adsabs/AstroCLIMB huggingface dataset:
Paper: Collisional Shaping of Nuclear Star Cluster Density Profiles
Authors: Sanaea C. Rose, Morgan MacLeod
Figure caption: Assuming a uniform population of 1 M ⊙ stars, we plot relevant timescales for a range of stellar density profiles, α = 1.25 (solid line) to α = 1.75 (dashed line), in the nuclear star cluster. The collision and relaxation timescales are in red and green, respectively. To guide the eye, the gray line shows the total simulation time of 10 Gyr. The vertical red line marks the radius at which the main-sequence lifetime of a Sun-like star, also the total simulation time, becomes equal to the collision timescale for a cuspy profile. Within this distance, most stars will experience a collision before evolving off the main sequence. Additionally, we plot the approximate time needed for the two stellar cores to collide, or the collision timescale (Equation (3)) calculated for r  c  = 2 × 0.33R ⊙, in green. The green vertical line shows where the velocity dispersion becomes approximately equal to the escape speed from a Sun-like star. Within this distance, 0.01 pc from the SMBH, the kinetic energy is sufficiently high that a collision could unbind the stars and destroy them.
Paper: Follow-up on the Supermassive Black Hole Binary Candidate J1048+7143: Successful Prediction of the Next Gamma-Ray Flare and Refined Binary Parameters in the Framework of the Jet Precession Model
Authors: Emma Kun, Ilja Jaroschewski, Julia Becker Tjus, Silke Britzen, Sándor Frey, Krisztina Éva Gabányi, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Gamma-ray and radio flares of J1048+7143. Top: the new exponential fit of the γ-ray light curve of J1048+7143 with 5% adaptive binning (best-fit parameters are shown in Table 1). The sum of the contributions from individual subflares is displayed as the blue continuous line. Application of the centroid method is indicated via the red crosses. Their weighted average determines the centers of main flares as a green dashed line. Intersections of these lines with the blue lines indicate the duration of the flares, illustrated as gray areas. The red continuous line shows the latest data point available in the Fermi-LAT Light Curve Repository (2023 September 22 or MJD 60209). Bottom: the extended radio flux density curve of J1048+7143, obtained with the RATAN600 and Nanshan (Urumqi) radio telescopes at 4.8 GHz (see details in Kun et al. 2022b).
Paper: Collisional Shaping of Nuclear Star Cluster Density Profiles
Authors: Sanaea C. Rose, Morgan MacLeod
Figure caption: The evolution of the stellar density profile for different simulations. The title of each column states the collision outcome prescription used in the simulation shown below. The black lines represent the initial, unmodified density profile, with α = 1.75. The colored lines show the profile at a given time, indicated by the color bar on the right. The gray lines in the upper left corner of each plot show other examples of density profile slopes to guide the eye. The left column presents results for fully destructive collisions. These density profiles exhibit clear turning points coinciding with where the time elapsed, or population age, equals the collision timescale (see Figure 1). In the other rows, a more complex treatment of collision outcomes obscures the inflection point in the density profiles. However, a similar trend is present: the inflection point moves further from the SMBH with time, corresponding roughly to where the population age equals the collision timescale. The red arrows draw attention to this approximate distance from the SMBH for an old (∼10 Gyr) population.
Paper: Collisional Shaping of Nuclear Star Cluster Density Profiles
Authors: Sanaea C. Rose, Morgan MacLeod
Figure caption: The stellar population at four different times over the course of two simulations. As indicated by the column labels, time increases left to right. The gray points show the masses of the stars at the given time as determined by main-sequence evolution alone. The red dots show the simulated masses of the stars in our sample, which can also change due to collisions. The top row corresponds to fully destructive collisions, meaning a star is removed from the sample when it undergoes a single collision. The bottom row shows results that use the mass loss prescription from Rauch (1999). Both simulations assume a Bahcall–Wolf (α = 1.75) profile for the surrounding stars. We mark r coll with a red dashed vertical line, where r coll is calculated from Equation (8).
Paper: Collisional Shaping of Nuclear Star Cluster Density Profiles
Authors: Sanaea C. Rose, Morgan MacLeod
Figure caption: The stellar density profile with varying initial density profile of the stars. The title of each column indicates the value of α used for the stellar density profile. Each plot has the same axes to facilitate a comparison between them. The form of the evolving density profiles suggests that the initial profile is always preserved outside of 0.2 pc, where collisions are more rare. A steeper initial profile, however, also results in a more pronounced break in the density profile at a further distance from the SMBH. To highlight this trend, we have added a dashed gray line marking where the mass density is halved due to collisions for the oldest population shown in the figure (darkest red curve, 7 Gyr).
Paper: Follow-up on the Supermassive Black Hole Binary Candidate J1048+7143: Successful Prediction of the Next Gamma-Ray Flare and Refined Binary Parameters in the Framework of the Jet Precession Model
Authors: Emma Kun, Ilja Jaroschewski, Julia Becker Tjus, Silke Britzen, Sándor Frey, Krisztina Éva Gabányi, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Prediction plot for γ-ray flares from J1048+7143. Gray areas show the durations of the four flares determined with the centroid method in Table 2. The blue hashed bands represent an overlap of the predictions using the period P  n→n+1, where n = 1 or 2. Invalid mass ratios are displayed via the red crossed area. This plot is based on the duration of the second flare and the jet half-opening angle ζ = 8.°3. The latter was derived from the parsec-scale jet kinematics of J1048+7143 seen at the f = 8.6 GHz observing frequency with VLBA.
Paper: Follow-up on the Supermassive Black Hole Binary Candidate J1048+7143: Successful Prediction of the Next Gamma-Ray Flare and Refined Binary Parameters in the Framework of the Jet Precession Model
Authors: Emma Kun, Ilja Jaroschewski, Julia Becker Tjus, Silke Britzen, Sándor Frey, Krisztina Éva Gabányi, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Geometry of the jet-precession-induced light-curve variation. The jet, driven by the spin–orbit precession in an SMBBH, goes through a target that supplies target protons for the hadronic processes between them and high-energy cosmic rays accelerated in a spine–sheath structured jet.
Paper: Follow-up on the Supermassive Black Hole Binary Candidate J1048+7143: Successful Prediction of the Next Gamma-Ray Flare and Refined Binary Parameters in the Framework of the Jet Precession Model
Authors: Emma Kun, Ilja Jaroschewski, Julia Becker Tjus, Silke Britzen, Sándor Frey, Krisztina Éva Gabányi, Lang Cui, Xin Wang, Yuling Shen
Figure caption: Linear (left) and accelerated (right) proper motion fits for jet components C1 and C2 of J1048+7143 at 8.6 GHz. Only observations before the flaring behavior of J1048+7143 started are used to make these plots.
Paper: Restoration of the Tully–Fisher Relation by Statistical Rectification
Authors: Hai Fu
Figure caption: The rectified distribution ψ  r (ξ, η) after 30 iterations. This is the restored i-band TFR. The red dashed curve in the main panel shows the best-fit power law. The inset shows the curvature of the relation by comparing the peak positions of the ridge (black circles) with the same power law. The gray shaded areas show the Gaussian σ widths of the ridge in velocity. The side panels compare the marginalized distributions before and after rectification (blue and yellow, respectively). They illustrate the differences between the observed H I-velocity width function and i-band luminosity function and the rectified functions. Note that selection effects, such as the magnitude limit and the volume incompleteness, have not been corrected.
Paper: Restoration of the Tully–Fisher Relation by Statistical Rectification
Authors: Hai Fu
Figure caption: The joint pdf ﹩P(\tilde{x},\tilde{y}| \xi ,\eta ,{\sigma }_{x},{\sigma }_{y})﹩ for ξ = 330 km s−1, η = −18, σ  x  = 20 km s−1, σ  y  = 0.14, σ 0 = 30 km s−1, and γ = 0.73. The intrinsic values are indicated by the red cross, which is offset from the peak of the pdf. The top panel shows the pdf marginalized over the ﹩\tilde{y}﹩-axis (yellow). This gives the pdf of the measured values, ﹩P(\tilde{x}| \xi ,{\sigma }_{x})﹩ per Equation (13), which can be compared with the pdf of the true projected values P(x∣ξ) from Equation (10) (blue) to see the effects of measurement errors. The right panel shows the joint pdf marginalized over the ﹩\tilde{x}﹩-axis and P(y∣η) from Equation (11).
Paper: Role of Planetary Radius on Atmospheric Escape of Rocky Exoplanets
Authors: Laura Chin, Chuanfei Dong, Manasvi Lingam
Figure caption: The calculated atmospheric ion escape rates as a function of planetary radius, which manifest a nonmonotonic trend, peaking at R = 0.75R  V .
Paper: Restoration of the Tully–Fisher Relation by Statistical Rectification
Authors: Hai Fu
Figure caption: The distribution of the ALFALFA-SDSS galaxy sample after individual inclination angle correction based on the axial ratio (b/a). The red dashed curve shows the best-fit power law in Figure 4. The side panels compare the marginalized distributions before and after the inclination-angle correction.
Paper: Restoration of the Tully–Fisher Relation by Statistical Rectification
Authors: Hai Fu
Figure caption: Data vs. model. From left to right are, respectively, the observed ﹩\tilde{\phi }﹩ distribution (same as Figure 1), the model ϕ  r  distribution after 30 iterations, and the absolute differences between the two distributions. For a fair comparison, the same color scale and contrast are used in all panels.
Paper: Role of Planetary Radius on Atmospheric Escape of Rocky Exoplanets
Authors: Laura Chin, Chuanfei Dong, Manasvi Lingam
Figure caption: Logarithmic scale contour plots of the escaping O+ ion density (units of cm−3) in the meridional plane for cases with different planetary radii subjected to the same ancient solar conditions. The second plot from the left in the top row (R = 0.75R  V ) has the highest atmospheric ion escape rate.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Illustrations of LFs and samples. Horizontal lines show m  I,OGLE for the four samples, Allstars (blue), SARGs (black), A sequence (yellow), and B sequence (red). From left to right: CMD of the Allstars sample (see Table 3) with contours (95th and 99th percentiles) of the A and B sequences overlaid; OGLE-III SARGs (black points) in the vicinity of the A and B PL sequences shown as yellow and red points; binned and smoothed LFs (here σ  s  = 0.15 mag) normalized to the number of stars within 0.1 mag of m  I,OGLE = 14.7 mag; and Sobel filter response curves normalized to peak height. Variability information is required to distinguish the A and B sequences from other RGs and SARGs, since the samples fully overlap in color–magnitude space.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Dependence of m  I  on σ  s . Error bars are plotted for the Allstars, SARG, and A- and B-sequence samples across the range of σ  s  values deemed stable, which is narrow for Allstars and wide for SARGs. Results from Table 2 are shown as large error bars on the right.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Virtually all stars at the TRGB are variable. Left: coarsely binned CMD indicating the fraction of SARGs to all stars using a color map indicated at the top. Blue contours highlight the RGB’s location by delineating the 70% (thicker) and 20% (thinner) contours of all stars in the OGLE-III LMC photometric map (Udalski et al. 2008; Soszyński et al. 2009). The TRGB’s location is shown as a dotted line. The fraction of variable stars increases upward toward the TRGB, reaching nearly 100% at the tip. Right: LFs of Allstars (black), SARGs (orange), and their complement (gray).
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Ages of SARGs from Povick et al. (2023), based on APOGEE near-infrared spectra. Left: histogram of stellar ages on SARG sequences A and B. Sequence B is significantly older than sequence A, as well as less metallic (not shown). The ages of the oldest stars are particularly uncertain. Right: period–Wesenheit relations of OGLE-III SARGs near sequences A and B with ages color-coded. Sequence A exhibits significant age differences from its short-period boundary to its long-period boundary, consistent with an evolutionary sequence. Stars on sequence B are significantly older.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Simulated LFs probe the dependence of ﹩{m}_{\mathrm{SARG},\mathrm{mode}}﹩ on LF shape. Left: observed (error bars) and simulated (shaded regions) values of m TRGB against smoothing parameter. The simulations reproduce observed trends at a level of approximately 0.005 mag. The simulated true m TRGB,0 = 14.495 coincides with the 1σ interval of our measured TRGB shown as red horizontal lines. Right: observed (steps) and simulated (smooth curves) LFs.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Inferring the EDR weighting scheme and σ  s  values used by H23. We sought to reproduce both the sample selection and methodology explained by H23 (color cut applied, low R  I  = 1.219 used) and measured m TRGB over a range of σ  s  values using different EDR weighting schemes for the five “calibration” fields used by H23 as well as their combination. Left: difference of TRGB magnitude minus H23 for three weighting schemes using combined fields. Poisson weighting and σ  s  ≈ 0.13 mag exactly reproduces H23. Center: difference of TRGB magnitude minus H23 for individually selected fields using Poisson weighting, which yields the best consistency. No single value of σ  s  reproduces the individual results reported by H23. Right: m TRGB for the five selected fields using Poisson EDR weighting. The result from the combined sample is shown as a solid black horizontal line for reference together with the most likely σ  s  value used by H23. NB: averaging m TRGB from individual fields does not and is not expected to yield the same m TRGB as the combined set of stars in all fields.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Bias induced by weighting Sobel filter responses using different methods. Simulated LFs (σ  s  = 0.11 mag) for Allstars (open circles), SARGs (filled cyan, yellow, and magenta circles), and the B sequence (filled blue, green, and red circles) exhibit consistent bias as a function of tip contrast R when using the same EDR. Regardless of sample, the unweighted EDR yields the least biased and the Poisson EDR the most biased results. Differences in R arise from the biased estimation of m TRGB. All TCRs are nonlinear; the linear trend by Scolnic et al. (2023; black dotted line) is a good approximation for R between 2 and 5. Solid lines represent fits to solid symbols and dashed lines those to open symbols. The quadratic fit to the Poisson EDR Allstars sample (dashed magenta line) yields −0.060 mag at R = 6.4.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Comparison of input ﹩{C}_{-}^{+}﹩ used to simulate the LFs (see Equation (B7)) and the tip contrast R determined using different samples and EDR weighting schemes. R can differ greatly according to EDR weighting scheme because it is evaluated at increasingly biased m TRGB. Based on the same LFs shown in Figure 8.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: The ratio of SARGs on sequences A and B is rather even across the OGLE-III LMC footprint. Left: TRGB magnitudes from H23 measured from different spatial following H23 using their Voronoi tessellation vs. the ratio of SARGs on sequence A to B. The calibration fields used by H23 are highlighted in red, and the vertical dashed line indicates the mean ratio of A to B. Center: same as left but vs. the ratio of SARGs on sequences A and B to all SARGs. Right: ratio of stars on the A and B sequences across the LMC OGLE-III footprint with Voronoi spatial bins numbered as in H23.
Paper: Small-amplitude Red Giants Elucidate the Nature of the Tip of the Red Giant Branch as a Standard Candle
Authors: Richard I. Anderson, Nolan W. Koblischke, Laurent Eyer
Figure caption: Investigating bias due to TRGB contrast (left) and steepness (center) for the Allstars (blue) and SARG (black) samples at σ  s  = 0.15 mag. Equation (B7) defines ﹩{C}_{-}^{+}﹩ independently of m TRGB. Higher-contrast (larger ﹩{C}_{-}^{+}﹩) and steeper (smaller w) TRGB features reduce bias and enhance precision. Vertical dashed lines indicate the values of the observed samples at ﹩{C}_{-}^{+}﹩ (Equation (B7)) from Table 4. The right-hand panel illustrates how varying these parameters changes the SARG LF.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. IV. NIRISS Aperture Masking Interferometry Performance and Lessons Learned
Authors: Steph Sallum, Shrishmoy Ray, Jens Kammerer, Anand Sivaramakrishnan, Rachel Cooper, Alexandra Z. Greebaum, Deepashri Thatte, Matthew De Furio, Samuel M. Factor, Michael R. Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Sasha Hinkley, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Sarah K. Betti, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Daniel Kitzmann, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Cecilia Lazzoni, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Anna Lueber, Bruce Macintosh, Elena Manjavacas, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, B. A. Sargent, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Ben J. Sutlieff, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo
Figure caption: Uncalibrated Fourier observables. The small black circles, medium gray circles, and large purple circles show observables for HD 115842, HD 116084, and HIP 65426, respectively. The top left panel shows complex visibility amplitudes vs. baseline length, normalized by the total signal in the images and multiplied by the number of mask holes. These values should all be equal to 1 for a perfect-Strehl point-source observation. The bottom left panel shows squared visibilities vs. baseline length with the same normalization applied. The top right panel shows complex visibility phases vs. baseline length, and the bottom right panel shows closure phases vs. the average length of the three baselines in each triangle. In all panels statistical error bars (estimated from the standard error measured across all integrations) are smaller than the size of the symbols.