the 3-helium problem: constraining the chemical …dbalser/ppt/tmb_he3_umass.pdfhelium-3 conclusions...
TRANSCRIPT
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The 3-Helium Problem:Constraining the ChemicalEvolution of the Milky Way
TOM BANIAInstitute for Astrophysical Research
Department of AstronomyBoston University
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Light Elements as Baryometers
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Primordial Nucleosynthesis: BBNS
Burles et al. (2001)
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He: Optical recombination lines
Izotov et al. (1999)
Metal poor blue compact galaxies
4
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He Abundances
Olive & Skillman (2004) Peimbert & Peimbert (2002)Yp [mass] Reference
0.2421 (0.0021) Izotov & Thuan (2004)0.249 (0.009) Olive & Skillman (2004)0.2371 (0.0015) Peimbert & Peimbert (2002)
4
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Li: Resonance Line
Boesgaard et al. (2005)
Metal poorHalo stars
7
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Li: The Spite Plateau
Ryan et al. (2000)
Log(7Li/H) + 12 Reference
2.09 (+0.19,-0.13) Ryan et al. (2000)2.37 (0.1) Melendez & Ramirez (2004)2.44 (0.18) Boesgaard et al. (2005)
7
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Deuterium: Lyman series
Kirkman et al. (2003)
O’Meara et al. (2001)
Q1243+3047 HS 0105+1619
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Deuterium Abundances
Kirkman et al. (2003)Steigman (2005)
D/H 2.78 -0.380.44 10-5
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The 327 MHz Deuterium LineRogers, Dudevoir, Carter, Fanous, Kratzenberg, and Bania
2005, ApJ, 630, L41-44 (RDCFKB):“Deuterium Abundance in the Interstellar Gas of the Galactic Anticenter from
the 327 MHz Line” 92 cm wavelength
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Haystack Observatory, Westford, MA
Array: 24 stationsStation: 24 crossed Yagis Station Area: 12 m2
Station Beam: 14o
Beam Steering: +/- 40o
Frequency: 327.4 MHzBandwidth: 250 kHzChannels: 1024Resolution: 244 HzPolarization: Dual LinearSystem Temperature: 40 K + sky# Rx Ports: 48 x 24 = 1152
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D I Beam
Continuum
H I
Model D ISpectra
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Mar 2006L = 183o
L = 171o
BlankFields
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ANTICENTER D/H ABUNDANCE
* Spin Temperature Range: 100-150 K* Continuum Uniformly Distributed Along Line of Sight* 1 Sigma measurement errors
=> <D/H> = (2.0+/-0.5) x 10-5 <=for Rgal = (10+/-1) kpc
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3
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Stalking the Cosmic He Abundance3
Tom Bania (BU),Bob Rood (UVa),
Dana Balser (NRAO), Miller Goss (NRAO),
Cintia Quireza (ON, Brazil), Tom Wilson (MPIfR)
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He: Stellar Evolution
1 H 1 H 2 H+e Production2 H 1 H 3 He+ T 6 x 105 K
3 He 3 He 4 He+2 p Destruction3 He 4 He 7 T 7 x 106 K
Daniele Galli
1 H 1 H 2 H+e Production2 H 1 H 3 He+ T 6 x 105 K
3 He 3 He 4 He+2 p Destruction3 He 4 He 7 T 7 x 106 K
3
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He: Observations3
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He Hyperfine Transition
F=0 Singlet
F=1 Triplet
N=3
N=2
N=1
01 8665.65 MHz 3.46 cmA01 1.950 x 10 12 s 1 16 ,300 years
2 S1 2 F=0 1
3 +
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NRAO 140 ft MPIfR 100 m
H II Regions Planetary Nebulae (PNe)
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NRAO 140 Foot: HII Regions
Galactic HII Regions (1982 – 1999)
(~50)
Orion nebula (M42)Eagle nebula (M16)Rosette nebulaW49S209G0.60+0.32
HPBW = 3.5 arcmin
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3He+
H171ηinterference
G93.06+2.8 45.8 hr integration
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HII Region He Spectra Bania et al. (1997)
3 +
HII Region 3He+ Spectra+++
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Sharpless HII Regions Bania et al. (1997)
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Radio Recombination Lines Bania et al. (1997)
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200 Day Integration: 27 microKelvin RMS
He+3
H171 eta
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T = 50 Ksys
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He Abundance Determination3
OBSERVE THE EQUIVALENT WIDTHDERIVE THE ABUNDANCE
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H II Region Continuum Balser et al. (1995)
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H II Region Continuum
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H II Region Models Balser et al. (1999)
W43 S209
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Galli et al. (1995)
WMAP
“The He Problem”3
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“Simple” H II Regions
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Bania, Rood, & Balser 2002η10 = 5.4+2.2
-1.2ΩB = 0.04
Spergel et al. 2003, WMAPη10 = 6.5+0.4
-0.3ΩB = 0.047 ± 0.006
For D highest observed value is a lower limit for cosmological D
For 3He lowest observed 3He/H is an upper limit for cosmological 3He
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Bania, Rood & Balser (2002)
3He Abundance in H II Regions --““The The 33He PlateauHe Plateau””
WMAP(3He/H)p = 1.1 x 10-5
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BBNS CONSTRAINTSIzotov & Thuan (2004)Peimbert & Peimbert (2002)Olive & Skillman (2004)
Kirkman et al. (2003)
Bania, Rood, & Balser (2002)
Ryan et al. (2003)Boesgaard et al. (2006)
Burles et al. (2001)Spergel et al. (2006)
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MPIfR 100 m: PNe
Galactic Planetary Nebulae(1991 – 1995)
NGC 3242 (Eye)NGC 6543 (Cat’s Eye)NGC 6720 (Ring)NGC 7009 (Saturn)NGC 7662 (Blue Snowball)
HPBW = 80 arcsec
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NGC 3242: Eye Nebula
Balick et al.
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MPIfR 100 m PNe Survey Balser, et al. 1997, ApJ 483, 320
106 hr
443 hr
Composite: NGC 6543 + NGC 6720 + NGC 7009 + NGC 7662 + IC 289
He+3
1987-1997
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NGC 3242 Confirmation Balser, et al. 1999 ApJ 522, L73
He+3
H171 eta
NRAO 140 ft spectrum is a 270 hour integration
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Abundance versus [O/H]
Bania, Rood & Balser (2002)
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Abundance versus Rgal
Bania, Rood & Balser (2002)
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3He evolution with extra-mixing
protosolar
HII regions
3He/H x 105
Time (Gyr)
Tosi (1996)
70%
80%90%
100%
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Extra-Mixing Hypothesis
Charbonnel 1995 (see also Hogan 1995) : an extra-mixing mechanism acting during the RGB and/or AGB phases of stars with mass M 2 M can reduce the surface 3He abundance
Extra-mixing decreases the surface 12C/13C : the 3He problem is linked to other isotopic anomalies in RGB and AGB stars
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convective envelope
H-burning shellHe coresurface 3He destroyed
13C dredged-up
Mixing on the RGB
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Extra-mixing Process
Charbonnel (1995)
96% of low-mass stars
Charbonnel &do Nascimento (1998)
Extra-mixing
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No Mixing in NGC 3242
Balser et al. (1999) Palla et al. (2002)
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The rescue of the standard model
NGC 3242 (HST)
3He yes!
Rood, Bania & Wilson (1992)Balser, Rood & Bania (1999)
13C no!
Palla et al. (2002)
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3He abundance is a good test for cosmology, stellar evolution (standard and non-standard), and Galactic chemical evolutionSolving the 3-He Problem requires extra-mixing in ~ 90% of stars with M ~ 2 M
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One is not enough!
Except in cosmology
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The PN sample:PNe progenitor stars with no extra mixing:
4He / H < 0.125
[ N / O ] < -0.313C / 12C as low as possible
Oldest possible stellar population has highest 3-He:
Peimbert Class IIb, III, and IV
Helium is singly ionized
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Balser, Goss, Bania, Rood (2005)
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Jonckheere 320 – PN G190.3-17.7
J320
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VLA Planetary Nebula J320
3He / H abundance = 1.9 x 10 --33 by number\
Model
He3 +
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J320 3He+
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J320 Halo: 30 arcsec
Balser et al. (2006)
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NGC 6543
HST
ACS
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Balick, Wilson & Hajian (2001) AJ, 121, 354
NGC 6543: The Rings Around the Cat's Eye
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NGC 6720: Rings around the Ring
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Corradi et al. (2004) A&A,417, 637
Rings in the Haloes of Planetary Nebulae
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The Robert C. Byrd
GREEN BANK TELESCOPE
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Conventional
Blocked
Aperture
Is a very
Bad
Design
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Standing Waves and Multipath
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GBT: Clear Aperture Optics
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S 209 H II Region
140 ft March 1995 GBT June 2004
33.1 hr 3.2 hr
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GBT S 209 H II Region
14.5 hour integrationCalibrated Raw Spectrum
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DC Level Subtracted 15.1 hr integration
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S 209 H II Region
14.5 hour integration 5 km/sec resolution
He+3H171 eta
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GBT PNe Composite SpectrumNGC 3242 + NGC 6543 + NGC 6826 + NGC 7009
H171 eta
He3 +
125.7 hour integration
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NGC 7009 + NGC 6543 + NGC 6826
Composite PNe Spectrum 180.3 hr integration
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NGC 7009 H 91alpha 61.8 hr
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NGC 7009 H 92alpha 61.2 hrs
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NGC 7009 H 114beta 62.1 hrs
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NGC 7009 H130gamma 62.1 hrs
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Conclude reliability level for NGC7009 ~ 0.5 mK
NGC 7009 H 144delta 61.7 hrs
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This looks as real as He3but is much too strong
NGC 7009 H 171eta 3-He 62.1 hrs
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NAIC Arecibo Observatory 305 m
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3-Helium Experiment Status
• VLA He detection for PN J 320. It has a substantial halo, just as NGC 3242 does.
• Composite GBT PNe spectrum consistent with MPIfR 100 m survey result.
• Probable GBT He detection for NGC 7009 A second detection in NGC 6543 is likely.
• First epoch Arecibo observations complete.
3
3
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3-Helium Experiment Status
• 25% of all planetary nebulae meet our selection criteria. To be consistent with Galactic Chemical Evolution models, only 1/5 of these should show detectible He.
• The EVLA (10 times more sensitive than the VLA) has great potential.
• LMC/SMC campaign using Parkes planned. (Suprising perhaps, but feasible.)
3
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GBT Conclusions• Standing waves are not a problem
• There is still baseline structure (BS) probably resulting from the broadband feed, the polarizer, and or mismatches in the IF system.
BS varies with frequency sometimes almost invisible other times very problematic
BS amplitude is proportional to source continuum and moves with sky frequency
• At the mK level there are pseudo-lines
• In some AC bands there are short duration spikes in the ACF at seemingly random times, lags, and amplitudes
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Helium-3 Conclusions
• We have found helium-3 in another PN, J320, using the VLA
• We probably have found helium-3 in NGC7009 using the GBT and may have a second detection in NGC6543
• Roughly 25% of PNe meet our selection criteria. To avoid conflict with Monica we should detect 3He in only 1/5
• The scheduling mode and proposal pressure on the GBT may not allow us to solidify these results in the near future.
• The EVLA (10 x more sensitive than the VLA) has great potential
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NGC 7009 NGC 7354
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3-Helium Experiment Status
GBT now fully operational for 3-HeTwo GBT 3-He epochs complete Spectral baselines of excellent qualityComposite PNe spectrum consistent with MPIfR survey resultsVLA 3-He 4-sigma detection' for PN J320 (see Balser et al. poster)First epoch NAIC Arecibo Observatory observations complete
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Some days it’s chicken; some days it’s feathers
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NGC7009
NGC6826
NGC6543
Sum
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PNe: J320
Balser et al. (2006)
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Bania, Rood, & Balser 2002η10 = 5.4+2.2
-1.2ΩB = 0.04
Spergel et al. 2003, WMAPη10 = 6.5+0.4
-0.3ΩB = 0.047 ± 0.006
For D highest observed value is a lower limit for cosmological D
For 3He lowest observed 3He/H is an upper limit for cosmological 3He
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Bania, Rood, & Balser 2002η10 = 5.4+2.2
-1.2ΩB = 0.04
Spergel et al. 2003, WMAPη10 = 6.5+0.4
-0.3ΩB = 0.047 ± 0.006
For D highest observed value is a lower limit for cosmological D
For 3He lowest observed 3He/H is an upper limit for cosmological 3He
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Mixing and the 3He problem
Daniele Galli (INAF-Arcetri)Francesco Palla (INAF-Arcetri)Monica Tosi (INAF-Bologna)Federico Ferrini (Univ. Pisa)
Letizia Stanghellini (HST)Oscar Straniero (INAF-Teramo)
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A long standing problemRood, Steigman & Tinsley (1976)
Low-mass stars produce substantial amounts of 3He, enriching the ISM: X3 10-3
But the measured protosolar value is much lower: X3 10-5 problem!
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3He profile in a 1.25 M PopII star
Weiss, Wagenhuber & Denissenkov (1996)
ejected as a PN
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The “standard” 3He yields
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Theorists at work…
Wrong extrapolation of the 3He-3He nuclear cross section at low energies?
Pollution of winds from massive stars in HII
regions?
Continuous infall of primordial gas?
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Mixing takes over
Charbonnel 1995 (see also Hogan 1995) : an extra-mixing mechanism acting during the RGB and/or AGB phases of stars with mass M 2 M can reduce the surface 3He abundance
Extra-mixing decreases the surface 12C/13C : the 3He problem is linked to other isotopic anomalies in RGB and AGB stars
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convective envelope
H-burning shellHe coresurface 3He destroyed
13C dredged-up
Mixing on the RGB
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NGC7009
NGC6826
NGC6543
Sum
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He3 in S209 in only 7.5hr!
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A bonus: He++ or O++ RRL (a first?)
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Calibrating the mixing on the RGB
Charbonnel (1995)
0.8 M
Z=10-4
extra-mixing
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The “new” 3He yields
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NGC 3242
3He data from Balser et al. (1997, 1999)
stellar masses from Galli et al. (1997)
one more detection in a PN! (see poster by Balser et al.)
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Palla, Galli, Marconi, Stanghellini & Tosi (2002)
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Palla et al. (2000)
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Standard yields With mixing
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Bania, Rood & Balser (2002)
3He abundance in HII regions
(3He/H)p 1.1 10-5
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Bania, Rood, & Balser 2002
η10 = 5.4+2.2-1.2
ΩB = 0.04
Spergel et al. 2003, WMAP
η10 = 6.5+0.4-0.3
ΩB = 0.047 ± 0.006
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GBT Conclusions
• There is still baseline structure (BS) probably resulting from the broadband feed, the polarizer, and or mismatches in the IF system.
BS varies with frequency sometimes almost invisible other times very problematic
BS amplitude is proportional to source continuum and moves with sky frequency
• Standing waves are not a problem
• At the mK level there are pseudo-lines
• In some AC bands there are short duration spikes in the ACF at seemingly random times, lags, and amplitudes
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Jonckheere 320 – PN G190.3-17.7
J320
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NGC 6543
HST
ACS
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Balick, Wilson & Hajian (2001) AJ, 121, 354
NGC 6543: The Rings Around the Cat's Eye
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