adsabs/AstroCLIMB huggingface dataset:
Paper: Solar Evolution Models with a Central Black Hole
Authors: Earl P. Bellinger, Matt E. Caplan, Taeho Ryu, Deepika Bollimpalli, Warrick H. Ball, Florian Kühnel, R. Farmer, S. E. de Mink, Jørgen Christensen-Dalsgaard
Figure caption: H-R diagram showing the MS and subsequent evolution of the Sun with and without a central BH. The solid black line representing the normal case becomes dotted when the Sun has exhausted its central hydrogen abundance. The tracks with a BH become dotted when the accretion luminosity exceeds the luminosity from fusion. In all cases, the star expands into a red giant. Stars with lower BH masses than those shown proceed through these evolutionary phases as normal. Ages and the ZAMS are indicated; notice that a star with a BH dims rapidly before climbing redward of the RGB slowly over 7 Gyr. The normal Sun climbs the RGB much quicker over a span of about 50 Myr.
Paper: Solar Evolution Models with a Central Black Hole
Authors: Earl P. Bellinger, Matt E. Caplan, Taeho Ryu, Deepika Bollimpalli, Warrick H. Ball, Florian Kühnel, R. Farmer, S. E. de Mink, Jørgen Christensen-Dalsgaard
Figure caption: The transition between Bondi and Eddington accretion onto the central BH for ZAMS. Left panel: the accretion luminosity of a 1 M ⊙ star at ZAMS (white-dashed line) as a function of the mass of the PBH that it formed about. Middle panel: the difference in Bondi and Eddington luminosities at ZAMS. Right panel: the transition mass between Bondi and Eddington accretion at ZAMS. For small BHs, the accretion proceeds at the Bondi rate (Equation (4)); larger BHs accrete at the Eddington limit (Equation (3)). More massive stars have significantly higher Bondi–Eddington transition masses. Metallicity is very important in determining this transition in low-mass stars.
Paper: Solar Evolution Models with a Central Black Hole
Authors: Earl P. Bellinger, Matt E. Caplan, Taeho Ryu, Deepika Bollimpalli, Warrick H. Ball, Florian Kühnel, R. Farmer, S. E. de Mink, Jørgen Christensen-Dalsgaard
Figure caption: Central speed of sound (left), opacity (center), and density (right) for ordinary ZAMS models as a function of mass and shown for 1%, 10%, 100%, and 150% of the solar metallicity.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: The SPT+Base+H  0  (green) combination are less constraining of the TPM model than the Planck TTTEEE+Base+H  0  (gray) combination, where the Base data set includes Planck CMB lensing, BAO, and supernova data. In particular, broader posterior distributions for Ω b  h 2, Ω c  h 2, and n  s  allow for larger amplitude (more negative) transitions in the Planck mass with a best-fit value of Ω0 = −0.073 or about a 7.3% shift in the Planck mass. This shift in the Planck mass is compensated for by a large increase in n  s  (n  s  = 1.003 ± 0.016) and allows for higher values of H 0 (﹩{H}_{0}={71.94}_{-0.85}^{+0.86}﹩ km m−1 Mpc−1) and lower values of S 8 (﹩{S}_{8}={0.802}_{-0.023}^{+0.022}﹩) than the TPM fit to Planck TTTEEE+Base+H  0 . Because the Planck mass is allowed larger amplitude transitions, there is less need for shifts in the c 0 parameter, which acts as an equation of state parameter for dark energy in the late Universe, to raise H 0 to match the H 0 prior better. This results in a preferred value of c 0 closer to 0. In both the SPT and Planck cases, the timing of the transition, x  T , and the rapidity of the transition, σ, are unconstrained by the data. Notably, the SPT+Base+H  0  constraints of S 8 from ΛCDM (red) are lower than the corresponding case for TPM, suggesting that the TPM model is not doing better on clustering than ΛCDM for this data combination.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: Allowing the helium fraction to vary within the TPM model when fit to Planck TTTEEE+Base+H  0  (dark blue) opens up the degeneracy between the sound horizon, r *, and H 0 to match the degeneracy found when the TPM model is fit to SPT+Base+H  0  (green). Note that the preferred values of the helium fraction found by this fit are not physical, but this test illuminates the differences between fitting the SPT and Planck data. The helium fraction only enters the CMB calculations in the ionization fraction of electrons and primarily affects the photon damping scale, k  D . Larger amplitude transitions in the TPM model lead to suppressed power on small angular scales. Both the Planck and SPT small angular scale anisotropy data disfavor this suppression in power, meaning other parameters have to shift to compensate. For the TPM model fit to SPT+Base+H  0 , this can be compensated for by increasing n  s  to have more primordial power on small scales. However when the TPM model is fit to Planck TTTEEE+Base+H  0  (gray) or SPT+Planck TT650TEEE+Base+H  0  (red), n  s  is restricted by the lower-multipole data in combination with the higher-multipole data, which prevents the model from finding higher H 0 and lower r * values. We cut the parameter values in the plot for Ω0 > 0.0035 for visualization purposes.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: The combination of SPT+Planck TT650TEEE+Base+H  0  (red) constrains the TPM model more tightly than either the Planck TTTEEE+Base+H  0  (gray) or SPT+Base+H  0  (green) data. While the SPT+Base+H  0  data prefer roughly 7% transitions in value of the Planck mass, the inclusion of Planck TT650TEEE restricts the amplitude of the transitions to be less than 5.1% at the 95% confidence level. Additionally, it also restricts the allowed parameter space of Ω b  h 2, Ω c  h 2, and n  s . While the inclusion of Planck TT650TEEE constrains the TPM model preferred values of H 0 to be lower than with SPT alone, the data still prefer H 0 = 70.65 ± 0.66 km m−1 Mpc−1 and S 8 = 0.815 ± 0.026. Because the inclusion of Planck TT650TEEE constrains Ω0 more tightly, the c 0 parameter, which acts as the dark energy equation of state in the late Universe, decreases to allow for a higher H 0 value to fit the H 0 prior. The preferred value of S 8 for the TPM fit to SPT+Planck TT650TEEE+Base+H  0  is slightly higher than the corresponding ΛCDM-preferred value of S 8 = 0.7956 ± 0.0099, suggesting that the TPM model is not doing better than ΛCDM (blue) on the clustering tension for these data. We cut the parameter values in the plot for Ω0 > 0.0035 for visualization purposes.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: Including RSD f σ 8 data results in minimal changes to the posterior parameter distribution functions, but including RSD data does remove the non-Gaussian tail present in the parameter posterior for S 8 for the TPM model fit Planck TTTEEE+Base+H  0 . In Figure 5 of B22, we showed that the part of the allowed parameter space where S 8 > 0.85 corresponds to later (closer to recombination) transitions in the Planck mass. This is supported by the slight restriction of allowed parameter space for x  T  to disfavor x  T  > −4 in the TPM fit to Planck TTTEEE+Base+RSD+H  0  relative to the case without the RSD likelihood. The RSD data still allow for parameter value of H 0 > 70 km m−1 Mpc−1 and S 8 < 0.8, which would alleviate both the Hubble and clustering tensions.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: The best-fit TPM model fit to Planck TTTEEE+Base+RSD+H  0  (blue) prefers an enhanced growth of structure compared to the best-fit ΛCDM model (red) to the same data. The data points (black) are BOSS DR12 fσ 8 constraints at redshifts 0.38, 0.51, and 0.61 (Alam et al. 2017). In the TPM model, later transitions in the Planck mass result in longer-wavelength modes experiencing enhanced gravity, which increases the amount of clustering on these scales. The RSD data rule out the late transitions that lead to values of S 8 ⪆ 0.85 (see Figure 4) because these transitions enhance the growth of structure to a point that is strongly disfavored.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Spectroastrometric analysis of the Hα emission within the central 3″ × 3″ diameter region. The upper portion of the left panel shows the 3″ × 3″ spectrum (black continuous line) together with the multicomponent fit of the emission line spectrum (red continuous line) in the Hα + [N II] λ λ6548, 6583 window. The Gaussian components denoting Hα NLR emission are shown by the green-shaded regions. The purple-shaded Gaussian components represent the [N II] λ λ6548, 6583 emission lines, and the orange-shaded Gaussian components describe the [S II] λ λ6716, 6731 emission line doublets. We adopt light-colored shading for the narrow core and dark shading for the blue wing components. The gray-shaded Gaussian components define three broad-line region (BLR) Gaussians B 0, B 1, and B 2. The lower portion of the left panel shows the normalized residual spectrum (black line), which is contained in the 3σ region (shaded red) across the entire wavelength range, representing the residuals divided by the error spectra. The corresponding 2D light profiles Σ2D of the Hα broad and wing components are shown in the right panels. From top to bottom, the panels describe the measured Σ2D profile, the best-fit Moffat model, and the residual maps normalized by the uncertainty. The red cross describes the AGN location, whereas the green cross highlights the flux-weighted centroid of Σ2D, i.e., the component’s location. The corresponding error-normalized residual maps show no systematic substructures, implying that both the Hα broad and wing components are spatially unresolved.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Mapping HE 0040-1105's ionized gas flux and kinematics across the host galaxy. The left panels show the maps extracted from the single-component [O III] model, and the right panels are those for Hα. From top to bottom, the panels show the emission line flux, rest-frame velocity v, and velocity dispersion σ, respectively. The EELR that is local to the galaxy (see Section 4.2.1) is highlighted by the red contour in panel (d). The contours of ionized gas outflow in the center (see Section 3.2) are shown as dashed cyan lines. In addition, we highlight the contours of the kinematic features analyzed in Section 3.3 where the red line in panel (b) describes the morphology of the receding shell C1, and the red line in panel (e) indicates the Hα emitting receding region C3. Both [O III] emission line nebulae have similar morphologies. However, while the Hα velocity field has a clear rotational pattern and a nucleated peak of the velocity dispersion, the [O III] shows a more chaotic motion with a velocity dispersion in C1 that is lower than average.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Kinematic modeling of HE 0040-1105's stellar (left columns) and Hα ionized gas (right columns) velocity field. From top to bottom, the panels show the velocities measured from the MUSE observations (see Sections 3.1 and 3.3.2), the tilted-ring model fitted to it, and the map with the residual velocities normalized by the uncertainty. In both cases, the thin rotating disk provides a good description of the velocity field, although the rotation axis between both host galaxy components is tilted by 53°.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Overview of the data sets and their spatial coverage. From left to right the panels show the FoV of VLT/MUSE, VLA, a zoom-in onto the nucleus in the HST/WFC3 UVIS F225W image, and the EVN image. While the MUSE and VLA observations cover a large fraction of the host galaxy, HST allows a zoom into the central few 100 pc of the galaxy. The radio interferometry from EVN ultimately resolves the innermost few 10 pc near the AGN. The object 25″ east of HE 0040-1105 is a foreground star.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Kinematical diagnostic (k-plot) comparing the line broadening vs. line shift, with a pencil-beam approach (pixel-by-pixel). The yellow contours show the 1σ–3σ confidence intervals predicted by CCA simulations, while the black points denote a diverse sample of central and isolated galaxies (see Gaspari et al. 2018). We overlay the results for the [O III] emitting ionized gas in the O1 outflow (blue circles), C1 shell (brown square), and isolated [O III] cloud C2a (green stars). We adopt similar but light-colored markers to denote the Hα-emitting gas clouds. The small gray and purple circles denote the ionized [O III] and Hα gas in the EELR. Most gas elements are within the ∼2σ CCA contours suggesting that our main features are likely experiencing turbulent multi-phase condensation, which will soon stimulate a rain back on the SMBH.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: BPT diagram showing the [O III] λ5007/Hβ vs. [N II] λ6583/Hα ratios for different regions across the entire ionized nebula. Left panel: [O III] flux map with the extraction of different regions shown by curved lines and arrows. The red cross denotes the AGN location. Right panel: the black dotted line represents the upper limit of ionization due to pure star formation. The region between the black dotted line and the black solid line represents ionization due to both star formation and AGN. The area within the black and gray solid lines represents ionization due to shock. Above the black and gray solid lines, the hard ionization photoionizing field from the AGN dominates the line ratios. The blue cross and black stars describe the regions O1 and C2a, respectively, and are plotted with error bars with similar colors. The green and brown dots represent the feature C1 and the EELR and are not plotted with error bars because they are spatially resolved. O1 resides between the composite and AGN-photoionized region within uncertainties. The EELR, C1, and C2a are photoionized by the AGN.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Multiwavelength view of region C1. Left panel: MUSE optical spectra extracted from a 3 × 3 spaxel region (in gray), along with its multi-Gaussian component fit (in red). The green-shaded Gaussian components represent the narrow core, which is a part of the EELR, whereas the dark brown-shaded components trace the red-wing component, corresponding to region C1. Right panel: HST/WFC3 near-UV image centered at 3350 Å. The green region describes the area covered by the deconvolved C1, and the white line denotes its centroids. A clumpy structure on the northeastern side of the nucleus is shaded with white to showcase its spatial location and morphology. C1 overlaps with the gas clumps on the north where S/N > 5. Such spatial coincidence indicates that C1 is a part of the clumpy region.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Spectroastrometric analysis of the multicomponent [O III] cloud C2. Lower left panel: 2D flux profile of [O III] with C2 being highlighted with a box (upper panel). Upper left panel: optical Hβ + [O III] spectrum extracted from a 9 × 9 spaxel aperture, and its multicomponent fit. The gray lines describe the data, and the blue and green-shaded Gaussian components correspond to the regions C2a and C2b, respectively (top panel). The residual spectrum is divided by the error spectrum. The brown-shaded region defines the residuals within 3σ and the red dotted line indicates a region with zero residual (bottom panel). Right panel: 2D Moffat modeling results for C2. From top to bottom, the panels show the measured Σ2D, the corresponding best-fit 2D Moffat model, and the residual maps normalized by the uncertainty. From left to right, the panels correspond to C2a and C2b. The blue and green crosses indicate the flux-weighted centroids of C2a and C2b. The Σ2D profile of C2a is well described by the Moffat PSF, whereas, for C2b, the Moffat model leads to high residuals.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Outflow energetics parameters vs. the shell thickness for different v out and different outflow geometries. (a) Mass outflow rates, (b) momentum injection rates, and (c) kinetic energy injection rates. The blue, purple, and yellow lines correspond to ﹩{v}_{\mathrm{out}}={v}_{\max }﹩, W 80/1.3, and v broad, respectively. We use solid lines to showcase the parameters derived for the shell geometry and dashed lines for the cone geometry. The red dashed line in (a) corresponds to the Hα-derived nuclear SFR. The green dotted line in (b) shows the momentum injection by the AGN radiation field, P AGN = L bol/c. The black lines in (c) show the 0.1% (dotted line), 1% (dashed line), and 10% (solid line) energy released from the AGN, respectively. The energy-driven mechanism is feasible. The brown-shaded region denotes the possible values of the jet power P jet.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: VLA continuum images of HE 0040-1105 in the central 3″. Left panel: the 6 GHz image with the yellow contour in the bottom left indicates the clean beam (0.″53 × 0.″27 and PA = −36.°9). Right panel: the 10 GHz image with yellow contour indicating the clean beam (0.″26 × 0.″17 and PA = −22°). Green contours correspond to the 5σ sensitivity levels at 35 and 40 μJy for the C- and X-bands, respectively. The spectroastrometric positions of the AGN, [O III] wing, and Hα components are highlighted as green, red, and cyan crosses, respectively.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: EVN contour image of HE 0040-1105 at 18 cm. The image shows four unresolved components. We identify the brightest component S0 with the galaxy nucleus and name the remaining components S1, S2, and S3. The synthesized beam is 24.9 × 10.7 mas at an 8.°97 PA and is shown on the left edge of the image as a gray-shaded ellipse. The contour levels are −30%, 30%, 40%, 50%, 60%, 70%, 80%, and 90% of the peak intensity 83.7 μJy beam−1. The positive contours are plotted with green lines, whereas the negative contours are indicated with red lines. The crosses describe the flux-weighted centroids of the AGN (red), the Hα blue wing (yellow), and the [O III] blue wing (cyan) emission. The associated error bars indicate the 3σ uncertainties of the respective locations determined using spectro-astrometry. Assuming the brightest spot in S0 originates from the AGN, S1 and S3 overlap with the flux-weighted centroids of the blue wings within their uncertainties.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Radio continuum spectrum for HE 0040-1105 between 880 MHz and 10 GHz, showing the variation of the integrated flux density values (millijansky) with frequency. Note that we include only the upper limit for the VLA FIRST survey. The black dashed line indicates the best-fitted power-law model to the radio spectrum within the frequency range 880 MHz–10 GHz, yielding a spectral index of α int,0.88–10 GHz = −1.30 ± 0.28. We ignored the EVN observation during the fitting procedure as it could capture only a small fraction of the source's flux density. The radio spectrum is most consistent with a steep spectrum component.
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Similar to the left panel of Figure 6, the left panel here shows the 3 × 3 spaxel aperture spectra extracted from C1 and their two-component modeling. The figure organization and symbols are similar to Figure 6 (left panel). The right panel shows the 9 × 9 spaxel aperture spectra extracted at the location of C2 together with the best-fit two-component model and the emission line spectra of the individual components. The figure organization and symbols are similar to the upper left panel of Figure 7.