Untersuchungen über die Folgen des Verlustes von retinalem Pigmentepithel nach chirurgischer Extraktion von chorioidalen Neovaskularisationen aufgrund altersbedingter Makuladegeneration

Einleitung: Die altersbedingte Makuladegeneration (AMD) ist der führende Grund für Blindheit im Sinne des Gesetzes in den westlichen Industrienationen mit stark steigender Inzidenz und Prävalenz. Es gibt verschiedene Formen der AMD. Besonders die so genannte „feuchte Form“, die durch die Entstehung von chorioidalen Neovaskularisationsmembranen (CNV) am Ort des schärfsten Sehens gekennzeichnet ist, führt oft zu einem rasch progredienten Abfall des Visus. Für die Diagnostik solcher Neovaskularisationsmembranen dient neben der klinischen Untersuchung vor allem die Darstellung mittels Fluoreszenzangiographie (FLA), anhand derer auch eine weitere Einteilung von CNVs in verschiedene Typen (z.B. „klassische“ oder „okkulte“ Membranen) vorgenommen wird. Auch Defekte im retinalen Pigmentepithel, das topographisch der Netzhaut benachbart liegt, lassen sich diagnostisch mittels der FLA darstellen und quantifizieren. Bis dato stand als einzige aktive Therapieoption für diese Membranen die Verödung mittels Argon-Laser zur Verfügung, die allerdings auch unweigerlich mit einer Zerstörung der darüber liegenden neurosensorischen Netzhaut einhergeht. Daher wurde an der Augenklinik der Ludwig-Maximilians-Universität der Weg der chirurgischen Intervention beschritten, bei dem nach einer Pars-Plana-Vitrektomie und Retinotomie die entsprechende subfoveal gelegene Membran oder Blutung aus dem Subretinalraum extrahiert wird. Zwangsweise kommt es – wie sich herausstellte – dabei durch die Membranstruktur bedingt jedoch auch immer zu einer Mitentfernung von retinalem Pigmentepithel (RPE), das für die Netzhaut eine trophische Funktion besitzt. Methodik: Bei der Nachbeobachtung der Patienten fiel auf, dass es zu Rezidiven von CNVs kam. Ausgangspunkt dieser Studie war die Fragestellung, ob ein Zusammenhang zwischen Größe der RPE-Defekte und Rezidivwahrscheinlichkeit besteht. Hierzu wurden retrospektiv die Krankenakten und Fluoreszenzangiographien von 51 operierten Patienten ausgewertet, die Größe der RPE-Defekte auf postoperativ angefertigten Angiographien ausgemessen und zum Auftreten eines Rezidives bzw. zum Rezidivzeitpunkt in Relation gesetzt. Ergebnisse: Dabei konnte festgestellt werden, dass kleinere RPE-Defekte mit einer erhöhten Wahrscheinlichkeit sowohl für ein Auftreten eines Rezidives, als auch mit der für einen früheren Rezidivzeitpunkt einhergehen. Des weiteren ergab sich eine negative Korrelation zwischen der Größe des RPE-Defektes und dem bestkorrigierten Visus zu verschiedenen postoperativen Zeitpunkten während des ersten Jahres nach der Operation (bei einer Nachbeobachtungszeit von bis zu vier Jahren). Dementsprechend ergab sich auch eine positive Korrelation mit dem benötigten Vergrößerungsfaktor einiger Patienten. Zudem lässt sich eine Funktionsdiagnostik der Netzhaut, v.a. der Makula, mit Hilfe der Mikroperimetrie betreiben. Bei den mit dieser Diagnostikmöglichkeit untersuchten Patienten zeigten sich statistisch signifikante positive Korrelationen zwischen den RPE-Defekten und den gemessenen absoluten und relativen Skotomen. Ein statistischer Zusammenhang zwischen der Größe des RPE-Defektes und einer Visusverbesserung oder –verschlechterung konnte dabei nicht festgestellt werden, jedoch eine positive Korrelation zwischen präoperativen und dem besten postoperativ erreichten Visus. Diskussion: Mit Hilfe der chirurgischen Membranektomie lässt sich zwar eine Stabilisierung der Sehschärfe erreichen, die entstandenen RPE-Defekte sind aber Ursache des fehlenden Anstiegs des Visus. Andere Faktoren wie Vorschädigungen der Strukturen von Aderhaut, Bruch’scher Membran, RPE und Netzhaut durch den Krankheitsprozess spielen eine zusätzliche Rolle. Auch Lokalisation und Wachstumsmuster von Neovaskularisationen können einen Einfluss auf die postoperativ erreichten Sehschärfen haben. Dies zeigt sich insbesondere im Vergleich mit in der Literatur angegebenen Ergebnissen nach subfovealer Membranektomie bei anderen Erkrankungen, die mit der Bildung chorioidaler Neovaskularisationen einherge-hen. Die Beobachtung, dass kleinere RPE-Defekte mit einer erhöhten Rezidivrate einhergehen, lässt Rückschlüsse auf die mögliche Rolle des RPE bei der primären Krankheitsentstehung zu. Insbesondere unterstützt sie die These, dass zwischen zentralem und mittelperipherem retina-len Pigmentepithel Unterschiede bestehen z.B. in Bezug auf die Synthese von Wachstumsfak-toren, die bei der Entstehung solcher Membranen eine entscheidende Rolle spielen oder al-tersbedingte Unterschiede bezüglich der regenerativen Kapazität der RPE-Zellen. Für künfti-ge Therapieoptionen mit dem Resultat einer verbesserten Sehschärfe müssten Wege gefunden werden, den geschädigten Komplex von Bruch’scher Membran und RPE wiederherzustellen

Retinal Architecture in ​\u3cem\u3eRGS9-\u3c/em\u3e and ​\u3cem\u3eR9AP\u3c/em\u3e-Associated Retinal Dysfunction (Bradyopsia)

Purpose To characterize photoreceptor structure and mosaic integrity in subjects with RGS9- and R9AP-associated retinal dysfunction (bradyopsia) and compare to previous observations in other cone dysfunction disorders such as oligocone trichromacy. Design Observational case series. Methods setting: Moorfields Eye Hospital (United Kingdom) and Medical College Wisconsin (USA). study population: Six eyes of 3 subjects with disease-causing variants in RGS9 or R9AP. main outcome measures: Detailed retinal imaging using spectral-domain optical coherence tomography and confocal adaptive-optics scanning light ophthalmoscopy. Results Cone density at 100 μm from foveal center ranged from 123 132 cones/mm2to 140 013 cones/mm2. Cone density ranged from 30 573 to 34 876 cones/mm2 by 600 μm from center and from 15 987 to 16,253 cones/mm2 by 1400 μm from center, in keeping with data from normal subjects. Adaptive-optics imaging identified a small, focal hyporeflective lesion at the foveal center in both eyes of the subject with RGS9-associated disease, corresponding to a discrete outer retinal defect also observed on spectral-domain optical coherence tomography; however, the photoreceptor mosaic remained intact at all other observed eccentricities. Conclusions Bradyopsia and oligocone trichromacy share common clinical symptoms and cannot be discerned on standard clinical findings alone. Adaptive-optics imaging previously demonstrated a sparse mosaic of normal wave-guiding cones remaining at the fovea, with no visible structure outside the central fovea in oligocone trichromacy. In contrast, the subjects presented in this study with molecularly confirmed bradyopsia had a relatively intact and structurally normal photoreceptor mosaic, allowing the distinction between these disorders based on the cellular phenotype and suggesting different pathomechanisms

Deep phenotyping of PROM1-associated retinal degeneration

BACKGROUND/AIMS: The purpose of this study was to investigate retinal structure in detail of subjects with autosomal-dominant (AD) and autosomal-recessive (AR) PROM1-associated retinal degeneration (PROM1-RD), study design: institutional, cross-sectional study. METHODS: Four eyes from four subjects (three with AD and one with AR) PROM1-RD were investigated by ophthalmic examination including best-corrected visual acuity (BCVA) and multimodal retinal imaging: fundus autofluorescence (FAF), spectral-domain optical coherence tomography (SD-OCT) and adaptive optics scanning light ophthalmoscopy. Quantitative assessment of atrophic lesions determined by FAF, thickness of individual retinal layers and cone photoreceptor quantification was performed. RESULTS: BCVA ranged from 20/16 to 20/200. Initial pathological changes included the presence of hyperautofluorescent spots on FAF imaging, while later stages demonstrated discrete areas of atrophy. In all patients, thinning of the outer retinal layers on SD-OCT with varying degrees of atrophy could be detected depending on disease-causing variants and age. Cone density was quantified both in central and/or at different eccentricities from the fovea. Longitudinal assessments were possible in two patients. CONCLUSIONS: PROM1-RD comprises a wide range of clinical phenotypes. Depending on the stage of disease, the cone mosaic in PROM1-RD is relatively preserved and can potentially be targeted by cone-directed interventions

Intravitreal ranibizumab versus isovolemic hemodilution in the treatment of macular edema secondary to central retinal vein occlusion: Twelve-month results of a prospective, randomized, multicenter trial

PURPOSE This is a prospective, randomized, multicenter, investigator-initiated trial to evaluate the 12-month effectiveness of isovolemic hemodilution (IH) with prompt versus deferred intravitreal injections (IVI) of ranibizumab 0.5 mg for the treatment of macular edema secondary to early central retinal vein occlusion (CRVO). METHODS Eyes with macular edema due to CRVO having occurred not more than 8 weeks previously received either monthly ranibizumab IVI in combination with IH (group I, n = 28) or IH alone (group II, n = 30). From month 2 to 12, the patients in both groups could be treated with monthly intravitreal ranibizumab. The main outcome variables were gain of visual acuity and the course of central retinal thickness as measured with optical coherence tomography. RESULTS At 12 months, eyes in group I on average gained +28.1 (±19.3) letters compared to +25.2 (±20.9) letters in group II (p = 0.326). This result was achieved with significantly fewer injections in group II. Additionally, 30% of the eyes in group II did not need ranibizumab IVI during the 12 months of the trial. CONCLUSION Ranibizumab IVI in addition to IH proved to be highly effective in increasing visual acuity and reducing macular edema secondary to CRVO. Initial IH in early CRVO may be a first treatment option in patients anxious about IVI

The SDSS-III Baryon Oscillation Spectroscopic Survey: Quasar Target Selection for Data Release Nine

The SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS), a five-year spectroscopic survey of 10,000 deg^2, achieved first light in late 2009. One of the key goals of BOSS is to measure the signature of baryon acoustic oscillations in the distribution of Ly-alpha absorption from the spectra of a sample of ~150,000 z>2.2 quasars. Along with measuring the angular diameter distance at z\approx2.5, BOSS will provide the first direct measurement of the expansion rate of the Universe at z > 2. One of the biggest challenges in achieving this goal is an efficient target selection algorithm for quasars over 2.2 < z < 3.5, where their colors overlap those of stars. During the first year of the BOSS survey, quasar target selection methods were developed and tested to meet the requirement of delivering at least 15 quasars deg^-2 in this redshift range, out of 40 targets deg^-2. To achieve these surface densities, the magnitude limit of the quasar targets was set at g <= 22.0 or r<=21.85. While detection of the BAO signature in the Ly-alpha absorption in quasar spectra does not require a uniform target selection, many other astrophysical studies do. We therefore defined a uniformly-selected subsample of 20 targets deg^-2, for which the selection efficiency is just over 50%. This "CORE" subsample will be fixed for Years Two through Five of the survey. In this paper we describe the evolution and implementation of the BOSS quasar target selection algorithms during the first two years of BOSS operations. We analyze the spectra obtained during the first year. 11,263 new z>2.2 quasars were spectroscopically confirmed by BOSS. Our current algorithms select an average of 15 z > 2.2 quasars deg^-2 from 40 targets deg^-2 using single-epoch SDSS imaging. Multi-epoch optical data and data at other wavelengths can further improve the efficiency and completeness of BOSS quasar target selection. [Abridged]Comment: 33 pages, 26 figures, 12 tables and a whole bunch of quasars. Submitted to Ap

The Eighth Data Release of the Sloan Digital Sky Survey: First Data from SDSS-III

The Sloan Digital Sky Survey (SDSS) started a new phase in August 2008, with new instrumentation and new surveys focused on Galactic structure and chemical evolution, measurements of the baryon oscillation feature in the clustering of galaxies and the quasar Ly alpha forest, and a radial velocity search for planets around ~8000 stars. This paper describes the first data release of SDSS-III (and the eighth counting from the beginning of the SDSS). The release includes five-band imaging of roughly 5200 deg^2 in the Southern Galactic Cap, bringing the total footprint of the SDSS imaging to 14,555 deg^2, or over a third of the Celestial Sphere. All the imaging data have been reprocessed with an improved sky-subtraction algorithm and a final, self-consistent photometric recalibration and flat-field determination. This release also includes all data from the second phase of the Sloan Extension for Galactic Understanding and Evolution (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars at both high and low Galactic latitudes. All the more than half a million stellar spectra obtained with the SDSS spectrograph have been reprocessed through an improved stellar parameters pipeline, which has better determination of metallicity for high metallicity stars.Comment: Astrophysical Journal Supplements, in press (minor updates from submitted version

The Baryon Oscillation Spectroscopic Survey of SDSS-III

The Baryon Oscillation Spectroscopic Survey (BOSS) is designed to measure the scale of baryon acoustic oscillations (BAO) in the clustering of matter over a larger volume than the combined efforts of all previous spectroscopic surveys of large scale structure. BOSS uses 1.5 million luminous galaxies as faint as i=19.9 over 10,000 square degrees to measure BAO to redshifts z<0.7. Observations of neutral hydrogen in the Lyman alpha forest in more than 150,000 quasar spectra (g<22) will constrain BAO over the redshift range 2.15<z<3.5. Early results from BOSS include the first detection of the large-scale three-dimensional clustering of the Lyman alpha forest and a strong detection from the Data Release 9 data set of the BAO in the clustering of massive galaxies at an effective redshift z = 0.57. We project that BOSS will yield measurements of the angular diameter distance D_A to an accuracy of 1.0% at redshifts z=0.3 and z=0.57 and measurements of H(z) to 1.8% and 1.7% at the same redshifts. Forecasts for Lyman alpha forest constraints predict a measurement of an overall dilation factor that scales the highly degenerate D_A(z) and H^{-1}(z) parameters to an accuracy of 1.9% at z~2.5 when the survey is complete. Here, we provide an overview of the selection of spectroscopic targets, planning of observations, and analysis of data and data quality of BOSS.Comment: 49 pages, 16 figures, accepted by A

The Ninth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey

The Sloan Digital Sky Survey III (SDSS-III) presents the first spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS). This ninth data release (DR9) of the SDSS project includes 535,995 new galaxy spectra (median z=0.52), 102,100 new quasar spectra (median z=2.32), and 90,897 new stellar spectra, along with the data presented in previous data releases. These spectra were obtained with the new BOSS spectrograph and were taken between 2009 December and 2011 July. In addition, the stellar parameters pipeline, which determines radial velocities, surface temperatures, surface gravities, and metallicities of stars, has been updated and refined with improvements in temperature estimates for stars with T_eff<5000 K and in metallicity estimates for stars with [Fe/H]>-0.5. DR9 includes new stellar parameters for all stars presented in DR8, including stars from SDSS-I and II, as well as those observed as part of the SDSS-III Sloan Extension for Galactic Understanding and Exploration-2 (SEGUE-2). The astrometry error introduced in the DR8 imaging catalogs has been corrected in the DR9 data products. The next data release for SDSS-III will be in Summer 2013, which will present the first data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) along with another year of data from BOSS, followed by the final SDSS-III data release in December 2014.Comment: 9 figures; 2 tables. Submitted to ApJS. DR9 is available at http://www.sdss3.org/dr

Cosmological implications of baryon acoustic oscillation measurements

We derive constraints on cosmological parameters and tests of dark energy models from the combination of baryon acoustic oscillation (BAO) measurements with cosmic microwave background (CMB) data and a recent reanalysis of Type Ia supernova (SN) data. In particular, we take advantage of high-precision BAO measurements from galaxy clustering and the Lyman-α forest (LyaF) in the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). Treating the BAO scale as an uncalibrated standard ruler, BAO data alone yield a high confidence detection of dark energy; in combination with the CMB angular acoustic scale they further imply a nearly flat universe. Adding the CMB-calibrated physical scale of the sound horizon, the combination of BAO and SN data into an “inverse distance ladder” yields a measurement of H0 =67.3 ± 1.1 km s-1 Mpc-1, with 1.7% precision. This measurement assumes standard prerecombination physics but is insensitive to assumptions about dark energy or space curvature, so agreement with CMB-based estimates that assume a flat Λ CDM cosmology is an important corroboration of this minimal cosmological model. For constant dark energy (Λ), our BAO + SN + CMB combination yields matter density Ωm = 0.301 ± 0.008 and curvature Ωk = -0.003 ± 0.003. When we allow more general forms of evolving dark energy, the BAO + SN + CMB parameter constraints are always consistent with flat Λ CDM values at ≈1σ. While the overall χ2 of model fits is satisfactory, the LyaF BAO measurements are in moderate (2–2.5σ) tension with model predictions. Models with early dark energy that tracks the dominant energy component at high redshift remain consistent with our expansion history constraints, and they yield a higher H0 and lower matter clustering amplitude, improving agreement with some low redshift observations. Expansion history alone yields an upper limit on the summed mass of neutrino species, ∑mν (95% confidence), improving to ∑mν if we include the lensing signal in the Planck CMB power spectrum. In a flat Λ CDM model that allows extra relativistic species, our data combination yields Neff = 3.43 ± 0.26; while the LyaF BAO data prefer higher Neff when excluding galaxy BAO, the galaxy BAO alone favor Neff ≈ 3. When structure growth is extrapolated forward from the CMB to low redshift, standard dark energy models constrained by our data predict a level of matter clustering that is high compared to most, but not all, observational estimates

The Baryon Oscillation Spectroscopic Survey of SDSS-III

The Baryon Oscillation Spectroscopic Survey (BOSS) is designed to measure the scale of baryon acoustic oscillations (BAO) in the clustering of matter over a larger volume than the combined efforts of all previous spectroscopic surveys of large-scale structure. BOSS uses 1.5 million luminous galaxies as faint as i = 19.9 over 10,000 deg(2) to measure BAO to redshifts z < 0.7. Observations of neutral hydrogen in the Ly alpha forest in more than 150,000 quasar spectra (g < 22) will constrain BAO over the redshift range 2.15 < z < 3.5. Early results from BOSS include the first detection of the large-scale three-dimensional clustering of the Ly alpha forest and a strong detection from the Data Release 9 data set of the BAO in the clustering of massive galaxies at an effective redshift z = 0.57. We project that BOSS will yield measurements of the angular diameter distance d(A) to an accuracy of 1.0% at redshifts z = 0.3 and z = 0.57 and measurements of H(z) to 1.8% and 1.7% at the same redshifts. Forecasts for Ly alpha forest constraints predict a measurement of an overall dilation factor that scales the highly degenerate D-A(z) and H-1(z) parameters to an accuracy of 1.9% at z similar to 2.5 when the survey is complete. Here, we provide an overview of the selection of spectroscopic targets, planning of observations, and analysis of data and data quality of BOSS