SIMULASI PERENCANAAN INFRASTRUKTUR LAN ITTELKOM BERBASIS PLC

ABSTRAKSI: Penggelaran infrastruktur jaringan LAN cukup rumit, yaitu harus memasang kabel melalui langit-langit dan melubangi dinding. Oleh karena itu dibutuhkan suatu teknologi LAN lain yang mudah dalam pengimplementasiannya. PLC merupakan salah satu cara menyelesaikan masalah tersebut, karena jaringan ini sudah tergelar bersama infrastruktur sistem tenaga listrik, dan sudah menjangkau sampai tiap ruang atau bangunan sehingga tidak diperlukannya penggelaran kabel baru. Teknologi PLC ini sangat cocok diimplementasikan di gedung-gedung bertingkat karena dapat menjangkau lantai diatasnya, yaitu selama ada kabel listrik yang menghubungkan antara satu lantai dengan lantai lain.ITTELKOM merupakan institusi pendidikan yang memiliki gedung-gedung yang cukup banyak. Saat ini teknologi LAN yang sudah diterapkan di ITTELKOM yaitu berupa jaringan Wireless LAN dan LAN berbasis kabel UTP. Namun ada beberapa kekurangan pada kedua jenis teknologi tersebut, yaitu sinyal pada Wireless LAN tidak dapat menembus dinding bangunan di sebelah atau diatas atau dibawahnya yang berbahan beton, sedangkan LAN kabel UTP untuk jarak yang jauh membutuhkan kabel yang cukup panjang, pemasangannya cukup rumit sehingga menambah ongkos investasi yang cukup besar. Oleh karena itu pada tugas akhir ini dilakukan simulasi perancangan jaringan infrastruktur LAN ITTELKOM yang berbasis PLC, sebagai alternatif lain yang mudah tanpa menggelar kabel baru sebagai penopang jaringan LAN.Dari hasil simulasi dan perancangan dapat diketahui kualitas dari hasil perancangan, yaitu mengenai garansi Qos. Dari hasil simulasi didapatkan bahwa throughput yang didapat dari simulasi memenuhi kebutuhan User ITTELKOM (60 Mbps) yaitu sebesar 97 Mbps. Delay terbesar yang didapat dari simulasi sebesar 11,881 ms (Standard ITU-T 0-150 ms), packet loss 2,218% (standard packetloss requirement maksimal 5%). Dengan kata lain hasil perancangan layak untuk diimplementasikan di ITTELKOM.Kata Kunci : PLC, LAN, kabel listrikABSTRACT: Realization of LAN network infrastruktur is uneasy, because we need to install the wire through the ceiling and drill the wall. Because of that we needs another LAN technology that easy to installed. PLC is another way to solve this problem, because it just using existing electrical wire, and had cover each room or building so we do not need to build new wire. This technology is very suitable to be impelemented in building that have a lot of floor because it can reach to another floor as long as there is still wire conected each floor.ITTELKOM had a lot of building. Nowadays the technology that have been implemented were Wireless LAN and UTP LAN. But there are still lack with both technology, that are the signal of Wireless LAN cannot penetrate to the wall, and UTP LAN need more wire for a long distance so affect bigger investation cost. That’s why in this Final Task will be discuss about the designing of LAN PLC network for ITTELKOM, as another easier alternative without need new wire.The result of simulation and designing can be take as Qos parameter. From the simulation there is throughput which can give ITTELKOM user need(60Mbps) that is 97 Mbps. The biggest delay is 11,881 ms (Standard ITU-T 0-150 ms), packetloss 2,218% (standard packetloss requirement maksimal 5%). Thus the designing result is deserve to be implemneted in ITTELKOM.Keyword: PLC, LAN, electric wir

Galaxy Halo Masses from Galaxy-Galaxy Lensing

We present measurements of the extended dark halo profiles of bright early type galaxies at redshifts 0.1 to 0.9 obtained via galaxy-galaxy lensing analysis of images taken at the CFHT using the UH8K CCD mosaic camera. Six half degree fields were observed for a total of 2 hours each in I and V, resulting in catalogs containing ~20 000 galaxies per field. We used V-I color and I magnitude to select bright early type galaxies as the lens galaxies, yielding a sample of massive lenses with fairly well determined redshifts and absolute magnitudes M ~ M_* \pm 1. We paired these with faint galaxies lying at angular distances 20" to 60", corresponding to physical radii of 26 to 77 kpc (z = 0.1) and 105 to 315 kpc (z = 0.9), and computed the mean tangential shear of the faint galaxies. The shear falls off with radius roughly as expected for flat rotation curve halos. The shear values were weighted in proportion to the square root of the luminosity of the lens galaxy. Our results give a value for the average mean rotation velocity of an L_* galaxy halo at r~50-200 kpc of v_* = 238^{+27}_{-30} km per sec for a flat lambda (Omega_m0 = 0.3, Omega_l0 = 0.7) cosmology (v_* = 269^{+34}_{-39} km per sec for Einstein-de Sitter), and with little evidence for evolution with redshift. We compare to halo masses measured by other groups/techniques. We find a mass-to-light ratio of ~121\pm28h(r/100 kpc) and these halos constitute Omega ~0.04 \pm 0.01(r/100 kpc) of closure density. (abridged)Comment: Accepted for publication in ApJ (minor modifications) - 32 pages, 11 figs, 5 table

Galaxy-galaxy(-galaxy) lensing as a sensitive probe of galaxy evolution

The gravitational lensing effect provides various ways to study the mass environment of galaxies. We investigate how galaxy-galaxy(-galaxy) lensing can be used to test models of galaxy formation and evolution. We consider two semi-analytic galaxy formation models based on the Millennium Run N-body simulation: the Durham model by Bower et al. (2006) and the Garching model by Guo et al. (2011). We generate mock lensing observations for the two models, and then employ Fast Fourier Transform methods to compute second- and third-order aperture statistics in the simulated fields for various galaxy samples. We find that both models predict qualitatively similar aperture signals, but there are large quantitative differences. The Durham model predicts larger amplitudes in general. In both models, red galaxies exhibit stronger aperture signals than blue galaxies. Using these aperture measurements and assuming a linear deterministic bias model, we measure relative bias ratios of red and blue galaxy samples. We find that a linear deterministic bias is insufficient to describe the relative clustering of model galaxies below ten arcmin angular scales. Dividing galaxies into luminosity bins, the aperture signals decrease with decreasing luminosity for brighter galaxies, but increase again for fainter galaxies. This increase is likely an artifact due to too many faint satellite galaxies in massive group and cluster halos predicted by the models. Our study shows that galaxy-galaxy(-galaxy) lensing is a sensitive probe of galaxy evolution.Comment: 11 pages, 8 figures, accepted in A&

MEASURING GALAXY MASSES USING GALAXY-GALAXY GRAVITATIONAL LENSING

We report a significant detection of weak, tangential distortion of the images of cosmologically distant, faint galaxies due to gravitational lensing by foreground galaxies. A mean image polarisation of $=0.011\pm 0.006$ is measured for 3202 pairs of source galaxies with magnitudes $23< r \le 24$ and lens galaxies with magnitudes $20\le r\le 23$. The signal remains strong for lens-source separations \lo 90'', consistent with quasi-isothermal galaxy halos extending to large radii (\go 100h^{-1} kpc). Our observations thus provide the first evidence from weak gravitational lensing of large scale dark halos associated with individual galaxies. The observed polarisation is also consistent with the signal expected on the basis of simulations incorporating measured properties of local galaxies and modest extrapolations of the observed redshift distribution of faint galaxies. From the simulations we derive a best-fit halo circular velocity of $V\sim 220$ km/s and characteristic radial extent of s \go 100h^{-1} kpc. Our best-fit halo parameters imply typical masses for the lens galaxies within a radius of $100h^{-1}$ kpc on the order of $1.0^{+1.1}_{-0.7}\times 10^{12}h^{-1} M_\odot$, in good agreement with recent dynamical estimates of the masses of local spiral galaxies. This is particularly encouraging as the lensing and dynamical mass estimators rely on different sets of assumptions. Contamination of the gravitational lensing signal by a population of tidally distorted satellite galaxies can be ruled out with reasonable confidence. The prospects for corroborating and improving this measurement seem good, especially using deep HST archival data.Comment: uuencoded, compressed PostScript; 26 pages (6 figures included

Moderate Galaxy-Galaxy Lensing

We study moderate gravitational lensing where a background galaxy is magnified substantially, but not multiply imaged, by an intervening galaxy. We focus on the case where both the lens and source are elliptical galaxies. The signatures of moderate lensing include isophotal distortions and systematic shifts in the fundamental plane and Kormendy relation, which can potentially be used to statistically determine the galaxy mass profiles. These effects are illustrated using Monte Carlo simulations of galaxy pairs where the foreground galaxy is modelled as a singular isothermal sphere model and observational parameters appropriate for the Large Synoptic Survey Telescope (LSST). The range in radius probed by moderate lensing will be larger than that by strong lensing, and is in the interesting regime where the density slope may be changing.Comment: 8 pages, 12 figures, MNRAS, comments welcom

Galaxy subgroups in galaxy clusters

Galaxies which fall into clusters as part of the same infall halo can retain correlations due to their shared origin. N-body simulations are used to study properties of such galaxy subgroups within clusters, including their richnesses and prevalence. The sizes, densities and velocity dispersions of all subgroups with >= 8 galaxies are found and compared to those of the host clusters. The largest galaxy subgroup provides a preferred direction in the cluster and is compared to other preferred directions in the cluster. Scatter in cluster mass measurements (via five observables), along ~ 96 lines of sight, is compared to the relation of the line of sight to this preferred direction: scatter in cluster velocity dispersion measurements show the strongest correlation. The Dressler-Shectman test (Dressler & Shectman 1988), is applied to these clusters, to see whether the substructure it identifies is related to these subgroups. The results for any specific line of sight seem noisy; however, clusters with large subgroups tend to have a higher fraction of lines of sight where the test detects substructure.Comment: 12 pages, final version for publication with helpful comments from referee and others include

PROFIL DESA PANCAKARYA BERKELANJUTAN UNIVERSITAS BUANA PERJUANGAN KARAWANG

Kuliah Kerja Nyata (KKN) merupakan kegiatan pengabdian kepadamasyarakat di daerah tertentu sebagai implementasi dari Tri Dharma PerguruanTinggi. Kegiatan KKN bertujuan untuk memberikan pengalaman lapangan kepadamahasiswa tentang kondisi masyarakat secara langsung dan juga untukmembentuksikap mandiri dan tanggung jawab dalam melaksanakan kegiatan KKN.PelaksanaanKKNdimulai dari tanggal 01Agustus 2020 sampai dengan 31Agustus2020 di Desa Pancakarya Kecamatan Tempuran, Kabupaten Karawang.Metode yang dilakukan pada KKN ini adalah observasi, dan program yangdilakukan pun tidak banyak karena pelaksanaan KKN tahun ini berbeda dengantahun-tahun sebelumnya, mengingat di tahun 2020 ini sedang mewabahnyapenyakit/virus COVID-19 yang menyebabkan status di Indonesia menjadiPandemi. Oleh karena itu kita diharuskan untuk menjaga jarak dengan tidak terlaluberdekatan dan tidak terlalu sering bertatap muka.Secara umum KKN yang dilaksanakan di Desa Pancakarya KecamatanTempuran Kabupaten Karawang ini berjalan dengan baik karena respon dari pihakDesa juga baik.Kata kunci:Kuliah Kerja Nyata, Desa Pancakarya, Profil Des Berkelanjutan Real Work Lecture (KKN) is a community service activity in certain areasas an implementation of the Tri Dharma of Higher Education. The KKN activityaims to provide field experiences to students about the condition of the communitydirectly and also to form an independent and responsible attitude in carrying outKKN activities. The implementation of the Community Service Program starts fromAugust 1, 2020 to August 31, 2020 in Pancakarya Village, Tempuran District,Karawang Regency. The method used in this KKN is observation, and the programscarried out are not many because this year's KKN implementation is different fromthe previous years, considering that in 2020 there is an outbreak of the COVID-19disease / virus which has caused the status of Indonesia to become a pandemic.Therefore we are required to keep our distance not too close together and notmeeting face to face too often. In general, the KKN which was carried out inPancakarya Village, Tempuran District, Karawang Regency went well because theresponse from the Village was also good.Keywords: Real Work Lecture, Pancakarya Village, Sustainable Desa Profil