adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: Comparison of IRX, β UV, and M star properties with other high-z star-forming galaxies constrained from recent large ALMA surveys of ASPECS at z ∼ 2–3 (Walter et al. 2016), ALPINE at z ∼ 4–6 (green square; Le Fèvre et al. 2020), and REBELS z ∼ 7 (blue square; Bouwens et al. 2022). Note that ASPECS and ALPINE results are taken from the stacking results (Bouwens et al. 2020; Fudamoto et al. 2020), while REBELS results are taken from the individual results based on detection (e.g., Inami et al. 2022; Sommovigo et al. 2022). The red symbols represent the UV-bright (M UV ≈ [−24: −21]) high-z candidates at z ∼ 11–17 constrained from our optical to millimeter SED analysis. The solid and light red symbols are estimated from the T d–z relation of Sommovigo et al. (2022) and a constant assumption of T d = 50 K, respectively. The upper limits are placed at the 2σ level, while we place the 2.6σ upper limit for GHZ1/GLz11 that has been reported to have a tentative (2.6σ) continuum emission (Yoon et al. 2023). Left: IRX–β UV relation. The solid and dashed curves indicate the relations derived with the dust attenuation of SMC and Calzetti et al. (2000), respectively. The dotted curve shows the relation derived with the SMC dust attenuation and bluer intrinsic β UV. Middle and right: IRX–M star and M star–β UV relations from middle to right. The black shade shows the 1σ range of the best-fit relations at z ∼ 2–3 estimated in Bouwens et al. (2020). Although both UV-bright z ∼ 11–17 candidates and the REBELS sources dominate the bright-end of the UV LF and the similar M star range at these redshifts, the former is generally bluer and lower IRX.
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: Optical to millimeter SED of the z ∼ 11–17 candidates so far observed with ALMA. The red open squares and arrows indicate the observed flux densities and the 2σ upper limits, respectively. The blue curve is the best-fit SED with the optical to millimeter photometry, showing that the high-z solution is favored in all candidates. For comparison, the green and gray curves indicate the best-fit SEDs forced at z < 8 with and without the ALMA photometry. The lower-z IR-bright objects, implied from the gray curves, are ruled out by the new constraints from ALMA in all candidates. The ﹩{\rm{\Delta }}{\chi }_{\mathrm{pre}}^{2}﹩ and ﹩{\rm{\Delta }}{\chi }_{\mathrm{new}}^{2}﹩ values in the labels indicate the difference of the χ 2 values between the forced low-z and the best-fit high-z solutions without and with ALMA data, respectively. All candidates show ﹩{\rm{\Delta }}{\chi }_{\mathrm{new}}^{2}﹩ increased from ﹩{\rm{\Delta }}{\chi }_{\mathrm{pre}}^{2}﹩, indicating that their high-z solutions are much strengthened with the new ALMA photometry. The open circles and black crosses denote the predicted photometry from the SEDs in each filter and ALMA band.
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: ALMA Band 7 observation results. Top: ALMA 4″ × 4″ × cutout of the continuum at 866  μm (left), the velocity-integrated map for the 5.1σ line feature at around 338.7 GHz (middle), JWST/NIRCam F356W image (right). The dashed contours indicate the −2σ and −3σ levels, while the solid contours denote the 2σ, 3σ, 4σ, and 5σ levels. The red contours overlaid on the F356W image indicate the line intensity in the moment-0 map. The green ellipse shows the ALMA synthesized beam. Bottom: ALMA ∼24 GHz width spectrum (green) obtained from three frequency setups. The gray dashed line denotes the 1σ noise per channel. The gray shades show 120 MHz gaps between basedbands.
Paper: ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11–17: Blue Monsters or Low-z Red Interlopers?
Authors: Seiji Fujimoto, Steven L. Finkelstein, Denis Burgarella, Chris L. Carilli, Véronique Buat, Caitlin M. Casey, Laure Ciesla, Sandro Tacchella, Jorge A. Zavala, Gabriel Brammer, Yoshinobu Fudamoto, Masami Ouchi, Francesco Valentino, M. C. Cooper, Mark Dickinson, Maximilien Franco, Mauro Giavalisco, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Takashi Kojima, Rebecca L. Larson, E. J. Murphy, Casey Papovich, Pablo G. Pérez-González, Rachel S. Somerville, Ilsang Yoon, Stephen M. Wilkins, Hollis Akins, Ricardo O. Amorín, Pablo Arrabal Haro, Micaela B. Bagley, Katherine Chworowsky, Nikko J. Cleri, Olivia R. Cooper, Luca Costantin, Emanuele Daddi, Henry C. Ferguson, Norman A. Grogin, E. F. Jiménez-Andrade, Stéphanie Juneau, Allison Kirkpatrick, Dale D. Kocevski, Aurélien Le Bail, Arianna Long, Ray A. Lucas, Benjamin Magnelli, Jed McKinney, Caitlin Rose, Lise-Marie Seillé, Raymond C. Simons, Benjamin J. Weiner, L. Y. Aaron Yung
Figure caption: Distribution of the rest-frame EW([O III]+Hβ) for several quasar and galaxy populations that might attribute to the z ∼ 11–17 candidates: type II QSOs (Zakamska et al. 2003), dusty-reddened type I QSOs (Finnerty et al. 2020), and QGs with emission lines from AGNs (Forrest et al. 2020). The gray shaded region indicates the required EW([O III]+Hβ) range implied from the CIGALE modeling, showing the minimum to maximum range among the best-fit SEDs of S5-z17-1, GHZ1/GLz13, GHZ2/GLz11, and HD1 forced at z < 8. When the literature does not show the Hβ line measurement, we include the Hβ contribution by assuming the typical line ratio of [O III]/Hβ from Richardson et al. (2014).
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Dimensionless GW amplitude for NSs as a function of frequency as given in Tables 1 and 2 along with the sensitivity curves of various detectors. Here h = 0.0110297h 0 with χ = 3°.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Dimensionless GW amplitude for NSs as a function of frequency as given in Table 3 along with the sensitivity curves of various detectors. Here h = 0.0110297h 0 with χ = 3°.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Cartoon diagram of a magnetized rotating compact star with misalignment between the magnetic field and rotation axes.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Density isocontours of a uniformly rotating toroidally magnetized NS of mass M = 1.97 M ⊙ with ν = 500 Hz, ﹩{B}_{\max }=4.5\times {10}^{17}﹩ G, ME/GE  =  5.6 × 10−2, and KE/GE  =  2.3 × 10−2.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Magnetic field as a function of radius before and after magnetic field decay as given in Table 4 for toroidal fields.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Density isocontours of a uniformly rotating poloidally magnetized NS of mass M = 1.92 M ⊙ with ν = 50 Hz, ﹩{B}_{\max }=4.4\times {10}^{17}﹩ G, ME/GE = 2 × 10−2, and KE/GE = 2 × 10−4.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Maximum magnetic field as a function of time of a NS as given in Table 4 for toroidal fields.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption:  L  D  ≫ L GW: variations of ν, χ, L GW, and L  D  with time for B  P  = 1015 G, initial ν = 100 Hz, and χ = 3°, as given in Table 6. Red solid and blue dashed lines show the variations of ν and χ, respectively.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: For toroidally dominated NSs, variations of ν, χ, and L GW as functions of time for ﹩{B}_{\max }=1.4\times {10}^{17}﹩ G, initial ν = 500 Hz, and χ = 3°, as given in Table 7. Red solid and blue dashed lines in the upper panel show the variations of ν and χ, respectively.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption:  L GW ≫ L  D : variations of ν, χ, L GW, and L  D  with time for B  P  = 1012 G, initial ν = 100 Hz, and χ = 3°, as given in Table 6. Red solid and blue dashed lines show the variations of ν and χ, respectively.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Dimensionless GW amplitude for NSs before and after ν and χ decay along with the sensitivity curve of various detectors for ﹩{B}_{\max }=1.4\times {10}^{17}﹩ G, initial ν = 500 Hz, and χ = 3°, as given in Table 8.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Dimensionless GW amplitude as a function of time due to decays of Ω and χ (and thus h) for ﹩{B}_{\max }=1.4\times {10}^{17}﹩ G, initial ν = 500 Hz, and χ = 3°, as given in Table 8.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Dimensionless GW amplitude for NSs before and after magnetic field decay as given in Table 4 for toroidal fields. Here h = 0.0110297h 0 with χ = 3°.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Dimensionless GW amplitude for NSs before and after magnetic field decay as given in Table 5 for poloidal fields. Here h = 0.0110297h 0 with χ = 3°.
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Variations of ν and L GW as functions of time for different rotation and keeping the magnetic field the same (﹩{B}_{\max }=9\times {10}^{16}﹩ G).
Paper: Detection Possibility of Continuous Gravitational Waves from Rotating Magnetized Neutron Stars
Authors: Mayusree Das, Banibrata Mukhopadhyay
Figure caption: Magnetic field as a function of radius before and after magnetic field decay as given in Table 5 for poloidal fields.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The evolution of SN bolometric luminosity and the temperature on the photosphere in case A. Areas with different color shading show the contribution from different heating mechanisms to the bolometric luminosity. The black and red solid lines represent the temperature of regions I and II, respectively. In our calculation, d = 1013 cm, M ej = 2 M ⊙, ﹩{E}_{\mathrm{sn}}={10}^{51}﹩ erg, ﹩{v}_{\min }=50\ \mathrm{km}\ {{\rm{s}}}^{-1}﹩, ﹩{v}_{\max }=0.1c﹩, M BH = 20 M ⊙, and M Ni = 0.5 M ⊙ are adopted.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: An illustration of a special SN physical model. The companion BH injects energy into the SN ejecta through accretion feedback. The radiation from the BP outflow divides the ejecta photosphere into region I and region II along the angle θ BP with the equatorial plane, where the energy from region I contains contributions from both the radioactive element decay and the BP outflow.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The emergent spectra of case A (left panel) and case B (right panel) in the LOS direction θ los = 90°, where a distance of 10 pc is adopted. The panels from top to bottom show three angular configurations for area I: θ BP = 15°, θ BP = 45°, and θ BP = 75°, respectively. Each panel shows the emergent spectra on days 25, 39, 50, 60, 80, and 100 after the SN explosion with different-colored dotted–dashed lines.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The emergent spectra of case A (left panel) and case B (right panel) with the same angular configuration (θ BP = 45°) for area I, where a distance of 10 pc is adopted. The panels from top to bottom show the emergent spectra on days 39, 60, and 80 after the SN explosion, respectively. Each panel shows the emergent spectrum in the LOS direction θ los for 0°, 15°, 30°, 45°, 60°, and 90°, respectively, using different-colored dotted–dashed lines.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: The continuum polarization degree observed on day 39 after the SN explosion in case A at different viewing angles θ los, where the color of the curve represents the continuum polarization degree for different θ BP of region I. The Stokes vector U is 0 owing to symmetry.
Paper: Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems
Authors: Xudong Wen, He Gao, Shunke Ai, Liang-Duan Liu, Jin-Ping Zhu, Wei-Hua Lei
Figure caption: Same as Figure 2, but for case B. A value of d = 3 × 1013 cm is adopted, while other model parameters remain unchanged.
Paper: TESS Photometric Variability of Young Brown Dwarfs in the Taurus Star-forming Region
Authors: Rajib Kumbhakar, Soumen Mondal, Samrat Ghosh, Diya Ram
Figure caption: Flare events for MHO 4 in sector 44 (top left), CT 11 (top right), and 2M J0444+2512 (below).
Paper: Secondary Proton Beam Instability in a Turbulent Solar Wind at 50 R ⊙ 
Authors: S. A. Markovskii, Bernard J. Vasquez
Figure caption: Distribution functions F of the relative rms amplitude A for (a) the entire data set (black dotted line) and (b) a subset of the intervals in which V A0/V SW < 0.25. The distributions are normalized to the respective total number of intervals.
Paper: Secondary Proton Beam Instability in a Turbulent Solar Wind at 50 R ⊙ 
Authors: S. A. Markovskii, Bernard J. Vasquez
Figure caption: Sample magnetic power P  B  spectra with a break at the kinetic scales. The red dashed line is a least-squares power-law fit. The green dashed line marks the reference scale at which the intensity of the fluctuations was evaluated for this interval. The spectrum was obtained from the solar wind interval between 7.71479 × 106 and 7.71659 × 106 s in 2019.
Paper: Secondary Proton Beam Instability in a Turbulent Solar Wind at 50 R ⊙ 
Authors: S. A. Markovskii, Bernard J. Vasquez
Figure caption: Magnetic power spectrum calculated from the interval between 2018 November 1 06:00 and 2018 November 2 05:00, when the spacecraft was between 0.22 and 0.24 au during encounter 1. The magenta line is a reference power-law spectrum that flattens from a slope of −5/3 to −1 at ν = 5.6 × 10−4 Hz.
Paper: Secondary Proton Beam Instability in a Turbulent Solar Wind at 50 R ⊙ 
Authors: S. A. Markovskii, Bernard J. Vasquez
Figure caption: Same as Figure 1 but showing a sample with a power elevation. The spectrum was obtained from the solar wind interval between 2.06334 × 107 and 2.06352 × 107 s in 2019.
Paper: Secondary Proton Beam Instability in a Turbulent Solar Wind at 50 R ⊙ 
Authors: S. A. Markovskii, Bernard J. Vasquez
Figure caption: The 2D wavenumber spectrum S of the magnetic field fluctuations, normalized to ﹩{B}_{0}^{2},﹩ in the case of coexisting turbulence and instability near the saturation time of the instability (﹩t=600{{\rm{\Omega }}}_{p}^{-1}﹩).
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Comparison of the bias correction measured in this work to those in Lam et al. (2022b) and Sahu et al. (2022). The left (right) column shows the bias in F814W (F606W). The top (bottom) row shows the astrometric (photometric) bias, where the bias is defined as the recovered minus injected value. The biases measured in this work performed using injection-and-recovery tests with hst1pass are shown in black circles. The biases measured in Lam et al. (2022b) performed using injection-and-recovery tests with ks2 are shown as light blue squares. The astrometric bias reported by Sahu et al. (2022) performing PSF subtraction is shown as the dashed gray line. Sahu et al. (2022) report a single value for the astrometric bias; we show this same value in both the F814W and F606W panels.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Comparison of the HST astrometry derived by Lam et al. (2022a, 2022b), Sahu et al. (2022), and this work. The top (bottom) row shows the astrometry in R.A. (decl.) vs. time, with the source proper motion reported in Sahu et al. (2022) (R.A. decl.) = (−2.263, −3.597) mas yr−1 subtracted in order to compare the astrometric deflections more easily. The left (right) column compares the astrometry in Sahu et al. (2022) to Lam et al. (2022a, 2022b) (this work). The positions of Sahu et al. (2022; black squares) are the average of all F814W and F606W measurements. Lam et al. (2022a, 2022b) and this work keep the F814W and F606W sets separate; the F814W (F606W) positions are shown in red (blue) circles.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Comparison of the measured positions and magnitudes using the new hst1pass and tabular CTE correction vs. the old hst1pass and pixel-based CTE correction. These comparisons are performed on a single exposure, i.e., on the individual flc.xym or flt.XYM files. The y-axis is the difference between the new tabular and old pixel-based correction for the detector’s x-position, y-position, and instrumental magnitude. The top (bottom) plot shows the differences as a function of the detector’s y-position (instrumental magnitude).
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Comparison of the color differences in OB110462 astrometry. The top row shows the difference in F606W and F814W position for OB110462 vs. time from Lam et al. (2022a, 2022b). The bias correction calculated in Lam et al. (2022b) has been applied, but the constant positional offset between F814W and F606W is not included. The dashed line is the “empirical color offset” applied by Lam et al. (2022b) to get the data in the two filters to agree better with each other. There is a significant difference between the positions measured between the two filters, especially in R.A. The bottom row shows the difference in the F606W and F814W positions for OB110462 vs. time as derived in this work. The color difference has largely disappeared from the R.A. and also slightly decreased in decl.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Microlensing parallax π E vs. Einstein crossing time t E (left) and maximum astrometric shift ﹩{\delta }_{{\rm{c}},\max }﹩ (right) of five BH microlensing candidates analyzed in Lam et al. (2022a, 2022b). It is the same as Figure 6 of Lam et al. (2022a), except the contours for OB110462 have been updated with the values inferred in this work. MB09260, MB10364, OB110037, and OB110310 are low-mass (<4 M ⊙) lenses and not BHs. The points are simulated microlensing events from the PopSyCLE microlensing simulation (Lam et al. 2020). Compared to the simulated BH population, OB110462 has a relatively large astrometric shift, large microlensing parallax, and long Einstein crossing time.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: OB110462 in the context of the observed Galactic BH population. Left: dynamically confirmed BHs, coded by their type (isolated, detached field binary, detached globular cluster binary, LMXB, and high-mass X-ray binary). Right: histogram of Galactic BH mass measurements, coded by type. Note that not all BHs in the left panel are included in the right panel, as some only have lower limits on the mass. Note the histogram does not account for the uncertainties on the measurements.