Research identifies segments of the voting population by use of the media in the region of Puno. It was conducted under the application of probabilistic sampling, a questionnaire was administered by personal interview to a sample of 323 potential voters, the data was collected based on personal characteristics and use of media; five indicators of this relationship they are chosen, those who participated in the multiple correspondence analysis. The most representative personal characteristics were: 42,1% of potential voters are 20 to 34 years, 30.3% are engaged in the study as the main activity, 37,2% are center-right political trend. On the use of media 76,5% if you use the internet, with television (87,3%) frequently use the medium for information on daily events. We identified four segments, the first segment covers 51,8% of potential voters, they being under 34 years, intraday use the internet, is not politically defined and communicated via television or internet. The second segment includes 12,69% of potential voters, who work for the private sector, use the Internet once or twice a week for information and are defined politically center-right. The third segment covers 6,5% of potential voters, aged between 50 and 69, use the internet less than once a week and are defined center-left. The fourth segment includes 29,72% of potential voters, aged between 34-69 years old, do not
Context. The nearby ultra-compact multiplanetary system YZ Ceti consists of at least three planets, and a fourth tentative signal. The orbital period of each planet is the subject of discussion in the literature due to strong aliasing in the radial velocity data. The stellar activity of this M dwarf also hampers significantly the derivation of the planetary parameters. Aims. With an additional 229 radial velocity measurements obtained since the discovery publication, we reanalyze the YZ Ceti system and resolve the alias issues. Methods. We use model comparison in the framework of Bayesian statistics and periodogram simulations based on a method by Dawson and Fabrycky to resolve the aliases. We discuss additional signals in the RV data, and derive the planetary parameters by simultaneously modeling the stellar activity with a Gaussian process regression model. To constrain the planetary parameters further we apply a stability analysis on our ensemble of Keplerian fits. Results. We find no evidence for a fourth possible companion. We resolve the aliases: the three planets orbit the star with periods of 2.02 d, 3.06 d, and 4.66 d. We also investigate an effect of the stellar rotational signal on the derivation of the planetary parameters, in particular the eccentricity of the innermost planet. Using photometry we determine the stellar rotational period to be close to 68 d and we also detect this signal in the residuals of a three-planet fit to the RV data and the spectral activity indicators. From our stability analysis we derive a lower limit on the inclination of the system with the assumption of coplanar orbits which is i(min) = 0.9 deg. From the absence of a transit event with TESS, we derive an upper limit of the inclination of i(max) = 87.43 deg. Conclusions. YZ Ceti is a prime example of a system where strong aliasing hindered the determination of the orbital periods of exoplanets. Additionally, stellar activity influences the derivation of planetary parameters and modeling them correctly is important for the reliable estimation of the orbital parameters in this specific compact system. Stability considerations then allow additional constraints to be placed on the planetary parameters. ; German Research Foundation (DFG) FOR2544 RE 2694/4-1 German Max-Planck-Gesellschaft (MPG) Consejo Superior de Investigaciones Cientificas (CSIC) European Union through FEDER/ERF FICTS -2011 -02 Spanish Ministry of Economy German Science Foundation through the Major Research Instrumentation Programme Klaus Tschira Stiftung state of Baden-Wurttemberg state of Niedersachsen Junta de Andalucia High Performance and Cloud Computing Group at the Zentrum fur Datenverarbeitung of the University of Tubingen state of Baden-Wurttemberg through bwHPC German Research Foundation (DFG) INST 37/935 -1 FUGG European FEDER/ERF funds AYA2015-69350-C3-2-P AYA2016-79425-C3-1/2/3-P ESP2017-87676-C5-2-R ESP2017-87143-R Centre of Excellence "Severo Ochoa" award SEV-2015-0548 Centre of Excellence "Maria de Maeztu" award SEV-2015-0548 Instituto de Astrofisica de Andalucia SEV-2017-0709 Centro de Astrobiologia MDM-2017-0737 Generalitat de Catalunya/CERCA programme Science & Technology Facilities Council (STFC) ST/M001008/1 ST/P000584/1 Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) CONICYT FONDECYT 1161218 Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) PB06 Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) CONICYT FONDECYT 3180405 Hong Kong RGC grant HKU 17305618 European Research Council under the Horizon 2020 Framework Program via the ERC 83 24 28 Max-Planck-Institut fur Astronomie Instituto de Astrofisica de Andalucia Landessternwarte Konigstuhl Institut de Ciencies de l'Espai Insitut fur Astrophysik Gottingen Universidad Complutense de Madrid Thuringer Landessternwarte Tautenburg Instituto de Astrofisica de Canarias Hamburger Sternwarte Centro de Astrobiologia Centro Astronomico Hispano -Aleman Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades AYA2015-69350-C3-2-P AYA2016-79425-C3-1/2/3-P ESP2017-87676-C5-2-R ESP2017-87143-R
We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, mb = 30.8 ± 1.5Mpdbl, Rb = 4.7 ± 0.3 Rpdbl) located in the "hot Neptune desert". Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST-South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TÜBITAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (Teff = 3950 ± 51 K) with a mass of 0.59 ± 0.02Mpdbl and a radius of 0.58 ± 0.02Rpdbl. From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained. ; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
