Total Mass Distribution Research Articles

Cold compression of nuclei induced by antiprotons

On the basis of a dynamical Relativistic Mean Field (RMF) model we study the response of a nucleus on the antiproton implanted in its interior. We solve the Vlasov equation for the antiproton-nuclear system and show assuming a moderately attractive antiproton optical potential that the compressed state is formed on a rather short time scale of about 4-10 fm/c. The evolution of the system after antiproton annihilation is simulated using the Giessen Boltzmann-Uehling-Uhlenbeck (GiBUU) transport model. Finally, several sensitive observables to the antiproton annihilation in a compressed nuclear configuration are proposed, e.g. the nucleon kinetic energy spectra and the total invariant mass distributions of produced mesons.

Early rheumatoid arthritis and body composition

RA is associated with joint destruction and cardiovascular diseases (CVDs). Possible predictors for CVD are early changes in body composition. We therefore evaluated whether lean mass of arms and legs (LMAL), total body fat mass (BFM) or truncal fat distribution (TFD) are altered early in RA, and if so, which factors are associated. We included 132 RA patients (95 women) with disease duration of < or =12 months. Disease activity score (DAS28), HAQ, BMI, comorbidity, smoking and medications were recorded. Total and regional lean mass and fat mass were measured with DXA. Data were compared with 132 age- and gender-matched controls, and possibly associated factors were analysed in linear regression models. LMAL was low in patients for both women and men (P = 0.007 and <0.001, respectively). BMI (P = 0.012), BFM (P = 0.014) and TFD (P < 0.001) were higher than expected in RA women. In bivariate analyses, all adjusted for age and current smoking, disease duration was independently associated with low LMAL in women (P = 0.021). High BFM was associated with HAQ x disease duration in men (P = 0.033) and DAS28 in women (P = 0.011). High TFD was associated with a history of diabetes or CVD in men with RA (P = 0.005). Low LMAL, high BFM and high TFD are present in early RA patients. The long-term significant consequences of these abnormalities need to be determined.

A particle-based approach to close-range blast loading

Abstract A new approach to describe blast loading is suggested, herein referred to as the corpuscular approach. The detonation products are modeled as a set of discrete particles following Maxwell's original kinetic molecular theory. For numerical purposes, the number of molecules has to be greatly reduced compared to what one has in real gases. However, the total molecular mass and temperature dependent velocity distribution are the same as in an ideal gas. Pressure loading on structures is then numerically represented by the momentum transfer as particles impact and rebound from the surface of the structure. The suggested approach has significant advantages compared to today's state-of-the-art continuum-based approaches to fully coupled blast-loading computations. The computational time can be significantly reduced, the method is numerically robust and the approach will easily cope with complex geometries in the fluid–structure interface.

Temperature dependence of yields of secondary organic aerosols from the ozonolysis of &amp;lt;i&amp;gt;α&amp;lt;/i&amp;gt;-pinene and limonene

Abstract. Secondary organic aerosol (SOA) formation has been investigated as a function of temperature and humidity for the ozone-initiated reaction of the two monoterpenes α-pinene (243–313 K) and limonene (253–313 K) using the 84.5 m3 aerosol chamber AIDA. This paper gives an overview of the measurements done and presents parameters specifically useful for aerosol yield calculations. The ozonolysis reaction, selected oxidation products and subsequent aerosol formation were followed using several analytical techniques for both gas and condensed phase characterisation. The effective densities of the SOA were determined by comparing mass and volume size distributions to (1.25±0.10) g cm−3 for α-pinene and (1.3±0.2) g cm−3 for limonene. The detailed aerosol dynamics code COSIMA-SOA proved to be essential for a comprehensive evaluation of the experimental results and for providing parameterisations directly applicable within atmospheric models. The COSIMA-assisted analysis succeeded to reproduce the observed time evolutions of SOA total mass, number and size distributions by adjusting the following properties of two oxidation product proxies: individual yield parameters (αi), partitioning coefficients (Ki), vapour pressures (pi) and effective accommodation coefficients (γi). For these properties temperature dependences were derived and parameterised. Vapour pressures and partitioning coefficients followed classical Clausius – Clapeyron temperature dependences. From this relationship enthalpies of vaporisation were derived for the two more and less volatile product proxies of α-pinene: (59±8) kJ mol−1 and (24±9) kJ mol−1, and limonene: (55±14) kJ mol−1 and (25±12) kJ mol−1. The more volatile proxy components had a notably low enthalpy of vaporisation while the less volatile proxy components gave enthalpies of vaporisation comparable with those of typical products from α-pinene oxidation, e.g. pinonaldehyde and pinonic acid.

X-ray and strong lensing mass estimate of MS2137.3-2353

We present new mass estimates of the galaxy cluster MS2137.3-2353, inferred from X-ray and strong lensing analyses. This cluster exhibits an outstanding strong lensing configuration and indicates a well-relaxed dynamical state, being most suitable for a mass reconstruction which combines both techniques. Despite this, several previous studies have claimed a significant discrepancy between the X-ray and the strong lensing mass estimates. The primary aim of this paper is to address and explain this mismatch. For this purpose, we have analysed Chandra observations to recover the profiles of the intra-cluster medium properties and, assuming a functional form for the matter density, the total mass distribution. The notable strong-lensing features of MS2137.3 allow us to reconstruct its projected mass in the central regions with good accuracy, by taking advantage of the lensing inversion code Lenstool. We find a good agreement between our X-ray and strong lensing mass estimates for MS2137, leading to a mean, extrapolated value of M_200 ~ 4.4 +/- 0.3*10^14 M_sun, under the assumption of the Navarro-Frenk-White (NFW) density profile. However, the strong lensing mass estimate is affected by the details of the BCG mass modeling. In particular, we do not find evidence for a high concentration for the NFW density profile, as reported in some earlier works.

Total mass distributions of Sersic galaxies from photometry and central velocity dispersion

We develop a novel way of finding total mass density profiles in Sersic ellipticals, to about 3 times the major axis effective radius, using no other information other than what is typically available for distant galaxies, namely the observed surface brightness distribution and the central velocity dispersion $\sigma_0$. The luminosity density profile of the observed galaxy is extracted by deprojecting the measured brightness distribution and scaling it by a fiduciary, step-function shaped, $raw$ mass-to-light ratio profile ($M/L$). The resulting raw, discontinuous, total, 3-D mass density profile is then smoothed according to a proposed smoothing prescription. The parameters of this raw $M/L$ are characterised by implementing the observables in a model-based study. The complete characterisation of the formalism is provided as a function of the measurements of the brightness distribution and $\sigma_0$. The formalism, thus specified, is demonstrated to yield the mass density profiles of a suite of test galaxies and is successfully applied to extract the gravitational mass distribution in NGC 3379 and NGC 4499, out to about 3 effective radii.

Revealing the Properties of Dark Matter in the Merging Cluster MACS J0025.4−1222

We constrain the physical nature of dark matter using the newly identified massive merging galaxy cluster MACS J0025.4–1222. As was previously shown by the example of the Bullet Cluster (1E 0657–56), such systems are ideal laboratories for detecting isolated dark matter and distinguishing between cold dark matter (CDM) and other scenarios (e.g., self-interacting dark matter, alternative gravity theories). MACS J0025.4–1222 consists of two merging subclusters of similar richness at z = 0.586. We measure the distribution of X-ray-emitting gas from Chandra X-ray data and find it to be clearly displaced from the distribution of galaxies. A strong (information from highly distorted arcs) and weak (using weakly distorted background galaxies) gravitational lensing analysis based on Hubble Space Telescope observations and Keck arc spectroscopy confirms that the subclusters have near-equal mass. The total mass distribution in each of the subclusters is clearly offset (at >4 σ significance) from the peak of the hot X-ray-emitting gas (the main baryonic component) but aligned with the distribution of galaxies. We measure the fractions of mass in hot gas (0.09+ 0.07−0.03) and stars (0.010+ 0.007−0.004), consistent with those of typical clusters, finding that dark matter is the dominant contributor to the gravitational field. Under the assumption that the subclusters experienced a head-on collision in the plane of the sky, we obtain an order-of-magnitude estimate of the dark matter self-interaction cross section of σ/m < 4 cm 2 g−1, reaffirming the results from the Bullet Cluster on the collisionless nature of dark matter.

Total mass biases in X-ray galaxy clusters

Context. The exploitation of clusters of galaxies as cosmological probes relies on accurate measurements of their total gravitating mass. X-ray observations provide a powerful means of probing the total mass distribution in galaxy clusters, but might be affected by observational biases and rely on simplistic assumptions originating from our limited understanding of the intracluster medium physics.

Mass distribution and orbital anisotropy of early-type galaxies: constraints from the mass plane

Massive early-type galaxies are observed to lie on the mass plane (MP), a two-dimensional manifold in the space of effective radius Re, projected mass M p (measured via strong gravitational lensing) and projected stellar velocity dispersion σ e2 withinRe/2. The MP is less ‘tilted’ than the traditional Fundamental Plane, and the two have comparable associated scatter. This means that the dimensionless structure parameter ce2 = 2GM p /(Reσ 2 ) is a nearly universal constant in the range σ e2 = 175–400 km s −1 . This finding can be used to constrain the mass distribution and internal dynamics of early-type galaxies: in particular, we explore the dependence of ce2 on light profile, dark matter distribution, and orbital anisotropy for several families of spherical galaxy models. We find that a relatively wide class of models has values of ce2 in the observed range, because ce2 is not very strongly sensitive to the mass distribution and orbital anisotropy. The degree of fine-tuning required to match the small intrinsic scatter of ce2 depends on the considered family of models: if the total mass distribution is isothermal (∝ r −2 ), a broad range of stellar luminosity profile and anisotropy is consistent with the observations, while Navarro, Frenk & White dark matter haloes require more fine-tuning of the stellar mass fraction, luminosity profile and anisotropy. If future data can cover a broader range of masses, the MP could be seen to be tilted by the known non-homology of the luminosity profiles of early-type galaxies, and the value of any such tilt would provide a discriminant between models for the total mass–density profile of the galaxies.

Dynamical simulation of bound antiproton-nuclear systems and observable signals of cold nuclear compression

On the basis of the kinetic equation with self-consistent relativistic mean fields acting on baryons and antibaryons, we study dynamical response of the nucleus to an antiproton implanted in its interior. By solving numerically the time-dependent Vlasov equation, we show that the compressed state is formed on a rather short time scale of about 4-10 fm/c. This justifies the assumption, that the antiproton annihilation may happen in the compressed nuclear environment. The evolution of the nucleus after antiproton annihilation is described by the same kinetic equation including collision terms. We show, that nucleon kinetic energy spectra and the total invariant mass distributions of produced mesons are quite sensitive observables to the antiproton annihilation in the compressed nucleus.

USING WEAK-LENSING DILUTION TO MEASURE LIGHT PROPERTIES OF A1689

Weak-lensing induced by clusters of galaxies can probe the total mass distribution out to the virial radius of the cluster, regardless of the nature of the mass or its dynamical state. To make a robust analysis, the cluster and background galaxy populations need to be separated. The E/S0 sequence of a cluster defines a boundary redward of which a reliable weak-lensing signal can be obtained from background galaxies, uncontaminated by the cluster. Below this limit, the signal is diluted by the proportion of unlensed cluster members. Employing deep Subaru and HST/ACS images of the massive cluster A1689, we use this dilution effect to carefully separate between the cluster members and the background, and thus derive the cluster light profile and luminosity functions to large radius. The light profile of A1689 is found to decline steadily to the limit of the data, r &lt; 2 h−1 Mpc , with a constant slope, d log (L)/d log (r) = −1.12 ± 0.06. We derive a cluster luminosity function with a flat faint-end slope of α = −1.05 ± 0.07, nearly independent of radius and with no faint upturn to Mi′ &lt; −12. The major advantage of this new approach is that no subtraction of far-field background counts is required.

Constraining the Mass Profiles of Stellar Systems: Schwarzschild Modeling of Discrete Velocity Data Sets

We present a new Schwarzschild orbit superposition code designed to model discrete data sets composed of velocity measurements of individual kinematic tracers in a dynamical system. This constitutes an extension of previous implementations that can only address continuous data in the form of (the moments of) velocity distributions, thus avoiding potentially important losses of information due to data binning. The code can handle any combination of velocity components, i.e., only line-of-sight velocities, only proper motions, or both. The code determines the combination of orbital mass weights as a function of the three integrals of motion E, Lz, and I3 that best reproduces, in a maximum likelihood sense, the available kinematic and photometric observations in a given axisymmetric gravitational potential. The fully numerical approach ensures considerable freedom on the form of the distribution function -->f(E, Lz, I3) , avoiding restrictive assumptions about the degree of orbital (an)isotropy. We describe the implementation of the discrete code and present a series of performance tests based on the modeling of simulated data sets generated from a known distribution function. Exploring pseudo-data sets with varying degrees of overall rotation and different inclinations on the sky, we study the results as a function of relevant observational variables such as the size of the data set and the type of velocity information available. The discrete Schwarzschild code recovers the original orbital structure, mass-to-light ratio, and inclination of the input data sets to satisfactory accuracy. The code will be valuable, e.g., for modeling stellar motions in Galactic globular clusters and the motions of individual stars, planetary nebulae, or globular clusters in nearby galaxies. This can shed new light on the total mass distributions of these systems, with central black holes and dark halos being of particular interest.

Unveiling dark haloes in lensing galaxies

We present a spatially resolved comparison of the stellar mass and total mass surface distributions of nine early-type galaxies. The galaxies are a subset of the Sloan Lens ACS Survey. The total mass distributions are obtained by exploring pixelated mass models that reproduce the lensed images. The stellar mass distributions are derived from population-synthesis models fit to the photometry of the lensing galaxies. Uncertainties – mainly model degeneracies – are also computed. Stars can account for all the mass in the inner regions. A Salpeter initial mass function actually gives too much stellar mass in the inner regions and hence appears ruled out. Dark matter becomes significant by the half-light radius and becomes increasingly dominant at larger radii. The stellar and dark components are closely aligned, but the actual ellipticities are not correlated. Finally, we attempt to intuitively summarize the results by rendering the density, stellar versus dark ratio, and uncertainties as false-colour maps.

Molecular lines from protoplanetary nebulae: observations with ALMA

Planetary nebulae (PNe) are formed in a very fast process. In just about 1000 years, the nebula evolves from a spherical and slowly expanding AGB envelope to a PN, with usually axial symmetry and high axial velocities. Molecular lines are known to probe most of the nebular material in young PNe and protoplanetary nebulae (PPNe), and are therefore very useful to study such an impressive evolution. Many quantitative results on these objects have been so obtained, including general structure, total mass and density distribution, kinetic temperatures, velocity fields, etc. Existing observations probe both the gas accelerated by post-AGB shocks and the quiescent components. But the study of crucial regions to understand PN formation (recently shocked shells, regions heated by the stellar UV and inner rotating disks) requires observations at higher frequency and with better spatial resolution.

Globulettes as Seeds of Brown Dwarfs and Free-Floating Planetary-Mass Objects

Some H II regions surrounding young stellar clusters contain tiny dusty clouds, which on photos look like dark spots or teardrops against a background of nebular emission. From our collection of H? images of 10 H II regions gathered at the Nordic Optical Telescope, we found 173 such clouds, which we call globulettes, since they are much smaller than normal globules and form a distinct class of objects. Many globulettes are quite isolated and located far from the molecular shells and elephant trunks associated with the regions. Others are attached to the trunks (or shells), suggesting that globulettes may form as a consequence of erosion of these larger structures. None of our objects appear to contain stellar objects. The globulettes were measured for position, dimension, and orientation, and we find that most objects are smaller than 10 kAU. The Rosette Nebula and IC 1805 are particularly rich in globulettes, for which the size distributions peak at mean radii of ~2.5 kAU, similar to what was found by Reipurth and coworkers and De Marco and coworkers for similar objects in other regions. We estimate total mass and density distributions for each object from extinction measures and conclude that a majority contain <13 MJ, corresponding to planetary-mass objects. We then estimate the internal thermal and potential energies and find, when also including the effects from the outer pressure, that a large fraction of the globulettes could be unstable and would contract on short timescales, <10 6 yr. In addition, the radiation pressure and ram pressure exerted on the side facing the clusters would stimulate contraction. Since the globulettes are not screened from stellar light by dust clouds farther in, one would expect photoevaporation to dissolve the objects. However, surprisingly few objects show bright rims or teardrop forms. We calculate the expected lifetimes against photoevaporation. These lifetimes scatter around 4 ? 106 yr, much longer than estimated in previous studies and also much longer than the free-fall time. We conclude that a large number of our globulettes have time to form central low-mass objects long before the ionization front, driven by the impinging Lyman photons, has penetrated far into the globulette. Hence, the globulettes may be one source in the formation of brown dwarfs and free-floating planetary-mass objects in the galaxy.

Particle size and composition distribution analysis of automotive brake abrasion dusts for the evaluation of antimony sources of airborne particulate matter

Abrasion dusts from three types of commercially available non-steel brake pads were generated by a brake dynamometer at disk temperatures of 200, 300 and 400 °C. The number concentration of the abrasion dusts and their aerodynamic diameters ( D p) were measured by using an aerodynamic particle sizer (APS) spectrometer with high temporal and size resolution. Simultaneously, the abrasion dusts were also collected based on their size by using an Andersen low-volume sampler, and the concentrations of metallic elements (K, Ti, Fe, Cu, Zn, Sb and Ba) in the size-classified dusts were measured by ICP-AES and ICP-MS. The number distributions of the brake abrasion dusts had a peak at D p values of 1 and 2 μm; this peak shifted to the coarse side with an increase in the disk temperature. The mass distributions calculated from the number distributions have peaks between D p values of 3 and 6 μm. The shapes of the elemental mass distributions (Ti, Fe, Cu, Zn, Sb and Ba) in size-classified dusts were very similar to the total mass distributions of the brake abrasion dusts. These experimental results indicated that the properties of brake abrasion dusts were consistent with the characteristics of Sb-enriched fine airborne particulate matter. Based on these findings and statistical data, the estimation of Sb emission as airborne particulate matter from friction brakes was also discussed.

Effects of Treatment With Testosterone Alone or in Combination With Estrogen on Insulin Sensitivity in Postmenopausal Women

Treatment with androgens such as testosterone has a number of salutary effects on postmenopausal women, including greater energy, improved sexual function, preservation of bone mass, and possibly a protective effect on the breast. There is concern, however, that excessive androgen may lead to an insulin-resistant state. This study addressed the issue of insulin sensitivity using testosterone undecenoate (TU), an orally active preparation with only minor liver-related side effects. Participants were 63 naturally postmenopausal women in good general health, 2 of whom were obese. The women were randomly assigned to receive 40 mg testosterone (T) in the form of TU every other day, 2 mg estradiol (E) valerate daily, or both treatments (T+E), all for 3 months. The euglycemic hyperinsulinemic clamp technique served to estimate insulin sensitivity. The 3 groups were similar in age, body weight, bone mass index, blood pressure, serum hormone levels, and a history of using conventional hormone therapy. Diastolic but not systolic blood pressure fell significantly in the T group but, in general, treatment was well tolerated. No hyperandrogenic signs such as acne or hirsutism developed. Total serum testosterone rose to median levels of 35 to 46 ng/dL in both the T and T+E groups-within the normal range for premenopausal women. Fasting blood glucose levels did not change significantly, but plasma insulin levels fell significantly in the E and T+E groups. Basal insulin sensitivity increased significantly in E-treated women only. Steady-state plasma insulin and blood glucose levels were similar in all groups before and after treatment. Whole-body glucose uptake fell significantly by approximately 20% in the T group and also after combined treatment. No significant correlation was found between changes in free T levels and altered anthropometric or metabolic variables. Body weight increased by approximately 1 kg, a small but significant change, in all treatment groups. Total body fat mass and fat distribution remained stable, but total lean body mass increased significantly in the T+E group. Total cholesterol fell significantly by approximately 20 mg/dL in the same group. High-density lipoprotein cholesterol decreased significantly in the T group but increased in the E group. Low-density lipoprotein cholesterol decreased significantly in both E-treated groups. It appears that short-term treatment with TU, alone or combined with estradiol, induces insulin resistance in postmenopausal women and also worsens the serum lipid profile. Treatment may, however, increase lean body mass. More work is needed to appreciate the clinical significance of these findings.

The Influence of Baryons on the Mass Distribution of Dark Matter Halos

Using a set of high-resolution N-body/SPH cosmological simulations with identical initial conditions but run with different numerical setups, we investigate the influence of baryonic matter on the mass distribution of dark halos when radiative cooling is not included. We compare the concentration parameters of about 400 massive halos with virial mass from 1013 to 7.1 × 1014 h-1 M☉. We find that the concentration parameters for the total mass and dark matter distributions in nonradiative simulations are on average larger by ~3% and 10% than those in a pure dark matter simulation. Our results indicate that the total mass density profile is little affected by a hot gas component in the simulations. After carefully excluding the effects of resolutions and spurious two-body heating between dark matter (DM) and gas particles, we conclude that the increase of the DM concentration parameters is due to interactions between baryons and DM. We demonstrate this with the aid of idealized simulations of two-body mergers. The results of individual halos simulated with different mass resolutions show that in the gas profiles of densities, temperature and entropy are subjects of mass resolution of SPH particles. In particular, we find that in the inner parts of halos, as the SPH resolution increases the gas density becomes higher but both the entropy and temperature decrease.

The Sloan Lens ACS Survey. III. The Structure and Formation of Early‐Type Galaxies and Their Evolution since z ≈ 1

We present a joint gravitational lensing and stellar-dynamical analysis of 15 massive field early-type galaxies selected from the Sloan Lens ACS (SLACS) Survey. The following numerical results are found: (1) A joint likelihood gives an average logarithmic density slope for the total mass density of ⟨γ'⟩ = 2.01 (68% CL; ρtot ∝ r) inside ⟨REinst⟩ = 4.2 ± 0.4 kpc (rms of 1.6 kpc) for isotropic models. The inferred intrinsic rms spread in logarithmic density slopes is σ = 0.12. (2) The average position-angle difference between the light distribution and the total mass distribution is found to be ⟨Δθ⟩ = 0° ± 3° (rms of 10°), setting an upper limit of ⟨γext⟩ ≲ 0.035 on the average external shear. The total mass has an average ellipticity ⟨qSIE⟩ = 0.78 ± 0.03 (rms of 0.12), which correlates extremely well with the stellar ellipticity, q*, resulting in ⟨qSIE/q*⟩ = 0.99 ± 0.03 (rms of 0.11) for σ ≳ 225 km s-1 omitting three S0 lens galaxies. (3) The average projected dark matter mass fraction is inferred to be ⟨fDM⟩ = 0.25 ± 0.06 (rms of 0.22) inside ⟨REinst⟩, using the stellar mass-to-light ratios derived from the fundamental plane as priors. (4) Combined with results from the Lenses Structure and Dynamics (LSD) Survey at z ≳ 0.3, we find no significant evolution of the total density slope inside one effective radius for galaxies with σap ≥ 200 km s-1: a linear fit gives α ≡ d⟨γ'⟩/dz = 0.23 ± 0.16 (1 σ) for the range z = 0.08-1.01. The small scatter and absence of significant evolution in the inner density slopes suggest a collisional scenario in which gas and dark matter strongly couple during galaxy formation, leading to a total mass distribution that rapidly converges to dynamical isothermality.

Detection Rate Estimates of Gravity Waves Emitted during Parabolic Encounters of Stellar Black Holes in Globular Clusters

The rapid advance of gravitational wave (GW) detector facilities makes it very important to estimate the event rates of possible detection candidates. We consider an additional possibility of GW bursts produced during parabolic encounters (PEs) of stellar-mass compact objects in globular clusters (GCs). We estimate the rate of successful detections for specific detectors: the initial Laser Interferometric Gravitational-Wave Observatory (InLIGO), the French-Italian gravitational wave antenna VIRGO, the near-future Advanced-LIGO (AdLIGO), the space-based Laser Interferometric Space Antenna (LISA), and the Next Generation LISA (NGLISA). Simple GC models are constructed to account for the compact object mass function, mass segregation, number density distribution, and velocity distribution. We both calculate encounters classically and account for general relativistic corrections by extrapolating the results for infinite mass ratios. We also include the cosmological redshift of waveforms and event rates. We find that typical PEs with masses m1 = m2 = 40 M☉ are detectable with matched filtering over a signal-to-noise ratio S/N = 5 within a distance dL ~ 200 Mpc for InLIGO and VIRGO, z = 1 for AdLIGO, 0.4 Mpc for LISA, and 1 Gpc for NGLISA. We estimate single data stream detection rates of 5.5 × 10-5 yr-1 for InLIGO, 7.2 × 10-5 yr-1 for VIRGO, 0.063 yr-1 for AdLIGO, 2.9 × 10-6 yr-1 for LISA, and 1.0 yr-1 for NGLISA, for reasonably conservative assumptions. These estimates are subject to uncertainties in the GC parameters, most importantly the total number and mass distribution of BHs in the cluster core. In reasonably optimistic cases, we get ≳1 detection for AdLIGO per year. We expect that a coincident analysis using multiple detectors and accounting for GW recoil capture significantly increases the detection rates. The regular detection of GWs during PEs would provide a unique observational probe for constraining the stellar BH mass function of dense clusters.