adsabs/AstroCLIMB huggingface dataset:
Paper: Are the Magnetic Field Directions of Surrounding Loops a Key Parameter for Confining a Solar Filament Eruption?
Authors: Tao Ding, Jun Zhang, Junchao Hong
Figure caption: DEM results at the interaction region of FS2 and L2. The first two rows show the EM and temperature maps. Purple boxes in panels (a1) and (b1) outline the FOV of panels (a2), (a3), (b2), and (b3). The temperature curves of regions “M” (panels (a2) and (b2)) and “N” (panels (a3) and (b3)) are given in panel (c). Panels (d)–(e) display the averaged DEM distributions of regions “M” and “N,” respectively. The red curves in panels (d)–(e) are the optimum DEM distributions while the black curves are the results of 100 Monte Carlo simulations, suggesting that the solutions are very reliable.
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: Probability distribution function of the Doppler (b) parameter comparing TNG (black line) and Illustris (red lines). From top left to bottom right, the panels show the distribution broken down by column density ranges. The bottom right shows the full range of column density for the low and intermediate column density range of the IGM (1012.5 ≤ N H I  ≤ 1015 cm−2). The top-right plot includes the COS observations first analyzed in Danforth et al. (2016) (pink points) and later reanalyzed in Viel et al. (2017) (blue points) in the same column density bin. For each plot, b values less than 13 km s−1 were removed as those approximately correspond to the cooling floor of the simulations. Values higher than 100 km s−1 were removed as b values higher than this are typically not observed and also tend to correspond to bad Voigt fits.
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: A visual comparison of the z = 0.1 (left panel) and z = 2.0 (right panel) of 1 Mpc thick slices of the IGM column density (left columns) and mass-weighted temperature (right columns) in Illustris (top row) and TNG (bottom row). At z = 2.0, there are very minor differences between Illustris and TNG but by z = 0.1 significant visual differences are obvious in the temperature and density of the IGM. The differences seen here are nearly entirely due to the changes in the AGN jet feedback model. HIM gas above 107 K (traced in X-rays wavelengths; red color in the temperature color bar) dominates in Illustris while the IGM volume is more filled by warm Lyα-emitting gas in TNG (gas around 104 K (blue color in the temperature color bar).
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: A comparison of the z = 0.1 CDD between Illustris (red solid line) and TNG (black solid line) with the D16 data set (blue points). Both Illustris and TNG use the fiducial boxes. In order to see if the altered AGN feedback model could mimic the effects of the UVB, we include the CDD of Illustris with a UVB field strength 0.4 times the original (i.e., dashed red line). Changing the Illustris UVB by this factor provides a good match to TNG for column densities below 1015 cm−2
Paper: The Low-redshift Lyα Forest as a Constraint for Models of AGN Feedback
Authors: Blakesley Burkhart, Megan Tillman, Alexander B. Gurvich, Simeon Bird, Stephanie Tonnesen, Greg L. Bryan, Lars Hernquist, Rachel S. Somerville
Figure caption: Mass-weighted temperature–density contour plot for hydrogen gas in the IGM in Illustris (far right) and TNG (far left) and their ratio (center). The central plot is colored by the gas mass ratio of TNG to Illustris.
Paper: Finding Lensed Direct-collapse Black Holes and Supermassive Primordial Stars
Authors: Anton Vikaeus, Daniel J. Whalen, Erik Zackrisson
Figure caption: Minimum number densities n min required for the photometric detection of one single gravitationally lensed DCBH (top), blue SMS (center), and red SMS (bottom) as a function of redshift. The gray shaded area (extending down to 10−9 Mpc−3 in all figures) shows the expected range of number densities of halos that can host SMSs and DCBHs from simulations (Habouzit et al. 2016; Valiante et al. 2017).
Paper: Finding Lensed Direct-collapse Black Holes and Supermassive Primordial Stars
Authors: Anton Vikaeus, Daniel J. Whalen, Erik Zackrisson
Figure caption: Minimum magnification (﹩{\mu }_{\min }﹩) required for photometric detection of a gravitationally lensed DCBH (top), blue SMS (center), and red SMS (bottom) as a function of redshift for the different surveys. The filter used for each object and survey is specified in Table 2. Note that the lines are only plotted for μ > 1. Therefore, the ultradeep NIRCam exposures are not included for the DCBH because no magnification is required in that particular case. The two dashed–dotted black lines indicate the magnification above which an object with a given intrinsic size (1 pc and 10 pc plotted here) could become resolved in imaging.
Paper: Finding Lensed Direct-collapse Black Holes and Supermassive Primordial Stars
Authors: Anton Vikaeus, Daniel J. Whalen, Erik Zackrisson
Figure caption: Source-frame spectra for the 105 M ⊙ DCBH (left) and 1.0 M ⊙ yr−1 SMSs (right) after reprocessing by the host gas envelope.
Paper: A Green Pea Starburst Arising from a Galaxy–Galaxy Merger
Authors: S. Purkayastha, N. Kanekar, J. N. Chengalur, S. Malhotra, J. Rhoads, T. Ghosh
Figure caption: The HI spatial distribution around GP J0213+0056 (in contours), at resolutions of (a) 16″, (b) 12″, (c) 9″, and (d) 7″, each overlaid on the Subaru HSC i-band image. The GMRT synthesized beam FWHM is indicated by the circle on the bottom left of each panel. The contours in each panel are at (− 2.0, 2.0, 3.0, 4.0, 5.0) × σ, with the base contours at HI column densities of (a) 1.4 × 1020 cm−2, (b) 2.2 × 1020 cm−2, (c) 3.5 × 1020 cm−2, and (d) 5.3 × 1020 cm−2; negative values are shown with dashed contours. The locations of GP J0213+0056 and G1 are indicated in each panel by the label “GP” and the symbol “×”, respectively.
Paper: ALMA Images the Eccentric HD 53143 Debris Disk
Authors: Meredith A. MacGregor, Spencer A. Hurt, Christopher C. Stark, Ward S. Howard, Alycia J. Weinberger, Bin Ren, Glenn Schneider, Elodie Choquet, Dmitri Mawet
Figure caption: The flux density of the central star varies over the course of our eight ALMA observations, indicating potential flaring. Each point in this light curve represents the best-fit stellar flux density in each individual observation. For reference, the expected photospheric flux of 33 μJy for a G9V star is indicated by the dashed red line. Simultaneous TESS observations plotted in gray indicate significant spot modulation.
Paper: ALMA Images the Eccentric HD 53143 Debris Disk
Authors: Meredith A. MacGregor, Spencer A. Hurt, Christopher C. Stark, Ward S. Howard, Alycia J. Weinberger, Bin Ren, Glenn Schneider, Elodie Choquet, Dmitri Mawet
Figure caption: An eccentric disk model (bottom) provides a better fit to the ALMA data than a symmetric one (top). In both figures, panels are as follows: (left) the ALMA 1.3 mm continuum image, (left, center) the best-fit model at full resolution, (right, center) the best-fit model imaged like the data with no noise, and (right) the residuals produced by subtracting the best-fit model from the data. For reference, the dashed outline and star symbol indicate the edges of the outer disk and the stellar position in the residual image. Contours are in steps of 3σ (3× the rms noise of 5.6 μJy beam−1) in all panels. As in Figure 1, the gray ellipse in the lower-left corner indicates the 1.″13 × 0.″92 synthesized beam with natural weighting.
Paper: ALMA Images the Eccentric HD 53143 Debris Disk
Authors: Meredith A. MacGregor, Spencer A. Hurt, Christopher C. Stark, Ward S. Howard, Alycia J. Weinberger, Bin Ren, Glenn Schneider, Elodie Choquet, Dmitri Mawet
Figure caption: The first millimeter image of HD 53143 taken with ALMA shows an asymmetric distribution of dust with a bright point source in the center coincident with the star. Contours are in steps of 3σ (3× the rms noise of 5.6 μJy beam−1). The gray ellipse in the lower-left corner indicates the 1.″13 × 0.″92 synthesized beam with natural weighting.
Paper: A Green Pea Starburst Arising from a Galaxy–Galaxy Merger
Authors: S. Purkayastha, N. Kanekar, J. N. Chengalur, S. Malhotra, J. Rhoads, T. Ghosh
Figure caption: The HI velocity field of GP J0213+0056 at an angular resolution of 12″ × 12″; the velocity is relative to z = 0.03995, halfway between the redshifts of GP J0213+0056 and G1. A velocity gradient is visible in the image, with the gas to the south and east moving toward us and the gas to the north and southwest moving away from us.
Paper: A Green Pea Starburst Arising from a Galaxy–Galaxy Merger
Authors: S. Purkayastha, N. Kanekar, J. N. Chengalur, S. Malhotra, J. Rhoads, T. Ghosh
Figure caption: (a) The SDSS spectrum of the galaxy G1, showing strong Hα, [OIII]λ5007 Å, and [OII]λ3727 Å emission. (b) The SDSS spectrum of GP J0213+0056 showing the extreme optical emission lines.
Paper: A Green Pea Starburst Arising from a Galaxy–Galaxy Merger
Authors: S. Purkayastha, N. Kanekar, J. N. Chengalur, S. Malhotra, J. Rhoads, T. Ghosh
Figure caption: GMRT HI 21 cm emission spectrum from GP J0213+0056, from the 37″ × 32″ resolution spectral cube. The spectrum has a velocity resolution of 10 km s−1.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Top-right panel: physical evolution in model MC. Other panels: abundance ranges for selected species with respect to H nuclei as functions of time in 10,000 different simulation runs, where the f value for each species was randomly varied (gray shaded area). The purple shaded area indicates abundance ranges in another 10,000 simulations, where the f for several species was fixed to be 0.45 (see the main text). Red solid, dashed, and dotted lines show the results of models where f was set to 0.2, 0.45, and 0.7, respectively, for all species except atomic H, H2, and CO.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: TEM images of CH4 deposited on c-ASW at different substrate temperatures. The corresponding electron diffraction patterns are shown in some panels. a-CH4 indicates amorphous CH4. The contrast in the TEM images increases from bright (gray) to dark (black) with increasing atomic number (scattering contrast). The contrast for crystalline samples is much stronger (darker) than that for the amorphous sample because of diffraction contrast. Broken lines represent critical temperatures for the formation of crystalline or amorphous solids.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Mean diffusion distance X for the deposited molecules on c-ASW as a function of the inverse of the substrate temperature. Gray dashed lines represent least-squares fits.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption:  E des vs. E sd for various molecules on c-ASW. The crosses inside each symbol indicate error bars. Gray lines indicate f = 0.2, 0.4, 0.6, or 0.8. The filled blue circle indicates CO on p-ASW for comparisons.
Paper: An Isolated Mass-gap Black Hole or Neutron Star Detected with Astrometric Microlensing
Authors: Casey Y. Lam, Jessica R. Lu, Andrzej Udalski, Ian Bond, David P. Bennett, Jan Skowron, Przemek Mróz, Radek Poleski, Takahiro Sumi, Michał K. Szymański, Szymon Kozłowski, Paweł Pietrukowicz, Igor Soszyński, Krzysztof Ulaczyk, Łukasz Wyrzykowski, Shota Miyazaki, Daisuke Suzuki, Naoki Koshimoto, Nicholas J. Rattenbury, Matthew W. Hosek, Fumio Abe, Richard Barry, Aparna Bhattacharya, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Sho Matsumoto, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Yuki Satoh, Stela Ishitani Silva, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Natasha S. Abrams, Shrihan Agarwal, Sam Rose, Sean K. Terry
Figure caption: Microlensing parallax π  E  vs. Einstein crossing time t  E  (left) and maximum astrometric shift δ  c,max (right). Points are from the PopSyCLE simulation. Contours are 1σ−2σ−3σ (39.3–86.5–98.9%) credible regions from the microlensing model fits to the five BH candidates. There are two fits for OB110462 (DW and EW; see Supplemental Section 5.3 of Lam et al. 2022 for details). The OB110462 DW solution has a smaller π  E  than the OB110462 EW solution and has a correspondingly more massive lens mass. Both solutions fall solidly in the NS–BH mass gap, making OB110462 the best BH candidate. MB09260 and OB110310 are most likely white dwarfs or NSs, although due to the uncertainty in π  E  and δ  c,max higher- and lower-mass lenses cannot be definitively ruled out. OB110037 and MB10364 are not BHs as they have very large π  E , as well as relatively short t  E  and small δ  c,max. MB09260, MB10364, OB110037, and OB110310 are discussed in detail in the Supplemental paper.
Paper: A Dynamical Model of the M101/NGC 5474 Encounter
Authors: Sean T. Linden, J. Christopher Mihos
Figure caption: Position–velocity plots of the M101–NGC 5474 interaction model observed at the present time. The top left panel shows the sky view, while the top-right and lower-left panels show the model velocities collapsed along the X and Y coordinates, respectively. Radial velocity is measured relative to M101's systemic velocity. The lower-right panel shows a deep B-band image of M101 from Mihos et al. (2013), with companion galaxies and tidal features marked.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 4, but for selected complex organic molecules in model PE. The horizontal axes represent t final − t, where t final represents the final time of the simulation and t = 0 corresponds to the onset of the collapse to highlight the rapid changes in the physical conditions near and at the final stage.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 5, but for simple species and species relevant to warm carbon-chain chemistry.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 5, but for the corresponding gas-phase molecules.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 5, but for additional complex organic molecules in the gas phase and on dust grains.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 1, but for H2S.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 1, but for CH3OH.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 1, but for CH3CN.
Paper: Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Authors: Kenji Furuya, Tetsuya Hama, Yasuhiro Oba, Akira Kouchi, Naoki Watanabe, Yuri Aikawa
Figure caption: Similar to Figure 1, but for OCS.
Paper: An Isolated Mass-gap Black Hole or Neutron Star Detected with Astrometric Microlensing
Authors: Casey Y. Lam, Jessica R. Lu, Andrzej Udalski, Ian Bond, David P. Bennett, Jan Skowron, Przemek Mróz, Radek Poleski, Takahiro Sumi, Michał K. Szymański, Szymon Kozłowski, Paweł Pietrukowicz, Igor Soszyński, Krzysztof Ulaczyk, Łukasz Wyrzykowski, Shota Miyazaki, Daisuke Suzuki, Naoki Koshimoto, Nicholas J. Rattenbury, Matthew W. Hosek, Fumio Abe, Richard Barry, Aparna Bhattacharya, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Sho Matsumoto, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Yuki Satoh, Stela Ishitani Silva, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Natasha S. Abrams, Shrihan Agarwal, Sam Rose, Sean K. Terry
Figure caption: On-sky lensing geometry of OB110462 showing the resolved motion of the lens and source, as inferred from the default-weight (DW) model (left) and the equal-weight (EW) model (right); see Supplemental Section 5.3 of Lam et al. (2022) for details about the different models. The Einstein ring is shown as a gray circle of radius θ  E . The solid red line shows the trajectory of the source, while the dashed black line shows the trajectory of the lens. Note that the red line shows the unlensed position or the source and not the centroid of the source's lensed images. The dots on top of the trajectories are spaced at intervals of 100 days. The red and black arrows indicate the proper motion of the source and lens, respectively. The tail of the arrow is at the location of the source and lens at time t 0; the length of the arrows is proportional to the magnitude of the source and lens proper motions.
Paper: An Isolated Mass-gap Black Hole or Neutron Star Detected with Astrometric Microlensing
Authors: Casey Y. Lam, Jessica R. Lu, Andrzej Udalski, Ian Bond, David P. Bennett, Jan Skowron, Przemek Mróz, Radek Poleski, Takahiro Sumi, Michał K. Szymański, Szymon Kozłowski, Paweł Pietrukowicz, Igor Soszyński, Krzysztof Ulaczyk, Łukasz Wyrzykowski, Shota Miyazaki, Daisuke Suzuki, Naoki Koshimoto, Nicholas J. Rattenbury, Matthew W. Hosek, Fumio Abe, Richard Barry, Aparna Bhattacharya, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Sho Matsumoto, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Yuki Satoh, Stela Ishitani Silva, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Natasha S. Abrams, Shrihan Agarwal, Sam Rose, Sean K. Terry
Figure caption: OB110462 astrometry, using the DW (solid) and EW (dashed) likelihoods. Left column, top to bottom: R.A. (Δα*) vs. time with source's unlensed motion subtracted; residuals to the maximum likelihood (MLE) model for Δα* vs. time fit. HST F814W astrometry data are shown in red; HST F606W astrometry data are shown in blue. The MLE model is shown in black. Middle column, top to bottom: same as the left column, except decl. (Δδ) instead of Δα*. Right panel: astrometry as seen on sky, in the barycentric frame. OB110462 shows a strong >1 mas, nonlinear astrometric microlensing signal.
Paper: An Isolated Mass-gap Black Hole or Neutron Star Detected with Astrometric Microlensing
Authors: Casey Y. Lam, Jessica R. Lu, Andrzej Udalski, Ian Bond, David P. Bennett, Jan Skowron, Przemek Mróz, Radek Poleski, Takahiro Sumi, Michał K. Szymański, Szymon Kozłowski, Paweł Pietrukowicz, Igor Soszyński, Krzysztof Ulaczyk, Łukasz Wyrzykowski, Shota Miyazaki, Daisuke Suzuki, Naoki Koshimoto, Nicholas J. Rattenbury, Matthew W. Hosek, Fumio Abe, Richard Barry, Aparna Bhattacharya, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Sho Matsumoto, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Yuki Satoh, Stela Ishitani Silva, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Natasha S. Abrams, Shrihan Agarwal, Sam Rose, Sean K. Terry
Figure caption: HST image (inset) and photometric light curve (top) for OB110462. In the image, OB110462 is circled in black and is shown in its unmagnified state. Observations are shown as points in blue (OGLE), red, and black (HST). The default-weighted (DW; solid) and equal-weighted (EW; dashed) maximum likelihood models are shown along with their corresponding residuals (DW: middle, EW: bottom). See Supplemental Section 5.3 of Lam et al. (2022) for more details on the two different models.
Paper: An Isolated Mass-gap Black Hole or Neutron Star Detected with Astrometric Microlensing
Authors: Casey Y. Lam, Jessica R. Lu, Andrzej Udalski, Ian Bond, David P. Bennett, Jan Skowron, Przemek Mróz, Radek Poleski, Takahiro Sumi, Michał K. Szymański, Szymon Kozłowski, Paweł Pietrukowicz, Igor Soszyński, Krzysztof Ulaczyk, Łukasz Wyrzykowski, Shota Miyazaki, Daisuke Suzuki, Naoki Koshimoto, Nicholas J. Rattenbury, Matthew W. Hosek, Fumio Abe, Richard Barry, Aparna Bhattacharya, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Sho Matsumoto, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Yuki Satoh, Stela Ishitani Silva, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Natasha S. Abrams, Shrihan Agarwal, Sam Rose, Sean K. Terry
Figure caption: Lens-mass posterior probabilities for the five microlensing BH candidates. Two mass posteriors are shown for OB110462, one for each model (DW and EW). See Supplemental Section 5.3 of Lam et al. (2022) for details on the two models. MB09260, MB10364, OB110037, and OB110310 are discussed in detail in the Supplemental paper.
Paper: An Isolated Mass-gap Black Hole or Neutron Star Detected with Astrometric Microlensing
Authors: Casey Y. Lam, Jessica R. Lu, Andrzej Udalski, Ian Bond, David P. Bennett, Jan Skowron, Przemek Mróz, Radek Poleski, Takahiro Sumi, Michał K. Szymański, Szymon Kozłowski, Paweł Pietrukowicz, Igor Soszyński, Krzysztof Ulaczyk, Łukasz Wyrzykowski, Shota Miyazaki, Daisuke Suzuki, Naoki Koshimoto, Nicholas J. Rattenbury, Matthew W. Hosek, Fumio Abe, Richard Barry, Aparna Bhattacharya, Akihiko Fukui, Hirosane Fujii, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Sho Matsumoto, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Arisa Okamura, Yuki Satoh, Stela Ishitani Silva, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Natasha S. Abrams, Shrihan Agarwal, Sam Rose, Sean K. Terry
Figure caption: Probability of detecting N BHs as calculated from the PopSyCLE simulation. Two predictions are shown, depending on the likelihood used for OB110462 (DW or EW)). See Supplemental Section 5.3 of Lam et al. (2022) for details on the two models. Our observation of 0 or 1 BHs is consistent with either OB110462 model prediction.