deletions | additions       diff --git a/subsection_Source_detection_Introduce_that__.tex b/subsection_Source_detection_Introduce_that__.tex  index 5fd96a0..24da6a4 100644  --- a/subsection_Source_detection_Introduce_that__.tex  +++ b/subsection_Source_detection_Introduce_that__.tex 
...
\subsection{Source detection}  All images examined were from the Hubble Space Telescope's MAST archive, using different filters and cameras for each galaxy depending upon availability of data; Filter and camera choice for each galaxy is shown in Table 1. On these images, two point source detection methods were used: The primary method used was the "white light" detection method as in (KAVIRAJ 2012). The other method was to compile separate source catalogs for the F555W filter and the filter closest to F336W and take the overlapping sources as the output catalog. The Cross-comparison method was used whenever the galaxy had a combination of too many different cameras and low source counts leading to an unusable white light image.  Table 1:  \begin{table}  \begin{tabular}{l|lllllllllll}  \hline  ~ & F225W & F300W & F330W & F435W & F450W & F475W & F555W & F814W & Cluster Detection Method/ Detection Threshold(s) used & Distance Modulus & Minimum Log Mass for observability \\ \hline  NGC 524 & WFC3 & ~ & ACS & ~ & ~ & ~ & WFPC2 & WFPC2 & Cross-Compare/ F555W: 45\$\backslashsigma\$\\F330W: 6\$\backslashsigma\$ & 32.10 & 2.9926 \\  NGC 2685 & WFC3 & ~ & ~ & ~ & WFPC2 & ~ & WFPC2 & WFPC2 & Cross-Compare/ F555W: 45\$\backslashsigma\$\\F450W: 40\$\backslashsigma\$ & 30.57 & 1.81605 \\  NGC 2768 & WFC3 & ~ & ~ & ACS & ~ & ~ & WFPC2 & WFPC2 & Cross-Compare/ F555W: 45\$\backslashsigma\$\\F336W: 40\$\backslashsigma\$ & 31.38 & 2.27633 \\  NGC 3032 & WFC3 & ~ & ~ & ~ & ~ & WFC3 & WFC3 & WFC3 & White light/ 5\$\backslashsigma\$ & 30.48 & 1.83302 \\  NGC 3156 & WFC3 & ~ & ~ & ~ & ~ & WFC3 & WFC3 & WFC3 & White light/ 50\$\backslashsigma\$ & 31.50 & 2.04135 \\  NGC 3489 & WFC3 & ~ & ~ & ~ & ~ & WFC3 & WFC3 & WFC3 & White light/ 200\$\backslashsigma\$ & 29.60 & 1.68015 \\  NGC 4459 & WFC3 & WFPC2 & ~ & ~ & ~ & WFC3 & WFC3 & WFC3 & White light/ 200\$\backslashsigma\$ & 31.02 & 2.10882 \\  NGC 4477 & WFC3 & ~ & ~ & ~ & ~ & WFC3 & WFC3 & WFC3 & White light/ 100\$\backslashsigma\$ & 31.34 & 2.32347 \\  NGC 4550 & WFC3 & WFPC2 & ~ & ~ & ~ & ACS & WFPC2 & WFPC2 & Cross-Compare/ F555W: 45\$\backslashsigma\$\\F300W: 6\$\backslashsigma\$ & 31.06 & 2.13877 \\ \hline  \end{tabular}  \end{table}  Because of the vast variety of cameras (WFC3, ACS, and  WFPC2), low NUV brightness, and mildWCS dierences which were  not correct-able with tweakreg due to low source counts, images were  not able to be combined into a white light source. Instead, separate  source catalogs were found for both the ACS f330w and WFPC2  f555w lters and cross-compared.  Introduce that HST data are what is used. Different filters for each galaxy, reference table.  Info on how point (or close to point) sources were found using the two different methods. Reference the table for which method used for each galaxy as well as the relevant thresholds used.      TABLE: galaxy name, filters, method, thresholds, distand modulus, mass detection threshold.