adsabs/AstroCLIMB huggingface dataset:
Paper: Repeating Fast Radio Bursts Reveal Memory from Minutes to an Hour
Authors: F. Y. Wang, Q. Wu, Z. G. Dai
Figure caption: The rescaled range analysis of repeating FRBs. Panel (a): Red scatters correspond to the R/S ratio value of FRB 20121102. The black solid line is the power-law fit and the power-law exponent is the Hurst exponent. The Hurst exponent is 0.62 ± 0.04 at 1σ confidence level, which is shown as the shaded region. Panel (b): The blue points and black solid lines are the R/S ratio value and power-law fit of FRB 20201124A, respectively. The Hurst exponent of FRB 20201124A is 0.70 ± 0.04 at 1σ confidence level, which is shown as the shaded region.
Paper: Repeating Fast Radio Bursts Reveal Memory from Minutes to an Hour
Authors: F. Y. Wang, Q. Wu, Z. G. Dai
Figure caption: The frequency distribution of burst energy for FRB 20121102 and FRB 20201124A. Panel (a): The energy distribution of FRB 20121102. The black solid line with the error bar shows the differential distribution of energy for the “Long” bursts and the blue solid line for the “Short” bursts. The red dashed line at E = 2.5 × 1037 erg indicates the 90% detection completeness threshold of FAST. Panel (b): same with Panel (a), but for FRB 20201124A and the red dashed line shows the 95% detection completeness threshold of FAST.
Paper: Repeating Fast Radio Bursts Reveal Memory from Minutes to an Hour
Authors: F. Y. Wang, Q. Wu, Z. G. Dai
Figure caption: Time series of the lattice energy (panels (a) and (c)) and the released energy of simulated avalanches (panels (b) and (d)) in three-dimensional cellular automaton simulation. A 303 lattice with 1 × 106 iterations is applied in this simulation. While two panels on the left represent the SOC process with random drives and two panels on the right represent the time-dependent drives. Panels (b1) and (d1) demonstrate a portion of the time series of released energy, which can identify an individual burst. Simulated waiting time can be derived from the time between two consecutive pulses.
Paper: Repeating Fast Radio Bursts Reveal Memory from Minutes to an Hour
Authors: F. Y. Wang, Q. Wu, Z. G. Dai
Figure caption: Waiting time distributions from cellular automaton simulations of three-dimensional SOC lattice model. Panel (a): The differential distribution of waiting times for random driving forces. It conforms to a single exponential distribution (blue line), which is characterized by an extreme decrease in long waiting times. Panel (b): The differential distribution of waiting times for the driving force is related to a random walk function. The blue line is the power-law fit for the waiting times.
Paper: Estimating AGN Black Hole Masses via Continuum Reverberation Mapping in the Era of LSST
Authors: Shu Wang, Hengxiao Guo, Jong-Hak Woo
Figure caption: Upper panels: comparison between the BLR and CER size–luminosity relation. The red symbols represent the Hβ BLR sizes (R BLR) except for NGC 4395 where only Hα is available, while the blue symbols represent the CER sizes (R CER) at rest-frame λ = 5100Å. Parent, core, and local samples are displayed by squares, diamonds, and circles, respectively. The CER size has a luminosity dependence of R CER ∝ L 0.48 (G22), comparable to that of BLR, i.e., R BLR ∝ L 0.48 (Dalla Bontà et al. 2020). Lower panels: the BLR–CER size comparison using 21 objects with both BLR and CER size well measured. The symbols are same as two upper panels. The brown dashed line represents the best-fit relation from linear regression, and the orange lines are randomly selected realizations in the Markov chain Monte Carlo chains derived by emcee. The left two panels show the results including NGC 4395, while the two right panels show the results without NGC 4395.
Paper: Estimating AGN Black Hole Masses via Continuum Reverberation Mapping in the Era of LSST
Authors: Shu Wang, Hengxiao Guo, Jong-Hak Woo
Figure caption: Left panel: application of the fiducial R BLR–R CER relation to the rest objects in our CRM sample to predict the R BLR. Different samples are labeled using different symbols as in Figure 1. Filled and open black symbols represent the objects with and without available BLR size measurements, respectively. The light orange circles refer to the R BLR of Hβ from spectroscopic RM observation. The red dashed line shows the best-fit relation of Hβ R BLR–L relation by Dalla Bontà et al. (2020). Right panel: application of the fiducial R BLR–R CER relation to the rest objects in our CRM sample to calculate the CRM BH mass, compared with their Hβ RM (filled symbols)/SE (open symbols) BH mass. For crossmatched sample, both their RM and SE mass are included in comparison. The black dashed line indicates the 1:1 correspondence. The CRM and Hβ RM/SE BH mass show good consistency.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: Image cutouts and light curves with various bin sizes for a transient candidate detected in TESS sector 30. The top left panel is the reference image centered on the location of the transient, while the top right panel is a similar cutout, albeit for the rms image for all difference images across the sector (this is further discussed in Section 2.2.1). There is a clear point source that appears in the rms image that is not present in the reference image. The bottom panels contain the light curves for this transient at various bin sizes: from left to right, 10 minutes, 8 hr, and 24 hr (1 day), respectively. The black dotted line represents the 3σ detection limit for that level of stacking; these limits are also indicated in the corresponding plots. The light curves’ y-coordinates are in units of TESS magnitude (i.e., the bandpass in Figure 1), and the x-axis is in TESS Julian Date (TJD), which is JD–2,457,000.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: TESS band (black line), including the detector quantum efficiency, compared to the optical and near-infrared bands of Pan-STARRS (Tonry et al. 2012; dotted lines). These have been plotted alongside the early-time (light blue) and late-time (tan) SEDs of the optical counterpart to GW170817 (Shappee et al. 2017). The SED of the kilonova becomes redder as time passes, showing that TESS's bandpass is uniquely positioned to continuously observe the decay of the afterglow over a timescale of days.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: Cumulative distribution of GW sky map probability enclosed in the earliest possible TESS observations for O3 events, the Frostig O4 BNS simulation, and the Petrov O4 simulation. The O3 distribution includes all 75 events (BBH, NSBH, and BNS) publicly released by the LVK as part of GWTC-2 and -3. If the GW event happened while TESS was not observing due to a data downlink (seven of the 75 events), the overlap integral was calculated for the next available set of observations. For the remaining events, the overlap is with the concurrent sector. In this study, we primarily use the Frostig simulations but include here the Petrov simulations for comparison. The difference in the enclosed area on the left end of the distribution between the two sets of O4 simulations is primarily due to the Petrov simulation’s inclusion of events detected in a single GW detector. Both sets of O4 simulations find that about 10% of BNS events will have at least 10% of their sky probability covered in TESS. See Section 4 for details on the differences between the two sets of simulations.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: Examples of TESS coverage of GW sky maps, plotted in celestial coordinates, for two individual GW events. Left: best TESS-covered event in O3, the BBH merger GW200209_085452, which was concurrent with TESS sector 21. The enclosed probability is 0.719. No EM counterparts were found in a search of TESS data. Right: example simulated BNS event for O4, where the entire probability is enclosed in the concurrent TESS. This event’s associated simulated light curve peaks at 19.4 mag in the TESS band, which is easily detectable in TESS with an 8 hr stack of FFIs (this 8 hr stack pushes the 3σ detection limit to ∼21). For an event such as this, the entire GW localization region would be observed in the TESS FOV, meaning that TESS would be able to supply not only a precise localization but also photometry showing the full rise and evolution of the kilonova light curve.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: Distribution of the fraction of GW-detected events observable as a function of the overall stacked integration time (top axis) and TESS limiting magnitude (bottom axis) at a variety of lanthanide fractions. Stacking TESS FFIs lowers the limiting magnitude, allowing us to detect more events, especially for kilonovae with lower lanthanide fractions. For higher lanthanide fractions (e.g., X lan = 10−2), over three-fourths of the events will not be detectable at an 8 hr stack (∼21 mag); the majority will require an FFI stack of a day or more to be detectable. Lower lanthanide fractions, on the other hand, will result in almost 60% of GW-detected events being bright enough to be detectable using an ∼8 hr stack of FFIs. Note that the limiting magnitude as a function of stacked exposure time presented here is based only on counting noise from the source and background. In practice, the limiting magnitude can vary significantly, by up to 2–3 mag, due to image backgrounds, proximity of targets to other bright objects, and other factors.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: Example TESS-band kilonova light curves for one of the brightest GW-detected events in the simulation, a BNS merger at a luminosity distance of 64 Mpc. Light curves for various values of the lanthanide fraction (X lan) are shown, along with an estimate for the 3σ TESS limiting magnitude of a 4 hr stack (T mag ∼ 20.5). Ejecta with higher lanthanide fractions have lower opacity, which obscures the optical and near-infrared emission. Since the TESS bandpass is in the optical and near-infrared, it is more sensitive to kilonovae with lower lanthanide fractions. For all lanthanide fractions, TESS should be able to observe at least part of the rise and decay of the light curve of a sufficiently bright kilonova.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: TESS-band light curves for all 96 simulated O4 BNS events found in GWs for X lan = 10−5. Individual light curves are shown in light blue. The median light curve is in solid black, and the 90% interval is bounded by the black dotted lines. The brightest light curves can peak at almost 18 mag, whereas the median light curve peaks near 21 mag. Despite varying dynamical ejecta mass M ej and ejecta expansion velocity v ej across the simulated events, the light curves all tend to peak ∼1 day after merger and subsequently decay at a similar rate.
Paper: Searching for Gravitational-wave Counterparts Using the Transiting Exoplanet Survey Satellite
Authors: Geoffrey Mo, Rahul Jayaraman, Michael Fausnaugh, Erik Katsavounidis, George R. Ricker, Roland Vanderspek
Figure caption: TESS light curves of J1249, the AGN with a flare reported by Graham et al. (2020). The light curves are binned to 8 hr, and the error bars show the standard deviation in each bin scaled by the square root of the number of data points. In sector 22, the light curve is consistent with a constant light curve. In sector 49, there is excess variability at the 5% level, but inspection of the difference images suggests that these are residual systematic errors.
Paper: Formation of the Transition Region for the Quiet Sun
Authors: Paul Song, Jiannan Tu, David B. Wexler
Figure caption: Model of the chromosphere with the size of a supergranule, ∼30 Mm (not to scale), of which the strong network magnetic field area is located in the center of the diagram rooted in the photosphere with weaker photospheric fields that do not reach the upper chromosphere. The solid lines indicate the magnetic field lines, and the dashed lines indicate the convection streamlines of neutral flow. The orange shaded regions indicate high heating rates. The green region is the photosphere, adapted from Song (2017).
Paper: Formation of the Transition Region for the Quiet Sun
Authors: Paul Song, Jiannan Tu, David B. Wexler
Figure caption: Evaluation of the would-be radiative loss rate (Equation (15), blue line), ionization potential energy (Equation (16), green line), sum of the cooling effects (black dashed line), and loss rate of the heat flux (red line) based on temperature and densities given by the AL model.
Paper: Formation of the Transition Region for the Quiet Sun
Authors: Paul Song, Jiannan Tu, David B. Wexler
Figure caption: Blue solid lines are model predictions of temperature T, neutral density N n, flow velocity V, and plasma density N i from the present theory, and black dashed lines are the comparison with the semiempirical AL model.
Paper: Formation of the Transition Region for the Quiet Sun
Authors: Paul Song, Jiannan Tu, David B. Wexler
Figure caption: Temperature (blue line), total hydrogen number density (green line), and electron number density (red line; Avrett & Loeser 2008).
Paper: Constraints on Magnetic Braking from the G8 Dwarf Stars 61 UMa and τ Cet
Authors: Travis S. Metcalfe, Klaus G. Strassmeier, Ilya V. Ilyin, Jennifer L. van Saders, Thomas R. Ayres, Adam J. Finley, Oleg Kochukhov, Pascal Petit, Victor See, Keivan G. Stassun, Sandra V. Jeffers, Stephen C. Marsden, Julien Morin, Aline A. Vidotto
Figure caption: Rotation−activity relation for stars published in Corsaro et al. (2021), with the critical value of Ro from Section 3 shown as a vertical dashed line. Bright asteroseismic targets are shown with red circles. The highest density of stars (yellow and green) exhibit a broad range of activity levels at nearly constant Ro, which may correspond to the long-period edge of the Kepler sample.
Paper: Constraints on Magnetic Braking from the G8 Dwarf Stars 61 UMa and τ Cet
Authors: Travis S. Metcalfe, Klaus G. Strassmeier, Ilya V. Ilyin, Jennifer L. van Saders, Thomas R. Ayres, Adam J. Finley, Oleg Kochukhov, Pascal Petit, Victor See, Keivan G. Stassun, Sandra V. Jeffers, Stephen C. Marsden, Julien Morin, Aline A. Vidotto
Figure caption: Evolution of the wind braking torque with Ro from the calibration of Corsaro et al. (2021). Points are grouped by Gaia color, corresponding to solar analogs (yellow circles) and hotter (blue triangles) or cooler stars (red squares). The empirical constraint for Rocrit on this scale is shown with a vertical dashed line.
Paper: Constraints on Magnetic Braking from the G8 Dwarf Stars 61 UMa and τ Cet
Authors: Travis S. Metcalfe, Klaus G. Strassmeier, Ilya V. Ilyin, Jennifer L. van Saders, Thomas R. Ayres, Adam J. Finley, Oleg Kochukhov, Pascal Petit, Victor See, Keivan G. Stassun, Sandra V. Jeffers, Stephen C. Marsden, Julien Morin, Aline A. Vidotto
Figure caption: Stokes V polarization profile for τ Cet from LBT observations on 2022 September 18. The mean profile is shown as a black line with uncertainties indicated by the gray shaded area. The dashed blue line is an axisymmetric model profile assuming dipole morphology with the inclination fixed at i = 20°.
Paper: MAXI J1848-015: The First Detection of Relativistically Moving Outflows from a Globular Cluster X-Ray Binary
Authors: A. Bahramian, E. Tremou, A. J. Tetarenko, J. C. A. Miller-Jones, R. P. Fender, S. Corbel, D. R. A. Williams, J. Strader, F. Carotenuto, R. Salinas, J. A. Kennea, S. E. Motta, P. A. Woudt, J. H. Matthews, T. D. Russell
Figure caption: Left: VLA 10 GHz image of MAXI J1848−015 as observed on 2021 February 27. Two bright lobes are clearly detected. At the midpoint between the two lobes, a low-significance source (at 3.5σ) is present (denoted by a gray arrow). We demonstrate the motion of these lobes in Section 3.2. The white dashed circle indicates the localization of the X-ray transient by Kennea et al. (2021) based on Swift/XRT, while the yellow dotted circle represents the localization by Chakrabarty et al. (2021) based on Chandra/ACIS (both plotted with 90% confidence localization radii). The VLA synthesized beam is represented with a filled gray ellipse in the corner of the image. Right: MeerKAT 1.3 GHz image of outflows from MAXI J1848−015 as observed on 2022 June 3 (as an example for comparison with the VLA image on the left). The MeerKAT synthesized beam is represented with a filled gray ellipse in the corner of the image. The white box in the center indicates the region shown in the left panel and the red/orange contours are representative of the VLA flux densities on 2021 February 27 as shown in the left panel (representing 15, 30, and 60 μJy, from red to yellow). Note that the two panels have different spatial and flux density scales.
Paper: MAXI J1848-015: The First Detection of Relativistically Moving Outflows from a Globular Cluster X-Ray Binary
Authors: A. Bahramian, E. Tremou, A. J. Tetarenko, J. C. A. Miller-Jones, R. P. Fender, S. Corbel, D. R. A. Williams, J. Strader, F. Carotenuto, R. Salinas, J. A. Kennea, S. E. Motta, P. A. Woudt, J. H. Matthews, T. D. Russell
Figure caption: Left: position of the outflows from MAXI J1848−015 as observed over time. Unfilled markers represent observations in which the lobes could not be distinguished clearly. These observations were not included in the modeling. The gray line represents the jet axis on the sky plane as determined by the location of the lobes in the first VLA observation. The shaded gray interval represents the scatter angle (posterior median) as determined by our model (Section 3.2). Right: proper motion of the radio lobes parallel to the jet axis (colored triangles) and perpendicular to the jet axis (gray triangles), over time as observed during our monitoring campaign (error bars are smaller than the markers). The yellow line indicates a best-fit model, based on posterior medians, and the shaded yellow interval represent the 90% highest density interval of model posteriors.
Paper: MAXI J1848-015: The First Detection of Relativistically Moving Outflows from a Globular Cluster X-Ray Binary
Authors: A. Bahramian, E. Tremou, A. J. Tetarenko, J. C. A. Miller-Jones, R. P. Fender, S. Corbel, D. R. A. Williams, J. Strader, F. Carotenuto, R. Salinas, J. A. Kennea, S. E. Motta, P. A. Woudt, J. H. Matthews, T. D. Russell
Figure caption: Pairwise plots of the posterior samples for parameters in the model described in Section 3.2. All samples appear unimodal. Significant anticorrelations are noticeable between proper motions and decelerations of the lobes. This is expected as with a lower initial proper motion; less deceleration would be needed to achieve a similar displacement. Initial proper motions and decelerations also show some degree of (anti)correlation with the predicted outflow launch date. This is likely due to the fact that the very early behavior of the outflows is only captured by a single highly influential observation (the VLA observation in 2021 February; see Figure 3).
Paper: MAXI J1848-015: The First Detection of Relativistically Moving Outflows from a Globular Cluster X-Ray Binary
Authors: A. Bahramian, E. Tremou, A. J. Tetarenko, J. C. A. Miller-Jones, R. P. Fender, S. Corbel, D. R. A. Williams, J. Strader, F. Carotenuto, R. Salinas, J. A. Kennea, S. E. Motta, P. A. Woudt, J. H. Matthews, T. D. Russell
Figure caption: Pairwise plots for the ejection angle and the intrinsic speed of ejection (β int = v/c, where c is speed of light), estimated using the posterior samples for μ 0,N  and μ 0,S , and assuming a distance of 3.4 ± 0.3 kpc (Hare et al. 2018). The shaded light and dark gray intervals in the pairwise panels containing distance indicate the median and 95% quantile, respectively, on the maximum possible distance as inferred in Section 4.1.
Paper: MAXI J1848-015: The First Detection of Relativistically Moving Outflows from a Globular Cluster X-Ray Binary
Authors: A. Bahramian, E. Tremou, A. J. Tetarenko, J. C. A. Miller-Jones, R. P. Fender, S. Corbel, D. R. A. Williams, J. Strader, F. Carotenuto, R. Salinas, J. A. Kennea, S. E. Motta, P. A. Woudt, J. H. Matthews, T. D. Russell
Figure caption: Detection and evolution of the outflows from MAXI J1848−015 as seen by MeerKAT (in the L band at 1.28 GHz), since it was first detected in 2021 February. Following the initial detection, both south and north lobes showed varying brightness. The two lobes were clearly distinguishable for the first time in 2021 April, approximately 2 months after the initial detection of the lobes by the VLA.
Paper: JWST and ALMA Imaging of Dust-obscured, Massive Substructures in a Typical z ∼ 3 Star-forming Disk Galaxy
Authors: Wiphu Rujopakarn, Christina C. Williams, Emanuele Daddi, Malte Schramm, Fengwu Sun, Stacey Alberts, George H. Rieke, Qing-Hua Tan, 清华 谈, Sandro Tacchella, Mauro Giavalisco, John D. Silverman
Figure caption: JWST images of UDF2. The left panel shows JWST color composite; the four subpanels on the right show an F182M image with the cyan dotted circle indicating the position of the brightest feature previously seen in an HST/F160W image (Figure 1 of Rujopakarn et al. 2019) that is now resolved into multiple pointlike features; F210M image with the yellow dotted arc indicating the semicircular feature around the center of stellar-mass distribution that is clearly visible in the F430M and F480M images. Each cutout is 3″ × 3″; north is up, and east is to the left.
Paper: JWST and ALMA Imaging of Dust-obscured, Massive Substructures in a Typical z ∼ 3 Star-forming Disk Galaxy
Authors: Wiphu Rujopakarn, Christina C. Williams, Emanuele Daddi, Malte Schramm, Fengwu Sun, Stacey Alberts, George H. Rieke, Qing-Hua Tan, 清华 谈, Sandro Tacchella, Mauro Giavalisco, John D. Silverman
Figure caption: The star-forming substructures (orange contours starting from 3σ in 1σ increments), in the context of the rest of the galaxy. Notably, the HST/F606W image (rest-frame 160 Å) shows the spatial dislocation between unobscured SF and the northern ridge; the JWST/F182M and F210M images show that the northern ridge appears to be a part of the semicircular arc around the central stellar-mass distribution observed at F430M. The red contour delineates the 10σ isophotal extent of unsubtracted ALMA emission (with the red dot marking the peak).
Paper: JWST and ALMA Imaging of Dust-obscured, Massive Substructures in a Typical z ∼ 3 Star-forming Disk Galaxy
Authors: Wiphu Rujopakarn, Christina C. Williams, Emanuele Daddi, Malte Schramm, Fengwu Sun, Stacey Alberts, George H. Rieke, Qing-Hua Tan, 清华 谈, Sandro Tacchella, Mauro Giavalisco, John D. Silverman
Figure caption: Three other massive galaxies spectroscopically confirmed to be at z = 2.690–2.697 are within a projected distance of 70 kpc from UDF2, suggesting a potentially overdense region that may have implications on the origin of the substructures identified.