What I learned about ADQL queries at the Gaia sprint; WD binaries

Morgan F. ran some tutorial with me on ADQL etc..

the idea is to find WD wide binary candidates that commove with TGAS

stars within 300 pc. Go to TOPCAT;  preload a table of TGAS stars within

300 pc; activate that table and then go to TAP queries; select GAVO; select gps1; 

Then:

SELECT

   TOP 10000  *

   FROM gps1.main AS db

   JOIN TAP_UPLOAD.t2 AS tc

   ON 1= CONTAINS(POINT('ICRS', db.ra, db.dec),

                 CIRCLE('ICRS', tc.ra, tc.dec, (10.3*tc.parallax/3600.))) 

   WHERE  db.e_pmra * 3.6e6 < 5. AND db.e_pmde * 3.6e6 < 5.

AND

                 SQRT( (power(tc.pmra-db.pmra*3.6e6 , 2) + power(tc.pmdec-db.pmde*3.6e6 , 2)) /

                 (power(db.e_pmra* 3.6e6,2)+power(db.e_pmde* 3.6e6,2)) ) < 5

Morgan's version of that query yielded nice results.

speeding up iCannon

In a thesis meeting with Christina, Joe brought up the following idea: currently we fit the pixel fluxes (and their variance) in the Cannon, why do we not fit the projection of the data onto a set of principal components? That would be far fewer data points?

JWST Wide Survye (Discussion with M. Franx @ Berkeley Oct 2016)

From today's discussion the following proposal emerged:

What if we did a 700 sqarcmin survey of R=100 only survey of the entire CANDELS
area; 1h per setting

This yields 2000 galaxies to m_AB=24.8 for which we get continuum S/N >10/pix;
good enough to do quite good age, FeH and a/Fe.
at z>2
We also get good enough H/alpha for 2Msun/year

AS4 stellar astrophysics concept

Science scope:
  broad spectrum of ground-breaking stellar astrophysics,
 telling us how stars work, live and die...

With Gaia & TESS there are transformational space missions 
that focus on imaging/photometry/astrometry (some spectra) of bright stars.
The proposed program is tailored towards a spectroscopic survey that
in many ways ideally complements this:
 -- it is all sky
 -- it is matched in apparent magnitude
 -- it is time-domain
 -- it is dust-penetrating (disk/young stars)

Natural operational meshing of stellar astrophysics & DISCO

It is focussed on
 -- age-chemo-orbital mapping of the entire galaxy 
 -- binary stars across the HR (as calibrators, stellar evolution, SF,SN)
 -- astroseimsology to understand stellar evolution (need spectra)
 -- planet hosts 

It is a full sky program, with APOGEE and BOSS (1 each) in both hemispheres,
2/3 is multi-epoch observations; 2/3 APOGEE; 1/3 BOSS; still based on a 10min minimal cadence.

"Surprise" element:
Instead of a ROBOT, a 4-5 fold-set of 300 APOGEE fibers, feeding 4-5 gang connectors,
still using plug plates would enable:
 -- simultaneous use of 300 APOGEE and 500 BOSS fibers 
     --> better use of instrument/detectors
 -- more flexibility in fiber placement

This would mean:
-- minimal new hardware development 
   (RV improvement; fiber cart upgrade with BOSS and more APOGEE fibers)
-- move 1 BOSS spectrograph to LCO
-- plug plate costs in two hemisphere continues
-- could start 2019

All science can be done in minimally 3 years; comfortably 4 years;
minimum 25 Million x 10min x spectrum
few million fiberx10min open (for BOSS)

Much of the same science would work within fiber-robot framework,
too, in comparable survey duration.

Exercises for the cosmology block course

Though on exercises for the Cosmology Block course:

Day 1: Newtonian cosmology:
   Exercise: things to do with the collapsing top hat:
   -- explain that (in three days) we'll see that overdose parts of the Universe
can be treated as Newtonian Universes
  -- the collapsing sphere:
     -- toy-problem
     -- "virializing"
     -- properties
     -- application to the Milky Way:
        we take v_circ --> v_virial --> mass, size, etc..


Day 2: Friedman-Robertson Walker Universe
    -- code up, and plot, the angular diameter distances; luminosity distances
       as a function of cosmological parameters;
   -- what are the uncertainties implied by current cosmol. parameter uncertainties
       (which we prod ad hoc at this point)
    -- application: what's size of a galaxy at z=0.5,2,7
    [TOO Early; move all of this to day 3?]

Day 3: Linear growth of structure etc...
    -- code up the solution of contrast growth for non-trivial (i.e. realistic) cosmological parameters
    -- compare the (linear) growth of structure between toy-cases of cosmological parameters
    -- do top-hat now in a cosmological context  
    -- or code up and plot Press-Schechter

Exercises for the cosmology block course

Though on exercises for the Cosmology Block course:

Day 1: Newtonian cosmology:
   Exercise: things to do with the collapsing top hat:
   -- explain that (in three days) we'll see that overdose parts of the Universe
can be treated as Newtonian Universes
  -- the collapsing sphere:
     -- toy-problem
     -- "virializing"
     -- properties
     -- application to the Milky Way:
        we take v_circ --> v_virial --> mass, size, etc..


Day 2: Friedman-Robertson Walker Universe
    -- code up, and plot, the angular diameter distances; luminosity distances
       as a function of cosmological parameters;
   -- what are the uncertainties implied by current cosmol. parameter uncertainties
       (which we prod ad hoc at this point)
    -- application: what's size of a galaxy at z=0.5,2,7
    [TOO Early; move all of this to day 3?]

Day 3: Linear growth of structure etc...
    -- code up the solution of contrast growth for non-trivial (i.e. realistic) cosmological parameters
    -- compare the (linear) growth of structure between toy-cases of cosmological parameters
    -- have students walk themselves through the argument why CMB+LSS basically rules out    
baryonic dark matter.

Exercises for the cosmology block course

Though on exercises for the Cosmology Block course:

Day 1: Newtonian cosmology:
   Exercise: things to do with the collapsing top hat:
   -- explain that (in three days) we'll see that overdose parts of the Universe
can be treated as Newtonian Universes
  -- the collapsing sphere:
     -- toy-problem
     -- "virializing"
     -- properties
     -- application to the Milky Way:
        we take v_circ --> v_virial --> mass, size, etc..


Day 2: Friedman-Robertson Walker Universe
    -- code up, and plot, the angular diameter distances; luminosity distances
       as a function of cosmological parameters;
   -- what are the uncertainties implied by current Cosmol. parameter uncertainties
    -- application: what's size of a galaxy of 1kpc size at z=0.5,2,7