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Name

ccdvel - create a velocity field; grid or retrace

Synopsis

ccdvel out=velfie [parameters=values ...]

Description

ccdvel creates a model velocity field for a disk with material in circular orbits. The user supplies the program with a table of a rotation curve (see also rotcurshape(3NEMO) for another approach) with a set of radii and rotation velocities. The position angle and inclination of each ’ring’ can also be varied to simulate geometrical warps.

Two gridding methods exist:

retracing: the GIPSY method retraces each pixel in the sky plane to its (smallest) radius in the (warped) galactic disk: its ring parameters (velocity, position angle, and inclination) are then (linearly) interpolated from the input arrays, and that point is appropriately projected into that pixel ( bug? it might still wind up in the next pixel)

gridding: the NEMO method places particles in rings, as prescribed by the input values, and computes a properly intensity weighted (number of particles in this case) mean velocity per pixel. This may however results in a ’meaningless’ mean velocity in areas where rings are projected on top of each other. Note: This mode, originally the only one, merely served as a shortcut between the various N-body creators, followed by subsequent gridding with snapgrid. It may not work anymore, since it is not well maintained.

The center coordinates and systemic velocity are currently fixed for all rings.

Using keywords mexp= and phexp= a circular orbit can have its expansion velocity modulated: 

    vexp*cos(mexp*(phi-phiexp))
instead of a constant vexp (i.e. mexp=0), where phi is measured from the major axis in the plane of the disk (check!). This only works for the retracing method though. Although the rotation speed has a similar modulation implemented, it is not a good idea to use that. Instead, it will probably be better to re-define this as 
    vrot+vexp*sin(mexp*(phi-phiexp))
though this would suggest the local velocity ellipsoid to be isotropic (cf. Binney & Tremaine ....)

Parameters

The following parameters are recognized in order; they may be given in any order if the keyword is also given. Use --help to confirm this man page is up to date.
out=image_out
Output velocity field map, will be in image(5NEMO) format. No default.
radii=r1,r2,...
Radii (arcsec). Note they must be sorted by increasing radius. The default is taken from the rotcur_table table below, or from this keyword.
vrot=v1,v2,...
Array of rotation velocities, one for each radius, If less than the number of radii is given, the trailing ones are filled with the last supplied value. The default values from the rotcur_table table below can be also be overridden with this keyword.
vexp=v1,v2,...
Array of expansion velocities, one for each radius. If less than the number of radii is given, the trailing ones are filled with the last supplied value. Default: 0
inc=i1,i2,...
Array of inclinations (degrees), one for each radius. The default values from the rotcur_table table below can be also be overridden with this keyword.
pa=p1,p2,...
Array of position angles (degrees), one for each radius. The default values from the rotcur_table table below can be also be overridden with this keyword.
phrot=p1,p2,p3,...
Array of rotation phase angles (degrees), one for each radius. Don’t use this right now. Default: 0
phexp=p1,p2,p3,...
Array of expansion phase angles (degrees), one for each radius, for the modulation of the expansion velocities.
mrot=m
Fourier mode for the rotation speed modulation. Currently not a good idea to use this, since we would modulate the whole rotation, not a tiny bit on top of rotation. Use mexp=,phexp=. Default: 0
mexp=m
Fourier mode for the expansion speed modulation. Default: 0
size=nx,ny
Size of map, up to two numbers. If one number supplied, the map will be square. Note that in NEMO (0-based) coordinates, the center of rotation will be at ((nx-1)/2,(ny-1)/2). [Default: 128].
cell=dx,dy
Cell size, up to two numbers. If one number supplied, the cells will be square. [Default: 1].
center=x0,y0
Rotation center (grids with lower left corner being 0,0). Default: center of map if rotcur_table is not used, else the center_ring entry from the rotcur_table.
blc=xmin,ymin
Lower left corner of the grid. Default: 0,0.
vsys=vsys
Systemic velocity. Default: 0 if rotcur_table is not used, else the center_ring entry from the rotcur_table.
rotcurfit=rotcur_table
All ring parameters can also be read from this table, that is normally output by rotcur(1NEMO) ’s tab= keyword. That table needs to be commented with tabcomment(1NEMO) .
fixring=center_ring
Ring number (1..Nring), from the rotcur_table, of which the center (vsys, center) is used. If 0 is used, they must have been given by the appropriate keywords. If a large number is given, the last table entry is used.
noise=v_sigma
Dispersion of the gaussian noise added to the map. Default: 0
amp=t|f
If set to true (or 1) it will create an amplitude (surface brightness) map, instead of a velocity field. In this case, the rotation speed is taken as the amplitude of the density map. See also ccdgen(1NEMO) . Default: false
seed=
Initial seed for random number generator. See xrandom(3NEMO) for defaults. Default: 0
in=ccd-file
Template (2d) image to provide the WCS for a cube. (deprecated)
intpol=linear|constant
Interpolation method used for rings in retrace method. For linear each computed galactic radius has linearly interpolated values for the rotation curve, inclincation, position angle etc., whereas for constant the starting value of ring is used. Default: linear.
headline=comments
Random verbiage added to the output image [Default: none].

Example

A velocity field in a file map1 is fitted with rotcur, starting at the outskirts of the galaxy, 100", and working on inwards to 10", the table is commented to feed it into ccdvel (note the numeric sort) and compute a model velocity field, after which that is subtracted from the observations (only in points were both model and observations are not undefined, i.e. 0.0): 


    1% rotcur in=map1 radii=100:10:-5 vrot=100 pa=20 inc=45 vsys=1200 \
         center=100,110 fixed=center,vsys,inc tab=map1.tmp units=arcsec
    2% tabcomment map1.rotcur - | sort -n > map1.rotcur
    3% ccdvel out=map1.model rotcurfit=map1.rotcur
    4% ccdmath in=map1,map1.model out=map1.diff \
            fie="ifeq(%1,0.0,0.0,ifeq(%2,0.0,0.0,%1-%2))"

One can also use ccdvel to create a surface brightness. Creating a functional form for the density can be done using tabmath(1NEMO) . E.g. the following example creates an exponential surface density profile: 

    5% set rad=‘nemoinp 0:100:5‘
    6% set den=‘nemoinp 0:100:5 | tabmath - - "exp(-%1/20)" all‘
    7% ccdvel out=map1.den radii="$rad" vrot="$den" pa=30 inc=60 amp=t
or
    8% nemoinp 0:100:5 > map1.radt
    9% nemoinp 0:100:5 | tabmath - - "exp(-%1/20)" all > map1.dent
   10% ccdvel out=map1.den radii=@map1.radt vrot=@map1.dent pa=30 inc=60 amp=t

Now one can create a velocity field in a simular way,

11% nemoinp 0:100:5 | tabmath - - "%1/sqrt(40+%1*%1)" all > map1.velt
12% ccdvel out=map1.vel radii=@map1.radt vrot=@map1.velt pa=30 inc=60 

and with simulated beamsmearing create a beam smeared velocity field:
   13% ccdsmooth map1.den map1.dens 4
   13% ccdmath map1.den,map1.vel - "%1*%2" | ccdsmooth - map1.dvels 4
   14% ccdmath map1.den,map1.dvels map1.vels "%2/%1"
Note however that this method of beamsmearing is only approximate, and ignores the internal velocity dispersion, which can be very important in areas of large velocity gradients.

Rotcurfit

The table rotcurfit assumes the radius, systemic velocity, rotation velocity, position angle, inclination, x center and y center are in columns 1, 2, 4, 6, 8, 10 and 12 resp.

See Also

snapgrid(1NEMO) , ccdgrid(1NEMO) , snapslit(1NEMO) , ccdgen(1NEMO) , rotcur(1NEMO) , rotcurshape(1NEMO) , velcube(1NEMO) , velfi(GIPSY)

Author

Peter Teuben

Bugs

The output map is patched with the undefined value 0.0 where-ever no information is requested for these pixels.

The gridding method is currently not available. The retracing (GIPSY) method will be used.

Different versions of rotcur exist (NEMO, Gipsy) that use different columns, so the rotcurfit= tables should be used with caution.

Update History


20-may-91    original program                         PJT
31-jul-92    V1.3 new rotcurfit=; rings are now radii        PJT
3-aug-92    (b) fixed mapsize bug; override center=       PJT
12-aug-92      (d) added headline=                          PJT
oct-99           doc additions                                   PJT
apr-01        V1.5b added in=, but deprecated it        PJT
1-may-01    V1.6 added amp= for CARMA simulations        PJT/LGM
3-may-01    V1.7 added vexp=                                PJT
29-jun-02    V1.8 added blc= keyword (Joshua Simon)        PJT
6-feb-03    V2.0 modulated orbits (mexp,phexp,mrot,phrot)    PJT
11-sep-03    V2.1 added intpol=                PJT

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