201 research outputs found
Assembly of the Inner Perivitelline Layer, a Homo log of the Mammalian Zona Pellucida: An Immunohistochemical and Ultrastructural Study
No full textThe avian inner perivitelline layer (IPVL), a homologous structure to the mammalian zona pellucida, is deposited between the granulosa cells and the oocyte cell membrane during folliculogenesis. The glycoprotein meshwork of the IPVL forms a 3-dimensional matrix and possesses important functions in the fertilization process: it contributes to the binding of avian spermatozoa to the oocyte and induces acrosomal exocytosis. In contrast to the zona pellucida of mammals, the IPVL does not prevent the physiological polyspermy found in birds. Previous studies have shown that in the Japanese quail (Cotumix japonica) at least 5 glycoproteins are constituents of the IPVL (ZP1, ZP2, ZP3, ZP4, and ZPD). In this study, we investigated the spatiotennporal assembly pattern of the IPVL during folliculogenesis using immunohistochemical and ultrastructural methods. The obtained results clearly show that these glycoproteins are incorporated into the IPVL at distinct points during follicular development, supporting the hypothesis that ZP2 and ZP4 form a type of prematrix into which ZP1, ZP3, and ZPD are integrated at a later stage of development. Copyright (C) 2011 S. Karger AG, Base
Oioceros atropatenes Rodler & Weithofer 1890
No full textOioceros atropatenes Rodler & Weithofer, 1890 (Fig. 7E, F) LOCALITY. — Quarry 1, Ivand district, north of Tabriz, Iran. MATERIAL EXAMINED. — Left horn-core (HMNH-IV 200; Fig. 7E, F), right mandible with p4-m3 (HMNH-IV 67; Table 3), right mandible with broken m2 and complete m3 (HMNH-IV 69; Table 3). DESCRIPTION The horn-core specimen is partly broken at the base and the tip. The antero-posterior diameter cannot be measured precisely due to the basal missing part on both the anterior and posterior sides. However, we estimate that it exceeds 17 mm. The medio- A M1 M2 M3 M4 M6 M7 M14 M15 M23 M25 M30 M31 M32 M33 lateral diameter is 17.4 mm. The DAP and DT at 5 cm above the base are 12.7 mm and 10.9 mm, respectively. The total preserved length is 75 mm from the pedicle. By the preserved part of the orbit and remnant of the frontal, the horn-core is located above the posterior part of the orbit, tilted slightly backwards with a weak curvature. The horn-core is slender with a roughly oval cross section. The antero-posterior and transverse diameters diminish slowly from the base upwards. There are two weak keels, one starting from the antero-lateral side, and the other from the postero-lateral side. These two keels enclose a slightly convex outer surface and a more rounded inner surface. The keels spiral clock- wise roughly one gyre from the base to the tip by estimation. There is also a postcornual fossa. p4 is long and narrow. The paraconid is not separated from the parastylid. The anterior valley is wide. The metaconid is situated posterior to the protoconid. The entoconid is close to the entostylid. A wide and shallow valley separates the protoconid from the hypoconid.m1 is well worn. The parastylid is developed, and well separated from the metaconid. There is no goat fold, thus rendering the anterior border much narrower. The lingual wall is flat with weak metastylids. The entostylid is larger. There is a large basal pillar between the protoconid and the metaconid. m2 is very similar in morphology to m1, except for its larger, more convex lingual wall, and lower basal pillar. The parastylid on m3 is more pronounced and well separated from the metaconid. The basal pillar is small and low. The hypoconulid is large and postero-labially offset. COMPARISON Based on the small size, insertion above the posterior part of orbit, the clockwise torsion on the left horn-core from the base, and two keels, the horn-core IV200 from Ivand locality can readily be assigned to the genus Oioceros (type species Antelope rothii Wagner, 1857 from Pikermi, Greece) (Gaillard 1902). Since then, numerous species were included or assigned to this genus. De Mecquenem (1924) recognized three species from Maragheh: O. rothii (Wagner, 1857), O. atropatenes and O. boulei Mecquenem, 1924. Heintz (1963) synonymized O. boulei with O. atropatenes based on his detailed description and comparison. Roussiakis (2003) recently described in detail an almost complete skull with mandibles of Oioceros rothii from Pikermi and reviewed the generic status. Besides the type species, he listed only Oioceros atropatenes in the genus. The present specimen is smaller and less laterally compressed than Oioceros rothii from Pikermi. The main keel is much weaker and the upper part of the horn-core diverges less. The size falls into the variation of Oioceros atropatenes from Maragheh, Iran (Heintz 1963). The morphology of the horn-core is also consistent with those from Maragheh. Hence, the horn-core specimen can be assigned to Oioceros atropatenes.Published as part of Ataabadi, Majid Mirzaie, Mohammadalizadeh, Jafar, Zhang, Zhaoqun, Watabe, Mahito, Kaakinen, Anu & Fortelius, Mikael, 2011, Late Miocene large mammals from Ivand (Northwestern Iran), pp. 709-728 in Geodiversitas 33 (4) on pages 718-720, DOI: 10.5252/g2011n4a7, http://zenodo.org/record/459712
Author Correction: Metaverse in surgery — origins and future potential (Nature Reviews Urology, (2024), 10.1038/s41585-024-00941-4)
No full textCorrection to: Nature Reviews Urologyhttps://doi.org/10.1038/s41585-024-00941-4, published online 30 September 2024. In the version of the article initially published, Enrico Checcucci was wrongly stated to be affiliated with the University of Verona. This has now been amended in the HTML and PDF versions of the article so that Enrico Checcucci’s only affiliation is Department of Surgery, Candiolo Cancer Institute, FPO-IRCCS, Candiolo, Turin, Italy
Three planets around HD 27894: A close-in pair with a 2:1 period ratio and an eccentric Jovian planet at 5.4 AU
No full textAims. Our new program with HARPS aims to detect mean motion resonant planetary systems around stars which were previously reported to have a single bona fide planet, often based only on sparse radial velocity data.
Methods. Archival and new HARPS radial velocities for the K2V star HD 27894 were combined and fitted with a three-planet self-consistent dynamical model. The best-fit orbit was tested for long-term stability.
Results. We find clear evidence that HD 27894 is hosting at least three massive planets. In addition to the already known Jovian planet with a period Pb≈ 18 days we discover a Saturn-mass planet with Pc≈ 36 days, likely in a 2:1 mean motion resonance with the first planet, and a cold massive planet (≈5.3 MJup) with a period Pd ≈ 5170 days on a moderately eccentric orbit (ed = 0.39).
Conclusions. HD 27894 is hosting a massive, eccentric giant planet orbiting around a tightly packed inner pair of massive planets likely involved in an asymmetric 2:1 mean motion resonance. HD 27894 may be an important milestone for probing planetary formation and evolution scenarios.published_or_final_versio
Rodler, Barbara A. (Death, 1906-01-01)
No full textAddress: Hildreth Avenue- WestwoodAge at death: 206/Pg 2/1906/F W S/Cincinnati/Dr. Walter Musekamp/Fred C. Walter/BridgetownOriginal record filed in drawer labeled 'ROBINSON,J-ROHAN'
Observing the Universe at infrared wavelengths and high spectral resolution
No full textThe CRyogenic InfraRed Echelle Spectrograph (CRIRES) Upgrade project CRIRES + extended the capabilities of CRIRES. It transformed this VLT instrument into a cross-dispersed spectrograph to increase the wavelength range that is covered simultaneously by up to a factor of ten. In addition, a new detector focal plane array of three Hawaii 2RG detectors with a 5.3 μm cutoff wavelength replaced the existing detectors. Amongst many other improvements, a new spectropolarimetric unit was added and the calibration system has been enhanced. The instrument was installed at the VLT on Unit Telescope 3 at the beginning of 2020 and successfully commissioned and verified for science operations during 2021, partly remotely from Europe due to the COVID-19 pandemic. The instrument was subsequently offered to the community from October 2021 onwards. This article describes the performance and capabilities of the upgraded instrument and presents on sky results
Comment on “Artificial intelligence to predict oncological outcome directly from hematoxylin and eosin-stained slides in urology: a systematic review”
No full textThe Long but Necessary Journey Towards Optimization of the Cause-Effect Relationship Between Input and Output for Accountable Use of ChatGPT for Academic Purposes
No full textN/
FIG. 7 in Late Miocene large mammals from Ivand (Northwestern Iran)
No full textFIG. 7. — Gazella sp. (A-D, G, H) and Oioceros atropatenes Rodler & Weithofer,1890 (E, F) from Ivand locality (NW Iran):A, B, HMNH-IV140 in frontal (A) and lateral (B) views; C, D, HMNH-IV138 in frontal (C) and lateral (D) views; E, F, HMNH-IV200 in lateral-posterior (E) and frontal (F) views; G, H, HMNH-IV139 in lateral (G) and frontal (H) views. Scale bars: A, B, G, H, 20 mm; C, D, 15 mm; E, F, 25 mm.Published as part of Ataabadi, Majid Mirzaie, Mohammadalizadeh, Jafar, Zhang, Zhaoqun, Watabe, Mahito, Kaakinen, Anu & Fortelius, Mikael, 2011, Late Miocene large mammals from Ivand (Northwestern Iran), pp. 709-728 in Geodiversitas 33 (4) on page 725, DOI: 10.5252/g2011n4a7, http://zenodo.org/record/459712
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