adsabs/AstroCLIMB huggingface dataset:
Paper: Crustal Magnetic Fields Do Not Lead to Large Magnetic-field Amplifications in Binary Neutron Star Mergers
Authors: Michail Chabanov, Samuel D. Tootle, Elias R. Most, Luciano Rezzolla
Figure caption: Distributions on the (x, z) plane of the magnetic-field strength ∣B∣ from the HR simulations soon before merger. Magnetic-field lines are shown in yellow, while the left and right panels refer to the full and crust configurations, respectively.
Paper: Crustal Magnetic Fields Do Not Lead to Large Magnetic-field Amplifications in Binary Neutron Star Mergers
Authors: Michail Chabanov, Samuel D. Tootle, Elias R. Most, Luciano Rezzolla
Figure caption: Gravitational-wave strain in the ℓ = 2, m = 2 mode of the + –polarization extracted at ∼740 km for a source at and normalized to a distance of 100 Mpc and for the two configurations. Thick solid lines report the corresponding amplitudes.
Paper: Star Formation Laws and Efficiencies across 80 Nearby Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Adam K. Leroy, Eve C. Ostriker, Sharon Meidt, Erik Rosolowsky, Eva Schinnerer, Christine D. Wilson, Dyas Utomo, Francesco Belfiore, Guillermo A. Blanc, Eric Emsellem, Christopher Faesi, Brent Groves, Annie Hughes, Eric W. Koch, Kathryn Kreckel, Daizhong Liu, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Amy Sardone, Antonio Usero, Thomas G. Williams, Frank Bigiel, Alberto D. Bolatto, Mélanie Chevance, Daniel A. Dale, Jindra Gensior, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, María J. Jiménez-Donaire, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Lukas Neumann, Yu-Hsuan Teng, David A. Thilker
Figure caption: Left panel: the  molecular Kennicutt–Schmidt (mKS) relation across the PHANGS–ALMA sample. The density contours (40%–80%–95% levels) show the distributions of all 1.5 kpc scale regions with >3σ detections for both Σmol and ΣSFR, and the downward arrows show 3σ upper limits for ΣSFR (see Section 3). The solid black line shows the best-fit power-law model for all detections and upper limits above Σmol = 1 M ⊙ pc−2 (i.e., the nonshaded side for the contours and symbols), where there is minimal censoring on Σmol. The other colored lines show the best-fit model when using alternative SFR calibrations or CO-to-H2 conversion factors. The thin dotted lines mark linear relations with constant molecular gas depletion times of 0.1, 1, and 10 Gyr (top left to bottom right). Right panel: normalized histograms of the molecular gas depletion time t dep = Σmol/ΣSFR, color-coded similarly to the left panel. The median value and 16th–84th percentile range are marked by a dot and a horizontal bar beneath each histogram, with their values displayed to the left of each histogram.
Paper: Star Formation Laws and Efficiencies across 80 Nearby Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Adam K. Leroy, Eve C. Ostriker, Sharon Meidt, Erik Rosolowsky, Eva Schinnerer, Christine D. Wilson, Dyas Utomo, Francesco Belfiore, Guillermo A. Blanc, Eric Emsellem, Christopher Faesi, Brent Groves, Annie Hughes, Eric W. Koch, Kathryn Kreckel, Daizhong Liu, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Amy Sardone, Antonio Usero, Thomas G. Williams, Frank Bigiel, Alberto D. Bolatto, Mélanie Chevance, Daniel A. Dale, Jindra Gensior, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, María J. Jiménez-Donaire, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Lukas Neumann, Yu-Hsuan Teng, David A. Thilker
Figure caption: Similar to Figure 1, but here showing the mES relation (left panel) and normalized histograms of the SF efficiency per orbital time, ϵ orb = (ΣSFR/Σmol)t orb (right panel). The thin dotted lines in the left panel mark linear relations with constant ϵ orb of 1%, 10%, and 100% (bottom right to top left). Note that data below the Σmol threshold shown in Figure 1 are also excluded in the power-law fit for the mES (and all other) relations.
Paper: Star Formation Laws and Efficiencies across 80 Nearby Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Adam K. Leroy, Eve C. Ostriker, Sharon Meidt, Erik Rosolowsky, Eva Schinnerer, Christine D. Wilson, Dyas Utomo, Francesco Belfiore, Guillermo A. Blanc, Eric Emsellem, Christopher Faesi, Brent Groves, Annie Hughes, Eric W. Koch, Kathryn Kreckel, Daizhong Liu, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Amy Sardone, Antonio Usero, Thomas G. Williams, Frank Bigiel, Alberto D. Bolatto, Mélanie Chevance, Daniel A. Dale, Jindra Gensior, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, María J. Jiménez-Donaire, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Lukas Neumann, Yu-Hsuan Teng, David A. Thilker
Figure caption: Similar to Figure 1, but here showing the FFTR relation (left panel) and normalized histograms of the SF efficiency per free fall time, ﹩{\epsilon }_{\mathrm{ff}}=({{\rm{\Sigma }}}_{\mathrm{SFR}}/{{\rm{\Sigma }}}_{\mathrm{mol}}){\bar{t}}_{\mathrm{ff}}﹩ (right panel). The thin dotted lines in the left panel mark linear relations with constant ϵ ff of 0.1%, 1%, and 10% (bottom right to top left).
Paper: Star Formation Laws and Efficiencies across 80 Nearby Galaxies
Authors: Jiayi Sun, 嘉懿 孙, Adam K. Leroy, Eve C. Ostriker, Sharon Meidt, Erik Rosolowsky, Eva Schinnerer, Christine D. Wilson, Dyas Utomo, Francesco Belfiore, Guillermo A. Blanc, Eric Emsellem, Christopher Faesi, Brent Groves, Annie Hughes, Eric W. Koch, Kathryn Kreckel, Daizhong Liu, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Amy Sardone, Antonio Usero, Thomas G. Williams, Frank Bigiel, Alberto D. Bolatto, Mélanie Chevance, Daniel A. Dale, Jindra Gensior, Simon C. O. Glover, Kathryn Grasha, Jonathan D. Henshaw, María J. Jiménez-Donaire, Ralf S. Klessen, J. M. Diederik Kruijssen, Eric J. Murphy, Lukas Neumann, Yu-Hsuan Teng, David A. Thilker
Figure caption: Similar to Figure 1, but here showing the PR relation (left panel) and normalized histograms of the feedback yield, ϒfb = P DE/ΣSFR (right panel). The thin dotted lines in the left panel mark linear relations with constant ϒfb of 102, 103, and 104 km s−1 (top left to bottom right).
Paper: Removal of Hot Saturns in Mass–Radius Plane by Runaway Mass Loss
Authors: Daniel P. Thorngren, Eve J. Lee, Eric D. Lopez
Figure caption: Three views of the observed exoplanet population (our selection criteria are described in Section 2). The top two panels show the conventional view (mass/radius vs. period) of the sub-Jovian desert, which is the shaded area (following Mazeh et al. 2016). We are primarily interested in the low-density boundary seen in mass–radius space (constant 0.1 g cm−3, black dotted line, bottom panel), which is roughly equivalent to the black dotted line in the middle panel and partially overlaps with the mass–period desert. We have also plotted model radius lines (see Section 2) for various incident fluxes demonstrating that planets with density less than 0.1 g cm−3 can exist but nevertheless do not in nature.
Paper: Removal of Hot Saturns in Mass–Radius Plane by Runaway Mass Loss
Authors: Daniel P. Thorngren, Eve J. Lee, Eric D. Lopez
Figure caption: The model planets at 1 Gyr, varying the stellar mass (left), bulk metallicity (center), and XUV-mass-loss efficiency (right), color-coded with respect to the rate of mass loss. Symbols and the dotted line follow the convention of Figure 3. For the metallicity Z pl, we take the ±1σ value away from the mean of the mass–metallicity distribution reported by Thorngren & Fortney (2018). This range is broad; for example, a Saturn-mass planet with −1σ metallicity has 15M ⊕ of metal, whereas at +1σ it has 50M ⊕. With all else equal, planets appear larger around more-massive (and brighter) parent stars or for those with low bulk metallicity. These planets are more susceptible to mass loss and so the closest-in planets (triangles) are lost by 1 Gyr. At larger orbital distances, these puffier planets still survive owing to lower XUV flux and fill up the high mass (≳140M ⊕) and large radii (≳1.5R  J ). The right column shows that our results are only modestly sensitive to mass-loss efficiency with the region to the left of the density boundary being largely vacated between low and high η.
Paper: Removal of Hot Saturns in Mass–Radius Plane by Runaway Mass Loss
Authors: Daniel P. Thorngren, Eve J. Lee, Eric D. Lopez
Figure caption: The thermal and mass evolution of a Saturn-mass planet at various semimajor axes. The planet bulk metallicity was tuned to Z  p  = .225 to match Saturn’s radius (blue x) at 4.5 Gyr and 9.58 au. If instead placed at 0.07 au, the planet experiences modest mass loss over Gyr timescales, but the radius is mostly unchanged. At 0.05 au, the planet loses mass at increasing rates until the runaway mass loss strips the envelope from the planet. For part of this process the planet is also filling its Roche lobe (dotted line), ejecting about 40 M ⊕ and expanding the semimajor axis out to .095 au. Even after Roche lob overflow fully stops (the overflow appears intermittent; see Valsecchi et al. 2014 and Section 3), XUV-driven mass loss continues to erode what little is left of the H/He envelope.
Paper: Nucleosynthesis in Outflows from Black Hole–Neutron Star Merger Disks with Full GR(ν)RMHD
Authors: Sanjana Curtis, Jonah M. Miller, Carla Fröhlich, Trevor Sprouse, Nicole Lloyd-Ronning, Matthew Mumpower
Figure caption: Left: azimuthally averaged density (left half) and Y  e  (right half) of each of the four disk models going from the least massive disk (top) to the most massive disk (bottom). The snapshots are taken at approximately 50 ms. Right: average Y  e  of gravitationally unbound material as a function of latitude and time. The angle off the equator is given by ∣90° – θ  bl  ∣, where θ  bl  is the Boyer–Lindquist angle. Note the different end times for the four simulations.
Paper: Nucleosynthesis in Outflows from Black Hole–Neutron Star Merger Disks with Full GR(ν)RMHD
Authors: Sanjana Curtis, Jonah M. Miller, Carla Fröhlich, Trevor Sprouse, Nicole Lloyd-Ronning, Matthew Mumpower
Figure caption: Mass-weighted abundance as a function of mass number for outflows from all four accretion disks. Solar abundances from Arnould et al. (2007) are shown in gray and scaled to approximately match Disk 1 around the second peak.
Paper: Nucleosynthesis in Outflows from Black Hole–Neutron Star Merger Disks with Full GR(ν)RMHD
Authors: Sanjana Curtis, Jonah M. Miller, Carla Fröhlich, Trevor Sprouse, Nicole Lloyd-Ronning, Matthew Mumpower
Figure caption: From top to bottom: histograms representing the electron fraction, mean dynamical timescale, and entropy of the ejecta for all four BH–disk systems.
Paper: Elucidating the Formation of Ethynylbutatrienylidene (HCCCHCCC; X1A′) in the Taurus Molecular Cloud (TMC-1) via the Gas-phase Reaction of Tricarbon (C3) with the Propargyl Radical (C3H3)
Authors: Alexander M. Mebel, Marcelino Agúndez, José Cernicharo, Ralf I. Kaiser
Figure caption: Potential energy surfaces (PESs) of three reactions, (a) l-HCCC + HCCCH, (b) l-HCCC + H2CCC, and (c) C3+ C3H3, leading to ethynylbutatrienylidene (HCCCHCCC) and/or its isomers. Relative energies are given in kJ mol−1. The most favorable pathway to p3 is shown in red.
Paper: Elucidating the Formation of Ethynylbutatrienylidene (HCCCHCCC; X1A′) in the Taurus Molecular Cloud (TMC-1) via the Gas-phase Reaction of Tricarbon (C3) with the Propargyl Radical (C3H3)
Authors: Alexander M. Mebel, Marcelino Agúndez, José Cernicharo, Ralf I. Kaiser
Figure caption: Molecular orbitals involved in the barrierless addition of the tricarbon molecule to the propargyl radical.
Paper: Elucidating the Formation of Ethynylbutatrienylidene (HCCCHCCC; X1A′) in the Taurus Molecular Cloud (TMC-1) via the Gas-phase Reaction of Tricarbon (C3) with the Propargyl Radical (C3H3)
Authors: Alexander M. Mebel, Marcelino Agúndez, José Cernicharo, Ralf I. Kaiser
Figure caption: Hydrocarbon molecules detected in circumstellar and interstellar environments. Atoms are color coded in black (carbon) and gray (hydrogen). Molecules only detected in circumstellar envelopes are denoted with an “*.”
Paper: Elucidating the Formation of Ethynylbutatrienylidene (HCCCHCCC; X1A′) in the Taurus Molecular Cloud (TMC-1) via the Gas-phase Reaction of Tricarbon (C3) with the Propargyl Radical (C3H3)
Authors: Alexander M. Mebel, Marcelino Agúndez, José Cernicharo, Ralf I. Kaiser
Figure caption: Molecular structures, point groups, electronic wave functions, and relative stabilities of three lowest energy C6H2 isomers. Optimized bond lengths are given in Å and angles are given in degrees. Relative energies are shown in bold, in kJ mol−1.
Paper: Optical Spectropolarimetry of Binary Asteroid Didymos–Dimorphos before and after the DART Impact
Authors: Stefano Bagnulo, Zuri Gray, Mikael Granvik, Alberto Cellino, Ludmilla Kolokolova, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: Symbols joined by dashed curves show the synthetic broadband polarization values as a function of the phase angle obtained from FORS2 spectropolarimetric observations. Solid curves represent the best fits obtained with Equation (2) on the data obtained prior to impact. Different symbols and colors refer to different filters as shown in the legend. The error bars would have a size about the same as the symbol size or smaller and hence are not shown. The dotted lines represent the ±1σ uncertainties around the best fits on the B- and R-filter values. The vertical dotted line shows the phase angle at the time of impact. Data for the I filter are not plotted, as they would largely overlap with the data in the R filter. Postimpact data are marked with the time at which they were obtained, measured in hours from impact. The inset shows the fractional variation of the observed polarization as explained in the text.
Paper: Simultaneous Millimeter-wave, Gamma-Ray, and Optical Monitoring of the Blazar PKS 2326-502 during a Flaring State
Authors: J. C. Hood II, A. Simpson, A. McDaniel, A. Foster, P. A. R. Ade, M. Ajello, A. J. Anderson, J. E. Austermann, J. A. Beall, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, J. E. Carlstrom, C. L. Chang, P. Chaubal, H. C. Chiang, T-L. Chou, R. Citron, C. Corbett Moran, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, W. Everett, J. Gallicchio, E. M. George, N. Gupta, N. W. Halverson, G. C. Hilton, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, L. Knox, A. T. Lee, D. Li, A. Lowitz, G. Madejski, M. Malkan, J. J. McMahon, S. S. Meyer, J. Montgomery, T. Natoli, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, S. Patil, C. Pryke, C. L. Reichardt, J. E. Ruhl, B. R. Saliwanchik, K. K. Schaffer, C. Sievers, G. Smecher, A. A. Stark, C. Tucker, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, J. A. Zebrowski, L. Zhang
Figure caption: Light curves for PKS 2326-502. Top: Fermi-LAT. Middle: SMARTS optical R. Bottom: SPTpol 150 GHz. Evident by eye are long-timescale correlation between millimeter-wave and γ-ray observations and short-timescale correlation between optical and γ-ray observations. For reference, MJD 56,400 was calendar date 2013 April 18. The time gaps in the SPTpol data are periods during the austral summer when the primary 500 deg2 field was not observed to avoid solar contamination.
Paper: Simultaneous Millimeter-wave, Gamma-Ray, and Optical Monitoring of the Blazar PKS 2326-502 during a Flaring State
Authors: J. C. Hood II, A. Simpson, A. McDaniel, A. Foster, P. A. R. Ade, M. Ajello, A. J. Anderson, J. E. Austermann, J. A. Beall, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, J. E. Carlstrom, C. L. Chang, P. Chaubal, H. C. Chiang, T-L. Chou, R. Citron, C. Corbett Moran, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, W. Everett, J. Gallicchio, E. M. George, N. Gupta, N. W. Halverson, G. C. Hilton, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, L. Knox, A. T. Lee, D. Li, A. Lowitz, G. Madejski, M. Malkan, J. J. McMahon, S. S. Meyer, J. Montgomery, T. Natoli, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, S. Patil, C. Pryke, C. L. Reichardt, J. E. Ruhl, B. R. Saliwanchik, K. K. Schaffer, C. Sievers, G. Smecher, A. A. Stark, C. Tucker, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, J. A. Zebrowski, L. Zhang
Figure caption: Year-1 boxcar-smoothed light curves (left column), smoothed and detrended light curves (middle column), and detrended CCFs (right column). The gray shaded regions represent the 1σ, 2σ, and 3σ contours of simulated CCFs.
Paper: Simultaneous Millimeter-wave, Gamma-Ray, and Optical Monitoring of the Blazar PKS 2326-502 during a Flaring State
Authors: J. C. Hood II, A. Simpson, A. McDaniel, A. Foster, P. A. R. Ade, M. Ajello, A. J. Anderson, J. E. Austermann, J. A. Beall, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, J. E. Carlstrom, C. L. Chang, P. Chaubal, H. C. Chiang, T-L. Chou, R. Citron, C. Corbett Moran, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, W. Everett, J. Gallicchio, E. M. George, N. Gupta, N. W. Halverson, G. C. Hilton, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, L. Knox, A. T. Lee, D. Li, A. Lowitz, G. Madejski, M. Malkan, J. J. McMahon, S. S. Meyer, J. Montgomery, T. Natoli, J. P. Nibarger, G. Noble, V. Novosad, Y. Omori, S. Padin, S. Patil, C. Pryke, C. L. Reichardt, J. E. Ruhl, B. R. Saliwanchik, K. K. Schaffer, C. Sievers, G. Smecher, A. A. Stark, C. Tucker, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, J. A. Zebrowski, L. Zhang
Figure caption: Same as Figure 2 but for year 2.
Paper: JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58
Authors: Vasily Kokorev, Shuowen Jin, Georgios E. Magdis, Karina I. Caputi, Francesco Valentino, Pratika Dayal, Maxime Trebitsch, Gabriel Brammer, Seiji Fujimoto, Franz Bauer, Edoardo Iani, Kotaro Kohno, David Blánquez Sesé, Carlos Gómez-Guijarro, Pierluigi Rinaldi, Rafael Navarro-Carrera
Figure caption: Top: cutouts showing galaxies A and B, in HST H band and all available JWST/NIRCam SW and LW observations. Each stamp is 8.″0 per side. The galaxy A is largely undetected at λ obs < 2 μm in both HST and JWST images, except clumpy substructures. A spiral shape becomes apparent in the F277W image and beyond. Bottom left: best-fit EAZY SED of the entire galaxy A. Blue line show the best-fit model, red circles represent the template fluxes, and the black points show the measured flux density. For added clarity we re-plot the SED of galaxy B in light green. Bottom right: A compilation of the redshift probability distributions (p(z)) for the combined source A (blue), and B (light green). The spectroscopic redshift of A, from Sun et al. (2022) and F. Bauer et al. (2023, in preparation) is indicated by the dashed black line.
Paper: JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58
Authors: Vasily Kokorev, Shuowen Jin, Georgios E. Magdis, Karina I. Caputi, Francesco Valentino, Pratika Dayal, Maxime Trebitsch, Gabriel Brammer, Seiji Fujimoto, Franz Bauer, Edoardo Iani, Kotaro Kohno, David Blánquez Sesé, Carlos Gómez-Guijarro, Pierluigi Rinaldi, Rafael Navarro-Carrera
Figure caption: Top: color composite images constructed by using SW (left) and LW (right) NIRCam channels. Each cutout is 8.″0 × 8.″0. On the SW stamp, we show the 3σ, 5σ, 7σ, and 12σ contours from the ALMA 1.15 mm image. The synthesized ALMA beam size is shown at the bottom right. On the LW stamp, we overlay the segmentation map, in white, and names of our sources of interest. Green labels denote the catalog number and photometric redshifts of neighboring sources. The physical scale shown corresponds to the image plane. Bottom: best-fit EAZY SEDs of each component belonging to the dusty spiral (A1, A2, and A3) and the compact quiescent companion (B). Black and gray points show the measured flux density and upper limits, respectively. Red circles represent the template fluxes.
Paper: JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58
Authors: Vasily Kokorev, Shuowen Jin, Georgios E. Magdis, Karina I. Caputi, Francesco Valentino, Pratika Dayal, Maxime Trebitsch, Gabriel Brammer, Seiji Fujimoto, Franz Bauer, Edoardo Iani, Kotaro Kohno, David Blánquez Sesé, Carlos Gómez-Guijarro, Pierluigi Rinaldi, Rafael Navarro-Carrera
Figure caption: Left: spatially resolved A  V  map of the 4.″0 stamp centered on galaxy A and B. Black contours correspond to the 3σ, 5σ, 7σ, and 12σ levels of the ALMA continuum. In the bottom we also show the average PSF FWHM of SW and LW images. Lime crosses show positions of A1, A2, A3, and B. Solid lime lines highlight the segment borders. Top right: Classification of our segments A1, A2, A3, the combined galaxy A, and its companion B by using the U − V and V − J rest-frame colors. The UVJ galaxy selection separation from Williams et al. (2009) is shown as a dashed red line. The uncertainty on the colors fits within the marker size. Bottom right: spatially resolved UVJ diagram for the 4 × 4 arcsec2 regions around the spiral galaxy. The diamonds denote spatial bins corresponding to galaxy A, and circles belong to galaxy B. The color coding represents the source plane distance (in kiloparsecs) from the centroid of galaxy A. The center of galaxy B is highlighted with a red star. A typical uncertainty on the UVJ colors is shown with the error bars on the bottom left of each figure.
Paper: JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58
Authors: Vasily Kokorev, Shuowen Jin, Georgios E. Magdis, Karina I. Caputi, Francesco Valentino, Pratika Dayal, Maxime Trebitsch, Gabriel Brammer, Seiji Fujimoto, Franz Bauer, Edoardo Iani, Kotaro Kohno, David Blánquez Sesé, Carlos Gómez-Guijarro, Pierluigi Rinaldi, Rafael Navarro-Carrera
Figure caption: SED of the HST-dark galaxy A in the unlensed and higher-z cases. Overlaid are NIRCam and MIRI detection limits of major surveys (Bagley et al. 2022; Bezanson et al. 2022; Casey et al. 2022). Quoted detection limits are 5σ depth for extended emission within a D = 0.″5 aperture. At the bottom of the figure we show the transmission curves of the relevant NIRCam and MIRI filters.
Paper: JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58
Authors: Vasily Kokorev, Shuowen Jin, Georgios E. Magdis, Karina I. Caputi, Francesco Valentino, Pratika Dayal, Maxime Trebitsch, Gabriel Brammer, Seiji Fujimoto, Franz Bauer, Edoardo Iani, Kotaro Kohno, David Blánquez Sesé, Carlos Gómez-Guijarro, Pierluigi Rinaldi, Rafael Navarro-Carrera
Figure caption: Best-fit multicomponent STARDUST fit to galaxy A. The SED is separated into two components—stellar emission (blue), dust (red). The combined emission (gray line and shaded areas), the observed photometry (red squares) are also displayed. The dashed purple line shown best-fit of the generalized form of the MBB function.
Paper: Meet the Parents: The Progenitor Binary for the Supermassive Black Hole Candidate in E1821+643
Authors: James Paynter, Eric Thrane
Figure caption: Left: the distribution of kick velocity v  k  for the three models considered Section 3 describing the environment of the supermassive binary black hole merger that formed E1821+643. Right: the distribution of line-of-sight velocity v los for the same three models.
Paper: Meet the Parents: The Progenitor Binary for the Supermassive Black Hole Candidate in E1821+643
Authors: James Paynter, Eric Thrane
Figure caption: A corner plot showing the posterior distribution for parameters describing the progenitor binary for E1821+643 for the best-explanation “hot” model. The priors are indicated by dashed curves while the solid curves represent the posterior distribution.
Paper: Meet the Parents: The Progenitor Binary for the Supermassive Black Hole Candidate in E1821+643
Authors: James Paynter, Eric Thrane
Figure caption: The distribution for dimensionless black hole spin χ (left) and the tilt angle θ between the black hole spin vector and the orbital angular momentum of the supermassive binary black hole. Different models for the merger environment are denoted with different colors.