Konsep Perancangan Museum Gula di Surabaya

Indonesia telah dikenal sebagai produsen gula semenjak era penjajahan Belanda dan sempat menduduki peringkat kedua di dunia. Akan tetapi, setelah kemerdekaan, produktivitas gula justru mengalami penurunan bahkan pada masa kini Indonesia menjadi negara yang mengimpor gula dari luar negeri. Kebutuhan untuk mengenang sejarah dan masa kejayaan gula di Indonesia menjadi latar belakang dari proyek ini. Proyek museum gula di Surabaya ini dirancang memberikan informasi dan edukasi kepada pengujung mengenai sejarah perkembangan gula dari masa keemasan pada era penjajahan Belanda hingga masa kini. Sejarah dihadirkan dalam desain museum melalui tata ruang yang kronologis dan sirkulasi ruang yang berurutan. Untuk mendukung kesan kronologis, maka digunakan pendalaman karakter ruang. Ruang-ruang dalam museum dirancang tidak hanya sebagai diorama pameran perkembangan gula, namun juga menampilkan suasana dan karakter ruang yang sesuai dengan kronologis sejarah gul

The deuterium fractionation of water on solar-system scales in deeply-embedded low-mass protostars

(Abridged) The water deuterium fractionation (HDO/H$_2$O abundance ratio) has traditionally been used to infer the amount of water brought to Earth by comets. Measuring this ratio in deeply-embedded low-mass protostars makes it possible to probe the critical stage when water is transported from clouds to disks in which icy bodies are formed. We present sub-arcsecond resolution observations of HDO in combination with H$_2^{18}$O from the PdBI toward the three low-mass protostars NGC 1333-IRAS 2A, IRAS 4A-NW, and IRAS 4B. The resulting HDO/H$_2$O ratio is $7.4\pm2.1\times10^{-4}$ for IRAS 2A, $19.1\pm5.4\times10^{-4}$ for IRAS 4A-NW, and $5.9\pm1.7\times10^{-4}$ for IRAS 4B. Derived ratios agree with radiative transfer models within a factor of 2-4 depending on the source. Our HDO/H$_2$O ratios for the inner regions (where $T>100$ K) of four young protostars are only a factor of 2 higher than those found for pristine, solar system comets. These small differences suggest that little processing of water occurs between the deeply embedded stage and the formation of planetesimals and comets.Comment: 10 pages, 6 figures, accepted for publication in Astronomy and Astrophysic

EVALUATION OF MADURA LANGUAGE TEXTBOOKS AT ELEMENTARY SCHOOL LEVEL

The purpose of this study was to find out information and describe the quality of Madurese language textbooks both in terms of content, presentation, and language. The type of this research is evaluation research, namely by conducting an elementary level Madura language curriculum document study (syllabus) and research instruments provided to students and material experts. The results of the study showed that students' responses to Madurese language textbooks at the elementary level included a very good category, which was 80.86. While the results of the validation of material experts state that Madurese language textbooks are in a valid category and can be used but need minor revisions, ie with a value of 80.60

The Effect of Temulawak Extract on Alkohol Fermentation From Molase Substrate by Saccharomyces Cerevisiae

Temulawak dimanfaatkan untuk meningkatkan nafsu makan dan pelindung hati bagi manusia. Ekstrak Temulawak memiliki potensi sebagai antimikrobia dalam konsentrasi yang besar. Penelitian bertujuan untuk mengetahui pengaruh penambahan sari temulawak dalam proses fermentasi alkohol dari molase menggunakan Saccharomyces cerevisiae komersial, dan berharap adanya peningkatan konsumsi gula- molase yang diiringi peningkatan alkohol oelah adanya peningkatan nafsu makan khamir. Substrat larutan molase 30% sebanyak 300 ml ditambah sari temulawak pekat (10, 20, 30,40 ml/ per 300 ml) diulang dua kali, kemudian ditambah 1 gram Saccharomyces cerevisiae lalu diinkubasikan dengan kondisi suhu kamar dan karbondioksida ditampung dalam akuades. Parameter yang diukur adalah total sel, pH, kadar gula metode spektrofotometri, kadar karbondioksida secara titrimetri, dan total akolhol metode gas kromatografi setelah tujuh hari fermentasi. Hasil menunjukkan bahwa ada Perubahan yangbtidak signifikan pada total sel khamir, pH dan residu gula, sedangkan Perubahan yang nyata pada produksi karbodioksida (meningkat sampai tiga kali lipat), dan alkohol ( menurun sampai 3%) pada pada penambahan sari temulawak 20 dan 40ml. Simpulannya sari temulawak tidak membunuh Saccharomyces cerevisiae dan menyebabkan Perubahan fermentasi alkohol akibat penambahan sari temulawak, namun tidak ada pola yang jelas

Pengaruh Strategi Know Want to Learn (Kwl) Dan Minat Membaca Terhadap Kemampuan Membaca Intensif Siswa SMP Negeri Di Temanggung

: The purpose of this study is to determine: (1) the influence of reading strategy “Know Want to Learn” (KWL) to an intensive reading skills of students; (2) the influence of high and low reading interest on students intensive reading skills; (3) the interaction between reading strategies and reading interest of students intensive reading skills. This study uses an experiment method with a 2x2 factorial design. The study population is all students in grade VII of Secondary School academic year 2011/2012 in Temanggung residence. Analysis of data using two-way analysis of variance. The results showed that: (1) there are differences in students reading skills who were taught intensively with KWL strategy and Conventional, which is an intensive reading skills of students who were taught by the KWL strategy are better than students who were taught with conventional strategies. It is shown from the experimental class averages 77.97 while the control class is 71.25; (2) there are differences in the ability of intensive reading students who have high interest in reading are better than students who have low interest in reading. It is shown that the average student has a high interest in reading is 77.80, while average students who have low reading 69.91; (3) there is no interaction between reading strategies to read interest with intensive reading skills of students. It is evident from the value of the significance of the interaction strategies of reading and interest in reading is 0.742> 0.05. The result is greater than the significance level 0.05

Physical and chemical fingerprint of protostellar disc formation

(Abridged) The purpose of this paper is to explore and compare the physical and chemical structure of Class I low-mass protostellar sources on protoplanetary disc scales. We present a study of the dust and gas emission towards a representative sample of 12 Class I protostars from the Ophiuchus molecular cloud with the Atacama Large Millimeter/submillimeter Array (ALMA). The continuum at 0.87 mm and molecular transitions from C17O, C34S, H13CO+, CH3OH, SO2 , and C2H were observed at high angular resolution (0.4", ~60 au diameter) towards each source. Disc and stellar masses are estimated from the continuum flux and position-velocity diagrams, and six of the sources show disc-like structures. Towards the more luminous sources, compact emission and large line widths are seen for transitions of SO2 that probe warm gas (Eu ~200 K). In contrast, C17O emission is detected towards the least evolved and less luminous systems. No emission of CH3OH is detected towards any of the continuum peaks, indicating an absence of warm CH3OH gas towards these sources. A power-law relation is seen between the stellar mass and the bolometric luminosity, corresponding to a mass accretion rate of (2.4 +/- 0.6) x 10^-7 Msun/year for the Class I sources. This mass accretion rate is lower than the expected value if the accretion is constant in time and rather points to a scenario of accretion occurring in bursts. The differentiation between C17O and SO2 suggests that they trace different physical components: C17O traces the densest and colder regions of the disc-envelope system, while SO2 may be associated with regions of higher temperature, such as accretion shocks. The lack of warm CH3OH emission suggests that there is no hot-core-like region around any of the sources and that the CH3OH column density averaged over the disc is low.Comment: 20 pages, 16 figures, 8 table

Chemistry of a newly detected circumbinary disk in Ophiuchus

(Abridged) Astronomers recently started discovering exoplanets around binary systems. Therefore, understanding the formation and evolution of circumbinary disks is crucial for a complete scenario of planet formation. The aim of this paper is to present the detection of a circumbinary disk around Oph-IRS67 and analyse its structure. We present high-angular-resolution (0.4", 60 AU) observations of C17O, H13CO+ , C34S, SO2, C2H and c-C3H2 molecular transitions with ALMA at 0.8 mm. The spectrally and spatially resolved maps reveal the kinematics of the circumbinary disk as well as its chemistry. Molecular abundances are estimated using RADEX. The continuum emission reveals the presence of a circumbinary disk around the two sources. This disk has a diameter of ~620 AU and is well traced by C17O and H13CO+ emission. C2H and c-C3H2 trace a higher-density region which is spatially offset from the sources (~430 AU). Finally, SO2 shows compact emission around one of the sources, Oph-IRS67 B. The molecular transitions which trace the circumbinary disk are consistent with a Keplerian profile on disk scales (< 200 AU) and an infalling profile for envelope scales (> 200 AU). The Keplerian fit leads to a mass of 2.2 Msun. Inferred CO abundances w.r.t. H2 are comparable to the canonical ISM value of 2.7e-4. This study proves the first detection of the circumbinary disk associated with Oph-IRS67. The disk is chemically differentiated from the nearby high-density region. The lack of methanol emission suggests the extended disk dominates the mass budget in the inner- most regions of the protostellar envelope, generating a flat density profile where less material is exposed to high temperatures. Thus, complex organic molecules would be associated with lower column densities. Finally, Oph-IRS67 is a promising candidate for the detection of both circumstellar disks with higher-angular-resolution observations.Comment: 19 pages, 14 figures, 6 table

A recent accretion burst in the low-mass protostar IRAS 15398-3359: ALMA imaging of its related chemistry

Low-mass protostars have been suggested to show highly variable accretion rates through-out their evolution. Such changes in accretion, and related heating of their ambient envelopes, may trigger significant chemical variations on different spatial scales and from source-to-source. We present images of emission from C17O, H13CO+, CH3OH, C34S and C2H toward the low-mass protostar IRAS 15398-3359 on 0.5" (75 AU diameter) scales with the Atacama Large Millimeter/submillimeter Array (ALMA) at 340 GHz. The resolved images show that the emission from H13CO+ is only present in a ring-like structure with a radius of about 1-1.5" (150-200 AU) whereas the CO and other high dipole moment molecules are centrally condensed toward the location of the central protostar. We propose that HCO+ is destroyed by water vapor present on small scales. The origin of this water vapor is likely an accretion burst during the last 100-1000 years increasing the luminosity of IRAS 15398-3359 by a factor of 100 above its current luminosity. Such a burst in luminosity can also explain the centrally condensed CH3OH and extended warm carbon-chain chemistry observed in this source and furthermore be reflected in the relative faintness of its compact continuum emission compared to other protostars.Comment: Accepted for publication in ApJ Letters; 14 pages, 5 figure

Cometary ices in forming protoplanetary disc midplanes

Low-mass protostars are the extrasolar analogues of the natal Solar system. Sophisticated physicochemical models are used to simulate the formation of two protoplanetary discs from the initial prestellar phase, one dominated by viscous spreading and the other by pure infall. The results show that the volatile prestellar fingerprint is modified by the chemistry en route into the disc. This holds relatively independent of initial abundances and chemical parameters: physical conditions are more important. The amount of CO2 increases via the grain-surface reaction of OH with CO, which is enhanced by photodissociation of H2O ice. Complex organic molecules are produced during transport through the envelope at the expense of CH3OH ice. Their abundances can be comparable to that of methanol ice (few per cent of water ice) at large disc radii (R > 30 au). Current Class II disc models may be underestimating the complex organic content. Planet population synthesis models may underestimate the amount of CO2 and overestimate CH3OH ices in planetesimals by disregarding chemical processing between the cloud and disc phases. The overall C/O and C/N ratios differ between the gas and solid phases. The two ice ratios show little variation beyond the inner 10 au and both are nearly solar in the case of pure infall, but both are subsolar when viscous spreading dominates. Chemistry in the protostellar envelope en route to the protoplanetary disc sets the initial volatile and prebiotically significant content of icy planetesimals and cometary bodies. Comets are thus potentially reflecting the provenances of the midplane ices in the solar nebula