Title    Gas densities and dynamics in central regions
Pi     N. Nakai
Time   99 hrs
   1. Name: Gas densities and dynamics in central regions
	Tatematsu, K., Nakai, N., et al.

   2. One short paragraph with science goal(s)

Fueling AGNs and nuclear activity on the sub-kpc scale. (May overlap
with another sub-theme.) Study the gas morphology, dynamics, physical
properties in nuclear regions of active galaxies (Seyferts, liners, AGN)
and "apparent" normal galaxies. Example is the study by Schinnerer et al. 
in NGC 1068. How may active galaxies have severely warped inner disks? 
Can we see mini-spirals inside the Inner Lindblad Resonance that might 
feed the AGN? Can we detect a molecular torus very close in to the central 
engine? Do double-barred galaxies have a role to play in nuclear activity?
Do all galaxies have massive black holes?

   3. Number of sources

	15, about half AGN and half non-AGN

   4. Coordinates:

      4.1. all over the sky (probably)

      4.2. Moving target: no

      4.3. Time critical: no

   5. Spatial scales:

      5.1. Angular resolution (arcsec): 0.05"  (2.4 pc at 10 Mpc)

      5.2. Range of spatial scales/FOV (arcsec): single field (23")

      5.3. Single dish total power data: yes

      5.4. ACA: yes

      5.5. Subarrays: no

   6. Frequencies:

      6.1. Receiver band: Band 6

      6.2. Lines and Frequencies (GHz):
		CO 230.0 GHz (redshifted for 10 Mpc and Ho = 75)

      6.3. Spectral resolution (km/s): 10 km/s

      6.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s max

   8. Line intensity:

      8.1. Typical value (K or Jy): 10 - 30  K

      8.2. Required rms per channel (K or Jy): 1.5 K

      8.3. Spectral dynamic range: 10

   9. Polarization:  no

   10. Integration time for each observing mode/receiver setting (hr):
		6.6 hr per galaxy

   11. Total integration time for program (hr): 6.6 x 15 = 99 hours

   12. Comments on observing strategy (e.g. line surveys, Target of
       Opportunity, Sun, ...): (optional)

Will be important to fill the gap between pc scale measured with water-vapor 
maser emission and several hundred pc scale measured with existing arrays.

Will pick targets that are reasonably close, because gain
in resolution and sensitivity, but the number of very close AGN is limitted.
10 Mpc seems like a reasonable estimate for a typical distance. 

************************************************************************

Review Chris Carilli: OK.
--------------------------------------------------
Review v2.0:
 
Gas densities and dynamics in central regions
Tatematsu et al. 

This appears unchanged from the viable program in DRSP1.  Is the
target list of 15 unduly small? How big a project could the authors
propose without exhausting target lists or yielding duplicate
information? I suspect much more than 15 sources for 99 hours in
total. Does the ACA information help to see pc-scale structure in the
innermost disk?