adsabs/AstroCLIMB huggingface dataset:
Paper: Prospects of Constraining Equilibrium Tides in Low-mass Binary Stars
Authors: Jessica Birky, Rory Barnes, James R. A. Davenport
Figure caption: Same system as Figure 24, but modeled with CTL tides coupled with stellar evolution.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Summary of the results for our test of the orbiter–disk collision model for QPEs. The y-axis shows the change in QPE temperature between 2014 and 2018, with the blue region representing the range allowed by the data (i.e., QPEs detected in 2018 but not in 2014). The x-axis shows the change in disk surface density at the orbiter radius (Σ(rorb)), with the gray shaded region indicating the range inferred from our time-dependent disk modeling. The red line shows the prediction from the model of I. Linial & B. D. Metzger (2023) (Equations (24) and (25)). The figure illustrates that a change in ﹩{T}_{\mathrm{obs}}^{\mathrm{QPE}}﹩ toward undetectable values does not seem to be able to account for the absence of QPEs in 2014 and their appearance in 2018, as the change in Σ(rorb) was insufficient. See the text for a detailed discussion.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Evolution of observable and physical properties of GSN 069, ASASSN-14li, and AT2019dsg, all normalized by the median value of the best-fit tvisc parameter (as listed in Table 2). This normalization demonstrates that the solutions to the disk evolution equations are scalable by tvisc and, to first order, follow the forms given in Equations (17), (18), and (19). The remaining differences in their properties—primarily in the amplitudes—are governed by the other disk-back hole parameters, while the time evolution becomes largely universal once normalized by tvisc.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Comparison between 0.2 and 2.0 X-ray luminosity light curves between GSN 069, ASASSN-14li, and AT2019dsg. The shaded region represents the 68% credible interval of FitTeD-SPEC fitting for all three sources. The figure illustrates how the same physical framework can describe the evolution of the three sources, with tvisc being the main parameter driving their distinct time evolution. The main best-fitted parameters for the three sources are shown in Table 2.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Study of the 2020–2022 rebrightening event. Top: illustrative addition of a second FitTeD solution to reproduce the flare. This is not a fit—neither to the flare’s luminosity nor its spectra. The green points were simply scaled linearly from the count rate, without accounting for spectral evolution or uncertainties. Shown for illustrative purposes only. Bottom: fraction of the remaining disk mass with local temperatures T ≤ 104 K, as a function of time. This is a relevant quantity for the H.I.I., which can only be calculated with a time-dependent model of the disk. Vertical colored lines mark key timescales in the source’s evolution; see the text for a discussion.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Correlation between peak disk bolometric luminosity of GSN 069 (gray), ASASSN-14li (red), and AT2019dsg (green), and the ratio between their best-fitted initial disk mass (Md) and “viscous” timescale (tvisc). The figure illustrates how even disks with lower mass content (AT2019dsg) will produce brighter peak luminosities if the rate of angular momentum transport (i.e., ﹩{W}_{\,\phi }^{r}\propto {t}_{{\rm{visc}}}^{-1}﹩) is higher, such that the absolute mass accretion rate, ﹩\dot{M}({r}_{I})﹩, is higher.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: UV spectra processing. Right: observed unbinned spectra in the two epochs 2014 (purple) and 2018 (pink). Green spectra show the best-fitted stellar contribution modeled in Paper I. Dotted lines show the wavelength range used to bin the spectra. Left: binned spectra. All the spectra are shown as observed, with no extinction correction.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Examples of our time-dependent fitting on the X-ray spectral of ASASSN-14li (top) and AT2019dsg (bottom) at different epochs. Left: unfolded flux spectra with no absorption correction. Right: unfolded luminosity spectra, with both intrinsic and Galactic absorption corrections. The Δt’s in the legend refer to the interval between the observation and the predicted X-ray peak.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Probability density function of the change in disk’s mass surface density at the position of the proposed orbiter (for disk collision QPE models), from 2014 to 2018.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: The seven folded X-ray spectra normalized by their instrument’s effective area as a function of energy.
Paper: A Time-dependent Solution for GSN 069 Disk Evolution and the Nature of Long-lived Tidal Disruption Events
Authors: M. Guolo, A. Mummery, A. Ingram, M. Nicholl, S. Gezari, E. Nathan
Figure caption: Simultaneous fitting of the disk and eruption components in 2014 and 2018. Top: the left panel shows the intra-observation XMM-Newton light curves, with colors indicating the intervals used to extract the corresponding spectra. The middle and right panels show the best-fit intrinsic (i.e., absorption-corrected) spectra: the purple/pink curves represent the disk component, while the red curves represent the blackbody/eruption component. Contours denote 68% credible intervals, except for the red contours in the middle panel, which show the 99% credible interval for the (undetected) eruption component in 2014. Bottom: posterior probability densities for the free parameters of the eruption component. In the panels showing the 2014 temperature, the dotted lines mark the 99% credible limit.
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Follow-up time-series photometry from 2022 March through 2023 November for ZTF J1944+4557 from Palomar (g-, r-, and i-bands), McDonald (BG40-band), Perkins (BG40-band), and Lowell (g-band) observatories, folded on a period of 4.9704 hr. Light curves are shown in chronological order from top to bottom, with each row representing a single orbital cycle. The UTC observation dates for each row are shown at right along with orbital cycle numbers in brackets, with phase = 0 during cycle  =  0 corresponding to BJDTDB  =  2459661.9693637. The shaded regions overlapping the 2023 June 20 (Cycle 2192) light curve represent the times during which we acquired five consecutive spectra with the Keck Low-Resolution Imaging Spectrograph (see Figure 4). The dual-channel CHIMERA photometry stringently constrains the transits as colorless (see Figure 8). In-transit variations evolve from one cycle to the next, yet the ingresses and egresses from consecutive nights align on the 4.9704 hr orbital period. The location in phase of the transits appears dynamic on a timescale of ﹩{ \mathcal O }(10)﹩ cycles. As of 2024 May 14 (Cycle 3780) the transits appear to have vanished until reappearing in 2025 March (see Figure 2). Our Large Monolithic Imager photometry is shown only in Figure 2 (see Appendix A).
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Top: the Lomb–Scargle periodogram of all nonoverlapping 2023 CHIMERA-g, McD-BG40, and PTO-BG40 observations. Black shows the raw periodogram while blue shows the residual periodogram after prewhitening the peaks detected in excess of the 5〈A〉 threshold (the green dashed–dotted line, where 〈A〉 is the mean of the residual periodogram within a sliding window of width 2000 μHz), indicated by yellow triangles. The frequency corresponding to the orbital period of 4.9713 hr (f) is indicated by a vertical red dotted line. High-harmonic power is present given the nonsinusoidal nature of the transits, and we label up to the 11th harmonic (11f) even if the peaks fall below the 5〈A〉 threshold. The period in hours is given along the top axis for each labeled peak, while an inset plot shows the spectral window of the observations. Bottom: conditional entropy periodogram for the same nonoverlapping 2023 CHIMERA-g, McD-BG40, and PTO-BG40 observations, set on the same frequency and period scales as the above Lomb–Scargle periodogram. A ρ = 10 threshold (see M. L. Katz et al. 2021) is plotted as the dashed–dotted green line. Harmonics of the fundamental are labeled in the same fashion as above. We inset the Gaussian fit that yields the annotated best period of P = 4.9704 ± 0.0019 hr.
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Concurrent time-series photometry and spectroscopy from CHIMERA and LRIS, respectively, during one of the transits observed on 2023 June 20. (Top) A portion of the 2023 June 20 r-band CHIMERA light curve, zoomed in on the transit feature throughout which we acquired five 600 s LRIS exposures, whose time spans are denoted by the gray shaded regions. (Middle) Each continuum-normalized LRIS spectrum, centered on the Ca-K absorption feature at 3934 Å. Green lines denote the rest wavelength of Ca-K. (Bottom) The measured Ca-K equivalent widths vs. the average photometric transit depth during each spectrum. Within our measurement uncertainties of around 0.15−0.2 Å (about 15%−20%), the equivalent widths are consistent with being nonvariable throughout the transit event. Variations could occur if some portion of the observed absorption were of circumstellar origin, and the transiting debris preferentially obscured a larger portion of the white dwarf than a gas disk interior to the transiting cloud of debris, or vice versa. WD 1145+017 shows in-transit bluing due to weaker circumstellar gas absorption from such a geometric effect (N. Hallakoun et al. 2017; M. Karjalainen et al. 2019; S. Xu et al. 2019b).
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Magnifications of the Ca-K (top), Fe-II 5018 Å (center left), 5169 Å, which could be a blend of Fe-II and Mg-II lines (center right), and Na-D doublet (bottom) transitions as observed by our 2023 June 20 Keck+LRIS spectra and modeled by our synthetic DAZ spectrum, all converted to velocity space. We aggregate all five spectra from Figure 4 and fit Gaussian profiles to the cores and report the associated velocity dispersions. Our synthetic spectrum is generated for a Teff = 20,794 K, ﹩{\mathrm{log}}(g\,[{\rm{cgs}}])=8.276﹩ DA white dwarf accreting bulk Earth material scaled to [Ca/H] = −5.0, convolved to the LRIS instrumental resolution (R ≈ 1500). Our synthetic spectrum fails to reproduce the observed equivalent widths of these transitions by photospheric absorption alone, suggesting circumstellar gas could be casting these features, especially the Fe-II and Na-D absorption.
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Same as Figure 1 but showing follow-up time-series photometry from 2024 May–November and 2025 March–July. Aside from a possible small dip at the beginning of the 2024 November 1 observations, no transit features are observed in 2024. Transits were again observed in 2025 March, with the two observed egresses phasing together on P = 4.9704 hr. We similarly do not resolve entire transits in our 2025 May observations due to inclement weather, but do capture two egresses and two ingresses that still align at the orbital period. Our uninterrupted 2025 July epochs fully resolve transit recurrence.
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Top: the ZTF forced-photometry light curve of ZTF J1944+4557 partitioned into eight seasons, distinguished by shading. We draw dotted silver-colored lines at the median timestamp of each season, across which we evaluate the skewness (bottom) for each half-season; the eighth season is not halved for its shortness. The skew uncertainties are taken as the standard deviation of the skew values found from a Monte Carlo simulation with 10,000 draws for each half-season. The smaller gray points are the averages of the same calculations for three nearby nonvariable white dwarfs of the same magnitude to provide a benchmark for expected seasonal flux variations. We find a general agreement with our follow-up photometry (Figure 6) that the transits were at heightened activity during the summer of 2023, ceased during the summer and fall of 2024, and recurred in 2025. This could suggest that the transit activity at ZTF J1944+4557 is variable over years-long timescales, fluctuating between heightened stages of transit activity (e.g., Fall 2021) and quiescent periods (e.g., Fall 2022). All half-seasons are consistent with transiting activity or quiescence, with the in-transit seasons showing much larger dispersion than observed for the nonvariable reference stars.
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Left: SED of ZTF J1944+4557 including photometry from Gaia DR3, Pan-STARRS DR1, CatWISE, unWISE, and Warm Spitzer. We superimpose this photometry above a synthetic spectrum for a DA white dwarf with Teff = 21,000 K and ﹩{\mathrm{log}}(g)=8.25﹩ (D. Koester 2010). The error bars on the Gaia and PS1 photometry are smaller than the marker sizes at these scales (σm ≲ 0.1 mag). Horizontal bars are spurious detections and downward-pointing arrows indicate upper limits. We are unable to currently place reliable constraints on the presence of an infrared excess at ZTF J1944+4557. The middle (PS1 i-band) and right (Spitzer IRAC Channel 1) images elucidate the unreliability of these near-infrared photometries. The 6﹩\mathop{.}\limits^{\unicode{x02033}}﹩1-radius aperture of WISE is shown as a black dashed circle, centered on the Gaia-measured centroid of ZTF J1944+4557 (green circle) and enclosing the centroid of the nearest source to ZTF J1944+4557 as measured by CatWISE (maroon circle). The CatWISE and unWISE centroids are coincident with a bright field source as imaged by Spitzer. The smaller 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 radius we use for our Spitzer photometry is shown as the black dotted circle in the rightmost panel, illustrating how the pixels at the Gaia-measured centroid of ZTF J1944+4557 are indistinguishable from empty sky.
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: Top: 2023 May 25 g+i and 2023 June 19 and 20 g+r light curves taken with CHIMERA shown in the same style as Figure 1, now magnified and unbinned to better appreciate the rapid variation in transit morphologies and lack of observed color terms. Bottom: comparison between the transit depths in the g-band vs. either the r- (left) or i-band depths (right), all in differential magnitudes, for our CHIMERA light curves from 2023 May, June, and August. The overlap with the dashed–dotted purple lines that trace the 1:1 relationships suggests the transits at ZTF J1944+4557 lack color variations (i.e., gray). The transiting effluents appear devoid of small (≲0.2 μm) dust particles. This is rigorously supported by our finding that the extinction coefficients are consistent with zero (Section 5.2).
Paper: Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 hr Orbit—and its Vanishing
Authors: Joseph A. Guidry, Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, Kareem El-Badry, Malia L. Kao, Lou Baya Ould Rouis, Antonio C. Rodriguez, Jan van Roestel
Figure caption: The total transit activity level measured as the percent of white dwarf flux blocked along the line of sight during transit events relative to the duration of the light curve. We exclude light curves from 2022 because of their relatively short baselines and minimal transit activity. All light curve fluxes except those from 2024 May to October are shifted down by the mean of the flux values greater than the 80th percentile to compensate for deep transits skewing the out-of-transit continuum from zero when normalizing the light curve during our reduction process. Marker colors map to the fractional phase coverage of the light curve (Porb = 4.9704 hr). At the highest activity levels observed, just over 19% of white dwarf flux is blocked along our line of sight during transit events, while at the lowest activity levels, few if any transits are observed (see also Figures 1 and 2).
Paper: Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers
Authors: Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke, Anna Wittje
Figure caption: Raw distributions of various galaxy properties in our lens catalog (M⋆ ≥ 1010 M⊙), before matching sample properties. (a) The raw stellar mass distribution. (b) The raw redshift distribution. (c) The raw distribution of the geometric mean distance to each galaxy’s three nearest neighbors.
Paper: Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers
Authors: Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke, Anna Wittje
Figure caption: The weighted distributions of our final lens samples’ galaxy properties. These galaxies are selected to live in low-density environments, as discussed in the text, and matched in (a) stellar mass, (b) redshift, and (c) the geometric mean distance to their three nearest neighbors. Two-sample KS test p-values for the controls and postmergers are: (a) 0.38, (b) 0.35, and (c) 0.34, indicating that differences in these weighted samples are not statistically significant. The redshifts of the randoms come from directly sampling the postmerger’s redshift KDE; a KS test between these two distributions yields p = 0.80.
Paper: Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers
Authors: Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke, Anna Wittje
Figure caption: The effective redshift distribution of the sources, n(zs), compared to the postmerger spectroscopic redshift distribution from Figure 4(b). For cosmology calculations, the n(zs) redshifts are still blinded; the source redshift distribution in this plot is close, but not identical, to the source redshift catalog used in this paper.
Paper: Unions with UNIONS: Using Galaxy–Galaxy Lensing to Probe Galaxy Mergers
Authors: Isaac Cheng, Jack Elvin-Poole, Michael J. Hudson, Ruxin Barré, Sara L. Ellison, Robert W. Bickley, Thomas J. L. de Boer, Sébastien Fabbro, Leonardo Ferreira, Sacha Guerrini, Fabian Hervas Peters, Hendrik Hildebrandt, Martin Kilbinger, Alan W. McConnachie, Ludovic van Waerbeke, Anna Wittje
Figure caption: 2D hexbin plots showing our metrics for environmental density: the number of neighboring galaxies within 1.5 Mpc and the geometric mean distance to the three nearest neighbors of each galaxy, Ravg. The coloring represents the number of galaxies, Ngal, in a hexbin. The vertical dashed line indicates Ravg = 2.25 Mpc. We want to select galaxies that live in low-density environments (i.e., the bottom right region of these plots).
Paper: Fermi Detection of γ-Rays from the Radio-quiet Seyfert Galaxy NGC 3281
Authors: Jun-Rong Liu, Hua Feng, Jian-Min Wang
Figure caption: Multiwavelength SED of NGC 3281 with best-fit model components. The red curves represent the intrinsic (thin) and observed (thick) model flux due to inverse Compton scattering in the corona. The blue curves represent the external inverse Compton (solid), synchrotron (dashed), and synchrotron self-Compton (dotted) processes in the jet. The black curves represent the SEDs of seed photons. The radio (J. S. Ulvestad & A. S. Wilson 1989; J. J. Condon et al. 1998; H. R. Schmitt et al. 2001; T. Mauch et al. 2003; Y. A. Gordon et al. 2021; T. Kawamuro et al. 2023; C. Ricci et al. 2023; K. Ross et al. 2024), infrared (D. B. Sanders et al. 2003; M. Meléndez et al. 2014; T. T. Shimizu et al. 2016; F. Marocco et al. 2021), optical-UV (M. F. Skrutskie et al. 2006; M. Koss et al. 2011), and X-ray data (C. N. Cardamone et al. 2007; C. Ricci et al. 2017; K. Oh et al. 2018; M. Baloković et al. 2020) are collected from the archive.