Title  SNR-cloud interaction search in LMC
Pi     K. Tatematsu
Time   86 hrs

 1. Name: SNR-cloud interaction search in LMC
     Authors: K. Tatematsu, Y. Fukui,....


  2. LMC contains many supernova remnants (e.g. Mathewson et al. 1985).
It is of our interest
how supernova remnants affect the global properties in a
galaxy. SNRs will input enrmous energy into the interstellar medium,
and this will affect the evolution of the interstellar medium
and the star formation activity.  Then this will caracterize the
evolution of the galaxy.

Because LMC is the galaxy closest to us, this provides us with
a great opportunity for a detailed scrutiny.
With ALMA, we will be able to study the SNR-cloud interaction
with appropriate angular resolution for the first time.
Previouslly, SNR-cloud interaction was studied with SEST (Banas et al. 1997),
but the angular resolution is too low to see the direct evidence
of the interaction.
We will take a census of the SNR-cloud in a galaxy
with sufficient angular resolution and sensitivity
for the first time.

Arikawa, Tatematsu et al. (1999, PASJ 51, L7) have studied the
supernova remnant W28
by using JCMT (beam size is about 15"=0.25 pc at 3 kpc).
This study showed that CO 3-2 is one of the best tracers of
the shocked molecular gas.
The linear resolution of 0.25 pc corresponds to 1" at the distance of LMC,
and with ALMA we will reach even better angular resolution.
We can carry out a very promising statistical study of SNR-cloud interaction
in LMC. This study will help our understanding the dynamical and thermal
evolution of a galaxy.
For a comparison, we will also observe CO 1-0 to distinguish the shocked and
unshocked gas.

References
Arikawa et al. 1999
Banas et al. 1997
Mathewson et al. 1985

3. Number of sources: 30


4. Coordinates:


   4.1. 30 sources in LMC (RA=05:30, DEC=-69:45)


   4.2. Moving target: no


   4.3. Time critical: no



5.  Spatial scales:


   5.1. Angular resolution: 1.5" at 115GHz, 0.5" at 345 GHz

   5.2. Range of spatial scales/FOV: 1' (16-field mosaic at 345 GHz)


   5.3. Single dish: yes

   5.4. ACA: yes


   5.5. Subarrays: no



6. Frequencies:


   6.1. Receiver band: Bands 3 and 7


   6.2. Line: CO 1-0 and 3-2
        Frequency: 115 GHz and 345 GHz


   6.3. Spectral resolution (km/s): 0.5 km/s

   6.4. Spectral coverage (km/s or GHz): 100 km/s



7. Continuum flux density:


   7.1. Typical value: N/A


   7.2. Continuum peak value: N/A


   7.3. Required continuum rms: N/A


   7.4. Dynamic range in image: N/A



8. Line intensity:


   8.1. Typical value: 2-10 K


   8.2. Required rms per channel: 0.3 K

   8.3. Spectral dynamic range: 10-30



9. Polarization: no



10. Integration time per setting: 
  115 GHz: 30 sources x 4 mosaic  x 3min
  345 GHz: 30 sources x 16 mosaic x 10min


11. Total integration time for program: 86 hr