10:00:47	 From Eric Agol : Yes!
10:00:48	 From Rafael Garcia Bustinduy : YES
10:00:49	 From Rajeev Singh Rathour : Yes 
10:00:51	 From Maria Pia Di Mauro  To  All Panelists : yes sure
10:00:55	 From David Montes  To  All Panelists : yes
10:01:44	 From Katja Poppenhaeger - Coordinator  To  David Montes and  All Panelists : Questions/discussion re: Tyler's talk...
10:02:16	 From Katja Poppenhaeger - Coordinator : Questions/discussion re: Tyler's talk (just to structure the chat export file)
10:16:04	 From Jake Clark : Would large scale surveys like GALAH. K2-HERMES, LAMOST, RAVE etc., help at all?
10:16:22	 From Philip Muirhead : Nice result Tyler!
10:16:52	 From Eric Agol : Tyler:  Nice talk! Have you examined how the coefficients of the GP model vary across the period/color diagram?
10:17:30	 From Eric Agol : (This is related to Ruth’s question.)
10:19:05	 From Jamie Tayar : Tyler: Does the factor that the cluster pile up is not at the same place as lower edge of the gap mean that there are two unrelated issues in the physics of spin down? 
10:20:13	 From Katja Poppenhaeger - Coordinator : Questions to Aomawa start here.
10:20:35	 From Julián David Alvarado Gómez : Q for Tyler: Why would you favor a model that assumes the origin of such period bi-furcation in processes happening inside the star (and most likely not measurable by any means, not even in the future) rather than models using predictions on the wind properties of cool stars (measurable in the near future by LUVOIR or Lynx)?
10:22:43	 From Andrew McWilliam : I'm interested to know whether these GCM models include heat input from stellar winds.
10:22:57	 From Julián David Alvarado Gómez : +1
10:28:14	 From Natalie Hinkel : The latitude vs pressure plot looks like a polar bear wearing a hat… 😉
10:28:32	 From Katja Poppenhaeger - Coordinator : :-)
10:34:48	 From Aomawa	Shields  To  All Panelists : We almost named it that
10:36:54	 From Katja Poppenhaeger - Coordinator : Questions to Adam start here
10:48:42	 From Ry Cutter  To  Miriam Rosario Saldana Munoz and  All Panelists : I may have missed it, but are mass ratios important? Would you need to account for GR effects for high mass ratios/close orbits?
10:49:21	 From Pierre Maxted : Yes
10:50:23	 From Julián David Alvarado Gómez : Q for Adam: If you reduce the degrees of freedom (i.e. not take into account the radial shear), how much latitudinal shear you would get?
10:50:38	 From Adam Jermyn : The mass ratios don’t enter into the calculation we’re doing (because we set the torque to zero). But I haven’t thought about GR effects so it may enter there.
10:51:36	 From Adam Jermyn : Julián - I don’t know, but that’s a good idea to try.
10:52:15	 From Ruth Angus : Wow, cool result, Ekaterina!
10:52:30	 From Jim Fuller - Coordinator : I agree with Adam: I don't think mass ratios will affect the result, except when looking at longer period binaries which may or may not be synchronized (depending on the mass ratio). I don't see how GR would change anything here. 
10:53:35	 From Pierre Maxted : I have a question about the faint young Sun problem
11:07:56	 From lynne hillenbrand : A question for Tyler:   how much are your results limited by requiring BP-RP instead of using infrared colors which would allow you get further into the M spectral types
11:09:50	 From Aomawa	Shields  To  All Panelists : Pierre, here are a couple of papers on the faint young Sun problem:
11:09:51	 From Aomawa	Shields  To  All Panelists : https://agupubs.onlinelibrary.wiley.com/doi/full/10.1002/jgrd.50808
11:10:05	 From Aomawa	Shields  To  All Panelists : https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2011RG000375
11:11:13	 From Julián David Alvarado Gómez : Q for Aomawa: You mentioned that the stellation(?) required for an M-dwarf planet is lower than for an G-dwarf planet. Stellar wind modeling on M-dwarfs predicts generally strong winds at the HZ of M-dwarfs, with significant contribution from stellar wind (joule) heating to the upper atmosphere of the planets (several times the value on Earth of ~120 GW). Would this mean that planets further than the standard HZ could get the missing heating from the stellar winds?
11:14:02	 From Philip Muirhead : Thank you Katja and Victor for hosting today!
11:14:04	 From Aomawa	Shields  To  All Panelists : This is a really cool question. We think the stronger radiative response of CO2 for M-dwarf planets vs. G- or F-dwarf planets might impact climate and instellation levels for freezing. Perhaps stellar wind heating could do something similar. Perhaps extend HZ for M dwarfs?
11:14:29	 From Miriam Rosario Saldana Munoz : Great talks! Thank you
11:14:31	 From Rafael Garcia Bustinduy : bye
11:14:32	 From David Montes  To  All Panelists : Bye
11:14:38	 From Eric Agol : Ciao
11:14:40	 From Yilen Gomez Maqueo Chew : thank you to all speakers and coordinators!
11:14:53	 From Rukmini Jagirdar  To  All Panelists : Bye, great talks. Thankyou
11:15:01	 From Mutlu YILDIZ  To  All Panelists : thank you...
11:15:02	 From Bihan Banerjee : Thank you all! Excellent talks, bye!