adsabs/AstroCLIMB huggingface dataset:
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: [O III] flux map, kinematics, and line fits from the MUSE data. (a) Map of the [O III] 5007 Å emission line flux after processing with q3dfit (quasar and stellar continuum emission removed). The white flux contour marks a value of 3 × 10−16 erg s−1 cm−2 spaxel−1. The green dot marks the quasar center with the size of the PSF FWHM. (b) Map of the 50th percentile (median) velocities, v 50. (c) Map of the 80th percentile line widths, w 80. (d)–(g) Representative spectra extracted from the regions indicated in panels (a)–(c). In the top panel of these spectra, the red line is the sum of the scaled quasar template, host continuum model, and the line fit, the last of which is shown as the purple dashed line. The data are the dark gray line. In the bottom panel, the blue spectrum shows the residuals of the data from the line fit and the red line is the sum of the scaled quasar template and host continuum model.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Two methods are used to measure the fluxes of the PAH features in the nuclear spectrum of PDS 456: the questfit template model method (top panel) and the direct fitting method (bottom panel). In the top panel, the difference between the extracted spectra and the non-PAH emission from the questfit model is shown in gray, the questfit PAH template is shown in yellow-gray, the polynomial fit to the continuum in orange, the individual Lorentzian components to the PAH components in green, the main PAH complexes at 6.2, 7.7, and 11.3 μm in black, and the sum of all Lorentzian components in blue. The color code is the same in the bottom panel except there is no questfit template. In this case, the polynomial continuum is allowed to be negative to correct for the imperfect continuum fitting from questfit. In both panels, the features in the dark gray vertical bands are data artifacts and the feature in the light gray band is a residual from the line fitting around [Ne II] 12.8 μm.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Paα flux map, kinematics, and line fits from the NIRSpec data. (a) Map of the Paα emission line flux after processing with q3dfit (quasar and stellar continuum emission removed). The white contour traces the extended [O III] emission shown in Figure 6(a). The green dot marks the quasar center with the size of the PSF FWHM. (b) Map of the 50th percentile (median) velocities, v 50. (c) Map of the 80th percentile line widths, w 80. (d)–(g) Representative spectra extracted from the regions indicated in panels (a)–(c). In the top panel of these spectra, the red line is the sum of the scaled quasar template and the line fit, the latter of which is shown as the purple dashed line. The data are the dark gray line. In the bottom panel, the blue spectrum shows the residuals of the data from the line fit and the red line is the scaled quasar template. Cosmic rays are marked in panel (e) with “CR” in red.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Flux and kinematic maps of five lines from the MIRI/MRS data cubes: three molecular lines H2 0–0 S(1), S(3), and S(5) and two atomic fine structure lines, [Ne III] 15.56 μm and [Ne VI] 7.65 μm. Each column shows maps of the emission line flux, v 50, and w 80, from top to bottom. The white contour in the flux maps traces the extended [O III] emission shown in Figure 6(a). The green dot marks the quasar center with the size of the PSF FWHM. Spaxels with bad fits have been removed from these maps based on a visual inspection informed by the MUSE and NIRSpec fits.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: AGN diagnostics adapted from S. Veilleux et al. (2009). (a) [Ne III] 15.56 μm to [Ne II] 12.81 μm flux ratios vs. the 30-to-15 μm flux ratios, (b) [Ne III] 15.56 μm to [Ne II] 12.81 μm flux ratios vs. the equivalent widths of the 7.7 μm PAH feature, (c) L bol histogram of all QUEST sources, (d) equivalent widths of the 7.7 μm PAH feature vs. the 30-to-15 μm flux ratios, (e) AGN/H II/PDR mixing diagram based on the O. Laurent et al. (2000) method, modified by L. Armus et al. (2007) and S. Veilleux et al. (2009): PAH (6.2 μm) to continuum (5.3–5.8 μm) flux ratios vs. the continuum (14–16 μm) to (5.3–5.8 μm) flux ratios, and (f) 6.2 and 7.7 μm PAH luminosities to FIR luminosity ratios. Note that in panels (b), (d), and (e) the small, medium, and large black circles correspond to the FIR-undetected, FIR-faint, and FIR-bright Palomar-Green quasars (“PG QSOs”), as defined in H. Netzer et al. (2007).
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Fine structure atomic lines in the PDS 456 nuclear spectrum. The continuum was fit with a third-order polynomial using q3dfit and the flux values have been normalized to the line peak. The spectra have been lightly smoothed using a moving average to eliminate high frequency fringing.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: (Left) Map of v 50 for H2 0–0 S(3). The kinematic major axis (PA = 165°, measured from north to east, taken from the M. Bischetti et al. 2019 CO(3–2) measurements) is shown as a dashed black line. (Right) The gray line shows the H2 0–0 S(3) spectrum extracted from the red circular aperture shown in the left panel, which displays a blueshift of v 50 ∼ −150 km s−1, evidence for the molecular outflow. The red line is the sum of the continuum fit from the scaled quasar spectrum (blue line) and the line fit (purple dashed line).
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Fit of a 1D extracted spectrum (teal) with the questfit continuum fitting package within q3dfit. The spectrum is fit with three blackbodies with different temperatures, cool (green), warm (orange), and hot (blue), a PAH template (red), and a silicate emission model (purple). The sum fit is the yellow curve and the residuals of the fit are plotted in the bottom panel. The features in the dark gray boxes on the second axis are data artifacts and the features in the light gray boxes are residual features from the line fitting.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: H2 1–0 S(3) flux maps, kinematics, and line fits from the NIRSpec data. (a) Map of the H2 1–0 S(3) emission line flux. The white contour traces the extended [O III] emission shown in Figure 6(a). The green dot marks the quasar center with the size of the PSF FWHM. (b) Map of the 50th percentile (median) velocities, v 50. (c) Map of the 80th percentile line widths, w 80.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Ratios of the fine structure lines emitted by the warm ionized gas compared to the predictions of the dusty photoionized AGN models from B. A. Groves et al. (2004). We plot the line ratios from three regions: nuclear (red), region A (green), and region C (blue), all without PSF removal. The model grids show the dependence on the ionization parameter (U; grayscale nodes) and power-law index of the ionizing source (α; pink and cyan lines). The predictions do not depend significantly on metallicity (it is fixed to solar here). We also plot the sample of Seyfert galaxies from I. Garcia-Bernete et al. (2022, orange circles) and the sample of PG QSOs (S. Veilleux et al. 2009, gray diamonds) in order to corroborate our results. See text for more details.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Excitation diagram for the rotational transitions of H2 in region C. Values of g(J  u ), E(J  u ), and A were gathered from E. Roueff et al. (2019) in order to convert from line intensities to N(J  u ). We fit the data points with a linear regression to determine the temperature of the gas based on the slope. Three separate fits are shown: all of the H2 lines (gray line), the cooler H2 tracers (S(1), S(2), S(3), and S(4); blue line), and the warmer H2 tracers (S(4), S(5), and S(7); red line).
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: PAH ratio diagnostic diagram. Flux ratios of the PAH 6.2 μm/7.7 μm and PAH 11.3 μm/7.7 μm from Table 1. The grids are estimated from D. Rigopoulou et al. (2021). They correspond to mixtures of PAH species ionized to various levels (0%, 70%, and 100% ionized PAH molecules). The individual grids range from softer (1 × interstellar radiation field (ISRF); top of the grid) to harder (103 × ISRF; bottom of the grid) incident radiation fields and from smaller (N  c  = 20, the number of carbon atoms; right side of the grid) to larger (N  c  = 400; left side of the grid) PAHs. The colored circles are PAH ratios for Seyfert galaxies colored by their MIR AGN fraction as defined in I. Garcia-Bernete et al. (2022). Values for PDS 456 are plotted as the star and square with error bars, and the color reflects the high AGN contribution of PDS 456 (93%).
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Comparison of the outflow kinematics of PDS 456 to those of other AGN-driven outflows. Data for cold molecular winds (blue) and warm ionized winds (green) are taken from F. Fiore et al. (2017). For PDS 456, the cold molecular wind measurements (blue star) are based on the CO(3–2) measurements of M. Bischetti et al. (2019), the warm ionized wind measurements (green star) are calculated from the [Ne III] luminosities, and the warm molecular wind measurements (yellow star) are calculated from the MIR rotational H2 lines. See text for more details.
Paper: Dark Photon Dark Matter and Low-frequency Gravitational-wave Detection with Gaia-like Astrometry
Authors: Haipeng An, Tingyu Li, Jing Shu, Xin Wang, Xiao Xue, Yue Zhao
Figure caption: The average PSDs of the injected white noise (WN), proper motion (PM), and stellar binary motion, along with the associated error bars for each bin, obtained from 104 simulations. For clarity, the error bars have been magnified by a factor of 3 to improve visibility. The green and pink dashed lines correspond to the cases with WN removed. The vertical dashed line refers to f = 2/T obs, with T obs = 10 yr being Gaia’s observation period. The input Gaia operational parameters align with the discussion in Section 4.
Paper: Eridanus III and DELVE 1: Carbon-rich Primordial Star Clusters or the Smallest Dwarf Galaxies? 
Authors: Joshua D. Simon, Ting S. Li, Alexander P. Ji, Andrew B. Pace, Terese T. Hansen, William Cerny, Ivanna Escala, Sergey E. Koposov, Alex Drlica-Wagner, Sidney Mau, Evan N. Kirby
Figure caption: Left: spatial distribution of DELVE 1 member stars. The dashed ellipses indicate 1, 3, and 5 times the half-light radius of the system, using structural parameters reported in the DELVE 1 discovery paper (S. Mau et al. 2020). Middle: color–magnitude diagram of DELVE 1, using DECaLS DR9 photometry. The spectroscopic members are displayed as red circles, and fainter candidate members within the half-light radius are plotted as blue dots with error bars. A Dartmouth isochrone (A. Dotter et al. 2008) based on the parameters for DELVE 1 estimated in the discovery paper (m − M = 16.39 mag, [Fe/H] = −1.5, and age = 12.5 Gyr) is shown as the solid curve. However, using the spectroscopically confirmed member stars and a more appropriate lower-metallicity ([Fe/H] = −2.5) isochrone, we find that a larger distance modulus of m − M = 16.68 mag (d = 22 kpc, dashed curve) fits the data better, suggesting that DELVE 1 is farther away than was initially reported. Right: IMACS spectra of the two brightest DELVE 1 members from the 2023 March observing run (top: g 0 = 16.35, bottom: g 0 = 19.25). The black curves show the best-fit model with a Gaussian + Lorentzian fit to each of the CaT lines.
Paper: Dark Photon Dark Matter and Low-frequency Gravitational-wave Detection with Gaia-like Astrometry
Authors: Haipeng An, Tingyu Li, Jing Shu, Xin Wang, Xiao Xue, Yue Zhao
Figure caption: The 95% exclusion limits from Gaia (green lines) and XG-Gaia (red lines) on the GW strain ﹩{h}_{0}^{\mathrm{GW}}﹩ from a binary system, the energy density ρ DM of the DPDM with purely gravitational interactions, and the coupling constant ϵ of U(1) B /U(1) B−L  DPDM, respectively. Model parameters regarding all the angles have been integrated out. The solid lines represent the bounds with linear subtraction, while the dashed lines correspond to quadratic subtraction. We also use the blue lines to denote the results including the time-dependent noise from unresolved binary systems. For comparison, the constraints from NANOGrav 15 yr (A. Afzal et al. 2023; G. Agazie et al. 2023b), EPTA DR2 (C. Smarra et al. 2023), and PPTA DR2 (Y.-M. Wu et al. 2022; X. Xue et al. 2022) are shown by the orange, cyan, and purple curves, respectively, with the solid (dashed) curves being the (un)correlated constraints. In the top right panel, the black dashed line shows the amount of local dark matter density near the Earth as a reference. In the bottom two panels, the horizontal solid lines are the limits from the MICROSCOPE WEP experiment (P. Touboul et al. 2017, 2022; P. Fayet 2018, 2019; D. W. P. Amaral et al. 2024). In addition, the vertical dashed line in each plot refers to the reference frequency f = 1/T obs, with T obs = 10 yr being Gaia’s observation period.
Paper: Eridanus III and DELVE 1: Carbon-rich Primordial Star Clusters or the Smallest Dwarf Galaxies? 
Authors: Joshua D. Simon, Ting S. Li, Alexander P. Ji, Andrew B. Pace, Terese T. Hansen, William Cerny, Ivanna Escala, Sergey E. Koposov, Alex Drlica-Wagner, Sidney Mau, Evan N. Kirby
Figure caption: Left: spatial distribution of Eri III member stars. The dashed ellipses indicate 1, 3, and 5 times the half-light radius of the system, using structural parameters from B. C. Conn et al. (2018). Middle: color–magnitude diagram of Eri III, using DES Data Release 2 photometry. Overplotted is an old (12.5 Gyr) metal-poor ([Fe/H] = −2.5, [α/Fe] = 0.4) Dartmouth isochrone (A. Dotter et al. 2008) at a heliocentric distance of 91 kpc (B. C. Conn et al. 2018). As the Dartmouth isochrones do not include a horizontal branch, an empirical M92 ridge line is added for the BHB stars. Right: IMACS 600-line CaT spectra of Eri III stars. The black curves show the best-fit model with a Gaussian + Lorentzian fit to each of the CaT lines (see text for more details). The top spectrum corresponds to the brightest RGB member at g 0 = 19.33, the middle spectrum corresponds to the second brightest RGB star at g 0 = 21.66, and the bottom spectrum is from a weighted average of the four faint RGB stars clumped near g 0 ∼ 22.3. The SNR per pixel as well as the derived metallicity from the CaT EWs are shown for each spectrum.
Paper: Eridanus III and DELVE 1: Carbon-rich Primordial Star Clusters or the Smallest Dwarf Galaxies? 
Authors: Joshua D. Simon, Ting S. Li, Alexander P. Ji, Andrew B. Pace, Terese T. Hansen, William Cerny, Ivanna Escala, Sergey E. Koposov, Alex Drlica-Wagner, Sidney Mau, Evan N. Kirby
Figure caption: [X/Fe] vs. [Fe/H] for the brightest stars in DELVE 1 (red circle) and Eri III (blue square) compared to Milky Way halo red giant stars (gray; ﹩\mathrm{log}g\lt 3.5﹩; P. S. Barklem et al. 2005; I. U. Roederer et al. 2014; H. R. Jacobson et al. 2015, as compiled in A. Abohalima & A. Frebel 2018); ultra-faint dwarf galaxies (purple diamonds; A. Koch et al. 2008, 2013; S. Feltzing et al. 2009; A. Frebel et al. 2010, 2014, 2016; J. E. Norris et al. 2010b, 2010c; J. D. Simon et al. 2010; G. Gilmore et al. 2013; M. N. Ishigaki et al. 2014a; I. U. Roederer & E. N. Kirby 2014; P. François et al. 2016; A. P. Ji et al. 2016a, 2016b, 2019, 2020b; I. U. Roederer & M. Mateo et al. 2016; T. T. Hansen et al. 2017, 2020, 2024; E. N. Kirby et al. 2017; A. Chiti et al. 2018a, 2023; D. Q. Nagasawa et al. 2018, M. Spite et al. 2018; J. L. Marshall et al. 2019; F. Waller et al. 2023, K. B. Webber et al. 2023, open symbols with arrows indicate upper limits); and the Phoenix globular cluster stream (A. P. Ji et al. 2020a; A. R. Casey et al. 2021, yellow circles). The dotted horizontal line in each panel indicates [X/Fe] = 0. For the Eri III star, Co is not measured and Al and Si have sufficiently large error bars as to be considered unreliable.
Paper: Eridanus III and DELVE 1: Carbon-rich Primordial Star Clusters or the Smallest Dwarf Galaxies? 
Authors: Joshua D. Simon, Ting S. Li, Alexander P. Ji, Andrew B. Pace, Terese T. Hansen, William Cerny, Ivanna Escala, Sergey E. Koposov, Alex Drlica-Wagner, Sidney Mau, Evan N. Kirby
Figure caption: Distribution of absolute magnitude as a function of half-light radius for stellar systems in the Milky Way halo. Dwarf galaxies are displayed as blue circles, globular clusters listed in the W. E. Harris (2010) compilation are plotted as gray triangles, and recently discovered ultra-faint star clusters are shown as cyan squares. The subjects of this paper, Eridanus III (Eri III) and DELVE 1, are represented by larger red diamonds, nominally located within the distribution of ultra-faint clusters. The dotted gray lines are lines of constant surface brightness, plotted at (from left to right) 24, 26, 28, 30, and 32 mag arcsec−2.
Paper: Eridanus III and DELVE 1: Carbon-rich Primordial Star Clusters or the Smallest Dwarf Galaxies? 
Authors: Joshua D. Simon, Ting S. Li, Alexander P. Ji, Andrew B. Pace, Terese T. Hansen, William Cerny, Ivanna Escala, Sergey E. Koposov, Alex Drlica-Wagner, Sidney Mau, Evan N. Kirby
Figure caption: C and N abundances of DELVE 1 and Eri III compared to NGC 7078 (J. C. Roediger et al. 2014) and the Phoenix Stream (A. P. Ji et al. 2020a; A. R. Casey et al. 2021). Both C and N are high in our target stars, and thus clearly inconsistent with the C–N anticorrelation typically seen in multiple populations within globular clusters (even though Phoenix only has upper limits for [N/Fe], these limits are sufficient to establish that its N abundances are substantially lower than the Eri III and DELVE 1 stars). The same is true for the Na–O anticorrelation, except that there are only upper limits for O (not shown).
Paper: Eridanus III and DELVE 1: Carbon-rich Primordial Star Clusters or the Smallest Dwarf Galaxies? 
Authors: Joshua D. Simon, Ting S. Li, Alexander P. Ji, Andrew B. Pace, Terese T. Hansen, William Cerny, Ivanna Escala, Sergey E. Koposov, Alex Drlica-Wagner, Sidney Mau, Evan N. Kirby
Figure caption: Cutouts of the MIKE spectra for DELVE 1-S1 and Eri III-S1 around (from left to right) CN and Sr, CH, C2 and Mg b, and Ba features. The 1σ spectrum uncertainties are shown as gray bars. The Sr line at 4215 Å is not detected for Eri III-S1, consistent with a low abundance inferred from the 4077 Å line. On the CH panels, the thin black curve indicates a synthesis with no carbon, whereas the red curve and shaded red region indicate the best-fit synthesis and syntheses with the carbon abundance varied by ±0.3 dex, respectively. Both stars are highly enhanced in C and N but have low abundances of Sr and Ba.
Paper: Eridanus III and DELVE 1: Carbon-rich Primordial Star Clusters or the Smallest Dwarf Galaxies? 
Authors: Joshua D. Simon, Ting S. Li, Alexander P. Ji, Andrew B. Pace, Terese T. Hansen, William Cerny, Ivanna Escala, Sergey E. Koposov, Alex Drlica-Wagner, Sidney Mau, Evan N. Kirby
Figure caption: [X/Fe] vs. atomic number for the DELVE 1 and Eri III stars. They are compared to abundances of other CEMP stars with [C/Fe] > 1 in ultra-faint dwarfs: GDR3-0928 (Ret II; C. R. Hayes et al. 2023), Psc II-10694 (M. Spite et al. 2018), Segue 1-7 (J. E. Norris et al. 2010a), Car III-1120 (A. P. Ji et al. 2020b), Boo I-119 (D. K. Lai et al. 2011; G. Gilmore et al. 2013), and two CEMP halo stars (CS22949-037 and CS29502-092; I. U. Roederer et al. 2014).
Paper: Compact Binary Merger Rate with Modified Gravity in Dark Matter Spikes
Authors: Saeed Fakhry, Sara Gholamhoseinian, Marzieh Farhang
Figure caption: The cumulative merger rate of PBH–PBH binaries as a function of the power-law index γ for different gravitational models. Top panels: results for Hu–Sawicki f(R) gravity models compared to GR. Bottom panels: results for nDGP gravity models compared to GR. From left to right: merger rates calculated using the Benson, Vika, and Shankar SMBH mass functions, respectively. The shaded gray bands represent the BH–BH mergers estimated by the LVK detectors during the latest observing run, i.e., (17.9–44) Gpc−3 yr−1 (R. Abbott et al. 2023).
Paper: Compact Binary Merger Rate with Modified Gravity in Dark Matter Spikes
Authors: Saeed Fakhry, Sara Gholamhoseinian, Marzieh Farhang
Figure caption: The merger rate of PBH–PBH binaries per unit volume as a function of SMBH mass for different Hu–Sawicki f(R) gravity models compared to GR. Results are shown for three different SMBH mass functions and three values of the power-law index γ characterizing the steepness of the dark matter spike density profile. Top panels: Benson mass function. Middle panels: Vika mass function. Bottom panels: Shankar mass function. From left to right, each column represents γ = 0.5, 1.0, and 1.5, respectively.
Paper: Compact Binary Merger Rate with Modified Gravity in Dark Matter Spikes
Authors: Saeed Fakhry, Sara Gholamhoseinian, Marzieh Farhang
Figure caption: The merger rate of PBH–NS binaries per unit volume as a function of SMBH mass for different Hu–Sawicki f(R) gravity models compared to GR. Results are presented for three different SMBH mass functions and three values of the power-law index γ characterizing the steepness of the dark matter spike density profile. Top panels: Benson mass function. Middle panels: Vika mass function. Bottom panels: Shankar mass function. From left to right, each column represents γ = 0.5, 1.0, and 1.5, respectively.