Lensed type Ia supernovae in light of SN Zwicky and iPTF16geu

Strong gravitationally lensed supernovae (glSNe) are a powerful probe to obtain a measure of the expansion rate of the Universe, but they are also extremely rare. To date, only two glSNe with multiple images strongly lensed by galaxies have been found, but their short time delays make them unsuitable for cosmography. We simulate a realistic catalogue of lensed supernovae and study the characteristics of the population of detectable systems for different surveys. Our simulations show that the properties of glSNe in shallow surveys (such as the Zwicky Transient Facility; ZTF) are determined by the need for large magnifications, which favours systems of four images with short time delays and low image separations. This picture is consistent with the properties of iPTF16geu and SN~Zwicky, but is not representative of the population found in deeper surveys, which are limited by the volume of the Universe that is strongly lensed. In our simulations of the Legacy Survey of Space and Time (LSST), glSNe show longer time delays and greater angular separations. Of these systems in LSST, 35\% will allow for time-delay measurements with a precision of 10\% or better. In the 10 years of the survey LSST should be able to find $\approx$ 180 systems, of which 60 will be suited for cosmography enabling a $\approx 1.5 \%$ precision $H_0$ measurement with LSST glSNe.Comment: 11 pages, 9 figures. Submitte

Haze in Pluto's atmosphere: Results from SOFIA and ground-based observations of the 2015 June 29 Pluto occultation

On UT 29 June 2015, the occultation by Pluto of a bright star (r′ = 11.9) was observed from the Stratospheric Observatory for Infrared Astronomy (SOFIA) and several ground-based stations in New Zealand and Australia. Pre-event astrometry allowed for an in-flight update to the SOFIA team with the result that SOFIA was deep within the central flash zone (~22 km from center). Analysis of the combined data leads to the result that Pluto's middle atmosphere is essentially unchanged from 2011 and 2013 (Person et al. 2013; Bosh et al. 2015); there has been no significant expansion or contraction of the atmosphere. Additionally, our multi-wavelength observations allow us to conclude that a haze component in the atmosphere is required to reproduce the light curves obtained. This haze scenario has implications for understanding the photochemistry of Pluto's atmosphere

Micro-images of macro-lensed objects

Thesis: S.B., Massachusetts Institute of Technology, Department of Physics, 2018.Cataloged from PDF version of thesis.Includes bibliographical references (pages 79-80).The study of gravitational micro-lensing at high optical depth has only rarely involved the close examination of the individual actual micro-images that arise as a result of the phenomenon. We discuss methods that refine on previous work done in the search for micro-images, which have been largely ignored in favor of other methods to study micro-lensing. With the help of magnification maps generated by Herr Prof. Dr. Joachim Wambsganss, we ran simulations that track positions and magnifications of micro-minima as functions of source position. We discuss the breakdown of a commonly used approximation for magnifications near fold caustics. Our results show that the approximation is noticeably broken at a caustic strength-scaled distance of 0.1. The relevance of this breakdown to work done by other authors is briefly examined. We then then discuss a few new results for the statistics of micro-images, deriving a formula for the mean micro-minimum magnification. We present a method for exactly calculating the caustic networks of micro-lensed systems, and calculate probability distributions for the caustic strength for two sets of parameters of interest. We present the creation of videos of the micro-lensing affect for pedagogical purposes. Finally, we briefly examine micro-lensing near macro-caustics and study the motion of micro-images as a point source crosses a macro-caustic.by Luke Weisenbach.S.B