adsabs/AstroCLIMB huggingface dataset:
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: The expected localization uncertainties estimated for mock lensed sBBH GW events considering the effective network (EN) effects due to the motion of the Earth (ΔΩEN) against those without considering it (ΔΩnonEN). Left and right panels show the cases for those systems with triple and quadruple images, respectively. The color of each symbol represents the S/N of the faintest image, with values indicated by the right color bar. The blue dashed lines represent ΔΩEN = ΔΩnonEN. Our sample points are almost all located substantially below the blue dashed lines, which means that considering the motion of the Earth in space can improve the localization precision significantly. The black dotted lines represent the best fits to each sample, i.e., ﹩\mathrm{log}({\rm{\Delta }}{{\rm{\Omega }}}_{{\rm{s}},{\rm{EN}}}/{{\rm{\deg }}}^{2})=0.80\mathrm{log}({\rm{\Delta }}{{\rm{\Omega }}}_{{\rm{s}},{\rm{nonEN}}}/{{\rm{\deg }}}^{2})-1.66﹩ (left panel) and ﹩\mathrm{log}({\rm{\Delta }}{{\rm{\Omega }}}_{{\rm{s}},{\rm{EN}}}/{{\rm{\deg }}}^{2})=0.57\mathrm{log}({\rm{\Delta }}{{\rm{\Omega }}}_{{\rm{s}},{\rm{nonEN}}}/{{\rm{\deg }}}^{2})-3.07﹩ (right panel), which suggests that the improvement by the effective network to the localization is roughly a factor of 10−1.66 and 10−3.07, as also indicated by the top and right small panels for the one-dimensional distributions of ΔΩs,EN peaked at ∼0.01 deg2 (or ∼0.001 deg2) and ΔΩs,nonEN peaked at ∼0.14 deg2 (or ∼0.58 deg2).
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: Expected number of lensed GW events (Nlen; top panel), number of lensed GW events with triple or more image detection with identifiable lensed host galaxies (﹩{N}_{{\rm{len}}}^{{\rm{host}}}﹩; middle panel), and the corresponding fractional error of the H0 measurement obtained by using these lensed events together (bottom panel) as a function of time. Here we assume that the 2nd/2.5th/3rd generation (2G/2.5G/3G) GW detectors, i.e., LIGO A+/Voyager/CE, start to work in 2027/2030/2035. In the top panel, the dashed curves with diamond symbols show the results obtained for lensed merger events of sBBHs (red), BNSs (green), and NSBHs (blue) with double images (labeled as sBBH-2, BNS-2, and NSBH-2), while the solid curves with square symbols show those with three or more images, labeled as sBBH-3+ (red), BNS-3+ (green), and NSBH-3+(blue). In the middle and bottom panels, the shaded regions around these curves indicate the uncertainties of the estimates introduced by the uncertainty in the constraints of the local merger rate densities. Note that the numbers for detectable sources shown in the top and middle panel are obtained by averaging those from a large number of realizations.
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: A schematic diagram for the effective network of ground-based GW detectors for a lensed GW event with double images detected at different times. S1 and S2 are the double images of the event, L is the foreground lens galaxy, v0 denotes the velocity of the Sun in the Galaxy, and (A1, B1, C1) and (A2, B2, C2) represent the locations of three GW detectors in space when they receive the signal from S1 and S2, respectively. Due to the rotation of the Earth, usually the baselines A2B2, B2C2, and C2A2 are not parallel with A1B1, B1C1, and C1A1. However, the baselines A1A2, B1B2, and C1C2 are close to, though not exactly, parallel to each other due to the lengths of these baselines being much longer than those of A1B1, A1C1, and B1C1.
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: Flowchart of the dark lensed siren method for cosmological inference. In the left and right blocks, we show the basic recipes needed to obtain or infer from GW and EM (host galaxy) observation, respectively. We use a blue dotted outline to emphasize the key steps in such a method, i.e., (1) precisely localize the GW source via the effective network proposed and find the associated lensed host galaxy and (2) further subarcsecond localization of the GW source within the host galaxy via three or more images (with central image). With the above two key steps, we may constrain the cosmological parameters via the time delay and luminosity distance measurement from the lensed GW sources, together with the Fermat potential and magnification factor reconstructed by the EM image of the lensed host galaxies.
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: Mock image of the lensed system observed by JWST and the reconstructed light components of the mock system, with the JWST parameters of readout noise, 13.25e−; pixel scale, ﹩0.^{\prime} 063﹩; CCD gain, 1.82e/ADU; and zero-point magnitude, 26.47 mag. The exposure time is set to be 3600 s per image, and the sky brightness is ﹩28.39\,{{\rm{mag}}\,{\rm{arcsec}}}^{-2}﹩. The magnitude of the lensed host galaxy is set to be M⋆ ∼ 23 mag, and the reconstructed accuracy on the potential difference map is Δϕi,j ∼ 0.25%. The top left panel shows the mock observed system by JWST; the top middle panel shows the reconstructed image of the system; the bottom left and middle panels show the decomposed observed light from the mock source and lens galaxies, respectively; the top right panel shows the residual map after subtracting the reconstructed image from the mock observed system; and the bottom right panel shows the reconstructed original image of the source without being lensed.
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: The fractional errors of the constraints on H0 (left panel) and Ωm (right panel) via different numbers of lensed GW sources by assuming the ΛCDM model. The blue, green, and brown symbols show the results obtained from the lensed sBBHs, BNSs, and NSBHs detected by the third-generation GW detectors (i.e., ET and CE), respectively. The error bars associated with each show the variance (16%, 84%) among 50 realizations.
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: One realization of the cosmological parameter inferences on the open wkCDM model for ﹩{N}_{{\rm{len}}}^{{\rm{host}}}=100﹩ lensed sBBH mergers with both the GW signals detected by future third-generation GW detectors and host galaxies identified by EM telescopes.
Paper: Enhanced Localization of Dark Lensed Gravitational-wave Events Enables Host Galaxy Identification and Precise Cosmological Inference
Authors: Zhiwei Chen, Qingjuan Yu, Youjun Lu, Xiao Guo
Figure caption: Cumulative probability distribution functions of S/N (﹩{\varrho }_{{\rm{GW}},{i}_{j}}﹩) for all the images of the lensed GW sources (CDF(> ϱGW)), normalized to 1 at ϱGW = 5. The red, blue, and green solid lines show the results of triple-image cases of sBBHs, BNSs and NSBHs, while the dashed lines correspondingly represent the cases of quadruple images.
Paper: Distinct Solar Energetic Particle Shock Intensity–Diffusion Coefficient Relationships in the Inner Heliosphere
Authors: M. E. Cuesta, F. Fraschetti, G. Livadiotis, H. A. Farooki, M. M. Shen, L. Y. Khoo, J. R. Szalay, J. S. Rankin, D. J. McComas, D. G. Mitchell, E. R. Christian, J. G. Mitchell, G. D. Berland, C. M. S. Cohen, R. A. Leske, Z. Xu, G. D. Muro, F. Pecora, D. Ruffolo, W. H. Matthaeus, J. Giacalone, N. A. Schwadron, M. I. Desai, M. A. Dayeh, S. D. Bale, M. L. Stevens, R. Livi
Figure caption: Top row: values of ﹩{\kappa }_{\parallel }{\cos }^{2}{\theta }_{{\rm{BN}}}﹩ (left) and κfit (right) as a function of proton energy. Bottom row: values of jshock as a function of ﹩{\kappa }_{\parallel }{\cos }^{2}{\theta }_{{\rm{BN}}}﹩ (left) and κfit. For all panels, the symbol of each curve is keyed to the shock event time listed in Table 1. Reference curves for power laws E2/3 and E3/2 are shown in the top panels.
Paper: Caught in the Cosmic Web: Evidence for Ram Pressure Stripping of a Low-mass Galaxy by the Cosmic Web
Authors: Nicholas Luber, Sabrina Stierwalt, George C. Privon, Gurtina Besla, Kelsey E. Johnson, Nitya Kallivayalil, David R. Patton, Mary Putman, Jingyao Zhu
Figure caption: Left: false-color RGB composite image of AGC727130, created using Pan-STARRS g-, r-, and i- band images (K. C. Chambers et al. 2016), with a red-scale overlay showing the spatial distribution of the neutral atomic gas. This image is oriented with north pointing upwards, and west pointing rightwards. Right: the same optical image, with H I column density contours overlaid with levels 2n × 1020 atoms cm−2 for n = 1, 2, 3, 4. The hatched circle in the bottom left corresponds to the restoring beam for the H I observations, the red scale bar in the top left corresponds to 5 kpc in projection, and the arrow in the bottom right points to the direction of the interacting pair 60 kpc away in projection.
Paper: Caught in the Cosmic Web: Evidence for Ram Pressure Stripping of a Low-mass Galaxy by the Cosmic Web
Authors: Nicholas Luber, Sabrina Stierwalt, George C. Privon, Gurtina Besla, Kelsey E. Johnson, Nitya Kallivayalil, David R. Patton, Mary Putman, Jingyao Zhu
Figure caption: Ram pressure stripping criterion for AGC 727130. The gray-shaded region indicates combinations of intergalactic medium (IGM) density and galaxy velocity where the external ram pressure exceeds the galaxy’s restoring force, making gas removal via ram pressure stripping likely. The cyan regions correspond to the regions of parameter space expected in cosmic web filaments.
Paper: Caught in the Cosmic Web: Evidence for Ram Pressure Stripping of a Low-mass Galaxy by the Cosmic Web
Authors: Nicholas Luber, Sabrina Stierwalt, George C. Privon, Gurtina Besla, Kelsey E. Johnson, Nitya Kallivayalil, David R. Patton, Mary Putman, Jingyao Zhu
Figure caption: A position–velocity diagram taken across the major axis of the galaxy. The x-axis corresponds to the angular offset along the axis from optical center, the y-axis velocity corresponds to the observed line-of-sight velocity, and the grayscale and contours indicate the intensity level.
Paper: Caught in the Cosmic Web: Evidence for Ram Pressure Stripping of a Low-mass Galaxy by the Cosmic Web
Authors: Nicholas Luber, Sabrina Stierwalt, George C. Privon, Gurtina Besla, Kelsey E. Johnson, Nitya Kallivayalil, David R. Patton, Mary Putman, Jingyao Zhu
Figure caption: The orientation of AGC 727130 within the cosmic web. The blue cylinders indicate the spine of the filamentary network, as outputted by DisPerSE, and their width corresponds to 1 Mpc. The red dot marks the position of AGC 727130, and we note that the galaxy is placed within the intersection of the filaments at this point. The arrow indicates the direction of the asymmetric H I extension, corresponding to pointing toward the northwest in the plane of the sky as seen in Figure 1.
Paper: Distinct Solar Energetic Particle Shock Intensity–Diffusion Coefficient Relationships in the Inner Heliosphere
Authors: M. E. Cuesta, F. Fraschetti, G. Livadiotis, H. A. Farooki, M. M. Shen, L. Y. Khoo, J. R. Szalay, J. S. Rankin, D. J. McComas, D. G. Mitchell, E. R. Christian, J. G. Mitchell, G. D. Berland, C. M. S. Cohen, R. A. Leske, Z. Xu, G. D. Muro, F. Pecora, D. Ruffolo, W. H. Matthaeus, J. Giacalone, N. A. Schwadron, M. I. Desai, M. A. Dayeh, S. D. Bale, M. L. Stevens, R. Livi
Figure caption: Case example of the fitting procedure outlined in Section 3.2.1 for the shock observed by PSP on 2024 February 8 (period includes nearly 4 hr of observations prior to 2024 February 8 04:25). Top: observed particle intensities (jobs measured by IS⊙IS/EPI-Lo). Middle: model intensity (jfit) using Equation (6), with fitted parameters given in Table 1. Bottom: the logarithm-10 of the ratio of the model to observed intensities.
Paper: Distinct Solar Energetic Particle Shock Intensity–Diffusion Coefficient Relationships in the Inner Heliosphere
Authors: M. E. Cuesta, F. Fraschetti, G. Livadiotis, H. A. Farooki, M. M. Shen, L. Y. Khoo, J. R. Szalay, J. S. Rankin, D. J. McComas, D. G. Mitchell, E. R. Christian, J. G. Mitchell, G. D. Berland, C. M. S. Cohen, R. A. Leske, Z. Xu, G. D. Muro, F. Pecora, D. Ruffolo, W. H. Matthaeus, J. Giacalone, N. A. Schwadron, M. I. Desai, M. A. Dayeh, S. D. Bale, M. L. Stevens, R. Livi
Figure caption: Illustration on the left visualizing the connection of larger or smaller normalized magnetic field fluctuations (δB/B0) to smaller or larger values for the spatial diffusion coefficients, respectively, which is shown on the right that is taken from the bottom right panel of Figure 2.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: Black hole mass versus core radius across stellar populations. In red we show massive elliptical galaxies from S. P. Rusli et al. (2013) with resolved cores and dynamical black hole mass measurements. The red curve shows the best-fit linear correlation to these data from J. Thomas et al. (2016). In blue we show predicted masses of stellar-mass black hole populations for a number of Galactic globular clusters, with the best-fit linear correlation from Figure 3 shown again here in blue. The slopes of these two populations are consistent to within 1σ, despite spanning orders of magnitude across both axes. The dashed black curve shows our best-fit global correlation for globular clusters and massive ellipticals combined.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: Total mass of the stellar black hole populations predicted for various Milky Way globular clusters versus core radius. Blue scatter points show the black hole predictions using the methods of this paper (see Table A1), with stars highlighting a few specific clusters discussed further in the text. For the core-collapsed clusters NGC 6293 and NGC 6681, we plot the mass of the final black hole ejected from the best-fit simulations (12 M⊙), with the arrows indicating these clusters may host zero black holes at present. All core radius measurements are taken from H. Baumgardt & M. Hilker (2018). The dashed black curve shows our best-fit linear correlation ﹩{\mathrm{log}}_{10}({M}_{\bullet }/{M}_{\odot })=(2.92\pm 0.12)+(1.43\pm 0.23){\mathrm{log}}_{10}({r}_{c}/{\rm{pc}})﹩.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: Top panels: total mass of black hole populations in our Milky Way globular clusters of interest versus half-light radius, cluster mass, and central velocity dispersion, σc. As in Figure 4, open circles denote clusters from the CMC Cluster Catalog using the methods of N. Z. Rui et al. (2021a), while stars show clusters with previously published CMC fits. These three data sets feature Pearson coefficients of 0.58, 0.61, and 0.26, respectively (compared to r = 0.80 for the M•–rc correlation in Figure 4). Bottom panels: half-light radius, total cluster mass, and σc versus core radius for all Milky Way globular clusters (data from H. Baumgardt & M. Hilker 2018). Open circles again denote the specific clusters with black hole population estimates. Note the clusters with black hole estimates effectively span the full parameter space of the full Milky Way globular cluster population.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: Effective radius versus core radius (left panel) and total stellar mass versus core radius (right panel) for Galactic globular clusters (blue) and massive elliptical galaxies (red). Filled blue circles show the full population of Galactic globular clusters; open blue circles show those in Figure 4 with black hole mass estimates. Filled red circles show the massive early-type galaxies cataloged by T. R. Lauer et al. (2007); open circles show those with black hole mass and core measurements by S. P. Rusli et al. (2013)—also shown in Figure 4. Blue and red bands show the best-fit local linear correlations for globular clusters and massive ellipticals, respectively.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: The surface brightness and velocity dispersion profiles (SBPs and VDPs) of the Milky Way globular clusters NGC 0288, NGC 1904, NGC 4372, NGC 5024, NGC 5897, and NGC 5986. The data points are the observed profiles, with SBPs from S. C. Trager et al. (1995) and VDPs compiled from both stellar proper motions (L. L. Watkins et al. 2015; H. Baumgardt et al. 2019) and radial velocities (H. Baumgardt & M. Hilker 2018; F. R. Ferraro et al. 2018; S. Kamann et al. 2018). The gray curves correspond to model snapshots in the CMC Cluster Catalog (K. Kremer et al. 2020c) that fit well the observed profiles. We use the snapshots selected by N. Z. Rui et al. (2021a) that satisfy s < 10, where ﹩s={\rm{\max }}({\tilde{\chi }}_{{\rm{SBP}}}^{2},{\tilde{\chi }}_{{\rm{V\; DP}}}^{2})﹩ is the maximum of the reduced χ2 statistics of the SBP and VDP fits (see their Table 5, Column (9)). The solid black curves correspond to the single best-fitting snapshot, minimizing s.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: Left panel: surface brightness profiles (V-band) for Galactic globular clusters from E. Noyola & K. Gebhardt (2006), illustrating the diversity of cluster core sizes. We highlight five particular clusters that are discussed in further detail in the text. Right panel: surface brightness profiles (also V-band) for a sample of core and coreless elliptical galaxies out to a distance of 100 Mpc from T. R. Lauer et al. (2005). We highlight the brightest galaxies in the Leo Cluster (NGC 3842), Coma Cluster (NGC 4889), and Virgo Cluster (NGC 4472 as well as NGC 4486). We also highlight NGC 1600 from J. Thomas et al. (2016), which has one of the faintest stellar cores of any galaxy with a black hole mass measurement.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: Time evolution of the core radius—using the density-weighted definition of S. Casertano & P. Hut (1985)—for all globular cluster simulations computed by K. Kremer et al. (2020b). The curve color denotes the total mass in black holes at the end of each simulation (t = 13 Gyr). As shown, clusters with larger core radius generally host more-massive black hole populations. Blue ticks on the right-hand side denote present-day core radii of Milky Way globular clusters from H. Baumgardt & M. Hilker (2018).
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: As Figure A2 but for the Milky Way globular clusters NGC 6121, NGC 6171, NGC 6293, NGC 6352, NGC 6496, and NGC 6539.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: As Figure A2 but for the Milky Way globular clusters NGC 6723, NGC 6779, and Terzan 5.
Paper: Connecting Cores and Black Hole Dynamics across Scales: From Globular Clusters to Massive Ellipticals
Authors: Kyle Kremer, Newlin C. Weatherford, Philip F. Hopkins, Nicholas Z. Rui, Claire S. Ye
Figure caption: As Figure A2 but for the Milky Way globular clusters NGC 6553, NGC 6569, NGC 6624, NGC 6656, NGC 6681, and NGC 6712. For NGC 6624, the well-fitting CMC models come from N. Z. Rui et al. (2021a) rather than the raw CMC Cluster Catalog.
Paper: XRISM Resolves Relativistic Effects from the Innermost Accretion Disk in Serpens X-1
Authors: R. M. Ludlam, J. M. Miller, E. M. Cackett, J. A. García
Figure caption: Predicted Fe line profile from the use of (a) absorption, (b) photoionized emission models, and (c) different blurring kernals. Time-averaged data are shown in light gray and were rebinned for plotting purposes. The reflection (RELXILLNS) model-predicted line profile is shown as a solid orange line in panels (a) and (b). In panel (a) the green dashed line indicates the model-predicted line profile when a Gaussian absorber is required, whereas the blue dotted–dashed line shows the line profile when WARMABS is applied (the profile of which overlaps with the reflection-only model prediction). In panel (b) the purple dot-dot-dotted–dashed line shows the line profile with the addition of a photoionized emitting plasma in the system. The Fe XXV line is stronger and broader in comparison to the reflection model-predicted line profile, but the Fe XXVI line is less pronounced. The red long-dashed line in panel (b) denotes the line-predicted model profile after removing the reflection model and allowing relativistically blurred photoionized emission to fit the line complex. The model appears to underpredict the Fe XXVI emission. In panel (c) we show the photoionized emission component convolved with relativistic effect (red dashed line) versus a Gaussian blurring kernal (pink dotted line), the latter of which is unable to adequately describe the red wing of the line profile.
Paper: XRISM Resolves Relativistic Effects from the Innermost Accretion Disk in Serpens X-1
Authors: R. M. Ludlam, J. M. Miller, E. M. Cackett, J. A. García
Figure caption: The XRISM/Resolve counts spectrum and model components for (a) the time-averaged (tavg), (b) lower banana (LB), and (c) upper banana (UB) states, respectively. The overall model is indicated by the dot-dot-dotted–dashed line, the power law by the dotted line, the multitemperature disk blackbody by the dotted–dashed line, and the reflection model by the solid line. The panels (d)–(e) directly below the counts spectra show the ratio of the data to the overall model for each spectrum. Panels (g)–(i) show the Fe line profile from Figure 2 with the reflection model line-predicted profile overlaid based upon fitting the counts spectra. Data were rebinned for clarity.