fr´ed´eric gueth, iram grenoble 8th iram millimeter ... · large-field imaging fr´ed´eric...
TRANSCRIPT
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Large-field imaging
Frederic Gueth, IRAM Grenoble
8th IRAM Millimeter Interferometry School15–19 October 2012
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Large-field imagingThe problems
• The field of view is limited by the antenna primary beam width
Solution: observe a mosaic = several adjacent overlapping fields
• The field of view is limited because of the “2D approximation”
Solution: use appropriate algorithm if necessary
• The largest structures are filtered out due to the lack of the short spacings
Solution: add the short spacing information
• Deconvolution algorithms are not very good at recovering small- and large-scale
structures
Solution: try Multi-Scale CLEAN...
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MosaicsInterferometer field of view
Measurement equation of an interferometric observation:
F = D ∗ (B× I) + N
F = dirty map = FT of observed visibilities
D = dirty beam (−→ deconvolution)
B = primary beam = FT of transfert function
I = sky brightness distribution = FT of “true” visibilities
N = noise distribution
• An interferometer measures the product B× I
• B ∼ Gaussian −→ primary beam correction possible (proper estimate of the
fluxes) but strong increase of the noise
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MosaicsPrimary beam width
Gaussian illumination =⇒ B ∼ Gaussian Beam of 1.2λ/D FWHM
Plateau de Bure
D = 15 m
Frequency Wavelength Field of View
85 GHz 3.5 mm 58′′
100 GHz 3.0 mm 50′′
115 GHz 2.6 mm 43′′
150 GHz 2.0 mm 33′′
230 GHz 1.3 mm 22′′
345 GHz 0.8 mm 15′′
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MosaicsMosaicing with the PdBI
Mosaic :
• Field spacing = half the primary beam FWHM = 11′′ at 230 GHz
Observations :
• Fields are observed in a loop, each one during a few minutes −→ similar
atmospheric conditions (noise) and similar uv coverages (dirty beam,
resolution) for all fields
Calibration :
• Procedure identical with any other observation (only the calibrators are used)
• Produce one dirty map per field
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MosaicsMosaic reconstruction
• Forgetting the effects of the dirty beam:
Fi = Bi × I + Ni
• This is similar to several measurements of I , each one with a “weight” Bi
• Best estimate of I in least-square formalism (assuming same noise):
J =
∑iBi Fi∑iB2
i
• J is homogeneous to I , i.e. the mosaic is corrected for the primary beam
attenuation
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MosaicsNoise distribution
J =
∑iBi Fi∑iB2
i
=⇒ σJ = σ1√∑
Bi2
The noise depends on the position and strongly
increases at the edges of the field of view
In practice :
• Use truncated primary beams (Bmin = 0.1− 0.3) to avoid noise
propagation between adjacent fields
• Truncate the mosaic
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MosaicsNoise distribution
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MosaicsMosaic deconvolution
• Linear mosaicing: deconvolution of each field, then mosaic reconstruction
Non-linear mosaicing: mosaic reconstruction, then global deconvolution
• The two methods are not equivalent, because the deconvolution algorithms are
(highly) non-linear
• Non-linear mosaicing gives better results
• sidelobes removed in the whole map
• better sensitivity
• Plateau de Bure mosaics: non-linear joint deconvolution based on
CLEAN
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MosaicsExample
(Gueth & Guilloteau 1999)
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MosaicsExample
(Gueth & Guilloteau 1999)
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CO 1–0 in TT Cygni, Olofsson et al. 2000
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CO 1–0 in TT Cygni, Olofsson et al. 2000
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CO in the warped galaxy NGC 3718 (Krips et al. 2005)
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(Stanke et al. 2004)
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(Pety et al. 2005)
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Short SpacingsLack of the short spacings
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Short SpacingsLack of the short spacings
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Short SpacingsLack of the short spacings
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Short SpacingsLack of the short spacings
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Short SpacingsLack of the short spacings
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Short SpacingsThe problem
Missing short spacings :
• Shortest baseline Bmin = 24 m at Plateau de Bure
• Projection effects can reduce the minimal baseline – but baselines smaller than
antenna diameter D can never be measured
• In any case: lack of the short spacings information
Consequence :
• The most extended structures are filtered out
• The largest structures that can be mapped are ∼ 2/3 of the primary beam
(field of view)
• Structures larger than ∼ 1/3 of the primary beam may already be affected
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Short SpacingsExample
13CO (1–0) in the L 1157 protostar (Gueth et al. 1997)
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Short SpacingsSimulations
Simulations of small source
+ extended cold/warm
layer with narrow line
emission
Lack of short spacings can
introduce complex arti-
facts leading to wrong
scientific interpreta-
tion
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Short SpacingsSpatial frequencies
• A single-dish of diameter D is sensitive to spatial frequencies from 0 to D
• An interferometer baseline B is sensitive to spatial frequencies from B−D to
B + D
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Short SpacingsSpatial frequencies
• A single-dish of diameter D is sensitive to spatial frequencies from 0 to D
• An interferometer baseline B is sensitive to spatial frequencies from B−D to
B + D
• An inteferometer measures the product primary beam × sky
• In the uv plane: transfert function ∗ true visibilities
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Short SpacingsMeasurements
An interferometer measures the convolution of the
“true” visibility with the antenna transfert function
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Short SpacingsMeasurements
No short-spacings
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Short SpacingsMeasurements
Single-dish measurement (same antenna diameter)
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Short SpacingsMeasurements
Interferometer with smaller antennas
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Short SpacingsMeasurements
Small interferometer + Single-dish measurement
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Short SpacingsMeasurements
Single-dish measurement (larger antenna diameter)
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Short SpacingsShort spacings from SD data
• Combine SD and Interferometric maps in the image plane
• Joint deconvolution (MEM or Multi-scale CLEAN)
• Hybridization (aka feather): Combine SD and Interferometric maps in the uv
plane
• Combine data in the uv plane before imaging
1. Use the 30–m map to simulate what would have observed the PdBI, i.e. extract
“pseudo-visibilities”
2. Merge with the interferometer visibilities
3. Process (gridding, FT, deconvolution) all data together
This drastically improves the deconvolution
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Short SpacingsExtracting visibilities
SD map = SD beam ∗ Sky
Int. map = Dirty beam ∗ (Int beam × Sky)
• Image plane Gridding of the single-dish data −→ SD Beam ∗ Sky
• uv plane Correction for single-dish beam −→ Sky
• Image plane Multiplication by interferometer primary beam −→ Int Beam × Sky
• uv plane Extract visibilities up to DSD −DInt
• uv plane Apply a weighting factor before merging with the interferometer
data
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Short SpacingsExtracting visibilities
Weighting factor to SD data :
• Produce different images and dirty beams
• Methods are not perfect, noise −→ weight to be optimized
• Usually, it is better to downweight the SD data (as compared to natural
weight)
Optimization :
• Adjust the weights so that there is almost no negative sidelobes while
keeping the highest angular resolution possible
• Adjust the weights so that the weight densities in 0–D and D–2D areas
are equal −→ mathematical criteria
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Short spacingsExample
13CO (1–0) in the L 1157 protostar (Gueth et al. 1997)
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Short spacingExample
N2H+ in the IRAM 04191 protostar (Belloche et al. 2004)
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Short spacingExample
CO 1–0 in the direction of NRAO 530, Pety et al. 2008
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Mosaics and short spacingsThe problem
Effect of missing short spacings more severe on mosaics than on single-field images:
• Extended structures are filtered out in each field
• Lack of information on an intermediate scale as compared to the mosaic size
• Possible artefact: extended structures split in several parts
• In most cases cases, adding the short spacings is required
However, mosaics are able to recover part of the short spacings information
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Mosaics and short spacingsSimulations
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Mosaics and short spacingsThe problem
Effect of missing short spacings more severe on mosaics than on single-field images:
• Extended structures are filtered out in each field
• Lack of information on an intermediate scale as compared to the mosaic size
• Possible artefact: extended structures split in several parts
• In most cases cases, adding the short spacings is required
However, mosaics are able to recover part of the short spacings
information
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Mosaics and short spacingsImage formation
• An interferometer is sensitive to all spatial frequencies from B–D to B+D =⇒ it
measures a local average of the “true” visibilities
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Mosaics and short spacingsImage formation
• An interferometer is sensitive to all spatial frequencies from B–D to B+D =⇒ it
measures a local average of the “true” visibilities
• Measured visibilities: Vmes = FT(B × I) = T ∗V where T is the transfert function
of the antenna
• Pointing center (`p, mp) 6= Phase center: phase gradient across the antenna aperture
Vmes(u, v) =[T (u, v) e−2iπ(u`p+vmp)
]∗ V (u, v)
• Combination of measurements at different (`p, mp) should allow to
derive V
• The recovery algorithm is a simple Fourier Transform (Ekers & Rots)
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Conclusions
• Mosaicing is a standard observing mode at Plateau de Bure
• Adding short spacings from the IRAM 30–m is an standard procedure (box in
proposal form)
• ALMA designed from the beginning to include the short-spacings (ACA, SD
antennas) – but not for all projects
• New developments to come: on-the-fly interferometry