adsabs/AstroCLIMB huggingface dataset:
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: CO(3–2) outflows detected in S07 (a) and S09 (b). The upper panels show the spatial distribution of high-velocity CO gas. Blue contours represent the blueshifted component (integrated over 146–158 km s−1 for S07 and 108–121 km s−1 for S09), while red contours represent the redshifted component (integrated over 168–180 km s−1 for S07 and 138–150 km s−1 for S09). Background is the 850 μm continuum flux. The green stars represent the position of the protostar inferred from the continuum peak position. The synthesized beam size is shown by the gray filled circle in each panel. The lower panels show the CO(3–2) spectra extracted at the hot-core position as in Figures B1–B2. The velocity ranges of the blue- and redshifted high-velocity components are indicated by blue and red, respectively. The dotted lines indicate a systemic velocity of the source estimated from the SO(N  J  = 88–77) line.
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: Same as in Figure B1 but for S09. The adjacent stronger line seen in SO2(104,6–103,7) was subtracted before fitting the main line.
Paper: Evolution of Magnetic Field Fluctuations and Their Spectral Properties within the Heliosphere: Statistical Approach
Authors: Jana Šafránková, Zdeněk Němeček, František Němec, Daniel Verscharen, Timothy S. Horbury, Stuart D. Bale, Lubomír Přech
Figure caption: Evolution of (a) the magnetic field strength, ∣B∣; (b) proton β; (c) the standard deviation of the magnetic field strength, σ∣B∣; (d) the standard deviation of the perpendicular magnetic field component, σ B ⊥; (e) normalized σ∣B∣/∣B∣; and (f) normalized σ B ⊥/∣B∣ with distance from the Sun. Gray dots represent the values of each quantity averaged over a given 20 minute interval (light and heavy gray points show PSP and SolO intervals, respectively); full red (PSP) and black (SolO) bars show the standard deviation medians in distance bins; and dashed red and black bars show their first and third quartiles. The Spearman correlation coefficients are given on top of each panel. The light blue horizontal lines represent the median value of a particular parameter at 1 au determined from the Wind data.
Paper: Evolution of Magnetic Field Fluctuations and Their Spectral Properties within the Heliosphere: Statistical Approach
Authors: Jana Šafránková, Zdeněk Němeček, František Němec, Daniel Verscharen, Timothy S. Horbury, Stuart D. Bale, Lubomír Přech
Figure caption: (a) Dependence of the f min frequency as a proxy of the ion spectral break; and (b) PSD slope 2 of ∣B∣ fluctuations in the kinetic range for different distance bins. PSD slope 2 as a function of: (c) σ∣B∣, (d) σ∣B∣ normalized to background ∣B∣; (e) σ B ⊥, and (f) σ B ⊥ normalized to ∣B∣. The format follows Figure 2, the light blue dots in all panels and the horizontal line in the panel (b) show medians of slope 2 determined from Wind observations at 1 au.
Paper: Evolution of Magnetic Field Fluctuations and Their Spectral Properties within the Heliosphere: Statistical Approach
Authors: Jana Šafránková, Zdeněk Němeček, František Němec, Daniel Verscharen, Timothy S. Horbury, Stuart D. Bale, Lubomír Přech
Figure caption: Median PSD spectra of (a) compressive and (b) noncompressive magnetic field fluctuations in different distance bins from the Sun (in the spacecraft frame); (c) Variations of the magnetic field spectral index as a function of heliocentric distance in the inertial range (10−2–10−1 Hz). The light blue points indicate the values of the slopes in the large statistics of Wind data (Šafránková, 2019).
Paper: Evolution of Magnetic Field Fluctuations and Their Spectral Properties within the Heliosphere: Statistical Approach
Authors: Jana Šafránková, Zdeněk Němeček, František Němec, Daniel Verscharen, Timothy S. Horbury, Stuart D. Bale, Lubomír Přech
Figure caption: PSD slope 2 in two distance ranges. The left panels show PSP data (red) at distances between 0.1 and 0.3 au; the right panels show PSP data (red) and SolO data (black) at distances between 0.4 and 1 au. We overplot Wind data at 1 au for reference on all panels. The slopes are shown as a function of: (a, b) σ∣B∣ normalized to the background value of ∣B∣; and (c, d) σ B ⊥ normalized to ∣B∣.
Paper: Detection of Dust in High-velocity Cloud Complex C–Enriched Gas Accreting onto the Milky Way 
Authors: Andrew J. Fox, Frances H. Cashman, Gerard A. Kriss, Gisella de Rosa, Rachel Plesha, Yasaman Homayouni, Philipp Richter
Figure caption: Derivation of elemental abundances and dust depletions in Complex C toward Mrk 817. The top panel shows the ionization corrections (ICs) from our CLOUDY models for six ions as a function of gas density. The best-fit density (dotted line) is derived by matching the observed Fe III/Fe II ratio in Complex C. The middle panel shows the ionization-corrected abundances of each element relative to hydrogen [X/H]. The bottom panel shows the depletion of each element relative to sulfur [X/S], where S is chosen as an undepleted reference element. All data points are from our new COS analysis except oxygen, which is based on the O I measurement from Collins et al. (2003; see Table 1).
Paper: Detection of Dust in High-velocity Cloud Complex C–Enriched Gas Accreting onto the Milky Way 
Authors: Andrew J. Fox, Frances H. Cashman, Gerard A. Kriss, Gisella de Rosa, Rachel Plesha, Yasaman Homayouni, Philipp Richter
Figure caption: Top: H I 21 cm emission map of Complex C in Aitoff projection based on HI4PI data (Westmeier 2018). The map is integrated over the velocity range −175 < v LSR < −50 km s−1. The location of Mrk 817 is marked with a red circle, and major HVC complexes are labeled in pink. Bottom: full coadded COS/FUV spectrum of Mrk 817 labeled with MW lines used in this analysis. The extremely high S/N of this spectrum enables high-precision measurements of Complex C absorption. MW Lyman-alpha absorption was not observed because the G130M/1222 grating setting places it in the gap between COS detector segments A and B.
Paper: Detection of Dust in High-velocity Cloud Complex C–Enriched Gas Accreting onto the Milky Way 
Authors: Andrew J. Fox, Frances H. Cashman, Gerard A. Kriss, Gisella de Rosa, Rachel Plesha, Yasaman Homayouni, Philipp Richter
Figure caption: Voigt profile fits to the low-ion absorption from Complex C in the coadded HST/COS spectrum of Mrk 817. Normalized flux is plotted against LSR velocity for 11 low-ionization metal lines. A 21 cm spectrum from the GBT is included in the top-left panel. The Complex C components are centered at v LSR = −149, −114, and −86 km s−1. The pink curves show the Complex C model adopted in this study. Individual components are shown with gray lines, dashed for Complex C and solid for Milky Way components. The data have been binned by 3 pixels.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Schematic illustration of the runaway SMBH scenario as an explanation of the key observed features. Panels 1–5 show a “classical” slingshot scenario (e.g., Saslaw et al. 1974). First, a merger leads to the formation of a long-lived binary SMBH (1,2). Then a third galaxy comes in (3), its SMBH sinks to the center of the new merger remnant, and this leads to a three-body interaction (4). One black hole (usually the lightest) becomes unbound from the other two and receives a large velocity kick. Conservation of linear momentum implies that the remaining binary gets a smaller velocity kick in the opposite direction. If the kicks are large enough all SMBHs can leave the galaxy (5). There can be ≳1 Gyr between the events in panels (2) and (3). Panels (4) and (5) happened ∼40 Myr before the epoch of observation. The background of (6) is a frame from an Illustris TNG simulation (Pillepich et al. 2018), with lighter regions having higher gas density. This illustrates that there can be highly asymmetric flows in the circumgalactic medium, and we speculate that the SMBH at A is traveling through such a region of relatively dense and cold CGM (see text). Credit for the image in the top left panel: NAOJ.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Comparison of the observed colors of several knots in the feature (shown at the top) to model predictions of Conroy et al. (2009) for different ages. Dashed model predictions are for a metallicity Z = −1, solid for Z = −0.5, and dotted–dashed lines are for Z = 0. Blue lines are dust-free models, and red lines illustrate the effect of dust attenuation with A  V  = 1. Horizontal lines are measurements for the three knots. The ages of the youngest stars are likely ≲30 Myr, but there is no straightforward relation between age and color in this regime. The observed colors span a similar range as the models and are consistent with a wide range of possible metallicities, ages, and dust content.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Left: section of the summed ACS F606W+F814W image, with the LRIS slit indicated in blue. Besides the tip of the linear feature, A, there are two other bright spots in the vicinity, B and C. Object B falls in the slit. Center: section of the LRIS spectrum around the [O III] λ5007 line. Object B is detected, as well as faint emission in between B and the galaxy. The attached panel shows the intensity along the feature, on a logarithmic scale. Right: The presence of a “counter” feature is confirmed through its detection in the u band, which samples the rest-frame far-UV. For clarity the u-band image was binned by a factor of 6 in the direction perpendicular to the slit (and then expanded again to retain the correct spatial scale). Also note that the primary feature extends all the way to the galaxy, in marked contrast to the pronounced gap between the galaxy and the feature in the ACS image.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Observed F606W−F814W color along the wake, after smoothing with a 0.″15 boxcar filter. The red curve is a simple stellar population with Z = − 0.5, A  V  = 1.1 mag, and age varying linearly with position along the wake. The best-fit time since ejection is 39 Myr, corresponding to a projected black hole velocity of v BH ≈ 1600 km s−1.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Connection between velocities along the wake and its morphology. Top left: [O III] emission along the wake, with a fit to the velocity centroids in orange. Middle left: HST image of the wake, with stretched vertical axis to emphasize variations. The orange dots are centroids. Bottom right: fit of a kinematic model to the HST centroids, based on the [O III] velocity profile. This fit is also shown in the bottom left panel. Upper right: distribution of posteriors for the black hole velocity v BH, modified by an unconstrained geometric parameter β. For β ≈ 0.3 we find that v BH is consistent with the value derived from the color variation along the wake.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: The four panels correspond to the rest-frame near-UV continuum, F606W − F814W color, [O III], and Hβ emission along the linear feature (pictured at the top). The F606W continuum shows strong variation on all spatial scales, and is brightest at the furthest point from the galaxy. The color shows large and seemingly random variations. The [O III]/Hβ ratio varies by a factor of ∼10 along the feature, with some regions likely dominated by shock ionization and others dominated by H II regions.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Detailed view of the areas around A and B, in the summed F606W + F814W image. Green bands indicate the locations of [O III] knots in the LRIS spectrum. If B is a chance projection along the line of sight, an HCSS may be detectable near the cross in deeper data. In the vicinity of A, the complex interplay of shocks, star formation, and the SMBH itself could be investigated with high-resolution IFU spectroscopy.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Location of the galaxy in the BPT diagram, with SDSS galaxies in light gray. The lines divide “pure” star-forming galaxies from those with an AGN contribution to their line ratios, for z = 0 and z = 1 (Kewley et al. 2013). The location is as expected for a z = 1 star-forming galaxy. The inset shows the NIRES spectrum in the Hα region. The red line is the best fit.
Paper: Turbulence in Zeeman Measurements from Molecular Clouds
Authors: Zhuo Cao, Hua-bai Li
Figure caption: A comparison between the cloud cores from the idealized “textbook” model and from MHD simulations. Left: the textbook model of cloud core B–n relations (adopted from Li 2021). The arrows indicate the direction of effective compression. The case with dominant B-field or self-gravity will possess an index of 0 or 2/3, respectively. An index larger than 2/3 can result from nongravitational forces, e.g., turbulence, stellar wind, or supernova compression. Right: cores from MHD simulations appear markedly different from the textbook model. Each row presents the data from one core; from top to bottom are Cores 1 to 3. Each column is derived from one snapshot of each core; from left to right are starting, middle, and ending snapshots, which are defined in Appendix A.2.
Paper: Turbulence in Zeeman Measurements from Molecular Clouds
Authors: Zhuo Cao, Hua-bai Li
Figure caption: Density distributions and B–n relations. Left: the black lines represent the probability density functions (PDFs) of the whole simulated domain immediately before the gravity was turned on (dashed) and 2 Myr later at the end of the simulation (dotted–dashed). The trace of the clumps (red) and cores (blue) is detailed in Appendix A.2, and the PDFs are derived from their last snapshots. N is the number of pixels. Right: the red dots represent the spatial B–n relation immediately before the gravity was turned on; the blue dots are derived from the last snapshot, which is 2 Myr after the red dots. The black lines represent the temporal B–n relations of the cores, starting from the black filled circle and ending at the cross symbol. Along each black line there is a time lapse of 0.02 Myr between any adjacent symbols. For the temporal B–n, the typical error bar (standard deviation) of number density is 1e2, and that of the magnetic field is 1e-2. N  p  is the number of pixels within a density bin.
Paper: Turbulence in Zeeman Measurements from Molecular Clouds
Authors: Zhuo Cao, Hua-bai Li
Figure caption: How the forces regulate B-field strength. This figure illustrates the volume integration of the divergences of the force f  i ⊥ in the volume above the mean density of a core (details of the calculation can be found in Appendix A.3), where “i” can be G, Th, B, or Adv, corresponding to gravitational, thermal, magnetic, and advection, respectively. “⊥” indicates that only the component perpendicular to the mean field is considered here as only the perpendicular component is capable of affecting the strength of the field. Note that the negative of f Th⊥ divergence is plotted to conserve space as most of the divergences of other forces are negative. A positive/negative f  i ⊥ means that, in an average sense, the force was dispersing/compressing the field lines.
Paper: Turbulence in Zeeman Measurements from Molecular Clouds
Authors: Zhuo Cao, Hua-bai Li
Figure caption: The spatial B–n relations from individual cores. The “start” and “end” represent the starting and ending snapshots of each core, respectively (Appendix A.2). The dashed straight lines give a reference slope of 0.3. The typical error bar (standard deviation) of density is 1e2, and that of the magnetic field is 1e-2.
Paper: Turbulence in Zeeman Measurements from Molecular Clouds
Authors: Zhuo Cao, Hua-bai Li
Figure caption: A comparison of the virial parameters (α) from simulation and observation. Ranging from 0.2 to 2, the α of Cores 1 to 3 are plotted against time in the left three panels. With the core mass of two solar masses, α = 0.2 to 2 are plotted on top of the observed α-mass relation from Kerr et al. (2019; right panel).
Paper: Turbulence in Zeeman Measurements from Molecular Clouds
Authors: Zhuo Cao, Hua-bai Li
Figure caption: The clump-finding algorithm. (1) From zero to the minimum potential, 1/40 of this potential range is reduced in each step. (2) Defined by the CCL method.
Paper: Turbulence in Zeeman Measurements from Molecular Clouds
Authors: Zhuo Cao, Hua-bai Li
Figure caption: The core-finding algorithm.
Paper: Observation of Anomalous Electron Fluxes Induced by GRB221009A on CSES-01 Low-energy Charged Particle Detector
Authors: R. Battiston, C. Neubüser, F. M. Follega, R. Iuppa, V. Vitale, R. Ammendola, D. Badoni, S. Bartocci, A. Bazzano, S. Beolè, I. Bertello, W. J. Burger, D. Campana, A. Cicone, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, F. De Angelis, C. De Donato, C. De Santis, P. Diego, A. Di Luca, E. Fiorenza, G. Gebbia, A. Lega, M. Lolli, B. Martino, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, A. Morbidini, F. Nuccilli, F. Nozzoli, A. Oliva, G. Osteria, E. Papini, F. Palma, F. Palmonari, A. Parmentier, B. Panico, S. Perciballi, F. Perfetto, A. Perinelli, P. Picozza, M. Piersanti, M. Pozzato, G. Rebustini, D. Recchiuti, E. Ricci, M. Ricci, J. Rodi, A. Russi, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, X. Shen, A. Sotgiu, R. Sparvoli, S. Tofani, P. Ubertini, N. Vertolli, V. Vilona, U. Zannoni, Z. Zeren, S. Zoffoli, P. Zuccon
Figure caption: (a) The flux profile vs. time for channel 0 of HEPP-L. The blue and red curves show the flux corresponding to the second lowest (150–250 keV) and highest (1.05–3 MeV) energy bin, respectively. The horizontal lines mark the threshold of 3σ above the average for the corresponding L-α eq bins. (b) The flux significance of the particle bursts given in the number of standard deviations above the background.
Paper: Observation of Anomalous Electron Fluxes Induced by GRB221009A on CSES-01 Low-energy Charged Particle Detector
Authors: R. Battiston, C. Neubüser, F. M. Follega, R. Iuppa, V. Vitale, R. Ammendola, D. Badoni, S. Bartocci, A. Bazzano, S. Beolè, I. Bertello, W. J. Burger, D. Campana, A. Cicone, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, F. De Angelis, C. De Donato, C. De Santis, P. Diego, A. Di Luca, E. Fiorenza, G. Gebbia, A. Lega, M. Lolli, B. Martino, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, A. Morbidini, F. Nuccilli, F. Nozzoli, A. Oliva, G. Osteria, E. Papini, F. Palma, F. Palmonari, A. Parmentier, B. Panico, S. Perciballi, F. Perfetto, A. Perinelli, P. Picozza, M. Piersanti, M. Pozzato, G. Rebustini, D. Recchiuti, E. Ricci, M. Ricci, J. Rodi, A. Russi, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, X. Shen, A. Sotgiu, R. Sparvoli, S. Tofani, P. Ubertini, N. Vertolli, V. Vilona, U. Zannoni, Z. Zeren, S. Zoffoli, P. Zuccon
Figure caption: (a) Number of energy bins covered by PBs as a function of every minute in 2022. The PBs of the first and second peak due to the GRB221009A are circled in red and orange, respectively. The time line gaps are due to missing data, e.g., there are no data available in 2022 August. (b) Number of energy bins distribution (projection of (a) on y-axis) for 2022. The orange and green lines correspond to fits using a Poissonian distribution and exponential function.
Paper: Observation of Anomalous Electron Fluxes Induced by GRB221009A on CSES-01 Low-energy Charged Particle Detector
Authors: R. Battiston, C. Neubüser, F. M. Follega, R. Iuppa, V. Vitale, R. Ammendola, D. Badoni, S. Bartocci, A. Bazzano, S. Beolè, I. Bertello, W. J. Burger, D. Campana, A. Cicone, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, F. De Angelis, C. De Donato, C. De Santis, P. Diego, A. Di Luca, E. Fiorenza, G. Gebbia, A. Lega, M. Lolli, B. Martino, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, A. Morbidini, F. Nuccilli, F. Nozzoli, A. Oliva, G. Osteria, E. Papini, F. Palma, F. Palmonari, A. Parmentier, B. Panico, S. Perciballi, F. Perfetto, A. Perinelli, P. Picozza, M. Piersanti, M. Pozzato, G. Rebustini, D. Recchiuti, E. Ricci, M. Ricci, J. Rodi, A. Russi, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, X. Shen, A. Sotgiu, R. Sparvoli, S. Tofani, P. Ubertini, N. Vertolli, V. Vilona, U. Zannoni, Z. Zeren, S. Zoffoli, P. Zuccon
Figure caption: Electron flux of all HEPP-L channels summed over the energy range from 250 keV to 3 MeV on 2022 October 9 starting from 13:20:00 UTC. The blue curve shows the measured photon counts per second of the HEBS GRD01 instrument (Liu et al. 2022b), scaled to match the maximum of the first HEPP-L peak. The scaling factor is given in the legend. The vertical dashed lines mark the reference UTC times of the signals measured by other instruments; see Table 1. No corrections were applied to the timing provided by HEBS and HEPP-L instruments.