Large Binocular Telescope: LBT: stato, problemi, opportunita’rifatto/sait_2013/fontana.pdf ·...
Transcript of Large Binocular Telescope: LBT: stato, problemi, opportunita’rifatto/sait_2013/fontana.pdf ·...
Large Binocular Telescope: LBT: stato, problemi, opportunita’
A d r i a n o F o n t a n aI N A F O s s e r v a t o r i o d i R o m a
C e n t r o I t a l i a n o C o o r d i n a m e n t o O s s e r v a z i o n i L B T
Large Binocular Telescope: LBT: stato, problemi, opportunita’
A d r i a n o F o n t a n aI N A F O s s e r v a t o r i o d i R o m a
C e n t r o I t a l i a n o C o o r d i n a m e n t o O s s e r v a z i o n i L B T
Italian staff:
Scheduling & Service mode observationsRoberto Speziali (OAR-resp)Marco Faccini (OAR)Eleonora Sani (Arcetri)Felice Cusano (OABo)Angela Bongiorno (OAR)Marco Fumana (IASF-Mi)Konstantina Boutsia (OAR)
Data processing & Science+ OutreachVincenzo Testa (OAR-resp)Stefano Gallozzi (OAR)Riccardo Smareglia (OATs)Marco Faccini (OAR)Cristina Knapic (OATs)Diego Paris (OAR)Marco Fumana (IASF-Mi)
1) LBTO has a new Director
2) LBT as a working telescope: the performances of LBT and the exploitation of the italian community
3) Future developments: AO and 2nd gen instruments
4) Funds: Premiale 2012 and 2013
1) LBTO has a new Director
Christian Veillet is the LBTO Director since Feb 1, 2013.
Former Director of CFHT for 9 years (3 mandates)
In 2011 and 2012, LBT based papers were 18/yrA factor 2-3 below similar observatories after 4-5yr of operations
Drake equation: current number of civilizations in the Galaxy
“LBT” equation: scientific impact depends on a number of multiplicative factors
•Some of these factors are beyond our control;
•Some can be (partly) affected by the actions of Italian Board & STC Members
•Some depend on priorities and organization of the Italian community.
2) LBT as a working telescope: the performances of LBT and the exploitation of the italian community
3 Instruments in operations:LBC (2 instruments)
MODS (1 instr., 2 channels)LUCI
LBC and MODS have been working quite reliably over the last two years.
LUCI unfortunately suffered from repeated failures.
MOS is currently not operational.
2) LBT performances: official LBTO statistics
6.4%
30%
52-56%
2) LBT performances: use of Italian time
2011feb-2013apr45 Italian Proposals were observed
18 (40%) observed at 100%21 (47%) observed at >75%32 (71%) observed at >50%
Science data - open shutter time on science target
2012 Sep12-Apr13
Italian hours/nights 418h/45n 357h/36n
LBC-Blue 63.4h 60h
LBC-Red 65h 60h
LUCI1 50h 57h
MODS-B 74h 40
PISCES 12.4h
TOTAL (no PISCES, average LBC)
201h (45%) 157h (43%)
TOTAL IN SPEC 124h (35%)
Italy@ESO 2010
Total amount of science-quality data in ESO VLT archive(all science data, no calibration - includes out-of-spec data)
Total 6014 hrs 681 proposals
Italian PIs 1003hrs 60 proposals
16,6% 9%
VLT 4.1hr/night/telescope -> efficiency about 40-45%
LBT Strategic programs:Uband imaging of GOODS-N & CANDELS fieldsGrazian et al
20h in the Uband, seeing 1”
LBT U band, seeing 1”
10hr exposure
HST-ACS B band
LBC
21 Oct 2011
PI: Clementini
~15 min of exposure
out of 16hr of exposure
acquired over 5 days
INAF Discretionary Time Observations:GJ3470: planet transit with LBC (Nascimbeni, Piotto et al)
Redshift ~ 2 galaxies with LUCI
PI: Pentericci, Oct 2010, 4hrs exposure
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Publications
TOTALTOTAL ITALIANITALIAN %%
All no-AO
All no-AO
All no-AO
2007
2008
2009
2010
2011
2012
2013
TOT
2 2 1 1 50% 50%
12 12 2 2 17% 17%
9 9 3 3 33% 33%
6 6 3 3 50% 50%
17 17 5 5 29% 29%
18 15 1 1 5% 7%
11 8 3 1 27% 12%
75 69 18 16 24% 23%
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Feedback from users: a questionnaire to all Italian P.I.
Sent: 60 Answers: 46 (76%) (31 PIs, 80% of them replied)
Published papers: 9 / 46 (20%) - 3/46 used mainly LBT dataClosed to submit: 5/46 --> 30%
Of those still unpublished:Data Quality ok: 26/39 (66%)Data Quality & Quantity ok: 18/39 (46%)
Plan to publish anyway: 30/40 (75%)Need more data: 3/40 (7.5%)Won’t publish: 7/40 (17.5%)
Conclusion #1
LBT is operational and delivers world-class data.
Its operational efficiency is in line with similar telescopes. It can be improved but it is already good enough to complete several challenging programs for the Italian community.
The publication rate of the Italian community is lower than expected. It is not given to poor data nor to complex data reduction.Reasons unclear, possibly tied to over-busy PIs?
1) LBTO has a new Director
2) LBT as a working telescope: the performances of LBT and the exploitation of the italian community
3) Future developments: AO and 2nd gen instruments
4) Funds: Premiale 2012 and 2013
LBT AO: the first Extreme Adaptive Optics in the worldOct 2011
LBT AO: the first Extreme Adaptive Optics in the worldOct 2011
Hband WFC3@HST Hband PISCES@LBT
The path to AO science...
A PI instrument (Az) LBTI-NIRCAM (3-8μm imaging) is operational. A planet survey (LEECH) is starting now with italian coIs
The first science-grade instrument for AO will arrive in early 2014 (LUCI2 with AO camera)
The “smart” laser system ARGOS will gave first light in mid 2014
NIRVANA-pathfinder is coming in late 2013
NIRVANA planned for 2015
Proposal for a Coronagraph usingextreme AO for the LBT
Enrico Pinna on behalf of:J. Farinato1, F. Pedichini2, E. Pinna3, F. Baccio:3, C. Baffa3, M. Centrone2, S. Desidera1, M. Dima1, S. Esposito3, A. Fontana2, E. Giallongo2, R. GraGon1, F. Lisi3, D. Magrin1, R. Ragazzoni1, E. Sani2
1) INAF-‐Padova 2) INAF-‐ Monte Porzio 3) INAF-‐Arcetri
SHARKSystem for coronagraphy with High order AdapNve opNcs from R to K band
… this is why we propose SHARK•XAO system already built in LBT, based on unique components (Pyramid and ASM) •No other Planet Finders are foreseen in the Northern Hemisphere in the near future (Kepler targets follow up)•Extend the LBT scienIfic potenIality, indeed taking advantage and exploiIng its binocular capabiliIes
EntranceWindow
FP FilterWheel
Flat foldingmirrorApodyzer
Mask SelectorScience doubleFilter Wheel
2nd Off-‐AxisParabola
InsertableFlat Mirror
Beam to theIR Camera
1st Off-‐AxisParabola
ExitWindow
SHARK CONCEPT a Vis-‐NIR CORO
Study with the aim to assess:• Technical feasibility• Cost and schedule esImate• Volume and weight (as low as possible)• “Team” layout
Study Outcome:• Technical risk very low (the most risky sub-‐system, XAO, is already implemented!)
• 1 inch size opIcs with demanding polishing, but commercially available• Standard Cryo components for the IR part• Commercial Vis and IR detector
• Small dimensions (~600x250x130mm without Cryo shield)• 2.5/3 years from T0 to first light (depending on adopted soluIon)• Reasonable HW cost ranging from 1.5 to 3.0 M€ (depending on adopted soluIon)• 3 INAF Observatories already involved with experIse in all the relevant fields
GeneraPon 1.5
Possible upgrade with IFU
Science NIR – Imaging of exo-‐planets• ExploraIon of outer regions of planetary systems (P>a few thousands days)
• CharacterizaIon of planets: e.g. L-‐T spectral type transiIon
Imaging
FLAO + Pisces
FLAO + SHARK (NIR)
SPHERE & GPI
E-‐ELT + PCS
SimulaNon of planet contrast using MESS (Bonavita, 2012)
FLAO + SHARK may discover and characterize a few tens of planets
DetecPon of four planets around HR8799 with FLAO+Pisces in H-‐band
Science -‐ Planets in the Vis domain ?@800nm SR ≥45% -‐> resoluIon of 20mas
exoplanet detecPon at 4 λ/D ≈ 100mas (≤1AU at d≤ 10pc)
Cool & massive Jupiters: 800-‐1200nm color constraints on their age and thermal state (e.g. a color of 1-‐2mag would indicate young ages ≈107-‐108 y)
Possible detecPon of reflected-‐light from giant exoplanets if enough contrast/SNR SNR depends on the coronagraph and residual speckle noise aker AO correcIonOpIcal observaIons enable long total exposure (but very short ≈10-‐3s per frame), lower RON & background -‐> a good speckle noise suppression and reasonable faint magnitude limits (22-‐24mag at 5σ)
Combined with NIR detecPons, opPcal data will help to understand the relaPve contribuPon of thermal emission and reflected light in planets located at ~1 AU in nearby stars (5-‐10pc)
Science Vis-‐IR: Jets
Jet from DL Tau ,Grady et al. ‘04
Collimated jets are common around young stellar objects (YSOs)The jet generaPon mechanism influences the disk properPes,and hence the formaPon history of both star and planetsneed to study jet base ( < 0.3” in Taurus) with high angular res (HST 0.1”)
Despite jets emit only in UV-‐VIS-‐IR lines, severe star/jet contrast problem (102 – 104) :
Arempt 1: image reconstrucIon from HST/STISmulIple stepped spectra aker coonInuum subtracIoncons: too many orbits, analysis difficult, only for wide jets
star+disk
Baccio: et al. ‘00
jet
bow shock
Arempt 2: direct imaging with HST coronagraphcons: dependence on coordinates, min stop radius 0,6” -‐ 1” : stop too large !
PROS LBT/SHARK + Narrowband filters -‐ Stop size : only 0.04”! Angular resoluIon : 0.075” possibility to sample jets as close as 3-‐5 AU from star -‐ AO correcIon opImal (bright parent star) -‐ samples lines in both VIS and NIR: spectral diagnosIcs ! -‐ Northern hemisphere: most interesIng objects (Taurus, Orion)
SCIENCE GOALS: beier understanding of -‐ jet generaIon mechanism: feedback on star/disk system ? -‐ knots in the jet: instabiliIes due to giant planet(s) in eccentric orbit ?
Science Vis-‐IR: AGN-‐Gal co-‐evoluNonScienIfic raIonale: a) Discover and fully characterize AGN close pairs.b) Constrain the BH feeding mechanism (e.g. supernova driven winds vs gravitaIonal
asymmetries) in local Seyferts.c) Constrain the AGN feedback driver (e.g. radiaIve rather than mechanic) in bright QSOs.
NACO ADI of NGC 1068(Gratadour et al. 2005)
With extreme contrast and high Strehl raIos (expecially in the K band), SHARK will allow to:a) Detect unknown AGN close pairs (<200 pc) with a success probability up to 80%
b) Probe gaseous and dusty structures from the innermost regions (few tens of pc) to the kpc scales with unexplored fine details.
MulI band images in the Vis-‐IR range are crucial to:a) confirm the AGN pairs thought SED fixngb) full characterizaIon of the circumnuclear environment (dust, gas, ionized gas)
Premiale LBT 2012
3300 KE 70% ongoing activities
10% minor improvements20% 2nd gen. instruments
Premiale LBT 2013
3800 KE 60% ongoing activities
10% minor improvements30% 2nd gen. instruments