adsabs/AstroCLIMB huggingface dataset:
Paper: Unscrambling the Lensed Galaxies in JWST Images behind SMACS 0723
Authors: Massimo Pascale, Brenda L. Frye, Jose Diego, Lukas J. Furtak, Adi Zitrin, Tom Broadhurst, Christopher J. Conselice, Liang Dai, Leonardo Ferreira, Nathan J. Adams, Patrick Kamieneski, Nicholas Foo, Patrick Kelly, Wenlei Chen, Jeremy Lim, Ashish K. Meena, Stephen M. Wilkins, Rachana Bhatawdekar, Rogier A. Windhorst
Figure caption: The intracluster light for SMACS 0723 in a F277W+F356W+F444W color composite image. The ICL structure is especially clear in F277W and F356W, and is much less prominent in the SW bands. The pronounced ICL extends along the long axis of the cluster similar to the mass distribution from the lens model, as shown by the overlaid contours of projected mass density κ. Typically a smoothly varying feature, in SMACS 0723 the ICL has significant structures, including a large “loop” feature in the northwest component, and a large lobe-like feature in the southeast component.
Paper: Unscrambling the Lensed Galaxies in JWST Images behind SMACS 0723
Authors: Massimo Pascale, Brenda L. Frye, Jose Diego, Lukas J. Furtak, Adi Zitrin, Tom Broadhurst, Christopher J. Conselice, Liang Dai, Leonardo Ferreira, Nathan J. Adams, Patrick Kamieneski, Nicholas Foo, Patrick Kelly, Wenlei Chen, Jeremy Lim, Ashish K. Meena, Stephen M. Wilkins, Rachana Bhatawdekar, Rogier A. Windhorst
Figure caption: Image stamps depicting the 19 image multiplicities in the SMACS 0723 field, as labeled. The publicly available color image of SMACS 0723 is depicted, which is valuable for the identification of image family members by their similar colors and morphological components. We also require that the model be able to reproduce the positions of the members of each image family. A 5″ bar is shown for reference.
Paper: Unscrambling the Lensed Galaxies in JWST Images behind SMACS 0723
Authors: Massimo Pascale, Brenda L. Frye, Jose Diego, Lukas J. Furtak, Adi Zitrin, Tom Broadhurst, Christopher J. Conselice, Liang Dai, Leonardo Ferreira, Nathan J. Adams, Patrick Kamieneski, Nicholas Foo, Patrick Kelly, Wenlei Chen, Jeremy Lim, Ashish K. Meena, Stephen M. Wilkins, Rachana Bhatawdekar, Rogier A. Windhorst
Figure caption: The projected mass density of SMACS 0723. We show κ, the surface mass density distribution in units of the critical density for strong lensing, for the source redshift of system 1, at z = 1.45, plotted on a grid of constant R.A. and decl. (dashed lines). The resulting mass distribution exhibits a clear ellipticity along the same axis as the ICL as shown in Figure 4.
Paper: The X-Ray Polarization View of Mrk 421 in an Average Flux State as Observed by the Imaging X-Ray Polarimetry Explorer
Authors: Laura Di Gesu, Immacolata Donnarumma, Fabrizio Tavecchio, Iván Agudo, Thibault Barnounin, Nicolò Cibrario, Niccolò Di Lalla, Alessandro Di Marco, Juan Escudero, Manel Errando, Svetlana G. Jorstad, Dawoon E. Kim, Pouya M. Kouch, Ioannis Liodakis, Elina Lindfors, Grzegorz Madejski, Herman L. Marshall, Alan P. Marscher, Riccardo Middei, Fabio Muleri, Ioannis Myserlis, Michela Negro, Nicola Omodei, Luigi Pacciani, Alessandro Paggi, Matteo Perri, Simonetta Puccetti, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicolas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Spectropolarimetric fit of the NuSTAR (red), XMM EPIC-pn (black), and IXPE (blue, magenta, and orange) spectra. From the top to the bottom, we show the fit of the I, Q, and U spectra and the residuals of the best-fit model (solid line). The spectral channels have been rebinned for clarity.
Paper: Reduced Late Bombardment on Rocky Exoplanets around M Dwarfs
Authors: Tim Lichtenberg, Matthew S. Clement
Figure caption: Timing of reduced impacts onto potentially habitable exoplanets around stars of variable mass (panels (A)–(D)). The black lines illustrate the (inverse) cumulative debris mass fraction over time sourced from inside the water snow line. Red symbols indicate the timing of impact events larger than 250 km in diameter, an approximate efficacy threshold to trigger intermittent reduced climate states. Triangle symbols represent cases where the leftover debris field is sourced from an SFD comparable to the modern asteroid belt. Star symbols include an additional 5% of 80–130 km objects, similar to the peak of the birth planetesimal population generated by the streaming instability. Orange vertical lines demarcate the arrival of the star in each scenario onto the main sequence. In the pure steam limit (water-dominated atmospheres), the magma ocean lifetime can be shorter than this (blue arrow in B); in scenarios with substantial primordial H2/He atmospheres (green arrow in D), the magma ocean lifetime is enhanced. Only for G dwarfs, such as the Sun, do appreciable quantities of late bombardment hit potentially habitable planets beyond the pre-main-sequence phase.
Paper: Reduced Late Bombardment on Rocky Exoplanets around M Dwarfs
Authors: Tim Lichtenberg, Matthew S. Clement
Figure caption: Illustration of the planet formation scenario incorporated in the N-body and long-term planetesimal bombardment simulations, described in more detail in Clement et al. (2022). Varying initial conditions related to embryo and planetesimal water content across the three regions simulate differing physical scenarios of material devolatilization and redox gradients (Lichtenberg et al. 2022) across the planetesimal disk. Scenarios are listed in Table 1 and discussed in Section 3.2.
Paper: Reduced Late Bombardment on Rocky Exoplanets around M Dwarfs
Authors: Tim Lichtenberg, Matthew S. Clement
Figure caption: Water mass fraction distribution across the model scenarios (panels (A) to (K)) in Table 1 for 0.1 (red), 0.4 (yellow), and 1.0 (black) M ⊙ stars with the fiducial solar system composition gradient (light gray, yellow, and red lines) as reference cases. The modern Earth water mass fraction with uncertainties is indicated as a light blue-green band. The physical motivation for each model scenario is discussed in Section 3.2. Across most scenarios, M-dwarf exoplanets receive orders of magnitude more water than the modern Earth. Earth-like WMFs for M-dwarf exoplanets are produced with >50% probability for scenarios Dry 3 (panel (E)) and Desiccated Planetesimals 3 (panel (H)).
Paper: High-redshift Galaxies from Early JWST Observations: Constraints on Dark Energy Models
Authors: N. Menci, M. Castellano, P. Santini, E. Merlin, A. Fontana, F. Shankar
Figure caption: Exclusion regions in the w 0−w  a  plane derived from the observed stellar-mass density at z = 10 (Labbe et al. 2022). The regions above each colored line correspond to exclusion with the confidence levels shown in the upper bar. Our exclusion region is compared with the 2σ and 3σ contours allowed by CMB+weak lensing (gray and dark-gray regions) and by the combination of the same data with the Hubble diagram of supernovae and quasars (blue regions), derived from Figure 4 of Risaliti & Lusso (2019). The black dot corresponds to the ΛCDM case (w 0 = −1, w  a  = 0).
Paper: High-redshift Galaxies from Early JWST Observations: Constraints on Dark Energy Models
Authors: N. Menci, M. Castellano, P. Santini, E. Merlin, A. Fontana, F. Shankar
Figure caption: The maximal stellar-mass density predicted by DDE scenarios with w 0 = −1 and four different values of w  a  shown in the legend. In the predictions, we have considered an uncertainty of 0.5 dex in the value of M *. The point is the value measured by Labbe et al. (2022). For the sake of simplicity, the latter—derived assuming a ΛCDM cosmology—has not been rescaled to the different values corresponding to different cosmological scenarios (see text).
Paper: Prompt Emission of γ-Ray Bursts in the High-density Environment of Active Galactic Nucleus Accretion Disks
Authors: Davide Lazzati, Gustavo Soares, Rosalba Perna
Figure caption: Dynamics of the externally shocked material as a function of the distance from the central engine. The fireball is the one that gave rise to the light curve in Figure 4.
Paper: Prompt Emission of γ-Ray Bursts in the High-density Environment of Active Galactic Nucleus Accretion Disks
Authors: Davide Lazzati, Gustavo Soares, Rosalba Perna
Figure caption: Simulated light curve and peak frequency evolution for a burst exploding in a high-density medium n ISM = 1012 cm−3. The fireball is made with an initial shell at t = 0 followed by five equally spaced additional shells (Δt = 0.5 s). The individual pulses from the five collisions are shown with black lines, while the overall pulse profile is shown with a blue line. The orange line instead shows the evolution of the peak frequency of the spectrum (excluding SSC; see right y-axis). The inset shows a comparison between the prompt light curve (blue) and the prompt emission of an analogous fireball exploding in a low-density environment and therefore powered by ISs.
Paper: Prompt Emission of γ-Ray Bursts in the High-density Environment of Active Galactic Nucleus Accretion Disks
Authors: Davide Lazzati, Gustavo Soares, Rosalba Perna
Figure caption: Same as Figures 2, 3, and 4 but for a central engine with a short activity that mimics a short GRB. The case shown is for an engine that releases shells at 0.1 s intervals (Δt = 0.1 s). Despite the short duration of the engine activity (T eng = 0.55 s), the prompt light curve has a duration of T 90 = 3.7 s, placing this event firmly in the long burst category.
Paper: Prompt Emission of γ-Ray Bursts in the High-density Environment of Active Galactic Nucleus Accretion Disks
Authors: Davide Lazzati, Gustavo Soares, Rosalba Perna
Figure caption: Same as Figures 2 and 3 but for a central engine with an even longer pause of 20 s. In this case, the peak frequency of the second pulse shows an increase with respect to the one at the end of the first pulse.
Paper: Prompt Emission of γ-Ray Bursts in the High-density Environment of Active Galactic Nucleus Accretion Disks
Authors: Davide Lazzati, Gustavo Soares, Rosalba Perna
Figure caption: Same as Figure 2 but for a central engine that turns back on after a long pause of 5 s, ejecting another five shells analogous to the initial ones.
Paper: A Lower Bound of Star Formation Activity in Ultra-high-redshift Galaxies Detected with JWST: Implications for Stellar Populations and Radiation Sources
Authors: Kohei Inayoshi, Yuichi Harikane, Akio K. Inoue, Wenxiu Li, Luis C. Ho
Figure caption: Parameter regions of the UV radiative efficiency (ϵ ⋆,rad) and star formation efficiency (f ⋆) where the observed high-z UV LFs (and the brightest data points) are consistently explained. The blue vertical tick marks indicate the values of ϵ ⋆,rad for the Salpeter and top-heavy IMFs discussed in the text (see also Table 1), and horizontal lines show a constant value of f ⋆. For reference, the star formation efficiencies obtained from numerical simulations by Fukushima & Yajima (2021) are shown with star symbols (f ⋆ ≃ 0.13, 0.37, and 0.47 for an initial gas surface density of Σcl = 320, 800, and 1300 M ⊙ pc−2, respectively). Note that since the simulations adopted a Chabrier IMF, the corresponding value of ϵ ⋆,rad is approximately 1.6 times higher than that for a Salpeter IMF with the same mass range and metallicity (Madau & Dickinson 2014).
Paper: A Lower Bound of Star Formation Activity in Ultra-high-redshift Galaxies Detected with JWST: Implications for Stellar Populations and Radiation Sources
Authors: Kohei Inayoshi, Yuichi Harikane, Akio K. Inoue, Wenxiu Li, Luis C. Ho
Figure caption: Galaxy LFs at three different redshift ranges of (a) z ∼ 10, (b) z ∼ 13, and (c) z ∼ 17, along with the observed data points. The UV photon production efficiency per SFR is set to ϵ ⋆,rad = 2.79 × 10−4, assuming a stellar population with a Salpeter IMF in the mass range of 0.1–100 M ⊙ with Z = Z ⊙. Each curve corresponds to the cases with different star formation efficiencies of f ⋆ = 1.0 (solid), 0.6 (long dashed), 0.3 (short dashed), and 0.15 (dotted). The gray thick curve indicates the true upper bound, where the metal-free stellar population (i.e., Population III stars) with an extremely top-heavy IMF (the third model in Table 1) and f ⋆ = 1.0 are considered. The UV luminosity function data are taken from Oesch et al. (2016), Morishita et al. (2018), Donnan et al. (2022), Harikane et al. (2022c, 2022a), Finkelstein et al. (2022), and Naidu et al. (2022a). For comparison, we overlay the quasar LF at z ∼ 10 obtained with a semianalytical calculation (dashed–dotted; Li et al. 2022).
Paper: Early Results from GLASS-JWST. I: Confirmation of Lensed z ≥ 7 Lyman-break Galaxies behind the Abell 2744 Cluster with NIRISS
Authors: Guido Roberts-Borsani, Takahiro Morishita, Tommaso Treu, Gabriel Brammer, Victoria Strait, Xin Wang, Marusa Bradac, Ana Acebron, Pietro Bergamini, Kristan Boyett, Antonello Calabró, Marco Castellano, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Matthew Malkan, Danilo Marchesini, Sara Mascia, Charlotte Mason, Amata Mercurio, Emiliano Merlin, Themiya Nanayakkara, Laura Pentericci, Piero Rosati, Paola Santini, Claudia Scarlata, Michele Trenti, Eros Vanzella, Benedetta Vulcani, Chris Willott
Figure caption: Redshifts and observed H 160 magnitudes from a compilation of confirmed LBGs in the literature (Watson et al. 2015; Oesch et al. 2016; Hoag et al. 2018; Fujimoto et al. 2022) with clear continuum detections. Galaxy samples are color coded according to their confirmed redshifts: 7 ≤ z < 8 are highlighted in blue, 8 ≤ z < 9 in purple, and z > 9 in orange.
Paper: Early Results from GLASS-JWST. I: Confirmation of Lensed z ≥ 7 Lyman-break Galaxies behind the Abell 2744 Cluster with NIRISS
Authors: Guido Roberts-Borsani, Takahiro Morishita, Tommaso Treu, Gabriel Brammer, Victoria Strait, Xin Wang, Marusa Bradac, Ana Acebron, Pietro Bergamini, Kristan Boyett, Antonello Calabró, Marco Castellano, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Matthew Malkan, Danilo Marchesini, Sara Mascia, Charlotte Mason, Amata Mercurio, Emiliano Merlin, Themiya Nanayakkara, Laura Pentericci, Piero Rosati, Paola Santini, Claudia Scarlata, Michele Trenti, Eros Vanzella, Benedetta Vulcani, Chris Willott
Figure caption: Postage stamps of confirmed z > 7 LBGs in the Abell 2744 cluster field from NIRISS/WFSS observations. Each column shows results for a different filter (F115W, F150W, and F200W), while for each row top panels show the contamination-removed 2D drizzled stacks (over both grism orientations) as well as the spectral trace (gray lines) from which the 1D spectrum (blue lines and gray fill with associated scatter points and 1σ uncertainties) is optimally extracted (bottom panel). We also show the best-fit Grizli continuum model in red, as well as the contamination model in orange, the latter of which is accounted for in the extracted spectrum. Additionally, the HST photometry included in the fit are shown as black squares. We also indicate allowed wavelength windows for a suite of rest-frame UV emission lines, based on the spectroscopic redshift and associated 1σ uncertainty.
Paper: Early Results from GLASS-JWST. V: The First Rest-frame Optical Size–Luminosity Relation of Galaxies at z > 7
Authors: L. Yang, T. Morishita, N. Leethochawalit, M. Castellano, A. Calabrò, T. Treu, A. Bonchi, A. Fontana, C. Mason, E. Merlin, D. Paris, M. Trenti, G. Roberts-Borsani, M. Bradac, E. Vanzella, B. Vulcani, D. Marchesini, X. Ding, T. Nanayakkara, S. Birrer, K. Glazebrook, T. Jones, K. Boyett, P. Santini, V. Strait, X. Wang
Figure caption: Size comparison among five bands. Left: rest-frame optical (F444W) band size compared to those of the four other bluer bands, i.e., F356W (orange stars), F277W (green squares), F200W (blue triangles), and F150W (purple diamonds). The empty symbols represent those with a less-secure size determination, which are not used for calculating size ratio. Right: histograms of the size ratio distribution between F444W and each of the four bluer bands. In each panel, we indicate the median value of the distribution by the black dash line and reference (size ratio = 1) by the red dash line.
Paper: Early Results from GLASS-JWST. I: Confirmation of Lensed z ≥ 7 Lyman-break Galaxies behind the Abell 2744 Cluster with NIRISS
Authors: Guido Roberts-Borsani, Takahiro Morishita, Tommaso Treu, Gabriel Brammer, Victoria Strait, Xin Wang, Marusa Bradac, Ana Acebron, Pietro Bergamini, Kristan Boyett, Antonello Calabró, Marco Castellano, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Matthew Malkan, Danilo Marchesini, Sara Mascia, Charlotte Mason, Amata Mercurio, Emiliano Merlin, Themiya Nanayakkara, Laura Pentericci, Piero Rosati, Paola Santini, Claudia Scarlata, Michele Trenti, Eros Vanzella, Benedetta Vulcani, Chris Willott
Figure caption: A false-color image of the Abell 2744 cluster using JWST/NIRISS, HST/WFC3, and HST/ACS filters (red = F200W+F160W+F150W+F140W; green = F125W+F115W+F105W+F814W; blue = F606W+F435W), and the location of our three targeted z ≥ 7 candidate galaxies shown in magenta squares (if spectroscopically confirmed at z ≥ 7) or white circles (if confirmed as a low-z interloper). The locations of the z − and Y − dropout protocluster galaxies are marked in yellow triangles (adopting the Zheng et al. 2014 nomenclature), for reference.
Paper: Early Results from GLASS-JWST. V: The First Rest-frame Optical Size–Luminosity Relation of Galaxies at z > 7
Authors: L. Yang, T. Morishita, N. Leethochawalit, M. Castellano, A. Calabrò, T. Treu, A. Bonchi, A. Fontana, C. Mason, E. Merlin, D. Paris, M. Trenti, G. Roberts-Borsani, M. Bradac, E. Vanzella, B. Vulcani, D. Marchesini, X. Ding, T. Nanayakkara, S. Birrer, K. Glazebrook, T. Jones, K. Boyett, P. Santini, V. Strait, X. Wang
Figure caption: Example of the size measurement of a galaxy (ID = 2574, z = 7.38) in the F444W (rest-frame optical; upper) and F150W (UV; bottom) bands using Galight. In each panel, from left to right, the columns represent the (1) observed data, (2) best-fit model image, (3) normalized residual map, and (4) surface brightness profiles in 1D and its residuals.
Paper: Early Results from GLASS-JWST. V: The First Rest-frame Optical Size–Luminosity Relation of Galaxies at z > 7
Authors: L. Yang, T. Morishita, N. Leethochawalit, M. Castellano, A. Calabrò, T. Treu, A. Bonchi, A. Fontana, C. Mason, E. Merlin, D. Paris, M. Trenti, G. Roberts-Borsani, M. Bradac, E. Vanzella, B. Vulcani, D. Marchesini, X. Ding, T. Nanayakkara, S. Birrer, K. Glazebrook, T. Jones, K. Boyett, P. Santini, V. Strait, X. Wang
Figure caption: Size–luminosity distribution of galaxies observed in five NIRCam bands from F444W to F150W band, corresponding to rest-frame optical (∼4800 Å) to UV (∼1600 Å). The x-axes represent the absolute magnitude measured in each band, and the y-axes represent the effective radius measured by Galight using the Sérsic model. The solid points, solid lines, and shadow region in each panel represent, respectively, the data, the best fit of the size–luminosity relation, and the 1σ uncertainty range of the derived relation. The color transparency of the data points indicates the redshift. The empty circles show galaxies with less-secure size determinations, displayed here for completeness but not used for fitting. The red dash lines represent the best fits obtained in the F444W band. The black solid and dashed–dotted lines in the F150W panel show the relation derived from HST data by Shibuya et al. (2015; z ∼ 8) and Huang et al. (2013; z ∼ 5) at a similar rest-frame wavelength, respectively. The horizontal black dotted line in each panel indicates the PSF size (FWHM/2) for reference.
Paper: An Empirical Approach to Selecting the First Growing Black Hole Seeds with JWST/NIRCam
Authors: Andy D. Goulding, Jenny E. Greene
Figure caption: Examples of the assumed spectral energy distributions in the NIRCam bands. Left panel provides the “Median NLS1” spectrum from Constantin & Shields (2003), which has f  λ  ∝ λ −1.21 and is flatter and more shallow than the median quasar spectrum of substantially more-massive BHs typically observed in the SDSS (blue; Vanden Berk et al. 2001). The effect of increasing dust extinction (A  V  = 0.3, 0.7, 1.0) is additionally shown. Right panel shows the galaxy SEDs extracted from the JAGUAR mock combined with the NLS1-inspired AGN model for a range of galaxy stellar masses (logM * = 6.6–7.3, 7.3–8.0, 8.0–8.7) along with a range of Eddington ratios for the accreting BHs (λ Edd = 10−3, 0.1, 1.0). For an assumed M BH of 5 × 106 M ⊙, we expect to detect AGN with UV luminosities in the range M UV,1450 ∼ −16.6 to −19.1.
Paper: An Empirical Approach to Selecting the First Growing Black Hole Seeds with JWST/NIRCam
Authors: Andy D. Goulding, Jenny E. Greene
Figure caption: Comparison between the color distribution of the mock galaxies (grayscale) and galaxy+AGN models (colored contours) for M BH = 5 × 106 M ⊙ with a lognormal distribution in Eddington ratio between 0.1 and 1. Solid contours provide the 67%, 90%, and 99% distributions for AGN with no applied dust extinction (A V = 0) and dotted contours provide the 99% distribution for AGN with A V = 0.7. Galaxy masses run from M * ∼ 106.5–109 M ⊙, and 25% of galaxies harbor BHs accreting at or above 10% of their Eddington limit.
Paper: An Empirical Approach to Selecting the First Growing Black Hole Seeds with JWST/NIRCam
Authors: Andy D. Goulding, Jenny E. Greene
Figure caption: F150W-F200W vs. F200W-F277W color–color diagram and proposed AGN selection boxes assuming AGN fractions of f AGN = 0.05, 0.1, 0.25 for three potential science drivers: 90% purity (orange); 90% completeness (purple); balanced 75%–75% completeness to purity ratio (green). Grayscale region represents the distribution of AGN in our mock samples, and black contours provide the distribution of galaxy colors in the JAGUAR simulation with F090W, F115W < 1.4 nJy and F200W > 3.7 nJy.
Paper: Do High-spin High-mass X-Ray Binaries Contribute to the Population of Merging Binary Black Holes?
Authors: Monica Gallegos-Garcia, Maya Fishbach, Vicky Kalogera, Christopher P L Berry, Zoheyr Doctor
Figure caption: Summary of outcomes for the model with q crit following Belczynski et al. (2008) at Z ⊙/10. Points correspond to simulation outcomes for binaries ran with COSMIC. The left panel corresponds to donor masses within the range M donor = (25 ± 2.5)M ⊙, and the middle panel corresponds to M donor = (45 ± 2.5)M ⊙. In these panels, black rectangles correspond to the parameter space where the corresponding grid of MESA simulations for that donor mass results in BBHs. The right panel shows the fractions of each outcome as a function of donor mass. The hatched black bar corresponds to the fraction of BBHs for each donor mass given the grids of simulations ran with MESA. In all three panels, binaries that merged during CE are shown in green, systems that resulted in wide NSBHs are in yellow, and wide BBHs are in light blue.