Progect: Pulsar Wind Nebulae
PI: V. Kaspi
Time: 10 hrs

2. One short paragraph with science goal(s)
Young, energetic pulsars (and some older pulsars) produce extended wind 
nebulae that radiate synchrotron emission from radio up to TeV gamma rays.  
The spectra of these objects are interesting as they provide information 
about the ambient magnetic field and the pulsar wind itself.  There is an 
expected spectral break in/near the ALMA bands that has strong diagnostic 
potential.  So observing a large sample of PWNe (ie a pulsar wind nebula 
survey) with ALMA is one obvious project to undertake.

3. Number of sources 
   
16--22 PWNe (detected by Chandra observations)

4. Coordinates:

4.1. Rough RA and DEC 

Along the Galactic plane, RA: 05--20 hour; Decl: -70--60 degree.

4.2. Moving target: yes/no (e.g. comet, planet, ...)
No.

4.3. Time critical: yes/no (e.g. SN, GRB, ...)
No.

4.4. Scheduling constraints: (optional)


5. Spatial scales:

5.1. Angular resolution (arcsec):

~1 arcsec.

5.2. Range of spatial scales/FOV (arcsec):

10--100 arcsec.

5.3. Required pointing accuracy: (arcsec)


6. Observational setup

6.1. Single dish total power data: no

6.2. Stand-alone ACA: no

6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: 
     

6.4. Subarrays of 12m baseline-ALMA antennas: no


7. Frequencies:

7.1. Receiver band: 

 3, 6, 9

7.2. Lines and Frequencies (GHz): 


7.3. Spectral resolution (km/s):

7.4. Bandwidth or spectral coverage (km/s or GHz):


8. Continuum flux density:

8.1. Typical value (Jy):

0.01--0.1 Jy.

two examples

	Size	Surface flux in (band)	time*
Pulsar 1:
	6"	8.84e2 mJy (3)		77s
	6"	2.97e2 mJy (6)		75s
	6"	8.72e1 mJy (9)		483s
Pulsar 2:
	30"	2.30e1 mJy (3)		25.7hr
	30"	9.01e1 mJy (6)		23.3hr
	30"	3.15e0 mJy (9)		120hr

*time estimate based on 1" resolution, and 10 sigma detections

8.2. Required continuum rms (Jy or K): 0.001-0.01 Jy

8.3. Dynamic range within image:
assume SNR of 10 

8.4. Calibration requirements: 
Absolute, 10%.

9. Line intensity:

9.1. Typical value (K or Jy):


9.2. Required rms per channel (K or Jy):

9.3. Spectral dynamic range:

9.4. Calibration requirements: absolute      ( 1-3% / 5% / 10% / n/a )
                               repeatability ( 1-3% / 5% / 10% / n/a )
                               relative      ( 1-3% / 5% / 10% / n/a )

10. Polarization: no

10.1. Required Stokes parameters:

10.2. Total polarized flux density (Jy):

10.3. Required polarization rms and/or dynamic range:

10.4. Polarization fidelity:

10.5. Required calibration accuracy:


11. Integration time for each observing mode/receiver setting (hr):

for the bright source listed above (Pulsar 1), 77 s in band 3, 75 s in band 6 and 483 s in band 9 (total of 10.6 minutes on this source)


12. Total integration time for program (hr):  for 15 source (of which Pulsar 1 is one of the brightest), estimate 10 hours of observations


13. Comments on observing strategy : (optional)

A number of example pulsars were given as part of this DRSP.