adsabs/AstroCLIMB huggingface dataset:
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: Images of three disk galaxies (g7.08e11, g8.26e11, and g2.79e12) simulated by GASOLINE and GIZMO at z = 0. The dashed circle indicates the range of 15% virial radius. System names and codes are labeled on the left. Columns from left to right: 2D density map of gas in edge-on view with pixelized velocity vectors overlaid on top, 2D temperature map averaged by gas density in edge-on view, 2D metallicity map averaged by gas density in edge-on view, and 2D zoom-in density map of gas disk in face-on and edge-on views.
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: The temperature distribution of the inflow and outflow gas at different radii is depicted with varying colors indicating the density of gas particles. The 1D velocity dispersion of the halo, as well as the mass of total inflow/outflow gas within 2R vir, is denoted in each panel.
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: The 3D density profile of star and gas with different temperatures is compared across two simulations for three representative systems (g7.08e11, g8.26e11, and g2.79e12). The dark matter halo profile is shown in each panel for comparison with the profile of the hot gas halos. Solid lines and dashed lines denote samples run by GIZMO and GASOLINE, respectively.
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: Comparison of mock optical images of all 12 systems in this work in the wavelength bands i, v, and u. Here, we only plot the disk region with surface brightness lower than 26.5 mag arcsec−2.
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: The impact of stellar feedback on the inner halo dark density profile and baryon mass fraction. The y-axis gives the best-fitting value of the inner dark matter slope α within 0.01 R vir, and the x-axis is the corresponding virial mass at z = 0. Dots are galaxies in the NIHAO-I and NIHAO-UHD simulations, and the filled triangles are the corresponding galaxies run with GIZMO. The color is correlated with the baryon fraction within R vir, as labeled in the right vertical color bar.
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: Halo mass vs. stellar mass relation for galaxies with halo mass larger than 109.5 M ⊙. Shaded gray regions mark the observational results from the CFHTLenS galaxy lensing data (M. J. Hudson et al. 2014). As a comparison, results of all central galaxies from the TNG300-1 simulation (A. Pillepich et al. 2018), as well as two recent observation results of halo mass and stellar mass of the MW are also shown. Within each halo mass bin, the upper and lower limits of TNG300-1 represent the 1st and 99th percentiles, respectively.
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: Comparison of the hot CGM distribution in g8.26e11. Colors represent the volume density of gas with a temperature higher than 105 K. The streams in all four panels represent the flow distribution. The left two panels are in edge-on view, and the right two panels are in face-on view. The white dashed circle designates the halo virial radius.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Summary of the formation scenarios for the vertical X-ray emission of NGC 5084. Cosmic time increases from left to right. Top row: (1) Orientation change of AGN jet. Mergers, inflows, precession, and SMBH interactions can reorient the jet direction of an AGN over time; Central row: (2) Overpressured cocoon. AGN jet emission directed against the galactic disk can result in an expansion along the minor axis of the galaxy; Top: (3) Faded starburst. Circumnuclear starbursts can generate galactic winds, expelling hot gas in the direction vertical to the galactic plane. However, this scenario requires active star formation or at least a relatively young population of stars at the core, which is not observed (see Section 4.3).
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Detection of the X-ray extended emission around NGC 5084 without PSF deconvolution or adaptive smoothing. Left: Chandra/ACIS X-ray flux (0.3–2.0 keV) map rebinned to 12.2 × 12.2 arcsec2 (25 × 25 pixels) for visualization purposes. No PSF deconvolution or adaptive smoothing was applied (i.e., Voronoi binning). Yellow contours: 2σ and 3σ (dotted, dashed, respectively) detection limits as estimated by SAUNAS (see Section 3.1, for reference. Right: surface brightness profile of the non-PSF deconvolved, nonadaptively smoothed flux map (purple circles) and scaled Chandra/ACIS PSF (blue solid line). Red dashed circle and vertical line: SAUNAS 3σ radial detection limit. Silver solid circle and vertical line: surface brightness profile radial detection limit of the non-PSF deconvolved, non-adaptive smoothed flux map. Sky background subtraction was applied to the flux map and surface brightness profile. We remark that the spatial binning of the flux map in the left panel of Figure 11 is only for visualization purposes, and the surface brightness profile was generated based on the full resolution (0.″492) data set. See the legend for details.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Optical spectral energy distribution of NGC 5084 as detected by the 6dF survey and the APO/DIS observations. Top panel: 4300–7000 Å spectrum of the central 1.″5 slit (APO/DIS, blue and red channels, in color) and the 6.″7 radius fiber (6dF, black). Bottom left: details of the Hγ spectral range (4200–4550 Å), showing the core as detected by 6dF and APO/DIS, as well as the north, south, east, and west subregions avoiding the core. See the labels on each spectra. Bottom right: same as previous for the 6400–6800 Å(Hα) range. Vertical shadowed red lines represent the redshifted wavelengths of the typical absorption and emission lines in galaxies (Hβ, O III, Mg, Na I, Hα), for reference.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Detection of the X-ray extended lobes around NGC 5084 without Voronoi binning. Left: Chandra/ACIS X-ray flux (0.3–2.0 keV) map rebinned to 12.″2 × 12.″2 (25 × 25 pixels) for visualization purposes. PSF deconvolution was applied (see Section 2 and SAUNAS I). Color rectangles: fixed apertures to measure X-ray emission in the north (blue), west (red), south (green), and east (orange) lobes. Yellow contours: 2σ and 3σ (dotted, dashed, respectively) detection limits as estimated by SAUNAS (see Section 3.1 for reference. Right: color-coded histograms represent the event probability distributions for the background (gray) and the four lobe apertures. The p-values for the null hypothesis that the flux distributions in the lobe apertures are compatible with the background are represented in the legend.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: NGC 5084 color maps. Left panel: ground-based VLT/ATLAS g − i maps. Black contours represent the X-ray emission (see Figure 2). The dark blue square in the core represents the FOV in the right panel. Right panel: F475W–F702W color from Hubble WFPC2/WFC3 photometry. The circumnuclear disk is clearly visible in red. See the color bar for reference.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Morphology of the core of NGC 5084 obtained with Hubble. Top left: WFC3/UVIS F475W. Top right: WFPC2 F658N. Bottom left: WFPC2 F702W. Bottom right: F658N–F702W (proxy of the [N II, λ6548] + Hα emission). The area shown is 12.6 × 12.6 arcsec2 (1.82 × 1.82 kpc2 at a distance of 29.91 Mpc). See the scales and color bars for reference.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: Diffuse X-ray emission of NGC 5084 as detected with SAUNAS/Chandra in 0.3–1.0 keV (top), 1.0–2.0 keV (center), 2.0–8.0 keV (bottom). Left: optical gri color Pan-STARRS image (K. C. Chambers et al. 2016). Right: SAUNAS map of the diffuse X-ray emission, corrected for PSF, point sources, and sky background. Dashed and solid contours represent the 2σ and the 3σ detection levels of X-ray emission, represented in white (left panel) and black (right panel) for contrast.
Paper: SAUNAS. II. Discovery of Cross-shaped X-Ray Emission and a Rotating Circumnuclear Disk in the Supermassive S0 Galaxy NGC 5084
Authors: Alejandro S. Borlaff, Pamela M. Marcum, Pasquale Temi, Nushkia Chamba, S. Drew Chojnowski, Enrique Lopez-Rodriguez, Aneta Siemiginowska, Seppo Laine, Anton M. Koekemoer, Kelly N. Sanderson, Audrey F. Dijeau, Moire K. M. Prescott, Leslie Proudfit, Michael N. Fanelli
Figure caption: NGC 5084 morphological and environment scheme. Top left: main components at scales from 5 to 20 kpc, including the vertical and horizontal X-ray emission, its inner stellar disk, and the warped outer disk. Bottom left: NGC 5084 components at 0.1–5 kpc scales, including the symmetric radio lobes, the polar circumnuclear disk, and the SMBH at its center. Right panel: environment of NGC 5084. Each circle represents a satellite galaxy around NGC 5084. Original data from C. Carignan et al. (1997).
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: Three-dimensional view of the initial conditions (at T = 0h) of four different MFRs. The magnetic field lines are color-coded by their r-coordinates, with the yellow lines marking the boundary. The color contour on the semitransparent x = 0 plane displays the magnitude of B. (a) Regular MFR in the Lund model. Panels (b)–(d) are MFRs transformed into CHFRs using Equation (6). Specifically, panel (b) based on the Lund model, (c) on the GH model, and (d) on the SK model. Letters “R” and “L” in the figure indicate the local chirality of the MFRs.
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: The magnetic field and current density values across the radial direction of an MFR are represented by the colored solid curves, as produced by the four models described by Equations (1)–(5) with the parameters listed in Table 1. In units of current density j, nA = 10−9 Ampere. The vertical dashed line marks the position where r = R  0 .
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: Three-dimensional view of the time-evolution of a SK type CHFR at t = 1 and 3 hr. The magnetic field lines are color-coded in the same manner as in Figure 2. The black circle in panel (a) is a zoomed-in view of a spot in the transition region, to illustrate the directions of tension force (orange arrow) and generated flow (magenta arrows). The solid magenta arrows indicate the plasma flow components generated by the unwinding of the field. The two planes at (a) x = 200 Mm and (b) 600 Mm approximate the propagation front of the transition region, with the dashed–dotted arrows in panel (b) indicating the two directions of propagation.
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: Time evolution of the CHFR (SK model) shown with parameters extracted along the line x = 220, z = 0 (Mm). The solid lines representing parameter values are color-coded by time. The vertical red dashed lines indicate the boundary at r = R 0, while the black dashed lines at r = 48 Mm mark the location from which the values are extracted later along the axial direction. To highlight the variation, some parameters are plotted without their zero levels.
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: Time evolution of the SK-type CHFR shown with parameters extracted along the x-direction (y = 0, z = 48 Mm) in the CHFR. The solid lines representing these parameters are color-coded to represent the result at different evolution times. The vertical red dashed lines denote the boundaries of the transition region at x = x 0. The three black dashed lines are located at x = 140, 270, and 400 (Mm).
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: Radial dependence of plasma flow in SFRs. (a) Both uz and ut are averaged flow shear against the background, normalized by their local Alfvén speed v A. The lines are linear fit to these data points in the log–log plot, with line properties in the legend. The standard deviation of these fits for uz and ut is 0.04 and 0.05, respectively. (b) Averaged  ut ·  Bt  in SFRs plotted to linear radial distance. A line fit is also provided in this linear–linear plot, with a standard deviation of 0.2. (c) The size of each bin used to generate panels (a) and (b), plotted against the linear radial distance.
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: The left panels show test case 1 results of the CHFR evolution with parameters extracted along line y = 0, z = 48 (Mm). The vertical dashed lines are placed under the same criteria as used in Figure 6, where vertical black dashed lines are moved to where the 10% of the azimuthal B  φ  component remains in the B  φ  panel. The right panels show test case 2 results, with the vertical dashed lines placed at the same location as they are in Figure 6.
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: Time evolution of the case 2 CHFR using the GH model, presented in the same format as Figure 7. The left panels show results extracted along the radial direction at x = 220, z = 0 (Mm), with the vertical lines at 48 Mm (black) and R 0 (red). The right panels show results extracted along the line y = 0, z = 96 (Mm). The vertical dashed lines are in the same location as those in Figure 6.
Paper: Evolutionary Dynamics of Counterhelical Magnetic Flux Ropes
Authors: Ying-Dong Jia, Yu Chen, Yuxi Chen, Chen Shi, Qiang Hu, Yi Qi, Hanying Wei, C. T. Russell, Elizabeth A. Jensen, Xu Zhang
Figure caption: Streamlines of the current system  j  at t = 0 hr are plotted for the same four MFRs, as depicted in the same manner in Figure 2. The streamlines are selectively shown on each side of the symmetric CHFR to illustrate various potential connections.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Two-dimensional slices across the orbital plane of FLASH simulated inspiral and merger of LMC X-4 at three stages: early in the evolution (2.3 hr), at an intermediate time when the NS enters the stellar core (4.5 hr), and at a late time (13.8 hr) after the NS has settled in the center of the stellar core. Top panels: logarithm of gas density. Bottom panels: sum of specific kinetic and potential energy, ε = ε kin + ε grav, in units of 1016 cm2 s−2. The orange region corresponds to unbound material (ε > 0), and the green region corresponds to bound material (ε < 0).
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: The predicted radial evolution of the primary star as calculated by MESA using the mean LMC metallicity of [Fe/H] = −0.42. The initial mass of the model is 18M ⊙, with mass loss 2.4 × 10−7 M ⊙ yr−1 (S. Chernov 2020). The selected model (black symbol) is consistent with the properties given by M. Falanga et al. (2015) within 1σ. The model used for the hydrodynamical simulation performed with FLASH is marked with a turquoise symbol in the panel. At this stage, the donor has overfilled its Roche lobe, and its radial scale matches the forward-evolved separation a (dashed line).
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: The outward radial velocity histogram of the envelope debris expelled during the merger (with a total mass ≈1.4M ⊙). This is done by analyzing the velocity vectors and masses of each grid cell in the envelope with ε > 0 at t = 4.5 hr. Also plotted is the local escape velocity at the α = 1 critical radius, which is computed based on the enclosed mass of the initial model (Figure 4). This velocity is v  α=1 ≈ 1140 km s−1 and is shown as a vertical dashed line.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Relevant quantities required to estimate envelope unbinding during the merger, which are shown in mass coordinates. The binding energy of the primary’s stellar material exterior to a given mass coordinate (E grav, red line) and the change in orbital energy expected to be dissipated during the inspiral (ΔE orb, purple line) are plotted against the mass coordinate for the model used as the initial condition for the hydrodynamical simulation, with mass 18M ⊙ and neutron star mass ratio q ≈ 0.09. The mass coordinate at which the α = (E grav/ΔE orb) = 1 condition is satisfied is shown as a vertical dashed line.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Top left-hand panel: Comparison between ﹩{M}_{\star }^{\mathrm{gal}}﹩ and the adopted AGN-template-based M ⋆ values (﹩{\rm{\Delta }}\mathrm{log}{M}_{\star }=\mathrm{log}{M}_{\star }^{\mathrm{gal}}-\mathrm{log}{M}_{\star }﹩) for sources with preferred AGN models in W-CDF-S. Bottom left-hand panel: ﹩{\rm{\Delta }}\mathrm{log}{M}_{\star }﹩ vs. redshift. Top right-hand panel: Comparison between SFR measurements with and without FIR data in W-CDF-S. Bottom right-hand panel: ΔlogSFR vs. redshifts. The full and core samples are shown with empty and filled circles, respectively. X-ray detected and X-ray undetected DOGs are shown in blue and orange, respectively. The differences are generally within 0.5 dex and do not evolve with redshift. The median differences and σ NMAD are small, indicating that our M ⋆ and SFR measurements do not have significant biases.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: HMXBs in the context of luminous red novae (LRNe) and binary populations synthesis. The masses and radii of eclipsing HMXB systems (stars) studied by M. Falanga et al. (2015) and pre-CE transient observations for a sample LRNe progenitors (T. Matsumoto & B. D. Metzger 2022) are depicted (circles). Also shown are the progenitor population demographics of CE events generated with the rapid binary population synthesis code COMPAS version 02.27.05 (J. Riley et al. 2022). The COMPAS populations of primary stars include all systems involved in successful CE events, for which most companions are stars and white dwarfs (black outline), as well as CE events with NS accretors that either successfully ejected the envelope (blue region) or merge (purple region). The gravitational binding energy (in units of ergs) of a polytrope of index n = 3 with mass M and radius R (gray dashed lines) is shown for guidance.