genSED | R Documentation |
Convert target bulge and disk SFHs to SEDs.
genSED(SFRbulge_d, SFRbulge_m, SFRdisk, redshift = 0.1, time = NULL,
tau_birth = 1, tau_screen = 0.3, tau_AGN = 1, pow_birth = -0.7,
pow_screen = -0.7, pow_AGN = -0.7, alpha_SF_birth = 1, alpha_SF_screen = 3,
alpha_SF_AGN = 0, emission = FALSE, IGMabsorb = FALSE, Zbulge_d = 5,
Zbulge_m = 5, Zdisk = 5, AGNlum = 0, ab_nodust = TRUE, ap_nodust = TRUE,
ab_dust = TRUE, ap_dust = TRUE, emitdust = TRUE, unimax = 1.38e+10,
speclib = NULL, Dale = NULL, AGN = NULL, LKL10 = NULL, filtout = NULL,
H0 = 67.8, sparse = 5, intSFR = TRUE, addradio_SF = FALSE,
waveout = seq(2, 10, by = 0.01), ff_frac_SF = 0.1, ff_power_SF = -0.1,
sy_power_SF = -0.8, mode = "photom", spec_range = c(3600, 9600))
SFRbulge_d |
Numeric vector; star formation rate of the bulge (formed via disk instabilities) in units of physical Msun/yr (i.e. scaled by the correct value of H0, so a value near 70 km/s/Mpc). This is key since most simulations will natively output Msun/yr/h, so be careful here! |
SFRbulge_m |
Numeric vector; star formation rate of the bulge (formed via mergers) in units of physical Msun/yr (i.e. scaled by the correct value of H0, so a value near 70 km/s/Mpc). This is key since most simulations will natively output Msun/yr/h, so be careful here! |
SFRdisk |
Numeric vector; star formation rate of the disk in units of physical Msun/yr (i.e. scaled by the correct value of H0, so a value near 70 km/s/Mpc). This is key since most simulations will natively output Msun/yr/h, so be careful here! |
redshift |
Numeric scalar; redshift of the galaxy for computing apparent magnitudes. Must be above 0! |
time |
Numeric vector; lookback time in years. Must be same length as SFRbulge and SFRdisk. |
tau_birth |
Numeric scalar; dust tau for birth clouds. Associated with sub 10 Myr star formation. See |
tau_screen |
Numeric scalar; dust tau for screen. See |
pow_birth |
Numeric scalar; power to further raise the dust attenuation of birth clouds. See |
pow_screen |
Numeric scalar; power to further raise the dust attenuation of the dust screen. See |
Zbulge_d |
Numeric vector; metallicity of star formation in the bulge (formed via disk instabilities). Can be a single value or a vector that matches the history, in which case it must be same length as SFRbulge. |
Zbulge_m |
Numeric vector; metallicity of star formation in the bulge (formed via mergers). Can be a single value or a vector that matches the history, in which case it must be same length as SFRbulge. |
Zdisk |
Numeric vector; metallicity of star formation in the disk. Can be a single value or a vector that matches the history, in which case it must be same length as SFRdisk. |
alpha_SF |
Numeric scalar; desired interpolated alpha slope of the star forming population. See |
AGNfrac |
Numeric scalar; desired interpolated AGN fraction. See |
ab_nodust |
Logical; should absolute magnitudes for intrinsic SEDs be conmputed? |
ap_nodust |
Logical; should apparent magnitudes for intrinsic SEDs be conmputed? |
ab_dust |
Logical; should absolute magnitudes for dust attenuated SEDs be conmputed? |
ap_dust |
Logical; should apparent magnitudes for dust attenuated SEDs be conmputed? |
emitdust |
Logical; should attenuated light be re-emitted via Dale dust templates? |
unimax |
Numeric scalar; maximum allowed age of any stellar population relative to z=0 (i.e. today). Any star formation implied by massfunc that is older than this will be set to 0. |
speclib |
Pass in the spectral library directly. Must be one of |
Dale |
Pass in the Dale dust library directly. Must be one of |
filtout |
Pass in the photometric filters directly. If |
H0 |
Numeric scalar; Hubble constant as defined at z=0 (default is H0=67.8 (km/s)/Mpc, i.e. Planck 2018). This only adjusts the output absolute magnitudes, i.e. it acts like it would do in observations where apparent magniatudes of a galaxy do not change just because we update our knowledge of H0, but the absolute values computed will change. |
sparse |
Numeric scalar; amount of sparse sampling of the spectra to make. Higher values mean coarser spectra is processed, which means less accurate photometry, but faster processing. Generally done when computing higher resolution libraries for AB mags. |
intSFR |
Logical; should the massfunc be intergrated between ages? This might be necessary if the SFH is quite bursty, but it is more expensive to compute and not required if the SFH is quite smooth. |
addradio_SF |
Logical; should radio flux from star formation be included in the output? |
waveout |
Numeric vector; desired output log10 wavelength grid to use in Ang. See |
ff_frac_SF |
Numeric scalar; free-free HII nebular plasma thermal radio emission contribution fraction at 1.4 GHz used in |
ff_power_SF |
Numeric scalar; power-law slope of the free-free nebular plasma thermal radio emission associated with star-formation used in |
sy_power_SF |
Numeric scalar; power-law slope of the synchrotron radio emission associated with star-formation used in |
mode |
Character scalar; should the output be photometry in filters (photom) or the full resolution spectrum (spectrum). |
spec_range |
Numeric vector; the spectral wavelength range to limit the mode = 'spectrum' output to in Angstrom. |
Lower level function for computing bulge and disk SEDs. Most users will not use this function directly.
Note the output absolute magnitudes are rest frame, whilst the apparent magnitudes are observed frame.
List of named absolute and apparent magnitudes for bulge, disk and total photometry.
Aaron Robotham
genShark
, genSting
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