Control de los costos de servicio y la rentabilidad de la empresa Sisa Tours S.A.C, San José de Sisa, 2018-2021

El estudio tuvo como objetivo general determinar de qué manera el control de los costos de servicio se relaciona con la rentabilidad de la empresa Sisa Tours SAC, San José de Sisa, motivo por el cual fue necesario considerar metodológicamente una investigación básica, de enfoque cuantitativo, diseño no experimental de nivel descriptivo correlacional causal, cuya muestra se constituyó por un total de 04 Balances de situación financiera y 04 Estados de resultados de la organización, por lo que fue necesario emplear una guía de análisis documental como instrumento de recolección. Los principales resultados demostraron que la rentabilidad de activos, financiera y operativa no se relaciona con el control de los costos de servicio dado que los niveles de significancia presentan valores mayores a 0,05. Al término del estudio se logró comprobar la hipótesis general del estudio y se concluyó que la relación del control de los costos de servicio con la rentabilidad neta de la empresa Sisa Tours SAC, San José de Sisa, es significativa, en vista que el nivel de significancia es igual a p-valor= 0,005 < 0,05; además, la correlación es positiva y fuerte (r=0,995*)

A New Method for Identifying Coronary Artery Disease via Analysis of Human Serum

Coronary artery disease (CAD), the number one cause of death in the United States, has traditionally been combated by reactionary diagnostics. However, the current healthcare dynamic is shifting towards a preventative approach, which aims to treat disease prior to the manifestation of symptoms. A minimally invasive diagnostic method which provides insight into an individual’s blood chemistry has the potential to facilitate this transition. This study analyzes the protein chemistry of human blood serum in order to differentiate between CAD and Non-CAD serum, with the goal of discovering potential CAD biomarkers. The Beckman/Coulter P/ACE MDQ Capillary Electrophoresis System was coupled with a commercial SDS-Gel based buffer system in order to achieve highly resolved serum protein spectrums. Electropherograms for nineteen participants were analyzed in 32 KaratTM Software by integrating protein peak areas, which were then normalized using an internal standard. Based on these integrations, a Linear Discriminant Analysis (LDA) algorithm was generated using OriginPro 8.6 Data Analysis and Graphing Software for the purpose of distinguishing between CAD and Non-CAD individuals. Cohorts of twelve CAD and seven Non-CAD participants were used for training purposes. This training data was classified with 100% accuracy, and an obtained p-value of 0.00332 indicated a significant difference between the CAD and Non-CAD participants’ peak distributions. This study establishes the utilization of capillary gel electrophoresis techniques for serum classification purposes, and ultimately points toward the development of a new, minimally invasive diagnostic tool for CAD based on blood protein chemistry rather than symptom onset

Orbital Foregrounds for Ultra-Short Duration Transients

Reflections from objects in Earth orbit can produce sub-second, star-like optical flashes similar to astrophysical transients. Reflections have historically caused false alarms for transient surveys, but the population has not been systematically studied. We report event rates for these orbital flashes using the Evryscope Fast Transient Engine, a low-latency transient detection pipeline for the Evryscopes. We select single-epoch detections likely caused by Earth satellites and model the event rate as a function of both magnitude and sky position. We measure a rate of $1800^{+600}_{-280}$ sky$^{-1}$ hour$^{-1}$, peaking at $m_g = 13.0$, for flashes morphologically degenerate with real astrophysical signals in surveys like the Evryscopes. Of these, $340^{+150}_{-85}$ sky$^{-1}$ hour$^{-1}$ are bright enough to be visible to the naked eye in typical suburban skies with a visual limiting magnitude of $V\approx4$. These measurements place the event rate of orbital flashes orders of magnitude higher than the combined rate of public alerts from all active all-sky fast-timescale transient searches, including neutrino, gravitational-wave, gamma-ray, and radio observatories. Short-timescale orbital flashes form a dominating foreground for un-triggered searches for fast transients in low-resolution, wide-angle surveys. However, events like fast radio bursts (FRBs) with arcminute-scale localization have a low probability ($\sim10^{-5}$) of coincidence with an orbital flash, allowing optical surveys to place constraints on their potential optical counterparts in single images. Upcoming satellite internet constellations, like SpaceX Starlink, are unlikely to contribute significantly to the population of orbital flashes in normal operations.Comment: 8 pages, 4 figure

EvryFlare. III. Temperature Evolution and Habitability Impacts of Dozens of Superflares Observed Simultaneously by Evryscope and TESS

Superflares may provide the dominant source of biologically relevant UV radiation to rocky habitable-zone M-dwarf planets (M-Earths), altering planetary atmospheres and conditions for surface life. The combined line and continuum flare emission has usually been approximated by a 9000 K blackbody. If superflares are hotter, then the UV emission may be 10 times higher than predicted from the optical. However, it is unknown for how long M-dwarf superflares reach temperatures above 9000 K. Only a handful of M-dwarf superflares have been recorded with multiwavelength high-cadence observations. We double the total number of events in the literature using simultaneous Evryscope and Transiting Exoplanet Survey Satellite observations to provide the first systematic exploration of the temperature evolution of M-dwarf superflares. We also increase the number of superflaring M dwarfs with published time-resolved blackbody evolution by ∼10×. We measure temperatures at 2 minutes cadence for 42 superflares from 27 K5–M5 dwarfs. We find superflare peak temperatures (defined as the mean of temperatures corresponding to flare FWHM) increase with flare energy and impulse. We find the amount of time flares emit at temperatures above 14,000 K depends on energy. We discover that 43% of the flares emit above 14,000 K, 23% emit above 20,000 K and 5% emit above 30,000 K. The largest and hottest flare briefly reached 42,000 K. Some do not reach 14,000 K. During superflares, we estimate M-Earths orbiting <200 Myr stars typically receive a top-of-atmosphere UV-C flux of ∼120 W m−2 and up to 103 W m−2, 100–1000 times the time-averaged X-ray and UV flux from Proxima Cen

Low-Cost Access to the Deep, High-Cadence Sky: the Argus Optical Array

New mass-produced, wide-field, small-aperture telescopes have the potential to revolutionize ground-based astronomy by greatly reducing the cost of collecting area. In this paper, we introduce a new class of large telescope based on these advances: an all-sky, arcsecond-resolution, 1000-telescope array which builds a simultaneously high-cadence and deep survey by observing the entire sky all night. As a concrete example, we describe the Argus Array, a 5m-class telescope with an all-sky field of view and the ability to reach extremely high cadences using low-noise CMOS detectors. Each 55 GPix Argus exposure covers 20% of the entire sky to g=19.6 each minute and g=21.9 each hour; a high-speed mode will allow sub-second survey cadences for short times. Deep coadds will reach g=23.6 every five nights over 47% of the sky; a larger-aperture array telescope, with an \'etendue close to the Rubin Observatory, could reach g=24.3 in five nights. These arrays can build two-color, million-epoch movies of the sky, enabling sensitive and rapid searches for high-speed transients, fast-radio-burst counterparts, gravitational-wave counterparts, exoplanet microlensing events, occultations by distant solar system bodies, and myriad other phenomena. An array of O(1,000) telescopes, however, would be one of the most complex astronomical instruments yet built. Standard arrays with hundreds of tracking mounts entail thousands of moving parts and exposed optics, and maintenance costs would rapidly outpace the mass-produced-hardware cost savings compared to a monolithic large telescope. We discuss how to greatly reduce operations costs by placing all optics in a thermally controlled, sealed dome with a single moving part. Coupled with careful software scope control and use of existing pipelines, we show that the Argus Array could become the deepest and fastest Northern sky survey, with total costs below $20M.Comment: 17 pages, 5 figures, 2 table