The magnetic environment of the Orion-Eridanus superbubble as revealed by Planck

Using the 353-GHz polarization observations by the Planck satellite we characterize the magnetic field in the Orion-Eridanus superbubble, a nearby expanding structure that spans more than 1600 square degrees in the sky. We identify a region of both low dispersion of polarization orientations and high polarization fraction associated with the outer wall of the superbubble identified in the most recent models of the large-scale shape of the region. We use the Davis-Chandrasekhar-Fermi method to derive plane-of-the-sky magnetic field strengths of tens of microGauss toward the southern edge of the bubble. The comparison of these values with existing Zeeman splitting observations of HI in emission suggests that the large-scale magnetic field in the region was primarily shaped by the expanding superbubble.Comment: 7 pages, 8 figures. Accepted for publication as a Letter in A&A, section 1. Letters to the Editor (08/12/2017

Mid-J CO Shock Tracing Observations of Infrared Dark Clouds I

Infrared dark clouds (IRDCs) are dense, molecular structures in the interstellar medium that can harbour sites of high-mass star formation. IRDCs contain supersonic turbulence, which is expected to generate shocks that locally heat pockets of gas within the clouds. We present observations of the CO J = 8-7, 9-8, and 10-9 transitions, taken with the Herschel Space Observatory, towards four dense, starless clumps within IRDCs (C1 in G028.37+00.07, F1 and F2 in G034.43+0007, and G2 in G034.77-0.55). We detect the CO J = 8-7 and 9-8 transitions towards three of the clumps (C1, F1, and F2) at intensity levels greater than expected from photodissociation region (PDR) models. The average ratio of the 8-7 to 9-8 lines is also found to be between 1.6 and 2.6 in the three clumps with detections, significantly smaller than expected from PDR models. These low line ratios and large line intensities strongly suggest that the C1, F1, and F2 clumps contain a hot gas component not accounted for by standard PDR models. Such a hot gas component could be generated by turbulence dissipating in low velocity shocks.Comment: 14 pages, 8 figures, 5 tables, accepted by A&A, minor updates to match the final published versio

Progress of the National Air Quality Cooperation Programme (NSL)

Om de luchtkwaliteit in Nederland te verbeteren is het Nationaal Samenwerkingsprogramma Luchtkwaliteit (NSL) opgezet. In dit programma werken de Rijksoverheid en decentrale overheden samen om te zorgen dat Nederland overal tijdig aan de grenswaarden voor fijnstof (2011) en stikstofdioxide (2015) zal voldoen. Om de voortgang te volgen is bij het NSL een monitoringsprogramma opgezet. Centraal onderdeel daarvan is een rekeninstrument waarvoor de overheden de brongegevens aanleveren. De daaruitvolgende rekenresultaten zijn vervolgens door het Bureau Monitoring (samenwerkingsverband RIVM en InfoMil) samengevoegd in voorliggende voortgangsrapportage. De prognoses voor 2011 en 2015 laten zien dat voor een groot deel van Nederland de resultaten onder de Europese grenswaarden voor PM10 (fijnstof) en NO2 liggen. Op een aantal plekken zijn er wel nieuwe of grotere overschrijdingen van de PM10- en NO2-grenswaarden zichtbaar. Bij de fijnstof (PM10) overschrijdingen gaat het hoofdzakelijk om locaties bij veehouderijen en een aantal industriele gebieden. Vooral nabij veehouderijen is op een aantal plekken nog sprake van grote overschrijdingen die lastig voor medio 2011 op te lossen zijn. De huidige prognose voor de concentraties stikstofdioxide in 2015 laat een minder gunstige ontwikkeling zien ten opzichte van wat is berekend in de vaststelling van het NSL. Dit komt voor een belangrijk deel door tegenvallende verkeersemissies wat heeft geleid tot een aantal nieuwe overschrijdingen. De nu in de prognoses berekende concentraties liggen op veel locaties net onder de grenswaarde. Met veel concentraties net onder de grenswaarde neemt het aantal overschrijdingen snel toe bij een tegenvaller in een van de gemaakte aannamen. In combinatie met een grote en deels onbekende onzekerheid in de rekenresultaten vormt dit een risico voor het behalen van de doelstelling van het NSL.The NSL has been put in place to improve air quality in the Netherlands and to ensure that the Netherlands meets the date of compliance with the EU limit values for particulate matter and nitrogen dioxide. Local, regional and national authorities work together within the framework of this programme to ensure that these goals are met. A monitoring programme, centred around a specially designed assessment tool, has been set up to monitor the progress. This tool uses data that the participating authorities are required to provide as part of the annual monitoring cycle. The results of the tool have been bundled by the Bureau Monitoring into this progress report. The prognosis for 2011 and 2015, based on the results obtained using the assessment tool, are that the concentrations of PM10 and NO2 fall below the EU limit values in most parts of the Netherlands. However, exceedances of the limit values do occur at specific locations. For PM10, these exceedances mostly occur close to a number of industrial sites and stock farms. Particularly high exceedances in the vicinity of these stock farms will make it difficult to meet the limit values by mid 2011 at these locations. The prognostications for NO2 show a less favourable decline in NO2 concentrations than was modelled at the establishment of the NSL. This is mostly due to the decline in traffic emissions falling short of expectations, resulting in new exceedances. At many locations, the calculated concentrations in the prognostications fall just under the limit value and, consequently, there will be a large increase in the number of exceedances when one or more of the premises become less favourable. This possibility, together with the large and partially unknown uncertainty in the calculation results, add up to a risk for not meeting the limit values by the date of compliance.VRO

Is copyright blind to the visual?

This article argues that, with respect to the copyright protection of works of visual art, the general uneasiness that has always pervaded the relationship between copyright law and concepts of creativity produces three anomalous results. One of these is that copyright lacks much in the way of a central concept of 'visual art' and, to the extent that it embraces any concept of the 'visual', it is rooted in the rhetorical discourse of the Renaissance. This means that copyright is poorly equipped to deal with modern developments in the visual arts. Secondly, the pervasive effect of rhetorical discourse appears to have made it particularly difficult for copyright law to strike a meaningful balance between protecting creativity and permitting its use in further creative works. Thirdly, just when rhetorical discourse might have been useful in identifying the significance and materiality of the unique one-off work of visual art, copyright law chooses to ignore its implications

The Small-Scale Physical Structure and Fragmentation Difference of Two Embedded Intermediate Mass Protostars in Orion

Intermediate-mass (IM) protostars, the bridge between the very common solar-like protostars and the more massive, but rarer, O and B stars, can only be studied at high physical spatial resolutions in a handful of clouds. In this paper, we present and analyze the continuum results from an observing campaign at the Submillimeter Array (SMA) targeting two well-studied IM protostars in Orion, NGC 2071 and L1641 S3 MMS 1. The extended SMA (eSMA) probes structure at angular resolutions up to 0".2, revealing protostellar disks on scales of ∼200 AU. Continuum flux measurements on these scales indicate that a significant amount of mass, a few tens of M_⊙, is present. Envelope, stellar, and disk masses are derived using compact, extended, and eSMA configurations and compared against spectral energy distribution fitting models. We hypothesize that fragmentation into three components occurred within NGC 2071 at an early time, when the envelopes were less than 10% of their current masses, e.g., <0.5 M. No fragmentation occurred for L1641 S3 MMS 1. For NGC 2071, evidence is given that the bulk of the envelope material currently around each source was accreted after the initial fragmentation. In addition, about 30% of the total core mass is not yet associated to one of the three sources. A global accretion model is favored and a potential accretion history of NGC 2071 is presented. It is shown that the relatively low level of fragmentation in NGC 2071 was stifled compared to the expected fragmentation from a Jeans argument. Similarly, the lack of fragmentation in L1641 S3 MMS 1 is likely due to similar arguments

Tuna fisheries in India: Recent trends

Tuna is one of the least exploited resources of the Indian seas accounting for 0.98 % of the total marine fish catch of India at the 1978 level. On the other hand tuna resources have been exploited by countries such as Japan, Korea and Taiwan from the Indian Ocean. Relevant portions of the recommendations of the 'Symposium on scombroid fishes' held at Mandapam camp. The authorities involved with the planning of the Indian Ocean Expedition give due consideration to gathering and collating the information which should be useful in aiding the development of high seas fisheries for scombroid fishes in the Indian Ocean. In the context of these developments and the need for efficient utilisation of the resources of the Exclusive Economic Zone, a brief account on the trend in the tuna fisheries in the country is presented here

The JCMT Gould Belt Survey: properties of star-forming filaments in Orion A North

We develop and apply a Hessian-based filament detection algorithm to submillimetre continuum observations of Orion A North. The resultant filament radial density profiles are fitted with beam-convolved line-of-sight Plummer-profiles using Markov chain Monte Carlo techniques. The posterior distribution of the radial decay parameter demonstrates that the majority of filaments exhibit p = 1.5–3, with a mode at p = 2.2, suggesting deviation from the Ostriker p = 4 isothermal, equilibrium, self-gravitating cylinder. The spatial distribution of young stellar objects relative to the high column density filaments is investigated, yielding a lower limit on the star-forming age of the integral-shaped filament ∼1.4 Myr. Additionally, inferred lifetimes of filaments are examined which suggest long-term filament accretion, varying rates of star formation, or both. Theoretical filament stability measures are determined with the aid of HARP C18O J = 3–2 observations and indicate that the majority of filaments are gravitationally subcritical, despite the presence of young protostars. The results from this investigation are consistent with the one-dimensional accretion flow filament model recently observed in numerical simulations