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):
    I(
m) = 1 - e + me

 

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.