adsabs/AstroCLIMB huggingface dataset:
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Illustration of the photometric quality cuts in two example fields. (a) A typical field (SMC Field 15, Figure 4(b)); (b) a field with strong background emission (LMC Field 11, Figure 4(c)). Upper rows: spatial distribution of sources; lower rows: optical CMD of the same sources. Left: full photometric catalog (.st.fits); middle left: sources removed owing to lack of detection in all bands; middle right: sources removed after failing quality cuts; right: final catalog (.vgst.fits).
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Summary of how ASTs are placed for two example fields, one source density dominated (SMC Field 15; top) and one background density dominated (LMC Field 11; bottom). Left: source density maps; middle: background density maps; right: positions of ASTs generated before adding supplementary sources.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: CMDs of the input ASTs for background-density-dominated Scylla LMC Field 11 (15891_LMC-5389ne-11134), in UV (left), optical (middle), and IR (right).
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Stacked CMDs in the optical (top), UV (middle), and IR (bottom) bands for the LMC (left) and SMC (right) for the vgst catalogs. Sources brighter than the average 50% completeness limits are shown in color contours, and fainter sources are gray. Average photometric uncertainties as a function of flux, computed from the ASTs, are shown as error bars. Saturation limits in each band are shaded gray in the optical panels (all others are much brighter). Reddening vectors (gray, top right) and PARSEC isochrones are overlaid, indicating the main-sequence stellar mass range typical of our photometric catalogs.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Optical CMDs for all SMC fields from the vgst catalogs. Saturation limits in each band are shaded gray in each panel. Reddening vectors (gray, upper right corner) and PARSEC isochrones are overlaid, indicating the main-sequence stellar mass range typical of our photometric catalogs (same as Figure 11). We indicate the number of filters obtained for each field in the lower right corners.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Optical CMDs for all LMC fields from the vgst catalogs. Saturation limits in each band are shaded gray in each panel. Reddening vectors (gray, upper right corner) and PARSEC isochrones are overlaid, indicating the main-sequence stellar mass range typical of our photometric catalogs (same as Figure 11). We indicate the number of filters obtained for each field in the lower right corners.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Demonstration of simple reddening analysis of Scylla optical CMDs. In panels (a) and (b), we zoom in to the RGB of two example fields, SMC_21 and LMC_11. Two regions of the CMD are highlighted, and the reddening metric is computed by dividing the number of sources in the red box by the total number of sources in both boxes. In panel (c), we compare this RGB reddening metric with the dust mass surface density (C. J. R. Clark et al. 2023), finding a positive correlation. The two example fields from panels (a) and (b) are highlighted with black outlines.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: A comparison of optical CMDs from Scylla and ground-based surveys within Scylla (vgst; left), SMASH (middle), and VMC (right). For the ground-based surveys, we extract all sources within a single Scylla field (SMC_17) and apply no quality cuts. In each panel, we overlay PARSEC isochrones, indicating the main-sequence stellar mass range typical of our photometric catalogs.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: A summary of the completeness, bias, and uncertainty (σ) for all Scylla fields. In the left column, we plot completeness as a function of flux for the Scylla observing bands. In the right column, we plot bias (black lines), with shading corresponding to ±1σ.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: The difference in observed magnitude as a function of flux for fields that overlap spatially in Scylla. The black lines indicate the median difference in bins of decreasing flux (increasing magnitude), and the color-shaded regions denote ±1σ within each band. We overplot the results of the ASTs (bias+uncertainty) for each field in each panel and observe that the differences are all within measured uncertainties.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Left: 50% completeness as a function of source density for each band in fields that are source density dominated. Right: 50% completeness as a function of background density for each band in fields that are background density dominated.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Example SEDs of sources from different regions on a CMD. Left: an optical CMD of SMC Field 15 (15891_SMC-4292sw-13841) with 10 randomly selected sources in each of the three regions (young main sequence: blue; RGB: pink; dim main sequence: yellow). Right: SED of each source, colored by region on the CMD.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: The TPF of TESS Sector 61 for HD 69464, alongside aperture masks (red rectangles) corresponding to different C con ranging from 1% to 9% with a step of 2% are presented in panels (a)–(e). The position of HD 69464 is denoted by a red pentagram, while nearby contaminating stars within the aperture masks are represented by white pentagrams. Panels (f)–(i) show the fitting parameters of SLF variability as functions of C con. Compared with the results at C con = 1%, the value of ﹩\mathrm{log}{\alpha }_{0}﹩ exhibits a slight increase with rising C con, and the relative error remains below 3%, signifying a negligible impact from the C con. Regarding ν char and γ, the results are not significantly affected when C con ≤ 5%. However, when C con > 5%, significant deviations in ν char and γ are observed when compared to the results at C con = 1%.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: The pairwise relationships between ﹩\mathrm{log}({\alpha }_{0}\,[\mu \mathrm{mag}])﹩, log ν char, and γ for the residual amplitude spectra of stars of our sample. Each star is marked as a filled circle and color coded based on spectroscopic luminosity.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: Top panel: the logarithmic residual amplitude spectrum of the TESS short cadence photometric data for BD+36 4145 is shown in black, with the best-fit model obtained using Equation (5) depicted as the solid blue line. The red and white noise components are illustrated by the solid green line and red dashed lines, respectively. Bottom panel: posterior distributions from the Bayesian MCMC, with best-fit parameters.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Observed CTE-corrected magnitude variations as a function of chip gap distance. (a) On-sky spatial distribution of all vgst sources in SMC Field 41 (16235_SMC-286sw-34349). Sources in the lower 16th/upper 84th percentile of distances from the chip gap are highlighted in purple/green, respectively. The magnitude distributions of these sources in WFC3 UVIS filters F336W, F475W, and F814W are shown in panels (b), (c), and (d), respectively. The median values of each distribution are shown with a dashed line, and the 3σ magnitude uncertainties at 25 mag derived from ASTs in this particular field are shaded in blue (0.3, 0.09, and 0.15, respectively).
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: A sample field illustrating the selection process for the vgst quality cuts. Top left: first, we visually identify contaminant sources as indicated by diffraction spikes in the imaging footprint (blue). We then evaluate the sharpness, roundness, and crowding parameters of the full sample of stars and the diffraction spike sources, and we select ranges for these photometric quality parameters, which optimize the removal of diffraction spikes.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Accretion tori and photon shell of the Kerr BH. Upper left panel: the black region is the central BH with spin a = 0.9. There is ﹩r=\sqrt{{y}^{2}+{z}^{2}}﹩ and ﹩\theta =\arccos (z/r)﹩. Gray region is a corotating torus with angular momentum parameter ℓ                           D                        = 2.52 (the torus cusp is the outer ergosurface; light gray region). Yellow curve (σ ±) is the photon shell. Dashed and solid circles are sections of the spheres of fixed radius ﹩r={r}_{\mathrm{mso}}^{\pm }﹩ (red), green for ﹩r={r}_{\mathrm{mbo}}^{\pm }﹩, and blue for ﹩r={r}_{\gamma }^{\pm }﹩. On the equatorial plane, z = 0, the radii coincide with marginally stable circular orbit, marginally bounded circular orbit for counterrotating (+) and corotating (−) test particles, and photon circular orbits respectively, constituting the Kerr spacetime geodesic structure. The spheroidal surfaces r = constant, embedding the central BH, have been considered in our analysis to discuss the tori location in relation to the BH photon shell (Section 4). Upper right and bottom panels are a three-dimensional realization of the upper left panel. Bottom panel is a close-up view of the upper right panel. There is ﹩\{z=r\cos \theta ,y=r\sin \theta \sin \phi ,x=r\sin \theta \cos \phi \}﹩. The central black region is the BH; the yellow region is the photon shell. Spheres and sections of the spheres at fixed radii are also shown. The gray toroidal surface is the accretion disk.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Inversion surfaces and photon shell of the Kerr BH. Upper panels: Sections of the inversion surfaces with radius r   T   of the counterrotating flows (orange curves), where ﹩r=\sqrt{{y}^{2}+{z}^{2}}﹩ and ﹩\theta =\arccos (z/r)﹩, for different fluid specific angular momenta. Black region is the central BH. Gray region is the outer ergoregion. Radius r lim (dotted yellow curve) is defined in Equation (20). Radius r ( T ,Θ) is defined in Equation (25). Bottom panel: black sphere is the BH, gray surface is the outer ergosurface, yellow surfaces are the photon shell, and purple surface is the inversion surface for ℓ = 4.7. Dashed purple curve is the inversion surface on the equatorial plane. Yellow curves are null geodesics. There is ﹩\{z=r\cos \theta ,y=r\sin \theta \sin \phi ,x=r\sin \theta \cos \phi \}﹩.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Photon shell analysis and inversion points. Upper panels: Yellow region is the photon's shell. Black region is the central BH. Upper right panel is a close-up view of the upper left panel. Radii ﹩{r}_{* }^{\pm }﹩, with * = {mso, mbo, γ}, and ﹩{r}_{(* )}^{\pm }﹩ constraining the tori centers (see Table 1), coincide with the corotating and counterrotating geodesic structures' values. (± are for counterrotating/corotating momenta.) Notation ﹩{{\ell }}_{* }^{\pm }﹩ is for ℓ evaluated at radius ﹩{r}_{* }^{\pm }﹩ respectively. Spins are defined in Table 2. (See also Figure 6’s caption.) Radius r  λ , evaluated at different momenta (signed on the panel) is defined in Equation (14). The inversion radius r   T   is evaluated at different angle σ and counterrotating momenta as signed on the panels. Bottom left panel: solutions of the equation ﹩{r}_{\gamma }^{-}={r}_{{\boldsymbol{T}}}({\ell }^{+})﹩ in the plane (a, σ). Bottom right panel: impact parameter ℓ   T  (σ ±) solution of the equation σ   T   = σ ± as function of the radius r. σ   T   and r   T   are (σ, r) evaluated on the inversion surfaces, ℓ   T  (σ ±) is in Equation (27), and σ ± is introduced in Equation (18) and defines the photon shell.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Spherical photon orbit's radius r  λ  as function of a for relevant impact parameter values compared to fixed radii r. Black region is the BH. ﹩r={r}_{\epsilon }^{+}=2﹩ is the outer ergosurface (gray line). Radius r  λ , evaluated at different momenta (signed on the panel) is defined in Equation (14). The inversion radius r   T   (in upper panels) is evaluated at different angle σ and counterrotating momenta as signed on the panels. ( ± are for counterrotating/corotating momenta.) Notation ﹩{{\ell }}_{* }^{\pm }﹩ is for ℓ evaluated at radius ﹩{r}_{* }^{\pm }﹩, with * = {mso, mbo, γ}, coincident with the corotating and counterrotating geodesic structures' values. Spins (vertical lines in the panels) are listed in Table 2.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Spherical photon orbit's radius r  λ  as function of a and relevant impact parameter values. Left panel: black region is the central BH. Radius r  λ , evaluated at different impact parameter signed on the panel is defined in Equation (14). ( ± are for counterrotating/corotating momenta.) Here, ﹩{r}_{\epsilon }^{+}=2﹩ is the outer ergosurace on the equatorial plane. Notation ﹩{{\ell }}_{* }^{\pm }﹩ is for ℓ evaluated at radius ﹩{r}_{* }^{\pm }﹩, with * = {mso, mbo, γ}, coincident with the corotating and counterrotating geodesic structures' values. Spins (vertical lines in the panels) are listed in Table 2. Right panel: ﹩{{\ell }}_{* }^{-}﹩ are plotted as functions of a. Red curve is the parameter ℓ correspondent to r  λ  = 2.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of photon shell boundary on fixed spherical orbit radius r for different BH spin. Left panel: Carter constant q Θ, defined in Equation (11), evaluated on radius r lim (where ℓ = 0), defined in Equation (20), as function of the BH spin. Right panel: Functions σ ±(a, r) are evaluated at different radii signed on the panel and shown as function of the spin a. Angles σ ±, bounding the spacetime photon shell, are defined in Equation (18). Spins (vertical lines) are listed in Table 2. ﹩{r}_{\epsilon }^{+}(a,\sigma )﹩ is the outer ergosurface. The correspondent curve is the solution ﹩\sigma ={\sigma }_{\pm }(a,{r}_{\epsilon }^{+})﹩. Radii ﹩\{{r}_{\mathrm{mbo}}^{-},{r}_{\mathrm{mso}}^{-}\}﹩ coincide with the corotating marginally bounded and marginally stable orbit values.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of ℓ Θ as function of a, and extreme points. Central panel: Black region is the central BH, gray region is the outer ergoregion. Radius r  x , extreme of ℓ Θ as function of a, defined in Equation (12) and the corotating and counterrotating geodesic structures, radii ﹩{r}_{* }^{\pm }﹩, with * = {mso, mbo, γ}, and ﹩{r}_{(* )}^{\pm }﹩ containing the tori centers (see Table 1) are plotted as functions of the BH spin a. Left panel: Carter constant q Θ in Equation (11) and functions σ ± (inside panel) in Equation (18), defining the photons' shells, are evaluated on radius r  x  and plotted as functions of the BH spin. Right panel: parameter ℓ evaluated on ﹩{r}_{* }^{\pm }﹩ is also shown. (Notation Q • is for any quantity evaluated at radius r •.)
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of q Θ and ℓ Θ for relevant fixed values of the radius r. Carter constant q Θ and impact parameter ℓ Θ in Equation (11) are plotted as functions of the BH spin a for fixed radii coincident with the values of the corotating and counterrotating geodesic structures ﹩{r}_{* }^{\pm }﹩, with * = {mso, mbo, γ} as signed on the curves, and compared with and contrasted to the values of ﹩{{\ell }}_{* }^{\pm }﹩ the momenta of the geodesic structures. Spins signed on the panels (vertical lines) are defined in Table 2. Bottom left (right) panel is a close-up (extended) view of the upper right panel.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Photon shell analysis as function of the spherical orbit radius r and BH spin. Left panel: Angles σ ± of Equation (18), limiting the Kerr spacetime photon shell, are shown as functions of the radius r, for different BH spin signed on the curves. Right panel: solution of the equation σ ± = σ = constant in the plane (r, a). Radius r lim (where ℓ = 0) is in Equation (20). Spin ﹩{a}_{\gamma }^{\epsilon }﹩ is in Table 2. ﹩{r}_{\gamma }^{\pm }﹩ are the counterrotating and corotating photon circular orbit on the equatorial plane.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Carter constant q Θ and impact parameter ℓ Θ in Equation (11) are shown as functions of r for different spin values signed on the curves of the left panel. The limiting value ℓ Θ = 0 is also shown in the right panel as a dotted–dashed line.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of the photon spherical orbits r for a different impact parameter ℓ in different BH spacetimes. Function q Θ is defined in Equation (11). Functions σ ± in Equation (18), defining the photons' shells, are evaluated on radius r  λ , defined in Equation (14) (see also Equation (17)) and plotted as functions of the momentum ℓ for different spins signed on the curves.