PLT_SPEC
General purpose
program for comparing CMFGEN/CMF_FLUX spectral data with observational data.
Options are provide to redden the model, smooth the model, and to apply
rotational broadening. Although all care has been taken, it is the users
responsibility to check that options perform as indicated.
Options are
ordered under subject. Associated with each option are requested inputs. Some
inputs are not prompted for, and can only be changed from their default values
by specifying them in the call, e.g.,
RD_MOD(OVER=T)
Such inputs are placed in [ ].
There are five types of options:
(1)
Options such
as lx which change plotting style or units.
(2)
Option such
as RD_MOD(OVER=F) which pass data directly to the plot
program.
(3)
Option such
as RD_MOD(OVER=T) which place data into the (single) buffer
where it can be operated on by other commands.
(4)
Options such
as CNVLV that operate on the data in the buffer. In
some cases the data is left in the buffer -- in other cases it is sent to the
plot package.
(5)
Options which
call the plot package (default)
SVE file:
A text file containing options (transparent
and hidden) used in the execution of a command
Default is to write a file Ôcommand.sveÕ (e.g.,
rd_mod.sve) containing the options used when a command is executed.
Case is important for the sve file but not
for the option.
Append sve=filename to write a new .sve
file (no brackets).
To execute a previous command, enter
.command (e.g., .rd_mod). Options can be changed by supplying the in () after
the sve file name., e.g.,
.rd_mod(over=t)
NB: rd_obs, RD_OBS and RD_OBS1 (etc) are
treated as the same option in PLT_SPEC, but write different sve files with
distinct names.
BOX file:
A text file containing an ordered sequence
of commands as specfied by .sve files, e.g.,
.rd_mod
.cnvlv
.norm
Type box=filename to write a .box file
containing several .sve files
Type #filename to read .box file.
Particulalry useful for reading in multiple
data sets etc.
Observational Data Files
These are ascii files in column
format. All lines at the top of
the file are ignored until the key FLUX_UNIT= is found. Additional keywords
must follow on consecutive lines, and must contain an =. Only the key FLUX_UNIT
must be present. Available keywords, and their corresponding parameters (not case
sensitive) are described below. Subroutine that reads in data is
$cmfdist/spec_plt/subs/rd_obs_data_v2.f.
FLUX_UNIT |
ergs/cm^2/s/Ang ergs/cm^2/s/Hz mJy milli-Jansky Jansky Norm (normalized data) |
|
|
WAVE_UNIT |
Angstroms Um micrometers Hz |
|
|
AIR_LAM |
True (default
if l >
2000A) False |
|
|
SCALE_FACTOR |
Factor to scale
flux values. |
|
|
DATA_FORM |
HR_IUE (IUE
data format). Single column format. |
|
|
LAM_ST |
Start
wavelength (IUE data format only) |
|
|
DEL_LAM |
Increment (IUE
data format only). |
Input/output:
RD_CONT |
Reads in a model continuum
spectrum. The data is sent directly to the plotting package unless
OVER=.TRUE. This option can be used to read in a continuum. (Similar to
option RD_MOD) [WR]:
Write data to file (logical). Default is FALSE. [SCALE]:
Value to multiply data by. |
RD_EW |
Read in EW file. To plot EW
as a function of Lambda. |
RD_MOD |
Reads in a different model
spectrum (as contained in
OBSFLUX). The data is sent directly to the plotting package unless
OVER=.TRUE. [OVER]=T: Reads in a new model spectrum replacing the existing buffer
spectrum. No plots are done. [SCALE] : Value to normalize the model data by [Logical].(not done if OVER=T) |
RD_OBS |
READ in an observation and
plot it using existing switch settings. [SCALE]:
Value to normalize data by [Logical]. [CLEAN]:
Remove data points with zero flux. Useful for operating on UV data [Logical].
Simply averages the neighboriing data points. Option could be easily
improved. [SMOOTH]: Indicates whether data is to be smoothed. Only option presently
available is HAN. If the data is not monotonic (e.g., for overlapping echelle
orders) each section is smoothed separatley. [RAD_VEL]: Specifies a radial velocity. +ve refers to object moving away. After
correction, wavelengths will be smaller. [OVER]: Write observations into buffer. The observations
can then, for example, be reddened, or dereddened (formerly TREAT_AS_MOD). [WR]: Write data to file (unit 50). |
NORM |
Read in a spectrum, and
divide the present buffer spectrum by it. The existing model spectrum is not
corrupted. Wavelength scales need not be identical. [RD_OBS]: Red in continuum from file in column format. [LIN]: When TRUE, linear interpolation is used. The
default is to use monotonic cubic interpolation. [WR]: Write data to file. [OVER]: When set to T, the normalized spectrim is placed in
the buffer (instead of sending to plot package). [ADD]: Add poissonian noise to spectrum. If TRUE, mean
continuum counts and wavelength range are requested. |
Axis/Unit Options
LX or LOGX or LINX |
Switch between logarithmic
and linear X-AXIS (i.e., do the opposite to current setting) |
XU XUNITS |
Choices: Hz, um, Ang, AA (air
Ang), eV, keV, km/s, mm/s (case
not important). |
LY or LOGY or LINY |
Switch between logarithmic
and linear Y-AXIS (i.e., do the opposite to current setting) |
YU YUNITS |
Choices: FLAM
<=> ergs/cm^2/s/Ang FNU <=> Jy NU_FNU <=>
ergs/cm^2/s |
HZ_IN |
Switches frequency input
units to 10^15 Hz (def) |
KEV_IN |
Switches frequency input
units to KeV |
ANG_IN |
Switches frequency input
units to Angstroms |
|
|
GR |
Enter plot package. |
GRNL |
Enter plot package -- no
labels are passed |
EX |
Exit program |
Spectral options
BB |
Sends a Blackbody spectrum.
normalized by the radius or the flux at a particlar wavelength, to the
plotting package. OVER:
When TRUE, places spectrum in buffer. |
CUM |
Creates the cumulative
luminosity as function of lambda, and passes the data to the plot package. |
CNVLV |
Smooth the spectrum using a
Gaussian. Used for macroturbulance and instrumental broadening. The smoothing
may be carried out either in wavelength space (i.e., with fixed dl ) or in velocity space. Smoothing with fixed dl is the default: For smoothing in velocity space
specifu RES on the command line, i.e.., CNVLV(RES=3000). INST_RES -
Resolution in A. WAVE_MIN - Specify wavelength region WAVE_MAX - Upper
wavelength bound RES
- Ressolutin (l/dl) MIN_RES
- Minimum resolution of model spectrum (km/s FFT - Use FFT for convolution |
EBMV |
Plots A(Lambda) as a
function of X unit. R_EXT ---
(==A(V)/EBMV) If R_EXT is non zero, the
interstellar extinction formulation of Clayton, Cardelli, and Mathis is used.
If R_EXT is zero, the R_EXT is set to 3.1, and the galactic extinction and LMC
extinction laws summarized by Howarth (1983, MNRAS, 203, 301) are used |
EXT |
Extract a spectrum (from
buffer spectrum) at fixed resolution. Buffer spectrum is overwritten. Prior
to this command it may be
necessary to smooth the buffer spectrum to ensure Nyquist sampling theorem is
satisfied. |
FLAM |
Passes data in the buffer
to plot program; command control is then passed to the plot package. The type
of axes are determined by the X and Y axis options. E(B-V) and a distance are requested. Defaults are
zero and 1kpc |
FNU |
Same as FLAM |
GEN |
Combinaton of RD_MOD. ROT,
ISABS & NORM |
ISABS |
Applies interstellar line
absorption (primarily HI and H2) to buffer spectrum. The following
parameters are requested: T_IN_K
- Excitation temperature (km/s). V_TURB -
Turbulent velocity. Used with T_IN_K to compute absoption profile. LOG_NTOT
- HI column density (cm-2) LOG_H2_NTOT - H2 column density (cm-2) HI_ABS
- Allow for HI absorption
(logical) H2_ABS
- Allow for H2
absorption (lgical) V_R
- Radial velocity offset (km/s) WAVE_MIN -
Specifies region to be changed WAVE_MAX MIN_RES
- Minimum model resolution in km/s. |
ROT |
Rotationaly broaden the
spectrum. A simple convolution is performed. Required: Vsini
In km/s. Eps Limb-darkening
parameter -- default=0.5): |
WRFL |
Same as FLAM except data is
written to unit 50. |
Miscellaneous Options
DV |
Plots the coeficients for
the cubic polynomial used to interpolate the buffer spectrum. |
FILT |
|
MAG |
Output approximate
magnitudes in various filter systems. |
ZAN |
Output Zanstra parameters.
For example, the number of
photons emitted shortward of the Lyman limit. |