Put questions in this chat window or our slack channel and I will collate.

Breaking up!

For Nushkia, how do we measure R1 in observation?

For Preethi: If I understood, you are using complementary data with deeper imaging in some cases? If so, how do you deal quantifying the LSB features given there is a mixture of depths in the imaging?.

For Preethi, why bar fraction has correlation with HI, is it because bar funnels the gas ?

For Preethi: do you see LSB tidal features around galaxies at the lower mass end of your sample i.e 10^9 MSun

Ilsang - you may also be interested in Masters et al. 2012 where we also explored bar fraction and HI content.

Thanks Karen!

How does the new R1 measures correlate with Re?

I think you should also check correlations with Rp

The petrosian radius

Thanks everyone!

Thanks. :)

Post your questions here! I don’t want it to be just me!

actually i didn’t mention this because of time, but part of the sample i used for my work is from the 14000 objects in Nair & Abraham (2010) :D

Lior, Can you describe how you controlled for multiple testing when calculating the p-values?

A general question: how will Rubin improve this endevour? What is the expectation? (I am not from this field.)

for my case, it’s the depth. Rubin will provide deeper data to better characterise galaxy outskirts and their sizes (for our definition)

at least 10 times deeper or more than the images i am using now

Thanks!

good point, statistics!

Thank you!

Congrats Nushkia