adsabs/AstroCLIMB huggingface dataset:
Paper: Populations of Magnetized Filaments in the Intracluster Medium and the Galactic Center
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle
Figure caption: Left: a grayscale MeerKAT image of the radio galaxy 3C 40B and its long filaments (Rudnick et al. 2022). The filaments are connected to a portion of the jet shown at the top of the panel. Right: the three panels to the right display three groups of GC radio filaments based on a 4″ resolution MeerKAT mosaic of the GC at 1.28 GHz (Heywood et al. 2022), discussed in detail in Yusef-Zadeh et al. (2022b). The intensity I (Jy beam−1) scales are, for 3C 40B, ﹩-4\lt \mathrm{log}(I)\lt -1.4﹩ for the bright emission, and −1 ﹩\times ﹩ 10− 4 < I < 7.8 ﹩\times ﹩ 10− 4 for the fainter emission; Snake, ﹩-4\lt \mathrm{log}(I+3\times {10}^{-4})\lt -2.33﹩; Flamingo, ﹩-4.3\lt {\rm{log}}(I+3\times {10}^{-4})\lt -2.3﹩; and Eyebrow, ﹩-4.3\lt {\rm{log}}(I+5\times {10}^{-4})\lt -3﹩.
Paper: Populations of Magnetized Filaments in the Intracluster Medium and the Galactic Center
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle
Figure caption: Left: a grayscale MeerKAT image of the core and its radio jet (top of the panel) and the filaments (center of the panel) of IC 4296, an elliptical radio galaxy, is displayed (Condon et al. 2021). Because of the strong surface brightness of the core and the jet compared to the filaments, different color tables were applied. Right: a MeerKAT filtered image of the comet tail as discussed in Yusef-Zadeh et al. (2022b). The intensity I (Jy beam−1) scales are, for IC 4296, ﹩-4\lt {\rm{log}}(I)\lt -1.2﹩ where I > 3.6 × 10−4 and −4 × 10− 5 < I < 3.6 × 10−4 for the fainter emission, and the comet tail, ﹩-5\lt \mathrm{log}(I+3\times {10}^{-4})\lt -4﹩.
Paper: Populations of Magnetized Filaments in the Intracluster Medium and the Galactic Center
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle
Figure caption: Top (a): a MeerKAT image of the galaxy cluster A3562 (Giacintucci et al. 2022) convolved with a Gaussian kernel with FWHM ∼10.″3. Bottom (b): a portion of the Feather filament where the filament splits into two fainter components at a compact source (Yusef-Zadeh et al. 2022b). The intensity I (Jy beam−1) scales are listed as follows: Feather: ﹩-4.7\lt \mathrm{log}(I+3\times {10}^{-4})\lt -4.3﹩; A3562: ﹩-4\lt {\rm{log}}(I)\lt -2﹩ where I > 7× 10−5 and −2 × 10−5 < I < 7 × 10−5 for fainter regions.
Paper: Populations of Magnetized Filaments in the Intracluster Medium and the Galactic Center
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle
Figure caption: Top: a MeerKAT image of ESO 137–006 galaxy in the Norma galaxy cluster (Ramatsoku et al. 2020). The beam FWHM is ∼10″. 7.″62 × 7.″29. Bottom: a portion of the Bent Harp filament showing multiple parallel filaments (Yusef-Zadeh et al. 2022b). The intensity I (Jy beam−1) scale for the Bent Harp is ﹩-3.8\lt \mathrm{log}(I+3\times {10}^{-4})\lt -3﹩.
Paper: On the Origin of the Dichotomy of Stellar Activity Cycles
Authors: Alfio Bonanno, Enrico Corsaro
Figure caption: Magnetic activity cycle rate ω cyc as a function of the rotation rate Ω. The dashed and dotted–dashed lines represent the fits obtained from the double linear regression (Equations (3) and (4), respectively). The symbol type represents the group classification as stemming from the fits (circles for group 1 and squares for group 2). Open symbols are stars for which the color-coded measurement was not available; 1σ uncertainties on ω cyc as well as the 3σ credible region of each fit are overlaid. The red arrow shows the star HD 103095, having ﹩\left[{\rm{M/H}}\right]\simeq -1.34﹩, significantly lower than the average metallicity of the sample. The available measurements of ﹩\left[{\rm{M/H}}\right]﹩, age, and ﹩{\mathrm{log}}_{10}{R}_{\mathrm{HK}}^{{\prime} }﹩, are shown as color-coded information in the top, middle, and bottom panels, respectively. The Sun with its symbol is indicated and included in G2, color coded according to the corresponding measurements.
Paper: On the Origin of the Dichotomy of Stellar Activity Cycles
Authors: Alfio Bonanno, Enrico Corsaro
Figure caption: Distribution of metallicity ﹩\left[{\rm{M/H}}\right]﹩, age, and chromoshperic activity index ﹩{\mathrm{log}}_{10}{R}_{\mathrm{HK}}^{{\prime} }﹩ from top to bottom for the stars of groups 1 and 2 as identified in Section 4. The overlaid vertical lines, having the same color as the histograms, represent the corresponding median values for each group. The metallicity range has been restricted to a range similar to that adopted in Figure 1 for clarity purposes.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: PDFs of the sound speed obtained for different values of the number of segments. More specifically, the first three panels from the left refer to N = 3, 4, 5, respectively. They clearly show that the steep increase of the distribution beyond ﹩{c}_{s}^{2}\simeq 1/3﹩ at small energy densities is a robust result that is independent of the number of segments and filtering. The rightmost panel refers instead to a PDF for N = 5 in which the filtering on the energy-density gradient is applied. Note how the filtering does modify the behavior of the PDF at very large energy densities removing the most extreme EOSs.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: Outermost contours of constraint-satisfying EOSs. Gray curves are obtained from unfiltered sampling with three, four, five, and seven segments; the light-red contour refers to the five-segment EOS after filtering.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: PDF of stellar radii at a fixed mass M = 1.4 M ⊙ for different fractions of our sample. Clearly, having a large number of EOSs decreases the size of the fluctuations; however 10% of the sample is already sufficient to obtain robust estimates of the median.
Paper: Optical–Radio Position Offsets Are Inversely Correlated with AGN Photometric Variability
Authors: Nathan J. Secrest
Figure caption: Percentage of objects above the fractional variability F var with significant optical–radio position offsets (X > 5). The gray shaded region denotes the 90% CI.
Paper: Optical–Radio Position Offsets Are Inversely Correlated with AGN Photometric Variability
Authors: Nathan J. Secrest
Figure caption: Left: distribution of fractional excess variability in the Gaia G band for the 1938 ICRF3 S/X objects in Gaia-CRF3 meeting the astrometric quality cuts employed here. Right: fractional excess variability as a function of G, indicating a very weak dependence.
Paper: Optical–Radio Position Offsets Are Inversely Correlated with AGN Photometric Variability
Authors: Nathan J. Secrest
Figure caption: Percentage of objects with significant optical–radio position offsets (X > 5), in F var bins of 100 objects. Error bars denote the 90% CI.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: PDF for the sound speed (left panel) and the mass–radius relation (right right) of monotonic EOSs without observational constraints. Note that no stellar model can be found with mass M ≳ 2 M ⊙.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: The same as Figure 1 in the main text, but with the overlay of the sound-speed curves relative to 1000 different EOSs.
Paper: Non-detection of He I in the Atmosphere of GJ 1214b with Keck/NIRSPEC, at a Time of Minimal Telluric Contamination
Authors: Jessica J. Spake, A. Oklopčić, L. A. Hillenbrand, Heather A. Knutson, David Kasper, Fei Dai, Jaume Orell-Miquel, Shreyas Vissapragada, Michael Zhang, Jacob L. Bean
Figure caption: Comparison of the planetary absorption spectrum of GJ 1214b from CARMENES and Keck. The red line shows the best-fit Gaussian model from Orell-Miquel et al. (2022) and the black line is the fiducial mass-loss model based on Salz et al. (2016). Note that pixels contaminated by telluric emission have been removed from the analysis.
Paper: Non-detection of He I in the Atmosphere of GJ 1214b with Keck/NIRSPEC, at a Time of Minimal Telluric Contamination
Authors: Jessica J. Spake, A. Oklopčić, L. A. Hillenbrand, Heather A. Knutson, David Kasper, Fei Dai, Jaume Orell-Miquel, Shreyas Vissapragada, Michael Zhang, Jacob L. Bean
Figure caption: Comparison of in-transit and out-of-transit spectra of GJ 1214b obtained with Keck/NIRSPEC, in the stellar rest frame. Gray and black lines show the telluric absorption (H2O) and emission (OH) lines, respectively. Vertical dotted lines indicate the location of the helium absorption line triplet.
Paper: Non-detection of He I in the Atmosphere of GJ 1214b with Keck/NIRSPEC, at a Time of Minimal Telluric Contamination
Authors: Jessica J. Spake, A. Oklopčić, L. A. Hillenbrand, Heather A. Knutson, David Kasper, Fei Dai, Jaume Orell-Miquel, Shreyas Vissapragada, Michael Zhang, Jacob L. Bean
Figure caption: Individual planet absorption spectra through time. The top panel is order 70, and the bottom panel is order 71. The start and end of the transit are indicated by the dotted white lines. The radial velocity trace of the expected position of the helium triplet is indicated by dashed blue lines. Pixels contaminated by telluric absorption and emission (see Figure 1) have been removed from the analysis (white vertical bars).
Paper: Non-detection of He I in the Atmosphere of GJ 1214b with Keck/NIRSPEC, at a Time of Minimal Telluric Contamination
Authors: Jessica J. Spake, A. Oklopčić, L. A. Hillenbrand, Heather A. Knutson, David Kasper, Fei Dai, Jaume Orell-Miquel, Shreyas Vissapragada, Michael Zhang, Jacob L. Bean
Figure caption: Maps showing the regions of parameter space that are rejected by our data. We compared our absorption spectrum to the helium absorption signal produced by our 1D, escaping atmosphere models with varying thermospheric temperatures and mass-loss rates. The color indicates the statistical significance of the deviation from a good fit, as described in Section 5.
Paper: Search for Coincident Gravitational Waves and Long Gamma-Ray Bursts from 4-OGC and the Fermi-GBM/Swift-BAT Catalog
Authors: Yi-Fan Wang, 一帆 王, Alexander H. Nitz, Collin D. Capano, Xiangyu Ivy Wang, Yu-Han Yang, Bin-Bin Zhang
Figure caption: Cumulative number of GW/long-GRB association candidates vs. the inverse false-alarm rate. The dashed line and shading show the expected results from background noise fluctuation and 1σ, 2σ, and 3σ uncertainty from a Poisson process. The most significant associated pair 200205_201716/GRB 200205845 has a ranking statistic λ gw+grb = 5.53, which corresponds to a false-alarm rate of 1 in 2.2 yr.
Paper: Search for Coincident Gravitational Waves and Long Gamma-Ray Bursts from 4-OGC and the Fermi-GBM/Swift-BAT Catalog
Authors: Yi-Fan Wang, 一帆 王, Alexander H. Nitz, Collin D. Capano, Xiangyu Ivy Wang, Yu-Han Yang, Bin-Bin Zhang
Figure caption: The posterior distribution of sky location for 200205_201716 from Bayesian inference and GRB 200205845 from the Fermi-GBM burst catalog. The inner and outer contours correspond to 50% and 90% credible intervals, respectively. The sky map overlap integral is ﹩\mathrm{ln}{B}_{\mathrm{overlap}}=1.35﹩.
Paper: Connection between Emission and Absorption Outflows through the Study of Quasars with Extremely High Velocity Outflows
Authors: Paola Rodríguez Hidalgo, Amy L. Rankine
Figure caption: The C  IV emission space color-coded by minimum to maximum values of bolometric luminosity (left), black hole mass (middle), and Eddington ratio (right) for both the DR9Q parent sample (hexagons) and EHVOs (circles). The hexagonal binning is modified due to the smaller numbers in the parent sample relative to Rankine+2020; the median values of the objects within each hexagon are calculated, and only hexagons with four or more objects are plotted. Notice that the values of black hole mass, and therefore Eddington ratio, are only included for cases with C  IV blueshift >500 km s−1 because the correction used here and described in Coatman et al. (2017) is not well defined for cases with negative or modest positive blueshifts (see Section 2 for information about measurements). Except for some outliers, most EHVOs are not distinguishable from the parent sample based on these three properties.
Paper: Connection between Emission and Absorption Outflows through the Study of Quasars with Extremely High Velocity Outflows
Authors: Paola Rodríguez Hidalgo, Amy L. Rankine
Figure caption: The C  IV emission space color-coded by minimum (left) and maximum (right) velocities of the Rankine+2020 BALs (blue hexagons) and EHVOs (purple circles). Note that, due to the definition of an EHVO, the minimum and maximum EHVO velocities are significantly greater than their BAL counterparts to warrant separate color maps in order for any trends to be visible. The EHVO sample is split into BALs (stars) and non-BALs (circles). The hexagonal binning is a reproduction of Rankine+2020's Figure 16; the median velocities of the objects within each hexagon are calculated, and only hexagons with five or more objects are plotted. The BAL minimum and maximum velocities both clearly increase with increasing C  IV blueshift. The maximum EHVO velocity also appears to increase; however, the minimum EHVO velocity shows no such trend. Notice also that EHVOs seem to occupy the same parameter space as BALs with speeds in the upper half (﹩{V}_{\max }\gtrsim 15,000﹩ km s−1).
Paper: Connection between Emission and Absorption Outflows through the Study of Quasars with Extremely High Velocity Outflows
Authors: Paola Rodríguez Hidalgo, Amy L. Rankine
Figure caption: Comparison of Rankine et al. (2020) and RH+2020) samples in the studied parameter space. The lack of overlap in the top left quadrant is due to the different S/Ns in both samples, but it is reduced once we establish the same cutoff.
Paper: Connection between Emission and Absorption Outflows through the Study of Quasars with Extremely High Velocity Outflows
Authors: Paola Rodríguez Hidalgo, Amy L. Rankine
Figure caption: The scatter plot shows non-BALs (aqua), BALs (light blue; both from Rankine+2020), and EHVOs from RH+2020 (purple) in the C  IV emission line blueshift and EW parameter space. A progression toward larger blueshifts and smaller EWs is shown from the samples of non-BALs and BALs toward the EHVOs.
Paper: A Transient “Changing-look” Active Galactic Nucleus Resolved on Month Timescales from First-year Sloan Digital Sky Survey V Data
Authors: Grisha Zeltyn, Benny Trakhtenbrot, Michael Eracleous, Jessie Runnoe, Jonathan R. Trump, Jonathan Stern, Yue Shen, Lorena Hernández-García, Franz E. Bauer, Qian Yang, Tom Dwelly, Claudio Ricci, Paul Green, Scott F. Anderson, Roberto J. Assef, Muryel Guolo, Chelsea MacLeod, Megan C. Davis, Logan Fries, Suvi Gezari, Norman A. Grogin, David Homan, Anton M. Koekemoer, Mirko Krumpe, Stephanie LaMassa, Xin Liu, Andrea Merloni, Mary Loli Martínez-Aldama, Donald P. Schneider, Matthew J. Temple, Joel R. Brownstein, Hector Ibarra-Medel, Jamison Burke, Craig Pellegrino, Juna A. Kollmeier
Figure caption: Optical light curves of J1628+4329 obtained from SDSS (left), Pan-STARRS (middle), and ZTF (right) imaging, in the g and r bands (open circles; see legend) over a period of two decades. For clarity, only measurements with magnitude uncertainties less than 0.1 mag are displayed. Dashed vertical lines mark the epochs of the spectra shown in Figure 1, and the corresponding synthetic photometry is marked with filled circles. Note the fast, <2 month transitions observed within ZTF during 2021, and the slower dimming observed within Pan-STARRS, during 2012–2014. The middle and right panels also show light curves obtained from WISE, in the W1 and W2 bands, where each data point shows the median magnitude at the given epoch. Note the vertical offset of the WISE data (for clarity; see legend).
Paper: A Transient “Changing-look” Active Galactic Nucleus Resolved on Month Timescales from First-year Sloan Digital Sky Survey V Data
Authors: Grisha Zeltyn, Benny Trakhtenbrot, Michael Eracleous, Jessie Runnoe, Jonathan R. Trump, Jonathan Stern, Yue Shen, Lorena Hernández-García, Franz E. Bauer, Qian Yang, Tom Dwelly, Claudio Ricci, Paul Green, Scott F. Anderson, Roberto J. Assef, Muryel Guolo, Chelsea MacLeod, Megan C. Davis, Logan Fries, Suvi Gezari, Norman A. Grogin, David Homan, Anton M. Koekemoer, Mirko Krumpe, Stephanie LaMassa, Xin Liu, Andrea Merloni, Mary Loli Martínez-Aldama, Donald P. Schneider, Matthew J. Temple, Joel R. Brownstein, Hector Ibarra-Medel, Jamison Burke, Craig Pellegrino, Juna A. Kollmeier
Figure caption: The spectral ratio between the 2016 intermediate state and 2021 dim state of J1628+4329 (black), smoothed over 7 pixels. The colored areas indicate different extinction laws: Milky Way (MW)-like extinction with R  V  = 4.4 and LMC-like extinction (red and green, respectively; see Salim & Narayanan 2020, and references therein), and “Maiolino-active-galactic-nucleus” (AGN) extinction (blue; Maiolino et al. 2001; Li 2007). A range of possible A  V  values for each extinction law is shown. Steeper extinction laws, e.g., MW-like with R  V  = 3.1, are not consistent with the spectral ratio (see dashed line).
Paper: A Transient “Changing-look” Active Galactic Nucleus Resolved on Month Timescales from First-year Sloan Digital Sky Survey V Data
Authors: Grisha Zeltyn, Benny Trakhtenbrot, Michael Eracleous, Jessie Runnoe, Jonathan R. Trump, Jonathan Stern, Yue Shen, Lorena Hernández-García, Franz E. Bauer, Qian Yang, Tom Dwelly, Claudio Ricci, Paul Green, Scott F. Anderson, Roberto J. Assef, Muryel Guolo, Chelsea MacLeod, Megan C. Davis, Logan Fries, Suvi Gezari, Norman A. Grogin, David Homan, Anton M. Koekemoer, Mirko Krumpe, Stephanie LaMassa, Xin Liu, Andrea Merloni, Mary Loli Martínez-Aldama, Donald P. Schneider, Matthew J. Temple, Joel R. Brownstein, Hector Ibarra-Medel, Jamison Burke, Craig Pellegrino, Juna A. Kollmeier
Figure caption: Representative host- and narrow-line-subtracted spectra of J1628+4329: 2001 bright state (blue), 2016 intermediate state (green), 2021 dim state (red; SDSS-V), and 2021 intermediate state (purple; LCO). Along those, we plot reddened spectra of the bright state, obtained by applying the “Maiolino AGN” extinction law. The appropriate A  V  values were selected to best reproduce the intermediate (A  V  = 0.67;  black) and dim (A  V  = 1.6;  gray) states.
Paper: Connection between Emission and Absorption Outflows through the Study of Quasars with Extremely High Velocity Outflows
Authors: Paola Rodríguez Hidalgo, Amy L. Rankine
Figure caption: Left: C  IV emission space color-coded by He II EW. In agreement with the parent sample, the EHVO He II EW decreases as C  IV blueshift increases and EW decreases. The EHVOs with the largest He II EWs have perhaps too-strong He II for their location in C  IV space. Right: He II EW against C  IV distance. The EHVO quasars are shifted to the bottom right compared to the BALs and non-BALQSOs, while the EHVOs with the highest He II EWs appear to be at the limit of allowed He II values.
Paper: A Transient “Changing-look” Active Galactic Nucleus Resolved on Month Timescales from First-year Sloan Digital Sky Survey V Data
Authors: Grisha Zeltyn, Benny Trakhtenbrot, Michael Eracleous, Jessie Runnoe, Jonathan R. Trump, Jonathan Stern, Yue Shen, Lorena Hernández-García, Franz E. Bauer, Qian Yang, Tom Dwelly, Claudio Ricci, Paul Green, Scott F. Anderson, Roberto J. Assef, Muryel Guolo, Chelsea MacLeod, Megan C. Davis, Logan Fries, Suvi Gezari, Norman A. Grogin, David Homan, Anton M. Koekemoer, Mirko Krumpe, Stephanie LaMassa, Xin Liu, Andrea Merloni, Mary Loli Martínez-Aldama, Donald P. Schneider, Matthew J. Temple, Joel R. Brownstein, Hector Ibarra-Medel, Jamison Burke, Craig Pellegrino, Juna A. Kollmeier
Figure caption: Multiepoch optical spectra of J1628+4329. This AGN shows a gradual dimming of its quasar-like continuum and Balmer BELs across ∼20 yr, through the 2001 bright-state Sloan Digital Sky Survey (SDSS) spectrum, the 2016 intermediate-state WHT spectrum (MacLeod et al. 2019), and the 2021 dim-state SDSS-V spectra. Subsequent observations performed by Las Cumbres Observatory (LCO) revealed a brightening to an intermediate state in ≲2 months.
Paper: A General, Scale-independent Description of the Sound Speed in Neutron Stars
Authors: Christian Ecker, Luciano Rezzolla
Figure caption: Top panels:  PDFs for the sound speed as a function of the normalized radial coordinate r/R for three fixed values of the masses M = 0.5 (left), 0.75 (middle), and 1 M TOV (right). Red lines represent the median of the distribution, black solid lines are the upper and lower bounds of the 95% credibility interval, while black dashed lines indicate the conformal limit ﹩{c}_{s}^{2}\,=\,1/3﹩. Bottom panels: same as the top panels but shown for representative stellar masses in units of solar mass: M = 1.0 (left), 1.4 (middle), and 2.0 M ⊙ (right).
Paper: A General, Scale-independent Description of the Sound Speed in Neutron Stars
Authors: Christian Ecker, Luciano Rezzolla
Figure caption: Scale-independent description of the sound speed as a function of the mass M normalized by the maximum mass M TOV and the radial location r normalized by the neutron-star radius R. The blue region represents the median of the PDF, while the cyan and purple regions mark the lower and upper 95% credibility intervals, respectively. Different lines are used to show the important properties of the PDF. The red solid line shows the value of the maximum sound speed, ﹩{c}_{s,\max }^{2}﹩, as a function of the stellar mass, while the red dashed line shows the location within the star of ﹩{c}_{s,\max }^{2}﹩ as a function of the stellar mass; the green solid line reports the sound speed at the stellar center, ﹩{c}_{s,\mathrm{center}}^{2}﹩, as a function of the stellar mass.
Paper: A General, Scale-independent Description of the Sound Speed in Neutron Stars
Authors: Christian Ecker, Luciano Rezzolla
Figure caption: The PDF of the sound speed for M = M TOV. The red line represents the median of the distribution, the black solid lines are the upper and lower bounds of the 95% credibility interval, and the black dashed line indicates the conformal limit ﹩{c}_{s}^{2}\,=\,1/3﹩. Orange, green, and cyan lines report the cold beta equilibrium sound speed for the HS(DD2) (Hempel & Schaffner-Bielich 2010; Typel et al. 2010), BHBΛ (Banik et al. 2014), and intermediately stiff VQCD (Demircik et al. 2021) EOS, respectively.
Paper: A General, Scale-independent Description of the Sound Speed in Neutron Stars
Authors: Christian Ecker, Luciano Rezzolla
Figure caption: Mass dependence of the median of the local maximum sound speed ﹩{c}_{s,\max }^{2}﹩ (red line) and the sound speed at the neutron-star center ﹩{c}_{s,\mathrm{center}}^{2}﹩ (green line); the red and green shaded areas indicate the corresponding 95% credibility intervals. Black dashed and dotted lines mark half the speed of light and the conformal limit, respectively.
Paper: A General, Scale-independent Description of the Sound Speed in Neutron Stars
Authors: Christian Ecker, Luciano Rezzolla
Figure caption: The PDFs for the sound speed as a function of the normalized radial coordinate r/R for three fixed values of the masses M = 0.5 (left), 0.75 (middle), and 1 M TOV (right). Red lines represent the median of the distribution, black solid lines are the upper and lower bounds of the 95% credibility interval, and black dashed lines indicates the conformal limit ﹩{c}_{s}^{2}\,=\,1/3﹩. This figure is analogous to Figure 2; the only difference is that here an upper limit on the maximum mass M TOV < 2.16 M ⊙ is imposed.
Paper: A General, Scale-independent Description of the Sound Speed in Neutron Stars
Authors: Christian Ecker, Luciano Rezzolla
Figure caption: Mass dependence of the median sound speed for various different values of the normalized radial position location inside neutron stars as indicated by the color bar. Black dashed and dotted lines mark half the speed of light and the conformal limit, respectively.