UltraPhot, a photometric mode for FLAMES. Françoise Roques LESIA Observatoire de Paris
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1 UltraPhot, a photometric mode for FLAMES Françoise Roques LESIA Observatoire de Paris
2 UltraPhot Science : Variable Objects, Transits, Occultations Temporal resolution is a relatively unexplored region of the observational parameter space: CCD cameras =>> frame rate one frame per minute Few instruments =>> continuous high-speed observations : telescope Hale GHO Mayall Keck II ULTRACAM SAAO Gemini South SALT NOT frame rate Hz (Dhillon, 2008) t dyn " 2R3 GM ranges from second (white dwarfs) to millisecond (neutron stars and black holes) UltraPhot allows high speed visible photometry in three colors of large number of objects with frame rate of 100 Hz
3 UltraPhot Science : Variable Objects, Transits, Occultations 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 ULTRACAM : ultrafast triple beam camera (Dhillon, Marsh) 87 nights on WHT and 23 nights on VLT - 25 refereed papers - in 4 years ULTRACAM imaging 1-2 targets 500 Hz UltraPhot photometry (3 pts) targets 100 Hz
4 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
5 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 and optic :UltraPhot-ASTROSAT (launched in 2009) Dhillon et al. 2009
6 UltraPhot Science - Outer solar system - Stellar occultations (NASA: Whipple - Canadian-Space-Agency : microsatellite) 3 km at 42 AU, 40 Hz 10 km at 10 4 AU, 5 Hz 600 m at 42 AU, 40 Hz 4 km at 3000 AU, 10 Hz Nihei et al., 2007, Roques et al., 2008
7 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 M moon (Algol et al. 2005) Exomoon => 0.44M (Kipping et al., 2008) Transits Research : Earth-like planet are detectable. Fast photometry avoids red noise Corot targets monitoring : hundredths of potentials transits need to be confirmed by multi-colors observations Kepler targets (Carpano et al., 2009)
8 UltraPhot Science - Exoplanets «Transit Timing»
9 UltraPhot : scientific specifications 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
10 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
11 UltraPhot - aperture size UltraCam data r=2.4
12 UltraPhot - Optical design 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. David Horville, GEPI
13 UltraPhot - photometer design Michel Marteaud, LESIA
14 UltraPhot - position or under the floor? Michel Marteaud, LESIA
15 UltraPhot - camera
16 UltraPhot - camera
17 UltraPhot - camera Full Frame CCD => no dead time one cycle = integration : 8.7 ms - transfert+binning+reading : 1.3 ms Jean-Tristan Buey, LESIA
18 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
19 UltraPhot and Giraffe 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 to position the UltraPhot fibres. 2. UltraPhot inside the Giraffe enclosure presents several advantages but needs careful studied to insure no perturbation for the spectrograh : mecanic stability, thermal stability, accessibility 3. Software: the FLAMES observing mode and P2PP
20 UltraPhot - Realisation Technical manpower :2.8 FTE LESIA-GEPI implication >2.2 FTE Estimation of cost (optics-mechanic): Lesia, Gepi, NTHU Fibre link 50 k Mechanical 45 k Optical 30 k ANR (french research agency) : 140k Camera 70 k NSC (taiwanese research agency): 70k Others 15 k Total 210 k Estimation of cost (retractors, soft) AAO Total 62 k Planning T0 + 9 months : end of the design T0 +21 months : end of the manufacturing T months : end of integration
21 UltraPhot team Scientific PI Technical PI Scientific involvement Technical involvement Financial involvement Paris O.-LESIA X X X X Paris O.-GEPI X X X NTHU (Taiwan) X X X Napoli O. (Italia) X Paris O.-Luth X IAP X AAO X Paris observatory - LESIA : F. Roques, A. Doressoundiram, Y. Boissel, B. Sicardy, J-T. Buey, M. Marteaud Paris Observatory - GEPI : I. Guinouard, D. Horville National Tsing Hua University - Department of Physics : H.-K. Chang, A. Kong, S.-P. Lai, I.-C. Shieh Naples 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
22 Conclusions UltraPhot : - unexplored domain of observation parameters - challenging science - reliable - versatile - small - cheap - rapid manufacturing - experienced team - test for more sophisticated instrument? so why not? Thank you!
23
24 SNR : VLT/ULTRACAM - 46 Hz
25 Whipple: A Space-Based Occultation Survey of the Outer Solar System Smithsonian Astrophysical Observatory Ball Aerospace Jet Propulsion Laboratory
26 Spacecraft based on Kepler design 95 cm Schmidt optical system 100 square degree field of view Articulated solar arrays Hybrid CMOS focal plane array (Rockwell HyViSI/Hawaii-2RG) 140,000 stars, 40 Hz readout
27
28 ULTRACAM : an ultra-fast, triple-beam CCD camera (V. Dhillon and T. Marsh) William Herschel Telescope VLT - u : 0.36 µm, g :0.48 µm and i :0.77 µm) - two fields : one target + one reference 5
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