adsabs/AstroCLIMB huggingface dataset:
Paper: Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
Authors: Suman Kumar Kundu, Eric R. Coughlin, C. J. Nixon
Figure caption: The integrated column density at the time when the center of mass of the star reaches pericenter. The value of β is shown in the top left of each panel. The left panels show the distribution of stellar material in the orbital plane, and the corresponding right panels show the view perpendicular to that plane. In the convention we adopt, both the initial x, y coordinates of the center of mass of the star start with negative values and arrive at the pericenter with a positive x-coordinate value and y = 0. Thus, any fluid element with a positive (negative) y-value has already (not yet) passed through its pericenter. Increasing β clearly leads to an increase in the flattening, or “crushing” of the star, into the orbital plane near the pericenter.
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: Results from the bootstrapping method for F  γ‐ray>100 MeV and F C,opt (6024–6092 Å) light curves. (a) PyDCF output with the centroid values of DCF (DCFcent; dotted horizontal line) and lag τ cent (dashed vertical line) for the original data. (b) DCFcent distribution obtained from cross-correlation results of the bootstrap output light curves. The peak of the distribution is represented by the solid magenta horizontal line. The 68%, 95%, and 99% confidence limits of DCFpeak are shown by red, green, and blue dashed lines, respectively. (c) Distribution of the centroid lag values obtained from cross-correlation analysis of the simulated light curves. The solid brown vertical line indicates the peak of the distribution (τ peak). The confidence limits of τ peak are plotted in red, green, and blue dashed lines. (d) Plot showing the significance of the correlations at the 1σ (red dashed line), 2σ (green dashed line), and 3σ (blue dashed line) levels for different lags.
Paper: Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
Authors: Suman Kumar Kundu, Eric R. Coughlin, C. J. Nixon
Figure caption: The maximum value of the central stellar density (left) and temperature (right) as a function of β normalized by their initial values. The dashed curves represent the scalings derived by Luminet & Carter (1986; olive) and Coughlin & Nixon (2022b; teal), the solid, teal curves are from the analytic model (also in Coughlin & Nixon 2022b), and the solid, orange curves are from the numerical simulations.
Paper: Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
Authors: Suman Kumar Kundu, Eric R. Coughlin, C. J. Nixon
Figure caption: The central density normalized to its original value as a function of time normalized by the dynamical time of the star. The different curves are appropriate to the β in the legend, with solid (dashed) curves resulting from the numerical simulations (analytic model). The magnitude of the compression and time of the maximum compression agrees reasonably well between the SPH and analytic results.
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: Cross-correlation plots obtained with PyDCF for a time range of ±1200 days and lag bin size of 20 days for γ-ray (F  γ‐ray>100 MeV) and optical continuum (F C,opt (6024–6092 Å)) light curves (left) and γ-ray F  γ‐ray>100 MeV and Hγ (F Hγ ) light curves (right).
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: SEDs of the source fitted with the Jetset code for the γ-ray flaring and quiescent epochs. The optical/UV photometric data were obtained from Swift UVOT filters (V, B, U, UVW1, UVM2, and UVW2), and the X-ray (0.3–10 keV) spectra were taken from XRT observations. LAT spectra were used for the high-energy γ-ray emission. The upper limits in the LAT spectra are plotted as downward arrows.
Paper: Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
Authors: Suman Kumar Kundu, Eric R. Coughlin, C. J. Nixon
Figure caption: The maximum central density (left) and temperature (right) normalized to their original values as a function of β. The blue dashed lines indicate the large-β behavior of our analytic solution, while the black dashed lines indicate the corresponding scaling predicted by Carter & Luminet (1983) and Luminet & Carter (1986).
Paper: Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
Authors: Suman Kumar Kundu, Eric R. Coughlin, C. J. Nixon
Figure caption: The ratio of the central density normalized to its original value as a function of time normalized by the dynamical time of the star. As β increases the extent of compression increases significantly, and the time at which the maximum density is reached approaches 0 (which is the time when the center of the star reaches the pericenter).
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: 1994–2021 Guitar/Filament Evolution. Left panels show four 22″ × 21″ cutouts from the HST Hα images (1994, 2001, 2006, 2020). The top panel has the pulsar positions at the four HST and four Chandra epochs marked on lines representing 50 yr (9.″7) of proper motion. The lower panels have the outline of the 2020 HST Hα limb marked, for comparison. The right panels show the filament evolution over the four Chandra epochs (﹩4^{\prime} \times 1^{\prime} ﹩ cutouts). The filament leading edge from the 2021 epoch is marked by the blue line, while the red arrow in the top and bottom panels shows the 50 yr proper motion, and a stationary background source is marked for reference.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: The Wilkin-model bow shock fits for the four different Hα epochs. All images are shown in native resolution of 0.″05 per pixel. The left column shows a cutout of the bow shock apex for the four epochs, using pixels up to ≈ 1″ behind the apex. The 1994 and 2001 epochs have been lightly smoothed for visualization. The middle column shows the Wilkin model, and the rightmost column shows the residual (data-model)2 σ−  2. The red cross shows the location of the pulsar, which for the 2020 epoch is a free parameter, and for the other three epochs is referenced to Gaia using a set of reference stars.
Paper: Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
Authors: Suman Kumar Kundu, Eric R. Coughlin, C. J. Nixon
Figure caption: The ratio of the maximum to the original density at the geometric center of the star as a function of β. The different solid curves are obtained by varying the spatial resolution, with the corresponding number of particles shown in the legend. The analytic prediction is shown by the dashed curve.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: The posterior distributions for the standoff distance r 0 in each epoch (left to right, top to bottom: 1994, 2001, 2006, 2020. Shown for reference are the estimated standoff distances of Ocker et al. (2021) and Chatterjee & Cordes (2004).
Paper: Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
Authors: Suman Kumar Kundu, Eric R. Coughlin, C. J. Nixon
Figure caption: The ratio of maximum central density to the original central density against the dynamic time of the star with β = 7. The resolution and gravity are specified by the legend (solid blue and dotted orange use the Schwarzschild metric for the gravitational field of the SMBH). The compression is stronger (by a factor of ≲1.5) with relativistic effects included, and the time of maximum compression occurs later in comparison to the Newtonian case; the latter effect arises from time dilation (note that the horizontal axis is coordinate time, i.e., time as measured by an observer at infinity) normalized by the dynamic time of the star.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: Overview of the Guitar/filament complex in the most recent HST and Chandra epochs. Red: 2020 HST ACS/WFC Hα, green: PanSTARRS2 r, blue: 2021 Chandra 1–5 keV X-rays. The pulsar point source lies at the tip of the Hα nebula. Filament X-ray emission extends primarily to the right (northwest). This has a sharp leading edge and extension behind. The Guitar “body” shows faintly in the Hα in the lower half of the image.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: Velocity profile just behind the nebula apex (oval in Figure 2). A reflected version of the profile (red) shows that it is centered at ∼−12 km s−1. The high-velocity ∣v∣ = 150–300 km s−1 wings (blue points, shifted from the red profile to match original apex profile wings) show a slight additional blueshift.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: GMOS-N IFU Hα velocity channel images, covering 5.″5 × 6.″1. The combined IFU image from 2016 is shown in the middle panel. This is flanked by velocity slices (central velocity, in km s−1, at upper right in each frame), with the Hα limb as a red outline, for comparison. The oval region near the apex provides the line spectrum shown in Figure 3.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: Regions used for spectral analysis of the filament in the 2021 Chandra epoch. We divided the filament into three main sections: the inner section where the leading edge is sharpest (0′–0.′7), the middle section where the filament appears to become more diffuse (0.″7–1.″3), and the outer, most-diffuse section where the sharp leading edge has largely disappeared (1.′3–2.′4). Additionally, the inner and middle sections are divided by the green dashed line into the "Leading" and "Trailing" regions. We also identify a “Remnant” region of bright emission around 12″ behind the leading edge in the middle section. The red regions show the contours of the Guitar nebula head (solid line) and body (dashed line) in the 2020 HST Hα image.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: Spread of the emission behind the leading edge in the filament middle section across four epochs. The data are well described by a steady shift of the peak behind the leading edge, a steady increase in the width, and a constant integrated flux. The y-axis indicates the 1–5 keV photon surface brightness. Labels indicate the best-fit parameter values (with 1σ errors): x 2000 and σ 2000 are the peak position and standard deviation of the Gaussian component in 2000, respectively; ﹩\dot{\sigma }﹩ indicates the increase in σ over time; and μ indicates the shift of the peak away from the leading edge over time.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: Light curves of the inner counterfilament and inner and middle filament sections. Data points have been slightly offset from each other for legibility. The y-axis indicates the 1–5 keV photon flux per arcminute length of filament. The lengths of the inner counterfilament, and inner and middle filament sections are 0.″25, 0.″65, and 0.″68, respectively, and fluxes have been integrated across the width of the main filament.
Paper: A Quarter Century of Guitar Nebula/Filament Evolution
Authors: Martijn de Vries, Roger W. Romani, Oleg Kargaltsev, George Pavlov, Bettina Posselt, Patrick Slane, Niccolo' Bucciantini, C.-Y. Ng, Noel Klingler
Figure caption: Light curves of the leading edge (1′ width) of the inner filament (0′–0.′7 segment), showing the flux in each epoch and the flux of that same region of the sky in following epochs. The y-axis indicates the 1–5 keV photon surface brightness.
Paper: Tidally Distorted Barytropes and Their Roche Limits, with Application to WASP-12b
Authors: Victoria Antonetti, Jeremy Goodman
Figure caption: Solid curve: a steady-state, solar-metallicity MESA model for WASP-12b with the OPAL/SVCH equation of state, core mass 10 M ⊕, core mean density 10 g cm−3 (not shown in plot), dayside irradiation 1010 erg cm−2 s−1, and internal heating 2.82 × 10−4 erg g−1.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Emission at 1420 MHz toward the SNR G46.8 − 0.3 reconstructed from THOR and VGPS observations. The green contour levels correspond to 14, 19, 24, 29, 34 and 39 mJy beam−1. The red box indicates the region in which we performed a grid search for polarization and Faraday rotation. The object on the right-hand side of the box is the H II region G046.495-00.247 (Lockman 1989; Anderson et al. 2018).
Paper: The 3.3 μm Infrared Emission Feature Profile in HD 44179
Authors: Alan T. Tokunaga, Lawrence S. Bernstein, Michael Connelley
Figure caption: Slit position and orientation superimposed on a black and white adaptation of Figure 1 of Candian et al. (2012). The contours show the spatial distribution of the 3.3 μm emission band. It consists of two lobes separated by a dark lane that is caused by the extinction of a circumstellar disk. The central star is completely obscured and its position is shown with a white “X.” The green vertical strip shows the orientation of the SpeX slit (0.″3 width) and the brown strip shows the orientation of the slit (0.″6 width) in the Song et al. (2003) observations. The 0.″3 × 2.″0 portion of the SpeX slit that was used for the spectral extraction is shown by the black box.
Paper: The 3.3 μm Infrared Emission Feature Profile in HD 44179
Authors: Alan T. Tokunaga, Lawrence S. Bernstein, Michael Connelley
Figure caption: Comparison of the SpeX HD 44179 average spectrum (black) to that of the ISO SWS spectrum of HD 44179 (red), normalized to the 3.3 μm emission feature peak. Since the SpeX spectrum is affected by strong telluric CH4 absorption at 3.32 μm this part was removed, leaving a gap centered at 3.32 μm. The ISO spectrum comes from the ISO archive published by Sloan et al. (2003). The SpeX spectrum has a redder continuum due to the dust continuum emission from the disk. The peak-to-continuum ratio is smaller in the SpeX spectrum because the dust emission is stronger at HD 44179 compared to the nebula in the larger ISO SWS aperture.
Paper: The 3.3 μm Infrared Emission Feature Profile in HD 44179
Authors: Alan T. Tokunaga, Lawrence S. Bernstein, Michael Connelley
Figure caption: Ratio of the average HD 44179 spectrum divided by the Sirius spectrum (black line). For comparison, the Kurucz model atmosphere spectrum of Sirius is also shown (red line). Note the strong Pf absorption lines in the Sirius spectrum at 2.873, 3.039, and 3.296 mic. The Pf lines appear in emission in the ratio of the HD 44179 spectrum to the Sirius spectrum. The lines are resolved and so a precise correction requires taking into account the line profile, especially the wings of the line. Note that the very strong telluric absorption by telluric H20 absorption at 2.8–2.9 μm and by CH4 at 3.32 μm causes the noise in the ratio to increase substantially.
Paper: The 3.3 μm Infrared Emission Feature Profile in HD 44179
Authors: Alan T. Tokunaga, Lawrence S. Bernstein, Michael Connelley
Figure caption: Comparison of the normalized SpeX spectrum of HD 44179, the ISO SWS spectrum of HD 44179, and the ISO SWS spectrum of NGC 7027 after removal of a linear continuum. The region affected by the telluric CH4 at 3.32 μm was removed in the SpeX spectrum. The ISO spectra come from the ISO archive published by Sloan et al. (2003). Note that the Pf-δ line is precisely located at the peak of the 3.3 μm emission feature in HD 44179. Compared to the ISO spectrum, the wings of the 3.3 μm emission feature are wider in the SpeX spectrum.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: The rotation measure spread function (RMSF) after RFI flagging is performed on the polarization image cubes, with an FWHM of 101.7 rad m−2. This RMSF is from the data used in the investigation of SNR G46.8−0.3. The RMSFs for the other SNRs in this study have a similar shape to the FWHM falling within the range from 100–103 rad m−2 due to different RFI flagging.
Paper: The 3.3 μm Infrared Emission Feature Profile in HD 44179
Authors: Alan T. Tokunaga, Lawrence S. Bernstein, Michael Connelley
Figure caption: Comparison of the SpeX spectrum of HD 44179 (black line), the ISO spectrum of HD 44179 (red line), and the ISO spectrum of NGC 7027 (blue line) after removal of the linear continuum and the plateau emission (see text). The NGC 7027 spectrum is typical of class A and is shifted to shorter wavelengths with a center wavelength of 3.289 μm and a FWHM of 0.041 μm (Tokunaga & Bernstein 2021). The ISO SWS spectra were obtained from the ISO spectral archive of Sloan et al. (2003).
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Grid plot of the Faraday depth spectra for the red box seen in Figure 3. The horizontal limits are −1500 rad m−2 < ϕ < 1500 rad m−2 and vertical axis limits are 0 < P < 0.95 mJy. The gray region illustrates our Faraday depth rejection range. The red horizontal line is our detection threshold where P = 0.27 mJy. Colors indicate spectra where zero (black), one (blue), or two (purple) peaks satisfy our detection criteria (see the Appendix). The coordinates of the bottom-left and top-right corners are (ℓ, b)  =  (46.°802, 0.°377) and (ℓ, b) = (46.°777, −0.°352). The physical size of this region is 2.36 pc on each side.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Fractional polarization map of SNR G46.8−0.3. Contours are from the THOR+VGPS map at 14, 19, 24, 29, 34, and 39 mJy beam−1. The colored subregions were calculated by Π  =  P/(I − I bg) where Π is the fractional polarization, P is the peak from the Faraday depth spectrum, I is the Stokes I from the THOR+VGPS map, and I bg is the average background Stokes I. The black subregions are upper limits for regions where the polarized signal is heavily affected by leakage. The criteria for these subregions is that Πupper  =  P limit/(I − I bg) < 1%, where P limit is the maximum from the noise profiles.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Faraday depth map of SNR G46.8−0.3. The contour levels correspond to 14, 19, 24, 29, 34, and 39 mJy beam−1. The subregions with a purple edge indicate the locations of two-component Faraday rotation. The Faraday depth shown for subregions with two-component Faraday rotation is derived from the strongest peak. The red box indicates the region where we present the individual Faraday depth spectra as a grid plot seen in Figure 6.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: Sample Faraday depth spectra for G46.8 − 0.3. Single-component spectra are presented in (a), at (ℓ, b) = (46.°834, −0.°178), ϕ  =  181.2 ± 3.5 rad m−2 (solid line), and at (ℓ,b) = (46.°746, −0.°323), ϕ  =  454.4 ± 5.2 rad m−2 (dashed line). Two-component spectra are presented in (b), at (ℓ,b) = (46.°800, −0.°398), ϕ 1  =  166.6 ± 3.1 rad m−2, and ϕ 2  =  437.2 ± 3.1 rad m−2 (solid line), and at (ℓ,b) = (46.°817, −0.°382), ϕ 1  =  353.6 ± 2.3 rad m−2, and ϕ 2  =  552.2 ±2.3 rad m−2 (dashed line). The gray region indicates our Faraday depth rejection range of ∣ϕ∣ < 100 rad m−2. The red horizontal line indicates the detection threshold 0.27 mJy, which is derived in the Appendix.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: (a) Distribution of Faraday depth for all single-component peaks that satisfy all detection criteria. (b) Faraday depth complexity attributed to the internal structure of the SNR. This histogram is found from subregions where two peaks are observed that satisfy all detection criteria. The values have been shifted by the mean Faraday depth of 357 rad m−2 found from all of the subregions where single-component Faraday rotation was observed. The purple bars represent the highest peak, and the orange bars represent the secondary peak.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: (a) The dirty Faraday depth spectra for 30 randomly chosen profiles that are outside the SNR where no Stokes I is observed at λ21 cm. (b) The red and black curves represent the dirty and clean Faraday depth spectra for three profiles that are outside the lowest contour in Figure 3.
Paper: Polarized Emission from Four Supernova Remnants in the THOR Survey
Authors: Russell Shanahan, Jeroen M. Stil, Loren Anderson, Henrik Beuther, Paul Goldsmith, Jürgen Ott, Michael Rugel, Juan Soler, Jonas Syed
Figure caption: THOR and VGPS total intensity map of the SNR G46.8−0.3. Red vectors indicate B-vectors in the plane of the sky at λ21 cm wavelength rotated to λ6 cm using the observed Faraday depth. Green vectors represent the B-vectors at λ6 cm from the Sino-German survey. The length of the vectors is proportional to the polarized intensity observed in the associated subregion. Orange contours are the polarized intensity from the Sino-German survey at 23, 35, 45, 55, and 65 mK.