Report drawn up on behalf of the Committee on Economic and Monetary Affairs on the proposal from the Commission of the European Communities to the Council (Doc. 1-99/83-COM(83) 85 final) for a Council Decision implementing the decision empowering the Commission to borrow under the New Community Instrument for the purpose of promoting investment within the Community, Working Documents 1983-1984, Document 1-236/83, 3 May 1983

The 4MOST([1]) instrument is a concept for a wide-field, fibre-fed high multiplex spectroscopic instrument facility on the ESO VISTA telescope designed to perform a massive (initially >25x10(6) spectra in 5 years) combined all-sky public survey. The main science drivers are: Gaia follow up of chemo-dynamical structure of the Milky Way, stellar radial velocities, parameters and abundances, chemical tagging; eROSITA follow up of cosmology with x-ray clusters of galaxies, X-ray AGN/galaxy evolution to z similar to 5, Galactic X-ray sources and resolving the Galactic edge; Euclid/LSST/SKA and other survey follow up of Dark Energy, Galaxy evolution and transients. The surveys will be undertaken simultaneously requiring: highly advanced targeting and scheduling software, also comprehensive data reduction and analysis tools to produce high-level data products. The instrument will allow simultaneous observations of similar to 1600 targets at R similar to 5,000 from 390-900nm and similar to 800 targets at R>18,000 in three channels between similar to 395-675nm (channel bandwidth: 45nm blue, 57nm green and 69nm red) over a hexagonal field of view of similar to 4.1 degrees2. The initial 5-year 4MOST survey is currently expect to start in 2020. We provide and overview of the 4MOST systems: opto-mechanical, control, data management and operations concepts; and initial performance estimates

4MOST: Project overview and information for the First Call for Proposals

We introduce the 4-metre Multi-Object Spectroscopic Telescope (4MOST), a new high-multiplex, wide-field spectroscopic survey facility under development for the four-metre-class Visible and Infrared Survey Telescope for Astronomy (VISTA) at Paranal. Its key specifications are: a large field of view (FoV) of 4.2 square degrees and a high multiplex capability, with 1624 fibres feeding two low-resolution spectrographs ($R = \lambda/\Delta\lambda \sim 6500$), and 812 fibres transferring light to the high-resolution spectrograph ($R \sim 20\,000$). After a description of the instrument and its expected performance, a short overview is given of its operational scheme and planned 4MOST Consortium science; these aspects are covered in more detail in other articles in this edition of The Messenger. Finally, the processes, schedules, and policies concerning the selection of ESO Community Surveys are presented, commencing with a singular opportunity to submit Letters of Intent for Public Surveys during the first five years of 4MOST operations

Calibration system for the 4MOST multi object fiber-fed spectrographs

A novel concept for the calibration of multi object fiber-fed spectrographs is described for the 4MOST instrument. The 4MOST facility is foreseen to start science operations in 2022 at the ESO VISTA telescope. The calibration system provides intensity, wavelength and resolution calibrations for the 4MOST spectrographs. The heart of the system is a combination of a bright broad band lamp and a Fabry-Perot etalon. The lamp is able to provide sufficient flux to illuminate the VISTA focal plane and the Fabry-Perot etalon provides a regular comb of spectral lines. The Fabry-Perot etalon can be moved in and out of the optical beam to choose between intensity and spectral calibrations. A fiber bundle of 156 fibers is guided to the VISTA spider arms where each fiber is connected to a small integrating sphere. The integrating spheres are attached to the bottom side of the four VISTA telescope spider struts and provide unvignetted illumination of the telescope. The exit port of the integrating spheres is projected on the VISTA focal plane with a small collimator lens. The integrating spheres assure a uniform illumination of the focal plane and are insensitive to FRD effects of the input fibers due to motion and stress during telescope movements. The calibration system illumination only originates from the telescope spiders and therefore the telescope pupil is not fully filled. The calibration system uses the azimuthal scrambling properties of the fibers that connect the telescope focal plane and the spectrometers to completely fill the spectrograph pupil

Rapid and Accurate Detection of Urinary Pathogens by Mobile IMS-Based Electronic Nose: A Proof-of-Principle Study

Urinary tract infection (UTI) is a common disease with significant morbidity and economic burden, accounting for a significant part of the workload in clinical microbiology laboratories. Current clinical chemisty point-of-care diagnostics rely on imperfect dipstick analysis which only provides indirect and insensitive evidence of urinary bacterial pathogens. An electronic nose (eNose) is a handheld device mimicking mammalian olfaction that potentially offers affordable and rapid analysis of samples without preparation at athmospheric pressure. In this study we demonstrate the applicability of ion mobility spectrometry (IMS) -based eNose to discriminate the most common UTI pathogens from gaseous headspace of culture plates rapidly and without sample preparation. We gathered a total of 101 culture samples containing four most common UTI bacteries: E. coli, S. saprophyticus, E. faecalis, Klebsiella spp and sterile culture plates. The samples were analyzed using ChemPro 100i device, consisting of IMS cell and six semiconductor sensors. Data analysis was conducted by linear discriminant analysis (LDA) and logistic regression (LR). The results were validated by leave-one-out and 5-fold cross validation analysis. In discrimination of sterile and bacterial samples sensitivity of 95% and specificity of 97% were achieved. The bacterial species were identified with sensitivity of 95% and specificity of 96% using eNose as compared to urine bacterial cultures.These findings strongly demonstrate the ability of our eNose to discriminate bacterial cultures and provides a proof of principle to use this method in urinanalysis of UTI

4MOST: 4-metre Multi-Object Spectroscopic Telescope

1134MOST is a wide-field, high-multiplex spectroscopic survey facility under development for the VISTA telescope of the European Southern Observatory (ESO). Its main science drivers are in the fields of galactic archeology, high-energy physics, galaxy evolution and cosmology. 4MOST will in particular provide the spectroscopic complements to the large area surveys coming from space missions like Gaia, eROSITA, Euclid, and PLATO and from ground-based facilities like VISTA, VST, DES, LSST and SKA. The 4MOST baseline concept features a 2.5 degree diameter field-of-view with ~2400 fibres in the focal surface that are configured by a fibre positioner based on the tilting spine principle. The fibres feed two types of spectrographs; ~1600 fibres go to two spectrographs with resolution R<5000 (λ~390-930 nm) and ~800 fibres to a spectrograph with R>18,000 (λ~392-437 nm and 515-572 nm and 605-675 nm). Both types of spectrographs are fixed-configuration, three-channel spectrographs. 4MOST will have an unique operations concept in which 5 year public surveys from both the consortium and the ESO community will be combined and observed in parallel during each exposure, resulting in more than 25 million spectra of targets spread over a large fraction of the southern sky. The 4MOST Facility Simulator (4FS) was developed to demonstrate the feasibility of this observing concept. 4MOST has been accepted for implementation by ESO with operations expected to start by the end of 2020. This paper provides a top-level overview of the 4MOST facility, while other papers in these proceedings provide more detailed descriptions of the instrument concept[1], the instrument requirements development[2], the systems engineering implementation[3], the instrument model[4], the fibre positioner concepts[5], the fibre feed[6], and the spectrographs[7].nonenonede Jong Roelof S.; Barden Sam; Bellido-Tirado Olga; Brynnel Joar; Chiappini Cristina; Depagne Éric; Haynes Roger; Johl Diana; Phillips Daniel P.; Schnurr Olivier; Schwope Axel D.; Walcher Jakob; Bauer Svend M.; Cescutti G; Cioni Maria-Rosa L.; Dionies Frank; Enke Harry; Haynes Dionne M.; Kelz Andreas; Kitaura Francisco S.; Lamer Georg; Minchev Ivan; Müller Volker; Nuza Sebastián. E.; Olaya Jean-Christophe; Piffl Tilmann; Popow Emil; Saviauk Allar; Steinmetz Matthias; Ural Uǧur; Valentini Monica; Winkler Roland; Wisotzki Lutz; Ansorge Wolfgang R.; Banerji Manda; Gonzalez Solares Eduardo; Irwin Mike; Kennicutt Robert C.; King David M. P.; McMahon Richard; Koposov Sergey; Parry Ian R.; Sun Xiaowei; Walton Nicholas A.; Finger Gert; Iwert Olaf; Krumpe Mirko; Lizon Jean-Louis; Mainieri Vincenzo; Amans Jean-Philippe; Bonifacio Piercarlo; Cohen Matthieu; François Patrick; Jagourel Pascal; Mignot Shan B.; Royer Frédéric; Sartoretti Paola; Bender Ralf; Hess Hans-Joachim; Lang-Bardl Florian; Muschielok Bernard; Schlichter Jörg; Böhringer Hans; Boller Thomas; Bongiorno Angela; Brusa Marcella; Dwelly Tom; Merloni Andrea; Nandra Kirpal; Salvato Mara; Pragt Johannes H.; Navarro Ramón; Gerlofsma Gerrit; Roelfsema Ronald; Dalton Gavin B.; Middleton Kevin F.; Tosh Ian A.; Boeche Corrado; Caffau Elisabetta; Christlieb Norbert; Grebel Eva K.; Hansen Camilla J.; Koch Andreas; Ludwig Hans-G.; Mandel Holger; Quirrenbach Andreas; Sbordone Luca; Seifert Walter; Thimm Guido; Helmi Amina; trager Scott C.; Bensby Thomas; Feltzing Sofia; Ruchti Gregory; Edvardsson Bengt; Korn Andreas; Lind Karin; Boland Wilfried; Colless Matthew; Frost Gabriella; Gilbert James; Gillingham Peter; Lawrence Jon; Legg Neville; Saunders Will; Sheinis Andrew; Driver Simon; Robotham Aaron; Bacon Roland; Caillier Patrick; Kosmalski Johan; Laurent Florence; Richard Johande Jong Roelof, S.; Barden, Sam; Bellido-Tirado, Olga; Brynnel, Joar; Chiappini, Cristina; Depagne, Éric; Haynes, Roger; Johl, Diana; Phillips Daniel, P.; Schnurr, Olivier; Schwope Axel, D.; Walcher, Jakob; Bauer Svend, M.; Cescutti, G; Cioni Maria-Rosa, L.; Dionies, Frank; Enke, Harry; Haynes Dionne, M.; Kelz, Andreas; Kitaura Francisco, S.; Lamer, Georg; Minchev, Ivan; Müller, Volker; Nuza, Sebastián. E.; Olaya, Jean-Christophe; Piffl, Tilmann; Popow, Emil; Saviauk, Allar; Steinmetz, Matthias; Ural, Uǧur; Valentini, Monica; Winkler, Roland; Wisotzki, Lutz; Ansorge Wolfgang, R.; Banerji, Manda; Gonzalez Solares, Eduardo; Irwin, Mike; Kennicutt Robert, C.; King David, M. P.; Mcmahon, Richard; Koposov, Sergey; Parry Ian, R.; Sun, Xiaowei; Walton Nicholas, A.; Finger, Gert; Iwert, Olaf; Krumpe, Mirko; Lizon, Jean-Louis; Mainieri, Vincenzo; Amans, Jean-Philippe; Bonifacio, Piercarlo; Cohen, Matthieu; François, Patrick; Jagourel, Pascal; Mignot Shan, B.; Royer, Frédéric; Sartoretti, Paola; Bender, Ralf; Hess, Hans-Joachim; Lang-Bardl, Florian; Muschielok, Bernard; Schlichter, Jörg; Böhringer, Hans; Boller, Thomas; Bongiorno, Angela; Brusa, Marcella; Dwelly, Tom; Merloni, Andrea; Nandra, Kirpal; Salvato, Mara; Pragt Johannes, H.; Navarro, Ramón; Gerlofsma, Gerrit; Roelfsema, Ronald; Dalton Gavin, B.; Middleton Kevin, F.; Tosh Ian, A.; Boeche, Corrado; Caffau, Elisabetta; Christlieb, Norbert; Grebel Eva, K.; Hansen Camilla, J.; Koch, Andreas; Ludwig, Hans-G.; Mandel, Holger; Quirrenbach, Andreas; Sbordone, Luca; Seifert, Walter; Thimm, Guido; Helmi, Amina; trager Scott, C.; Bensby, Thomas; Feltzing, Sofia; Ruchti, Gregory; Edvardsson, Bengt; Korn, Andreas; Lind, Karin; Boland, Wilfried; Colless, Matthew; Frost, Gabriella; Gilbert, James; Gillingham, Peter; Lawrence, Jon; Legg, Neville; Saunders, Will; Sheinis, Andrew; Driver, Simon; Robotham, Aaron; Bacon, Roland; Caillier, Patrick; Kosmalski, Johan; Laurent, Florence; Richard, Joha

4MOST-4-metre Multi-Object Spectroscopic Telescope

4MOST is a wide-field, high-multiplex spectroscopic survey facility under development for the VISTA telescope of the European Southern Observatory (ESO). Its main science drivers are in the fields of galactic archeology, high-energy physics, galaxy evolution and cosmology. 4MOST will in particular provide the spectroscopic complements to the large area surveys coming from space missions like Gaia, eROSITA, Euclid, and PLATO and from ground-based facilities like VISTA, VST, DES, LSST and SKA. The 4MOST baseline concept features a 2.5 degree diameter field-of-view with similar to 2400 fibres in the focal surface that are configured by a fibre positioner based on the tilting spine principle. The fibres feed two types of spectrographs; similar to 1600 fibres go to two spectrographs with resolution R> 5000 (lambda similar to 390-930 nm) and similar to 800 fibres to a spectrograph with R> 18,000 (lambda similar to 392-437 nm & 515-572 nm & 605-675 nm). Both types of spectrographs are fixed-configuration, three-channel spectrographs. 4MOST will have an unique operations concept in which 5 year public surveys from both the consortium and the ESO community will be combined and observed in parallel during each exposure, resulting in more than 25 million spectra of targets spread over a large fraction of the southern sky. The 4MOST Facility Simulator (4FS) was developed to demonstrate the feasibility of this observing concept. 4MOST has been accepted for implementation by ESO with operations expected to start by the end of 2020. This paper provides a top-level overview of the 4MOST facility, while other papers in these proceedings provide more detailed descriptions of the instrument concept[1], the instrument requirements development[2], the systems engineering implementation[3], the instrument model[4], the fibre positioner concepts[5], the fibre feed[6], and the spectrographs[7]