Light Propagation in inhomogeneous Universes

Using a multi-plane lensing method that we have developed, we follow the evolution of light beams as they propagate through inhomogeneous universes. We use a P3M code to simulate the formation and evolution of large-scale structure. The resolution of the simulations is increased to sub-Megaparsec scales by using a Monte Carlo method to locate galaxies inside the computational volume according to the underlying particle distribution. The galaxies are approximated by isothermal spheres, with each morphological type having its own distribution of masses and core radii. The morphological types are chosen in order to reproduce the observed morphology-density relation. This algorithm has an effective resolution of 9 orders of magnitudes in length, from the size of superclusters down to the core radii of the smallest galaxies. We consider cold dark matter models normalized to COBE, and perform a large parameter survey by varying the cosmological parameters Omega_0, lambda_0, H_0, and n (the tilt of the primordial power spectrum). The values of n are chosen by imposing particular values or sigma_8, the rms mass fluctuation at a scale of 8/h Mpc. We use the power spectrum given by Bunn & White. This is the largest parameter survey ever done is this field.Comment: 3 pages, gzip'ed tar file, including TeX source (not Latex). To be published in a periodical of the Yukawa Institute for Theoretical Physics (1998

Analysis of ``Gauge Modes'' in Linearized Relativity

By writing the complete set of $3 + 1$ (ADM) equations for linearized waves, we are able to demonstrate the properties of the initial data and of the evolution of a wave problem set by Alcubierre and Schutz. We show that the gauge modes and constraint error modes arise in a straightforward way in the analysis, and are of a form which will be controlled in any well specified convergent computational discretization of the differential equations.Comment: 11pages LaTe

Laju Pengembangan Alam Semesta Berdasarkan Data Supernova Tipe Ia

Analisa data yang diperoleh dari supernova tipe Ia (SN Ia) dapat memberikan informasi mengenai pengembangan alam semesta. Laju pengembangan alam semesta didefiniskan dengan konstanta Hubble (H0). Dalam tugas akhir ini digunakan 151 data SN Ia dengan z ≤ 0,05 yang diunduh dari Supernova Cosmology Project. Metode yang digunakan untuk mendapatkan nilai H0 yaitu dengan mendapatkan nilai gradien dari diagram Hubble memberikan hasil H0 = 66,67 ± 1,20 km s-1 Mpc-1 dan menggunakan persamaan Friedmann yang dilambangkan dengan H0’ dengan masukkan beberapa nilai konstanta perlambatan (q0). Residu (H0’-H0) terkecil memberikan H0’ = 66,73 km s-1 Mpc-1  (q0 = -0,55) dengan residu 0,059087403, H0’= 66,69 km s-1 Mpc-1 (q0 = 0,5) dengan residu 0,023110894, H0 = 67,94 km s-1 Mpc-1  (q0 = -1) dengan residu 0,069846939 dan H0 = 67,91 km s-1 Mpc-1 (q0 = 0,15) dengan residu 0,036582237. Hasil ini menunjukkan bahwa menggunakan data dengan z rendah akan memberikan nilai H0 yang berbeda dengan z tinggi. Berdasarkan keempat nilai residu di atas yang memiliki perbedaan sangat kecil namun memberikan bentuk geometri yang berbeda sehingga geometri alam semesta tidak dapat ditentukan dari hanya menggunakan data supernova tipe Ia dengan redshift rendah.Kata Kunci : Supernova tipe Ia, konstanta Hubble, gradien, persamaan Friedman

Measuring the impact of Indonesian antennas on global geodetic VLBI network

International audienceIn the near future, two radio telescopes will be installed in the Indonesian region. These telescopes are proposed to be integrated into the existing Very Long Baseline Interferometry (VLBI) network both for astronomical and geodetical purposes. Here we simulate the impact of the inclusion of the future Indonesian antennas to the estimates of Earth Orientation Parameters and the station position. The simulation was performed in two types of VLBI sessions. First, we analyse the contribution of Indonesian antennas to the existing intensive session INT3 (IN320-314), which focuses on the estimation of dUT1. We found that the addition of Indonesian antennas has reduced the estimated dUT1 repeatability value by about 25%. Next, we simulate the 24-hour session by considering two existing network configurations, which are R4 (R4934) and AOV (AOV049). Overall we found that the addition of Indonesian antennas to each network configuration decreases the repeatability value of the Earth Orientation Parameter by about 20%. Meanwhile, the repeatability value of station position is reduced up to 12%. This reduction is already achieved even when we include only one Indonesian antenna