UltraPhot, a photometric mode for FLAMESFrançoise Roques LESIA Observatoire de Paris UltraPhot, a...
Transcript of UltraPhot, a photometric mode for FLAMESFrançoise Roques LESIA Observatoire de Paris UltraPhot, a...
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
Françoise RoquesLESIA
Observatoire de Paris
UltraPhot,a photometric mode for FLAMES
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
Temporal resolution is a relatively unexplored region of the observational parameter space:CCD cameras =>> frame rate ≤ one frame per minuteFew instruments =>> continuous high-speed observations :
UltraPhot Science : Variable Objects, Transits, Occultations
30NOT10SALT7Gemini South1SAAO
500ULTRACAM14Keck II
24000Mayall7.5GHO
1000Haleframe rate Hztelescope
UltraPhot allows high speed visible photometry in three colorsof large number of objects with frame rate of 100 Hz
(Dhillon, 2008) !
tdyn "2R
3
GMranges from second (whitedwarfs) to millisecond (neutronstars and black holes)
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
Potential interested scientific fields are numerous :
• Cataclysmic Variables, accreting white dwarfs• Black-holes, X-ray binaries• Stellar occultations (outer solar system)• Extrasolar Planets Transits• Pulsars• Young Stellar Objects
UltraPhot Science : Variable Objects, Transits, Occultations
ULTRACAM : ultrafast triple beam camera (Dhillon, Marsh)87 nights on WHT and 23 nights on VLT - 25 refereed papers - in 4 years
100 Hz500 Hz
50-100 targets1-2 targets
photometry (3 pts)imaging
UltraPhotULTRACAM
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot Science- Young Stellar Objects
Variability of Young Stellar Objects :• Rotation, derived from hot spots• Eclipse/occultation - protoplanets,protoplanetary disks• Accretion• Flares
Goal : flares frequency with mass/age - disks accretion rates…
A possible target : Orion Nebula Cluster : 2000 stars in a 8’ radius sphere
Feigelson et al, 2002
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot Science - Compact Objects
Neutron stars, black holes in X-ray binaries
Variability of compact binaries :• orbital period•Super orbital period (precession)•Pulsation•Quasi-Periodic-Oscillations
Dynamical time scale:seconds (white dwarfs) - milliseconds (black holes)
Echo-tomography : time delay between X andoptic :UltraPhot-ASTROSAT (launched in 2009)
Dhillon et al. 2009
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
3 km at 42 AU, 40 Hz
600 m at 42 AU, 40 Hz
10 km at 104 AU, 5 Hz
4 km at 3000 AU, 10 Hz
UltraPhot Science - Outer solar system - Stellar occultations
Nihei et al., 2007, Roques et al., 2008
(NASA: Whipple - Canadian-Space-Agency : microsatellite)
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot Science - Exoplanets
Transit Timing Variations : changes in the parameters of the transits.Timing accuracy of 6 seconds par epoch (Steffen et al. 2007)Multiple planetary systems: => 5 Mmoon (Algol et al. 2005)Exomoon => 0.44M⊕ (Kipping et al., 2008)
Transits Research : Earth-like planet are detectable. Fast photometryavoids red noise
Corot targets monitoring : hundredths of potentials transits need tobe confirmed by multi-colors observations
Kepler targets (Carpano et al. , 2009)
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot Science - Exoplanets « Transit Timing »
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot : scientific specifications
•300-900 nm spreaded in 3 colors• acquisition frequency ≥ 100 Hz• number of targets ≈ 100• photometric precision
T: transmission factor > 20%(Ultracam/VLT => T=30%)
input aperture on the sky >5 arcsec diameter temporal and relative stability of the fibres
Two operating modes : • dedicated program • survey mode (occultations, transits)simultaneously with Giraffe/UVES
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot concept
Ultraphot is composed of :- a multi-object fibres link + Ozpoz (magnetic buttons + retractors)- a photometer :optics (relays, mirrors, lenses, dichroics…) + CCD-camera
The photometer is - small (600x600x60mm)- with no moving part- motorized setting
Two options :- equipate free places (84-69) on existing plates- build 2 supplementary plates
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
r=2.4’’
UltraCam data
UltraPhot - aperture size
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
The optical design below allows to throw 3 images of fibres in 3 different spectral ranges.The parabolic mirror collimates the beam and allows to use a dichroic mirror.The camera reduces the image size of the entrance field to the dimensions of the detector.
UltraPhot - Optical design
David Horville, GEPI
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot - photometer design
Michel Marteaud, LESIA
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
orunder the floor?
UltraPhot - position
Michel Marteaud, LESIA
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot - camera
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot - camera
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
“Full Frame CCD” => no dead timeone cycle = integration : 8.7 ms - transfert+binning+reading : 1.3 ms
UltraPhot - camera
Jean-Tristan Buey, LESIA
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot - Software
- Ozpoz Robot software : introduction of more fibres, back-illumination system control- Fibres configuration program to support the new fibre type- UltraPhot observing mode :- P2PP software- Tests, calibration, documentation
The linear CCD can be read with the new NGC (Next Generation Controller)
Data rate is quite important : 20 Gbits/night
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
A concern about this project is to assure it does not modify FLAMES programs.
The coexistence of UltraPhot and Giraffe must be studied at several interfaces :
1. focal plate and positioner: Buttons are added and the Ozpoz software must be modified toposition the UltraPhot fibres.
2. UltraPhot inside the Giraffe enclosure presents several advantages but needs careful studied toinsure no perturbation for the spectrograh : mecanic stability, thermal stability, accessibility
3. Software: the FLAMES observing mode and P2PP
UltraPhot and Giraffe
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
Estimation of cost (optics-mechanic): Lesia, Gepi, NTHU Fibre link 50 k€Mechanical 45 k€Optical 30 k€Camera 70 k€Others 15 k€Total 210 k€Estimation of cost (retractors, soft) AAO Total 62 k€
ANR (french research agency) : 140k€NSC (taiwanese research agency): 70k€
PlanningT0 + 9 months : end of the designT0 +21 months : end of the manufacturingT0 + 24 months : end of integration
Technical manpower :2.8 FTE LESIA-GEPI implication >2.2 FTE
UltraPhot - Realisation
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
X
X
X
Financialinvolvement
XAAO
XIAP
XParis O.-Luth
XNapoli O. (Italia)
XXNTHU (Taiwan)
XXParis O.-GEPI
XXXParis O.-LESIA
Technicalinvolvement
Scientificinvolvement
Technical PIScientific PI
Paris observatory - LESIA :F. Roques, A. Doressoundiram, Y. Boissel, B. Sicardy, J-T. Buey, M. MarteaudParis Observatory - GEPI : I. Guinouard, D. HorvilleNational Tsing Hua University - Department of Physics :H.-K. Chang, A. Kong, S.-P. Lai, I.-C. ShiehNaples Observatory - INAF : D. de Martino, R. Silvotti Institut d’Astrophysique de Paris : J.P. Beaulieu Paris Observatory - LUTH:J. Schneider Anglo-Australian Observatory : T. Farrell, K. Shortridge
UltraPhot team
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
UltraPhot : - unexplored domain of observation parameters - challenging science- reliable- versatile- small - cheap- rapid manufacturing- experienced team- test for more sophisticated instrument ?
so why not?
Conclusions
Thank you!
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
SNR : VLT/ULTRACAM - 46 Hz
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
Whipple: A Space-BasedOccultation Survey of the Outer
Solar System
Smithsonian Astrophysical Observatory
Ball Aerospace
Jet Propulsion Laboratory
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
• 95 cm Schmidt optical system
• 100 square degree field of view
• Articulated solar arrays
• Hybrid CMOS focal plane array (RockwellHyViSI/Hawaii-2RG)
• 140,000 stars, 40 Hz readout
Spacecraft based on Keplerdesign
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
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March 9-10, 2009 ESO Spectroscopic Survey Workshop
• William Herschel Telescope • VLT
ULTRACAM :an ultra-fast, triple-beam CCD camera (V. Dhillon and T. Marsh)
- u’: 0.36 µm, g’:0.48 µm and i’:0.77 µm)- two fields : one target + one reference
5’