# Difference between revisions of "Full Disk Simulations"

(→Creating Disk Models in CASA) |
(→Estimating disk axes and flux density from the data) |
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One can use the data themselves to estimate the size of the disk needed to fit the data. As it turns out, EOVSA visibilities provide excellent measures of the disk shape and flux density if we can make use of it. After a lot of effort, I believe we have an understanding of how to interpret the EOVSA visibilities in terms of the disk shape and flux density, and therefore how to fit the data to derive estimates for the three key parameters: equatorial radius, polar radius, and flux density. In practice, the flux density seems to fit quite well with the flux density imposed by the total power/auto-correlation calibration, so it is likely that we will do better just using the nominal flux density imposed from RSTN. Figure 1 shows an example of some data for 2019 Sep 01. [[file:Disk_vis.png|thumb|right|500px|'''Fig. 1:''' Example all-day visibilities for baselines 1-*, showing the periodic nulls due to the solar disk.]] | One can use the data themselves to estimate the size of the disk needed to fit the data. As it turns out, EOVSA visibilities provide excellent measures of the disk shape and flux density if we can make use of it. After a lot of effort, I believe we have an understanding of how to interpret the EOVSA visibilities in terms of the disk shape and flux density, and therefore how to fit the data to derive estimates for the three key parameters: equatorial radius, polar radius, and flux density. In practice, the flux density seems to fit quite well with the flux density imposed by the total power/auto-correlation calibration, so it is likely that we will do better just using the nominal flux density imposed from RSTN. Figure 1 shows an example of some data for 2019 Sep 01. [[file:Disk_vis.png|thumb|right|500px|'''Fig. 1:''' Example all-day visibilities for baselines 1-*, showing the periodic nulls due to the solar disk.]] | ||

− | The first 15 zeros of the airy disk are listed as: | + | The visibilities due to the solar disk are the same as the Fourier Transform of a circular aperture, which is an Airy pattern (not an Airy function, which apparently is a different mathematical function). The power distribution vs. radius in an Airy disk is <math>P = P_0 \bigg({2J_1(z) \over z}\bigg)^2</math>, where <math>J_1(z)</math> is the first-order Bessel function and <math>P_0</math> is the peak intensity. However, in the uv-plane we are looking not at the power, but rather the electric field pattern itself, hence we are interested in the square root of this function, i.e. |

+ | <math>I = I_0 \bigg({2J_1(z) \over z}\bigg)</math>. Note that the first 15 zeros of the airy disk are listed as: | ||

m = array([ 1.21967, 2.23313, 3.23831, 4.24106, | m = array([ 1.21967, 2.23313, 3.23831, 4.24106, | ||

5.24276, 6.24392, 7.24476, 8.24539, | 5.24276, 6.24392, 7.24476, 8.24539, | ||

9.24589, 10.24629, 11.24662, 12.24689, | 9.24589, 10.24629, 11.24662, 12.24689, | ||

13.24713, 14.24733, 15.24750]) | 13.24713, 14.24733, 15.24750]) | ||

− | + | which must correspond to the nearly periodic dips (nulls) in Figure 1. From which the diameter of the solar disk, in arcsec, is found from the location of the ''i''th minimum, in uv wavelengths <math>s_{\lambda,i}</math> as | |

<math>D^{''} = 206265 {m_i \over \pi s_{\lambda,i}}</math>. | <math>D^{''} = 206265 {m_i \over \pi s_{\lambda,i}}</math>. |

## Revision as of 23:31, 8 September 2019

# Purpose

EOVSA's 13 antennas provide limited uv coverage for imaging the solar disk, but the baselines do contain considerable flux, especially on shorter baselines. We have good evidence that weak features of the quiet Sun (e.g. filament channels, prominences, and weak plage areas) do show up in the data, but the variations in brightness due to the poorly sampled disk often swamp them. The correct approach to imaging such features is to model the quiet solar disk and remove it from the uv data. then clean the residual flux that contains these weaker features, and finally add the disk model back. Self calibration also requires a good source model that includes the disk.

The purpose of this page is to describe the nuts and bolts of that procedure and document the performance.

**NB: Since we are just getting started with this procedure, this page will initially present a number of tests. Ultimately it should become a definitive description of the procedure without a lot of false starts.**

# Creating Disk Models in CASA

The first step in simulating a source is to create a "sky model," which is an image and associated descriptive header information to represent a source in the sky. CASA's componentlist routines provide a recipe for creating different image components, including gaussian sources, point sources, disks, and so on. I created a python script diskmodel.py that eases the work of creating a disk model, which allows one to create a disk with unequal axes (generally larger in the equatorial axis and smaller in the polar axis). However, before it can be used one must have a good idea of the disk size and flux density of the disk.

## Estimating disk axes and flux density from the data

One can use the data themselves to estimate the size of the disk needed to fit the data. As it turns out, EOVSA visibilities provide excellent measures of the disk shape and flux density if we can make use of it. After a lot of effort, I believe we have an understanding of how to interpret the EOVSA visibilities in terms of the disk shape and flux density, and therefore how to fit the data to derive estimates for the three key parameters: equatorial radius, polar radius, and flux density. In practice, the flux density seems to fit quite well with the flux density imposed by the total power/auto-correlation calibration, so it is likely that we will do better just using the nominal flux density imposed from RSTN. Figure 1 shows an example of some data for 2019 Sep 01.The visibilities due to the solar disk are the same as the Fourier Transform of a circular aperture, which is an Airy pattern (not an Airy function, which apparently is a different mathematical function). The power distribution vs. radius in an Airy disk is , where is the first-order Bessel function and is the peak intensity. However, in the uv-plane we are looking not at the power, but rather the electric field pattern itself, hence we are interested in the square root of this function, i.e. . Note that the first 15 zeros of the airy disk are listed as:

m = array([ 1.21967, 2.23313, 3.23831, 4.24106, 5.24276, 6.24392, 7.24476, 8.24539, 9.24589, 10.24629, 11.24662, 12.24689, 13.24713, 14.24733, 15.24750])

which must correspond to the nearly periodic dips (nulls) in Figure 1. From which the diameter of the solar disk, in arcsec, is found from the location of the *i*th minimum, in uv wavelengths as

.

So the different minima will give different estimates and the final size would have to be some sort of mean of them. In some comparisons with the data, I do find that there is a systematic trend for the diameter to get smaller for larger *m*. One possibility that I explored is whether a fuzzy disk has different minima than a sharply defined disk, but this does not seem to be the case.