adsabs/AstroCLIMB huggingface dataset:
Paper: A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj
Authors: Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell, Curtis McCully
Figure caption: Multiband MOSFiT model light curves. The fit excludes the pre- and postpeak bumps (data points without a black outline). The model provides a good fit to the data during the rise, peak, and decline of the main peak, including following the postpeak bump.
Paper: A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj
Authors: Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell, Curtis McCully
Figure caption: The location of SN 2024rmj (crosshairs) in a preexplosion Legacy Survey Data Release 10 image (H. Flewelling 2018). The SN is located on the outskirts of its dwarf host galaxy (white circle), ≈2﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 ≈ 6.8 kpc from the host center.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Left: peak frequency vs. luminosity at peak frequency. Right: size vs. rest-frame peak frequency (legend shared). We compare the poststarburst targets to samples of AGN (copper colors; P. Patil et al. 2022; M. Kunert-Bajraszewska et al. 2025 and compilations by T. An & W. A. Baan (2012), S. Jeyakumar (2016), peak–linear size relations from C. P. O’Dea & S. A. Baum (1997) and M. Orienti & D. Dallacasa (2014)) and TDEs (cool colors; relativistic jetted TDEs from Swift J1644 (T. Eftekhari et al. 2018) and AT2022cmc (D. R. Pasham et al. 2023), optically selected events from Y. Cendes et al. (2024), A. J. Goodwin et al. (2022) (including AT2019azh), the delayed jetted event AT2018hyz (Y. Cendes et al. 2022), radio-identified TDEs from J. J. Somalwar et al.(2025a), and X-ray identified TDEs from A. J. Goodwin et al. (2025a)). For the poststarburst targets, we plot both the limits on the largest size from the VLA Ku-band beam sizes, as well as the inferred sizes from equipartition modeling. For comparison samples, sources with size corresponding to a direct measurement of the largest linear size are shown as × or +, while sources with equipartition-inferred sizes are shown as filled circles or lines. For inferred equipartition sizes for AT2018hyz and AT2019azh, models assuming a spherical outflow are shown as solid lines, while those assuming a collimated jet are shown as dotted lines. The poststarburst sources have lower luminosities and smaller sizes than most of the AGN samples, though the poststarburst source luminosities overlap with the transient sample from M. Kunert-Bajraszewska et al. (2025). The poststarburst sources have properties similar to the nonrelativistic TDE samples, particularly those of J. J. Somalwar et al. (2025a) and A. J. Goodwin et al. (2025a).
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Radio and IR light curves. (Top) Light curves of 3 GHz flux from VLASS (squares) and our targeted VLA observations (circles). The top two sources show clear increases since the first epoch of VLASS, while the bottom two are more constant or variable. (Middle) 1.4 GHz light curves from the FIRST upper limits and targeted VLA observations. All four sources have brightened significantly in the L band since the nondetections in FIRST. The four sources have risen by at least 25, 6.6, 2.5, 2.5× (in order listed in each table, respectively), relative to the FIRST 3σ upper limits on nondetections. (Bottom) WISE W1 (3.4 μm) and W2 (4.6 μm) light curves for each source. No significant flares or trends are seen for two of our targets (PSB0800 and SPOG1033). A clear flare is seen for PCA1009, with a strong decline seen over several years. An IR increase is also seen for PCA1424, though in this case, we see an initial increase and plateau, dissimilar to the light echoes seen after transient events.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Cumulative distribution of the stellar masses of (gray) the parent sample of 5000 poststarburst galaxies from the SDSS, (blue) the subset with VLASS detections, (orange) the subset with FIRST detections, (purple) the subset of 16 with VLASS detections and FIRST nondetections, which could potentially be variable sources, and (black) the subset of 4 definitively variable source we present here. The VLASS- and FIRST-detected poststarburst galaxies tend to have higher stellar masses than the parent sample (blue and orange vs. gray), consistent with an AGN source. We also compare to TDE host galaxies (green). The four variable sources we consider here have lower stellar masses, more consistent with the TDE host galaxies (black vs. green) than expectations from AGN.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Luminosity at peak frequency vs. redshift for the poststarburst sources and comparison samples, with plot points as in Figure 4. While there is a clear trend with luminosity and redshift, the poststarburst sources (black squares) are among the lower luminosity sources, even at comparable redshifts.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: BPT (J. A. Baldwin et al. 1981; L. J. Kewley et al. 2001; G. Kauffmann et al. 2003) and WHAN (R. Cid Fernandes et al. 2011) diagrams for our sources, using data from MPA-JHU galspec. Two sources (SPOG1033, PCA1424) are Seyferts, but the others are more LINER-like.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Best-fit equipartition model parameters for the four poststarburst targets, as well as the TDE samples from Y. Cendes et al. (2024), J. J. Somalwar et al. (2025b), and A. J. Goodwin et al. (2025a). The poststarburst sources have parameters broadly consistent with the scatter from all three TDE samples.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Observed SEDs from our targeted VLA observations with best-fit models as discussed in Section 4.1.
Paper: Radio Variability in Recently Quenched Galaxies: The Impact of Tidal Disruption Event or Active Galactic Nucleus-Driven Outflows
Authors: K. Decker French, Kristina Nyland, Pallavi Patil, Kishalay De, Dillon Dong, Nicholas Earl, Samaresh Mondal, Kate Rowlands, Margaret Shepherd, Margaret E. Verrico
Figure caption: Optical light curves for each source, as described in Section 4.2. All upper limits shown are at the 3σ level. No clear flares or variability are detected in the optical for any of these data sets. However, we note that it is possible that an optical transient was missed prior to the first observations we consider here or was dust-obscured.
Paper: A Novel Formation Channel for Supermassive Black Hole Binaries in the Early Universe via Primordial Black Holes
Authors: Saiyang Zhang, Boyuan Liu, Volker Bromm
Figure caption: Onset of gaseous cloud collapse. We show projections of gas density (left panel) and temperature (right panel) for the gas surrounding the central PBH taken from the PBH_LW_str_fd005 simulation, within a physical 200 pc scale. The snapshot is taken at z ≃ 17.4, corresponding to the moment where the first collapsing sink particle emerges. The simulation assumes a BH thermal feedback efficiency of ϵr = 0.5%, a relative streaming velocity of vbχ = 0.8σbχ, and includes the LW radiation generated during PBH accretion. The black dot marks the position of the PBH, while the blue star indicates the location of the collapsing gas cloud, representing the site for potential DCBH formation. Red arrows denote the relative motions between the central PBH and the bulk velocity of the collapsing gas cloud. Velocity vectors for gas are overlaid on both panels, with arrow sizes scaled by magnitude (different from that for BHs) to illustrate the inflow of gas toward the PBH, as well as feedback-driven outflows in its vicinity.
Paper: A Novel Formation Channel for Supermassive Black Hole Binaries in the Early Universe via Primordial Black Holes
Authors: Saiyang Zhang, Boyuan Liu, Volker Bromm
Figure caption: Gas properties in the vicinity of the central PBH. We present phase diagrams of temperature (T) vs. hydrogen number density (nH) for several simulation runs at the moment where collapsing particles were first identified. The simulations without a PBH (CDM) and without Lyman–Werner (LW) feedback from BH accretion (PBH_fd005) are included as a reference (taken from S. Zhang et al. 2025) to demonstrate the effects of PBH accretion heating and LW feedback on the surrounding gas. For the runs with PBHs (PBH_fd005, PBH_LW_fd005, and PBH_LW_str_fd005), the same feedback efficiency of ϵr = 0.005 is assumed. The effect of including LW radiation is demonstrated in the lower panels with the PBH_LW_fd005 (left) and PBH_LW_str_fd005 (right) runs, showcasing the change in the thermal evolution of the gas. The additional effect in the presence of baryon–DM streaming is evident in the PBH_LW_str_fd005 run, where successful runaway collapse along the near-isothermal atomic cooling track is triggered.
Paper: A Novel Formation Channel for Supermassive Black Hole Binaries in the Early Universe via Primordial Black Holes
Authors: Saiyang Zhang, Boyuan Liu, Volker Bromm
Figure caption: Normalized Lyman–Werner (LW) intensity, JLW/J21, as a function of the Eddington ratio, ﹩\eta \equiv {\dot{m}}_{{\rm{acc}}}/{\dot{m}}_{{\rm{Edd}}}﹩, for black holes of varying masses (mBH = 103, 104, 105, 106 M⊙). The JLW values are computed at a distance of r = 1 kpc from the black hole. The results based on the semianalytical spectra models for TD and ADAF accretion profiles in V. Takhistov et al. (2022) are shown by the thin solid and dashed lines, respectively. Here, the ADAF regime is only expected to occur at low accretion rates (η ≲ 0.007), best fitted with ﹩{J}_{{\rm{LW}}}\propto {\eta }^{\alpha ({m}_{{\rm{BH}}})}{m}_{{\rm{BH}}}^{3/2}﹩, where ﹩\alpha ({m}_{\mathrm{BH}})=1.95+0.11\,{\mathrm{log}}\,\left({m}_{\mathrm{BH}}/1{0}^{6}\,{M}_{\odot }\right)﹩ (Equation (4); thick dashed lines). The TD regime, occurring at higher accretion rates (η > 0.007), satisfies the scaling relation ﹩{J}_{{\rm{LW}}}\propto {\eta }^{2/3}{m}_{{\rm{BH}}}^{4/3}﹩ (Equation (4); thick dotted lines).
Paper: A Novel Formation Channel for Supermassive Black Hole Binaries in the Early Universe via Primordial Black Holes
Authors: Saiyang Zhang, Boyuan Liu, Volker Bromm
Figure caption: Evolution of gas infall rate (left panel) and total collapsing cloud mass (right panel) as a function of cosmic time since the initial collapse event, comparing select simulation scenarios: PBH_LW_sstr_fd005 (blue), PBH_LW_mstr_fd005 (orange), and PBH_LW_str_fd005 (green). The left panel compares our simulation results with typical inflow rates encountered in Population III star formation (∼10−2–10−3 M⊙ yr−1; light-red shading) and the critical rate required for DCBH formation (∼0.01–0.1M⊙ yr−1; light-green shading). The right panel summarizes the growth of the collapsing cloud mass within ∼5 Myr of cosmic time, approaching values characteristic of DCBH seeds (∼105 M⊙), compared to the primary PBH mass (∼106 M⊙; solid line). As can be seen, cases that combine LW feedback with the presence of (strong) baryon–DM streaming encounter conditions favorable for massive black hole seed formation.
Paper: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Authors: Chunming Zhu, Joel T. Dahlin, C. Richard DeVore, Jiong Qiu, Maria D. Kazachenko, Vadim M. Uritsky
Figure caption: Quadrupolar magnetic configuration of AR 13590. (a) The background (gray color scale) is the normal magnetic field component observed by SDO/HMI during the X6.4 flare on 2024 February 22. The positive/negative polarities are displayed in white/black colors. The boundaries of the four polarities are denoted with contours at around ±100 G. (b) Extrapolated magnetic field lines using potential field extrapolation. The location of an existing null point is marked with a red plus sign. Panel (c) showcases the extrapolated loops around the null point viewed from the south.
Paper: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Authors: Chunming Zhu, Joel T. Dahlin, C. Richard DeVore, Jiong Qiu, Maria D. Kazachenko, Vadim M. Uritsky
Figure caption: Evolution of the ribbons in the four magnetic polarities. (a) First brightening of the ribbons. The start time of each pixel’s first brightening is denoted by the color as shown in the color bar on the right. (b) Some locations of the ribbon display a second brightening. The contours mark the boundaries of the ribbons in (a). The same color bar in (a) is used to denote the start time of the second brightening. (c)–(f) AIA 1600 Å lightcurves of selected flaring pixels with one in each polarity, are marked with red “+” signs in panel (b). Their coordinates (in arcsec) are noted at the lower left of each panel. The red curves are Gaussian fittings to each local peak.
Paper: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Authors: Chunming Zhu, Joel T. Dahlin, C. Richard DeVore, Jiong Qiu, Maria D. Kazachenko, Vadim M. Uritsky
Figure caption: Reconnection rate profiles in this X6.4 flare. (a) The reconnection rate profile is displayed in a pink curve, and the accumulated reconnection flux is in blue. The width of each curve corresponds to the difference of the positive and negative polarities. (b) The total reconnection fluxes for each of the four major magnetic polarities.
Paper: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Authors: Chunming Zhu, Joel T. Dahlin, C. Richard DeVore, Jiong Qiu, Maria D. Kazachenko, Vadim M. Uritsky
Figure caption: Decay index above the PIL near the flare ribbons beside the filament. (a) The flaring PIL is associated with the filament, shown in cyan color, using the same method from X. Sun et al. (2015). (b) Profiles of overlying field strength Bh (in black) and decay index n (in red) above this flaring PIL region, using the median values along the PIL at varying heights from potential field extrapolation. Two heights at 2 Mm and 42 Mm are marked with plus signs. A vertical dotted line marks the critical height (n = 1.5) of 59 Mm.
Paper: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Authors: Chunming Zhu, Joel T. Dahlin, C. Richard DeVore, Jiong Qiu, Maria D. Kazachenko, Vadim M. Uritsky
Figure caption: Statistics of the ribbon brightening. (a) Number of pixels for the number of Gaussian components identified at each flaring pixel. (b) Distribution of the time difference between the two peaks at the pixels with multiple brightening. The black curve is for the whole flare region, while the colored curves correspond to the four polarities.
Paper: Identifying the Secondary Jet in the RadioAstron Image of OJ 287
Authors: Mauri J. Valtonen, Lankeswar Dey, Staszek Zola, Alok C. Gupta, Shubham Kishore, Achamveedu Gopakumar, Paul J. Wiita, Minfeng Gu, Kari Nilsson, Zhongli Zhang, Rene Hudec, Katsura Matsumoto, Marek Drozdz, Waldemar Ogloza, Andrei V. Berdyugin, Daniel E. Reichart, Markus Mugrauer, Tapio Pursimo, Stefano Ciprini, Tatsuya Nakaoka, Makoto Uemura, Ryo Imazawa, Michal Zejmo, Vladimir V. Kouprianov, James W. Davidson, Alberto Sadun, Jan Štrobl, Martin Jelínek, Abhimanyu Susobhanan
Figure caption: An illustration of the proposed astrophysical system of OJ 287. The primary black hole lies at the focal point of the eccentric orbit that has been determined in Paper I. The primary black hole is surrounded by an accretion disk. Due to spin–orbit interaction, the central part of the disk out to a few Schwarzschild radii is slanted relative to the main disk (J. M. Bardeen & J. A. Petterson 1975). There is a smooth transition from the inner disk to the outer disk (unlike in the figure). The primary jet starts out along the axis of the disk. The time evolution of the axis of the inner disk is calculated in Paper II. The secondary black hole is shown at two different orbital phases. Its accretion disk is parallel to the main accretion disk, and its jet therefore starts out perpendicular to the main disk. However, after Lorentz transformation to the observer’s frame, the secondary jet is seen tilted in the direction of the orbital motion, and thus, its direction changes constantly. Here the orbital motion is counterclockwise.
Paper: Identifying the Secondary Jet in the RadioAstron Image of OJ 287
Authors: Mauri J. Valtonen, Lankeswar Dey, Staszek Zola, Alok C. Gupta, Shubham Kishore, Achamveedu Gopakumar, Paul J. Wiita, Minfeng Gu, Kari Nilsson, Zhongli Zhang, Rene Hudec, Katsura Matsumoto, Marek Drozdz, Waldemar Ogloza, Andrei V. Berdyugin, Daniel E. Reichart, Markus Mugrauer, Tapio Pursimo, Stefano Ciprini, Tatsuya Nakaoka, Makoto Uemura, Ryo Imazawa, Michal Zejmo, Vladimir V. Kouprianov, James W. Davidson, Alberto Sadun, Jan Štrobl, Martin Jelínek, Abhimanyu Susobhanan
Figure caption: The image of OJ 287 at the record-breaking resolution of 12 μas, achieved in space VLBI when the RadioAstron telescope was 15 Earth diameters away from the ground-based telescopes (a distance of about 190,000 km, comparable to about half of the semimajor axis of the Moon orbit). The present primary jet direction is at about −45°, i.e., it goes through component J5. The path of the primary jet between the primary core C1a and J5 is not known and has to be determined by future high-resolution observations. The highest-resolution image agrees with the secondary jet, starting from the knot between components C1a and C1b toward a PA of about +15°. The two innermost components at the beginning of the jet lie at positions expected for the two black holes at the time of the observations in 2014 (see Figure 1). Superposed on the map is the jet line from Table 1 (star symbols). For the original RadioAstron map, see Paper III.
Paper: Identifying the Secondary Jet in the RadioAstron Image of OJ 287
Authors: Mauri J. Valtonen, Lankeswar Dey, Staszek Zola, Alok C. Gupta, Shubham Kishore, Achamveedu Gopakumar, Paul J. Wiita, Minfeng Gu, Kari Nilsson, Zhongli Zhang, Rene Hudec, Katsura Matsumoto, Marek Drozdz, Waldemar Ogloza, Andrei V. Berdyugin, Daniel E. Reichart, Markus Mugrauer, Tapio Pursimo, Stefano Ciprini, Tatsuya Nakaoka, Makoto Uemura, Ryo Imazawa, Michal Zejmo, Vladimir V. Kouprianov, James W. Davidson, Alberto Sadun, Jan Štrobl, Martin Jelínek, Abhimanyu Susobhanan
Figure caption: Left panel: the theoretical model of Paper II, after fitting to the radio jet observations. The primary black hole is at the center, and the secondary black hole is at a PA of about 35°. The blue dashed line is the initial direction of the secondary jet, while solid lines represent the primary jet at different times. The 2014 jet direction should be close to the green line. Right panel: a detail of the RadioAstron map of J. L. Gómez et al. (2022) in the same scale and orientation as the theoretical map. If the central component corresponds to the primary black hole, then the next one upwards marks the secondary black hole, and the highest component represents a knot in its jet. The elongation of the individual components is not real but is a reflection of the beam shape.
Paper: Identifying the Secondary Jet in the RadioAstron Image of OJ 287
Authors: Mauri J. Valtonen, Lankeswar Dey, Staszek Zola, Alok C. Gupta, Shubham Kishore, Achamveedu Gopakumar, Paul J. Wiita, Minfeng Gu, Kari Nilsson, Zhongli Zhang, Rene Hudec, Katsura Matsumoto, Marek Drozdz, Waldemar Ogloza, Andrei V. Berdyugin, Daniel E. Reichart, Markus Mugrauer, Tapio Pursimo, Stefano Ciprini, Tatsuya Nakaoka, Makoto Uemura, Ryo Imazawa, Michal Zejmo, Vladimir V. Kouprianov, James W. Davidson, Alberto Sadun, Jan Štrobl, Martin Jelínek, Abhimanyu Susobhanan
Figure caption: The PA of the radio jet in observations at 5 GHz and 8 GHz (points) from 1981 to 2010 and the theoretical line in the binary model (left; M. Valtonen et al. 2012). Subsequent observational points at 86 GHz have continued to remain more or less on the theoretical line (right; L. Dey et al. 2021). Preliminary data from 2017 to 2021 indicate that the jet continues to follow the model (G.-Y. Zhao 2025, private communication).
Paper: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Authors: Chunming Zhu, Joel T. Dahlin, C. Richard DeVore, Jiong Qiu, Maria D. Kazachenko, Vadim M. Uritsky
Figure caption: Schematic diagrams for the evolution of the confined X6.4 flare. Top panels: Phase I, breakout reconnection that removes the magnetic flux (blue) ahead of the rising filament (thick magenta), and interaction of the rising filament with its nearby fields. Lower panels: Phase II, antibreakout, relaxation of (overlying) fields progressively reconnecting the short/lower fields toward the north direction.