal isolation” parameter, ηH (see Section 3.1). Our most conservative value, ηH = 0.1, is the dashed purple line, denoting a local tidal acceleration 0.1% of the average relative acceleration between bodies during three-body scattering. Larger ηH yields more binaries, but risks breaking the model assumption of isolated three-body scattering.) The Gaia binary separations within 100 pc of the Sun (black curve) are taken from K. El-Badry et al. (2021) using their <0.1 binary chance-alignment criterion. The left panel is the final distribution when applying “phase mixing” (Appendix C.1), while the right panel uses the “cumulative scatter” prescription (Appendix C.2). The CS prescription represents the most physically accurate model. It is highly improbable that a wide binary can secularly evolve in isolation over the course of the MW’s entire history, as is assumed in the PM model. The overall shape of the separation distribution closely matches the observed distribution when 〈s〉 > 103 au. The total number (i.e., from summing over Nbin) of 3BBs is reported in Figure 1.
Paper: A Million Three-body Binaries Caught by Gaia
Authors: Dany Atallah, Yonadav Barry Ginat, Newlin C. Weatherford
Figure caption: Contour plots (top) and an accompanying set of cumulative distribution functions (middle) illustrating the relationship between (i) the initial binary SMA, a0, and its final SMA, a, following CS field evolution; and (ii) a0 and the initial mass of the binary’s natal cluster, Mcl0. In column (ii), we include the samples of binaries eventually disrupted through CS. The bottom panels show the fraction of disrupted field binaries given (i) a0 or (ii) Mcl0. The tighter the initial binary, the less its SMA tends to change. Critically, we predict that wide field 3BBs in the solar neighborhood today with SMA a > 4000 au are overwhelmingly born with a0 < 4000 au. Hence, the wider the initial binary, the more rapidly it is destroyed in the field. Separately, low-mass clusters tend to produce the highest numbers of binaries, with over 75% of binaries born in clusters with Mcl0 < 103 M⊙.