Difference: CosmoTelecon20180125 (1 vs. 2)

AMPEL

• What is the status of alerts from UW? unclear
• Most of the infrastructure is being implemented but we would best like to have a list of alerts from one night to test things
• Stockholm 6th floor people would like to do some manual scanning to select their follow-up targets. Will be possible with AMPEL.
• With Eric on parental leave it is unclear who is the best point of contact at UW re alerts.
• What kinds of catalogs should be included? CLU (contact Mansi/Dave), photo-z catalogs (start with SDSS)
• What kind of photo-typing/LC-fit do we want to implement? Maybe just start with a quick SALT2 fit at first (implemented by Mickael or Uli)
• Valéry will push T2 example very soon and is working on T3.

U-band

• Getting the titanium feature will reduce RMS and reduce dependency on host mass and star formation
• Actually requires UV spectroscopy, so mostly for subset of SNe that get SNIFS observations
• We should always attempt to get early U-band spectroscopy because this constrains Nickel mass

i-band

• Adjusted selection to larger blocks in beginning and end.
• Also made sure that high-cadence fields are always observed (or for as long as possible).
• E(B-V) <= 0.1 is now sufficient for field selection.

Agenda:

• Update on i-band fields
• SEDm target selection
• Update on AMPEL (if any)
• Implications of Jakob's U-band study

Minutes

Connection:

https://zoom.us/j/272828651

Or iPhone one-tap (US Toll): +16468769923,,272828651# or +16699006833,,272828651#

Or Telephone: Dial: +1 646 876 9923 (US Toll) or +1 669 900 6833 (US Toll) Meeting ID: 272 828 651 International numbers available: https://zoom.us/zoomconference?m=yUACqd9q0rOg7icOHZs3wWcqWHdt5lib

-- UlrichFeindt - 24 Jan 2018