adsabs/AstroCLIMB huggingface dataset:
Paper: The First X-Ray Polarization Observation of the Black Hole X-Ray Binary 4U 1630–47 in the Steep Power-law State
Authors: Nicole Rodriguez Cavero, Lorenzo Marra, Henric Krawczynski, Michal Dovčiak, Stefano Bianchi, James F. Steiner, Jiri Svoboda, Fiamma Capitanio, Giorgio Matt, Michela Negro, Adam Ingram, Alexandra Veledina, Roberto Taverna, Vladimir Karas, Francesco Ursini, Jakub Podgorný, Ajay Ratheesh, Valery Suleimanov, Romana Mikušincová, Silvia Zane, Philip Kaaret, Fabio Muleri, Juri Poutanen, Christian Malacaria, Pierre-Olivier Petrucci, Ephraim Gau, Kun Hu, Sohee Chun, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, 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, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Paolo Soffitta, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: (a) NICER (2–10 keV) and NuSTAR (3–50 keV) spectra of the HSS (black) from Paper I and from the current SPL Period 1 (blue) and Period 2 observations (green). The spectra were unfolded using a unit constant model for both instruments. (b) Hardness–intensity diagram from NICER data of the HSS (black) and SPL state Period 1 (blue) and Period 2 (green), in 8 s intervals. Data from all previous NICER observations of 4U 1630–47 are shown in gray. Rates have been normalized as if all 52 of NICER’s FPMs were pointing at the source.
Paper: The First X-Ray Polarization Observation of the Black Hole X-Ray Binary 4U 1630–47 in the Steep Power-law State
Authors: Nicole Rodriguez Cavero, Lorenzo Marra, Henric Krawczynski, Michal Dovčiak, Stefano Bianchi, James F. Steiner, Jiri Svoboda, Fiamma Capitanio, Giorgio Matt, Michela Negro, Adam Ingram, Alexandra Veledina, Roberto Taverna, Vladimir Karas, Francesco Ursini, Jakub Podgorný, Ajay Ratheesh, Valery Suleimanov, Romana Mikušincová, Silvia Zane, Philip Kaaret, Fabio Muleri, Juri Poutanen, Christian Malacaria, Pierre-Olivier Petrucci, Ephraim Gau, Kun Hu, Sohee Chun, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, 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, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Paolo Soffitta, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: X-ray light curves of 4U 1630–47. (a) MAXI light curve between MJD 59800 (2022 August 9) and MJD 60025 (2023 March 22). The flux in the 2–20, 2–4, and 4–20 keV energy bands are reported in black, orange, and purple, respectively. The gray-shaded region corresponds to the observation reported in Paper I when the source was in the HSS while the regions shaded in blue (Period 1) and green (Period 2) correspond to the observation reported in this paper when the source was in the SPL state. (b) From top to bottom: IXPE, NICER, and NuSTAR light curves from 2023 March 10 to March 14. Observations of Periods 1 and 2 are shown by the blue and green data points, respectively, with a sudden flux increase at around MJD 60014.57 indicated by the vertical dashed line.
Paper: The First X-Ray Polarization Observation of the Black Hole X-Ray Binary 4U 1630–47 in the Steep Power-law State
Authors: Nicole Rodriguez Cavero, Lorenzo Marra, Henric Krawczynski, Michal Dovčiak, Stefano Bianchi, James F. Steiner, Jiri Svoboda, Fiamma Capitanio, Giorgio Matt, Michela Negro, Adam Ingram, Alexandra Veledina, Roberto Taverna, Vladimir Karas, Francesco Ursini, Jakub Podgorný, Ajay Ratheesh, Valery Suleimanov, Romana Mikušincová, Silvia Zane, Philip Kaaret, Fabio Muleri, Juri Poutanen, Christian Malacaria, Pierre-Olivier Petrucci, Ephraim Gau, Kun Hu, Sohee Chun, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. García, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, 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, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Paolo Soffitta, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie
Figure caption: Best linear fits with respect to energy of thermal component (black), power-law component for Fit 1 (red), and power-law component for Fit 2 (yellow). The shaded regions show the 1σ confidence intervals.
Paper: Black Hole Mergers Driven by a Captured Low-mass Companion
Authors: Stephen Lepp, Rebecca G. Martin, Bing Zhang
Figure caption: Maximum eccentricity, ﹩{e}_{\max }﹩, for varying initial inclination, i, and orbital radius of the companion, r. The upper four panels each show a b = 10, 30, 50 and 250 R ⊙ and for a companion mass m = 0.5 (top left), 1 (top right), 2 (middle left), and 4 M ⊙ (middle right). The lower left panel explores the effect of the eccentricity of the tertiary mass with a b = 50 R ⊙ and m = 4 M ⊙. The lower right panel is the same as the upper right panel except m 1 = 30 M ⊙, m 2 = 8 M ⊙, and m = 38/60 M ⊙. The radii where the librating region (r c2, left arrow along the top) and stationary inclination (r c1, right arrow along the top) reach i = 180° are marked by black arrows at i = 180°. The location where the GR precession is just canceled by the three-body precession for the black hole binary (where i s = 90°), r c3, is marked by a black arrow at i = 90°. Note that for a b = 250 R ⊙ all the arrows are off the right side of the plot.
Paper: Black Hole Mergers Driven by a Captured Low-mass Companion
Authors: Stephen Lepp, Rebecca G. Martin, Bing Zhang
Figure caption: Same as Figure 3 except the colors represent the value of f speedup given by Equation (20). This shows how many times faster the binary merger is expected to be due to the KL cycle compared to a circular orbit binary. The color black is used for all speedup factors greater than 10,000 though individual pixels may have significantly faster speedups. The largest speedup in the m = 4 M ⊙ panel for a b = 30, 50, and 250 R ⊙ are 7 × 104, 8 × 105, and 7 × 108, respectively.
Paper: Black Hole Mergers Driven by a Captured Low-mass Companion
Authors: Stephen Lepp, Rebecca G. Martin, Bing Zhang
Figure caption: The ﹩i\cos \phi -i\sin \phi ﹩ phase plane (first and third columns) and the ﹩{e}_{{\rm{b}}}\cos \phi -{e}_{{\rm{b}}}\sin \phi ﹩ phase plane (second and fourth columns) for a binary composed of m 1 = m 2 = 30 M ⊙ with orbital separation of a b = 10 R ⊙ and initial binary eccentricity e b = 0.2. The companion has mass m = 1 M ⊙ and orbits the binary in an initially circular orbit with orbital radius of radii r = 5 (top left), 10 (top right), 10.5 (lower left), and 11.5 a b (lower right). The third body begins with ϕ = 90° with inclination in the range 0°–180° with an interval of 10°. The green lines show prograde circulating orbits, and the blue lines show retrograde circulating orbits. The red and cyan lines show librating orbits with initial inclination below and above the stationary inclination, respectively. The black stars show the initial conditions.
Paper: Black Hole Mergers Driven by a Captured Low-mass Companion
Authors: Stephen Lepp, Rebecca G. Martin, Bing Zhang
Figure caption: Eccentricity evolution of a black hole binary with masses m 1 = m 2 = 30 M ⊙ orbiting with semimajor axis a b = 10 R ⊙ and initial eccentricity e b = 0.2. The third body has mass m = 1 M ⊙ and orbits with semimajor axis r = 10 a b with initial inclination of i = 50°, 90°, 93°, 110°, 150°, and 170° and initial nodal phase angle ϕ = 90°.
Paper: J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467
Authors: Shuo Huang, Ryohei Kawabe, Kotaro Kohno, Toshiki Saito, Shoichiro Mizukoshi, Daisuke Iono, Tomonari Michiyama, Yoichi Tamura, Christopher C. Hayward, Hideki Umehata
Figure caption: Left: EAZY fit of the JWST photometry (black circles and error bars). The median and 16th–84th percentile ranges of the SED at the best-fit redshift z best are shown with the solid lines and shaded regions, respectively. The insert panels show the PDFs of photometric redshift. The photometric redshifts discussed in Section 3.3 are 16th–50th–84th percentile values of the PDF. The vertical dashed lines mark the spectroscopic redshift identification. Right: X-ray-to-millimeter SED fit of J0107a at z spec = 2.467. For the total SED model and individual components, we show median and 16th–84th percentile ranges with the solid lines and shaded regions, respectively.
Paper: J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467
Authors: Shuo Huang, Ryohei Kawabe, Kotaro Kohno, Toshiki Saito, Shoichiro Mizukoshi, Daisuke Iono, Tomonari Michiyama, Yoichi Tamura, Christopher C. Hayward, Hideki Umehata
Figure caption: The zeroth, first, and second moment maps of the CO(4–3) emission line of J0107a. Also shown are the GalPak3D/3D-Barolo models and corresponding residual maps. The black ellipse in the top left panel indicates the beam size. The residual in the first moment map with redshifted velocity on the northeast edge overlaps with a horn-like structure in the zeroth-moment map (Figure 1(b), the right panel) and may originate from gas inflow. However, the S/N is low so further observation is needed to confirm it.
Paper: Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations
Authors: Ke Fang, Kohta Murase
Figure caption: Same as Figure 3 but in ﹩{E}_{\nu }^{2.5}{{\rm{\Phi }}}_{\nu }﹩ and including all γ-ray sources. The source emission is evaluated based 63 sources from 3HWC, 539 sources from 4FGL, 64 sources detected by WCDA and 75 sources detected by KM2A from 1LHAASO, and 77 sources from HGPS. The IceCube isotropic flux is overlaid (in black hatched band; Aartsen et al. 2020).
Paper: Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations
Authors: Ke Fang, Kohta Murase
Figure caption: Measured and derived all-flavor neutrino flux from GDE averaged over the full sky (warm colors, unhatched) comparing with models, including the KRA models (Gaggero et al. 2015), the CRINGE models (Schwefer et al. 2023), and the HNR model (Ahlers & Murase 2014).
Paper: VERTICO and IllustrisTNG: The Spatially Resolved Effects of Environment on Galactic Gas
Authors: Adam R. H. Stevens, Toby Brown, Benedikt Diemer, Annalisa Pillepich, Lars Hernquist, Dylan Nelson, Yannick M. Bahé, Alessandro Boselli, Timothy A. Davis, Pascal J. Elahi, Sara L. Ellison, María J. Jiménez-Donaire, Ian D. Roberts, Kristine Spekkens, Vicente Villanueva, Adam B. Watts, Christine D. Wilson, Nikki Zabel
Figure caption: The H I (top panel) and H2 (bottom panel) fractions of TNG50 and TNG100 galaxies as a function of stellar mass at z = 0. Only galaxies with m * ≥ 109 M ⊙ and ﹩\mathrm{SFR}\geqslant 0.05\,{{M}_{\odot }\,{yr}}^{-1}﹩ are included (without any environmental subsampling). Hex bins show the number density of TNG50 galaxies. Lines are the running median (thick) and 16th and 84th percentiles (thin) for TNG50 (solid) and TNG100 (dashed). Points with approximate errors compare the VERTICO and HERACLES galaxies that we use in this paper (a subset of the full surveys; see Figure 1 of Zabel et al. 2022). We show these observational data for reference, but we do not necessarily expect the simulation medians to align closely with them (but they should be closer to HERACLES than VERTICO). Individual points from our TNG50 cluster and field samples, shown, can be respectively compared to VERTICO and HERACLES.
Paper: VERTICO and IllustrisTNG: The Spatially Resolved Effects of Environment on Galactic Gas
Authors: Adam R. H. Stevens, Toby Brown, Benedikt Diemer, Annalisa Pillepich, Lars Hernquist, Dylan Nelson, Yannick M. Bahé, Alessandro Boselli, Timothy A. Davis, Pascal J. Elahi, Sara L. Ellison, María J. Jiménez-Donaire, Ian D. Roberts, Kristine Spekkens, Vicente Villanueva, Adam B. Watts, Christine D. Wilson, Nikki Zabel
Figure caption: Resolved scaling relations for TNG50 galaxies per their field and cluster samples (and a high-mass field subsample), compared respectively with HERACLES and VERTICO. Lines are running medians in 0.2 dex bins of Σ*. Shaded regions cover the 16th to 84th percentiles (not shown for the high-mass field subsample). The left column accounts for all pixels in both the observations (provided they were detected in stellar emission) and simulations, setting non-detections in either ΣH I or ﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}﹩ in the observations to zero, which are accounted for in the percentiles. The right column removes any non-detections in the observations by cutting out any pixels that would fall below the axes as plotted. The lower boundary of each axis represents the 1st percentile of all gas-detected pixels (irrespective of whether the pixel is a detection in Σ*) across both observational surveys. This boundary also represents the cut in gas surface density applied to TNG50 in the right-hand panels, as to emulate a detection threshold. The top two panels show the one-dimensional histograms of Σ* for pixels in each sample, normalized by the number of galaxies in that sample. The y-axis in the top right panel is stretched by a factor of 2 for clarity.
Paper: VERTICO and IllustrisTNG: The Spatially Resolved Effects of Environment on Galactic Gas
Authors: Adam R. H. Stevens, Toby Brown, Benedikt Diemer, Annalisa Pillepich, Lars Hernquist, Dylan Nelson, Yannick M. Bahé, Alessandro Boselli, Timothy A. Davis, Pascal J. Elahi, Sara L. Ellison, María J. Jiménez-Donaire, Ian D. Roberts, Kristine Spekkens, Vicente Villanueva, Adam B. Watts, Christine D. Wilson, Nikki Zabel
Figure caption: Individual H I sequences for the nine most H I-deficient galaxies among VERTICO analogs in TNG50. Points are pixels from the TNG50 galaxies, with thick solid lines the running median of those points. The thin, solid red line that repeats in each panel is the median for the TNG50 field sample. Each dashed line is the running median for the VERTICO galaxy that the TNG50 galaxy is matched to, based on its stellar mass and distance from the star-forming main sequence. NGC4533 lacks any detected resolved H I. The lower bound of the y-axis in each panel is ∼0.5 dex lower than what is detected in VERTICO galaxies.
Paper: VERTICO and IllustrisTNG: The Spatially Resolved Effects of Environment on Galactic Gas
Authors: Adam R. H. Stevens, Toby Brown, Benedikt Diemer, Annalisa Pillepich, Lars Hernquist, Dylan Nelson, Yannick M. Bahé, Alessandro Boselli, Timothy A. Davis, Pascal J. Elahi, Sara L. Ellison, María J. Jiménez-Donaire, Ian D. Roberts, Kristine Spekkens, Vicente Villanueva, Adam B. Watts, Christine D. Wilson, Nikki Zabel
Figure caption: Same as Figure 3 but for the resolved molecular-gas main sequence.
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: Orange: joint distribution of the merger and formation redshifts of detected BBH events at GWTC-3 sensitivity, inferred under the default population model (with the α  τ  = −1 delay time distribution). We average over the population posterior uncertainty. The orange shading represents the probability density in a given (z merge, z form) hexagonal bin. For reference, the top and right axes show the corresponding lookback times. Green: at each z merge, the 90, 99, and 99.9 percentiles of the conditional z form distribution (see Equation (4)). These represent the maximum formation redshift that we expect to probe given ﹩{ \mathcal O }(10)﹩, ﹩{ \mathcal O }(100)﹩, and ﹩{ \mathcal O }(1000)﹩ observations at a fixed z merge.
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: EDFs of the merger redshifts (gray) and formation redshifts (green and blue) of the 69 BBH events in GWTC-3 for fixed delay time distributions. The green filled band assumes a delay time distribution with power-law slope α  τ  = −1, and the blue, unfilled band assumes α  τ  = −0.35. The solid green and dashed blue lines denote the median EDF, and bands enclose the 50% and 90% credibilities. Both delay time distributions assume ﹩{\tau }_{\min }=10\,\mathrm{Myr}﹩. The number of BBH events in GWTC-3 with a (merger or formation) redshift above a given value is denoted in the right-hand y-axis.
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: Similar to Figure 1, but binned by formation metallicity. This shows that the delay time distribution shifts toward longer delay times for high metallicities.
Paper: Open Magnetic Fields in the Martian Magnetosphere Revealing Dipole-like Intrinsic Magnetic Fields at Mars
Authors: Shaosui Xu, Janet G. Luhmann, David L. Mitchell, Tristan Weber, David A. Brain, Yingjuan Ma, Shannon M. Curry, Gina A. DiBraccio, Jasper Halekas, Suranga Ruhunusiri, Christian Mazelle, Robert J. Lillis, Benoit Langlais
Figure caption: The occurrence rates of the open topology as a function of the IMF clock angle (﹩{\tan }^{-1}{B}_{z}/{B}_{y}﹩) at different altitudes, (a) 200–300 km, (b) 300–500 km, (c) 500–700 km, red for “open-day,” blue for “open-night,” and black for all open fields. (d)–(f) The averaged local B  r /∣B∣ of open fields in geographic coordinates (with a bin size of 5° × 5°) as measured by MAVEN/MAG, limited to 200–300 km altitude, (d) for all subsolar geographic longitudes (SSL), (e) for southern strong crustal fields on the dayside (120° < SSL < 240°), and (f) for southern strong crustal fields on the nightside (SSL < 60° or SSL > 300°). The yellow dots and arrows in (e)–(f) indicate the ranges of SSL. The contours in (d)–(f) shows the radial component of modeled crustal magnetic fields at 250 km altitude (Langlais et al. 2019).
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: Inferred mean log10 metallicity as a function of redshift, assuming the default delay time distribution (α  τ  = −1; left panel) or a shallow delay time distribution (α  τ  = −0.35; right panel). We fix the standard deviation ﹩{\sigma }_{{\mathrm{log}}_{10}}﹩ of the metallicity distribution to 0.2 dex at each redshift, and assume three different functions for the BBH yield as a function of metallicity: high yield (pink), medium yield (green), and low yield (brown) as defined in Figure 4. The solid lines show the median ﹩\langle {\mathrm{log}}_{10}(Z/{Z}_{\odot })\rangle ﹩ at each z form and the shaded bands show the 50% and 90% credible regions. For comparison, we overplot three different measurements from the literature: Madau & Fragos (2017) as the dotted, light blue curve (MF17), and two of the variations from Chruślińska et al. (2021) as the dashed, yellow curve (CNBL21-1) and dotted–dashed gray curve (CNBL21-2).
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: Delay time distributions derived from all physics variations explored in van Son et al. (2022a). We show histograms of the delay times per 106 M ⊙ of stellar mass formed, assuming a flat-in-log distribution of metallicities, and bin sizes ﹩{\rm{\Delta }}\mathrm{log}{t}_{\mathrm{delay}}\,=\,0.2﹩. Thick dashed lines show the median for each formation channel and orange thin lines show the power laws used in this work.
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: Number of merging BBH systems formed per star-forming mass as a function of redshift z form, as inferred under three different delay time distributions with power-law slopes α  τ  = −1 (default, the green solid line), α  τ  = −0.7 (orange dashed line), and α  τ  = −0.35 (blue dotted–dashed line) and the Katsianis et al. (2021) UV SFR. The lines denote the median BBH yield at each formation redshift while the shaded bands enclose the 90% posterior probability.
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: Number of merging BBH systems formed per star-forming mass as a function of metallicity (i.e., the BBH yield) for the physics variations explored in van Son et al. (2022a) shown as the gray lines. We show analytical approximations of low (dotted), medium (dashed), and high (solid line) BBH yields following Equation (8).