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CHARA 2014 Science & Technology Review
Observations with JouFLUUpdate and First Results
Nicholas J ScottMarch 2014
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CHARA 2014 Science & Technology Review
Intro
Current status
2013 observing
Polarization issues
Spectral dispersion mode
Future
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CHARA 2014 Science & Technology Review
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CHARA 2014 Science & Technology Review
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CHARA 2014 Science & Technology Review
Differences• Remote operations• Software & hardware integrated with
CHARA environment• Pupil imaging• Improved fiber injection• Improved alignment procedure• Spectral dispersion mode• FTS
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CHARA 2014 Science & Technology Review
2011 2012 2013 2014 2014
Spectral dispersion mode
2/14
Ethernet readout
2/14
FLUOR run-IV10/13
FLUOR run-III10/13
Re-centered fiber bundle8/13
Changed ZABER mode7/13
FLUOR run-II6/13
Realigned OAPs5/13
Moved MONA, NICMOS, & output5/13
First on-sky fringes w NICMOS
5/13
Optimized MONA plz5/13
FLUOR run-IB5/13
FLUOR run-IA4/13
CALI replaced w NICMOS4/13
CALI tests12/12
CALI Meudon tests11/12
First fringes5/12
JouFLU hardware install2/12
1st remote run10/11
Remote obs setup9/11
Switch from LabView to C7/11
Software preparations 6/11 7/12
Component testing 11/11 3/14
Science 5/13 3/14
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CHARA 2014 Science & Technology Review
Current status report• First science data taken• Preliminary data reductions done
– Initial science data reduced– More testing of reduction code planned
• New alignment procedures being documented• Remote ops tested and working
– Barring network issues
• Polarization issues investigated• OAP improvement planned
Better throughput
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CHARA 2014 Science & Technology Review
New camera alignment gui stuff
JouFLU GUI
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CHARA 2014 Science & Technology Review
Fiber injection raster scan
2013-7-16 13:57:34 beam A NOSTARsize of raster= 9.00000zaber step size= 40.0000Mean = 240.138214Stddev = 524.807007baseline= 119.698peak= 3948.22peak half-width (x)= 0.496464peak half-width (y)= 0.789272Avg FWHM (steps)= 1.28574peak centroid (x)= 3.78804peak centroid (y)= 4.79696rotation angle (radians)= 0.000000size of raster= 9.00000micro step size (radians)= 5.95372e-005physical step size (um)= 6.04898number of steps across fiber diameter (um)=
1.07456Avg FWHM (microns)= 7.77739Number of zaber steps across FWHM=
1.28574
Configuration and log data saved with each alignment
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CHARA 2014 Science & Technology Review
Comparison to known diameter
• Tabby 0.981 0.015• One bracket, more obs planned
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CHARA 2014 Science & Technology Review
FLUOR nights awarded
13%
other programs
87%
Total CHARA nights
FLUOR data
collected71%
no data collected
29%
FLUOR nights
0
5
10
15
20
25
30
35
40
45
number of files per night
all nights good night
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CHARA 2014 Science & Technology Review
seeing/piston56%
clouds22%
instrument problem
7%
metrology problem
7%
network problem5%
user error3% Noted in log
0
50
100
150
200
250
300
0-5 5-10 10-15
seeing for number of files
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CHARA 2014 Science & Technology Review
HD 27789
4.86FU Ori
5.17
mK magnitude limit
Per hour
0.5 Per night
4.6
Number of brackets (1o2o3o1)
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CHARA 2014 Science & Technology Review
Polarization
Why can we only get a maximum V of ~0.3+?
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CHARA 2014 Science & Technology Review
0
0.2
0.4
0.6
0.8
1
1.2
0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180
2b-0 2a-0 2b-90 2a-90
FLUOR V_LOGNORM
Detector1 Mean Detector2 Mean Combined Mean
0
0.2
0.4
0.6
0.8
1
1.2
0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180
2b-0 2a-0 2b-90 2a-90
CLASSIC V_LOGNORM
Detector1 Mean Detector2 Mean Combined Mean
Polarizer at each beam entrance,One rotated.
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CHARA 2014 Science & Technology Review
-10
0
10
20
30
40
50
0 10 20 30 40 50 60 70 80 90 100110120130140150160170180
Sh
utt
er
B
One polarizer at input B, beam A blocked. Other at output and set to 0.
1b-0
Sig1 Sig2 Phot1 Phot2
-5
0
5
10
15
20
25
30
0 10 20 30 40 50 60 70 80 90 100110120130140150160170180
Sh
utt
er
A
One polarizer at input A, beam B blocked. Other at output and set to 0.
1a-0
Sig1 Sig2 Phot1 Phot2
-505
10152025303540
0 10 20 30 40 50 60 70 80 90 100110120130140150160170180
Sh
utt
er
B
One polarizer at input B, beam A blocked. Other at output and set to 90.
1b-90
Sig1 Sig2 Phot1 Phot2
-5
0
5
10
15
20
25
30
35
0 10 20 30 40 50 60 70 80 90 100110120130140150160170180S
hu
tte
r A
One polarizer at input A, beam B blocked. Other at output and set to 90.
1a-90
Sig1 Sig2 Phot1 Phot2
Polarization rotationSig1 Sig2
Test1-0 30 80Test1-90 40 110
differential polarization rotation=50°70°
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CHARA 2014 Science & Technology Review
00.050.1
0.150.2
0.250.3
0.350.4
0.45
0 10 20 30 40 50 60 70 80 90 100110120130140150160170180
V
one polarizer at WL source
Classic V_SCANS 4
V_SCANS Detector1 Mean V_SCANS Detector2 Mean
V_SCANS Combined Mean no plz det1
no plz det2 no plz combined
0
5
10
15
20
25
30
35
1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19one polarizer at WL source
JouFLU 4
BOTH_BEAMS Sig 1 BOTH_BEAMS Sig 2
BOTH_BEAMS Phot 1 BOTH_BEAMS Phot 2
00.10.20.30.40.50.60.70.8
0 10 20 30 40 50 60 70 80 90 100110120130140150160170180
V
one polarizer at WL source, no polarizer also shown
JouFLU V_SCANS 4
V_SCANS Detector1 Mean V_SCANS Detector2 Mean
V_SCANS Combined Mean no plz det1
no plz det2 no plz combined
differential delay wrt to polarizationdphi= 109 degree ;max
differential phase delay btw
orthogonal polarizations
0
50
100
150
200
250
0 10 20 30 40 50 60 70 80 90 100 110 120 130 140 150 160 170 180one polarizer at WL source
Classic test 4
I1 detector1 mean I1 dectector2 mean
I2 detector1 mean I2 dectector2 mean
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CHARA 2014 Science & Technology Review
Polarization Summary• Found differential polarization rotation and differential phase delay • Modelling differential phase delay gives dphi = 109°and 90°periodicity• Max V ~ 0.73
– bandwidth smearing / dispersion– beam intensity imbalance– fringe sampling & finite integration effects – AND differential polarization rotation.
Differential rotation:• V loss is analogous to beam intensity mismatch
50° 90%V70° 60%V
Additionally,- WL is probably not circularly polarized. - We observe average V~0.42 instead of expected 0.59.- WL is elliptically polarized (close to 50 or 150°).
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CHARA 2014 Science & Technology Review
Beam Balance• Factor of 2-3 diff between FLUOR beams
– Beam A weak• 15% difference between CLASSIC beams• Reduces maximum visibility
• Replace OAPs
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CHARA 2014 Science & Technology Review
0 50 100 150 200 250 300 350 4000
0.2
0.4
0.6
0.8
1
Baseline
Vis
ibil
ity
260 280 300 320 3400
0.02
0.04
0.06
0.08
Baseline
Spectral dispersion• K band • Up to 10 spectral channels• 500 Hz fastest rate possible with 5 spectral channels • Remove chromatic biases / bandwidth smearing• Expect factor of 100 improvement when science star
and calibrator are of different types
PA S2
S1 PB
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CHARA 2014 Science & Technology Review
Spectrally dispersed lab fringes
S1
S2
difference
S1 & S2 channels
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CHARA 2014 Science & Technology Review
2.218
2.119
2.024
2.166
2.052
2.216
2.130 2.145
2.063
1.944
y = -0.0285x + 2.2012R² = 0.3171
y = -0.0611x + 2.2826R² = 0.8866
1.8
1.9
2
2.1
2.2
2.3
2.4
2.5
0 1 2 3 4 5 6
lam
bd
a
spectral pixel
Scan vel for calc, fitted fringe to each scan for wavelength
S1
S2
Linear (S1)
Linear (S2)
S1 S2 avg
total bandwidth 0.17 0.27 0.22R 12.94 7.90 9.81
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CHARA 2014 Science & Technology Review
Evolution / dynamics• Dust production mechanism poorly understood• Close-in dust extremely short lived
≈ few yrs≈ 10-8 M⊕/yr to replenish
(10 Hale-Bopps per day)
• Destruction factors:– Sublimation– Radiation Pressure– Poynting-Robertson (P-R) drag
• Models:– Steady state/continuous replenishment– Steady state/trapped nano-grains [Su et al. (2013), Lebreton et al. (2013)]
– LHB & outgassing
time
Amount of
Dust105 years
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CHARA 2014 Science & Technology Review
Statistics, origin, and evolution Absil et al. Disk Survey
• Most common around A stars
Spectral type, age, metallicity, presence of cold dust
A F G-K Total
Cold disk 8 6 6 20No outer disk 4 7 9 19Unknown 0 2 0 2Total 12 15 15 42
Absil et al. 2013 (submitted)
42 stars A-K (mag limited)
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CHARA 2014 Science & Technology Review
54% 21% 14%0%
10%
20%
30%
40%
50%
60%
70%
A F GK
K-b
and e
xce
ss f
requen
cy
45% 16%0%
10%
20%
30%
40%
50%
60%
Outer reservoir No outer reservoir
K-b
and
ex
cess
fre
quen
cy
44% 75%50% 0%40% 0%0%
10%
20%
30%
40%
50%
60%
70%
80%
90%
100%
Outer reservoir No outer reservoir
K-b
and e
xce
ssfr
equen
cy
A stars
F stars
GK stars
Absil et al. 2013 (submitted)
Age or amount of available material?
• A stars: not clear if correlation with metallicity
• FGK stars lack warm dust due to ages > 1 Gyr
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CHARA 2014 Science & Technology Review
NASA Origins Program with Betrand Mennesson
• 3 year program: exozodi disk survey≈ 100 nearby MS stars20% long/short, rest only short baselines– hot dust (1000-1500K), expected in 25-30% of MS
systems• Goal: excesses at 0.5% level (5σ) for mK=5
– Determine grain properties, disk morphology, correlations b/t stellar properties
• Visibility precision to <0.1%
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CHARA 2014 Science & Technology Review
IRTF• SpeX
– 2-5 µm spectra– Followup to survey– Photosphere-subtracted SED slope– Cross-correlate with Interferometric data– Add constraints to dust disk models
• temperature, size of the dust grains, age estimate, composition, mass, albedo
– Look for spectroscopic debris disk markers
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CHARA 2014 Science & Technology Review
Future plans• CHARA AO
– Increased sensitivity– Fainter magnitude limit– More targets– On axis, small field of view AO
systems for each telescope.
• CHAMP – Full fringe tracking and locking
capability on all baselines.
• Spectral dispersion mode observations
• Integration with CHAMP• Further camera and
software improvements
for FLUOR
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CHARA 2014 Science & Technology Review
Complementary studies• Follow-up of gravitational
microlensing survey– Faint, 7th mag– Targets of opportunity– Alert network?
(Cassan 2012)
• CHEOPS(CHaracterizing ExOPlanet Satellite)
– Photometry of known exoplanethost stars
• Bright, low activity stars– Determine radii, dynamics, and
atmospheric properties• Investigate potential targets of EChO
transit space mission – 2022 launch– Feasibility study, full program requires
CHARA AO≈ 100 planetary spectra
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CHARA 2014 Science & Technology Review
References• Akeson et al. Dust in the inner regions of debris disks around
A stars. The Astrophysical Journal, Volume 691, Issue 2, pp. 1896-1908 (2009)
• Beichman et al. New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets. The Astrophysical Journal, Volume 652, Issue 2, pp. 1674-1693 (2006)
• Cassan et al. One or more bound planets per Milky Way star from microlensing observations. Nature, Volume 481, Issue 7380, pp. 167-169 (2012)
• Di Folco et al. A near-infrared interferometric survey of debris disk stars. I. Probing the hot dust content around ? Eridani and t Ceti with CHARA/FLUOR Astronomy and Astrophysics, Volume 475, Issue 1, November III 2007, pp.243-250 (2007)
• Exoplanets by Sara Seager. University of Arizona Press, 2011. ISBN: 978-0-8165-2945-2
• Gomes et al. Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets Nature, Volume 435, Issue 7041, pp. 466-469 (2005)
• Hanot et al. Improving Interferometric Null Depth Measurements using Statistical Distributions: Theory and First Results with the Palomar Fiber Nuller The Astrophysical Journal, Volume 729, Issue 2,110 (2011)
• Holland et al. Submillimetre images of dusty debris around nearby stars Nature, Volume 392, Issue 6678, pp. 788-791 (1998)
• http://www.cfa.harvard.edu/COMPLETE/learn/debris_disks/debris.html
• Kalas et al. Optical Images of an Exosolar Planet 25 Light-Years from Earth Science, Volume 322, Issue 5906, pp. 1345-
(2008)• Kuchner, Marc J.; Holman, Matthew J. The Geometry of
Resonant Signatures in Debris Disks with Planets The Astrophysical Journal, Volume 588, Issue 2, pp. 1110-1120 (2003)
• Lawler et al. Explorations Beyond the Snow Line: Spitzer/IRS Spectra of Debris Disks Around Solar-type Stars The Astrophysical Journal, Volume 705, Issue 1, pp. 89-111 (2009)
• Nesvorný et al. Cometary Origin of the Zodiacal Cloud and Carbonaceous Micrometeorites. Implications for Hot Debris Disks The Astrophysical Journal, Volume 713, Issue 2, pp. 816-836 (2010)
• O. Absil et al. Circumstellar material in the Vega inner system revealed by CHARA/FLUOR. AAP, 452:237244, (2006)
• Tsiganis et al. Origin of the orbital architecture of the giant planets of the Solar System Nature, Volume 435, Issue 7041, pp. 459-461 (2005)
• V. Coudé du Foresto, et al. FLUOR infrared beam combiner at the CHARA array. Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, volume 4838 SPIE conference, pages 280-285, February 2003.
• Wilner et al. Structure in the Dusty Debris around Vega The Astrophysical Journal, Volume 569, Issue 2, pp. L115-L119 (2002)
• Wyatt, Mark C. Evolutions of Debris Disks Annual Review of Astronomy & Astrophysics, vol. 46, Issue 1, pp.339-383 (2008)
• Wyatt, Mark C. Transience of hot Dust Around Sun-like Stars The Astrophysical Journal, Volume 658, pp. 569-583 (2007)
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CHARA 2014 Science & Technology Review
0
20
40
60
80
100
120
140
160
0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180 0 20 40 60 80 100 120 140 160 180
2b-0 2a-0 2b-90 2a-90
Photometry
BOTH_BEAMS Sig 1 BOTH_BEAMS Sig 2 BOTH_BEAMS Phot 1 BOTH_BEAMS Phot 2
-20
0
20
40
60
80
100
120
140
1600 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160 0 40 80 120
160
0-B 0-A 1b-0 1a-0 1b-90 1a-90 2b-0 2a-0 2b-90 2a-90 3-0 3-90
Photometry
SHUTTER_A Sig1 SHUTTER_A Sig2 SHUTTER_A Phot1 SHUTTER_A Phot2
SHUTTER_B Sig1 SHUTTER_B Sig2 SHUTTER_B Phot1 SHUTTER_B Phot2
BOTH_BEAMS Sig 1 BOTH_BEAMS Sig 2 BOTH_BEAMS Phot 1 BOTH_BEAMS Phot 2
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CHARA 2014 Science & Technology Review
CHARA systems interface
CHARA messages
server
Gtk clienthardware
Array systems
vpn
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CHARA 2014 Science & Technology Review
horizons
11.8963 % S2 obstruction8.83448 % W1 obstruction0.862847 % W2 obstruction6.49262 % E1 obstruction1.40250 % E2 obstruction
(solid angle above 20.0000 degrees)
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CHARA 2014 Science & Technology Review
Milestone(s)
Date Description
7/1/2011 Switch from LabView to C
9/29/2011 Remote obs setup
10/4/2011 1st remote run
2/1/2012 JouFLU hardware install
5/1/2012 First fringes
11/7/2012 CALI Meudon tests
12/19/2012 CALI CHARA tests
4/1/2013 CALI replaced w NICMOS
4/28/2013 FLUOR run-IA
5/5/2013 FLUOR run-IB
5/7/2013 Optimized MONA plz
5/14/2013 First on-sky fringes w NICMOS
5/29/2013 Moved MONA, NICMOS, & output
5/30/2013 Realigned OAPs
6/3/2013 FLUOR run-II
7/17/2013 Changed ZABER mode
8/14/2013 Re-centered fiber bundle
10/1/2013 FLUOR run-III
10/10/2013 FLUOR run-IV
2/17/2014 Switched to ethernet readout
2/18/2014 Spectral dispersion mode added
Timeline: 7/1/2011 - 2/18/2014