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NI-DPU ASW Static Analysis & Unit Test Report post QAR
No full textThe complete continuous integration suit was applied to the DPU-ASWv1.3.9 version, the results are
summarised in the following subsections. This document contains an update of the analysis presented
in [RD-1].
Special focus was put in the analysis of the DPU-ASW modules containing the changes introduced in
the version v1.3.9 described in [RD-2], leading to a high unit testing coverage of the packages under
scrutinity. It was also verified with the static analysis that there were no new issues besides the already
known and accepted ones (minor and warnings).
The conclusion of the overall analysis is that there are no new issues in the software, and all the ones
present are minor and already known an accepted
The edge-on protoplanetary disk HH 48 NE. I. Modeling the geometry and stellar parameters
Get PDFContext. Observations of edge-on disks are an important tool for constraining general protoplanetary disk properties that cannot be determined in any other way. However, most radiative transfer models cannot simultaneously reproduce the spectral energy distributions (SEDs) and resolved scattered light and submillimeter observations of these systems because the geometry and dust properties are different at different wavelengths. Aims: We simultaneously constrain the geometry of the edge-on protoplanetary disk HH 48 NE and the characteristics of the host star. HH 48 NE is part of the JWST early-release science program Ice Age. This work serves as a stepping stone toward a better understanding of the physical structure of the disk and of the icy chemistry in this particular source. This type of modeling lays the groundwork for studying other edge-on sources that are to be observed with the JWST. Methods: We fit a parameterized dust model to HH 48 NE by coupling the radiative transfer code RADMC-3D and a Markov chain Monte Carlo framework. The dust structure was fit independently to a compiled SED, a scattered light image at 0.8 µm, and an ALMA dust continuum observation at 890 µm. Results: We find that 90% of the dust mass in HH 48 NE is settled to the disk midplane. This is less than in average disks. The atmospheric layers of the disk also exclusively contain large grains (0.3-10 µm). The exclusion of small grains in the upper atmosphere likely has important consequences for the chemistry because high-energy photons can penetrate very deeply. The addition of a relatively large cavity (~50 au in radius) is necessary to explain the strong mid-infrared emission and to fit the scattered light and continuum observations simultaneously
Gaia white dwarfs within 40 pc - III. Spectroscopic observations of new candidates in the Southern hemisphere
Get PDFWe present a spectroscopic survey of 248 white dwarf candidates within 40 pc of the Sun; of these 244 are in the Southern hemisphere. Observations were performed mostly with the Very Large Telescope (X-Shooter) and Southern Astrophysical Research Telescope. Almost all candidates were selected from Gaia Data Release 3 (DR3). We find a total of 246 confirmed white dwarfs, 209 of which had no previously published spectra, and two main-sequence star contaminants. Of these, 100 white dwarfs display hydrogen Balmer lines, 69 have featureless spectra, and two show only neutral helium lines. Additionally, 14 white dwarfs display traces of carbon, while 37 have traces of other elements that are heavier than helium. We observe 35 magnetic white dwarfs through the detection of Zeeman splitting of their hydrogen Balmer or metal spectral lines. High spectroscopic completeness (> 97 per cent) has now been reached, such that we have 1058 confirmed Gaia DR3 white dwarfs out of 1083 candidates within 40 pc of the Sun at all declinations
The Athena X-ray Integral Field Unit: a consolidated design for the system requirement review of the preliminary definition phase
Get PDFThe Athena X-ray Integral Unit (X-IFU) is the high resolution X-ray spectrometer studied since 2015 for flying in the mid-30s on the Athena space X-ray Observatory. Athena is a versatile observatory designed to address the Hot and Energetic Universe science theme, as selected in November 2013 by the Survey Science Committee. Based on a large format array of Transition Edge Sensors (TES), X-IFU aims to provide spatially resolved X-ray spectroscopy, with a spectral resolution of 2.5 eV (up to 7 keV) over a hexagonal field of view of 5 arc minutes (equivalent diameter). The X-IFU entered its System Requirement Review (SRR) in June 2022, at about the same time when ESA called for an overall X-IFU redesign (including the X-IFU cryostat and the cooling chain), due to an unanticipated cost overrun of Athena. In this paper, after illustrating the breakthrough capabilities of the X-IFU, we describe the instrument as presented at its SRR (i.e. in the course of its preliminary definition phase, so-called B1), browsing through all the subsystems and associated requirements. We then show the instrument budgets, with a particular emphasis on the anticipated budgets of some of its key performance parameters, such as the instrument efficiency, spectral resolution, energy scale knowledge, count rate capability, non X-ray background and target of opportunity efficiency. Finally, we briefly discuss the ongoing key technology demonstration activities, the calibration and the activities foreseen in the X-IFU Instrument Science Center, touch on communication and outreach activities, the consortium organisation and the life cycle assessment of X-IFU aiming at minimising the environmental footprint, associated with the development of the instrument. Thanks to the studies conducted so far on X-IFU, it is expected that along the design-to-cost exercise requested by ESA, the X-IFU will maintain flagship capabilities in spatially resolved high resolution X-ray spectroscopy, enabling most of the original X-IFU related scientific objectives of the Athena mission to be retained. The X-IFU will be provided by an international consortium led by France, The Netherlands and Italy, with ESA member state contributions from Belgium, Czech Republic, Finland, Germany, Poland, Spain, Switzerland, with additional contributions from the United States and Japan
MAVIS Instrument Software User Requirements Specifications
No full textInstrument Software User Requirements Specifications of MAVIS projec
Test on LUCIFER calibrator science frames
Get PDFIn order to find the best way to combine together telluric spectra and compute a sensitivity function, we observed different scientific frames of telluric stars. During this exploration we detected strange changes in spectra obtained from consecutive frame, this variability prevents us to compute a suitable sensitivity function, so we need to investigate better these frames
Requirement Specification for Science Alert Generation Pipeline of the ACADA System
No full textThis specification establishes the performance, design, development, test and qualification requirements for the Science Alert Generation (SAG) Pipeline sub-system of the Array Control and Data Acquisition (ACADA) System of CTAO.
SAG is the analysis pipeline running on-line that performs a Cat A/quick-look analysis [AD6] of the acquired data and produces data quality indicators, to be exposed to the support astronomer at the control room and transferred to the DPPS and the SUSS. It also serves to generate internal candidate scientific alerts, submitted to the Transients Handler
Weekly Report on JIRAM Status JRM2JNO - 20230127
No full textThis weekly report from JIRAM team to Juno’s Project started on July 2020, due to the Project's decision to remove as of October 2020 the IOSE (Instrument Operations System Engineer), role covered by Dr. Shawn Brooks from JPL.
In detail, an email exchange was established from the Juno Project to JIRAM (called JNO2JRM_YYYYMMDD and sent every Monday evening) and from JIRAM to the Project (called JRM 2JNO_YYYYMMDD and sent every Friday evening) to ensure interactions and mutual exchange of information between the team of JIRAM and the Juno Project.
In this document we report the information sent in the report JRM2JNO – 20230127
Rapporto sulle Celebrazioni per i 250 anni dalla fondazione dell’Osservatorio Astronomico di Padova
Get PDFNell’anno 2017 l'Osservatorio Astronomico di Padova ha celebrato i 250 anni dalla sua fondazione. Dall’inaugurazione del 21 marzo 2017 fino all’accensione della nuova illuminazione della Specola a fine settembre dello stesso anno è stato realizzato un nutrito programma di eventi pubblici che hanno coinvolto a vari livelli scienziati, autorità e il più largo pubblico. In questo rapporto descriviamo la rassegna “Specola 2.5.0”