Product Planning techniques: investigating the differences between research trajectories and industry expectations

According to several literature sources, Product Planning is acknowledged as a primary driver of future commercial success for new designed products, and it is schematically constituted by the identification of business opportunities and the selection of most promising alternatives. Despite the recalled relevance of Product Planning, it emerges that a marginal quantity of companies have adopted formal methods to carry out this task. The paper attempts to provide a major understanding about such a limited implementation of Product Planning techniques and other open issues emerging from the analysis of the literature concerning the initial phases of engineering design cycles. The presented study investigates the claimed benefits of methods described in the literature, the level to which such tools are diffused through educational programs in Technical Institutes, the expectations and the demands of a sample of enterprises with respect to new tools supporting Product Planning. It emerges that, whereas existing methods strive to fulfil relevant properties according to the perception of the companies, limitations come out in terms of the transfer of the proposed techniques and their perceived reliability

ALMA observations of polarized emission toward the CW Tau and DG Tau protoplanetary disks: constraints on dust grain growth and settling

We present polarimetric data of CW Tau and DG Tau, two well-known Class II disk/jet systems, obtained with the Atacama Large Millimeter/submillimeter Array at 870 $\mu$m and 0."2 average resolution. In CW Tau, the total and polarized emission are both smooth and symmetric, with polarization angles almost parallel to the minor axis of the projected disk. In contrast, DG Tau displays a structured polarized emission, with an elongated brighter region in the disk's near side and a belt-like feature beyond about 0."3 from the source. At the same time the total intensity is spatially smooth, with no features. The polarization pattern, almost parallel to the minor axis in the inner region, becomes azimuthal in the outer belt, possibly because of a drop in optical depth. The polarization fraction has average values of 1.2% in CW Tau and 0.4% in DG Tau. Our results are consistent with polarization from self-scattering of the dust thermal emission. Under this hypothesis, the maximum size of the grains contributing to polarization is in the range 100 - 150 $\mu$m for CW Tau and 50 - 70 $\mu$m for DG Tau. The polarization maps combined with dust opacity estimates indicate that these grains are distributed in a geometrically thin layer in CW Tau, representing a settling in the disk midplane. Meanwhile, such settling is not yet apparent for DG Tau. These results advocate polarization studies as a fundamental complement to total emission observations, in investigations of the structure and the evolution of protoplanetary disks.Comment: 8 pages, 5 figures. Accepted for publication in ApJ Letter

Polarization in Disks

This white paper discusses how disk polarization observations can be used to study disk and grain properties during the planet formation process. Such studies require very sensitive and high resolution multi-wavelength observations.Fil: Stephens, Ian W.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Li, Zhi Yun. University of Virginia; Estados UnidosFil: Yang, Haifeng. Tsinghua University; ChinaFil: Kataoka, Akimasa. National Astronomical Observatory of Japan; JapónFil: Looney, Leslie. University of Illinois at Urbana; Estados UnidosFil: Hull, Charles L. H.. National Astronomical Observatory Of Japan; JapónFil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Sadavoy, Sarah. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Kwon, Woojin. Korea Astronomy And Space Science Institute; Corea del SurFil: Satoshi, Ohashi. Riken Cluster For Pioneering Research; JapónFil: Tazaki, Ryo. Tohoku University; JapónFil: Li, Dan. National Optical Astronomy Observatory; Estados UnidosFil: Hoang, Thiem. Korea Astronomy And Space Science Institute; Corea del SurFil: Bertrang, Gesa H. M.. Max Planck Institute For Extraterrestrial Physics; AlemaniaFil: Carrasco Gonzalez, Carlos Eugenio. Instituto de Radioastronomía y Astrofísica; MéxicoFil: Dent, William. Atacama Large (sub)millimeter Array; ChileFil: Takahashi, Satoko. National Institutes Of Natural Sciences - National Astronomical Observatory Of Japan; JapónFil: Bacciotti, Francesca. Istituto Nazionale di Astrofisica; ItaliaFil: Alves, Felipe O.. Max Planck Institute For Extraterrestrial Physics; AlemaniaFil: Girart, Josep M.. Instituto de Ciencias del Espacio; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Rao, Ramprasad. Academia Sinica; ChinaFil: Pohl, Adriana. Max Planck Institute For Extraterrestrial Physics; AlemaniaFil: Padovani, Marco. Istituto Nazionale di Astrofisica; ItaliaFil: Galli, Daniele. Istituto Nazionale di Astrofisica; ItaliaFil: Lee, Chin Fei. Academia Sinica; ChinaFil: Segura Cox, Dominique. Max Planck Institute For Extraterrestrial Physics; AlemaniaAstro2020: APC Science White PapersEstados UnidosAmerica Astronomical Societ

SHARK-NIR, the coronagraphic camera for LBT, moving toward construction

SHARK-NIR is one of the two coronagraphic instruments proposed for the Large Binocular Telescope. Together with SHARK-VIS (performing coronagraphic imaging in the visible domain), it will offer the possibility to do binocular observations combining direct imaging, coronagraphic imaging and coronagraphic low resolution spectroscopy in a wide wavelength domain, going from 0.5{\mu}m to 1.7{\mu}m. Additionally, the contemporary usage of LMIRCam, the coronagraphic LBTI NIR camera, working from K to L band, will extend even more the covered wavelength range. In January 2017 SHARK-NIR underwent a successful final design review, which endorsed the instrument for construction and future implementation at LBT. We report here the final design of the instrument, which foresees two intermediate pupil planes and three focal planes to accomodate a certain number of coronagraphic techniques, selected to maximize the instrument contrast at various distances from the star. Exo-Planets search and characterization has been the science case driving the instrument design, but the SOUL upgrade of the LBT AO will increase the instrument performance in the faint end regime, allowing to do galactic (jets and disks) and extra-galactic (AGN and QSO) science on a relatively wide sample of targets, normally not reachable in other similar facilities.Comment: 8 pages, 6 figures, AO4ELT5 conference proceeding

SHARK-NIR: from K-band to a key instrument, a status update

SHARK-NIR channel is one of the two coronagraphic instruments proposed for the Large Binocular Telescope, in the framework of the call for second generation instruments, issued in 2014. Together with the SHARK-VIS channel, it will offer a few observing modes (direct imaging, coronagraphic imaging and coronagraphic low resolution spectroscopy) covering a wide wavelength domain, going from 0.5μm to 1.7μm. Initially proposed as an instrument covering also the K-band, the current design foresees a camera working from Y to H bands, exploiting in this way the synergy with other LBT instruments such as LBTI, which is actually covering wavelengths greater than L' band, and it will be soon upgraded to work also in K band. SHARK-NIR has been undergoing the conceptual design review at the end of 2015 and it has been approved to proceed to the final design phase, receiving the green light for successive construction and installation at LBT. The current design is significantly more flexible than the previous one, having an additional intermediate pupil plane that will allow the usage of coronagraphic techniques very efficient in term of contrast and vicinity to the star, increasing the instrument coronagraphic performance. The latter is necessary to properly exploit the search of giant exo-planets, which is the main science case and the driver for the technical choices of SHARK-NIR. We also emphasize that the LBT AO SOUL upgrade will further improve the AO performance, making possible to extend the exo-planet search to target fainter than normally achieved by other 8-m class telescopes, and opening in this way to other very interesting scientific scenarios, such as the characterization of AGN and Quasars (normally too faint to be observed) and increasing considerably the sample of disks and jets to be studied. Finally, we emphasize that SHARK-NIR will offer XAO direct imaging capability on a FoV of about 15"x15", and a simple coronagraphic spectroscopic mode offering spectral resolution ranging from few hundreds to few thousands. This article presents the current instrument design, together with the milestones for its installation at LBT. <P /

SHARK-NIR, toward the installation at the Large Binocular Telescope

SHARK-NIR in an instrument that will provide direct imaging, coronagraphic imaging, dual band imaging and low resolution spectroscopy in Y, J and H bands, and it will be soon installed at the Large Binocular Telescope. Used in combination with SHARK-VIS (operating in V band) and LMIRCam of LBTI (operating from K to M bands), SHARKNIR will exploit coronagraphic simultaneous observations in three different wavelengths. Exoplanets search and characterization, young stellar systems, jets and disks are the main science cases, but the extreme performance of the LBT AO systems, above all in the faint end regime, will allow to open to science difficult to be achieved from other similar instruments, such as AGN and QSO morphological studies. A variety of coronagraphic techniques have been implemented, as the Gaussian Lyot, Shaped Pupil and Four Quadrant masks, with the aim to possibly have a suitable coronagraphic masks for each science case, since the coronagraphic requirement in term of contrast and inner and outer working angle are depending on the target and on the science to be achieved. We report here about the SHARK-NIR status, that should be installed at LBT in mid-2021 © 2020 SPIE.This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]

SHARK-NIR, first results of the commissioning at LBT

International audienceSHARK-NIR, first results of the commissioning at LB