adsabs/AstroCLIMB huggingface dataset:
Paper: Influence of Orbit and Mass Constraints on Reflected Light Characterization of Directly Imaged Rocky Exoplanets
Authors: Arnaud Salvador, Tyler D. Robinson, Jonathan J. Fortney, Mark S. Marley
Figure caption: Orbital distance and planet radius joint/bivariate (center) and marginal/univariate (top and right side) posterior distributions for different scenarios of prior knowledge and for the vNIR and S/N = 20. The contours of the 2D posterior distributions denote the 1σ, 2σ, and 3σ levels, encompassing 68%, 95%, and 99.7% of the observed values, respectively (note that the relevant 1σ, 2σ, and 3σ levels for a 2D distribution of samples are 39.3%, 86.5%, and 98.9% of the volume, and correspond to the 68%, 95%, and 99.7% for 1D distributions). Earth-like input values are depicted with dashed horizontal and vertical lines. The small image of Earth indicates its position in the diagram. The sketch illustrates the degenerate relationship between increasing orbital distance and increasing planet radius, in yielding an equivalent amount of reflected light. A larger planet orbiting further away from its host star may essentially reflect the same amount of light as a smaller planet but closer to the star. As a result, if the orbit-related parameters are known or constrained, the range of planet radius yielding the same amount of reflected light is necessarily restricted. Retrieval results are given in Table 2.
Paper: Influence of Orbit and Mass Constraints on Reflected Light Characterization of Directly Imaged Rocky Exoplanets
Authors: Arnaud Salvador, Tyler D. Robinson, Jonathan J. Fortney, Mark S. Marley
Figure caption: Corner plot illustrating the marginal univariate (along the diagonal) and bivariate (off-diagonal) posterior distributions for all retrieved parameters, considering various scenarios of color-coded prior knowledge for observations conducted in the vNIR at S/N = 20 (see Table 2 for quantitative estimates). The contours of the 2D posterior distributions denote the 1σ, 2σ, and 3σ levels, encompassing 68%, 95%, and 99.7% of the observed values, respectively. Earth-like input values are depicted with dashed horizontal and vertical lines.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: The NRS1 (top) and NRS2 (bottom) light curves and best-fitting map models, compared against Spitzer phase curves from Stevenson et al. (2017). The Spitzer data have been binned temporally by a factor of 20 for clarity. We only show the second 3.6 μm Spitzer visit, as the first is afflicted by intrapixel sensitivity variations that cannot be accurately corrected (Stevenson et al. 2017). Our data show a brighter (hotter) nightside in both bands and a dimmer (colder) dayside at the shorter wavelengths, smaller phase-curve offsets, and less asymmetry in the NRS2 phase curve than the Spitzer 4.5 μm phase curve, which exhibits a phase-curve maximum before the eclipse and minimum after the transit. We also show the Exo-FMS GCM light curves overplotted.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: Top: brightness-temperature maps from fits to the NRS1 and NRS2 light curves. See the description of the inset in Figure 3. Bottom: 100 samples of slices along the equator and substellar meridian from the posterior distributions of temperature maps from the fits to the NRS1 and NRS2 light curves.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: Allan variance plots of the NRS1 (top) and NRS2 (bottom) light-curve residuals. The black line shows the standard deviation of the model residuals with uncertainties and the red line shows the expected ﹩1/\sqrt{N}﹩ trend. If correlated noise is present at a given timescale, the black line would be above the red line. For both detectors, the black line follows the red line, showing no significant residual correlated noise. The vertical dashed lines mark a region between the ingress/egress time and a tenth of the ingress/egress time, approximating the range of timescales where correlated noise could interfere with our mapping signal.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: The effect of varying system parameters by ±1σ on the latitudinal hotspot offset. The vertical dashed black line marks the equator. The retrieved latitudinal hotspot offset remains consistent and is nonequatorial.
Paper: FAST Discovery of Eight Isolated Millisecond Pulsars in NGC 6517
Authors: Dejiang Yin, Li-yun Zhang, Lei Qian, Ralph P. Eatough, Baoda Li, Duncan R. Lorimer, Yinfeng Dai, Yaowei Li, Xingnan Zhang, Minghui Li, Tianhao Su, Yuxiao Wu, Yu Pan, Yujie Lian, Tong Liu, Zhen Yan, Zhichen Pan
Figure caption: The average pulse profiles and timing residuals of all pulsars in NGC 6517. The left panel of each subplot is the integrated pulse profile obtained by summing all detections over 64 pulse phase bins. The timing residuals from the best-fit timing model are shown in the right panel. The phase-connected timing solutions of NGC 6517A to O were obtained, while for NGC 6517P, Q, and R, solutions with only the spin frequencies (f) were fitted, with commonly used arbitrary phase offsets (so-called “JUMPs”) between observations.
Paper: C/O Ratios and the Formation of Wide-separation Exoplanets
Authors: Edwin A. Bergin, Richard A. Booth, Maria Jose Colmenares, John D. Ilee
Figure caption: Radial distributions of derived C/O ratios in named disk systems from C2H (Bergin et al. 2016; Kama et al. 2016; Cleeves et al. 2018; Bosman et al. 2022; Sturm et al. 2023) and CS/SO (Rivière-Marichalar et al. 2022). Also shown is the range of C/O ratios estimated by Miotello et al. (2019) in a survey of C2H in Lupus disks. This survey had some lower limits that imply smaller disks or lower C/O ratios. In the figure A stars are shown in red and later spectral types in blue. The filled gray squares denote the estimated elemental C/O ratios toward direct detection planets β Pic b (GRAVITY Collaboration et al. 2020), HR 8799bcde (Nasedkin et al. 2024), and HIP 65426 b (Petrus et al. 2021). The estimated error bars for some of the planet C/O ratios are smaller than the marker size. The open diamonds superposed on a given C/O ratio line are the estimated location of the CO snowline for that object, with references given in Appendix C. For AB Aur the CO snowline is located at r > 200 au, and for IM Lup the CO snowline is near ∼15 au.
Paper: X-Ray View of Little Red Dots: Do They Host Supermassive Black Holes?
Authors: Tonima Tasnim Ananna, অনন্যা তনিমা তাসনিম, Ákos Bogdán, Orsolya E. Kovács, Priyamvada Natarajan, Ryan C. Hickox
Figure caption: The relationship between the SMBH mass and the stellar masses of galaxies. The yellow data points represent the upper limits obtained for the individual LRDs. The thick dark green data point corresponds to the upper limit measured for the stacked sample of 21 LRDs assuming Eddington-limited accretion. The uncertainty in stellar mass corresponds to the standard deviation. For reference, we also show the SMBH mass upper limits for the full stacked sample assuming accretion at 10% and 1% of the Eddington limit (green thin dashed). The tentative 2.6σ detection for the sample of nine LRDs with broad Hα line is shown with the solid dark green data point. The arrow pointing left from this data point indicates that the stellar masses used for this plot from Labbe et al. (2023) assume galaxy-only fits to calculate the masses. However, galaxy+AGN fits lead to lower AGN masses (e.g., Barro et al. 2024) by up to 2 orders of magnitude; therefore, this point might shift leftwards, as illustrated by the green dashed arrow. We overplot the scaling relations observed for local early-type galaxies using the relation observed by Kormendy & Ho (2013) that was scaled following Reines & Volonteri (2015), the best-fit relation for local AGN (Reines & Volonteri 2015), and for AGN up to z < 2.5 (Suh et al. 2020). The black data point (square) shows the median SMBH mass inferred from the broad line Hα emission line measured by JWST (Greene et al. 2024). We also plot the z = 10.07 galaxy, UHZ 1, which hosts an overmassive SMBH (Bogdán et al. 2024).
Paper: C/O Ratios and the Formation of Wide-separation Exoplanets
Authors: Edwin A. Bergin, Richard A. Booth, Maria Jose Colmenares, John D. Ilee
Figure caption: Left: estimated C/O of the dust, as in Figure 2, but considering a depletion (solid lines) or enhancement (dotted lines) of icy material before chemical evolution alters the disk composition. The black line represents the solar ratio. Right: constraints on the level of carbon depletion and dust depletion provided by the planets in the HR 8799 system, assuming that the gas has a C/O ratio of 2. The filled regions in the contours show the regions where the disks can produce planets that match the observed composition to within 1σ, under the assumption that silicates condense into clouds and do not contribute to the observed composition. Note that a dust depletion smaller than 1 means that the dust-to-gas ratio has been increased. The other planets in Table 1 provide similar but weaker constraints.
Paper: C/O Ratios and the Formation of Wide-separation Exoplanets
Authors: Edwin A. Bergin, Richard A. Booth, Maria Jose Colmenares, John D. Ilee
Figure caption: A comparison between the observed composition of planets (crosses) and the compositions obtained by combining different amounts of solids and gases (lines). The solid lines show the potential planet compositions for a given disk C/O ratio; in different panels, we have varied the amount of carbon depletion as in Figure 2. The solid lines assume that all material contributes to the planet’s composition, while the dashed lines assume that silicates condense out. For HIP 65426 b, the C/O ratio shown is the upper limit (Petrus et al. 2021).
Paper: C/O Ratios and the Formation of Wide-separation Exoplanets
Authors: Edwin A. Bergin, Richard A. Booth, Maria Jose Colmenares, John D. Ilee
Figure caption: Estimated C/O ratio within the grain icy mantle and solid core as a function of the gas-phase C/O ratio and the overall carbon depletion factor. Here we assume a solar composition for the stellar content. The dashed line represents the solar/stellar C/O ratio.
Paper: C/O Ratios and the Formation of Wide-separation Exoplanets
Authors: Edwin A. Bergin, Richard A. Booth, Maria Jose Colmenares, John D. Ilee
Figure caption: Origin of the line emission in the HD 163296 disk as determined in Guzmán et al. (2021) and Ilee et al. (2021). Also shown are the approximate C/O ratios derived from the analysis of Bosman et al. (2021a, from C2H) and also Calahan et al. (2023, from CH3CN and HC3N).
Paper: C/O Ratios and the Formation of Wide-separation Exoplanets
Authors: Edwin A. Bergin, Richard A. Booth, Maria Jose Colmenares, John D. Ilee
Figure caption: Estimated mass of accreted solids from a simple model as a function of the carbon depletion factor (ΔC) and the dust depletion factor. The dust depletion factor was chosen to be the best-fit value based on the C/H of the planets, and it corresponds to ∼0.5–5, depending on the assumed C/O ratio. When the dust depletion factor is less than 1, it reflects a local dust enhancement.
Paper: X-Ray View of Little Red Dots: Do They Host Supermassive Black Holes?
Authors: Tonima Tasnim Ananna, অনন্যা তনিমা তাসনিম, Ákos Bogdán, Orsolya E. Kovács, Priyamvada Natarajan, Ryan C. Hickox
Figure caption: The distribution of 90% energy encircling radius (R 90) for the 21 AGN candidates presented in Labbe et al. (2023) in the Chandra observations of A2744. This radius varies as a function of distance from the Chandra ACIS-I pointing center. The median R 90 for all source-observation pairs for these sources is 1.″9 (shown with the black dashed line).
Paper: A New Lever on Exoplanetary B Fields: Measuring Heavy Ion Velocities
Authors: Arjun B. Savel, Hayley Beltz, Thaddeus D. Komacek, Shang-Min Tsai, Eliza M.-R. Kempton
Figure caption: Calculated properties of the model atmosphere described in Table 2. Left: the limb temperature–pressure structure calculated with HELIOS (Malik et al. 2017, 2019). Regions where the atmosphere is convective are highlighted in orange. Pressures generally probed in high-resolution transmission spectroscopy (e.g., Kempton et al. 2014; Gandhi et al. 2020; Hood et al. 2020; Wardenier et al. 2023) are filled in green. Middle: free electron volume mixing ratio calculated by FastChem equilibrium (in black; Kitzmann et al. 2024) and VULCAN disequilibrium (shaded blue; Tsai et al. 2021) chemistry. We run VULCAN over a wide range of parameters—hence, there is a width to this region. Right: ion–neutral velocity difference (Equation (11)), calculated under equilibrium and disequilibrium chemistry assuming two B field strengths. The gold line indicates the approximate minimum detectable velocity difference via high-resolution spectroscopy (e.g., Ehrenreich et al. 2020). The width of the disequilibrium chemistry grid is due almost entirely to the changing input stellar flux.
Paper: An IXPE-led X-Ray Spectropolarimetric Campaign on the Soft State of Cygnus X-1: X-Ray Polarimetric Evidence for Strong Gravitational Lensing
Authors: James F. Steiner, Edward Nathan, Kun Hu, Henric Krawczynski, Michal Dovčiak, Alexandra Veledina, Fabio Muleri, Jiri Svoboda, Kevin Alabarta, Maxime Parra, Yash Bhargava, Giorgio Matt, Juri Poutanen, Pierre-Olivier Petrucci, Allyn F. Tennant, M. Cristina Baglio, Luca Baldini, Samuel Barnier, Sudip Bhattacharyya, Stefano Bianchi, Maimouna Brigitte, Mauricio Cabezas, Floriane Cangemi, Fiamma Capitanio, Jacob Casey, Nicole Rodriguez Cavero, Simone Castellano, Elisabetta Cavazzuti, Sohee Chun, Eugene Churazov, Enrico Costa, Niccolò Di Lalla, Alessandro Di Marco, Elise Egron, Melissa Ewing, Sergio Fabiani, Javier A. García, David A. Green, Victoria Grinberg, Petr Hadrava, Adam Ingram, Philip Kaaret, Fabian Kislat, Takao Kitaguchi, Vadim Kravtsov, Brankica Kubátová, Fabio La Monaca, Luca Latronico, Vladislav Loktev, Christian Malacaria, Frédéric Marin, Andrea Marinucci, Olga Maryeva, Guglielmo Mastroserio, Tsunefumi Mizuno, Michela Negro, Nicola Omodei, Jakub Podgorný, John Rankin, Ajay Ratheesh, Lauren Rhodes, David M. Russell, Miroslav Šlechta, Paolo Soffitta, Sean Spooner, Valery Suleimanov, Francesco Tombesi, Sergei A. Trushkin, Martin C. Weisskopf, Silvia Zane, Andrzej A. Zdziarski, Sixuan Zhang, Wenda Zhang, Menglei Zhou, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Jeffery J. Kolodziejczak, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Ikuyuki Mitsuishi, Chi-Yung Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: IXPE PD for the composite of hard vs. soft states, where the energy bins have been scaled with respect to the disk temperature kT *. The consistent behavior in evidence is suggestive of commonality between the hard and soft states, despite radically different spectral-timing characteristics.
Paper: A New Lever on Exoplanetary B Fields: Measuring Heavy Ion Velocities
Authors: Arjun B. Savel, Hayley Beltz, Thaddeus D. Komacek, Shang-Min Tsai, Eliza M.-R. Kempton
Figure caption: An R = 145,000 CHIMERA optical transmission spectrum of an ultrahot Jupiter under chemical equilibrium. A spectrum with Ba II as the only spectrally active trace species is overplotted (gold), indicating the location and strength of Ba II absorption lines in our model atmosphere. Ba II lines in this model probe pressures near a microbar. We generate an analogous spectrum for neutral iron, as well (black).
Paper: A New Lever on Exoplanetary B Fields: Measuring Heavy Ion Velocities
Authors: Arjun B. Savel, Hayley Beltz, Thaddeus D. Komacek, Shang-Min Tsai, Eliza M.-R. Kempton
Figure caption: The stellar UV spectra input to VULCAN.
Paper: A New Lever on Exoplanetary B Fields: Measuring Heavy Ion Velocities
Authors: Arjun B. Savel, Hayley Beltz, Thaddeus D. Komacek, Shang-Min Tsai, Eliza M.-R. Kempton
Figure caption: The primary electron donors in our chemical calculations. The thick solid lines represent equilibrium chemistry. Thin solid lines represent VULCAN disequilibrium chemistry with the F5V stellar spectrum, and thin dotted lines represent disequilibrium chemistry with the HD 189733 stellar spectrum.
Paper: Discovery of the Optical and Radio Counterpart to the Fast X-Ray Transient EP 240315a
Authors: J. H. Gillanders, L. Rhodes, S. Srivastav, F. Carotenuto, J. Bright, M. E. Huber, H. F. Stevance, S. J. Smartt, K. C. Chambers, T.-W. Chen, R. Fender, A. Andersson, A. J. Cooper, P. G. Jonker, F. J. Cowie, T. de Boer, N. Erasmus, M. D. Fulton, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, H.-Y. Miao, P. Minguez, T. Moore, C.-C. Ngeow, M. Nicholl, Y.-C. Pan, G. Pignata, A. Rest, X. Sheng, I. A. Smith, K. W. Smith, J. L. Tonry, R. J. Wainscoat, J. Weston, S. Yang, D. R. Young
Figure caption: Left panel: radio luminosity of different classes of extragalactic transients adapted from Ho et al. (2020), including data from Laskar et al. (2023) and Rhodes et al. (2023). The yellow star indicates the radio luminosity derived from our MeerKAT detection of EP 240315a. The luminosity is consistent with both GRBs and jetted TDEs. Right panel: AT 2024eju optical (rest-frame UV) detections and Gemini upper limits compared to a sample of rest-frame, UV-detected, long GRB afterglows at redshifts of z > 2 (Kann et al. 2010); the UV counterpart of the jetted TDE AT 2022cmc (Yao et al. 2024); and upper limits from the candidate jetted TDE Swift J2058.4 + 0516 (Cenko et al. 2012; Andreoni et al. 2022).
Paper: Discovery of the Optical and Radio Counterpart to the Fast X-Ray Transient EP 240315a
Authors: J. H. Gillanders, L. Rhodes, S. Srivastav, F. Carotenuto, J. Bright, M. E. Huber, H. F. Stevance, S. J. Smartt, K. C. Chambers, T.-W. Chen, R. Fender, A. Andersson, A. J. Cooper, P. G. Jonker, F. J. Cowie, T. de Boer, N. Erasmus, M. D. Fulton, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, H.-Y. Miao, P. Minguez, T. Moore, C.-C. Ngeow, M. Nicholl, Y.-C. Pan, G. Pignata, A. Rest, X. Sheng, I. A. Smith, K. W. Smith, J. L. Tonry, R. J. Wainscoat, J. Weston, S. Yang, D. R. Young
Figure caption: The location of the counterparts to EP 240315a, marked with cross-hairs (red for the optical location from ATLAS, orange for the radio location from MeerKAT). Top panels: ATLAS stacked (4 × 30 s) target images of the field of AT 2024eju. Left to right: o-band observation taken at T 0 − 1.696 days, detection c-band observation taken at T 0 + 0.054 days, and the subsequent o-band observation taken at T 0 + 1.304 days. AT 2024eju faded below the detection threshold of ATLAS in ≲1.2 days (m  o  > 21.1 AB mag; 2σ upper limit). Middle panels: same as the top panels, but here we present the difference images. In the center panel, the presence of AT 2024eju is unmistakable. Bottom left panel: Pan-STARRS z-band image of the field of AT 2024eju, with the localization regions from the detections of EP 240315a by the EP-WXT (blue; from Zhang et al. 2024c) and EP-FXT (green; from Chen et al. 2024b) overlaid, to illustrate the spatial coincidence with the optical counterpart AT 2024eju. Bottom right panel: MeerKAT radio image of the field of EP 240315a. There is clear evidence for a bright radio source in the image, coincident with EP 240315a. The beam size for the observations is 3.″5 × 3.″5, illustrated by the stamp in the lower left corner. Note the much smaller scale in this image compared with the optical images.
Paper: Discovery of the Optical and Radio Counterpart to the Fast X-Ray Transient EP 240315a
Authors: J. H. Gillanders, L. Rhodes, S. Srivastav, F. Carotenuto, J. Bright, M. E. Huber, H. F. Stevance, S. J. Smartt, K. C. Chambers, T.-W. Chen, R. Fender, A. Andersson, A. J. Cooper, P. G. Jonker, F. J. Cowie, T. de Boer, N. Erasmus, M. D. Fulton, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, H.-Y. Miao, P. Minguez, T. Moore, C.-C. Ngeow, M. Nicholl, Y.-C. Pan, G. Pignata, A. Rest, X. Sheng, I. A. Smith, K. W. Smith, J. L. Tonry, R. J. Wainscoat, J. Weston, S. Yang, D. R. Young
Figure caption: Top panel: Gemini North/GMOS-N telluric-corrected spectrum of EP 240315a/AT 2024eju. The Pan-STARRS iz-band observations taken ≈0.1 days after the spectral observations are overlaid. The absorption lines from which we estimate the redshift of the system have been marked (vertical red lines). Prominent skylines (from Hanuschik 2003) have been marked with vertical gray lines. Bottom left panel: a zoom-in on the region of strong Lyα absorption (the width of the red band is representative of our redshift uncertainty). Bottom right panel: composite spectrum of AT 2024eju, constructed from the profiles of the four absorption features we used to measure the redshift to EP 240315a (N v λ λ1238.821, 1242.804 and Si IV λ λ1393.755, 1402.770). Note that this composite spectrum has been normalized and transformed to velocity space. The width of the red band is again representative of our estimated redshift uncertainty.
Paper: FAST Discovery of Eight Isolated Millisecond Pulsars in NGC 6517
Authors: Dejiang Yin, Li-yun Zhang, Lei Qian, Ralph P. Eatough, Baoda Li, Duncan R. Lorimer, Yinfeng Dai, Yaowei Li, Xingnan Zhang, Minghui Li, Tianhao Su, Yuxiao Wu, Yu Pan, Yujie Lian, Tong Liu, Zhen Yan, Zhichen Pan
Figure caption: The correlation between the number of pulsars and the central escape velocity of Galactic GCs. The lines with 95% credible interval in gray color shows the relation between the escape velocity and the number of estimated pulsars, while the stem plot shows the escape velocity of 39 GCs with known pulsars and the number of known pulsars in them. The blue dashed line and the black solid line present the model derived from all GCs and only GCs within FAST sky, respectively. GLIMPSE-C01 (with six known pulsars) was not included in the figure as its escape velocity was not available. In the sample, Pal 13 and M15 are the minimum and maximum escape velocities in the FAST sky, respectively. Liller 1 has the largest escape velocity in the Galactic GCs.