adsabs/AstroCLIMB huggingface dataset:
Paper: GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Thomas Bohn, Hanae Inami, Aditya Togi, Lee Armus, Thomas S.-Y. Lai, Loreto Barcos-Munoz, Yiqing Song, S. T. Linden, Jason Surace, Marina Bianchin, Vivian U, Aaron S. Evans, Torsten Böker, Matthew A. Malkan, Kirsten L. Larson, Sabrina Stierwalt, Victorine A. Buiten, Vassilis Charmandaris, Tanio Diaz-Santos, Justin H. Howell, George C. Privon, Claudio Ricci, Paul P. van der Werf, Susanne Aalto, Christopher C. Hayward, Justin A. Kader, Joseph M. Mazzarella, Francisco Muller-Sanchez, David B. Sanders
Figure caption: Full MIRI spectra (4.9–27.9 μm), extracted from the regions where we detect emission from the secondary (outflow) component seen in all MIRI channels, about 350 pc to the south (blue), and 350 pc (orange) and 650 pc (red) to the north of the S nucleus (see dotted circles in Figure 4). An aperture radius of r = 0.″8 was used, and the spectra here have been aperture corrected but are not corrected for extinction. The rotational H2 lines used in this study are labeled, along with other MIR emission lines. Prominent PAH features are also marked with upside-down triangles. While the emission features of both spectra are similar, the continuum of the blueshifted outflow is as much as 3 times lower than that of the redshifted outflow for regions equidistant from the nucleus.
Paper: Search for High-excitation Emission Lines from a Quasar-scale Active Nucleus in Arp 220
Authors: Charles E. Goldberg, Victorine A. Buiten, George H. Rieke, Almudena Alonso-Herrero, A. Paggi, Paul van der Werf, Meredith A. Stone, Jane E. Morrison, Stacey Alberts, Dan Dicken, Gillian Wright
Figure caption: Measurement of the [Ne VI] λ7.652 line. In both figures the wavelength of the [Ne VI] line is indicated by the orange line. The upper spectrum is for the western nucleus (solid blue line), which has a complex molecular spectrum, with a model described in V. Buiten et al. (2024, in preparation) and illustrated by the red dashed line. The lower spectrum (blue solid line) is of the eastern nucleus and is much simpler, being dominated in the vicinity of the [Ne VI] line by CH4 ice absorption; the dashed line shows the fit that was used to determine the local spectral behavior. In both cases upper limits to the line strength were determined, after subtracting the model spectra from the observed ones, by approximating the line as a Gaussian with a FWHM of 500 km s−1, centered at the wavelength indicated by the vertical orange lines.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: The amplitude spectrum of KIC 10855535 derived from Kepler LC data. The red vertical dashed line represents the Nyquist frequency (f N = 24.47 day−1). The low-frequency region is enlarged for better inspection. Note that the group of mirror frequencies (symmetrical about the Nyquist frequency) of low frequencies have too low S/N to be listed in Table 2 but are clear in the spectrum.
Paper: Search for High-excitation Emission Lines from a Quasar-scale Active Nucleus in Arp 220
Authors: Charles E. Goldberg, Victorine A. Buiten, George H. Rieke, Almudena Alonso-Herrero, A. Paggi, Paul van der Werf, Meredith A. Stone, Jane E. Morrison, Stacey Alberts, Dan Dicken, Gillian Wright
Figure caption: Comparison of strengths of [Ne V] 14.32 μm and [Ne VI] 7.65 μm for ULIRGs and AGNs. The blue circles are from S. Veilleux et al. (2009) and the red squares from other sources: (in order of strength) NGC 6552 (J. Alvarez-Marquez et al. 2023), NGC 4151 (E. Sturm et al. 1996), Circinus (A. F. M. Moorwood et al. 1997), NGC 1068 (D. Lutz et al. 2000), NGC 7319 (M. Pereira-Santaella et al. 2022), and NGC 7469 (narrow component; L. Armus et al. 2023). The unconstrained fit has a slope of 1.03 and an intercept close to zero, i.e., the lines are of close to equal strength.
Paper: Search for High-excitation Emission Lines from a Quasar-scale Active Nucleus in Arp 220
Authors: Charles E. Goldberg, Victorine A. Buiten, George H. Rieke, Almudena Alonso-Herrero, A. Paggi, Paul van der Werf, Meredith A. Stone, Jane E. Morrison, Stacey Alberts, Dan Dicken, Gillian Wright
Figure caption: Measurement of the [Ne V] λ14.32 line. The upper figure shows the spectrum of the western nucleus, with a preliminary molecular absorption model from V. Buiten et al. (2024, in preparation) overlaid. The [Ne V] measurement listed in Table 3 results from the difference of the model and measured spectrum. The bottom figure shows the area of the [Ne V] line in the eastern nucleus. The line measurement for [Ne V] listed for this nucleus is derived directly from this spectrum.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: Light curves of KIC 10855535. From Kepler LC data, the amplitude of the light curve is about 7 mmag at the start time and increases to approximately 8 mmag at the end of observation. The sampling frequency varies in different sectors of TESS, resulting in varying densities of data points.
Paper: Search for High-excitation Emission Lines from a Quasar-scale Active Nucleus in Arp 220
Authors: Charles E. Goldberg, Victorine A. Buiten, George H. Rieke, Almudena Alonso-Herrero, A. Paggi, Paul van der Werf, Meredith A. Stone, Jane E. Morrison, Stacey Alberts, Dan Dicken, Gillian Wright
Figure caption: Continuum-subtracted spectra around each line measurement in Arp 220 west and east. Spectra for Arp 220 west and east are shown in blue and orange, respectively. All plots use the same y-scaling, with the exception of [Mg VII] and [O IV]. The continuum subtraction for the 5.503 μm line was adversely affected by the 5.511 μm H2 S7 line (see upper right two plots). Much of the structure in the “continua” around 6 μm is due to H2O absorption features.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Comparison of the observed properties of HD 174881 against model isochrones from the MIST series (J. Choi et al. 2016) and the PARSEC series (Y. Chen et al. 2014). Rotation is not considered. The panels display the physical properties of the components (labeled) as a function of mass and temperature. The best compromise between the observations and theoretical predictions is reached for a metallicity of [Fe/H] = −0.1 for MIST, and solar composition for PARSEC. The corresponding ages are 255 and 273 Myr, respectively.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Astrometric model for HD 174881. Neither the PTI visibilities nor their uncertainties can be plotted on the plane of the sky, but we represent them here as green triangles at their predicted locations in the orbit, to illustrate the phase coverage they provide. The components are drawn with their sizes to scale relative to the orbit, and star B (the smaller and more massive component, in blue) is rendered at periastron. The dotted line marks the line of nodes, and the ascending node is indicated with the “Ω” symbol. In accordance with the classical convention, Ω is the node at which star B is receding from the observer relative to γ. The enlargement in the inset shows the two archival CHARA observations, with their corresponding error ellipses. The short line segments connecting the measured and predicted CHARA positions represent the residuals from the model.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Similar to Figure 8, for the absolute magnitudes of HD 174881 in V, H, and K S, as a function of M and T eff.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Spectral energy distribution for HD 174881 extended to the infrared via a Rayleigh–Jeans approximation, showing an apparent flux excess longward of about 5 μm. A blackbody model corresponding to a temperature of 15 K provides a reasonable representation of that excess.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Visualization of the fit of our orbit model to the calibrated PTI visibilities for HD 174881. The top panel shows the measurements and model for six nights over a one month stretch in 2001, and the bottom panel presents an enlargement of the first of those nights (2001 May 15). The visibility residuals are shown in both panels.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Spectroscopic orbit for HD 174881, together with our radial velocity measurements and those of J. R. De Medeiros & S. Udry (1999). The dotted line in the top panel marks the center-of-mass velocity of the system. Residuals are shown at the bottom.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Corner plot showing the correlations among a selection of the fitted parameters of the radiometric analysis.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Comparison of the measured MIRC squared visibilities from our 2007 July 7 observation with the model (solid lines) for the MACIM image in Figure 1.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Spectral energy distribution of HD 174881.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: LRIS optical spectra (blue and red arms separated) of new ultracompact binaries, plus archival spectra of ES Cet (K. Bąkowska et al. 2021) scaled by an arbitrary normalization constant for ease of comparison. All systems are dominated by double-peaked emission lines of ionized helium, nitrogen, and neon from the accretion disk. The offsets in normalization across the red and blue arms are due to flux-calibration systematic error.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: Lensing mass profile (ESD) for the full AGN sample (black circles) and the weighted control galaxy sample binned in stellar mass. The digits in the legend are the stellar mass range in ﹩\mathrm{log}({M}_{* }/{h}^{-2}{M}_{\odot })﹩.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: 2D density plot of stellar mass and redshift with the corresponding weight map (Left: AGNs. Middle: control galaxy sample. Right: weight map). Each panel has 21 × 21 bins with a minimum weight value of 0.003 and a maximum value of 2.28.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: The covariance matrix calculated using 2000 bootstrap of 43 regions from S16A area divided by HEALPix.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: SMHR of the AGN and control galaxy samples. The theoretical lines are from Leauthaud et al. (2010; orange and blue solid lines). The green square data points show the control galaxy sample in four mass bins. The red star is the result based on the full AGN sample. The stellar mass bin AGN results are denoted as purple diamonds.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: Modeling the lensing mass profile (ESD) of the control galaxies split by the stellar mass. We plot the different contributions to the ESDs in the upper left panel using different colors, i.e., stellar mass (red solid line) and the central galaxy with an NFW profile (blue). M * here denotes ﹩\mathrm{log}({M}_{\mathrm{star}}/{h}^{-2}{M}_{\odot })﹩.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: Galaxy–galaxy lensing signal (ESD) of the AGNs split by type (left), luminosity (middle), and redshift (right). The black solid lines are the results from the control sample as reference.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: The satellite fraction of the control galaxy sample (blue dots) and the AGNs (orange dots) as a function of stellar mass. The AGN samples contain low/high stellar mass samples, the AGN sample as a whole, as well as the low/high stellar mass sample with larger separations, as in Figure 8.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: Modeling the lensing mass profile (ESD) of all AGNs as a whole. We plot the different contributions to the ESDs using different colors, i.e., stellar mass (red solid line), the central galaxy with an NFW profile (blue), satellite contribution (green), and two-halo term (cyan).
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: Comparison of stellar mass between weak lensing modeling and SED fitting. The x-axis shows the stellar masses of galaxies and AGNs and the y-axis gives the weak lensing modeled stellar mass.
Paper: Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Wentao Luo, John D. Silverman, Surhud More, Andy Goulding, Hironao Miyatake, Takahiro Nishimichi, Chiaki Hikage, Lalitwadee Kawinwanichakij, Junyao Li, Qinxun Li, Xiangchong Li, Elinor Medezinski, Masamune Oguri, Taira Oogi, Cristobal Sifon
Figure caption: Lensing mass profile (ESD) of AGNs split by the stellar mass of their host galaxy as indicated.
Paper: Extreme-mass-ratio Inspirals in the Strong Segregation Regime—to Inspiral or to Get Ejected?
Authors: Karamveer Kaur, Hagai B. Perets
Figure caption: EMRI rates, Γ (including ejections, solid curves) and Γ0 (without ejections, dashed curves), in the left panel, and their ratio Γ/Γ0 in the right panel, are presented as a function of M • for various γ (in color) at time T 0. Both lower MBH masses (low M •) and steeper density slopes of clusters (high γ) support a higher number density of BHs in the inner regions, which can potentially increase the rates of both EMRIs and ejections. From the left panel, Γ0 is higher for higher γ and lower M •, and roughly follows the classical relation ﹩{{\rm{\Gamma }}}_{0}\propto {M}_{\bullet }^{-1/4}﹩ found in many previous works without the inclusion of ejections. However, the impact of ejections: (1) destroys these simplistic trends for EMRI rates Γ that become an increasing function of MBH mass M • for steep profiles with γ ≳ 2.25, and (2) caps the EMRI rates at a maximum Γ ≃ 200 Gyr−1 for the overall range of parameters explored here, while EMRI rates without ejections can attain high values of Γ0 ∼ a few ×1000 Gyr−1. From the right panel, suppression is stronger for higher γ and lower M •. For γ = 2, the rates are suppressed by a factor ≈3 for all M •, while the suppression becomes more important by an order of magnitude for (a) M • ≲ 106  M ⊙ for γ = 2.25, and (b) M • ≲ 107  M ⊙ for γ = 2.5.
Paper: Extreme-mass-ratio Inspirals in the Strong Segregation Regime—to Inspiral or to Get Ejected?
Authors: Karamveer Kaur, Hagai B. Perets
Figure caption: Evolution of EMRI rates, Γ (including ejections, in blue) and Γ0 (without ejections, in magenta), shown as a function of time in units of T 2b(a c) for various density slopes γ of the BH cusp and central MBH masses M •. Left: rates for various values of BH density index γ = 2−2.5 for fixed MBH mass M • = 4 × 106  M ⊙. Right: rates for γ = 2 while varying M • = 104−6  M ⊙. Evidently, the suppression is strongest for the steepest cluster densities with higher γ and/or lower MBH mass M •. Further, the level of rate suppression due to ejections driven by strong scatterings is time-dependent. The comparison at time T 0 = T 2b(a c0) (vertical gray lines) is apparently the most relevant in astrophysical settings that may sustain a steady state (see the text for more details).
Paper: Extreme-mass-ratio Inspirals in the Strong Segregation Regime—to Inspiral or to Get Ejected?
Authors: Karamveer Kaur, Hagai B. Perets
Figure caption: Evolution of BH number profiles N(a) with time (in color). As earlier, the solid (dashed) curves indicate the solution with (without) strong scatterings. The two panels correspond to γ = 2 and 2.25 for fixed M • = 106  M ⊙. The black curves depict the solutions at the reference time T 0, while the initial power-law profile is depicted in yellow. The depletion of BHs due to ejections triggered by strong scatterings is evidently higher in the inner regions of the cusp (smaller a), and for clusters with higher γ. The kink in these curves approximately corresponds to the BH depletion due to the capture by the central MBH, satisfying ﹩\mathrm{log}[1/{{ \mathcal R }}_{\mathrm{cap}}(a)]{T}_{2{\rm{b}}}(a)\approx t﹩. The solid gray line corresponds to the critical semimajor axis a c0, and the dashed gray line to its analytical counterpart a c.
Paper: Extreme-mass-ratio Inspirals in the Strong Segregation Regime—to Inspiral or to Get Ejected?
Authors: Karamveer Kaur, Hagai B. Perets
Figure caption: Evolution of 2D density ﹩{ \mathcal N }﹩ of BHs as a function of ﹩{ \mathcal R }﹩ at fixed a = a c0 with time in color. The solid (dashed) curves represent the solution with (without) strong scatterings, and black curves indicate the solution at time T 0 = T 2b(a c0). The panels are for γ = 2 and 2.25 and fixed M • = 106  M ⊙. Evidently, the solutions without strong scatterings follow the expected logarithmic profile in ﹩{ \mathcal R }﹩, while solutions that include this effect are highly depleted for low ﹩{ \mathcal R }﹩, corresponding to higher-eccentricity orbits that are more prone to ejections. The impact of strong scatterings is higher for the cluster with higher γ (right panel).
Paper: Extreme-mass-ratio Inspirals in the Strong Segregation Regime—to Inspiral or to Get Ejected?
Authors: Karamveer Kaur, Hagai B. Perets
Figure caption: Evolution of EMRI rates Γ (including strong scatterings; in blue) and ejection rates ﹩{\dot{N}}_{\mathrm{ej}}﹩ (in pink) is shown as a function of time for (left) various γ = 2−2.5 and fixed M • = 4 × 106  M ⊙, and (right) different M • = 104−6  M ⊙ and fixed γ = 2. The ejection rate ﹩{\dot{N}}_{\mathrm{ej}}﹩ is computed for BHs with a ≤ a c0, which are relevant for EMRI formation. As earlier, we depict the rates at time T 0 = T 2b(a c0) (vertical gray lines) as black points.
Paper: Extreme-mass-ratio Inspirals in the Strong Segregation Regime—to Inspiral or to Get Ejected?
Authors: Karamveer Kaur, Hagai B. Perets
Figure caption: EMRI rate ratio Γ/Γ0 as a function of density slope γ for an MW-type NSC with M • = 4 × 106  M ⊙ at various times in color. The black curve corresponds to the suitable reference timescale T 0 for comparison with a steady-state undepleted BH cusp. The rates (at T 0) are suppressed by a factor of ≃3 for γ = 2, while becoming an order of magnitude lower only for very steep cusps with γ ≳ 2.4.