Transcript irait

IR Astronomy with the
Italian 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?
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 be
changed into a more official International Scientific Board after
Commissioning.
Paris, June 14-16, 2006
The optical layout
Optical Scheme:
Classical Cassegrain +2 Nasmyth stations
•Primary Mirror Diameter
800 mm
•Focal Ratio of the primary
3
•Tolal Focal Ratio
20
Presently: all parts finished.
Mounting under way at ‘Marcon
Telescopes’ (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
Paris, June 14-16, 2006
Container
Was delivered to the Marcon Telescope company
on Jan 16
Paris, June 14-16,
2006
EXPEDITION IN AUTUMN!
Expedition
Paris, June 14-16, 2006
Mirrors – ready by now!
IRAIT M3
IRAIT M1
IRAIT M2
Paris, June 14-16, 2006
Mounting… (May 2006)
Elevation wheel-pinions
Telscope Basement
Top Ring
Optical tube
Paris, June 14-16, 2006
…and mounting…
Telescope center piece
Azimuth slewing bearing &
IRAIT Motors
Paris, June 14-16, 2006
… and mounting…
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
Paris, June 14-16, 2006
B
More details on subsystems?
IRAIT Control system is on board the telescope
B
C
A
Paris, June 14-16, 2006
IRAIT Power
Distribution Layout
Optical Tube Box
Infrared Camera Box
M2/M3
Telescope Fork Boxes
GPS
24VDC
PC1
TCS
Heater
SWITCH
400VAC
Heater
Heater
230VAC
F
Heater
Fan
Fan
Fan
C
C
C
C
PLC
KT 97
Mo
xa
C
C C C C
C C C C C C C C
F
AI
AI
AI
DC
M
T
M
T
24VDC
24 VDC PS
C
Mox
a
5 VDC PS
C
M
T
M
T
C
C C
T
M
M
Container Box
M
M
test
d
S
B
P
400VAC
T
Heater
SEC
M
T
C C C
TESTE
R
230VAC
400VAC
C
F
230VAC
C
Mox
a
Mox
a
Fan
24VDC
2x12 VDC PS
4
24 VDC PS
3
GALI
L
2
IO
G
1
C
T
O
F
Fan
SLIPRING
400VAC
Paris, June 14-16, 2006
M2/M3
IRAIT Internal Data Distribution
Layout
Infrared Camera Box
Optical Tube Box
AI
PC 2
(CAMERA)
AI
AI
D
C
Telescope Fork Box
1
2
3
4
G
PS
GALIL
CS31 Bus
SWITCH
PLC
KT 97
PC 1
(TCS)
Moxa 2p
Moxa 2p
AI
AI
AI
D
C
Moxa 2p
Moxa 2p
Ethernet
Ethernet
TESTE
R
Container Box
EnDAT
RCN 727
RCN 727
SLIPRING
AI
D
C
CS31 Bus
MM Optical Fiber
Paris, June 14-16, 2006
IRAIT software modules: TCS
Driver
TCS
TCP/IP
I am not the right person
for this!
Gino should have
Driver
Telescope
Controller
Control
been here, and he is in bed
with a flu, instead! Driver
M
M
M
System
Driver
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
M
Test done at Dome C in
summer 2005/2006
1.Power supply stability
2.WiFi Networking
3.Tests on greese
4.IRAIT PC server installation
5.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 experiments
near 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 is a 25 cm Cassegrain equatorially mounted
Small IRAIT Focal Plane instrumentation:
MAXCAM CM7-1ME Digital imaging system
UBVRI Filterrad 28mm, 8 Pos.
UBVRI filters
DF-2 Digital focuser (50mm aperture)
AD-1 Adapter MAXCAM AN DF-2
Paris, June 14-16, 2006
Science, a few examples
(for an 80-cm telescope)
•
•
•
•
•
•
•
Mid-IR wavelengths: stars  black-bodies (Rayleigh-Jeans, l-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
AN EXAMPLE: AGB STARS
At 12.5 mm, 0 mag  25.88 Jy. Suppose we measure down to 0.5 Jy in 10 min,
5s (a limit reached by us with TIRCAM2 at TIRGO, not in Antarctica! See
Busso et al. 2006).
This means m(12) = +4.8
Alcaino et al. 1999
I magnitudes: 17 to 14,
with large I-K (2 to 5)
Paris, June 14-16, 2006
LMC MIRAS in K
Indeed, K-magn
of LMC MIRAS
are 9-14
(Wood, 2000)
Paris, June 14-16, 2006
With a very cautious estimate we said we can measure a mag.
of 4.8 in a 1 mm wide filter at 12 mm.
Galactic AGBs (see
We can study in mid-IR the AGB phase of LMS
stars, e.g. on Friday)
Guandalini,
cluster.
Rich clusters
in LMCcorrections
are small: on
3x3’
typical number.
-Bolometric
K is
area huge;
With AMICA
(field
> 2x2)
can up
do to
‘limited
surveys’ and
-K-[12.5]
colors
arewe
huge,
10 or more
study
luminosities
and(in
mass
loss1ofmm
thewide)
final evolutionary
[12.5]
magnitudes
a filter
stages, at known
distance
are huge:
between -10 and -15 for
With long time red
availbale
is a-7unique, unprecedented
AGBs(variability)
with Mbol =this
-4 to
result
With a distance modulus of 18.5, we have
With a 4-m
telescope:
toLMC
200 Kpc
(allare
dwarf
apparent
[12.5]same
magsupfor
AGBs
1 -- spheroidals)
5
In MCs, down to the whole of the RGB
Paris, June 14-16, 2006
Post-AGB Sources…….
Paris, June 14-16, 2006
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