Francesco Lazzarotto, N. Vertolli, D. Maschietti, A. M. Lellis, J. Ryno, F. Camozzi, S. Orsini, A. Milillo, A. Mura, E. Angelis, R. Rispoli, L. Colasanti, S. Selci, M. D’Alessandro, R. Leoni, F. M. I. R. Italy, ISM-CNR Rome Italy, Amdl srl Rome Italy, IFN-CNR Rome Italy, Fmi Helsinki Finland, OHB-Italia Milan Italy
{"title":"The BepiColombo SERENA/ELENA Instrument On-Ground Testing with the ELENA Special Check Out Equipment (SCOE)","authors":"Francesco Lazzarotto, N. Vertolli, D. Maschietti, A. M. Lellis, J. Ryno, F. Camozzi, S. Orsini, A. Milillo, A. Mura, E. Angelis, R. Rispoli, L. Colasanti, S. Selci, M. D’Alessandro, R. Leoni, F. M. I. R. Italy, ISM-CNR Rome Italy, Amdl srl Rome Italy, IFN-CNR Rome Italy, Fmi Helsinki Finland, OHB-Italia Milan Italy","doi":"10.13140/RG.2.2.31705.06248","DOIUrl":"https://doi.org/10.13140/RG.2.2.31705.06248","url":null,"abstract":"The neutral particles sensor ELENA (Emitted Low Energy Neutral Atoms) for the ESA/JAXA BepiColombo mission to Mercury (in the SERENA instrument suite) is devoted to measure low energetic neutral atoms. The main goal of the experiment is measuring the sputtering emission from planetary surfaces, from E=20eV up to E=5keV, within 1D (2 deg. x 76 deg. ). ELENA original project had also a particle discrimination system based on Time-of-Flight (TOF) of particles through the shutter on the Micro Channel Plates detector (MCP), it has been withdrawn from the flight model due to design and development problems. The ELENA SCOE is the configuration/testing system of ELENA, it allows to command operations and to set up configuration parameters on the instrument and to monitor the incoming data. The TC/TM simulation/encoding/decoding software is developed respecting the CCSDS/ECSS standards implemented by ESA, and it's SCOS2000 compatible. TC generation, HK data monitoring and basic science data analysis are operated by the SERENA EGSE, developed by the Finnish Meteorological Institute (FMI), Helsinki, Finland. The data stream outcoming from the EGSE is then preprocessed from TM to user readable formats: FITS and then ASCII csv tables with metadata collected in a detached XML file, called label. This task is performed using the PacketLib, ProcessorLib, and DISCoS (PPD) framework and is going to be used as the first level prototype of the BepiColombo Science Ground Segment processing pipeline, based in ESAC, Madrid, Spain and implemented using the PDS4 data format.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2020-02-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89972520","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Rigorous \"Rich Argument\" in Microlensing Parallax","authors":"A. Gould","doi":"10.5303/JKAS.2020.53.5.99","DOIUrl":"https://doi.org/10.5303/JKAS.2020.53.5.99","url":null,"abstract":"I show that when the observables $(vec pi_{rm E},t_{rm E},theta_{rm E},pi_s,vec mu_s)$ are well measured up to a discrete degeneracy in the microlensing parallax vector $vec pi_{rm E}$, the relative likelihood of the different solutions can be written in closed form $P_i = K H_i B_i$, where $H_i$ is the number of stars (potential lenses) having the mass and kinematics of the inferred parameters of solution $i$ and $B_i$ is an additional factor that is formally derived from the Jacobian of the transformation from Galactic to microlensing parameters. The Jacobian term $B_i$ constitutes an explicit evaluation of the ``Rich Argument'', i.e., that there is an extra geometric factor disfavoring large-parallax solutions in addition to the reduced frequency of lenses given by $H_i$. Here $t_{rm E}$ is the Einstein timescale, $theta_{rm E}$ is the angular Einstein radius, and $(pi_s,vec mu_s)$ are the (parallax, proper motion) of the microlensed source. I also discuss how this analytic expression degrades in the presence of finite errors in the measured observables.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2020-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75706211","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
G. L. Mura, G. Chiaro, R. Conceiccao, A. Angelis, M. Pimenta, B. Tom'e
{"title":"Detection of very-high-energy gamma-ray transients with monitoring facilities","authors":"G. L. Mura, G. Chiaro, R. Conceiccao, A. Angelis, M. Pimenta, B. Tom'e","doi":"10.1093/mnras/staa2141","DOIUrl":"https://doi.org/10.1093/mnras/staa2141","url":null,"abstract":"The study of the sky in Very High Energy gamma rays (VHE, E > 100 GeV) has led to the identification of a wealth of processes that are responsible for the acceleration of particles at the highest observed energies within the Milky Way and beyond. Observations with VHE facilities, like the Cherenkov Telescope Array (CTA), will be fundamental to investigate the characteristics of these processes. Still, the transient and unpredictable nature of the most powerful sources requires that effective monitoring strategies should be adopted to track them. With this study, we focus on the type of VHE transients that can be effectively detected with monitoring facilities. Using the data collected by Fermi-LAT during its observing campaign, we investigate the frequency, luminosity and timescales of different VHE transients, focusing on blazar flares and Gamma-Ray Bursts. We compare their properties with the performance of existing and future instruments. We show that pursuing an enhanced spectral coverage in the sub-TeV range with a large field-of-view instrument, operating in the Southern hemisphere, will effectively contribute to the investigation of different types of transients, both by providing prompt alerts to activate follow-up observations of the most energetic events, as well as by collecting critical information on their temporal and spectral evolution.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2020-01-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79675653","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
H. Ngo, H. Kirk, Toby Brown, Tyrone Woods, G. Eadie, S. Lawler, Locke Spencer
{"title":"Opportunities and Outcomes for Postdocs in Canada","authors":"H. Ngo, H. Kirk, Toby Brown, Tyrone Woods, G. Eadie, S. Lawler, Locke Spencer","doi":"10.5281/ZENODO.3827799","DOIUrl":"https://doi.org/10.5281/ZENODO.3827799","url":null,"abstract":"Currently, postdoctoral fellow (PDF) researchers in Canada face challenges due to the precarious nature of their employment and their overall low compensation and benefits coverage. This report presents three themes, written as statements of need, to support an inclusive and thriving PDF community. These themes are the need for better terms of employment and conditions, the need for access to grants by non-permanent research staff, and the need for a sustainable PDF hiring model that considers the outcomes for the PDFs. \u0000We make six recommendations: \u0000R1. PDFs should be hired and compensated as skilled experts in their areas, not as trainees. \u0000R2. Standard PDF hiring practices should be revised to be more inclusive of different life circumstances. \u0000- R2.1 Allow PDFs the option of part-time employment. \u0000- R2.2 Remove years-since-PhD time limits from PDF jobs. \u0000- R2.3 Financially support PDF hires for relocation and visa expenses. \u0000R3. CASCA should form a committee to advocate for and provide support to astronomy PDFs in Canada. \u0000R4. CASCA should encourage universities to create offices dedicated to their PDFs. \u0000R5. PDFs and other PhD-holding term researchers with a host institution should be able to compete for and win grants to self-fund their own research. \u0000R6. Astronomy in Canada should hire general-purpose continuing support scientist positions instead of term PDFs to fill project or mission-specific requirements. \u0000In short, we ask for prioritization of people over production of papers.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2019-11-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84354515","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"The evolution of Astronomical Observatory design","authors":"Miguel 'Angel Castro Tirado, A. Castro-Tirado","doi":"10.5303/JKAS.2019.52.4.99","DOIUrl":"https://doi.org/10.5303/JKAS.2019.52.4.99","url":null,"abstract":"This work addresses the development of the astronomical observatory all through history, from an architectural point of view, as a building in relation to the observing instruments and their functioning as a heterogeneous work center. We focused on 32 observatories (in the period 1259-2007) and carefully analyzed the architectures. Considering the impact of the construction itself or its facilities on the results of the research (thermal or structural stability, poor weather protection, turbulence, etc.), there is little attention paid to theories or studies of the architectural or construction aspects of the observatories. Therefore, this work aims to present a theoretical-critical contribution that, at least, invites the reflection of those involved in the development of astronomical observatories in the future.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2019-11-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83480703","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
N. Zobrist, G. Coiffard, B. Bumble, Noah Swimmer, Sarah Steiger, M. Daal, Giulia Collura, A. Walter, C. Bockstiegel, Neelay Fruitwala, Isabel Lipartito, B. Mazin
{"title":"Design and performance of hafnium optical and near-IR kinetic inductance detectors","authors":"N. Zobrist, G. Coiffard, B. Bumble, Noah Swimmer, Sarah Steiger, M. Daal, Giulia Collura, A. Walter, C. Bockstiegel, Neelay Fruitwala, Isabel Lipartito, B. Mazin","doi":"10.1063/1.5127768","DOIUrl":"https://doi.org/10.1063/1.5127768","url":null,"abstract":"We report on the design and performance of Microwave Kinetic Inductance Detectors (MKIDs) sensitive to single photons in the optical to near-infrared range using hafnium as the sensor material. Our test device had a superconducting transition temperature of 395 mK and a room temperature normal state resistivity of 97 $mu Omega$ cm with an RRR = 1.6. Resonators on the device displayed internal quality factors of around 200,000. Similar to the analysis of MKIDs made from other highly resistive superconductors, we find that modeling the temperature response of the detector requires an extra broadening parameter in the superconducting density of states. Finally, we show that this material and design is compatible with a full-array fabrication process which resulted in pixels with decay times of about 40 $mu$s and resolving powers of ~9 at 800 nm.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2019-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73498676","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
K. Spekkens, C. Chiang, R. Kothes, E. Rosolowsky, Michael Rupen, S. Safi-Harb, J. Sievers, G. Sivakoff, I. Stairs, N. Marel, Bob Abraham, R. Alexandroff, N. Bartel, S. Baum, M. Bietenholz, A. Boley, D. Bond, Jo-Anne C. Brown, Toby Brown, Gary Davis, J. English, G. Fahlman, L. Ferrarese, J. Francesco, B. Gaensler, S. Gaudet, V. Graber, M. Halpern, A. Hill, J. Hlavacek-Larrondo, J. Irwin, D. Johnstone, G. Joncas, V. Kaspi, J. Kavelaars, Adrian Liu, B. Matthews, J. Mirocha, R. Monsalve, C. Ng, C. O’Dea, U. Pen, R. Plume, T. Robishaw, S. Sadavoy, V. Sanghai, P. Scholz, L. Simard, R. Shaw, Saurabh Singh, K. Sigurdson, Kendrick M. Smith, D. Stevens, J. Stil, S. Tulin, Cameron Van Eck, J. Wall, J. West, Tyrone Woods, D. Wulf
{"title":"Canada and the SKA from 2020-2030","authors":"K. Spekkens, C. Chiang, R. Kothes, E. Rosolowsky, Michael Rupen, S. Safi-Harb, J. Sievers, G. Sivakoff, I. Stairs, N. Marel, Bob Abraham, R. Alexandroff, N. Bartel, S. Baum, M. Bietenholz, A. Boley, D. Bond, Jo-Anne C. Brown, Toby Brown, Gary Davis, J. English, G. Fahlman, L. Ferrarese, J. Francesco, B. Gaensler, S. Gaudet, V. Graber, M. Halpern, A. Hill, J. Hlavacek-Larrondo, J. Irwin, D. Johnstone, G. Joncas, V. Kaspi, J. Kavelaars, Adrian Liu, B. Matthews, J. Mirocha, R. Monsalve, C. Ng, C. O’Dea, U. Pen, R. Plume, T. Robishaw, S. Sadavoy, V. Sanghai, P. Scholz, L. Simard, R. Shaw, Saurabh Singh, K. Sigurdson, Kendrick M. Smith, D. Stevens, J. Stil, S. Tulin, Cameron Van Eck, J. Wall, J. West, Tyrone Woods, D. Wulf","doi":"10.5281/ZENODO.3825168","DOIUrl":"https://doi.org/10.5281/ZENODO.3825168","url":null,"abstract":"This white paper submitted for the 2020 Canadian Long-Range Planning process (LRP2020) presents the prospects for Canada and the Square Kilometre Array (SKA) from 2020-2030, focussing on the first phase of the project (SKA1) scheduled to begin construction early in the next decade. SKA1 will make transformational advances in our understanding of the Universe across a wide range of fields, and Canadians are poised to play leadership roles in several. Canadian key SKA technologies will ensure a good return on capital investment in addition to strong scientific returns, positioning Canadian astronomy for future opportunities well beyond 2030. We therefore advocate for Canada's continued scientific and technological engagement in the SKA from 2020-2030 through participation in the construction and operations phases of SKA1.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2019-11-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74895638","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Expectations on mass determination using astrometric microlensing by Gaia","authors":"J. Klüter, U. Bastian, J. Wambsganss","doi":"10.1051/0004-6361/201937061","DOIUrl":"https://doi.org/10.1051/0004-6361/201937061","url":null,"abstract":"Context. Astrometric gravitational microlensing can be used to determine the mass of a single star (the lens) with an accuracy of a few percent. To do so, precise measurements of the angular separations between lens and background star with an accuracy below 1 milli-arcsecond at different epochs are needed. Hence only the most accurate instruments can be used. However, since the timescale is in the order of months to years, the astrometric deflection might be detected by Gaia, even though each star is only observed on a low cadence. Aims. We want to show how accurately Gaia can determine the mass of the lensing star. Methods. Using conservative assumptions based on the results of the second Gaia Data release, we simulated the individual Gaia measurements for 501 predicted astrometric microlensing events during the Gaia era (2014.5 - 2026.5). For this purpose we use the astrometric parameters of Gaia DR2, as well as an approximative mass based on the absolute G magnitude. By fitting the motion of lens and source simultaneously we then reconstruct the 11 parameters of the lensing event. For lenses passing by multiple background sources, we also fit the motion of all background sources and the lens simultaneously. Using a Monte-Carlo simulation we determine the achievable precision of the mass determination. Results. We find that Gaia can detect the astrometric deflection for 114 events. Further, for 13 events Gaia can determine the mass of the lens with a precision better than 15% and for 13 + 21 = 34 events with a precision of 30% or better.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2019-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81828446","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Calibration of the IceCube Neutrino Observatory","authors":"M. Rongen","doi":"10.18154/RWTH-2019-09941","DOIUrl":"https://doi.org/10.18154/RWTH-2019-09941","url":null,"abstract":"The IceCube Neutrino Observatory instruments roughly one cubic kilometer of deep, glacial ice below the geographic South Pole with 5160 optical sensors to register the Cherenkov light of passing relativistic, charged particles. Since its construction was completed in 2010, a wide range of analyses has been performed. Those include, among others, the discovery of a high energetic astrophysical neutrino flux, competitive measurements of neutrino oscillation parameters and world-leading limits on dark matter detection. With ever-increasing statistics the influence of insufficiently known aspects of the detector performance start to limit the potential gain of future analyses. This thesis presents calibration studies on both the hardware characteristics as well as the optical properties of the instrumented ice. Improving the knowledge of the detector systematics and the methods to study them does not only aid IceCube but also inform the design of potential future IceCube extensions.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2019-11-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91347739","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
E. Neilsen, J. Annis, H. Diehl, M. Swanson, C. D'Andrea, S. Kent, A. Drlica-Wagner
{"title":"Dark Energy Survey’s Observation Strategy, Tactics, and Exposure Scheduler","authors":"E. Neilsen, J. Annis, H. Diehl, M. Swanson, C. D'Andrea, S. Kent, A. Drlica-Wagner","doi":"10.2172/1574836","DOIUrl":"https://doi.org/10.2172/1574836","url":null,"abstract":"The Dark Energy Survey is a stage III dark energy experiment, performing an optical imaging survey to measure cosmological equation of state parameters using four independent methods. The scope and complexity of the survey introduced complex strategic and tactical scheduling problems that needed to be addressed. We begin with an overview of the process used to develop DES strategy and tactics, from the inception of the project, to task forces that studied and developed strategy changes over the course of the survey, to the nightly pre-observing meeting in which immediate tactical issues were addressed. We then summarize the strategic choices made for each sub-survey, including metrics, scheduling considerations, choice of time domain fields and their sequences of exposures, and wide survey footprint and pointing layout choices. We go on to describe the detailed process that determined which specific exposures were taken at which specific times. We give a chronology of the strategic and tactical peculiarities of each year of observing, including the proposal and execution of a sixth year. We give an overview of obstac, the implementation of the DES scheduler used to simulate and evaluate strategic and tactical options, and automate exposure scheduling; and describe developments in obstac for use after DES. Appendices describe further details of data quality evaluation, tau, and t_eff; airmass calculation; and modeling of the seeing and sky brightness. The significant corpus of DES data indicates that the simple scaling relations for seeing as a function of wavelength and airmass derived from the Kolmogorov turbulence model work adequately for exposure planning purposes: deviations from these relations are modest in comparison with short time-scale seeing variations.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2019-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81568885","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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