Penyidikan terhadap Pelaku USAha dalam Perkara Tindak Pidana di Bidang Perlindungan Konsumen

Tujuan dilakukannya penelitian ini adalah untuk mengetahui bagaimanakah bentuk-bentuk perbuatan yang merupakan tindak pidana pelaku USAha terhadap konsumen yang dapat dilakukan penyidikan dan bagaimana penyidikan terhadap pelaku USAha dalam perkara tindak pidana di bidang perlindungan konsumen. Metode penelitian yang digunakan dalam penyusunan Skripsi ini, yaitu metode penelitian hokum normative dan dapat disimpulkan, bahwa: 1. Jenis-jenis tindak pidana yang merugikan konsumen terjadi apabila pelaku USAha memproduksi dan/atau memperdagangkan barang dan/atau jasa yang tidak sesuai dengan persyaratan dalam undang-undang perlindungan konsumen dan tidak segera menarik barang dan/atau jasa dari peredaran. Pelaku USAha menawarkan, mempromosikan, mengiklankan suatu barang dan/atau jasa secara tidak benar atau membuat pernyataan yang tidak benar atau menyesatkan dan mengelabui konsumen dan membuat atau mencantumkan klausula baku pada setiap dokumen dan/atau perjanjian yang tidak sesuai dengan undang-undang perlindungan konsumen. 2. Penyidikan terhadap perkara tindak pidana konsumen dilakukan oleh Pejabat Polisi Negara Republik Indonesia, Pejabat Pegawai Negeri Sipil tertentu di lingkungan instansi pemerintah yang lingkup tugas dan tanggung jawabnya di bidang perlindungan konsumen juga diberi wewenang khusus sebagai penyidik sebagaimana dimaksud dalam Undang-undang Hukum Acara Pidana yang berlaku. Penyidik Pejabat Pegawai Negeri Sipil berwenang melakukan pemeriksaan atas kebenaran laporan, keterangan dan bahan bukti, terhadap orang atau badan hukum, tempat dan penyitaan terhadap barang hasil pelanggaran termasuk meminta bantuan ahli dalam rangka pelaksanaan tugas penyidikan tindak pidana di bidang perlindungan konsumen

Detection of Contact Binaries Using Sparse High Phase Angle Lightcurves

We show that candidate contact binary asteroids can be efficiently identified from sparsely sampled photometry taken at phase angles >60deg. At high phase angle, close/contact binary systems produce distinctive lightcurves that spend most of the time at maximum or minimum (typically >1mag apart) brightness with relatively fast transitions between the two. This means that a few (~5) sparse observations will suffice to measure the large range of variation and identify candidate contact binary systems. This finding can be used in the context of all-sky surveys to constrain the fraction of contact binary near-Earth objects. High phase angle lightcurve data can also reveal the absolute sense of the spin.Comment: 4 pages, 4 figures, 1 table. Accepted for publication in ApJ

The matricellular functions of small leucine-rich proteoglycans (SLRPs)

The small leucine-rich proteoglycans (SLRPs) are biologically active components of the extracellular matrix (ECM), consisting of a protein core with leucine rich-repeat (LRR) motifs covalently linked to glycosaminoglycan (GAG) side chains. The diversity in composition resulting from the various combinations of protein cores substituted with one or more GAG chains along with their pericellular localization enables SLRPs to interact with a host of different cell surface receptors, cytokines, growth factors, and other ECM components, leading to modulation of cellular functions. SLRPs are capable of binding to: (i) different types of collagens, thereby regulating fibril assembly, organization, and degradation; (ii) Toll-like receptors (TLRs), complement C1q, and tumor necrosis factor-alpha (TNFα), regulating innate immunity and inflammation; (iii) epidermal growth factor receptor (EGF-R), insulin-like growth factor receptor (IGF-IR), and c-Met, influencing cellular proliferation, survival, adhesion, migration, tumor growth and metastasis as well as synthesis of other ECM components; (iv) low-density lipoprotein receptor-related protein (LRP-1) and TGF-β, modulating cytokine activity and fibrogenesis; and (v) growth factors such as bone morphogenic protein (BMP-4) and Wnt-I-induced secreted protein-1 (WISP-1), controlling cell proliferation and differentiation. Thus, the ability of SLRPs, as ECM components, to directly or indirectly regulate cell-matrix crosstalk, resulting in the modulation of various biological processes, aptly qualifies these compounds as matricellular proteins

Evaluasi Kinerja Bangunan Berlubang Dengan Metode Direct Displacement-based Design

Banyak penelitian mengenai kinerja Direct Displacement Based Design (DDBD) dan Force Based Design (FBD) telah dilakukan sebelumnya. Penelitian-penelitian sebelumnya menunjukkan bahwa DDBD menghasilkan performa struktur yang lebih mendekati target desain. Namun, penelitian terhadap bangunan berlubang belum pernah dilakukan sebelumnya. Konfigurasi struktur dengan void memiliki kekakuan portal yang bervariasi diaman hal ini mempengaruhi distribusi gaya pada setiap portal. Distribusi gaya pada bagian yang memiliki void akan mengalami perpindahan yang lebih besar daripada bagian yang tidak memiliki void khususnya jika pelat lantai diasumsikan semi rigid. Penelitian ini membandingkan kinerja FBD dan DDBD pada bangunan yang didesain berlubang atau memiliki void dengan asumsi desain bangunan tanpa lubang dan gaya geser dasar didistribusikan secara merata. Penelitian akan dievaluasi terhadap wilayah beresiko gempa tinggi dan rendah di Indonesia. Struktur yang didesain diuji dengan analisis non-linear dinamis time history. Hasil dari penelitian ini menunjukkan bahwa struktur bangunan yang didesain dengan DDBD memberikan kinerja yang lebih baik daripada FBD baik dalam drift ratio ataupun failure mechanism. Selain itu, prosedur DDBD lebih efektif dan efisien karena hasil desain mendekati target desain dan durasi desain sangat singkat. Satu-satunya kelemahan dari DDBD adalah biaya yang lebih mahal karena hasil desain yang menggunakan lebih banyak materia

The Resolved Asteroid Program - Size, shape, and pole of (52) Europa

With the adaptive optics (AO) system on the 10 m Keck-II telescope, we acquired a high quality set of 84 images at 14 epochs of asteroid (52) Europa on 2005 January 20. The epochs covered its rotation period and, by following its changing shape and orientation on the plane of sky, we obtained its triaxial ellipsoid dimensions and spin pole location. An independent determination from images at three epochs obtained in 2007 is in good agreement with these results. By combining these two data sets, along with a single epoch data set obtained in 2003, we have derived a global fit for (52) Europa of diameters (379x330x249) +/- (16x8x10) km, yielding a volume-equivalent spherical-diameter of 315 +/- 7 km, and a rotational pole within 7 deg of [RA; Dec] = [257,+12] in an Equatorial J2000 reference frame (ECJ2000: 255,+35). Using the average of all mass determinations available forEuropa, we derive a density of 1.5 +/- 0.4, typical of C-type asteroids. Comparing our images with the shape model of Michalowski et al. (A&A 416, 2004), derived from optical lightcurves, illustrates excellent agreement, although several edge features visible in the images are not rendered by the model. We therefore derived a complete 3-D description of Europa's shape using the KOALA algorithm by combining our imaging epochs with 4 stellar occultations and 49 lightcurves. We use this 3-D shape model to assess these departures from ellipsoidal shape. Flat facets (possible giant craters) appear to be less distinct on (52) Europa than on other C-types that have been imaged in detail. We show that fewer giant craters, or smaller craters, is consistent with its expected impact history. Overall, asteroid (52) Europa is still well modeled as a smooth triaxial ellipsoid with dimensions constrained by observations obtained over several apparitions.Comment: Accepted for publication in Icaru

A low density of 0.8 g/cc for the Trojan binary asteroid 617 Patroclus

The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 Lagrange points of the Jupiter-Sun system (leading and following Jupiter by 60 degrees). The asteroid 617 Patroclus is the only known binary Trojan (Merline et al. 2001). The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680 km, move around the system centre of mass, describing roughly a circular orbit. Using the orbital parameters, combined with thermal measurements to estimate the size of the components, we derive a very low density of 0.8 g/cc. The components of Patroclus are therefore very porous or composed mostly of water ice, suggesting that they could have been formed in the outer part of the solar system.Comment: 10 pages, 3 figures, 1 tabl

A Giant Crater on 90 Antiope?

Mutual event observations between the two components of 90 Antiope were carried out in 2007-2008. The pole position was refined to lambda0 = 199.5+/-0.5 eg and beta0 = 39.8+/-5 deg in J2000 ecliptic coordinates, leaving intact the physical solution for the components, assimilated to two perfect Roche ellipsoids, and derived after the 2005 mutual event season (Descamps et al., 2007). Furthermore, a large-scale geological depression, located on one of the components, was introduced to better match the observed lightcurves. This vast geological feature of about 68 km in diameter, which could be postulated as a bowl-shaped impact crater, is indeed responsible of the photometric asymmetries seen on the "shoulders" of the lightcurves. The bulk density was then recomputed to 1.28+/-0.04 gcm-3 to take into account this large-scale non-convexity. This giant crater could be the aftermath of a tremendous collision of a 100-km sized proto-Antiope with another Themis family member. This statement is supported by the fact that Antiope is sufficiently porous (~50%) to survive such an impact without being wholly destroyed. This violent shock would have then imparted enough angular momentum for fissioning of proto-Antiope into two equisized bodies. We calculated that the impactor must have a diameter greater than ~17 km, for an impact velocity ranging between 1 and 4 km/s. With such a projectile, this event has a substantial 50% probability to have occurred over the age of the Themis family.Comment: 30 pages, 3 Tables, 8 Figures. Accepted for publication in Icaru

Ultraviolet and visible photometry of asteroid (21) Lutetia using the Hubble Space Telescope

The asteroid (21) Lutetia is the target of a planned close encounter by the Rosetta spacecraft in July 2010. To prepare for that flyby, Lutetia has been extensively observed by a variety of astronomical facilities. We used the Hubble Space Telescope (HST) to determine the albedo of Lutetia over a wide wavelength range, extending from ~150 nm to ~700 nm. Using data from a variety of HST filters and a ground-based visible light spectrum, we employed synthetic photometry techniques to derive absolute fluxes for Lutetia. New results from ground-based measurements of Lutetia's size and shape were used to convert the absolute fluxes into albedos. We present our best model for the spectral energy distribution of Lutetia over the wavelength range 120-800 nm. There appears to be a steep drop in the albedo (by a factor of ~2) for wavelengths shorter than ~300 nm. Nevertheless, the far ultraviolet albedo of Lutetia (~10%) is considerably larger than that of typical C-chondrite material (~4%). The geometric albedo at 550 nm is 16.5 +/- 1%. Lutetia's reflectivity is not consistent with a metal-dominated surface at infrared or radar wavelengths, and its albedo at all wavelengths (UV-visibile-IR-radar) is larger than observed for typical primitive, chondritic material. We derive a relatively high FUV albedo of ~10%, a result that will be tested by observations with the Alice spectrograph during the Rosetta flyby of Lutetia in July 2010.Comment: 14 pages, 2 tables, 8 figure