-
NOEMA tutorials: II. HLS 091828by
Cinthya Herrera & Jérôme PETYIRAM
The datasets are not public as of Oct. 2018⇒ We tampered with
the datasets so that it’s impossible to do quantitative science
from them.Scripts for this tutorixal are available in the
following files
pro/hls091828-beginner.map,
pro/hls091828-beginner.class,pro/hls091828-beginner.clic, and
pro/hls091828-selfcal.map
The scripts assume that you use oct18 or a more recent version
of GILDAS
IRAM Millimeter Interferometry Summer SchoolOct. 1 - 5 2018, St
Martin d’Hères
-
Size of the problem: I. UV plane
From this slide on, please look into file
pro/hls091828-beginner.map
[imiss@reducv2 hls091828]$ ls -lh usb.uvt-rw-r----- 1 imiss
project 701M Sep 21 15:28 usb.uvtMAPPING> header usb.uvtFile :
usb.uvt REAL*4Size Reference Pixel Value Increment
12196 2003.18396625438 90200.0000000000 1.9999999988631314540
0.00000000000000 0.00000000000000 1.00000000000000
Blanking value and tolerance 1.23455997E+34 0.0000000Source name
HLS091828Map unit JyAxis type UV-DATA RANDOMCoordinate system
EQUATORIAL Velocity LSRRight Ascension 09:18:28.60000 Declination
51:42:23.3000Lii 0.000000000000000 Bii 0.000000000000000Equinox
2000.0000Projection type AZIMUTHAL Angle 0.000000000000000Axis 0 A0
09:18:28.60000 Axis 0 D0 51:42:23.3000Baselines 0.0 0.0Axis 1 Line
Name usb Rest Frequency 90200.00000000000Resolution in Velocity
-6.6471243 in Frequency 1.9999523Offset in Velocity 0.0000000
Doppler Velocity 7.1420060Beam 55.9 0.00 0.00NO Noise levelNO
Proper motionTel: NOEMA 05:54:28.5 44:38:02.0 Alt. 2560.0 Diam
15.0UV Data Channels: 4063, Stokes: 1 None Visibilities: 14540
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: II. Image plane
MAPPING> let name usbMAPPING> go setupMAPPING> go
setupInput file: Interferometer (15m) usb.uvt
Single field observation (14540 visibilities)
Observed rest frequency 90.2 GHzHalf power primary beam 55.9
arcsecPhase center RA and Dec 09:18:28.600 51:42:23.300Field of
view / Largest Scale 55.9 x 55.9 arcsec
Recommended UsedMap size 256 x 256 256 x 256 pixelsMap cell 0.78
x 0.78 0.78 x 0.78 arcsecImage Size 199.4 x 199.4 199.4 x 199.4
arcsec
Still to be imagedStill to be cleaned
⇒ One data cube will weight ∼ 1 GB!
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: III. Making a continuum image to check
the actual source size. 1. Original uv coverage
MAPPING> let name usbMAPPING> go uvcov
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: III. Making a continuum image to checkthe
source size. 2. New uv coverage
MAPPING> read uv usbMAPPING> uv_contMAPPING> write uv
usb-contMAPPING> let name usb-contMAPPING> go uvcov
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: III. Making a continuum image to check
the source size. 3. Creating the image
MAPPING> let name usb-contMAPPING> go uvmapI-CLEAN, Beam
is 5.00" by 3.81" at PA -6.97 deg.I-CLEAN, Errors ( 0.01) ( 0.01) (
0.41)MAPPING> go cleanMAPPING> go plot
⇒ Pixel size too small. Field of view too large.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: IV. Adapting
MAPPING> let map_size 64 ! [pixels]MAPPING> let map_cell
1.0 ! [arcsec]MAPPING> go uvmapMAPPING> go cleanMAPPING>
go plot
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
The source seems shifted ⇒ Fitting in the uv plane.I. One point
source
MAPPING> let name usb-cont ! Start fitting the
visibilitiesMAPPING> let uvfit%subsf01 yes ! => Subtracting
the fitted functionMAPPING> let uvfit%funct01 "point"MAPPING>
go uvfitr.m.s.= 0.3482 Jy.POINT R.A. = 0.19067 ( .01156)
09:18:28.62051POINT DEC. = 1.04334 ( .01618) 51:42:24.3433POINT
FLUX = 20.44669 ( .14281) milliJyMAPPING> pauseMAPPING> let
name usb-cont-res ! Start imaging and deconvolving the
residualsMAPPING> let map_size 64MAPPING> let map_cell
1.0MAPPING> go uvmapMAPPING> go cleanMAPPING> go plot
clean
⇒ The source is indeed shifted, but residuals donot look like
noise!
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Is it a point source? ⇒ Fitting in the uv plane.II. Circular
Gaussian
MAPPING> let name usb-contMAPPING> let uvfit%subsf01
yesMAPPING> let uvfit%funct01 "c_gauss"MAPPING> let
uvfit%range01 0 0 0 1 0 0 0MAPPING> let uvfit%start01 0 0 0 2 0
0 0MAPPING> go uvfitr.m.s.= 0.3482 Jy.C_GAUSS R.A. = 0.19259 (
.01286) 09:18:28.62072C_GAUSS Dec. = 1.03904 ( .01689)
51:42:24.3390C_GAUSS Flux = 22.93308 ( .23938) milliJyC_GAUSS
F.W.H.P. = 1.55518 ( .05997)Imaging and deconvolving the
residuals...
⇒ Larger flux. Residual improved but not yetcompletely
noise-like.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Is it a point source? ⇒ Fitting in the uv plane.III. Elliptical
Gaussian
MAPPING> let name usb-contMAPPING> let uvfit%subsf01
yesMAPPING> let uvfit%funct01 "e_gauss"MAPPING> let
uvfit%range01 0 0 0 1 1 0 0MAPPING> let uvfit%start01 0 0 0 2 2
0 0MAPPING> go uvfitr.m.s.= 0.3482 Jy.E_GAUSS R.A. = 0.19137 (
.01260) 09:18:28.62059E_GAUSS Dec. = 1.03947 ( .01732)
51:42:24.3395E_GAUSS Flux = 23.25760 ( .24733) milliJyE_GAUSS Major
= 2.12268 ( .08142)E_GAUSS Minor = 1.13933 ( .10087)E_GAUSS
Pos.Ang. = 32.17092 ( 3.67679)Imaging and deconvolving the
residuals...
⇒Still larger flux and residual completelynoise-like.
⇒ Source slightly resolved.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: V. Getting back to the original uv
table
MAPPING> let name usbMAPPING> let map_size 64 !
[pixels]MAPPING> let map_cell 1.0 ! [arcsec]MAPPING> go
uvmapMAPPING> let fres 0MAPPING> let niter 100MAPPING> go
cleanMAPPING> go plot res
⇒ One data cube will weight ∼ 64 MB!
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: V. Getting back to the original uv
table
MAPPING> let name usbMAPPING> let map_size 64 !
[pixels]MAPPING> let map_cell 1.0 ! [arcsec]MAPPING> go
uvmapMAPPING> let fres 0MAPPING> let niter 100MAPPING> go
cleanMAPPING> go plot clean
⇒ Spectral resolution is too narrow to get good signal-to-noise
ratio.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Size of the problem: VI. Compressing the spectral axis
MAPPING> read uv usbMAPPING> uv_compress 15 ! To get 100
km/s-wide channelsMAPPING> write uv usb-compMAPPING> let name
usb-compMAPPING> let map_size 64 ! [pixels]MAPPING> let
map_cell 1.0 ! [arcsec]MAPPING> go uvmapMAPPING> let fres
0MAPPING> let niter 100MAPPING> go cleanMAPPING> go plot
clean
⇒ Spectral resolution is now OK.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Let’s center the source
MAPPING> read uv usb-compMAPPING> uv_shift 0.19 1.04 !
[arcsec]MAPPING> write uv usb-comp-shiftMAPPING> let name
usb-comp-shiftImaging and deconvolution...
⇒ Now it’s centered.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Let’s check the convergence of the deconvolution
MAPPING> let name usb-compMAPPING> go cct
⇒ Convergence is OK on channels where the line are.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Imaging the continuum: I. Before setting a 100 km/s
velocityrange around each line to zero
MAPPING> read uv usb-comp-shiftMAPPING> uv_filter /zero
/frequency 89217.523 92356.280 /width 1500 veloMAPPING> write uv
usb-comp-shift-filtImaging and deconvolution...
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Imaging the continuum: I. After setting a 100 km/s velocityrange
around each line to zero
MAPPING> read uv usb-comp-shiftMAPPING> uv_filter /zero
/frequency 89217.523 92356.280 /width 1500 veloMAPPING> write uv
usb-comp-shift-filtImaging and deconvolution...
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Imaging the continuum:
II. From a line uv table to a continuum uv table
MAPPING> read uv usb-comp-shift-filtMAPPING>
uv_contMAPPING> write uv usb-comp-shift-filt-contImaging and
deconvolution...
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Imaging the continuum:
III. Fitting again in the uv plane as a check
MAPPING> let name usb-comp-shift-filtMAPPING> let
uvfit%subsf01 yesMAPPING> let uvfit%funct01 "e_gauss"MAPPING>
let uvfit%range01 0 0 0 1 1 0 0MAPPING> let uvfit%start01 0 0 0
2 2 0 0MAPPING> go uvfitr.m.s.= 0.2442 Jy.E_GAUSS R.A. = 0.00989
( .01546) 09:18:28.62150E_GAUSS Dec. = 0.01090 ( .02123)
51:42:24.3509E_GAUSS Flux = 19.89969 ( .25953) milliJyE_GAUSS Major
= 2.10059 ( .10067)E_GAUSS Minor = 1.14766 ( .12325)E_GAUSS
Pos.Ang. = 32.18221 ( 4.67377)
⇒ It’s well centered.
⇒ The lines represented 17% of the actual flux (= 100× (23.26−
19.90)/19.90).
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Getting the lines in the LSB band
MAPPING> read uv lsbMAPPING> uv_comp 15MAPPING>
uv_shift 0.19 1.04MAPPING> uv_base 1 /frequency 72697 73889
78776 /width 1500 veloMAPPING> write uv
lsb-comp-shift-baseMAPPING> let name lsb-comp-shift-baseImaging
and deconvolution ...
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Getting the continuum in the LSB bandMAPPING> read uv
lsbMAPPING> uv_shift 0.19 1.04MAPPING> uv_filter /frequency
72697 73889 78776 /width 1500 veloMAPPING> uv_cont 15MAPPING>
write uv lsb-shift-filt-contMAPPING> let name
lsb-shift-filt-contImaging and deconvolution ...MAPPING> let
name lsb-shift-filt-contMAPPING> let uvfit%subsf01
yesMAPPING> let uvfit%funct01 "e_gauss"MAPPING> let
uvfit%range01 0 0 0 1 1 0 0MAPPING> let uvfit%start01 0 0 0 2 2
0 0MAPPING> go uvfitr.m.s.= 0.8856 Jy.E_GAUSS R.A. = 0.02668 (
.03837) 09:18:28.62331E_GAUSS Dec. = -0.04986 ( .05593)
51:42:24.2901E_GAUSS Flux = 11.27741 ( .31510) milliJyE_GAUSS Major
= 2.56787 ( .27767)E_GAUSS Minor = 1.55842 ( .23012)E_GAUSS
Pos.Ang. = -164.18299 ( 10.00366)
⇒ The source size appears bigger at lowerfrequency, but this is
within the 3σ confidence
interval.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Going to CLASS: I. Importing and plotting the central
spectrum
From this slide on, please look into file
pro/hls091828-beginner.class
LAS> transpose lsb-comp-shift-base.lmv-clean
lsb-comp-shift-base.vlm-clean 312LAS> file in
lsb-comp-shift-base.vlm-cleanLAS> set match 0.5 ! [arcsec]
position toleranceLAS> find /offset 0 0LAS> listLAS> get
firstLAS> plot
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Going to CLASS: II. Zooming in and baselining
LAS> set mode x 73200 74600 ! [MHz]LAS> plotLAS> set
window -1300 -450 ! [MHz] relative to the rest frequencyLAS>
draw windowLAS> base 0 /plot
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Going to CLASS: III. Gaussian fitting. 1. One line
LAS> method gaussLAS> lines 1 "0 0.1 0 -800 0 200"LAS>
minimizeLAS> iterateObservation 2081 RMS of Residuals : Base =
4.38E-03 Line = 1.69E-02
Bad fitLine Area Position Width Tpeak1 22.178 ( 0.498) -921.789
( 2.267) 195.808 ( 5.123) 0.10641LAS> visualize
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Going to CLASS: III. Gaussian fitting. 1. One line
LAS> residualLAS> plot
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Going to CLASS: III. Gaussian fitting. 2. Two lines
LAS> method gaussLAS> lines 2 "0 0.1 0 -950 0 120" "0 0.1
0 -800 0 70"LAS> minimizeLAS> iterateObservation 2081 RMS of
Residuals : Base = 4.60E-03 Line = 6.89E-03
Fit resultsLine Area Position Width Tpeak1 15.923 ( 0.506)
-946.268 ( 1.784) 119.170 ( 4.530) 0.125522 5.4585 ( 0.448)
-815.051 ( 2.486) 72.866 ( 6.825) 7.03756E-02LAS> visualize
⇒ Frequency in LSR frame of line #1:73854 MHz (= 74800− 946)
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Going to CLASS: III. Gaussian fitting. 2. Two lines
LAS> residualLAS> plot
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Going to CLASS: IV. Same steps for the USB bandLAS> transpose
usb-comp-shift-base.lmv-clean usb-comp-shift-base.vlm-clean
312LAS> file in usb-comp-shift-base.vlm-cleanLAS> set match
0.5LAS> find /offset 0 0LAS> listLAS> get firstLAS> set
mode x 91400 93300LAS> set window 1700 2600LAS> plotLAS>
draw windowLAS> base 0 /plotLAS> plotLAS> method
gaussLAS> lines 2 "0 0.1 0 2100 0 150" "0 0.1 0 2300 0
70"LAS> minimizeLAS> iterateObservation 2081 RMS of Residuals
: Base = 3.63E-03 Line = 7.81E-03
Fit resultsLine Area Position Width Tpeak1 23.387 ( 0.421)
2111.136 ( 1.305) 153.958 ( 3.410) 0.142712 6.1800 ( 0.328)
2270.643 ( 1.555) 69.653 ( 4.245) 8.33521E-02LAS> visualize
⇒ Frequency in LSR frame of line #1:92311 MHz (= 90200 +
2111)
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Science results: I. Redshift
Redshift radio νLSR =νrest1+z⇒ z = ν
2rest−ν1
rest
ν2LSR−ν1
LSR
− 1.
Measures
• CO line #1 is observed at frequency 73854± 2 MHz.• CO line #2
is observed at frequency 92311± 1 MHz.• ν2LSR − ν
1LSR = 18457±??? MHz.
Line catalogs
• CO(1-0): 115271.2018 MHz.• CO(2-1): 230538.0000 MHz.• CO(3-2):
345795.9899 MHz.• CO(4-3): 461040.7682 MHz.• CO(5-4): 576267.9305
MHz.• CO(6-5): 691473.0763 MHz.
Results
• If CO(2-1) and CO(1-0), ν2rest − ν1rest = 115266.7982 MHz and
z = 5.245153.
• If CO(3-2) and CO(2-1), ν2rest − ν1rest = 115257.9899 MHz and
z = 5.244676.
• If CO(4-3) and CO(3-2), ν2rest − ν1rest = 115244.7783 MHz and
z = 5.243960.
• If CO(5-4) and CO(4-3), ν2rest − ν1rest = 115227.1623 MHz and
z = 5.243006.
• If CO(6-5) and CO(5-4), ν2rest − ν1rest = 115205.1458 MHz and
z = 5.241813.
⇒ z = 5.2431 and the lines are CO(4-3) and CO(5-4).
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Science results: II. Continuum power spectrum index
Power spectrum F (ν) = F (νref)(
ννref
)α⇒ α = ln(F2)−ln(F1)
ln(ν2)−ln(ν1) .
Measures
• Continuum flux at (74 800× z =) 466 984 MHz: 11.27± 0.31 mJy.•
Continuum flux at (90 200× z =) 563 128 MHz: 19.90± 0.26 mJy.
Result α = 3.04.
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Producing the UV tables in CLIC: I. Tuning CLIC defaults
From this slide on, please look into file
pro/hls091828-beginner.clic
CLIC> set default ! Reset all global settings to their
natural defaultCLIC> set rf_passband on frequency antenna
fileCLIC> show rf_passband
RF Passband Calibration is appliedRF Passband Calibration is
frequency dependentRF Passband Calibration is antenna-basedRF
Passband Calibration from input file
CLIC> set phase relative antenna internal atmosphereCLIC>
show phase
Phases are relative to calibrator phasePhase Calibration is
antenna-basedPhase reference is internal (same receiver)Using
real-time atmospheric phase correction, antennas 1 2 3 4 5 6 7 8 9
:(according to validation by STORE CORRECTION)Using no off-line
atmospheric phase correction, antennas 1 2 3 4 5 6 7 8 9 :
CLIC> set amplitude relative antenna janskyCLIC> show
amplitude
Amplitudes are relative to calibrator amplitudeAmplitude
Calibration is antenna-basedAmplitudes are expressed in janskys
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Producing the UV tables in CLIC: II. Looking at the
frequencysetup
CLIC> sic log ipb_data: "./" ! Tell CLIC the directory where
IPB files are.CLIC> file in 10-jan-2018-d17sa001.hpbCLIC>
show file
Input file 10-jan-2018-d17sa001.hpb [Native]No output file
openedRaw data files are searched in:
./CLIC> find /proc corr /source hls091828 /offset 0 0CLIC>
if (found.ne.0) thenCLIC> listCLIC> get firstCLIC> header
/plotCLIC> endif
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Producing the UV tables in CLIC: III. Doing itCLIC> if
(found.ne.0) thenCLIC> set selection line LSB L1 and L2 and L5
and L6CLIC> set drop 0.002 0 ! Drop channels at edges of the
basebands (low resolution spectral windows)CLIC> sic delete
lsb.uvtCLIC> table lsb.uvt new /freq lsb 74800CLIC>
endifCLIC> $ls -ltrh-rw-r----- 1 imiss project 268M Sep 11 18:45
10-jan-2018-d17sa001.hpb-rw-r----- 1 imiss project 6.5G Sep 11
18:48 180110D17SA001.IPB-rw-r----- 1 imiss project 700M Sep 27
13:35 lsb.uvtCLIC> v\header lsb.uvtFile : lsb.uvt REAL*4Size
Reference Pixel Value Increment
12193 2047.00031853482 74801.7816622237 1.9999999988631314540
0.00000000000000 0.00000000000000 1.00000000000000
Blanking value and tolerance 1.23455997E34 0.0000000Source name
HLS091828Map unit JyAxis type UV-DATA RANDOMCoordinate system
EQUATORIAL Velocity LSRRight Ascension 09:18:28.60000 Declination
51:42:23.3000Lii 0.000000000000000 Bii 0.000000000000000Equinox
2000.0000Projection type AZIMUTHAL Angle 0.000000000000000Axis 0 A0
09:18:28.60000 Axis 0 D0 51:42:23.3000Baselines 0.0 0.0Axis 1 Line
Name lsb Rest Frequency 74800.00000000000Resolution in Velocity
-8.0156507 in Frequency 1.9999523Offset in Velocity 0.0000000
Doppler Velocity 0.0000000Beam 67.4 0.00 0.00NO Noise levelNO
Proper motionUV Data Channels: 4062, Stokes: 1 None Visibilities:
14540
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Phase self-calibration of the continuum:I. Get a correctly
imaged, deconvolved, and analyzed data
From this slide on, please look into file
pro/hls091828-selfcal.map
MAPPING> read uv lsbMAPPING> uv_shift 0.19 1.04MAPPING>
uv_filter /frequency 73889 78776 /width 1500 veloMAPPING>
uv_contMAPPING> write uv lsb-shift-filt-contMAPPING> let name
lsb-shift-filt-contMAPPING> let map_size 256MAPPING> let
map_cell 0.89MAPPING> go uvmapMAPPING> let ares 0MAPPING>
let fres 0MAPPING> let niter 30MAPPING> go cleanMAPPING>
go noise
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Phase self-calibration of the continuum:
I. Get a correctly imaged, deconvolved, and analyzed data
MAPPING> @ deconvolution-toolsMAPPING> @ deconv-plot 0
0
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Phase self-calibration of the continuum:
II. A bit of preparation
begin procedure
my-selfcal!---------------------------------------------------------------------------!
This procedure sets reasonable defaults for the self-calibration
tool.! It then executes the self-calibration and plot the result.!
&1: uv table name without extension! &2: number of selfcal
iteration! &3: number of clean components during each selfcal
step in double quote! for instance, "10 15" 10 and then 15 clean
components.! &4: Integration time used during each selfcal step
in double quote! for instance, "180 45" means 180 and then 45
seconds.!---------------------------------------------------------------------------let
self%iname &1 ! input uv tablelet self%oname &1-selfcal !
output uv tablelet self%loop &2 ! number of self cal loopslet
self%niter &3 /resize ! number of selected componentslet
self%times &4 /resize ! integration time for solutionlet
self%channel 0 0 ! channel rangelet self%refant 0 ! reference
antennalet self%sname &1-sol ! solution tablelet self%flux 0 !
maximum flux for displaylet self%restore no ! use uv_restore at
endlet self%display yes ! display clean image at each loopgo
selfcal@ deconv-plot 0 0ha ha/lsb-after-selfcal-plot-’niter’ /dev
epdf /overpause
end procedure my-selfcal
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Phase self-calibration of the continuum:
III. Before self-calibration
MAPPING> let name lsb-shift-filt-contMAPPING> let niter
30MAPPING> go cleanMAPPING> @ deconv-plot 0 0
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Phase self-calibration of the continuum:
III. During self-calibration
MAPPING> let name lsb-shift-filt-contMAPPING> @ my-selfcal
lsb-shift-filt-cont 2 "10 15" "180 45"MAPPING>MAPPING>
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018
-
Phase self-calibration of the continuum:
III. After self-calibration
MAPPING> let name lsb-shift-filt-cont-selfcalMAPPING> let
niter 30MAPPING> go cleanMAPPING> @ deconv-plot 0 0
NOEMA tutorials: II. HLS 091828 C. Herrera & J. Pety
2018