JuanCastillo29/space-mission-intelligence-data huggingface dataset:
A.

Sozzetti27, W.

Thuillot38, W. van Reeven47, Y.

Viala4, U.

Abbas27, A.

Abreu Aramburu61, S.

Accart62, J.J.

Aguado60, P.M.

Allan34, W.

Allasia63, G.

Altavilla31, M.A. Álvarez53, J.

Alves64, R.I.

Anderson65, 8, A.H.

Andrei66, 67, 36, E.

Anglada Varela57, 32, E.

Antiche10, T.

Antoja1, S.

Antón68, 69, B.

Arcay53, A.

Atzei21, L.

Ayache70, N.

Bach47, S.G.

Baker26, L.

Balaguer-Núñez10, C.

Barache36, C.

Barata54, A.

Barbier62, F.

Barblan8, M.

Baroni21, D.

Barrado y Navascués71, M.

Barros54, M.A.

Barstow72, U.

Becciani52, M.

Bellazzini31, G.

Bellei73, A.

Bello García74, V.

Belokurov7, P.

Bendjoya14, A.

Berihuete75, L.

Bianchi63, O.

Bienaymé45, F.

Billebaud23, N.

Blagorodnova7, S.

Blanco-Cuaresma8, 23, T.

Boch45, A.

Bombrun42, R.

Borrachero10, S.

Bouquillon36, G.

Bourda23, H.

Bouy71, A.

Bragaglia31, M.A.

Breddels76, N.

Brouillet23, T.

Brüsemeister6, B.

Bucciarelli27, F.

Budnik15, P.

Burgess7, R.

Burgon29, A.

Burlacu16, D.

Busonero27, R.

Buzzi27, E.

Caffau4, J.

Cambras77, H.

Campbell7, R.

Cancelliere78, T.

Cantat-Gaudin3, T.

Carlucci36, J.M.

Carrasco10, M.

Castellani79, P.

Charlot23, J.

Charnas33, P.

Charvet17, F.

Chassat17, A.

Chiavassa14, M.

Clotet10, G.

Cocozza31, R.S.

Collins41, P.

Collins15, G.

Costigan2, F.

Crifo4, N.J.G.

Cross41, M.

Crosta27, C.

Crowley42, C.

Dafonte53, Y.

Damerdji43, 80, A.

Dapergolas37, P.

David38, M.

David81, P.

De Cat39, F. de Felice82, P. de Laverny14, F.

De Luise83, R.

De March30, D. de Martino84, R. de Souza85, J.

Debosscher24, E. del Pozo47, M.

Delbo14, A.

Delgado7, H.E.

Delgado60, F. di Marco86, P.

Di Matteo4, S.

Diakite59, E.

Distefano52, C.

Dolding26, S.

Dos Anjos85, P.

Drazinos49, J.

Durán57, Y.

Dzigan87, 88, E.

Ecale17, B.

Edvardsson50, H.

Enke89, M.

Erdmann21, D.

Escolar21, M.

Espina15, N.W.

Evans7, G.

Eynard Bontemps62, C.

Fabre90, M.

Fabrizio58, 83, S.

Faigler91, A.J.

Falcão92, M.

Farràs Casas10, F.

Faye17, L.

Federici31, G.

Fedorets55, J.

Fernández-Hernández32, P.

Fernique45, A.

Fienga93, F.

Figueras10, F.

Filippi30, K.

Findeisen4, A.

Fonti30, M.

Fouesneau5, E.

Fraile94, M.

Fraser7, J.

Fuchs95, R.

Furnell21, M.

Gai27, S.

Galleti31, L.

Galluccio14, D.
as10, F.

Faye17, L.

Federici31, G.

Fedorets55, J.

Fernández-Hernández32, P.

Fernique45, A.

Fienga93, F.

Figueras10, F.

Filippi30, K.

Findeisen4, A.

Fonti30, M.

Fouesneau5, E.

Fraile94, M.

Fraser7, J.

Fuchs95, R.

Furnell21, M.

Gai27, S.

Galleti31, L.

Galluccio14, D.

Garabato53, F.

García-Sedano60, P.

Garé21, A.

Garofalo31, N.

Garralda10, P.

Gavras4, 37, 49, J.

Gerssen89, R.

Geyer11, G.

Gilmore7, S.

Girona96, G.

Giuffrida58, M.

Gomes54, A.

González-Marcos97, J.

González-Núñez32, 98, J.J.

González-Vidal10, M.

Granvik55, A.

Guerrier62, P.

Guillout45, J.

Guiraud16, A.

Gúrpide10, R.

Gutiérrez-Sánchez22, L.P.

Guy33, R.

Haigron4, D.

Hatzidimitriou49, M.

Haywood4, U.

Heiter50, A.

Helmi76, D.

Hobbs13, W.

Hofmann6, B.

Holl8, G.

Holland7, J.A.S.

Hunt26, A.

Hypki2, V.

Icardi30, M.

Irwin7, G.

Jevardat de Fombelle33, P.

Jofré7, 23, P.G.

Jonker99, 25, A.

Jorissen18, F.

Julbe10, A.

Karampelas49, 37, A.

Kochoska100, R.

Kohley12, K.

Kolenberg101, 24, 102, E.

Kontizas37, S.E.

Koposov7, G.

Kordopatis89, 14, P.

Koubsky95, A.

Kowalczyk15, A.

Krone-Martins54, M.

Kudryashova38, I.

Kull91, R.K.

Bachchan13, F.

Lacoste-Seris62, A.F.

Lanza52, J.-B.

Lavigne62, C.

Le Poncin-Lafitte36, Y.

Lebreton4, 103, T.

Lebzelter64, S.

Leccia84, N.

Leclerc4, I.

Lecoeur-Taibi33, V.

Lemaitre62, H.

Lenhardt6, F.

Leroux62, S.

Liao27, 104, E.

Licata63, H.E.P.

Lindstrøm28, 105, T.A.

Lister106, E.

Livanou49, A.

Lobel39, W.

Löffler6, M.

López71, A.

Lopez-Lozano107, D.

Lorenz64, T.

Loureiro15, I.

MacDonald41, T.

Magalhães Fernandes92, S.

Managau62, R.G.

Mann41, G.

Mantelet6, O.

Marchal4, J.M.

Marchant108, M.

Marconi84, J.

Marie109, S.

Marinoni79, 58, P.M.

Marrese79, 58, G.

Marschalkó110, 111,
Article number, page 1 of 36

D.J.

Marshall112, J.M.

Martín-Fleitas47, M.

Martino30, N.

Mary62, G.

Matijeviˇc89, T.

Mazeh91, P.J.

McMillan13, S.

Messina52, A.

Mestre113, D.

Michalik13, N.R.

Millar7, B.M.H.

Miranda54, D.

Molina10, R.

Molinaro84, M.

Molinaro114, L.

Molnár110, M.

Moniez115, P.

Montegriffo31, D.

Monteiro21, R.

Mor10, A.

Mora47, R.

Morbidelli27, T.

Morel43, S.

Morgenthaler116, T.

Morley86, D.

Morris41, A.F.

Mulone30, T.

Muraveva31, I.

Musella84, J.

Narbonne62, G.

Nelemans25, 24, L.

Nicastro117, L.

Noval62, C.

Ordénovic14, J.

Ordieres-Meré118, P.

Osborne7, C.

Pagani72, I.

Pagano52, F.

Pailler16, H.

Palacin62, L.

Palaversa8, P.

Parsons22, T.

Paulsen21, M.

Pecoraro63, R.

Pedrosa119, H.

Pentikäinen55, J.

Pereira21, B.

Pichon14, A.M.

Piersimoni83, F.-X.

Pineau45, E.

Plachy110, G.

Plum4, E.

Poujoulet120, A.

Prša121, L.

Pulone79, S.

Ragaini31, S.

Rago27, N.

Rambaux38, M.

Ramos-Lerate122, P.

Ranalli13, G.

Rauw43, A.

Read72, S.

Regibo24, F.

Renk15, C.

Reylé59, R.A.

Ribeiro92, L.

Rimoldini33, V.

Ripepi84, A.

Riva27, G.

Rixon7, M.

Roelens8, M.

Romero-Gómez10, N.

Rowell41, F.

Royer4, A.

Rudolph15, L.

Ruiz-Dern4, G.

Sadowski18, T.

Sagristà Sellés6, J.

Sahlmann12, J.

Salgado57, E.

Salguero57, M.

Sarasso27, H.

Savietto123, A.

Schnorhk21, M.

Schultheis14, E.

Sciacca52, M.

Segol124, J.C.

Segovia32, D.

Segransan8, E.

Serpell86, I-C.

Shih4, R.

Smareglia114, R.L.

Smart27, C.

Smith125, E.

Solano71, 126, F.

Solitro30, R.

Sordo3, S.

Soria Nieto10, J.

Souchay36, A.

Spagna27, F.

Spoto14, U.

Stampa6, I.A.

Steele108, H.

Steidelmüller11, C.A.

Stephenson22, H.

Stoev127, F.F.

Suess7, M.

Süveges33, J.

Surdej43, L.

Szabados110, E.

Szegedi-Elek110, D.

Tapiador128, 129, F.

Taris36, G.

Tauran62, M.B.

Taylor130, R.

Teixeira85, D.

Terrett34, B.

Tingley131, S.C.

Trager76, C.

Turon4, A.

Ulla132, E.

Utrilla47, G.

Valentini83, A. van Elteren2, E.

Van Hemelryck39, M. van Leeuwen7, M.

Varadi8, 110, A.

Vecchiato27, J.

Veljanoski76, T.

Via77, D.

Vicente96, S.

Vogt133, H.

Voss10, V.

Votruba95, S.

Voutsinas41, G.

Walmsley16, M.

Weiler10, K.

Weingrill89, D.

Werner15, T.

Wevers25, G.

Whitehead15, Ł.

Wyrzykowski7, 134, A.
elryck39, M. van Leeuwen7, M.

Varadi8, 110, A.

Vecchiato27, J.

Veljanoski76, T.

Via77, D.

Vicente96, S.

Vogt133, H.

Voss10, V.

Votruba95, S.

Voutsinas41, G.

Walmsley16, M.

Weiler10, K.

Weingrill89, D.

Werner15, T.

Wevers25, G.

Whitehead15, Ł.

Wyrzykowski7, 134, A.

Yoldas7, M. Žerjal100, S.

Zucker87, C.

Zurbach48, T.

Zwitter100, A.

Alecu7, M.

Allen1, C.

Allende Prieto26, 135, 136, A.

Amorim54, G.

Anglada-Escudé10, V.

Arsenijevic54, S.

Azaz1, P.

Balm22, M.

Beck33, H.-H.

Bernstein†6, L.

Bigot14, A.

Bijaoui14, C.

Blasco137, M.

Bonfigli83, G.

Bono79, S.

Boudreault26, 138, A.

Bressan139, S.

Brown7, P.-M.

Brunet16, P.

Bunclark†7, R.

Buonanno79, A.G.

Butkevich11, C.

Carret119, C.

Carrion60, L.

Chemin23, 140, F.

Chéreau4, L.

Corcione27, E.

Darmigny16, K.S. de Boer141, P. de Teodoro32, P.T. de Zeeuw2, 142, C.

Delle Luche4, 62, C.D.

Domingues143, P.

Dubath33, F.

Fodor16, B.

Frézouls16, A.

Fries10, D.

Fustes53, D.

Fyfe72, E.

Gallardo10, J.

Gallegos32, D.

Gardiol27, M.

Gebran10, 144, A.

Gomboc100, 145, A.

Gómez4, E.

Grux59, A.

Gueguen4, 146, A.

Heyrovsky41, J.

Hoar12, G.

Iannicola79, Y.

Isasi Parache10, A.-M.

Janotto16, E.

Joliet42, 147, A.

Jonckheere39, R.

Keil148, 149, D.-W.

Kim5, P.

Klagyivik110, J.

Klar89, J.

Knude28, O.

Kochukhov50, I.

Kolka150, J.

Kos100, 151, A.

Kutka95, 152, V.

Lainey38, D.

LeBouquin62, C.

Liu5, 153, D.

Loreggia27, V.V.

Makarov154, M.G.

Marseille62, C.

Martayan39, 155, O.

Martinez-Rubi10, B.

Massart14, 62, 17, F.

Meynadier4, 36, S.

Mignot4, U.

Munari3, A.-T.

Nguyen16, T.

Nordlander50, P.

Ocvirk89, 45, K.S.

O’Flaherty156, A.

Olias Sanz157, P.

Ortiz72, J.

Osorio68, D.

Oszkiewicz55, 158, A.

Ouzounis41, M.

Palmer10, P.

Park8, E.

Pasquato18, C.

Peltzer7, J.

Peralta10, F.

Péturaud4, T.

Pieniluoma55, E.

Pigozzi30, J.

Poels†43, G.

Prat159, T.

Prod’homme2, 21, F.

Raison160, 146, J.M.

Rebordao143, D.

Risquez2, B.

Rocca-Volmerange161, S.

Rosen26, 72, M.I.

Ruiz-Fuertes33, F.

Russo27, S.

Sembay72, I.

Serraller Vizcaino162, A.

Short1, A.

Siebert45, 89, H.

Silva92, D.

Sinachopoulos37, E.
Gaia is a cornerstone mission in the science programme of the European Space Agency (ESA). The spacecraft construction was approved in 2006, following a study in which the original interferometric concept was changed to a direct-imaging approach. Both the spacecraft and the payload were built by European industry. The involvement of the scientific community focusses on data processing for which the international Gaia Data Processing and Analysis Consortium (DPAC) was selected in 2007. Gaia was launched on 19 December 2013 and arrived at its operating point, the second Lagrange point of the Sun-Earth-Moon system, a few weeks later. The commissioning of the spacecraft and payload was completed on 19 July 2014. The nominal five-year mission started with four weeks of special, ecliptic-pole scanning and subsequently transferred into full-sky scanning mode. We recall the scientific goals of Gaia and give a description of the as-built spacecraft that is currently (mid-2016) being operated to achieve these goals. We pay special attention to the payload module, the performance of which is closely related to the scientific performance of the mission. We provide a summary of the commissioning activities and findings, followed by a description of the routine operational mode. We summarise scientific performance estimates on the basis of in-orbit operations. Several intermediate Gaia data releases are planned and the data can be retrieved from the Gaia Archive, which is available through the Gaia home page at http://www.cosmos.esa.int/gaia.
Key words. astrometry – parallaxes – proper motions – photometry – variable stars Article number, page 2 of 36
spelled as GAIA, for Global Astrometric Interferometer for Astrophysics, but the spelling was later changed because the final design was non-interferometric and based on monolithic mirrors and direct imaging and the final operating principle was actually closer to a large Rømer mission than the original GAIA proposal.

After the selection of Gaia in 2000 as an ESA-only mission, followed by further preparatory studies, the implementation phase started in 2006 with the selection of the prime contractor, EADS Astrium (later renamed Airbus Defence and Space), which was responsible for the development and implementation of the spacecraft and payload.

Meanwhile, the complex processing and analysis of the mission data was entrusted to the Data Processing and Analysis Consortium (DPAC), a pan-European, nationally funded collaboration of several hundred astronomers and software specialists.

Gaia was launched in December 2013 and the five-year nominal science operations phase started in the summer of 2014, after a half-year period of commissioning and performance verification.

Unlike the Hipparcos mission, the Gaia collaboration does not have data rights.

After processing, calibration, and validation inside DPAC, data are made available to the world without limitations; this also applies to the photometric and solar system object science alerts (Sect. 6.2).

Several intermediate releases, with roughly a yearly cadence, have been defined and this paper accompanies the first of these, referred to as Gaia Data Release 1 (Gaia DR1; Gaia Collaboration et al. 2016).

The data, accompanied by several query, visualisation, exploration, and collaboration tools, are available from the Gaia Archive (Salgado et al. 2016), which is reachable from the Gaia home page at http://www.cosmos.esa.int/gaia and directly at http://archives.esac.esa.int/gaia.

This paper is organised as follows: Section 2 summarises the science goals of the mission.

The spacecraft and payload designs and characteristics are described in Sect. 3.

The launch and commissioning phase are detailed in Sect. 4.

Section 5 describes the mission and mission operations.

The science operations are summarised in Sect. 6.

Section 7 outlines the structure and flow of data in DPAC.

The science performance of the mission is discussed in Sect. 8.

A summary can be found in Sect. 9.

All sections are largely stand-alone descriptions of certain mission aspects and can be read individually.

The use of acronyms in this paper has been minimised; a list can be found in Annex A.
optical bench, telescopes, instruments, and focal plane assembly (Sect. 3.3); (c) service module (structure): also housing some electronic payload equipment, e.g. clock distribution unit, video processing units, and payload data-handling unit (Sect. 3.2); (d) propellant systems (Sect. 3.2.1); (e) phased-array antenna (Sect. 3.2.2); and (f) deployable sunshield assembly, including solar arrays (Sect. 3.2). Credit: ESA, ATG Medialab.]

control, electrical power control and distribution, central data management, and communications with the Earth through low gain antennae and a high-gain phased-array antenna for science data transmission. In view of their relevance to the science performance of Gaia, the attitude and orbit control and phased-array antenna subsystems are described in more detail below.
3.3. Payload module The payload module (Fig. 3) is built around an optical bench that provides structural support for the two telescopes (Sect. 3.3.1) and the single integrated focal plane assembly (Sect. 3.3.2) that comprises, besides wave-front-sensing and basic angle metrology (Sects. 3.3.3 and 3.3.4), three science functions: astrometry (Sect. 3.3.5), photometry (Sect. 3.3.6), and spectroscopy (Sect. 3.3.7). The payload module is mounted on top of the service module via two (parallel) sets of three, V-shaped bipods. The first set of launch bipods is designed to withstand mechanical launch loads and these have been released in orbit to a parking position to free the second set of glass-fibre-
3.2.1. Attitude and orbit control The extreme centroiding needs of the payload make stringent demands on satellite attitude control over the integration time of the payload detectors (of order a few seconds). This requires in particular that rate errors and relative-pointing errors be kept at the milli-arcsecond per second and milli-arcsecond level, respectively. These requirements prohibit the use of moving parts, such as conventional reaction wheels, on the spacecraft, apart from moving parts within thrusters. The attitude- and orbit-control
Article number, page 7 of 36 information provided by the photometry collected for each object (Sect.

[Figure: Fig. 3. Schematic payload overview without protective tent. Most electronic boxes, e.g. clock distribution unit, video processing units, or payload data-handling unit, are physically located in the service module and hence not visible here. Credit: ESA.]
in combination with TDI operation, affect the detailed shape of the point spread function of all instruments in subtle yet significant ways through continuous trapping and de-trapping (Holl et al. 2012b; Prod’homme et al. 2012), removing charge from the leading edge and releasing it in the trailing edge of the images and spectra. The resulting systematic biases of the image centroids and the spectra will be calibrated in the on-ground data processing, for instance using a forward-modelling approach based on a charge-distortion model (CDM; Short et al. 2013).
Article number, page 9 of 36

16-bit analogue-to-digital converter (ADC). The PEMs allow for adjustment of the CCD operating points, which might become necessary at some point as a result of flat-band voltage shifts induced by ionising radiation (monitoring of which is described in Sect. 6.4). All CCD-PEM couples of a given row of CCDs are connected through a power- and command-distribution interconnection module to a video processing unit (VPU; Sect. 3.3.8), which is in charge of generating the CCD commanding and acquiring the science data. Operating the 100+ CCDs, comprising nearly a billion pixels, in TDI mode with a line period of ∼1 ms would generate a data rate that is orders of magnitude too high to be transmitted to ground. Three onboard reduction processes are hence applied:
1. Not all pixel data are read from the CCDs but only small areas, windows, around objects of interest; remaining pixel data are flushed at high speed in the serial register. This has an associated advantage of decreased read noise for the desired pixels; 2. The two-dimensional images (windows) are, except for bright stars, binned in the across-scan direction, nevertheless preserving the scientific information content (timing / along-scan centroid, total intensity / magnitude, and spectral information); 3. The resulting along-scan intensity profiles, such as linespread functions or spectra, are compressed on board without loss of information; the typical gain in data volume is a factor 2.0–2.5.

[Figure: Fig. 5. Schematic view of a Gaia CCD detector. Stars move from left to right in the along-scan direction (yellow arrow). Charges in the readout register are clocked from bottom to top. The first line of the CCD (left) contains the charge-injection structure (red). The last line of the CCD before the readout register (right) contains the summing well and transfer gate (blue). Dashed, grey lines indicate stitch-block boundaries. Solid, green vertical lines indicate TDI gates (the three longest lines are labelled at the top of the CCD). The inset shows some details of an individual pixel. See Sect. 3.3.2 for details.]
source of the contamination, suspected to be slowly releasing trapped air (water vapour) within multilayer insulation blankets and/or carbon fibre-reinforced polymer structural parts, is drying up.
4.2.2.

Straylight Soon after payload was switched on, it was discovered that straylight levels are modulated with the spacecraft rotation and some two orders of magnitude higher than expected.

The origin of the straylight has been traced back foremost to scattered sunlight and secondly to the integrated brightness (and extremely bright stars) of the Milky Way, the light of which can reach the focal plane through a few unbaffled straylight paths.

Although the telescope apertures are mostly shielded from direct illumination of the Sun by the double layer, deployable sunshield assembly, sunlight can scatter into the apertures through outward-protruding (bundles of) Nomex fibres; these fibres are present at the edges of the foldable sunshield blankets, which do not have a kapton tape finishing, and are present between each pair of fixed sunshield frames.

Although the increased background levels themselves can be dealt with in the data processing, the associated noise negatively impacts the performance of faint objects, in particular in the spectroscopic instrument, which operates at very low signal levels.

Therefore, a partial mitigation was implemented in the RVS windowing strategy allowing one to adaptively adjust the across-scan size of the windows to the instantaneous straylight level to increase the signal-to-noise ratio of the spectra.

In addition, the RVS object selection was modified to adapt the faint limit to the instantaneous background level, which does not directly mitigate the straylight, but optimises the overall science quality of the RVS data acquired on board and downlinked to ground.

Article number, page 15 of 36
et al. (2016). The curves are Chebyshev polynomials of the actual calibrations. Red lines refer to the preceding field of view; blue lines to the following field of view. The discontinuities and dotted vertical lines refer to the decontaminations (Sect. 6.4). OBMT stands for onboard mission timeline in units of six-hour revolutions since launch (Sect. 5.3.3). Gaia Data Release 1 is based on data covering the interval OBMT = 1078.3795–2751.3518, delimited by the dashed black lines.]

6.1. Interface to the Mission Operations Centre The SOC is the prime interface to the MOC for all payload- and science-related matters. Normal work includes
– generating the scanning law (Sect. 5.2), including the associated calibration of the representation of the azimuth of the Sun in the scanning reference system in the VPU software;
– generating the science schedule, i.e. the predicted onboard data rate according to the operational scanning law and a sky model, to allow for adaptive ground-station scheduling (Sect. 5.3.1);
– generating the avoidance file containing time periods when interruptions to science collection would prove particularly detrimental to the final mission products;
– generating payload operation requests (PORs; Mora et al. 2014a), i.e. VPU-parameter updates (e.g. TDI-gating scheme or CCD-defect updates);
– tracking the status and history of payload configuration parameters in the configuration database (CDB) through the mission timeline and telecommand history;
– hosting the science-telemetry archive;
– generating event anomaly reports (EARs) to inform downstream processing systems of bad time intervals, outages in the science data, or any (onboard) events that may have an impact on the data processing and/or calibration;
– monitoring (and recalibrating as needed) the star-packetcompression performance;
– monitoring (and recalibrating as needed) the BAM laser beam waist location inside the windows;
– reformatting the optical observations of Gaia received from GBOT for MOC processing in the orbit reconstruction (Sect. 5.3.2);
– disseminating to DPAC (Sect. 7) meteorological groundstation data received from MOC and required for delay corrections in the high-accuracy time synchronisation (Sect. 5.3.3).
To avoid ambiguity in case of clock resets, OBT counts are first transformed in the initial processing of the data (Fabricius et al. 2016) into the OBMT (onboard mission timeline) by adding a constant offset. The OBMT is conventionally expressed in units of six-hour (21,600 s) spacecraft revolutions since launch. For instance for the purpose of interpreting the timeline of figures (e.g. Fig. 8), OBMT can be converted into TCB at Gaia (expressed in Julian years) by the approximate relation, TCB ≈J2015.0 + (OBMT −1717.6256 rev)/(1461 rev). (3) This relation is valid only for the interval OBMT = 1078.3795– 2751.3518, which covers Gaia Data Release 1.