ir astronomy with the italian robotic antarctic infrared telescope (irait) (m. busso) irait status,...
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IR Astronomy with theItalian Robotic Antarctic
Infrared Telescope (IRAIT)(M. Busso)
• IRAIT status, June 2006 (Mounting - Container – Tent - Software)
• IRAIT – 2005/2006 & 2006/2007 activities on site.
• First examples of feasible science of interest for THIS meeting (IR surveys)
• Some characteristics of the camera (M. Dolci)
Paris, June 14-16, 2006
Who is involved?
Paris, June 14-16, 2006
University of Perugia – P.I. Gino Tosti (telescope)
INAF (various Institutes, coordinated by Teramo Observatory) – AMICA camera (Straniero, Dolci)
Spanish consortium (coordinated by Granada & Barcelona groups,P.I. C. Abia): M2 and M3 (moving optics)
Plus: a ‘commissioning’ advisory council (M. Busso et al); will bechanged into a more official International Scientific Board afterCommissioning.
The optical layout
Paris, June 14-16, 2006
Optical Scheme: Optical Scheme:
Classical Cassegrain +2 Classical Cassegrain +2 NNasmyth asmyth stationsstations
•Primary Mirror Diameter 800 mm
•Focal Ratio of the primary 3
•Tolal Focal Ratio 20Presently: all parts finished.Mounting under way at ‘MarconTelescopes’ (after sparate tests,in climatic room or Antarctica,of critical subsystems).From July, 1 to September, 30:Astronomical tests in Perugia.
Paris, June 14-16, 2006
Tent
Completed: end of May 2006
Container
Was delivered to the Marcon Telescope company on Jan 16 Paris, June 14-16, 2006
Expedition
Paris, June 14-16, 2006
EXPEDITION IN AUTUMN!
Mirrors – ready by now!
Paris, June 14-16, 2006
IRAIT M1
IRAIT M3
IRAIT M2
Mounting… (May 2006)
Paris, June 14-16, 2006
Telscope Basement
Elevation wheel-pinionsTop Ring
Optical tube
…and mounting…
Paris, June 14-16, 2006
Telescope center piece
Azimuth slewing bearing &IRAIT Motors
… and mounting…
Paris, June 14-16, 2006
IRAIT M2 & M3 DRIVER SUBSYSTEMS(PI Carlos Abia UGR-Spain)
Construction: NTE (Barcelona), including mirrors, supportrs, focuser motor and reducer, limit switches, chopper actuators and chopper sensors. Manufacturing of mechanical parts started in January 2006. Ready by end June 2006 (mounting will start on the pre-assembled IRAIT structure in 10 days from now)
A
B
A
B
C
IRAIT Control system is on board the telescope
More details on subsystems?
Paris, June 14-16, 2006
IRAIT Power Distribution Layout
MT
24
VD
C P
S
C
T
Heater Fan
T
PLCKT 97
AI AI AI DC1
Moxa
2 3 4
GA
LIL
C C CC C C C CC C C C C
Heater
Fan
Fan
Fan
Fan
Heater
Heater
Heater
MT
SWITCH
PC1 TCS
MT
C C CC C
MT
2x12
VD
C P
S
5 V
DC
PS
24 V
DC
PS
M
M
MT
SLIPRING
d
Telescope Fork Boxes
Infrared Camera Box
400VAC
M
M
Optical Tube Box
C
test
M2/M3
SBP
Container Box
SEC
CTOF
C
C
C
C
IO G C
Moxa
Moxa
C
MoxaC
GPS
24VDC
230VAC
230VAC
230VAC
24VDC
24VDC
400VAC
400VAC400VAC
F
F
F
TESTER
Paris, June 14-16, 2006
IRAIT Internal Data Distribution Layout
1
Moxa 2p
2 3
Moxa 2p
4 GALIL
Moxa 2p
SWITCH
Moxa 2p
PLCKT 97
AI AI AIDCPC 1
(TCS)
GPS
AI AI AIDC
M2/M3
PC 2 (CAMERA)
AIDC
EthernetEthernet
MM Optical Fiber
CS31 Bus
CS31 Bus
Telescope Fork Box
Optical Tube Box
Infrared Camera Box
Container Box
RCN 727
RCN 727
EnDAT
SLIPRING
TESTER
Paris, June 14-16, 2006
IRAIT software modules: TCS
TCSTelescope
Control System
Controller
Driver
Driver
Driver
Driver
M
M
M
M
TCP/IPI am not the right person for this! Gino should have been here, and he is in bed with a flu, instead!
But…..
You are all invited to see, and touch, and try, and drink a good glass of wine with us at the end of the test phase:
PERUGIA 12-13 September 2006: IRAIT kick-off(info will be posted on the ARENA web-page).
Paris, June 14-16, 2006
Test done at Dome C in summer 2005/2006
1.Power supply stability2.WiFi Networking3.Tests on greese4.IRAIT PC server installation5.Measurements of the sky polarization
(we need to operate ALSO in summer: polarizing skylight lets you see the stars for pointing) Paris, June 14-16, 2006
IRAIT Team A Dome C
Paris, June 14-16, 2006
IRAIT Team A Dome C
IRAIT first experimentsnear Concoriastro
Paris, June 14-16, 2006
IRAIT Team At Dome C
Paris, June 14-16, 2006
Campaign at Dome C 2006/7
• Preparation of the IRAIT Site
• Istallation of the IRAIT auxiliary devices (Meteo station, etc..)
• Transportation of IRAIT at Dumont d’Urville (Oct 2006)
• One person (R. Briguglio) of the IRAIT team during winter 2007 at Dome C.
Paris, June 14-16, 2006
IRAIT at Dome C 2006/2007
Paris, June 14-16, 2006
IRAIT at Dome C 2006/2007
sIRAIT (IRAIT Team + AIP Potsdam)Installation of a small optical telescope + CCD camera & Filters(more extended tests of software, motors etc.). We shall try to operate it during winter.
Small IRAIT Focal Plane instrumentation:MAXCAM CM7-1ME Digital imaging systemUBVRI Filterrad 28mm, 8 Pos.UBVRI filtersDF-2 Digital focuser (50mm aperture)AD-1 Adapter MAXCAM AN DF-2
Small IRAIT is a 25 cm Cassegrain equatorially mounted
Paris, June 14-16, 2006
Paris, June 14-16, 2006
Science, a few examples(for an 80-cm telescope)
• Mid-IR wavelengths: stars black-bodies (Rayleigh-Jeans, -4);• Circumstellar envelopes with dust dominate over photospheres.
(OR very cool objects: brown dwarfs, giant planets, ….).• Obvious targets: red Galactic objects, interactions between stellar
fluxes and the ISM Examples: 1. Small-scale surveys of mass losing evolved stars
(AGB);2. Small-scale surveys of dense ISM regions & SFR
• Variability studied with repeated observations (long obs. time).• (In principle, a sample of galaxies at low Z (< 0.1) accessible to
study colors, SF bursts. IR bright galaxies, as well.• Moreover, ~100 known AGN reachable - IRAS!).• Hence: science interesting in itself, not only as a test-bench for
larger instruments.
Paris, June 14-16, 2006
At 12.5 mm, 0 mag 25.88 Jy. Suppose we measure down to 0.5 Jy in 10 min, 5 (a limit reached by us with TIRCAM2 at TIRGO, not in Antarctica! See Busso et al. 2006).
This means m(12) = +4.8
AN EXAMPLE: AGB STARS
I magnitudes: 17 to 14, with large I-K (2 to 5)
Alcaino et al. 1999
Paris, June 14-16, 2006
LMC MIRAS in K
Indeed, K-magnof LMC MIRASare 9-14 (Wood, 2000)
Paris, June 14-16, 2006
-Bolometric corrections on K are huge;-K-[12.5] colors are huge, up to 10 or more[12.5] magnitudes (in a filter 1 m wide)
are huge: between -10 and -15 forred AGBs with Mbol = -4 to -7
With a distance modulus of 18.5, we haveapparent [12.5] mags for LMC AGBs are 1 -- 5
Galactic AGBs (seeGuandalini, on Friday)
With a very cautious estimate we said we can measure a mag. of 4.8 in a 1 mm wide filter at 12 mm.
We can study in mid-IR the AGB phase of LMS stars, e.g.cluster.
Rich clusters in LMC are small: 3x3’ is a typical number.With AMICA (field > 2x2) we can do ‘limited surveys’ and
study luminosities and mass loss of the final evolutionary stages, at known distance
With long time availbale (variability) this is a unique, unprecedentedresult
With a 4-m telescope: same up to 200 Kpc (all dwarf spheroidals)In MCs, down to the whole of the RGB
Paris, June 14-16, 2006
Post-AGB Sources…….
As a conseqeunce….
Best use of IRAIT:
i) Preparation of automated operations for survey mode observations
ii) Identification of key small-scale survey projects, on topics like those mentioned (SFR, AGB stars, old populations in the Galaxy, & MCs).
iii) Moreover, ToO, like gamma-ray bursters: we will be operative during GLAST)
Paris, June 14-16, 2006
Astronomy is continuing to change…
J. Vermeer, The Astronomer, XVII century (The Louvre, Paris)
The Astronomer, XXI century, (Dome C, Antarctica)
Paris, June 14-16, 2006