adsabs/AstroCLIMB huggingface dataset:
Paper: Follow-up Exploration of the TWA 7 Planet–Disk System with JWST NIRCam
Authors: Katie A. Crotts, Aarynn L. Carter, Kellen Lawson, James Mang, Beth Biller, Mark Booth, Rodrigo Ferrer-Chavez, Julien H. Girard, Anne-Marie Lagrange, Michael C. Liu, Sebastian Marino, Maxwell A. Millar-Blanchaer, Andy Skemer, Giovanni M. Strampelli, Jason Wang, Olivier Absil, William O. Balmer, Raphaël Bendahan-West, Ellis Bogat, Rachel Bowens-Rubin, Gaël Chauvin, Clémence Fontanive, Kyle Franson, Jens Kammerer, Jarron Leisenring, Caroline V. Morley, Isabel Rebollido, Nour Skaf, Ben J. Sutlieff, Evelyn L. Bruinsma, Sasha Hinkley, Kielan Hoch, Andrew D. James, Rohan Kane, Dimitri Mawet, Michael R. Meyer, Skyler Palatnick, Marshall D. Perrin, Shrishmoy Ray, Emily Rickman, Aniket Sanghi, Klaus Subbotina Stephenson
Figure caption: Color–color diagram showing the C6 companion (red) alongside a sample of brown dwarfs from S. A. Beiler et al. (2024a, gray). The F200W band for C6 represents a 3σ upper limit. Atmospheric model tracks from Figure 13 are overlaid, highlighting the distinct properties of C6 compared to the brown dwarf population.
Paper: An Ejection Event Captured by Very Long Baseline Interferometry during the Outburst of Swift J1727.8–1613
Authors: Hongmin Cao, Jun Yang, Sándor Frey, Callan M. Wood, James C. A. Miller-Jones, Krisztina É. Gabányi, Giulia Migliori, Marcello Giroletti, Lang Cui, Tao An, Xiaoyu Hong, WeiHua Wang
Figure caption: The X-ray photon flux, radio flux density, and X-ray hardness variations over time. The beginning and the end of the EVN observing period are shown by the two vertical red dashed lines. The X-ray data are taken from the MAXI archive (M. Matsuoka et al. 2009). The radio flux densities at 338 MHz, 4.7 GHz, and 5.3 GHz are taken from W. M. Peters et al. (2023), S. A. Trushkin et al. (2023), and J. C. A. Miller-Jones et al. (2023a), respectively.
Paper: A Nanosecond-duration Radio Pulse Originating from the Defunct Relay 2 Satellite
Authors: C. W. James, A. T. Deller, T. Dial, M. Glowacki, S. J. Tingay, K. W. Bannister, A. Bera, N. D. R. Bhat, R. D. Ekers, V. Gupta, A. Jaini, J. Morgan, J. N. Jahns-Schindler, R. M. Shannon, M. Sukhov, J. Tuthill, Z. Wang
Figure caption: The dedispersed burst. Total burst power at Nyquist resolution (points—lines to guide the eye only) after dedispersion and coherent addition over 19 antennas according to the near-field fit. Note that our ability to determine the signal flux density—and potentially also shape—is limited by our 1 bit sampling precision (see text).
Paper: A Nanosecond-duration Radio Pulse Originating from the Defunct Relay 2 Satellite
Authors: C. W. James, A. T. Deller, T. Dial, M. Glowacki, S. J. Tingay, K. W. Bannister, A. Bera, N. D. R. Bhat, R. D. Ekers, V. Gupta, A. Jaini, J. Morgan, J. N. Jahns-Schindler, R. M. Shannon, M. Sukhov, J. Tuthill, Z. Wang
Figure caption: Polarization properties of the burst. Upper panel: rotation measure (RM) fit to the position angle (PA) of the linear polarization (black filled circles) as a function of frequency, with channels not used in the fit shown in gray. Lower panel: the fractional linear (L) and circular (V) polarizations as a function of frequency. Calculations were performed at 10.5 MHz, 95.24 ns resolution.
Paper: A Nanosecond-duration Radio Pulse Originating from the Defunct Relay 2 Satellite
Authors: C. W. James, A. T. Deller, T. Dial, M. Glowacki, S. J. Tingay, K. W. Bannister, A. Bera, N. D. R. Bhat, R. D. Ekers, V. Gupta, A. Jaini, J. Morgan, J. N. Jahns-Schindler, R. M. Shannon, M. Sukhov, J. Tuthill, Z. Wang
Figure caption: The best-fitting near-field distance. Shown is the rms of the timing residuals over all 19 antennas used in the fit. The minimum at 4500 km corresponds to the best-fit distance for the burst.
Paper: A Nanosecond-duration Radio Pulse Originating from the Defunct Relay 2 Satellite
Authors: C. W. James, A. T. Deller, T. Dial, M. Glowacki, S. J. Tingay, K. W. Bannister, A. Bera, N. D. R. Bhat, R. D. Ekers, V. Gupta, A. Jaini, J. Morgan, J. N. Jahns-Schindler, R. M. Shannon, M. Sukhov, J. Tuthill, Z. Wang
Figure caption: The match of the observed burst position and the Relay 2 position. The orange filled square is the observed burst position. The blue filled circles are the positions of Relay 2, with green and red filled circles indicating the first and last time points, respectively, separated by 1 s and centered on the observed burst time.
Paper: An Ejection Event Captured by Very Long Baseline Interferometry during the Outburst of Swift J1727.8–1613
Authors: Hongmin Cao, Jun Yang, Sándor Frey, Callan M. Wood, James C. A. Miller-Jones, Krisztina É. Gabányi, Giulia Migliori, Marcello Giroletti, Lang Cui, Tao An, Xiaoyu Hong, WeiHua Wang
Figure caption: The MODELFIT images of Swift J1727.8–1613 and the fitted angular size vs. observing time. The two images were made using intra-European baselines only. The first contours are at ±5σ (left panel) and ±3σ (middle panel) image rms noise levels, respectively, and the positive contours increase by a factor of 2. The peak brightness and image rms noise level values are 138.8 and 2.6 mJy beam−1 for the left panel, and 65.4 and 1.8 mJy beam−1 for the middle panel, respectively. In the right panel, the red symbols represent the fitted sizes measured using only the European baselines, and the blue open circles are the ones measured when including Hh. The three vertical dashed lines are the same as in Figure 2.
Paper: An Ejection Event Captured by Very Long Baseline Interferometry during the Outburst of Swift J1727.8–1613
Authors: Hongmin Cao, Jun Yang, Sándor Frey, Callan M. Wood, James C. A. Miller-Jones, Krisztina É. Gabányi, Giulia Migliori, Marcello Giroletti, Lang Cui, Tao An, Xiaoyu Hong, WeiHua Wang
Figure caption: Visibility amplitude vs. observing time. The three vertical dashed lines in the upper panel indicate the approximate peak positions of the visibility amplitudes of Swift J1727.8–1613 on the Hh baselines (red curve). For the convenience of display, the plot is made with the baselines to the most sensitive Ef antenna, and only one IF (IF 5 at 4.927 GHz) is shown, with the data points further averaged over every 15 visibilities. The amplitudes measured on the Jb–Ef baseline are highlighted with magenta, and data points on baselines between Ef and other European antennas are shown in gray. For comparison, the lower panel shows the nearly constant visibility amplitudes measured for the compact phase-reference calibrator quasar J1724–1443.
Paper: An Ejection Event Captured by Very Long Baseline Interferometry during the Outburst of Swift J1727.8–1613
Authors: Hongmin Cao, Jun Yang, Sándor Frey, Callan M. Wood, James C. A. Miller-Jones, Krisztina É. Gabányi, Giulia Migliori, Marcello Giroletti, Lang Cui, Tao An, Xiaoyu Hong, WeiHua Wang
Figure caption: The simulated evolution of the visibility amplitude over time. The amplitudes at three points in the visibility plane, i.e., (0, 5) Mλ, (0, 10) Mλ, and (0, 110) Mλ, are selected to represent two short baselines and one long baseline. The model consists of two components. The flux density of the stationary component and the FWHM diameter of the moving component are 40 mJy and 0.5 mas for the left panel, 40 mJy and 1.0 mas for the middle panel, and 15 mJy and 1.0 mas for the right panel, respectively (see the text for further details). The start time of the EVN observation is indicated by the vertical red dashed line. The three vertical gray dashed lines are the same as those in Figure 2.
Paper: An Ejection Event Captured by Very Long Baseline Interferometry during the Outburst of Swift J1727.8–1613
Authors: Hongmin Cao, Jun Yang, Sándor Frey, Callan M. Wood, James C. A. Miller-Jones, Krisztina É. Gabányi, Giulia Migliori, Marcello Giroletti, Lang Cui, Tao An, Xiaoyu Hong, WeiHua Wang
Figure caption: The rise and fall timescales of the visibility amplitude. In the upper panel, the open circles are visibility amplitudes from IF 5, with the data further averaged over every 15 and 30 visibilities for the Jb–Ef (magenta) and Mc–O8 (blue) baselines, respectively, to improve the signal-to-noise ratio. The magenta curve indicates the broken exponential function fitted to the Jb–Ef visibility amplitudes. The source flux densities of the 14 slices, obtained by the MODELFIT program in DIFMAP (only European baselines), are shown with gray filled circles. The lower panel displays the ratio of the observed visibility amplitudes (SO) to those calculated by the exponential model (Sm).
Paper: An Ejection Event Captured by Very Long Baseline Interferometry during the Outburst of Swift J1727.8–1613
Authors: Hongmin Cao, Jun Yang, Sándor Frey, Callan M. Wood, James C. A. Miller-Jones, Krisztina É. Gabányi, Giulia Migliori, Marcello Giroletti, Lang Cui, Tao An, Xiaoyu Hong, WeiHua Wang
Figure caption: The simulated evolution of the visibility amplitude over time. The amplitudes at three points in the visibility plane, i.e., (0, 5) Mλ, (0, 10) Mλ, and (0, 110) Mλ, are selected to represent two short baselines and one long baseline. The model consists of two components. The flux density of the receding component and the FWHM diameters of the receding and approaching components are 10 mJy, 0.5 mas, and 0.5 mas for the left panel; 10 mJy, 0.75 mas, and 1.0 mas for the middle panel; and 20 mJy, 0.75 mas, and 1.0 mas for the right panel, respectively (see the text for further details). The start time of the EVN observation is indicated by the vertical red dashed line. The three vertical gray dashed lines are the same as those in Figure 2.
Paper: An Ejection Event Captured by Very Long Baseline Interferometry during the Outburst of Swift J1727.8–1613
Authors: Hongmin Cao, Jun Yang, Sándor Frey, Callan M. Wood, James C. A. Miller-Jones, Krisztina É. Gabányi, Giulia Migliori, Marcello Giroletti, Lang Cui, Tao An, Xiaoyu Hong, WeiHua Wang
Figure caption: The (u, v) coverage of the EVN experiment observing Swift J1727.8–1613. The intra-European baselines are clustered at the center, while the longer baselines between the European antennas and Hh are roughly aligned along the north–south direction. The (u, v) points belonging to the Jb–Ef, Mc–O8, and Ef–Hh baselines are highlighted by magenta, blue, and red colors, respectively.
Paper: Recurrent Cometary Activity Discovered on Quasi-Hilda Jupiter Family Comet 362P/(457175) 2008 GO98
Authors: Kennedy A. Farrell, Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jarod A. DeSpain, Mark Jesus Mendoza Magbanua, Maxwell K. Frissell, Phineas Stone
Figure caption: Images of 362P (at center) displaying cometary activity between the antivelocity (red arrow) and antisolar (yellow arrow) directions. The field of view is 126″ × 126″, with north up and east left. (a) UT 2024 January 12, Lowell Discovery Telescope (LDT), 5 × 300 s, VR-filter image taken with the Large Monolithic Imager (PI: C. Trujillo; observers: W. Oldroyd, K. Farrell). (b) UT 2024 January 13, ARC Telescope Imaging Camera (ARCTIC), 2 × 300 s, VR-filter images (Prop. ID 2024B-UW05; PI: C. Chandler; observers: C. Chandler, W. Oldroyd). (c) UT 2024 January 16, VATT 300 s, V-filter image (PI: C. Trujillo; observers: C. Chandler, M. Magbanua). (d) UT 2024 February 15, 6 × 300 s, VR-band images with ARCTIC (PI: C. Chandler; observers: W. Oldroyd, C. Chandler). (e) UT 2024 April 11, 2 × 300 s, r-band ARCTIC images (PI: C. Chandler; observer: W. Oldroyd). (f) UT 2024 May 9, 2 × 300 s, VR-band ARCTIC images (PI: C. Chandler; observers: W. Oldroyd, C. Chandler). (g) UT 2024 August 9, 2 × 300 s, VR-band ARCTIC images (PI: C. Chandler; observers: C. Chandler, M. Frissell, P. Stone). (h) UT 2024 September 4, 1 × 300 s, g-band ARCTIC image (PI: C. Chandler; observers: M. Frissell, C. Chandler).
Paper: Recurrent Cometary Activity Discovered on Quasi-Hilda Jupiter Family Comet 362P/(457175) 2008 GO98
Authors: Kennedy A. Farrell, Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jarod A. DeSpain, Mark Jesus Mendoza Magbanua, Maxwell K. Frissell, Phineas Stone
Figure caption: Observability and thermodynamical modeling of 362P from 2012 to 2033. Descending subpanels show heliocentric distance (r) in au with markers indicating positive activity detections (red) and negative activity detections (blue), both inbound and outbound (downward- and upward-pointing triangles, respectively); apparent V-band magnitude; observability in hours per day; and temperature (T) in Kelvin of 362P for the thermophysical extremes of χ = 1 (flat, Sun-facing slab) and χ = 4 (isothermal approximation). Activity markers include this work and the observations obtained by E. García-Migani & R. Gil-Hutton (2018) between 2016 September and 2017 July. Our observability metric for Cerro Tololo Inter-American Observatory, site code 807 (blue solid line), and the Lowell Discovery Telescope (LDT), site code G37 (orange dashed line), depicts the number of hours 362P was observable (>15° above the horizon between sunset and sunrise) during a given Universal time observing date. The location of 362P as of UT 2024 November 23 is noted as a vertical red dashed line. Heliocentric distance, apparent magnitude, and elevation information for each observatory site were retrieved from JPL on UT 2024 November 23.
Paper: Recurrent Cometary Activity Discovered on Quasi-Hilda Jupiter Family Comet 362P/(457175) 2008 GO98
Authors: Kennedy A. Farrell, Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jarod A. DeSpain, Mark Jesus Mendoza Magbanua, Maxwell K. Frissell, Phineas Stone
Figure caption: (a) and (b) Orbits (blue) of (153) Hilda and 362P, respectively, in the corotating reference frame with Jupiter (orange). The axis “X corotating frame” indicates the x-axis of the corotating frame, and “Y corotating frame” indicates the y-axis of the corotating frame. The aphelion distance of Mars (red) is shown for reference. (c) Orbit diagram; note the proximity of the orbits of 362P and Jupiter. (d) Semimajor axis evolution of 362P orbital clones over ±600 yr; the semimajor axis of Jupiter (orange) is shown for reference. (e) Heliocentric distance evolution of 362P clones with orbital distances of Jupiter (orange) and Mars (red) for reference. (f) Logarithmic distance between 362P and Jupiter. Horizontal lines representing the depth of close encounters (with fewer Hill radii corresponding to larger gravitational influence) and the orbital distance of two Jovian moons are given for reference.
Paper: Recurrent Cometary Activity Discovered on Quasi-Hilda Jupiter Family Comet 362P/(457175) 2008 GO98
Authors: Kennedy A. Farrell, Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jarod A. DeSpain, Mark Jesus Mendoza Magbanua, Maxwell K. Frissell, Phineas Stone
Figure caption: For all images, 362P is at the center of these 126″ × 126″ fields, with north up and east left. Antisolar (yellow arrow) and antimotion (red-outlined black arrow) on-sky directions are indicated. (a) UT 2016 March 7, coadded 2 × 150 s, VR-band DECam images (Prop. ID 2016A-0189; PI: Rest; observers: Armin Rest, David James). (b) UT 2016 April 9, 1 × 118 s, r-band DECam exposure (Prop. ID 2014B-0404; PI: Schlegel; observers: Arjun Dey, David James). (c) UT 2016 July 21, 1 × 211 s, z-band DECam image (Prop. ID 2016A-0190; PI: Dey; observers: Dustin Lang, Alistair Walker). (d) UT 2017 July 5, Las Cumbres Observatory Global Telescope (LCOGT), 3 × 180 s, R-band archival image taken on the 2 m Faulkes Telescope North (LCOGT site code “ogg”), Hawaii (Prop. ID FTPEPO2014A-004; user: Americo Watkins. (e) UT 2017 August 28, 7 × 120 s, r-band images acquired with the 2 m Siding Spring Observatory (Australia) LCOGT telescope, site “coj” (Prop. ID FTPEPO2017AB-002; user ID: Richard Mile). (f) UT 2017 September 21, 1 × 100 s, g-band + 1 × 100 s, r-band 1.35 m SkyMapper telescope (Siding Spring). (g) UT 2017 October 10, 1 × 100 s, r-band SkyMapper image. (h) UT 2024 April 3, 1 × 30 s, g-band + 1 × 30 s, r-band ZTF images acquired with the 48” Samuel Oschin Schmidt telescope (Palomar). (i) UT 2024 April 30, 2 × 30 s, g-band + 2 × 30 s, z-band ZTF exposures. (j) UT 2024 May 14, 1 × 30 s, g-band + 1 × 30 s, r-band ZTF exposures.
Paper: Supermassive Black Holes Stripping a Subgiant Star Down to Its Helium Core: A New Type of Multimessenger Source for LISA
Authors: Aleksandra Olejak, Jakob Stegmann, Selma E. de Mink, Ruggero Valli, Re'em Sari, Stephen Justham, Taeho Ryu
Figure caption: Evolution of a subgiant undergoing mass transfer as a function of time in the mass (top panel) and radius (middle panel) coordinates. The internal structure of the subgiant is divided into regions: the hydrogen envelope (red) and the helium core (blue). The main convective regions are highlighted with shaded areas. The bottom panel compares timescales for GW emission, ﹩{t}_{{\rm{GW}}}=a/{\dot{a}}_{{\rm{GW}}}﹩ (gray), and mass transfer, ﹩{t}_{{\rm{MT}}}={M}_{{\rm{don}}}/\dot{M}﹩ (orange). For comparison, we also plot the donor’s thermal timescale (blue). Different types of black markers have been used to highlight and localize characteristic features of mass transfer in the three panels and in Figure 3. The final unstable mass transfer is marked by the red star.
Paper: Supermassive Black Holes Stripping a Subgiant Star Down to Its Helium Core: A New Type of Multimessenger Source for LISA
Authors: Aleksandra Olejak, Jakob Stegmann, Selma E. de Mink, Ruggero Valli, Re'em Sari, Stephen Justham, Taeho Ryu
Figure caption: The strain spectral density h of the GW signal from an initially 2 M⊙ subgiant transferring mass to a 4.3 × 106 M⊙ SMBH, along with the LISA sensitivity curve for a 4 yr mission (T. Robson et al. 2019). The colored line represents the signal if the system were located in the Milky Way, while the gray lines correspond to signals at greater distances. The numbers above the colored line indicate the time until the final unstable mass transfer phase (red star) with the possible pTDE on a circular orbit. The star undergoes its first mass transfer phase at lower frequencies and subsequently enters the LISA band once it has been stripped of nearly its entire hydrogen envelope. Different types of black markers and labels: MT0–MT4 have been used to localize and highlight characteristic features of mass transfer, consistently marked in Figure 2. At the final time step, the signal reaches an SNR of ∼106 in the Galactic center, making it potentially detectable even from a distance of 1 Gpc.
Paper: Supermassive Black Holes Stripping a Subgiant Star Down to Its Helium Core: A New Type of Multimessenger Source for LISA
Authors: Aleksandra Olejak, Jakob Stegmann, Selma E. de Mink, Ruggero Valli, Re'em Sari, Stephen Justham, Taeho Ryu
Figure caption: Cartoon representation of four relevant evolutionary stages of the system. Top left panel: the initial binary star system enters the Hill sphere of an SMBH and is disrupted. One star becomes gravitationally bound to the SMBH in an eccentric orbit, while the other is ejected from the Galactic nucleus, becoming a hypervelocity star. Top right panel: the orbit of the star bound to the SMBH gradually shrinks and circularizes owing to the strong emission of GWs. Bottom left panel: as the orbit continues to tighten, a subgiant star fills its Roche lobe, initiating a phase of long, stable mass transfer onto the SMBH. Bottom right panel: the star is eventually stripped of its hydrogen envelope during the mass transfer process. The system continues to shrink owing to GW emission, eventually entering the LISA frequency band as a detectable GW source.
Paper: Supermassive Black Holes Stripping a Subgiant Star Down to Its Helium Core: A New Type of Multimessenger Source for LISA
Authors: Aleksandra Olejak, Jakob Stegmann, Selma E. de Mink, Ruggero Valli, Re'em Sari, Stephen Justham, Taeho Ryu
Figure caption: Evolution of the system on Hertzsprung–Russell (H-R) diagram. Different types of black markers and labels: MT0–MT4 have been used to localize and highlight characteristic features of mass transfer, consistently marked in Figures 2 and 3.
Paper: Intense Hard X-Ray Emissions in C-class Flares: A Statistical Study with ASO-S/HXI Data
Authors: Changxue Chen, Yang Su, Wei Chen, Jingwei Li, Fu Yu, Weiqun Gan
Figure caption: HXI flare identification process and data processing. (a) HXI raw spectrogram in 80 energy bands. It should be noted that many of the enhanced emissions are not originating from flares, but from particles in Earth’s radiation belts. (b) The background-subtracted spectrogram. For computational simplification, the data were binned into nine energy bins, with only pixels above the threshold presented. (c) Flare spectrogram, with pixels derived from those in panel (b) that satisfy both connectivity and flux thresholds, corresponding to genuine flare-induced emission enhancements. During the displayed time period, two flares were identified (annotated with red dashed boxes), with the details of one shown in the magnified inset. (d)–(i) The processing flow of SOL2023-03-19T02:15. (d) SXR light curve, with the blue shaded area representing the time range of the panel (g) image and the red dashed line representing the SXR background level we have selected. (e) Observation of the flare in the AIA 131 Å, with superimposed contour in red (80% of peak intensity), purple (50%), and black (20%) representing HXR 20–40 keV emission. (f), (i) The spectrum fitting results (including residuals) near the peak time for 10 s, where different fitting components are represented by different colored lines and displayed in the legend, and the gray lines represent the background level. (g) HXR light curves, with dashed lines of the same color representing the background level of each energy channel. The vertical solid and dashed lines represent the start and end times of flare identification, while the red shaded areas represent the time periods corresponding to the imaging in panels (e) and (h). (h) Similar to panel (e), but the background image shows observations in AIA 1600 Å, where the centroid corresponding to the flare ribbons is marked with a black plus sign.
Paper: Deciphering the Formation and Dynamics of Double-decker Filaments through Component Magnetic Reconnection
Authors: Dongxu Liu, Yuandeng Shen, Yi Bi, Zehao Tang, Chengrui Zhou, Surui Yao
Figure caption: The observations of small jets S7–S10 during the filament splitting process. Panel (a) displays an AIA 171 Å image to show the field of view of the small jets. Panels (b) and (e) highlight the locations of small jets S7 and S8, as captured in AIA 171 and 304 Å images. The velocity fields of S7 and S8 are shown in panels (c) and (f), where the blue arrows represent the flow magnitudes and directions derived using the FLCT method. Panels (d) and (g) depict the brightened flows along the filament threads, which are associated with these small jets. Panel (h) displays the brightening of different clusters of magnetic field lines, indicated by dashed lines, which form a small angle, as observed at 00:39 UT. The component reconnection of these clusters led to S9 at 00:40 UT (see panels (i) and (j)). The blue dashed lines in panel (i) illustrate the spinning motion of the brightened flow. Panel (k) shows S10 observed at 00:44 UT. Panel (l) presents the time–distance diagram along the dashed lines in panels (i)–(k), which represent the trajectory of the small jets. The velocities of both small jets are shown in panel (l). Additionally, the blue dashed lines in panel (l) highlight the rotational motion of the brightened flow. Panels (m) and (n) display the weighted temperature and weighted emission measures of the region, with the scales shown below the figures. The black boxes in panels (m) and (n) indicate the presence of S9 observed at 00:40 UT.