TCP SWG Notes 2014/11/24
(notes taken by PD)
Intro, Geoff: need to prepare for AAS workshop. Kawabe (SOC invite)
declined. Bryan: replacement has been invited (someone else from Japan,
not sure who). Geoff: we have asked Michael Kramer to talk about GC
pulsars, who has agreed. We have 1 hour total -- 30 min Michael, 30 min
GC Pulsars, Jim C: How much overlap with MeerKAT
/ SKA-mid? (some
general discussion of what MeerKAT
/SKA will/won't do, and when).
Argument could be made either way that this is more of a MeerKAT
topic? Seems to be some difference of opinion on this.
Michael: presentations for EVLA-II/NMArray on wiki, describing
time-domain imaging of "things that explode." Was well received by
NSF(?) when originally presented.
Cosmology, Geoff: Some previously suggested topics: megamasers (H0 / BH
mass); resolving binary AGN; dz/dt; evolution of fundamental consts;
intensity mapping. What is compelling / what are we missing?
Intensity mapping, Dan: intrinsically above 15 GHz; cross-correlate
other catalogs with observed CO; extract otherwise unrecoverable
signals. (upcoming instruments for x-corr LSST, DESI) Bryan: should we
consider full-time survey mode "radio LSST"? Dan: mapping speed more
important that point-source sensitivity for this; may be mismatch with
Geoff, discussion of "revolutionary vs evolutionary"
Microlensing (Avery?): radio survey could double sample of stellar mass
BH each year. Geoff: how many sources need to be monitored for 10
events per year? Update on wiki.
Tzu-Ching: dz/dt is argument for next-gen optical (ELT/etc). Geoff:
could also be done with ALMA? Dicussion of lensing, recap of previous
talk of strong lensing (argument was that it's more interesting for
individual source astrophyics instead of cosmology); what about weak
lensing? Source counts decline with freq so becomes less sensitive at
high freqs, ~1 GHz better.
Synoptic surveys: Gregg: FOV reduced at high freqs, maybe more of a
followup instrument? Should look at survey speed wrt long-GRB orphan
afterglows. Michael: could think about adding PAFs to a subset of the
instrument to use as a survey instrument. Gregg: sweet spot between
~10-20 GHz for long GRB afterglows, instrument should be unique for
GW counterparts: Gregg: might not win due to optically thin at high
What to present at AAS: Geoff will outline a few things to have a
target to shoot at. Who will be present -- email Geoff if you are