•This ESMO Clinical Practice Guideline provides key recommendations on the management of prostate cancer.•Authorship includes a multidisciplinary group of experts from different institutions and ...countries in Europe.•Key treatment recommendations are provided.•Recommendations have been updated in the light of new evidence.
•Abiraterone acetate with prednisone improved MFS and OS for patients with very-high-risk localised prostate cancer undergoing RT and ADT.•Combining ADT with docetaxel -abiraterone -prednisone in men ...with de novo mHSPC improved both rPFS and OS versus ADT -docetaxel.•Combining ADT with docetaxel and darolutamide in men with mHSPC improved OS versus ADT -docetaxel.•Olaparib improved OS in men with mCRPC and BRCA alterations post-novel androgen receptor axis inhibitor.•Cabazitaxel in men with mCRPC post-novel androgen receptor axis inhibitor and docetaxel improved both rPFS and OS.•177Lu-PSMA-617 in men with mCRPC post-novel androgen receptor axis inhibitor and taxanes improved both rPFS and OS.
Using 25 years of data from uninterrupted monitoring of stellar orbits in the Galactic Center, we present an update of the main results from this unique data set: a measurement of mass and distance ...to Sgr A*. Our progress is not only due to the eight-year increase in time base, but also to the improved definition of the coordinate system. The star S2 continues to yield the best constraints on the mass of and distance to Sgr A*; the statistical errors of 0.13 × 10 6 M and 0.12 kpc have halved compared to the previous study. The S2 orbit fit is robust and does not need any prior information. Using coordinate system priors, the star S1 also yields tight constraints on mass and distance. For a combined orbit fit, we use 17 stars, which yields our current best estimates for mass and distance: M = 4.28 0.10 stat . 0.21 sys × 10 6 M and R 0 = 8.32 0.07 stat . 0.14 sys kpc . These numbers are in agreement with the recent determination of R0 from the statistical cluster parallax. The positions of the mass, of the near-infrared flares from Sgr A*, and of the radio source Sgr A* agree to within 1 mas. In total, we have determined orbits for 40 stars so far, a sample which consists of 32 stars with randomly oriented orbits and a thermal eccentricity distribution, plus eight stars that we can explicitly show are members of the clockwise disk of young stars, and which have lower-eccentricity orbits.
•This ESMO Clinical Practice Guideline provides key recommendations for diagnosis, staging and management of bladder cancer.•Recommendations for personalised medicine are also included.•All ...recommendations were compiled by a multinational and multidisciplinary group of experts.•Recommendations are based on the latest available scientific data and the authors’ expert opinions.•These recommendations are updated continuously in order to include results of the latest clinical trials.
Stars orbiting the compact radio source Sgr A* in the Galactic Center serve as precision probes of the gravitational field around the closest massive black hole. In addition to adaptive ...optics-assisted astrometry (with NACO/VLT) and spectroscopy (with SINFONI/VLT, NIRC2/Keck and GNIRS/Gemini) over three decades, we have obtained 30–100 μas astrometry since 2017 with the four-telescope interferometric beam combiner GRAVITY/VLTI, capable of reaching a sensitivity of
m
K
= 20 when combining data from one night. We present the simultaneous detection of several stars within the diffraction limit of a single telescope, illustrating the power of interferometry in the field. The new data for the stars S2, S29, S38, and S55 yield significant accelerations between March and July 2021, as these stars pass the pericenters of their orbits between 2018 and 2023. This allows for a high-precision determination of the gravitational potential around Sgr A*. Our data are in excellent agreement with general relativity orbits around a single central point mass,
M
•
= 4.30 × 10
6
M
⊙
, with a precision of about ±0.25%. We improve the significance of our detection of the Schwarzschild precession in the S2 orbit to 7
σ
. Assuming plausible density profiles, the extended mass component inside the S2 apocenter (≈0.23″ or 2.4 × 10
4
R
S
) must be ≲3000
M
⊙
(1
σ
), or ≲0.1% of
M
•
. Adding the enclosed mass determinations from 13 stars orbiting Sgr A* at larger radii, the innermost radius at which the excess mass beyond Sgr A* is tentatively seen is
r
≈ 2.5″ ≥ 10× the apocenter of S2. This is in full harmony with the stellar mass distribution (including stellar-mass black holes) obtained from the spatially resolved luminosity function.
We derive new constraints on the mass, rotation, orbit structure, and statistical parallax of the Galactic old nuclear star cluster and the mass of the supermassive black hole. We combine star counts ...and kinematic data from Fritz et al., including 2500 line-of-sight velocities and 10 000 proper motions obtained with VLT instruments. We show that the difference between the proper motion dispersions σ
l
and σ
b
cannot be explained by rotation, but is a consequence of the flattening of the nuclear cluster. We fit the surface density distribution of stars in the central 1000 arcsec by a superposition of a spheroidal cluster with scale ∼100 arcsec and a much larger nuclear disc component. We compute the self-consistent two-integral distribution function f(E, L
z
) for this density model, and add rotation self-consistently. We find that (i) the orbit structure of the f(E, L
z
) gives an excellent match to the observed velocity dispersion profiles as well as the proper motion and line-of-sight velocity histograms, including the double-peak in the v
l
-histograms. (ii) This requires an axial ratio near q
1 = 0.7 consistent with our determination from star counts, q
1 = 0.73 ± 0.04 for r < 70 arcsec. (iii) The nuclear star cluster is approximately described by an isotropic rotator model. (iv) Using the corresponding Jeans equations to fit the proper motion and line-of-sight velocity dispersions, we obtain best estimates for the nuclear star cluster mass, black hole mass, and distance M
*(r < 100 arcsec) = (8.94 ± 0.31|stat ± 0.9|syst) × 106 M⊙, M
• = (3.86 ± 0.14|stat ± 0.4|syst) × 106 M⊙, and R
0 = 8.27 ± 0.09|stat ± 0.1|syst kpc, where the estimated systematic errors account for additional uncertainties in the dynamical modelling. (v) The combination of the cluster dynamics with the S-star orbits around Sgr A* strongly reduces the degeneracy between black hole mass and Galactic Centre distance present in previous S-star studies. A joint statistical analysis with the results of Gillessen et al., gives M
• = (4.23 ± 0.14) × 106 M⊙ and R
0 = 8.33 ± 0.11 kpc.
The GRAVITY instrument on the ESO VLTI pioneers the field of high-precision near-infrared interferometry by providing astrometry at the 10−100
μ
as level. Measurements at this high precision ...crucially depend on the control of systematic effects. We investigate how aberrations introduced by small optical imperfections along the path from the telescope to the detector affect the astrometry. We develop an analytical model that describes the effect of these aberrations on the measurement of complex visibilities. Our formalism accounts for pupil-plane and focal-plane aberrations, as well as for the interplay between static and turbulent aberrations, and it successfully reproduces calibration measurements of a binary star. The Galactic Center observations with GRAVITY in 2017 and 2018, when both Sgr A* and the star S2 were targeted in a single fiber pointing, are affected by these aberrations at a level lower than 0.5 mas. Removal of these effects brings the measurement in harmony with the dual-beam observations of 2019 and 2020, which are not affected by these aberrations. This also resolves the small systematic discrepancies between the derived distance
R
0
to the Galactic Center that were reported previously.
(ProQuest: ... denotes formulae and/or non-USASCII text omitted)We obtain the basic properties of the nuclear cluster of the Milky Way. First, we investigate the structural properties by constructing ...a stellar density map of the central 1000'' using extinction-corrected old star counts from VISTA, WFC3/IR, and VLT/NACO data. We describe the data using two components. The inner, slightly flattened (axis ratio of q= 0.80 + or - 0.04) 7 component is the nuclear cluster, while the outer component corresponds to the stellar component of the circumnuclear zone. For the nuclear cluster, we measure a half-light radius of 178 + or - 0.04 51" thickapproximate + or - 2 pc and a luminosity of M sub(ks)= - 16.0 + or - 0.5. Second, we measure detailed dynamics out to 4 pc. We obtain 10,351 proper motions from AO data, and 2513 radial velocities from VLT/SINFONI data. We determine the cluster mass by means of isotropic spherical Jeans modeling. We fix the distance to the Galactic Center and the mass of the supermassive black hole. We model the cluster either with a constant M/L or with a power law. For the latter case, we obtain a slope of 1.18 + or - 0.06. We get a cluster mass within 100'' of ... for both modeling approaches. A model which includes the observed flattening gives a 47% larger mass (see Chatzopoulos et al.). Our results slightly favor a core over a cusp in the mass profile. By minimizing the number of unbound stars within 8'', we obtain a distance of ... kpc when using an R sub(0) supermassive black hole mass relation from stellar orbits. Combining our results, we obtain ... , which is roughly consistent with a Chabrier IMF.
Two recent papers (Ghez et al. 2008; Gillessen et al. 2009) have estimated the mass of and the distance to the massive black hole (MBH) in the center of the Milky Way using stellar orbits. The two ...astrometric data sets are independent and yielded consistent results, even though the measured positions do not match when simply overplotting the two sets. In this Letter, we show that the two sets can be brought to excellent agreement with each other when we allow for a small offset in the definition of the reference frame of the two data sets. The required offsets in the coordinates and velocities of the origin of the reference frames are consistent with the uncertainties given in Ghez et al. The so-combined data set allows for a moderate improvement of the statistical errors of the mass of and the distance to Sgr A*, but the overall accuracies of these numbers are dominated by systematic errors and the long-term calibration of the reference frame. We obtain R{sub 0} = 8.28 +- 0.15|{sub stat} +- 0.29|{sub sys} kpc and M{sub MBH} = 4.30 +- 0.20|{sub stat} +- 0.30|{sub sys} x 10{sup 6} M{sub sun} as best estimates from a multi-star fit.
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