adsabs/AstroCLIMB huggingface dataset:
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: Linear-scale density map showing, for each galaxy, the standard deviations of the broad emission line spaxel FWHMs (normalized by the mean FWHM; σFWHM/﹩\overline{{\rm{FWHM}}}﹩) against the standard deviations of the spaxel spatial positions (quadrature sum of the standard deviation of the spaxels in the X- and Y-dimensions) in units of the MaNGA spatial resolution (σspax/2﹩\mathop{.}\limits^{^{\prime\prime} }﹩5) for Hα (left) and Hβ (right) emission line detections. Only sources with more than one broad emission line spaxel are shown. The distributions of σFWHM/﹩\overline{{\rm{FWHM}}}﹩ and σspax/2﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 (normalized to a sum of unity) are shown along the right and top axes, respectively, for Hα (solid) and Hβ (dashed). The concentration of abscissa values at σspax/2﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 = 0.1 is due to sources with two adjacent broad emission line spaxels. Of the σFWHM/﹩\overline{{\rm{FWHM}}}﹩ values, 100% are <1 for both Hα and Hβ detections. Of the σspax values, 99%, 96% (Hα, Hβ detections) are <2 × 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩5. These distributions show that the line widths and positions of the broad emission line detections in each galaxy are consistent and likely originate from a single source.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: Angular offsets of Hα (left) and Hβ (right) BLRs from the host galaxy centroids (ΔΘ) against the source extents (σspax; defined in Figure 1). The dotted gray line denotes the approximate MaNGA absolute astrometric uncertainty of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩1. The dashed black lines denote the threshold of ΔΘ > 3 × σspax, and the solid black line denotes the additional uniform offset minimum of ΔΘ > 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 (Section 2.2). The parent sample is indicated by the linear-scale density map, while sources that pass the offset criteria are shown as red stars. The concentrations at σspax = 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩25 and 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 are due to sources with two adjacent spaxels and those with only one spaxel (for which σspax ≔ 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩5, i.e., the extent of one spaxel), respectively.
Paper: The Dust Echo Emission of Fast Blue Optical Transients and Application to the Near-infrared Excess of AT 2018cow
Authors: Jing-Yao Li, 京谣 李, Yun-Wei Yu, 云伟 俞, Liang-Duan Liu, 良端 刘, Ming-Yan Xiao, 明燕 肖
Figure caption: The dust parameters (solid circles) for the spectral fittings of AT 2018cow for seven different times as shown in Figure 6, where the fittings are implemented without considering the physical connection between the spectra. For comparison, the corresponding parameter values obtained in our evolutionary dust echo model are shown by the red lines or bands, where the bands indicate that the parameters are actually distributed in a range rather than being fixed values. The dust evaporation occurs in the first day where the dust mass decreases a bit.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: Best fits to the (continuum-subtracted) spectral regions (in the host galaxy rest frame) where broad emission lines are detected. For clarity, each spectrum has been normalized by the peak flux. The narrow and broad line components are shown in orange and purple, respectively, and the model sum is shown in red. The uncertainty in the continuum-subtracted spectrum is denoted by the gray-shaded region, and the residuals are shown at the bottom. Sorted by R.A., these are the first two offset BLR sources in the sample. The remainder are shown and discussed in the Appendix (Figure 10).
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: BLR FWHM (maximum value among all spaxels in each source) against projected physical offset from the host galaxy centroid (ΔS) for the final sample of spatially offset BLR candidates with (orange squares) and without (magenta circles) optical counterpart detections (Section 3). The distributions of FWHM and ΔS (each normalized to a sum of unity) are shown along the right and top axes, respectively, for the subsets with (orange, dashed) and without (magenta, solid) optical counterparts, and their median values are indicated by straight lines. The distributions of FWHM and ΔS are typical of AGN BLRs and late-stage galaxy mergers, respectively.
Paper: The Dust Echo Emission of Fast Blue Optical Transients and Application to the Near-infrared Excess of AT 2018cow
Authors: Jing-Yao Li, 京谣 李, Yun-Wei Yu, 云伟 俞, Liang-Duan Liu, 良端 刘, Ming-Yan Xiao, 明燕 肖
Figure caption: Independent fittings for the spectra of AT 2018cow at seven epochs (dashed lines), in comparison with our fittings (solid lines) with the evolutionary dust echo model.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: AGN BPT spaxel fractions of the BLRs (fA,BL) against those of the host galaxy nuclei (fA,Nuc) for AGN selections based on the [N II] (left) and [S II] (right) BPT diagrams for the offset AGN without optical image counterpart detections (i.e., the ejected AGN candidates; magenta circles). See Section 4 for details on the AGN spaxel fraction calculations. Since sources cluster at fA,BL = fA,Nuc = 0, marker sizes indicate the number of sources: small and large circles indicate 1 and 5 sources, respectively (left panel), and 1 and 4 sources, respectively (right panel). The distributions of fA,BL and fA,Nuc are shown along the right and top axes, respectively, normalized to a sum of unity. For comparison, the distributions for the offset AGN with optical image counterparts (i.e., likely infalling AGN; orange dashed) are also shown. The mean values are indicated with straight lines of corresponding color and style. The mean values of fA,BL are smallest for the ejected AGN candidates (consistent with the recoil/slingshot scenario). The mean values of fA,Nuc are also smaller for the ejected AGN candidates, which is more consistent with the recoil (as opposed to slingshot) scenario.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: Broad emission line luminosity (LBL; total value from all spaxels) against the magnitude of the projected velocity offset relative to the host galaxy systemic velocity (ΔV; flux-weighted average from all spaxels) for the central BLRs (linear-scale density map) and the subset of spatially offset BLRs with (orange squares) and without (magenta circles) optical image counterpart detections. The distributions of LBL and ΔV are shown along the right and top axes, respectively, for the offset BLRs with (orange dashed) and without (magenta solid) image counterpart detections and for the central BLRs (gray dotted). The mean ∣ΔV∣ values of the spatially offset samples show a bias toward larger values relative to the central sample (by 78%). For comparison, the simulated distribution of recoiling MBH projected velocities from L. Blecha & A. Loeb (2008; BL08) is also shown (solid gray line), and the offset BLR mean values are consistent with it to within 41%.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: Broad emission line luminosities (LBL) against the optical image counterpart stellar masses (M⋆; orange squares) or upper limits (for those without counterpart detections; magenta circles and left-pointing arrows). The density map shows the central AGN sample from this work. The subset without counterpart detections has relatively large LBL/M⋆ ratios compared to central AGN, potentially due to merger-driven AGN enhancements and/or tidal stripping. Those without counterpart detections are also consistent with being ejected MBHs within faint hypercompact stellar systems.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption:                         Same as Figure 5 but for the full sample without optical image counterpart detections.
Paper: Recoiling Black Hole Candidates from Spatially Offset Broad Emission Lines in MaNGA
Authors: R. Scott Barrows, Julia M. Comerford, James Negus, Francisco Muller-Sanchez
Figure caption: Same as Figure 3 but for the remainder of the sample (sorted by R.A.).
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Pitch-angle distribution (PAD; blue dots) calculated from all pixels of the anisotropy map as a function of the cosine of the mapped pitch-angle to the LISM magnetic field. The orange dots are binned averages within a range of μ of a fixed width. The “×” symbols are smoothed binned averages using a Savitzky–Golay filter.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Comparison of the PAD (blue dots) with the output of the diffusion approximation using ﹩{D}_{\mu \mu }^{(S)}﹩.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Diffusion coefficient ﹩{D}_{\mu \mu }^{(S)}﹩ as a function of μ, fitted with a sinusoidal approximation.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Reciprocal of the derivative of the PAD, which shows the μ-dependence of the pitch-angle diffusion coefficient.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Top: anisotropy skymap from the Tibet ASγ experiment. Middle: nonlinear model fit based on the normalized Liouville mapping of CR intensity, truncated to 7th order. Bottom: renormalized relative intensity skymap of Tibet anisotropy measurements.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Comparison of the model fits for Φ(μ) truncated to third degree with and without magnetic focusing.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Model fits to the observed PAD.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: MSE between model values and data as a function of the number of polynomials, calculated separately for training (fitting) and testing data. Error bars are the standard errors in the means from all permutations of data folds.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Renormalized normalization factors constructed from ﹩{\bar{I}}_{\phi }(\theta )﹩ so that the relative intensity is averaged to 1 over the field of view.
Paper: Extended and Compact Ortho-H2D+ Structures Close to the Moment of Star Formation: Evidence from ALMA-ACA Observations in Taurus
Authors: Kazuki Tokuda, Kenji Furuya, Naofumi Fukaya, Kengo Tachihara, Ken'ichi Tatematsu, Shingo Nozaki, Nami Sakai, Yuri Aikawa, Kazuya Saigo, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Spatial distribution and spectra of the 0.83 mm continuum and ortho-H2D+(11,0–11,1) in L1544. (a) The color-scale image shows the 0.83 mm continuum obtained with the 7 m array. The contours represent the continuum emission at levels of 3σ, 5σ, and 7σ (1σ = 0.78 mJy beam−1). The synthesized beam size is shown in the bottom-left corner. (b) The color-scale image shows the integrated intensity of H2D+ over the velocity range of 7.0–7.5 km s−1 obtained with the 7 m array. The contours and the ellipse in the bottom-left corner are the same as those in panel (a). (c) The color scale shows the integrated intensity of H2D+ over the velocity range of 6.8–7.8 km s−1 obtained with the TP array. The beam size of the TP array, 17﹩\mathop{.}\limits^{^{\prime\prime} }﹩5, is shown in the bottom-left corner. The contours are the same as those in panel (a). (d) The yellow, magenta, and blue spectra represent the H2D+ spectra obtained with the 7 m array, the 7 m array averaged over a region corresponding to the TP beam size, and the TP array, respectively. The extraction regions are indicated by dashed circles in the corresponding colors in panels (b) and (c).
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Legendre polynomial amplitudes for the models. The orange dots correspond to the analytical weak-focusing and isotropic scattering model with Φ(μ) truncated to third degree. The black crosses correspond to the numerical weak-focusing and anisotropic scattering model, once again with Φ(μ) truncated to third degree. The blue dots correspond to the output of the 7th-order Legendre series produced by the Liouville mapping method. The green dots correspond to the 13th-order Legendre series in N. D. Maalal & M. Zhang (2024). The black dots correspond to the anisotropic diffusion approximation model.
Paper: Extended and Compact Ortho-H2D+ Structures Close to the Moment of Star Formation: Evidence from ALMA-ACA Observations in Taurus
Authors: Kazuki Tokuda, Kenji Furuya, Naofumi Fukaya, Kengo Tachihara, Ken'ichi Tatematsu, Shingo Nozaki, Nami Sakai, Yuri Aikawa, Kazuya Saigo, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Same as those in Figure 1 but for MC 35 mm. The velocity ranges integrated for the H2D+ data cube are 5.8–5.9 km s−1 in panel (b) and 5.5–6.5 km s−1 in panel (c). In panel (d), the spectrum from the 7 m array (orange) was extracted by averaging over a smaller region centered on the emission peak in panel (b), in contrast to the broader areas used for the other two sources.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Interstellar power spectra derived from the models. The y-axis displays a logarithmic scale. The orange stars correspond to the analytical weak-focusing and isotropic scattering model with Φ(μ) truncated to third degree. The red stars correspond to the numerical weak-focusing and anisotropic scattering model, once again with Φ(μ) truncated to third degree. The black stars correspond to the anisotropic diffusion approximation model. The green stars correspond to the output of the 13th-order Legendre series in N. D. Maalal & M. Zhang (2024). The blue stars correspond to the output of the 7th-order Legendre series produced by the Liouville mapping method.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Comparing approximations to the exponential integral function.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Comparing the output of the symmetrized anisotropic pitch-angle diffusion model to the output of the isotropic diffusion model, both with Φ(μ) truncated to third degree. The green dots correspond to the “×” signs in Figure 7.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Plot comparing the best-fit curve (labeled T0 = 0) and the curves corresponding to different T0 values. All three curves are for Φ(μ) truncated to third degree.
Paper: Pitch-angle Focusing and Scattering of TeV Galactic Cosmic Rays Propagating in Local Interstellar Magnetic Fields
Authors: N. D. Maalal, M. Zhang
Figure caption: Legendre polynomial amplitudes derived from the analytical weak-focusing and isotropic diffusion model, with various truncations of Φ(μ), as shown in the legend.
Paper: Extended and Compact Ortho-H2D+ Structures Close to the Moment of Star Formation: Evidence from ALMA-ACA Observations in Taurus
Authors: Kazuki Tokuda, Kenji Furuya, Naofumi Fukaya, Kengo Tachihara, Ken'ichi Tatematsu, Shingo Nozaki, Nami Sakai, Yuri Aikawa, Kazuya Saigo, Toshikazu Onishi, Masahiro N. Machida
Figure caption: (a) H2 density and (b) temperature profiles adapted from H. Masunaga & S.-i. Inutsuka (2000). The x-axis represents the radial offset in arcseconds assuming the typical distance to the Taurus molecular cloud (D ∼ 140 pc). (c) Radial intensity (peak brightness temperature) profiles of ortho-H2D+ derived from the first core and prestellar core models. The green dotted line shows half of the beam size, 2″, with the 7 m array. (d) Radial profiles of the fractional abundance of ortho-H2D+ relative to H2 for the first core and prestellar core models. (e) The normalized radial intensity profile of ortho-H2D+ and ﹩{N}_{{{\rm{H}}}_{2}}﹩ from the prestellar core model.
Paper: Extended and Compact Ortho-H2D+ Structures Close to the Moment of Star Formation: Evidence from ALMA-ACA Observations in Taurus
Authors: Kazuki Tokuda, Kenji Furuya, Naofumi Fukaya, Kengo Tachihara, Ken'ichi Tatematsu, Shingo Nozaki, Nami Sakai, Yuri Aikawa, Kazuya Saigo, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Same as those in Figure 1 but for MC 27. The velocity ranges integrated for the H2D+ data cube are 6.0–7.0 km s−1 in panels (b) and (c).
Paper: Stringent Constraints on the Nuclear Matter Equation of State from Heavy Nuclei and Neutron Star Properties with a Multi-iteration Bayesian Statistical Analysis
Authors: Xue-Ying Jing, Jian-Min Dong
Figure caption: Flowchart of the parameter estimation based on a multi-iteration Bayesian statistical method. The multi-iteration procedure is performed, aiming at eliminating the dependence of the posterior probability distribution on the initial sampling. After the convergence is achieved, the ultimate EoS is obtained.
Paper: Stringent Constraints on the Nuclear Matter Equation of State from Heavy Nuclei and Neutron Star Properties with a Multi-iteration Bayesian Statistical Analysis
Authors: Xue-Ying Jing, Jian-Min Dong
Figure caption: Posterior probability distribution functions of the six EoS parameters: K0, J0, Esym(ρ0), L, Ksym, and Jsym. The sky-blue curve corresponds the constraint [asym], the orange curve represents [asym] + [DUrca], and the blue curve shows the result with the full constraint set [asym] + [DUrca] + [L − asym]. The shaded regions denote the 68% confidence intervals, and the red dashed lines indicate the most probable values.
Paper: Stringent Constraints on the Nuclear Matter Equation of State from Heavy Nuclei and Neutron Star Properties with a Multi-iteration Bayesian Statistical Analysis
Authors: Xue-Ying Jing, Jian-Min Dong
Figure caption: (Upper panel) EoS of symmetric nuclear matter (i.e., energy per particle vs. density) and (lower panel) the density-dependent symmetry energy. The yellow, green, and blue shaded areas are based on [asym], [asym] + [DUrca], and [asym] + [DUrca] + [L − asym] constraints, respectively. The dashed line shows the most probable value obtained from the full set of constraints, which are given by E0(ρ) = −0.968 – 189.691ρ + 621.332ρ2 − 118.951ρ3 and Esym(ρ) = 2.174 + 288.015ρ − 798.814ρ2 + 994.481ρ3 for ρ > ρ0/2.
Paper: X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 13+1
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Herman L. Marshall
Figure caption: Upper panel: IXPE (2–8 keV) light curve of GX 13+1. Lower Panel: NICER (0.5–10 keV) light curve of GX 13+1. Time bins of 150 s (IXPE) and 8 s (NICER) are used.
Paper: X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 13+1
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Herman L. Marshall
Figure caption: Model fitted joint spectra of GX 13+1 as observed by IXPE DU1 (spring green), IXPE DU2 (green yellow), IXPE DU3 (dark green), and NICER (magenta) during the dip state (left) and nondip state (right). The spectra are fitted with the tbnew*(diskbb+bbodyrad+Gauss)*polconst*ionabs*ionabs*ionabs*ionabs*const model in the 2−10 keV energy band. The total model is shown with the solid black (NICER and IXPE), and the individual additive components diskbb, bbodyrad, and Gauss are shown with the dashed orange, dotted navy, and dashed–dotted crimson lines, respectively. The lower subpanel shows the residuals between the data and the best-fit model.
Paper: Stringent Constraints on the Nuclear Matter Equation of State from Heavy Nuclei and Neutron Star Properties with a Multi-iteration Bayesian Statistical Analysis
Authors: Xue-Ying Jing, Jian-Min Dong
Figure caption: Our constrained EoS compared with the theoretically calculated ones with various nuclear many-body approaches such as the APR EoS (red solid line; A. Akmal et al. 1998), the relativistic mean-field method (the other solid lines), the Skyrme–Hartree–Fock method (short dashed lines), the Brueckner–Hartree–Fock (blue double-dotted–dashed lines; Z. H. Li & H. J. Schulze 2008), and the relativistic Brueckner–Hartree–Fock (green double-dotted–dashed lines; H. Tong et al. 2022). The long red dashed line is the most probable value of E0(ρ) and Esym(ρ) we obtained.
Paper: X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 13+1
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Herman L. Marshall
Figure caption: Hardness–intensity diagram showing NICER observations of GX 13+1. Time bins of 64 s are used.
Paper: X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 13+1
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Herman L. Marshall
Figure caption: Contour plots of the polarization degree and angle, determined with the PCUBE algorithm, at the 68%, 95% and 99% confidence levels, in the 2–8 keV energy band during the overall (upper panel), dip state (middle panel), and nondip state (lower panel).
Paper: X-Ray and Radio Polarimetry of the Neutron Star Low-mass X-Ray Binary GX 13+1
Authors: Unnati Kashyap, Thomas J. Maccarone, Eliot C. Pattie, Mason Ng, Swati Ravi, Herman L. Marshall
Figure caption: Contour plots of the polarization degree and angle, determined with the PCUBE algorithm, at the 68%, 95% and 99% confidence levels, in the 2–4 and 4−8 keV energy band during the dip state (upper panel) and nondip state (lower panel).