SlideShare uses cookies to improve functionality and performance, and to provide you with relevant advertising. If you continue browsing the site, you agree to the use of cookies on this website. See our User Agreement and Privacy Policy.
SlideShare uses cookies to improve functionality and performance, and to provide you with relevant advertising. If you continue browsing the site, you agree to the use of cookies on this website. See our Privacy Policy and User Agreement for details.
Successfully reported this slideshow.
Activate your 14 day free trial to unlock unlimited reading.
17.
The cost of space astronomy
HST:
≈ $2 billion at launch
(1990)
$9.6 billion lifetime cost,
including servicing
missions
17 / 73
Image: ESA
Source: NY Times: “Refurbishments Complete, Astronauts Let Go of Hubble”
18.
Ground based astronomy
VLT:
$330 Me to build
$16.9 Me annual
running costs
‘Expensive’ is relative
18 / 73
Image: ESA
Source: www.eso.org
21.
Guide stars and sky coverage
Isoplanatic patch = area
for which perturbations
roughly the same
Require rmag ≤ 10 star
within 5” – 40”, depending
on observation
wavelength and
atmospheric conditions
21 / 73
See e.g. Racine, 2006
23.
Laser guide stars
23 / 73
Image: R. Tyson - An introduction to AO (2000)
24.
Laser guide stars
Still require a tip-tilt NGS of
rmag ≤ 14 within ≈ 40” of
science target.
Good quality sky coverage
≈ 10% at 30◦
galactic latitude.
(Strehl ≥ 0.3, J band)
24 / 73
Davies et al., 2008
Ellerbroek and Tyler, 1998
25.
(Strehl?)
The ratio of peak intensity compared to a perfect
telescope (0 to 1)
HST Strehl near 1, but suffers pixellation effects.
AO Strehl usually varies from around 0.2 – 0.6
Seeing “Strehl” depends on the telescope, but is
typically ≈ 0.01 on medium size telescopes in
the visible.
25 / 73
30.
How to take advantage of this?
Cross-correlate speckle image with an Airy psf
model
Cross-correlation values provide a proxy for
Strehl
Cross-correlation positions give a good estimate
of brightest speckle
Select desired frames, then shift and add.
30 / 73
33.
Early tests
Seeing width ≈ 0.4”
33 / 73
Baldwin et al., 2001
34.
Early tests
ζ Bootis, Seeing width ≈ 0.8”
34 / 73
Baldwin et al., 2001
35.
Fast imaging with EMCCD’s
35 / 73
Cost: Around £15K
36.
Fast imaging with EMCCD’s
Conventional CCD:
SNR= M√
M+σ2
N
EMCCD:
SNR= M√
2M+(σN /gA)2
36 / 73
37.
Fast imaging with EMCCD’s
Calibration:
37 / 73
38.
Fast imaging with EMCCD’s
Calibration:
38 / 73
39.
Fast imaging with EMCCD’s
Calibration:
39 / 73
40.
Fast imaging with EMCCD’s
Limited pixel size, 1K2
Can only get 30 sq. arcseconds Nyquist
sampled on 2.5m telescope.
Readout electronics are a bottleneck on the
frame rate
40 / 73
46.
Wide fields of view: M13
120 x 30 arcsecond FoV @ 33mas per pixel
Challenging data storage and processing
requirements
Astrometric calibration is non-trivial
46 / 73
47.
Wide fields of view: M13
Zoom — 6.7 arcseconds across this FoV
Conventional imaging 50% frame selection
47 / 73
48.
Wide fields of view: M13
0 10 20 30 40 50 60
Distance from guide star in arcseconds
100
200
300
400
500
FWHMinmilliarcseconds
10% selection
100% selection
Seeing FWHM
48 / 73
49.
Guiding on a faint reference: the
Einstein cross
Guiding on a 17th mag. star — FWHM≈ 0.1”
49 / 73
50.
Science at the faint limit:
thresholding
Read out noise still 0.1 electrons.
Faint limit around 23rd magnitude on a 2.5m
telescope (good seeing)
Thresholding eliminates read noise
But for now we are limited by CIC
50 / 73
51.
Science at the faint limit:
thresholding
51 / 73
52.
Science at the faint limit:
thresholding
52 / 73
54.
Applications
High resolution surveys (e.g. microlensing in
crowded field)
54 / 73
55.
Applications
High resolution surveys (e.g. microlensing in
crowded field)
Cheap high resolution follow-up (stellar transits,
etc)
55 / 73
56.
Applications
High resolution surveys (e.g. microlensing in
crowded field)
Cheap high resolution follow-up (stellar transits,
etc)
Planetary imaging
56 / 73
57.
Applications
High resolution surveys (e.g. microlensing in
crowded field)
Cheap high resolution follow-up (stellar transits,
etc)
Planetary imaging
Potentially better faint limits that conventional
imagers in future? (esp. for bright sky)
57 / 73
58.
Applications
High resolution surveys (e.g. microlensing in
crowded field)
Cheap high resolution follow-up (stellar transits,
etc)
Planetary imaging
Potentially better faint limits that conventional
imagers in future? (esp. for bright sky)
But still limited to smaller telescopes.
58 / 73
64.
Lucky at Mt. Palomar
5m Palomar “200 inch” Hale telescope
512 sq. pixel EMCCD detector
First generation AO system (since upgraded)
64 / 73
Law et al., 2009
69.
Lucky + AO: Applications
Probing binarity in GC cores
Exoplanet direct imaging (See e.g Gladysz
2010)
69 / 73
70.
Lucky + AO: Applications
Probing binarity in GC cores
Exoplanet direct imaging (See e.g Gladysz
2010)
Resolving close stars (Kervella 2009)
70 / 73
71.
Lucky + AO: Applications
Probing binarity in GC cores
Exoplanet direct imaging (See e.g Gladysz
2010)
Resolving close stars (Kervella 2009)
Cheap visible wavelength AO on 4m class
telescopes
71 / 73
72.
Lucky + AO: Applications
Probing binarity in GC cores
Exoplanet direct imaging (See e.g Gladysz
2010)
Resolving close stars (Kervella 2009)
Cheap visible wavelength AO on 4m class
telescopes
Expanding AO sky coverage
72 / 73
73.
Summary
Standard lucky imaging can now go wide and
faint
This gives HST class capabilities at very low
cost
EMCCD’s are pretty good and still improving
AO astronomers should consider fast imaging to
get the most from their systems
73 / 73
0 likes
Be the first to like this
Views
Total views
1,058
On SlideShare
0
From Embeds
0
Number of Embeds
3
You have now unlocked unlimited access to 20M+ documents!
Unlimited Reading
Learn faster and smarter from top experts
Unlimited Downloading
Download to take your learnings offline and on the go
You also get free access to Scribd!
Instant access to millions of ebooks, audiobooks, magazines, podcasts and more.
Read and listen offline with any device.
Free access to premium services like Tuneln, Mubi and more.