Multi-filter transit observations of WASP-39b and WASP-43b with three San Pedro M\'artir telescopes

Three optical telescopes located at the San Pedro M\'artir National Observatory were used for the first time to obtain multi-filter defocused photometry of the transiting extrasolar planets WASP-39b and WASP-43b. We observed WASP-39b with the 2.12m telescope in the U filter for the first time, and additional observations were carried out in the R and I filters using the 0.84m telescope. WASP-43b was observed in VRI with the same instrument, and in the i filter with the robotic 1.50m telescope. We reduced the data using different pipelines and performed aperture photometry with the help of custom routines, in order to obtain the light curves. The fit of the light curves (1.5--2.5mmag rms), and of the period analysis, allowed a revision of the orbital and physical parameters, revealing for WASP-39b a period ($4.0552947 \pm 9.65 \times 10^{-7}$ days) which is $3.084 \pm 0.774$ seconds larger than previously reported. Moreover, we find for WASP-43b a planet/star radius ($0.1738 \pm 0.0033$) which is $0.01637 \pm 0.00371$ larger in the i filter with respect to previous works, and that should be confirmed with additional observations. Finally, we confirm no evidence of constant period variations in WASP-43b.Comment: 13 pages, 7 figures, accepted in PASP, scheduled for the February 1, 2015 issu

VizieR Online Data Catalog: WASP-39b and WASP-43b light curves (Ricci+, 2015)

The instrument comes with a set of standard UBVRI Johnson filters among others. We present observations carried out using the VRI filters. Light curves of WASP-39b were obtained with the 0.84m telescope in R and I bands and with the 2.12m telescope in the U band. Light curves of WASP-43b were obtained with the 0.84m telescope in VRI bands and with the 1.50m telescope in the Gunn-i band. (2 data files

Escucha México: estrategias gráficas y cultura auditiva

Durante el periodo de Primavera 2021, el PAP Escucha México tiene como objetivo desarrollar vinculaciones con instituciones, organizaciones e iniciativas ciudadanas que se dedican al tema de la cultura auditiva y el ruido en la Zona Metropolitana de Guadalajara. Mediante la sensibilización de la comunidad ante la problemática de la contaminación sonora, la discapacidad auditiva y de lenguaje, se busca generar entornos incluyentes. A lo largo del semestre se intervino Cruzada Contra el Ruido, Clinica Mariana Anaya Doll y Escucha México Redes Sociales, en las cuales se trabajó con la rehabilitación de sus redes sociales y productos comunicativos buscando generar un impacto en su audiencia.ITESO, A.C

VizieR Online Data Catalog: HAT-P-3b and TrES-3b light curves and Mid-times (Ricci+, 2017)

Tables contain the light curves and the calculated Mid-times. (15 data files)

Absolute Colours And Phase Coefficients Of Trans-Neptunian Objects: HV - HR And Relative Phase Coefficients

The trans-Neptunian objects (TNOs) are small Solar System bodies at large distances from the Sun. As such, their physical properties are difficult tomeasure. Accurate determination of their physical parameters is essential to model and theorize the actual composition and distribution of the population, and to improve our understanding of the formation and evolution of the Solar System. The objective of this work is to construct phase curves in two filters, V and R, of a large TNO sample obtaining absolute magnitudes (H) and phase coefficients (β), and study possible relations between them and other physical parameters (orbital elements, sizes, and albedos).We used our own data, together with data from the literature, to create the phase curves assuming an overall linear trend. We obtained new magnitudes for 28 TNOs, 28 in the V filter and 36 in the R filter. These magnitudes, together with data from the literature, allowed us to obtain absolutes magnitudes, 114 in the V filter and 113 in the R filter, of which 106 have both. From the search for correlations, we found a strong anticorrelation between HV - HR and Δβ = βV - βR, which is probably more related to surface structure than to composition or size of the objects

Absolute colours and phase coefficients of trans-Neptunian objects: correlations and populations

The study of the visible colours of the trans-Neptunian objects opened a discussion almost 20 yr ago which, in spite of the increase in the amount of available data, seems far from subside. Visible colours impose constraints to the current theories of the early dynamical evolution of the Solar system such as the environment of formation, initial surface composition, and how (if) they were scattered to regions closer to the inner planets. In this paper, we present an updated version of our data base of absolute colours and relative phase coefficients for 117 objects. We define the absolute colours as the difference of the absolute magnitudes H-V - H-R, and the relative phase coefficient as the difference of the slopes of the phase curves Delta beta. These were obtained joining our own observations plus data from the literature. The methodology has been introduced in previous works and here we expand in some interesting results, in particular the strong anticorrelation found between H-V - H-R and Delta beta, which means that redder objects have steeper phase curves in the R filter, while bluer objects have steeper phase curves in the V filter. We analyse a series of results published in the literature in view of our data base, which is free of phase effects, and show that their statistical meaning is not very strong. We point out that phase-colouring and observational errors play an important role in the understanding of these proposed relationships.© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical SocietyAAC acknowledges support from FAPERJ (grant E26/203.186/2016) and CNPq (grants 304971/2016-2 and 401669/2016-5). CAL thanks CNPq's support (studentship 141784/2015-6). RGH gratefully acknowledge support by CONICET through PIP 112-201501-00525, and San Juan National University by a CICITCA grant for the period 2018-2019. JLO thanks support from grant AYA2017-89637-R. JLO, PSS, and RD acknowledge financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). PSS acknowledges financial support by the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no. 687378, as part of the project 'Small Bodies Near and Far' (SBNAF).Peer reviewe

Possible detection of a bimodal cloud distribution in the atmosphere of HAT-P-32Ab from multiband photometry

We present high-precision photometry of eight separate transit events in the HAT-P-32 planetary system. One transit event was observed simultaneously by two telescopes of which one obtained a simultaneous multiband light curve in three optical bands, giving a total of 11 transit light curves. Due to the filter selection and in conjunction with using the defocused photometry technique, we were able to obtain an extremely high-precision, ground-based transit in the u band (350 nm), with an rms scatter of ≈1 mmag. All 11 transits were modelled using PRISM and GEMC, and the physical properties of the system calculated. We find the mass and radius of the host star to be 1.182 ± 0.041 M☉ and 1.225 ± 0.015 R☉, respectively. For the planet, we find a mass of 0.80 ± 0.14 MJup, a radius of 1.807 ± 0.022 RJup, and a density of 0.126 ± 0.023 ρJup. These values are consistent with those found in the literature. We also obtain a new orbital ephemeris for the system T0 = BJD/TDB 2 454 420.447187(96) + 2.15000800(10) × E. We measured the transmission spectrum of HAT-P-32 A b and compared it to theoretical transmission spectra. Our results indicate a bimodal cloud particle distribution consisting of Rayleigh-like haze and grey absorbing cloud particles within the atmosphere of HAT-P-32 A b

Absolute colours and phase coefficients of trans-Neptunian objects: HV − HR and relative phase coefficients

The trans-Neptunian objects (TNOs) are small Solar System bodies at large distances from the Sun. As such, their physical properties are difficult tomeasure. Accurate determination of their physical parameters is essential to model and theorize the actual composition and distribution of the population, and to improve our understanding of the formation and evolution of the Solar System. The objective of this work is to construct phase curves in two filters, V and R, of a large TNO sample obtaining absolute magnitudes (H) and phase coefficients (β), and study possible relations between them and other physical parameters (orbital elements, sizes, and albedos).We used our own data, together with data from the literature, to create the phase curves assuming an overall linear trend. We obtained new magnitudes for 28 TNOs, 28 in the V filter and 36 in the R filter. These magnitudes, together with data from the literature, allowed us to obtain absolutes magnitudes, 114 in the V filter and 113 in the R filter, of which 106 have both. From the search for correlations, we found a strong anticorrelation between H - H and Δβ = β - β, which is probably more related to surface structure than to composition or size of the objects. © 2018 The Author(s).Based in part on observations collected at the German-Spanish Astronomical Center, Calar Alto, operated jointly by Max-Planck-Institut fur Astronomie and Instituto de Astrofisica de Andalucia (CSIC). Partially based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (MC-TIC) da Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). CAL acknowledges support from CNPq (141784/2015-6). AAC acknowledges support from CNPq and FAPERJ. Part of the research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement No. 687378. PSS and JLO would like to acknowledge financial support by the Spanish grant AYA-2014-56637-C2-1-P and the Proyecto de Excelencia de la Junta de Andalucia J.A. 2012-FQM1776