CCDSKY(1NEMO) manual page

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ccdsky - lazy (cosmology) sky scaling calculator

ccdsky is a lazy sky scaling calculator. It will give you the scaling parameters for a FITS file (which uses degrees for angles, and m/s for velocities), to make your typical observer or astronomical software package happy and print out values in units observers can be in awe about. It is also useful to remind yourself how many arcseconds/minutes a given object is at a given distance.

Although you can transform an image/cube, the default only needs to know the distance (in AU, pc, kpc, mpc, z, ...) and unit size (in AU, pc, kpc, mpc, ....) of the object. This will give you the scaling factors for length and velocities.

When the distance is given in z, Wright’s (2006) cosmology calculator is used.

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.

in=

Optional input image file. Must be in image(5NEMO) format.

out=

Output image file, only required if an input image is given. Will be in image(5NEMO) format, with optionally scaled image values and axes coordinates.

d=#,[unit]

Distance to your object, and optionally a unit. AU, pc, Kpc, Mpc, and Gpc are allowed. You can also specify a dimensionless number ’z’, in which case the special cosmology calculator is used. Or if you know the recession speed and assume a Hubble constant, d=4500/69,Mpc [default: 1,pc]

r=#,[unit]

Length scale of object, and optionally a unit. km, AU, pc, Kpc, Mpc, and Gpc are allowed. Together with a distance d=, this will convert the length scale in your maps to degrees, required for FITS. [default: 1,AU]

v=#,[unit]

Velocity scale of object, and optionally a unit. The output units will be the one that FITS uses, m/s. [Default: 1,km/s]

sdv=#

Total flux, in Jy.km/s, of the source. Based on the distance, it will the compute the HI and H2 (given some reasonable X factor) masses, in units of solar masses. Default: 1

scale=#

Scale the intensity values in the data itself. Default: 1.

H=

Specify the cosmology model, with up to 3 parameters. Only used when units in d= are ’z’ were specified. The first parameter is the Hubble Constant. Optionally followed by the WM (Omega(matter)) and WV (Omega(vacuum)), for different cosmologies. If only H0 and WM are given, a flat universe (WV=0) is used. See also Wright(2006). WMAP-9 values: H=71,0.27,0.73 (2011?), Planck-1 values: H=67.15,0.317,0.683 (2013) [Default: 71,0.27,0.73]

nsteps=

Max. number of integration steps in the cosmo code to achieve accuracy. [Default: 1000]

H

It will be amusing to see the evolution of H:

WMAP-9 (2011)    71    0.27    0.73
Planck (2013)    67.15    0.317    0.683
Planck (2018)    67.66    0.3111    0.6889

Examples

Viewing a model at a distance 1 pc, where 1 length unit represents 1 AU, the coordinates need to be multiplied by 0.000277785 in order for FITS to view them in the correct angular size of 1 arcsec.

% ccdsky d=1,pc r=1,AU v=1,km/s
d=1 pc
r=1 AU
v=1 km/s
rscale=0.000277785  (1.00003 arcsec)
vscale=1000

To find out the radius of 2 pc at the distance of the galactic center:

ccdsky r=2,pc d=8.5,kpc
rscale=0.0134814  (48.5329 arcsec)

Here is an example of creating a small bar, at position angle 30, and observed at RA=6h and DEC=30d:

% ccdgen "" map4 bar 1,10,0.5,30 size=512,512,1 
% ccdsky map4 map4b
% ccdfits in=map4b out=map4b.fits radecvel=t crval=90,30 crpix=256.5,256.5
% # now switch to MIRIAD
% fits in=map4b.fits out=map4b.mir op=xyin
% cgdisp in=map4b.mir device=/xs labtyp=arcmin

and you should see a bar (possibly with a sign error position angle) of about 1 arcmin in length, in an 8 arcmin field. Notice that ccdfits(1NEMO) also has various options to specify a WCS which can override the one set by ccdgen(1NEMO) .

Here is a cosmological example:

% ccdsky H=67.7,0.307,0.693   d=2.19,z
-------------------------------------------------------------
For H_o = 67.7  Omega_M = 0.31 Omega_vac = 0.69 z = 2.190
It is now 13.830 Gyr since the Big Bang.
The age at redshift z was 3.012 Gyr.
The light travel time was 10.818 Gyr.
The comoving radial distance, which goes into Hubbles law, is 5592.2 Mpc
or 18.239 Gly
The comoving volume within redshift z is 732.530 Gpc^3.
The angular size distance D_A is 1753.026 Mpc or 5.718 Gly.
This gives a scale of 8.499  kpc/arcsec
The luminosity distance D_L is 17839.0 Mpc or 58.183 Gly.
The distance modulus, m-M, is 46.26
-------------------------------------------------------------
d=2.19 z  [3635.8 Mpc]
r=1 AU
v=1 km/s
SdV=1 Jy.km/s
rscale=1.5846e-13  [ 5.70457e-10 arcsec   5.70457e-07 mas]
vscale=1000
iscale=1
Mass(HI) = 7.25098e+11  
Mass(H2) = 3.22675e+10  (alpha=4.3; includes 1.36 He contribution)

compare this with the (selected) output for gnuastro’s astcosmiccal(1) program:

  % astcosmiccal  --H0=67.7 --olambda=0.693 --omatter=0.307 -z2.19
  CosmicCalculator (GNU Astronomy Utilities) 0.11
Universe now
 ------------
 - Age of Universe now (Ga*):                             13.844296
 - Critical density now (g/cm^3):                         8.610662e-30
 - Proper distance to z (Mpc):                            5592.995113
 - Angular diameter distance to z (Mpc):                  1753.290004
 - Tangential distance covered by 1 arcsec at z (Kpc):    8.500190
 - Luminosity distance to z (Mpc):                        17841.654411
 - Distance modulus at z (no unit):                       46.257176
 - Conversion to absolute magnitude (no unit):            44.997699
Universe at desired redshift z
 ------------------------------
 - Age of Universe at z (Ga*):                            3.017860
 - Look-back time to z (Ga*):                             10.826436
 - Critical density at z (g/cm^3):                        9.177897e-29

17-Aug-2012    V1.0 Created        PJT
23-aug-2012    V1.1 added sdv=        PJT
28-aug-2012    V1.2 implemented scale=    PJT
28-feb-2013    V2.2 more verbose, added H=    PJT
16-mar-2013    V3.0 added Wright’s cosmology calculator    PJT

Table of Contents

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Synopsis
Description
Parameters
H
Examples
Caveats
See Also
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