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