genShark | R Documentation |
Takes Shark boxes and converts to apparent and absolute SEDs.
genShark(path_shark = ".", path_out = ".", snapshot = NULL,
subvolume = NULL, redshift = "get", h = "get", cores = 4,
id_galaxy_sam = "all", filters = c("FUV_GALEX", "NUV_GALEX",
"u_SDSS", "g_SDSS", "r_SDSS", "i_SDSS", "Z_VISTA", "Y_VISTA",
"J_VISTA", "H_VISTA", "K_VISTA", "W1_WISE", "W2_WISE",
"W3_WISE", "W4_WISE", "P100_Herschel", "P160_Herschel",
"S250_Herschel", "S350_Herschel", "S500_Herschel"), 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, stellarpop = "BC03lr",
speclib = NULL, read_extinct = FALSE, sparse = 5, final_file_output = "Shark-SED.csv",
extinction_file = "extinction.hdf5", intSFR = TRUE, addradio_SF = FALSE,
waveout = seq(2, 30, by = 0.01), ff_frac_SF = 0.1, ff_power_SF = -0.1,
sy_power_SF = -0.8, verbose = TRUE, write_final_file = FALSE,
mode = "photom")
path_shark |
Character scalar; path to top directory containing Shark outputs. The package will check that the files and path exists and we have read access. |
snapshot |
Integer scalar; snapshot number to use. |
subvolume |
Integer scalar; sub-volume snapshot number to use. |
redshift |
Numeric vector; can be a single value for all galaxies, or a vector the same length as select. If set to "get" (default) it will inherit the redshift from the target Shark snapshot and subvolume, which is probably what you want most of the time. |
h |
Numeric scalar; little-h assumed in Shark (needed to convert SFRs to actual SFR since they use Msun/yr/h). If set to "get" (default) it will inherit the redshift from the target Shark snapshot and subvolume, which is probably what you want most of the time. |
cores |
Integer scalar; number of cores to process on. |
id_galaxy_sam |
Integer vector; Shark IDs to extract for photometric processing. The default ('all') will process all galaxies in the sub-volume and snapshot requested. |
filters |
Character vector; filters to use for the photometry. |
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 |
read_extinct |
Logical; should an HDF5 be read in to vary extinction values per galaxy? |
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. |
final_file_output |
Character scalar; name for the final output file to write to. This should not be an existing file and end ".csv". |
extinction_file |
Character scalar; name of extinction file. Only relevant if read_extinct=TRUE. |
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 |
verbose |
Logical; should helpful verbose outputs be printed regarding the processing? |
write_final_file |
Logical; whether to write the output of this function into a .csv file within the path_shark directory. |
mode |
Character scalar; should the output be photometry in filters (photom) or the full resolution spectrum (spectrum). |
By default outputs all SEDs in the box.
Note the output absolute magnitudes are rest frame, whilst the apparent magnitudes are observed frame.
The apparent and absolute magnitudes are physical assuming a fixed H0=67.8 km/s/Mpc (Planck 2018) cosmology. This cannot be changed by the user (to remove silly H0 mistakes), so you should add 5.log10(0.678) (which is -0.844) to the absolute magnitudes if you want H0=100 km/s/Mpc type magnitudes. You should not adjust the apparent magnitudes since the Universe does not look different just because we change our mind about H0, and nor should our apparent magnitudes!
Data.frame of named absolute and apparent magnitudes for bulge, disk and total photometry.
Aaron Robotham
genSED
, genSting
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