RESUMO
This article describes the motivation, design, and progress of the Journal of Open Source Software (JOSS). JOSS is a free and open-access journal that publishes articles describing research software. It has the dual goals of improving the quality of the software submitted and providing a mechanism for research software developers to receive credit. While designed to work within the current merit system of science, JOSS addresses the dearth of rewards for key contributions to science made in the form of software. JOSS publishes articles that encapsulate scholarship contained in the software itself, and its rigorous peer review targets the software components: functionality, documentation, tests, continuous integration, and the license. A JOSS article contains an abstract describing the purpose and functionality of the software, references, and a link to the software archive. The article is the entry point of a JOSS submission, which encompasses the full set of software artifacts. Submission and review proceed in the open, on GitHub. Editors, reviewers, and authors work collaboratively and openly. Unlike other journals, JOSS does not reject articles requiring major revision; while not yet accepted, articles remain visible and under review until the authors make adequate changes (or withdraw, if unable to meet requirements). Once an article is accepted, JOSS gives it a digital object identifier (DOI), deposits its metadata in Crossref, and the article can begin collecting citations on indexers like Google Scholar and other services. Authors retain copyright of their JOSS article, releasing it under a Creative Commons Attribution 4.0 International License. In its first year, starting in May 2016, JOSS published 111 articles, with more than 40 additional articles under review. JOSS is a sponsored project of the nonprofit organization NumFOCUS and is an affiliate of the Open Source Initiative (OSI).
RESUMO
The carriers of the diffuse interstellar band spectrum represent an important baryonic component of the interstellar medium (ISM) and it is expected that their identification will contribute significantly to the understanding of the chemistry and physics of interstellar clouds. It is widely held that the carriers are linked to the presence of dust grains on account of the good correlation of their strengths with interstellar reddening, so they offer an important potential route to improving our understanding of the composition and chemistry of grains and grain surfaces. In addition to the challenge of making the spectral assignments, an important current question concerns the spatial distribution and physical state of interstellar material, with recent observational atomic and molecular line absorption studies suggesting that diffuse clouds are more 'clumpy' than previously thought. We describe here high signal-to-noise optical observations made at the Anglo-Australian Telescope using UCLES that were undertaken to investigate the spatial distribution of diffuse band carriers. We describe the first detection of 'small-scale-structure' in the diffuse band carrier distribution in the ISM, and comment on the possibilities that these data hold for contributing to the solution of the diffuse band problem and our understanding of the nature of small-scale-structure in the diffuse ISM.
