Status, Astrometric Solution and Gaia Data Releases€¦ · Object classification, BP/RP spectra +...
Transcript of Status, Astrometric Solution and Gaia Data Releases€¦ · Object classification, BP/RP spectra +...
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Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 1
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Gaia Status, Astrometric Solution and
Data Releases
Stefan Jordan
Astronomisches Rechen-Institut am Zentrum für Astronomie der Universität Heidelberg
http://www.stefan-jordan.de
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Gaia‘s Main Goals
• Positions, proper motions and parallaxes for 1 billion stars • All stars down to 20th (current limit actually 20.7) magnitude • 20-25 microarcsecond accuracy at 15th magnitude • Precise photometry (magnitudes and low-resolution spectra) for 1 billion stars • High-resolution NIR IR spectra for 50-100 million stars (G<16.2)
accuracy x 50
# of stars x 10000
HIPPARCOS ´Gaia
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Gaia�s schedule
• 1993: First proposal to ESA • 2000: accepted as „Cornerstone Mission� • 2006: Begin of the industrial phase • 2007: Preliminary Design Review • Several Reviews and hardware tests • Launch: December 19, 2013 • End of commissioning: July 18, 2014 • 2019: End of nominal measurements (5 years) • 2022/23: Publication of final catalogue? • Intermediate catalogues will come: first one in late
summer 2016
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15 million km: 25 microarcsecond
Parallaxes are small
380000 km: 1 milliarcsecond
1.75m HIPPARCOS
Gaia
σπ/π = 0.1% d = 40 pc σπ = 25µas σπ/π = 1 % d = 400 pc at V = 15 σπ/π = 10% d = 4 kpc
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5 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 5
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Gaia instruments
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Gaia‘s One-giga-pixel Camera
4500x2000 Pixel
106 CCD detektors
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The launch
• Soyuz-Fregat • 47 m high • Sinnamary in French Guyana • Launch date: 19. Dezember 2013
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Flight to L2
Animation: Toni Sagristà Sellés (ARI/ZAH University
of Heidelberg)
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Ground stations (Routine Phase)
Cebreros New Norcia
Australia Spain
Communication to ground
Telemetry: 3-8 Megabit per second
Malargüe
Argentina
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Scanning, Focal plane
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11 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 11
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Star motion in 10 s Astrometric Field
CCDs
Blue Photom
eter CC
Ds
Sky Mapper CCDs
104.26cm
Red Photom
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Ds
Radial-Velocity Spectrometer
CCDs
Basic Angle
Monitor
Wave Front Sensor
Basic Angle
Monitor
Wave Front Sensor
42.3
5cm
Figure courtesy Alex Short
Gaia�s focal plane
0.7 * 1.5 deg Total field:
- active area: 0.75 deg2
- CCDs: 14 + 62 + 14 + 12 - 4500 x 1966 pixels (TDI)
- pixel size = 10 µm x 30 µm = 59 mas x 177 mas
Sky mapper: - detects all objects to 20 mag
- rejects cosmic-ray events - FoV discrimination
Astrometry: - total detection noise: 6 e-
Photometry: - two-channel photometer
- blue and red CCDs Spectroscopy:
- high-resolution spectra - red CCDs
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Scanning law
Animation: Berry Holl, Lund
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Elementary observations
Over the mission, every source (star, QSO, asteroid, ...) will be observed ~ 600 times in the along-scan (AL) direction (timing data, t )
~ 70 times in the across-scan (AC) direction (pixel coordinate, p) These are the "elementary astrometric observations" of the source
Lindegren
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How do stars move?
proper motion (µα, µδ)
position at reference epoch
(α0, δ0)
parallax (ϖ)
path of star on the sky
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Gaia in March 2016
• 378 billion positional or astrometric measurements • 87.3 billion brightness or photometric data points • 8 billion spectra.
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16 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 16
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Gaia�s data reduction problem
With the same accuracy with which Gaia
• measures position of stars,
it is necessary to know • where Gaia is pointing at
(attitude), where Gaia is, how fast it is,
how exactly • the optic and detectors
are aligned • and, whether Einstein
was fully right!!
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Blue and Red Photometer
Abbildung: Anthony Brown
Δλ/λ<100
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Single RVS spectrum of K5 star HIP 86563 (V=6.63) compared to a ground-based spectrum Δλ/λ=11500
Field of view RVS Spektrograph CCD detector
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Discovery Machine
• 1-10 million new galaxies • 5 million new quasars • 100000 supernovae in other galaxies • Some thousand new asteroids • 100 million new double stars • 400000 new white dwarfs • A few hundred new brown dwarfs • 21000 (±6000) new planetary systems?
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Excessive Straylight
• Diffracted sunlight • Milky Way • Bright point objects
1. Sunshield 2. Insufficient baffling
A flight-spare blanket of the Gaia sun shield lit with a torch from the back to enhance the effect of scattered light from fibres protruding from the edge.
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21 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 21
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Contamination
After several decontamination with heaters the contamination with water ice has become very small. It is possible that no more decontaminations are necessary.
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Cyclic Variation of the Basic Angle
• The basic angle varies with a period of 6 hours=rotation with respect to the Sun
• Amplitude: 1.1 milliarcseconds • Specification: 4 microarcseconds • Corresponds to a shift of only a few
nanometers
1 mas = 5!10-9 rad < 4 nm movement of the main-mirror edges ~ 10 Si atoms (and even much less if it is a different mirror) Noise: a dozen or so picometers!
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HRD from TGAS
• Parallaxes from TGAS, photometry from Tycho 2 (V) and 2mass (J-K) • Left: relative parallax errors smaller than 20% • Right: relative parallax errors smaller than 10%
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Astrometric performance • http://www.cosmos.esa.int/web/gaia/science-performance • The standard-error calculation includes all known instrumental effects
o including the straylight levels • Appropriate calibration errors are included. • Warning: We are not yet fully calibrated! • Every single-CCD observation is more precise than the end-of-mission
precision of the Hipparcos catalogue (not in an absolute sense yet)!
• Depending on how well this mode can be calibrated, end-of-mission parallax standard errors at the level of a few dozen µas could potentially be achieved for these stars.
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25 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 25
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Photometric performance • End-of-mission photometric errors, in units of millimagnitude. • 30 millimagnitude calibration error at CCD-level
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26 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 26
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Radial velocity performance
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27 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 27
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Gaia�s release schedule
• http://www.cosmos.esa.int/web/gaia/release
• Late Summer 2016: (α, δ) positions only, G magnitudes. TGAS catalogue for 2 million stars. Release of photometric Ecliptic Pole data for Cepheids and RR Lyrae stars.
• 2017: Five parameter solution for single stars. Integrated BP/RP and AF photometry. Radial velocities for bright non-variable stars.
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28 Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 28
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Gaia�s schedule
• 2017/2018 (TBC): Five parameter solution for single stars + orbital solutions for binaries with appropriate periods. Object classification, BP/RP spectra + RVS spectra for well behaving objects.
• 2018/2019 (TBC): Additionally variable star classification, solar system objects, non-single star catalogue.
• 2022 (TBC): “Final” catalogue.
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Stefan Jordan ARI, Zentrum für Astronomie, Uni Heidelberg 29
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End of talk