adsabs/AstroCLIMB huggingface dataset:
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption:  Diffuse X-ray emission maps for ObsID 10957 to 10959: Soft X-ray emission is dominated by massive stars, with halos around some of the evolved ones, while more diffuse hot gas follows the spatial distribution of late O and/or early B MS stars. Again, the intriguing diffuse X-ray emission structure at R.A. = 308.48 and decl. = 41.375 appears with a clear spherical distribution of hard diffuse emission. Maps for ObsIDs 10960 to 10962: Note that a large part of ObsID 10961 is affected by scattering from Cyg X-3. The maps show clear evidence of X-ray halos around the massive evolved stars MT 516 (O6IV), Schutle #4 (O7III), and Schutle #5 (O7I + Ofpe + WN9). Diffuse X-ray emission maps for ObsID 10963 to 10964. The intrinsically X-ray-faint Schutle #73 (O8III + O8III) binary exhibits a diffuse X-ray halo, while the binary Schutle #11 (O5If + B0V) shows marginal evidence for a halo in the HR map. Of all the massive stars in the MS phase, the massive binary MT 771 (O7V + O9V) is the only one that has an associated diffuse X-ray halo. Another intriguing diffuse hard X-ray emission structure at R.A. = 308.765 and decl. = 41.585 appears to the south of A36. A more detailed examination of these intriguing results will be presented in future work.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption:  Maps for ObsIDs 10965 to 10968: The most conspicuous diffuse halo appears to be related to the strong wind–ISM interaction of WR 146. The structure spans a radial distance of more than 0.3 pc. Diffuse X-ray emission maps for ObsIDs 10969 to 10971: Here, the background radiation from Cygnus X-3 leads to scattering of X-ray photons over a large spatial scale, with an extension of about 3 pc (∼8′; see discussion in Section 4.2). The suspected pre-supergiant single star A20 (O8II) has an associated X-ray halo, although this is partially masked by the Cyg X-3 scattered background. Maps for ObsIDs 10972 to 10974: The left corner of ObsID 10974 shows a very intriguing partial view of an intense diffuse X-ray halo, which is also hard, contrary to what we observed around massive stars. Note in the flux and HR maps the existence of faint diffuse hard X-ray emission with a faint “jet-like” asymmetry.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption:  Diffuse X-ray emission maps for ObsIDs 10949 to 10950: The evolved massive binary system (O5If + B0V) Schutle #11 has a diffuse X-ray halo, while the evolved massive (O9I) Schutle #10 does not. In ObsID 10950, a large diffuse X-ray structure follows the spatial distribution of massive stars, even though all these stars do not have detectable intrinsic X-ray emission. This indicates that the diffuse X-ray emission is independent of any intrinsic X-ray emission of the massive stars, but not from their stellar wind properties. Maps for ObsIDs 10951 to 10953: The very massive evolved binary stars, Schutle #5 and #12, show clear X-ray halos. In ObsID 10953, a large diffuse structure is produced by the Cygnus X-3 X-ray binary dust scattering halo (see discussion in Section 4.2). Maps for ObsIDs 10954 to 10956: In the upper and middle maps, to the NW of Schutle #26, at R.A. = 308.48 and decl. = 41.375, there is an intriguing diffuse X-ray emission structure that does not correlate with any known massive star of the region. More interestingly, it has quite a hard spectrum (HR ≤ −0.15). The rest of the diffuse soft X-ray emission is clearly related to the massive stellar content of the region, especially the evolved stars. Note that MT 516 (O6IV + ?) produces harder diffuse emission than is typical of the other evolved massive stars. Colliding winds and diffusive motion of hot gas could be a plausible explanation for it.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: The dimmest F606W magnitude (blue-filled circle) at which each of the 94 M87 novae was observable via direct inspection of the epoch 1 images and the brightest magnitude (red-filled triangle) where each was not observable. The median (orange curve) and 1σ (15.9th and 84.1th) percentiles (magenta lines) of these points are plotted as a function of radial distance. Also plotted (the black curve) is the magnitude of a point source that would have S/N = 3 given the average local background noise measured in the F606W epoch 1 images at a given radial distance from the Galactic Center. The S/N = 3 line is observed to match the median line well outside of the inner 8″. See the text for details.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Top: the FOV of 53 HST pointings, and locations (cyan crosses) of all 94 novae detected in M87. North is up and east is left. Also shown as pink crosses are the 32 certain novae of Shara et al. (2016). The size of each nova’s circle scales linearly with the brightest observed F606W magnitude of that nova. Markers for novae whose peaks were not observed do not have a circle. The region encompassed by the large green circle is the inner circle defined in Section 2 and used throughout the paper. Bottom: a close-up of the nuclear region of M87 and its novae.
Paper: A 9 Month Hubble Space Telescope Near-UV Survey of M87. I. Light and Color Curves of 94 Novae, and a Redetermination of the Nova Rate 
Authors: Michael M. Shara, Alec M. Lessing, Rebekah Hounsell, Shifra Mandel, David Zurek, Matthew J. Darnley, Or Graur, Yael Hillman, Eileen T. Meyer, Joanna Mikolajewska, James D. Neill, Dina Prialnik, William Sparks
Figure caption: Top: the fraction of simulated novae detected once (blue) and twice (red) in F606W as a function of the percentage of template novae that are faint, fast (t 2 < 10  days and peak M(F606W) < −7). Bottom: the annual nova rate for the entirety of M87 implied by the recovery fraction, following the procedure of Section 4.5. Also shown (horizontal line) is the annual nova rate adopted in Section 4.5.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Simulated MaGIXS spectra in the 14–18 Å range showing multiple Fe XVII, Fe XVIII, O VII, and O VIII lines at constant log(T [K]) = 6.6. Maxwellian spectra are denoted by the black lines, while κ = 2 and 1.7 are denoted by red and violet, respectively. Note the spectra are scaled to keep the Fe XVII 15.01 Å/15.26 Å ratio constant, to highlight changes in other spectral lines.
Paper: KAPPA: A Package for the Synthesis of Optically Thin Spectra for the Non-Maxwellian κ-Distributions. III. Improvements to Ionization Equilibrium and Extension to κ < 2
Authors: Elena Dzifčáková, Jaroslav Dudík, Martina Pavelková, Božena Solarová, Alena Zemanová
Figure caption: Fe Maxwellian ionization equilibrium (top) and κ = 2 (bottom) in the vicinity of T = 106 K for the low electron density (full lines) and density-dependent equilibria for log(N e [cm−3]) = 9 (dotted–dotted–dotted–dashed lines) and 10 (dashed lines). Calculations for all distributions, including the Maxwellian, were based on the ionization cross sections of Hahn et al. (2017) and recombination rates from CHIANTI version 10.1.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Exemplification of the procedure for ObsID 10951. Left panels: the S/N significance map computed at the imposed condition of S/N = 12 and 16, respectively. Middle panels: the top-hat radius computed to reach the imposed S/N condition. Up to the borders of the observation, the top-hat radii increase as much as necessary to achieve the S/N, although once off the detector the signal falls to zero and can reduce the final S/N below the desired threshold. Right panels: X-ray diffuse emission flux (photons cm−2 s−1 arcsec−2) in the 0.5–7.0 keV energy range computed at S/N ∼ 12 and 16, respectively. Note that the peak of emission changes slightly for different S/N owing to the different binning, but by just 0.1 dex, or roughly 25%. At the limit of detection of the diffuse emission of log(F X) ≈ −8.64 or −8.69, for S/N = 12 or 16, respectively, the difference is only 0.05 dex, or about 11%. Black filled-star symbols indicate the evolved massive stars with conspicuous X-ray emission; open star symbols refer to evolved massive stars without X-ray emission; black filled and open circles indicate main-sequence massive stars, with and without detected X-ray emission, respectively. The list of massive stars in Cygnus OB2 was taken from Wright et al. (2015b).
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: ObsID 10951, illustrating the treatment of point sources and their exclusion from diffuse emission maps. The same analysis was applied to the whole set of observations. Left: the source PSF and readout streak intensity models that were computed on the list of detected sources in the observation. Right: the residual PSF wings image, which was computed as the difference between the observed source count image and the source+streak intensity models (left panel). Scale bars of both panels show the intensity range in which the image spans.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Exemplification of the HR analysis for ObsID 10951. The scale color bars show the range in HR that the image spans. Black filled and open star symbols indicate the evolved massive stars with and without intrinsic X-ray emission, respectively (from Wright et al. 2015b). Filled and open circles indicate MS massive stars, with and without intrinsic X-ray emission, respectively. Note that the diffuse gas follows the spatial distribution of the massive stellar population, regardless of whether they are strong X-ray emitters. The entire set of HR maps is shown in the Appendix.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Pulse height distribution of events for ObsID 10951 (black solid line), together with the stowed background normalized to match based on fluxes at energies of 7.47, 9.8, and 11 keV, where the sky has no emission (red dashed line). The weaker ∼2.1 keV emission line is also instrumental but was not used to match stowed observation events, and so it could be present in some diffuse X-ray spectra.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Downward-pointing arrows indicate maximum contributions of source wings to diffuse emission (see text for details). Red arrows indicate observations that are likely to be affected by gas and dust scattering processes related to the intense emission from Cygnus X-3. Black diamonds correspond to the median ratio of the wings to diffuse emission for the entire FOV of each observation.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Exemplification of the procedure for ObsID 10951. Left: source wing diffuse contribution in the 0.5–7.0 keV energy range computed using fixed smoothing radii for S/N ≥ 16 in the full band. Right: the ratio of wings to total diffuse emission has a maximum contribution of 0.24, which lies at the border of the map. The median contribution from wings all over the image is about 6%.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Cyg X-3 HR radial profiles of HR maps. Diffuse scattering extends to typical HR   ≈ −0.14 ± 0.07, where in the worst case it drops to the level of the ambient Cyg OB2 HR at a radial angular scale of ≈8′. Beyond this range we consider the influence of Cygnus X-3 scattering on the diffuse X-ray emission to be negligible.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: HR histogram for ObsID 10973. No obvious Cygnus OB2 X-ray diffuse emission was seen in this observation (see middle right panel of Figure 21 in the Appendix), so that the observed HR corresponds to that of the background emission. Colors in the histogram correspond to those of the color bar of the image. The peak of the HR distribution is about −0.16 for a 1σ of 0.06.
Paper: Diffuse X-Ray Emission in the Cygnus OB2 Association
Authors: J. F. Albacete-Colombo, J. J. Drake, E. Flaccomio, N. J. Wright, V. Kashyap, M. G. Guarcello, K. Briggs, J. E. Drew, D. M. Fenech, G. Micela, M. McCollough, R. K. Prinja, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: The exposure map for the Cygnus OB2 Chandra Legacy Survey and complementary observations for the study of diffuse X-ray emission. The bottom color bar shows the flux-to-color normalization factor in erg cm−2 s−1.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Top left: correlation between the observed intrinsic luminosities of the soft excess and the primary continuum in the 0.5–10 keV range, estimated from 21 bare AGNs. A linear fit is shown on the data set with a black dashed–dotted line, and the corresponding variation of χ is shown in the bottom panel. Top right: correlation between the observed intrinsic normalized luminosities of the primary continuum and soft excess in the energy range from 0.5 to 10 keV estimated from 21 bare AGNs. A linear fit is shown on the data set with a red dashed–dotted line, and the corresponding variation of χ is shown in the bottom panel. Bottom left: the average luminosity distribution of the primary continuum and soft excess across all sources with respect to redshift (z). Bottom right: the correlation between slope and intercept of individual sources is plotted.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Correlation between the intrinsic luminosities of primary continuum (PC) and soft excess (SE) in the 0.5–10.0 keV range, obtained from the powerlaw+powerlaw model fitting for different sources. Each data point is normalized by the Eddington luminosity of the source. The blue line shows the linear correlation fit between the intrinsic luminosities of primary continuum and soft excess.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Correlation of intrinsic luminosities of the primary continuum (PC) and soft excess (SE) of 0.5–10.0 keV obtained from powerlaw+powerlaw fitting for different sources. Each data point is normalized by the Eddington luminosity of the source. The blue line shows the linear correlation fit between the intrinsic luminosities of the primary continuum and soft excess.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Correlation of intrinsic luminosities of the primary continuum (PC) and soft excess (SE) of 0.5−10.0 keV obtained from powerlaw+powerlaw fitting for different sources. Each data point is normalized by the Eddington luminosity of the source. The blue line shows the linear correlation fit between the intrinsic luminosities of the primary continuum and the soft excess.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: The correlation between the observed intrinsic normalized luminosities of primary continuum (﹩\mathrm{log}({L}_{\mathrm{PC}}/{L}_{\mathrm{Edd}})﹩) and soft excess (﹩\mathrm{log}({L}_{\mathrm{SE}}/{L}_{\mathrm{Edd}})﹩) for 21 bare AGNs with ΓPC for different scenarios: (i) when ΓPC < 1.3, the variation of the ﹩\mathrm{log}({L}_{\mathrm{PC}}/{L}_{\mathrm{Edd}})﹩ versus ﹩\mathrm{log}({L}_{\mathrm{SE}}/{L}_{\mathrm{Edd}})﹩ is presented in the left panel; (ii) when ΓPC > 1.3, the variation of the ﹩\mathrm{log}({L}_{\mathrm{PC}}/{L}_{\mathrm{Edd}})﹩ versus ﹩\mathrm{log}({L}_{\mathrm{SE}}/{L}_{\mathrm{Edd}})﹩ is presented in the middle panel; and (iii) for all values of ΓPC, the variation of the ﹩\mathrm{log}({L}_{\mathrm{PC}}/{L}_{\mathrm{Edd}})﹩ versus ﹩\mathrm{log}({L}_{\mathrm{SE}}/{L}_{\mathrm{Edd}})﹩ is presented in the right panel. The color bar represents the variation of ΓPC.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: The distribution of the number of observations with respect to normalized intrinsic luminosities. The left panel shows the number distribution of intrinsic luminosity of normalized soft excess, the middle panel represents the distribution of intrinsic luminosity of normalized primary continuum, and the right panel shows the comparison of these intrinsic luminosities.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Correlation between slope and intercept of individual sources plotted with intrinsic parameters, such as ((a), (d)) redshift, ((b), (e)) ﹩\mathrm{log}({M}_{\mathrm{BH}})﹩, and ((c), (f)) ﹩\mathrm{log}({L}_{\mathrm{Edd}})﹩.
Paper: The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521
Authors: Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Figure caption: Positions of PG 1159 stars in the theoretical H-R diagram (﹩\mathrm{log}{L}_{\star }/{L}_{\odot }-\mathrm{log}{T}_{\mathrm{eff}}﹩). Star symbols: pulsating PG 1159 stars; circles: nonvariable; squares: with no reported photometric observations. Stars with planetary nebulae are marked with dashed circles. N-rich PG 1159 stars are shown with filled green symbols, while N-poor ones are shown with filled black symbols. Lines represent evolutionary tracks from Miller Bertolami & Althaus (2006): solid lines—VLTP (from left to right, final masses: 0.870, 0.741, 0.664, 0.609, 0.584, 0.565, 0.542, 0.530, 0.515 M ⊙); single dashed line—LTP (0.512 M ⊙). For illustration purposes, the blue dotted lines represent theoretical blue edges for l = 1 and l = 2 modes from Gautschy et al. (2005), but the blue edge is composition dependent. The red dotted lines indicate estimated observed red edges, beyond which no GW Vir star has been reported to date.
Paper: The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521
Authors: Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Figure caption: Positions of PG 1159 stars in the surface gravity–effective temperature ﹩\mathrm{log}g-\mathrm{log}{T}_{\mathrm{eff}}﹩ diagram. Star symbols: pulsating PG 1159 stars; circles: nonvariable; squares: with no reported photometric observations. Stars with planetary nebulae are marked with dashed circles. A typical error bar is shown in the lower left corner. Multiple stars overlap in this diagram, which can be seen as wider and darker borders of symbols. See text for details. Lines represent evolutionary tracks from Miller Bertolami & Althaus (2006): solid lines—VLTP (from left to right, final masses: 0.870, 0.741, 0.664, 0.609, 0.584, 0.565, 0.542, 0.530, 0.515 M ⊙); single dashed line—LTP (0.512 M ⊙).
Paper: The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521
Authors: Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Figure caption: Top: the period ranges of pulsating pre-WD stars (only of PG 1159 spectral type) vs. stellar radius (horizontal bars). Bottom: the period ranges of pulsating pre-WD stars (only of PG 1159 spectral type) vs. pulsation constant (horizontal bars). Objects surrounded by a planetary nebula are denoted with gray dotted bars. The object marked with an ellipse is RX J0122.9–7521 (see Section 10.1).