DOCSLIB.ORG

Gaia: Astrometric Survey of the Galaxy

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Gaia: Astrometric Survey of the Galaxy Çağrılı Bildiriler / Invited Papers Galaktik Astronomi Çalıştayı Bildiriler Kitabı Galactic Astronomy Workshop Proceedings Book DOI: 10.26650/PB/PS01.2021.001.002 Gaia: Astrometric Survey of the Galaxy Gerry GILMORE1 1Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, United Kingdom ORCID: G.G. 0000-0003-4632-0213 ABSTRACT Gaia provides 5-D phase space measurements, 3 spatial coordinates and two space motions in the plane of the sky, for a representative sample of the Milky Way’s stellar populations (over 2 billion stars, being ~1% of the stars over 50% of the radius). Full 6-D phase space data is delivered from line-of-sight (radial) velocities for the 300 million brightest stars. These data make substantial contributions to astrophysics and fundamental physics on scales from the Solar System to cosmology. 1. Introduction The ESA Gaia astrometric space mission is revolutionising astrophysics. Originally proposed in the early 1990’s to build on the proof of concept for absolute space astrometry demonstrated by the ESA HIPPARCOS mission, Gaia is currently operating superbly. The first two data releases have provided support for over 1000 research articles already, even though only a small subset of some types of the data being obtained have yet been calibrated, reduced and released. A convenient overview of the whole Gaia mission and its capabilities is available in Gilmore (2018a), while very substantially more detailed descriptions are available in the many Gaia Data Release papers, and on the ESA Gaia website. Gaia has in essence three scientific instruments, all based on a very large high-quality imaging billion-pixel camera. These instruments provide direct broad-band imaging, in the Gaia native (G-band) passband, which is analysed for photometry and astrometry, low-dispersion prism spectrophotometry in both blue (BP) and red (RP) wavelengths, together covering 300 nm to 1000 nm, and R = 12000 spectroscopy near the CaII triplet for radial velocities and spectroscopic analyses for brighter stars. The instruments and their observations are summarised in Figure 1. Submitted/Başvuru: 27.09.2019 Accepted/Kabul: 31.01.2020 Corresponding author/Sorumlu yazar: Gerry Gilmore (Prof. Dr.), Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, United Kingdom. E-mail: [email protected] Citation/Atıf: Gilmore, G. 2021, in: Gaia: Astrometric Survey of the Galaxy, eds. S. Ak & S. Bilir, Galactic Astronomy Workshop Proceedings Book, 15. https://doi.org/10.26650/PB/PS01.2021.001.002 15 Galaktik Astronomi Çalıştayı Bildiriler Kitabı 12-13 Eylül 2019 Galactic Astronomy Workshop Proceedings Book September 12-13, 2019 2. Gaia: The Early Years The Gaia mission was proposed in early 1993, building on the technical success of the ESA HIPPARCOS mission, then in operation, which proved that absolute space astrometry was viable. The original Gaia proposal was in response to a CaII for interfometry missions. During the detailed Study Phase, which ran until 2000, it was soon realised that an interferometer was not the optimal solution. Rather a design loosely based on the parallel ROEMER proposal was adopted. This study led to development of the Gaia “RED BOOK” proposal to ESA. This proposal is still available via the ESA Gaia web portal1. The study led to a presentation of the Gaia mission for ESA adoption at a (very large) meeting held at UNESCO HQ, Paris, on September 13, 2000, and a summary article outlining the mission (Perryman et al., 2001). The various stages of design optimisation, construction and test led eventually to successful launch of Gaia in December 2013, and the start of science operations in mid 2014. At present (September 2019) Gaia has completed its “nominal” 5-year mission, the spacecraft is operating very well, and the mission is anticipated to continue data taking until the precision-control fuel is exhausted at the end of 2024. Over 1.3 trillion observations have been recorded at the mission mid-life point. The various key documents which led to the Gaia mission are illustrated in Figure 2, while a more detailed description is available in Gilmore (2018b). Figure 1. An illustration of Gaia’s sky-scanning law (top left) and three forms of data gathering. The top centre row shows an image of the very large (1m × 0.6m, billion-pixel) Gaia focal-plane camera, with its three types of detectors, while the top-right shows an image, from which photometry and astrometry are derived (inset psf). The middle row shows the radial velocity spectrometer and a bright-star spectrum. The lower row shows the two low-dispersion (BP/RP) prisms, and time-series spectrophotometry from the prisms for a carbon star. This figure is taken from the mission overview presented by the DPACE Chair, Anthony Brown, at the ESA ESLAB#53 meeting in April 2019 3. Gaia and the Structure of the Milky Way Figure 3 illustrates the basic stellar populations, which were known prior to Gaia launch, and whose detailed mapping and origins were the goal of the Gaia mission. Enormous progress has been made already from Gaia’s early astrometric and photometric data in quantifying the 1 https://www.cosmos.esa.int/web/gaia/home 16 Galaktik Astronomi Çalıştayı Bildiriler Kitabı 12-13 Eylül 2019 Galactic Astronomy Workshop Proceedings Book September 12-13, 2019 Galaxy. Gaia’s photometry is calibrated at the milli-mag level, substantially superior to previous large-area (percent-accuracy) surveys. An interesting early conclusion from Gaia is that the earlier photometric studies, to which the Basle-Istanbul teams were major contributors, were in fact even more accurate than could reasonably have been expected. The most recent ground-based star-count Galactic structure analysis based on wide-area high-quality CCD data is that from the Dark Energy Survey (Pieres et al., 2020). This derives large-scale population parameters in good agreement with those derived from early photographic surveys. As a Gaia-test, we show in Figure 4 the results from Gaia photometry for the density profiles towards both the Galactic poles for G-stars. This is essentially reproducing the experiment of Gilmore & Reid (1983) which discovered the Galactic Thick Disk. Figure 2. The key documents which trace the Gaia mission from genesis to approval. Further details are available in Perryman et al. (2001) and in Gilmore (2018b). 17 Galaktik Astronomi Çalıştayı Bildiriler Kitabı 12-13 Eylül 2019 Galactic Astronomy Workshop Proceedings Book September 12-13, 2019 Figure 3. The high-latitude stellar populations. The figure shows a high-latitude stellar field with both optical (r, g-r: LHS) and near-infrared (K, H-K, RHS) colour-magnitude diagrams for the same stars. The optical data show the clear distinction between the (red-sequence) foreground thin-disk, the thick disk turnoff sequence (near g-r = 0.5) and the halo turnoff sequence (near g-r = 0.4). These distinctions are less evident in the near-infrared. Figure 4. The stellar density profile towards both Galactic poles for G-stars. The various curves are as described in the figure. The resulting Bayesian reconstruction of the density profile illustrates the impressive consistency between early photographic studies and more recent CCD-based surveys. A consequence is that the local density of Dark Matter remains fully consistent with the first precision determination, which was in 1989. Not everything from Gaia is different! This figure is from Sanders & Gilmore (in prep). 18 Galaktik Astronomi Çalıştayı Bildiriler Kitabı 12-13 Eylül 2019 Galactic Astronomy Workshop Proceedings Book September 12-13, 2019 4. Gaia and the Evolution of the Milky Way A primary ambition for Gaia was to determine the assembly history of the Milky Way. Remarkable progress has been made in this endeavour, through a combination of kinematic studies of the halo, to decipher the early merging history, and spectroscopy and stellar age determination to add a clock. Studies of halo kinematics have shown, in several parallel and independently authored studies which agree remarkably closely, that a major merger took place between the proto-Milky Way galaxy and an infalling satellite, of Large Magellanic Cloud scale, early in the Galaxy’s history. The stars from the infalling galaxy now make up much of the inner halo. The Milky Way parent, which at the time was already a disk-like galaxy, was puffed up in the merger, with the primordial disk being transformed into what we now see as the thick disk. Later gas accretion created a new thin disk, which continues to form stars today. This picture was not new, but is in excellent agreement with what had been deduced from earlier studies of small samples of stars with accurate abundances and approximate kinematics. Thus we see directly, in phase-space structure, the history of the Milky Way. An early disk- like proto-galaxy was forming stars and enriching, creating material enriched preferentially in “alpha” elements, products of Type II supernovae. These are primarily Mg, Si, Ti, Ca, and O. Over time more Type Ia supernovae had time to explode, creating more iron-peak elements, and diluting the alpha-rich material. The merger which re-structured the galaxy also bought in much new low-metallicity gas. Thus, the level of chemical enrichment of the disk gas was substantially reduced at the time of the merger. Can we see this event in the chemistry? To do so we need both chemical element abundances for large samples of stars, and stellar ages. Until recently providing the ages was the limiting factor. There has been much recent progress here. With Gaia parallaxes reasonably accurate ages can be determined for stars at the main-sequence turnoff or lower Red Giant Branch (RGB) from isochrone fitting. More generally, and allowing age determinations to very much larger distances, a new stellar age clock was derived which is based purely on RGB chemistry.
Load more

Recommended publications
  • Astrophysical Applications of Gravitational Microlensing in the Milky
    ASTROPHYSICAL APPLICATIONS OF GRAVITATIONAL MICROLENSING IN THE MILKY WAY Przemysław Mróz Ph.D. thesis written under the supervision of prof. dr hab. Andrzej Udalski Warsaw University Observatory Warsaw, April 2019 Acknowledgements First and foremost, I would like to thank my supervisor, Prof. Andrzej Udalski, for the encouragement and advice he has provided throughout my time as his student. I have been extraordinarily lucky to have the supervisor who gave me immeasurable amount of his time, as a researcher and a mentor. This dissertation would not be possible without the sheer amount of work from all members of the OGLE team and their time spent at Cerro Las Campanas. In particular, I would like to thank Prof. Michał Szymanski,´ Prof. Igor Soszynski,´ Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radek Poleski, and Jan Skowron, who have helped me since my very first steps at the Warsaw University Observatory. I thank all my collegues from the Warsaw Observatory for many helpful discussions and support. I am also grateful to Andrew Gould, Takahiro Sumi, and Yossi Shvartzvald, who shared the photometric data that are a part of this thesis. I thank Calen Henderson and all Pasadena-based microlensers for their hospitality during my stay at Caltech. I also thank my family for their support in my effort to pursue my chosen field of astronomy. I acknowledge financial support from the Polish Ministry of Science and Higher Education (“Diamond Grant” number DI2013/014743), the Foundation for Polish Science (Program START), and the National Science Center, Poland (grant ETIUDA 2018/28/T/ST9/00096). I also received support from the European Research Council grant No.
    [Show full text]
  • Full Orbital Solution for the Binary System in the Northern Galactic Disc Microlensing Event Gaia16aye
    This is a repository copy of Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/162837/ Version: Accepted Version Article: Wyrzykowski, Ł, Mróz, P, Rybicki, KA et al. (182 more authors) (2020) Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye. Astronomy & Astrophysics, 633 (January 2020). A98. ISSN 0004-6361 https://doi.org/10.1051/0004-6361/201935097 © 2019 ESO. Reproduced in accordance with the publisher's self-archiving policy. Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as permitted by national copyright laws. The publisher or other rights holders may allow further reproduction and re-use of the full text version. This is indicated by the licence information on the White Rose Research Online record for the item. Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request. [email protected] https://eprints.whiterose.ac.uk/ Astronomy & Astrophysics manuscript no. pap16aye c ESO 2019 October 30, 2019 Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye⋆ Łukasz Wyrzykowski1,⋆⋆, P. Mróz1, K. A. Rybicki1, M. Gromadzki1, Z. Kołaczkowski45, 79,⋆⋆⋆, M. Zielinski´ 1, P. Zielinski´ 1, N.
    [Show full text]
  • Arxiv:1802.03258V1 [Astro-Ph.SR] 9 Feb 2018 Every Example Mentioned Above (Besides the Rare Case for Example Double-Lined Eclipsing Binaries (See Torres Et Al
    MNRAS 000,1{17 (2017) Preprint 12 July 2021 Compiled using MNRAS LATEX style file v3.0 On the accuracy of mass measurement for microlensing black holes as seen by Gaia and OGLE Krzysztof A. Rybicki,1? Lukasz Wyrzykowski,1 Jakub Klencki,1;2 Jos de Bruijne,3 Krzysztof Belczy´nski,4 Martyna Chru´sli´nska1;2 1Warsaw University Astronomical Observatory, Aleje Ujazdowskie 4, 00-478 Warsaw, Poland 2Department of Astrophysics/IMAPP, Radboud University, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands 3Scientific Support Office, Directorate of Science, European Space Research and Technology Centre (ESA/ESTEC), Keplerlaan 1, 2201AZ, Noordwijk, The Netherlands 4Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, ul. Bartycka 18, PL-00-716 Warsaw, Poland Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We investigate the impact of combining Gaia astrometry from space with precise, high cadence OGLE photometry from the ground. For the archival event OGLE3-ULENS- PAR-02, which is likely a black hole, we simulate a realistic astrometric time-series of Gaia measurements and combine it with the real photometric data collected by the OGLE project. We predict that at the end of the nominal 5 years of the Gaia mission, for the events brighter than G ≈ 15:5 mag at the baseline, caused by objects heavier than 10 M , it will be possible to unambiguously derive masses of the lenses, with accuracy between a few to 15 per cent. We find that fainter events (G < 17:5) can still have their lens masses determined, provided that they are heavier than 30 M .
    [Show full text]
  • Microlensing 22 Auckland, New Zealand 25–28 January 2018
    Microlensing 22 Auckland, New Zealand 25{28 January 2018 Welcome Address and Introduction Welcome to Microlensing 22! On behalf of the Scientific Organising Committee, thank you for participating in this year's conference. If you have any questions or problems, please do not hesitate to come and chat with either me or Amy Edwards, our conference manager, and we will do our best to help. I hope you will enjoy your time in Auckland and perhaps take the opportunity to travel further afield around this beautiful country. If you have any tourism questions, a travel advisor will be available for you to consult while the conference registration desk is open. The Department of Physics at The University of Auckland is committed to provid- ing a harassment-free environment. This conference has adopted the London Code of Conduct and all participants are required to abide by this Code. If you have any questions about the Code of Conduct, please contact Nicholas Rattenbury. The Code itself is given below. Included next is the complete programme for the conference. As ever, there may be last minute changes to the programme line-up and we will endeavour to make you aware of any changes well in advance. Nicholas Rattenbury, for the SOC: Rachel Akeson (Caltech/IPAC) Valerio Bozza (University of Salerno) Scott Gaudi (The Ohio State University) Calen Henderson (Caltech//IPAC-NExScI) Jessica Lu (University of California Berkeley) David Nataf (Johns Hopkins University) Nick Rattenbury (University of Auckland) Rachel Street (Las Cumbres Observatory) Takahiro Sumi (Osaka University) Andrzej Udalski (Warsaw University) 1 London Code of Conduct The organisers are committed to making this meeting productive and enjoyable for everyone, regardless of gender, sexual orientation, disability, physical appearance, body size, race, nationality or religion.
    [Show full text]
  • Abstract Book
    ABSTRACT BOOK 8th Gaia Science Alerts Workshop 6-8 December 2017 Warsaw University Astronomical Observatory, Poland The titles are sorted following the agenda of the workshop. Workshop’s agenda on-line: https://www.ast.cam.ac.uk/ioa/wikis/gsawgwiki/index.php/Workshop2017:agenda Gaia overview and reports Simon Hodgkin Institute of Astronomy, University of Cambridge, UK I’ll give a summary of the current status of the Gaia Alerts system. PLATO Science Flux Alerts Steve Boudreault Max Planck Institute for Solar System Research The ESA mission PLAnetary Transits and Oscillations of stars (PLATO) is aiming at obtaining light curves of a few hundred thousand stars for detection of planetary transits and the characterization of the host star with asteroseismology. It is likely that, during PLATO’s lifetime, interesting events other than planetary transits or stellar oscillation will be detected, including supernovae, gamma-ray-burst, gravitational microlensing, stellar superflares, and other unexpected and unclassified transient events. The goal of the Science Flux Alerts is to detect and give an alert about a possible detection of one of these rare events, to trigger additional follow-up observations, considering their brevity and non-repeatability, while they are in progress. First results of spectroscopic and photometric survey of the northern sky at Moletai AO for the PLATO 2.0 input catalog Erika Pakstiene Institute of Theoretical Physics and Astronomy, Vilnius University Current photometric catalogs and spectroscopic surveys are still not able to provide all the necessary variability and spectroscopic information that is required for a development of the European Space Agency PLATO space mission input catalogue.
    [Show full text]
  • OGLE-2014-BLG-0289 Precise Characterization of a Quintuple
    LJMU Research Online Udalski, A, Han, C, Bozza, V, Gould, A, Bond, IA, Mroz, P, Skowron, J, Wyrzykowski, L, Szymanski, MK, Soszynski, I, Ulaczyk, K, Poleski, R, Pietrukowicz, P, Kozlowski, S, Abe, F, Barry, R, Bennett, DP, Bhattacharya, A, Donachie, M, Evans, P, Fukui, A, Hirao, Y, Itow, Y, Kawasaki, K, Koshimoto, N, Li, MCA, Ling, CH, Masuda, K, Matsubara, Y, Miyazaki, S, Munakata, H, Muraki, Y, Nagakane, M, Ohnishi, K, Ranc, C, Rattenbury, N, Saito, T, Sharan, A, Sullivan, DJ, Sumi, T, Suzuki, D, Tristram, PJ, Yamada, T, Yonehara, A, Bachelet, E, Bramich, DM, DAgo, G, Dominik, M, Jaimes, RF, Horne, K, Hundertmark, M, Kains, N, Menzies, J, Schmidt, R, Snodgrass, C, Steele, IA, Wambsganss, J, Pogge, RW, Jung, YK, Shin, I-G, Yee, JC, Kim, W-T, Beichman, C, Carey, S, Novati, SC and Zhu, W OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-peak Gravitational Microlensing Event http://researchonline.ljmu.ac.uk/id/eprint/8362/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Udalski, A, Han, C, Bozza, V, Gould, A, Bond, IA, Mroz, P, Skowron, J, Wyrzykowski, L, Szymanski, MK, Soszynski, I, Ulaczyk, K, Poleski, R, Pietrukowicz, P, Kozlowski, S, Abe, F, Barry, R, Bennett, DP, Bhattacharya, A, Donachie, M, Evans, P, Fukui, A, Hirao, Y, Itow, Y, Kawasaki, K, Koshimoto, LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners.
    [Show full text]
  • RVO 2019 Report.Pdf
    RVO progress report (Oct 2019) I. General Catalogue of Variable Stars (GCVS) group (INASAN and SAIMSU, led by Nikolai Samus) In 2019, it was announced that the Information Bulletin of Variable Stars (IBVS; Konkoly Observatory, Hungary) will be published no longer. By that time, the first part of our 82nd Name- list of Variable Stars was submitted to the IBVS. It contained, besides objects traditional for Name-lists, also variable stars in ten globular clusters of our Galaxy. In this situation, we are forced to continue our work on Name-lists of variable stars using facilities provided by the electronic journal Peremennye Zvezdy/Variable Stars. Since the IBVS had the advantage of the coverage by SCOPUS, we took effort to ensure that our journal is also covered by SCOPUS. Our effort succeeded, and now the main journal Peremennye Zvezdy/Variable Stars has SCOPUS coverage. However, SCOPUS did not provide coverage to our Supplement Series. The reason for that, formulated by SCOPUS, is that the Supplement Series, unlike the main journal, does not provide pdf files. The technical editor of Peremennye Zvezdy/Variable Stars has now solved the technical problems, and pdf files have been created for all the issues of the Supplement Series published electronically. We are planning to re-apply for SCOPUS coverage of the Supplement Series. The second and third parts of the 82nd Name-list will be published in Peremennye Zvezdy/Variable Stars main journal later this year. The large amount of research performed by our team in 2016–2019 and covered in the References makes it difficult to reflect every detail in the current brief report.
    [Show full text]
  • Na'ama Hallakoun
    NA’AMAHALLAKOUN July 2021 Address Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot, 7610001, Israel Phone +972-8-9346505 E-mail [email protected] Website http://www.weizmann.ac.il/˜naamaha GitHub profile https://github.com/naamach positions 2019– Benoziyo Prize Fellow Weizmann Institute of Science, Israel Astrophysics Postdoctoral Fellowship Benoziyo Center for Astrophysics education 2014–2019 Ph.D. in Astrophysics Tel-Aviv University, Israel Advisor: Prof. Dan Maoz School of Physics and Astronomy Thesis: Companions and Debris Around White Dwarfs 2011–2013 M.Sc. in Physics Tel-Aviv University, Israel Advisor: Prof. Lev Vaidman School of Physics and Astronomy Thesis: Subjective Randomness in Quantum Mechanics magna cum laude 2008–2011 B.Sc. in Physics Tel-Aviv University, Israel School of Physics and Astronomy 2002–2009 B.A. in History The Open University, Israel magna cum laude scholarships, awards and honors 2019–2022 Benoziyo Prize Postdoctoral Fellowship, Benoziyo Center for Astro- physics, Weizmann Institute of Science 2018 Certificate of Merit for Exceptional Contribution to the Tel-Aviv University Astronomy Club, School of Physics and Astronomy, Tel-Aviv University 2018 The John Bahcall Astrophysics Graduate Student Prize for Excel- lence in Research, School of Physics and Astronomy, Tel-Aviv University 2017 The Anne and Maurice Cohen Excellence in Research Award, School of Physics and Astronomy, Tel-Aviv University 1 of 8 2017 The Dan David Scholarship, Awarded by the Dan David Foundation and the Prize Laureates 2016 The Getty Excellence in Research Award, School of Physics and Astron- omy, Tel-Aviv University 2015–2017 ESO Studentship, European Southern Observatory, Germany ESO Advisor: Dr.
    [Show full text]
  • Full Orbital Solution for the Binary System in the Northern Galactic Disc Microlensing Event Gaia16aye?
    A&A 633, A98 (2020) Astronomy https://doi.org/10.1051/0004-6361/201935097 & c ESO 2020 Astrophysics Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye? Ł. Wyrzykowski1, P. Mróz1, K. A. Rybicki1, M. Gromadzki1, Z. Kołaczkowski44,78, y, M. Zielinski´ 1, P. Zielinski´ 1, N. Britavskiy4,5 , A. Gomboc34, K. Sokolovsky18,3,65 , S. T. Hodgkin6, L. Abe88, G. F. Aldi19,79 , A. AlMannaei61,99 , G. Altavilla71,7 , A. Al Qasim61,99 , G. C. Anupama8, S. Awiphan9, E. Bachelet62, V. Bakı¸s10, S. Baker99, S. Bartlett49, P. Bendjoya11, K. Benson99, I. F. Bikmaev75,86 , G. Birenbaum12, N. Blagorodnova23, S. Blanco-Cuaresma14,73 , S. Boeva15, A. Z. Bonanos18, V. Bozza19,79 , D. M. Bramich61, I. Bruni24, R. A. Burenin83,84 , U. Burgaz20, T. Butterley21, H. E. Caines33, D. B. Caton92, S. Calchi Novati82, J. M. Carrasco22, A. Cassan28, V. Cepasˇ 55, M. Cropper99, M. Chrusli´ nska´ 1,23 , G. Clementini24, A. Clerici34, D. Conti90, M. Conti47, S. Cross62, F. Cusano24, G. Damljanovic25, A. Dapergolas18, G. D’Ago80, J. H. J. de Bruijne26, M. Dennefeld28, V. S. Dhillon29,4 , M. Dominik30, J. Dziedzic1, O. Erece31, M. V. Eselevich85, H. Esenoglu32, L. Eyer73, R. Figuera Jaimes30,52 , S. J. Fossey33, A. I. Galeev75,86 , S. A. Grebenev83, A. C. Gupta98, A. G. Gutaev75, N. Hallakoun12, A. Hamanowicz1,35 , C. Han2, B. Handzlik36, J. B. Haislip93, L. Hanlon101, L. K. Hardy29, D. L. Harrison6,87 , H. J. van Heerden102, V. L. Hoette94, K. Horne30, R. Hudec38,75,39 , M. Hundertmark40, N. Ihanec34, E. N. Irtuganov75,86 , R.
    [Show full text]
  • GAIA Composition, Formation and Evolution of Our Galaxy
    2.5 Gerry Gilmore 1 The IoA Gaia team + Edinburgh, Leicester, MSSL, RAL, Italy, Spain Gaia Science case proposed vs today 3 GAIA Accuracies and our Galaxy 10 µas = 10% distances at 10 kpc 10 µas/yr = 1 km/sec at 20 kpc Sanna etal 2017 Science in press Gaia The goddess who came into being after Chaos and generated the starry sky (Hesiod, Theogony 116/117 and 126/127) a contrast to the unintelligible and generator of the explorable Gaia is transformational – the first 3-D galaxy precision distances and motions for 1 billion stars • Astrometry, photometry, spectroscopy, spectrophotometry, Teff, log g, Av, [Fe/H], binarity, planets, periods for variables,… Launch 12/2013 The heart of Gaia is a large Work started ~1993 camera array, 1 giga-pixel, Project approved 2000 sending us a video of the Operations start 7/2014 sky for 5-9 years. 5-9.5 years data Project end 2026+ The imaging data is being Total cost 960M€ processed in Cambridge. Gaia data processing develops “Big Data” technologies and training Absolute astrometry One field gives only relative measures model dependency Two fields break the degeneracy allows absolute measurements. Combining data at the limits of accuracy is not trivial! Single field astrometry Two field astrometry8 Photometric processing at DPCI Cambridge Flux calibration Evans etal 1701.05873 05/06/2014 9 astrometric data reduction • 1013 individual position measurements • 1010 unknowns – based on physical models • all connected: must be determined simultaneously • a vast modelling and parameter adjustment problem
    [Show full text]
  • Jessica Ryan Lu
    Jessica Ryan Lu Contact Astronomy Department Voice: (310)-709-0471 Information University of California, Berkeley Email: [email protected] 501 Campbell Hall #3411 http://astro.berkeley.edu/faculty-profile/jessica-lu Berkeley, CA 94720-3411 Position Associate Professor, University of California, Berkeley 2020 - current Research Black holes, star and cluster formation, initial mass function, galactic centers, stellar dynam- Interests ics, adaptive optics, astrometry, microlensing. Education University of California, Los Angeles, Ph.D., Astrophysics 2008 University of California, Los Angeles, M.S., Astrophysics 2005 Massachusetts Institute of Technology, S.B., Physics 2000 Past Research Assistant Professor, University of California, Berkeley 2016 - 2020 Appointments Assistant Astronomer Institute for Astronomy, University of Hawaii 2013 - 2016 NSF Astronomy and Astrophysics Postdoctoral Fellow, IfA Hawaii 2011 - 2013 Millikan Postdoctoral Fellow in Obs. Astronomy, Caltech 2008 - 2011 NSF Graduate Research Fellow, UCLA 2005 - 2008 Graduate Researcher, UCLA 2003 - 2005 Undergraduate Researcher, MIT 1997 - 2000 Research Project Scientist, UH/TNO Adaptive Secondary Mirror Prototype 2019 - present Activities Project Scientist, KAPA (Keck All-sky Precision Adaptive-optics) project 2018 - present Project Scientist, 'imaka Ground Layer Adaptive Optics Demonstrator 2013 - present Senior Member, Galactic Center Group @ UCLA 2003 - present Project Lead, UCLA Off-Axis PSF Reconstruction (AIROPA) 2014 - present co-PI, Keck Ground Layer Adaptive Optics
    [Show full text]
  • Full Orbital Solution for the Binary System in the Northern Galactic Disc Microlensing Event Gaia16aye? Łukasz Wyrzykowski1,??, P
    Astronomy & Astrophysics manuscript no. pap16aye c ESO 2019 October 30, 2019 Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye? Łukasz Wyrzykowski1,??, P. Mróz1, K. A. Rybicki1, M. Gromadzki1, Z. Kołaczkowski45, 79,???, M. Zielinski´ 1, P. Zielinski´ 1, N. Britavskiy4, 5, A. Gomboc35, K. Sokolovsky19, 3, 66, S.T. Hodgkin6, L. Abe89, G.F. Aldi20, 80, A. AlMannaei62, 100, G. Altavilla72, 7, A. Al Qasim62, 100, G.C. Anupama8, S. Awiphan9, E. Bachelet63, V. Bakı¸s10, S. Baker100, S. Bartlett50, P. Bendjoya11, K. Benson100, I.F. Bikmaev76, 87, G. Birenbaum12, N. Blagorodnova24, S. Blanco-Cuaresma15, 74, S. Boeva16, A.Z. Bonanos19, V. Bozza20, 80, D.M. Bramich62, I. Bruni25, R.A. Burenin84, 85, U. Burgaz21, T. Butterley22, H. E. Caines34, D. B. Caton93, S. Calchi Novati83, J.M. Carrasco23, A. Cassan29, V. Cepasˇ 56, M. Cropper100, M. Chrusli´ nska´ 1, 24, G. Clementini25, A. Clerici35, D. Conti91, M. Conti48, S. Cross63, F. Cusano25, G. Damljanovic26, A. Dapergolas19, G. D’Ago81, J. H. J. de Bruijne27, M. Dennefeld29, V. S. Dhillon30, 4, M. Dominik31, J. Dziedzic1, O. Erece32, M. V. Eselevich86, H. Esenoglu33, L. Eyer74, R. Figuera Jaimes31, 53, S. J. Fossey34, A. I. Galeev76, 87, S. A. Grebenev84, A. C. Gupta99, A. G. Gutaev76, N. Hallakoun12, A. Hamanowicz1, 36, C. Han2, B. Handzlik37, J. B. Haislip94, L. Hanlon102, L. K. Hardy30, D. L. Harrison6, 88, H.J. van Heerden103, V. L. Hoette95, K. Horne31, R. Hudec39, 76, 40, M. Hundertmark41, N. Ihanec35, E. N. Irtuganov76, 87, R. Itoh43, P. Iwanek1, M.D.Jovanovic26, R.
    [Show full text]