1,759,992 research outputs found
Additional file 1 of LINC01128 facilitates the progression of pancreatic cancer through up-regulation of LDHA by targeting miR-561-5p
No full textAdditional file 1: Fig. S1. miR-561-5p exerted an anti-oncogenic biological role in PC cell lines. a The relative growth rate of BxPC-3 and SW1990 transfected with miR-561-5p mimics or negative control. b The proliferation ability of PC cells with miR-561-5p overexpression. c-d The migration and invasion capability change of PC cells after miR-561-5p upregulation. Data are expressed as the mean ± SD of three independent experiments. *p < 0.05, **p < 0.01
Architecture of TOI-561 planetary system
No full textWe present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561's orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (Rp = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass(Mp = 12.4 ± 1.4 M?) estimates, implying a density of ρp = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f. © 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society
Architecture of TOI-561 planetary system
No full textWe present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7 days (TOI-561 d), and 77.1 days (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 days. The precise characterisation of TOI-561\u27s orbital architecture is interesting since old and metal-poor thick disk stars are less likely to host ultra-short period Super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be days, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius ( from 5 to 2 precision) and mass () estimates, implying a density of . Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet\u27s period is finally constrained, allowing us to predict transit times through 2030 with 20-minute accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.13 pages, 10 Figures. Accepted on MNRAS. Updated the author lis
Uher Spulentonbandgerät SG 561 ROYAL
No full textUHER SPULENTONBANDGERÄT SG 561 ROYAL
Uher Spulentonbandgerät SG 561 ROYAL ( -
Going Beyond Counting First Authors in Author Co-citation Analysis
No full textThe present study examines one of the fundamental aspects of author co-citation analysis (ACA) - the way co-citation
counts are defined. Co-citation counting provides the data on which all subsequent statistical analyses and mappings
are based, and we compare ACA results based on two different types of co-citation counting - the traditional type that
only counts the first one among a cited work's authors on the one hand and a non-traditional type that takes into
account the first 5 authors of a cited work on the other hand. Results indicate that the picture produced through this non-traditional author co-citation counting contains more coherent author groups and is therefore considerably clearer. However, this picture represents fewer specialties in the research field being studied than that produced through the traditional first-author co-citation counting when the same number of top-ranked authors is selected and analyzed. Reasons for these effects are discussed
TOI-561 b: A Low-density Ultra-short-period Rocky Planet around a Metal-poor Star
No full textTOI-561 is a galactic thick-disk star hosting an ultra-short-period (0.45-day-orbit) planet with a radius of 1.37 R¤, making it one of the most metal-poor ([Fe/H] = ?0.41) and oldest (?10 Gyr) sites where an Earth-sized planet has been found. We present new simultaneous radial velocity (RV) measurements from Gemini-N/MAROON-X and Keck/HIRES, which we combined with literature RVs to derive a mass of Mb = 2.24 ± 0.20 M¤. We also used two new sectors of TESS photometry to improve the radius determination, finding Rb = 1.37 ± 0.04 R¤ and confirming that TOI-561 b is one of the lowest-density super-Earths measured to date (?b = 4.8 ± 0.5 g cm?3). This density is consistent with an iron-poor rocky composition reflective of the host star’s iron and rock-building element abundances; however, it is also consistent with a low-density planet with a volatile envelope. The equilibrium temperature of the planet (?2300 K) suggests that this envelope would likely be composed of high mean molecular weight species, such as water vapor, carbon dioxide, or silicate vapor, and is likely not primordial. We also demonstrate that the composition determination is sensitive to the choice of stellar parameters and that further measurements are needed to determine whether TOI-561 b is a bare rocky planet, a rocky planet with an optically thin atmosphere, or a rare example of a nonprimordial envelope on a planet with a radius smaller than 1.5 R. © 2023. The Author(s). Published by the American Astronomical Society
Band 2, 561 (Sammlung Friedlaender)
No full textBAND 2, 561 (SAMMLUNG FRIEDLAENDER)
Band 2, 561 (Sammlung Friedlaender) (Public Domain) (1
The LCA<sub>840-561</sub> of each surface, total LCA<sub>840-561</sub>, corneal LCA<sub>840-561</sub>, and LCA<sub>840-561</sub> of IOL were calculated for each kind of IOL with the paraxial approximation.
No full textThe LCA840-561 of each surface, total LCA840-561, corneal LCA840-561, and LCA840-561 of IOL were calculated for each kind of IOL with the paraxial approximation.</p
Variations on the Author
No full text“Variations on the Author” discusses two of Eduardo Coutinho’s recent films (Um Dia na Vida, from 2010, and Últimas Conversas, posthumously released in 2015) and their contribution to the general question of documentary authorship. The director’s filmography is characterized by a consistent yet self-effacing form of authorial self-inscription: Coutinho often features as an interviewer that rather than express opinions propels discourses; an interviewer that is good at listening. This mode of self-inscription characterizes him as an author who is not expressive but who is nonetheless markedly present on the screen. In Um Dia na Vida, however, Coutinho is completely absent form the image, while Últimas Conversas, on the contrary, includes a confessional prologue that moves the director from the margins to the center of his films. This article examines the ways in which these works stand out in the filmography of a director who offers new insights into the notion of cinematic authorship
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