genSED: Generate SED

Description Usage Arguments Details Value Author(s) See Also Examples

View source: R/genSED.R

Description

Convert target bulge and disk SFHs to SEDs.

Usage

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genSED(SFRbulge_d, SFRbulge_m, SFRdisk, redshift = 0.1, time = NULL, tau_birth = 1,
tau_screen = 0.3, pow_birth = -0.7, pow_screen = -0.7, Zbulge_d = 5, Zbulge_m = 5,
Zdisk = 5, alpha_SF = 1, AGNfrac = 0, ab_nodust = TRUE, ap_nodust = TRUE, ab_dust = TRUE,
ap_dust = TRUE, emitdust = TRUE, unimax = 1.38e+10, speclib = NULL, Dale = NULL,
filtout = NULL, H0 = 67.8, sparse = 5, intSFR = TRUE)

Arguments

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 SFH.

tau_screen

Numeric scalar; dust tau for screen. See SFH.

pow_birth

Numeric scalar; power to further raise the dust attenuation of birth clouds. See CF_birth.

pow_screen

Numeric scalar; power to further raise the dust attenuation of the dust screen. See CF_screen.

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 Dale_interp.

AGNfrac

Numeric scalar; desired interpolated AGN fraction. See Dale_interp.

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 BC03lr, BC03hr, EMILES. Doing this speeds up the compute time, since there is no need to lazy load from the package.

Dale

Pass in the Dale dust library directly. Must be one of Dale_Orig, Dale_Msol, Dale_NormTot, Dale_NormAGN, Dale_NormSFR. Doing this speeds up the compute time, since there is no need to lazy load from the package.

filtout

Pass in the photometric filters directly. If filters is a vector of filter names, this can be achieved efficiently with a command like: filtout=foreach(i = filters)%do%getfilt(i) (see getfilt).

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.

Details

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.

Value

List of named absolute and apparent magnitudes for bulge, disk and total photometry.

Author(s)

Aaron Robotham

See Also

genShark, genSting

Examples

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# Nothing yet!

asgr/Viperfish documentation built on Oct. 18, 2020, 12:01 p.m.