fm_unred {astrolibR}R Documentation

Deredden a flux vector using the Fitzpatrick (1999) parameterization

Description

Deredden a flux vector using the Fitzpatrick (1999) parameterization

Usage

fm_unred(wave, flux, ebv, r_v = 3.1, avglmc=FALSE, lmc2=FALSE, x0=NULL,  
gamma=NULL, c4=NULL, c3=NULL, c2=NULL, c1=NULL)

Arguments

wave

wavelength in Angstroms, scalar or N-vector

flux

calibrated flux vector, scalar or N-vector

ebv

color excess E(B-V), scalar

r_v

ratio of total to selected extinction, (optional, default=3.1

avglmc

if set to TRUE, then the default fit parameters (c1,c2,c3,c4,gamma,x0) are set to the average values determined for reddening in the general Large Magellanic Cloud (LMC) field by Misselt et al. (1999), (optional)

lmc2

if set to TRUE, then the fit parameters are set to the values determined for the LMC2 field (including 30 Dor) by Misselt et al. Note that neither /AVGLMC or /LMC2 will alter the default value of R_V which is poorly known for the LMC.

x0

Centroid of 2200 A bump in microns (optional, default = 4.596)

gamma

Width of 2200 A bump in microns (optional, default = 0.99)

c4

FUV curvature (optional, default = 0.41)

c3

Strength of the 2200 A bump (optional, default = 3.23)

c2

Slope of the linear UV extinction component (optional, default = -0.824 + 4.717/R)

c1

Intercept of the linear UV extinction component (optional, default = 2.030 - 3.007*c2)

Details

The Galactic extinction curve is given by Fitzpatrick & Massa (FM, 1999). Parameterization is valid from the infrared to the far-ultraviolet (3.5 microns to 0.1 microns). The ultraviolet extinction curve is extrapolated down to 912 Angstroms. Many sightlines with peculiar ultraviolet interstellar extinction can be represented with the FM curve, if the proper value of R(V) is supplied.

When the inputs omit extinction curve parameters (x0, gamma, c4, c3, c2, and c1) then the default extinction curve is adopted from Clayton et al. (2003).

The parameter R_V specifies the ratio of total to selective extinction, R(V) = A(V) / E(B - V). Extreme values of R(V) range from 2.3 to 5.3, and the default is 3.1.

If a negative ebv is supplied, then fluxes will be reddened rather than dereddened.

The following comparisons between the FM curve and that of Cardelli, et al. (CCM, 1989) have been made (see function ccm_unred):
a) In the ultraviolet, the FM and CCM curves are similar for R < 4.0, but diverge for larger R
b) In the optical region, the FM more closely matches the monochromatic extinction, especially near the R band

Value

extcurve

E(wavelength - V)/E(B-V) extinction curve, interpolated onto the input wavelength vector

Author(s)

Written W. Landsman Raytheon STX October, 1998

R adaptation by Arnab Chakraborty June 2013

References

Cardelli, J.A., Clayton, G. C., Mathis, J. S., 1989, The relationship between infrared, optical, and ultraviolet extinction, Astrophys. J. 345, 245-256. http://adsabs.harvard.edu/abs/1989ApJ...345..245C

Clayton, G. C., Wolff, M. J., Sofia, U. J., Gordon, K. D., Misselt, K. A., 2003, Dust grain size distributions from MRN to MEM, Astrophys. J., 588, 871-880. http://adsabs.harvard.edu/abs/2003ApJ...588..871C

Fitzpatrick, E. L., 1999, Correcting the effects of interstellar extinction, Publ. Astron. Soc. Pacific, 111, 63-75. http://adsabs.harvard.edu/abs/1999PASP..111...63F

Misselt, K. A., Clayton, G. C., Gordon, K. D., 1999, A reanalysis of the ultraviolet extinction from interstellar dust in the Large Magellanic Cloud, Astrophys. J. 515, 128-139. http://adsabs.harvard.edu/abs/1999ApJ...515..128M

See Also

polyidl spline

Examples

w <- 1200 + seq(50, 2000, by=50)  # wavelength vector
f <- rep(1, length(w))   # flat initial spectrum
fm_unred(w, f, ebv=0.1)

[Package astrolibR version 0.1 Index]