adsabs/AstroCLIMB huggingface dataset:
Paper: A Mildly Relativistic Outflow Launched Two Years after Disruption in Tidal Disruption Event AT2018hyz
Authors: Y. Cendes, E. Berger, K. D. Alexander, S. Gomez, A. Hajela, R. Chornock, T. Laskar, R. Margutti, B. Metzger, M. F. Bietenholz, D. Brethauer, M. H. Wieringa
Figure caption: Luminosity light curve of AT2018hyz, including early upper limits (green triangles; 0.9, 3, and 15 GHz) and the late-time detections starting at about 970 days (green stars; 5 GHz). Also shown for comparison are the light curves of the relativistic TDE Sw J1644+57 at (6.7 GHz; red; Berger et al. 2012; Zauderer et al. 2013; Eftekhari et al. 2018; Cendes et al. 2021b), the nonrelativistic event AT2019dsg (6.7 GHz; orange; Cendes et al. 2021a), and two events with apparent late-rising radio emission: ASASSN-15oi (6-7 GHz; blue; Horesh et al. 2021a) and iPTF16fnl (15.5 GHz; gray; Horesh et al. 2021b).
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Final location of protons at the end of our calculations. Panels (a), (b), (c), and (d) show the distribution of protons with four energy ranges 20 keV < E < 200 keV, 200 keV < E < 1 MeV, 1 MeV < E < 2 MeV, and E > 2 MeV, marked by red, blue, black and green, respectively.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Same as Figure 9, but for electrons. The energy ranges of panels (a), (b), (c), and (d) are 20 keV < E < 50 keV, 50 keV < E < 80 keV, 80 keV < E < 100 keV, and E > 100 keV, respectively.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Variations in (a) proton and (b) electron energy spectra vs. time that has been specified by the line type and the corresponding number, (c, d) the associated spectrum indices, and (e) the magnetic reconnection rate at different times.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Same as Figure 4, but for case 3. Particle moves around the magnetic island and eventually escapes from the magnetic island.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Final energy of (a) protons and (b) electrons vs. the time that the particles remain in the computational domain at t = 1.43. Each circle represents a single particle.
Paper: Particle Accelerations in a 2.5-dimensional Reconnecting Current Sheet in Turbulence
Authors: Yan Li, Lei Ni, Jing Ye, Zhixing Mei, Jun Lin
Figure caption: Energy spectra of (a) protons and (b) electrons at t = 1.43.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Low-resolution Spitzer IRS spectrum of IC 860. Some important line features are labeled with vertical lines, and the numbers near the lines indicate the wavelengths. IC 860 exhibits deep silicate absorption feature at 9.7 μm, emission from PAH, nebular emission lines, and H2 rotational lines. The steep slope F 30 μm/F 15 μm is indicative of hot dust possibly heated by an AGN.
Paper: Key Parameters Controlling the Photodesorption Yield in Interstellar CO Ice Analogs: The Influence of Ice Deposition Temperature and Thickness
Authors: Ni-En Sie, Yun-Ting Cho, Chao-Hui Huang, Guillermo M. Muñoz Caro, Li-Chieh Hsiao, Hsien-Chou Lin, Yu-Jung Chen
Figure caption: Panel (a): Y ipd as a function of N re(CO) for CO deposited in the 12.5–25 K range. The shaded region represents the saturated photodesorption yield, becoming Y ipd(ave). Panel (b): Y ipd(ave) as a function of deposition temperature for 89 ML thick CO ice. Panel (c): W(λ) and σ(λ) of CO ice as a function of wavelength.
Paper: Key Parameters Controlling the Photodesorption Yield in Interstellar CO Ice Analogs: The Influence of Ice Deposition Temperature and Thickness
Authors: Ni-En Sie, Yun-Ting Cho, Chao-Hui Huang, Guillermo M. Muñoz Caro, Li-Chieh Hsiao, Hsien-Chou Lin, Yu-Jung Chen
Figure caption: Panel (a): the photodesorption yield of 21 ML thick CO ice, calculated using the carbon balance method as a function of fluence in the 12.5 and 25 K experiments. The dashed lines depict the linear photodepletion of CO ice mainly resulting from CO desorption. The arrows indicate the first data points that fall outside the linear fit. Panels (b) and (c): Y ipd as a function of N re(CO) in the 12.5 and 25 K experiments, respectively. Panel (d): Y ipd as a function of N re(CO) for four different ice thicknesses deposited at 25 K. The shaded region represents the saturated photodesorption yield.
Paper: Key Parameters Controlling the Photodesorption Yield in Interstellar CO Ice Analogs: The Influence of Ice Deposition Temperature and Thickness
Authors: Ni-En Sie, Yun-Ting Cho, Chao-Hui Huang, Guillermo M. Muñoz Caro, Li-Chieh Hsiao, Hsien-Chou Lin, Yu-Jung Chen
Figure caption: A schematic diagram of the incident VUV photon passing through the ﹩N^{\prime} ﹩ th layer. The “N” subscript represents the incident intensity passing through that layer, where “0” means the initial incident MDHL intensity.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Radial profiles of the density D = ρ W (left panel) and radial 3-velocity v  r  = u  r /W (right panel) on the equatorial plane at small radii. The vertical dashed line indicates the radial coordinate of the ISCO radius for a Kerr black hole with a spin parameter of a * = 0.98.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Distributions of χ eff from observed GWTC-3 BH+BH data (solid blue bins) and simulated BH+BH systems (open green or red bins). The left-hand column (green bins) includes tossing of the second-born BH spin axis and leads to remarkable agreement with data, whereas the right-hand column (red bins) assumes no BH tossing. Differences in assumed parameters for simulations in the top, middle, and bottom rows are marked in the legend with a black bullet point and explained in the text. The black, blue, and gray curves in panel (A) are explained in the text (see also caption of Figure 11).
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Distributions of simulated χ eff values assuming no kicks (w = 0, top row) or as a function of exploring different BH component spin values (χ 1 and χ 2, panels (C)–(F)). The left column shows simulations including BH tossing; the right column is excluding BH tossing (see the text). In panel (A), the curves (blue) represent the mean estimate of the PDF of χ eff from the GWTC-3 data (Abbott et al. 2022b), (gray) the 5% and 95% quantiles, and (black) the blue curve normalized to the number of simulated systems.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Distributions of simulated χ eff values as a function of applying different pre-SN orbital separations, a 0 (4 R ⊙ and 40 R ⊙, top panels) and masses of the two resulting BH components, (M BH,1/M ⊙, M BH,2/M ⊙) = (12, 8), (59, 16), (37, 24), (24, 37) (central and bottom panels). The χ eff distribution is basically invariant to a 0 (except that fewer systems merge within a Hubble time if a 0 = 40 R ⊙), whereas it is slightly affected by the BH component masses.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Distributions of simulated χ eff values as a function of applying different BH component spin distributions (χ 1 and χ 2) in panels (A)–(D) excluding BH spin-axis tossing and assuming a kick of w = 500 km s−1. Even such large kicks cannot shift the distributions to sufficiently small values of χ eff in general; only low-mass BH+BH systems (panel (D)) allow significant cases with χ eff < 0. Panels (E) and (F) only include BH spin-axis tossing if M BH,2 < 20 M ⊙ or if χ 2 < 0.30, respectively (see the text).
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Spin magnitude PDFs of the first- (χ 1) and second-born (χ 2) BHs in isolated binary systems. The green, orange, and blue curves reflect Planck-like PDFs ﹩P({\chi }_{1})=b{\chi }_{1}^{3}/(\exp (c{\chi }_{1})-1)﹩, and a power-fraction PDF ﹩P({\chi }_{1})\,\,={\left({\chi }_{1}/a\right)}^{m}/{\left(1+{\chi }_{1}/a\right)}^{n}﹩, respectively. The red curve is a simple power-function PDF given by ﹩P{({\chi }_{2})=24/(7(2-{\chi }_{2})}^{4})﹩. See the legends and Table 1 for values of b, c, a, m and n. The PDFs for χ 1 and χ 2 reflect different expectations of slow and fast-spinning BHs, respectively, based on binary star evolution (see the text). For comparison, the gray dotted line is a flat PDF.
Paper: Tossing Black Hole Spin Axes
Authors: Thomas M. Tauris
Figure caption: Distributions of simulated χ eff values as a function of applying different BH component spin distributions (χ 1 and χ 2). In general, the fit to the empirical data is best for small values of χ 1 ∼ 0.1 and medium to large values of χ 2, in accordance with expectations from binary evolution theory (see the text, and compare with histograms in other figures). Panels (A) (χ 1 = 0) and (C) (no alignment of first-born BH, i.e., in effect double BH tossing) have fully symmetric χ eff distributions as expected.
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Spectral strain sensitivities of decihertz GW detectors and the equivalents for the source amplitudes of inspiral GWs for equal-mass WD–WDs with different masses at 11 Mpc. The upper cutoff frequency is given by the frequency at the coalescence from Equation (16). The diamonds, triangles, and circle points correspond to 10 yr before merger, 3 yr before merger, and the upper cutoff frequency, respectively.
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Stellar mass distribution of nearby galaxies within 11 Mpc.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Spectral index expected from the sum of two power-law components as a function of the fraction between them (f). Specifically, the sum is represented as ﹩{S}_{\nu }\propto {(\nu /{\nu }_{0})}^{-{\alpha }_{1}}+f\times {(\nu /{\nu }_{0})}^{-{\alpha }_{2}}﹩, where α 1 = −3.5 (orange) and α 2 = 0.7 (blue) are considered the fiducial values for SF and an AGN, respectively. The result with these parameters is shown by a black solid curve. The red dashed line indicates α mm = 0.3, suggesting that the emission from objects with indices above ≈0.3 would be dominated by the AGN emission with α 2 ∼ 0.7 rather than the SF emission with α 1 = −3.5. Considering a possible range of α 1 = −3.60 ± 0.38 from β BB = 1.60 ± 0.38 (Casey 2012), we also plot the corresponding lines by dotted gray lines. In addition, the cases where the power-law indices of the AGN component are 0.5 and 1.0, expected from the SED models of IC 4329A and NGC 985 (Inoue & Doi 2018), are also indicated by dashed gray lines. For comparison, the black dotted–dashed line and gray shaded area represent the average of the observed values for our AGNs and their standard deviation, respectively.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Top: histogram of the logarithmic ratio of the mm-wave peak flux density measured by using an ALMA 7-m array data and that expected from the host-galaxy SED model. Sources with upper limits are indicated in orange. Middle: histogram of the logarithmic ratio of the mm-wave flux density expected from the host-galaxy SED model (i.e., thermal dust emission) and that predicted from synchrotron plus free–free emission. In each SED of Figure 4, these two components are shown as a gray dashed line and an orange pentagon, respectively. The thermal emission is generally stronger than the sum of the synchrotron and free–free components. Bottom: histogram of the logarithmic ratio of the mm-wave peak flux density and that predicted from the AGN SED model (blue dashed line in Figure 4). Sources with upper and lower limits are indicated in orange and gray, respectively.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Top: plot of the ﹩\nu {L}_{\nu ,\mathrm{mm}}^{\mathrm{peak}}/{L}_{14-150}﹩ ratio vs. the radio loudness based on the 3 GHz and 14–150 keV luminosities. AGNs with upper limits are shown in black. Bottom: correlations between the mm-wave and 14–150 keV luminosities for RQ AGNs (orange) and RL AGNs (blue). In both panels, fitted regression lines and ±1σ scat ranges are indicated by dashed lines and shaded areas, respectively.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Comparison of the flux density of an unresolved component constrained by the visibility fitting and the observed peak one. The gray solid and yellow dotted lines indicate the one-to-one relation and the fitted line with ﹩{S}_{\nu ,\mathrm{mm}}^{\mathrm{fit}}﹩ being the dependent parameter, respectively.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Luminosity correlation of the mm-wave and 14–150 keV emission for 31 AGNs with high mm-wave surface brightnesses, exceeding an Eddington limit for the SF. A regression line is indicated by the black dashed line.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Scatter plots of the ﹩\nu {L}_{\nu ,\mathrm{mm}}^{\mathrm{peak}}/{L}_{14-150}﹩ ratio vs. the bolometric luminosity, the black hole mass, and the Eddington ratio. AGNs with upper limits are shown as black circles. No correlations are found.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Spectral index vs. SFR surface density, estimated by converting the observed mm-wave luminosity to the SFR. An Eddington limit of 2000 M ⊙ yr−1 kpc−2 is indicated by the gray line, and the spectral index of −3.5, expected for thermal emission, is denoted by the yellow line. No correlation is found.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Luminosity correlation of the mm-wave and 14–150 keV emission for AGNs with mm-wave-based SFRs being higher than those expected from the IR decomposition analysis. A regression line is indicated by the black dashed line.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Scatter plot of the spectral index vs. the achieved beam size in units of parsecs. The spectral index is not correlated with the beam size.
Paper: The Origin and Distance of the High-velocity Cloud MI
Authors: J. T. Schmelz, G. L. Verschuur
Figure caption: Area maps centered on MI showing the details of the environment at different velocities using EBHIS data with a 2 km s−1 bandwidth. Legends are in degrees kelvin. In each frame the dashed circle highlights the approximate boundary of the low-velocity cavity seen in Figure 1. (a) the well-known two-peaked structure of MI at 120 km s−1; (b) the structure of MI at −110 km s−1; (c) the rim of a low-velocity cavity in the H I emission at −20 km s−1, which is particularly prominent in the lower right quadrant; (d) the more pronounced rim at −16 km s−1; (e) a low-velocity peak at the center of the cavity at −14 km s−1; (f) the low-velocity cavity at 0 km s−1.
Paper: The Origin and Distance of the High-velocity Cloud MI
Authors: J. T. Schmelz, G. L. Verschuur
Figure caption: (a) Pixels showing the enhanced soft X-rays seen by ROSAT (grayscale; Herbstmeier et al. 1995), the current position of 56 UMa (star), and the proper motion vector (red arrow) overlaid on the low-velocity H I gas at −10 km s−1 with the legend in degrees kelvin. (b) The same as (a) except overlaid on the MI contours at −120 km s−1 with the legend in degrees kelvin. (c) IRAS 100 μm data showing the MI cavity with the legend in MJy sr−1. (d) The diffuse soft X-ray image adapted from Figure 2 of Herbstmeier et al. (1995) overlain on a map of the total H I column density between ±25 km s−1 with the legend in degrees kelvin showing that the soft X-rays are found where the H I column density is lowest. The dashed circle highlights the approximate boundary of the low-velocity cavity seen in Figure 1.
Paper: The Origin and Distance of the High-velocity Cloud MI
Authors: J. T. Schmelz, G. L. Verschuur
Figure caption: Area map at −14 km s−1 showing the complex low-velocity gas structure and the cavity between l = 158° and 175° using EBHIS data with a 2 km s−1 bandwidth. Legend is in degrees kelvin.
Paper: The Origin and Distance of the High-velocity Cloud MI
Authors: J. T. Schmelz, G. L. Verschuur
Figure caption: Positive-velocity EBHIS H I maps at (a) +10 km s−1 and (b) +20 km s−1 with the legends in degrees kelvin; and WHAM Hα maps integrated over 10 km s−1 intervals at (c) +10 km s−1 and (d) +20 km s−1 with the legends in Rayleighs. The dashed circle highlights the approximate boundary of the low-velocity cavity seen in Figure 1.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: From top to bottom, a dirty image of NGC 985 and a residual image obtained by removing fitted unresolved and extended components, which are modeled by Gaussian functions. We note that the clear extended morphologies seen in the dirty image do not necessarily indicate the presence of such emission in a reconstructed image produced by the cleaning task.