The package provides utility code developed to facilitate the distribution and usage of IR templates presented in Boquien & Salim (2021). It contains three routines:
- bosa-templates for extracting custom templates (average IR spectra)
- bosa-estimators for estimating LTIR and SFR (total, obscured plus unobscured)
- bosa-plotter
The package requires python 3.8 or later and depends on three external libraries, numpy, matplotlib and astropy. The installation follows the standard python way: python setup.py install. Note that the data file take >140 MB, so if you want to keep the files locally rather than having a system-wide copy, you can do python setup.py develop --user.
The package contains:
- This
README.mdfile. - The source with the
estimators,plotter, andtemplatespackages. - Data files in
pickleformat insrc/*/data.
This routine produces average IR spectra (templates) corresponding to arbitrary TIR luminosities (single parameter mode), or arbitrary LTIR/sSFR combinations (two parameter mode). These luminosities must be provided as arguments and must be in logarithmic units and in solar luminosities between 10⁹ and 10¹² Lsun (a warning will be displayed if beyond these bounds). For instance bosa-templates LTIR 10 11 12 will produce the LTIR.fits with three spectra. Note that the script will display an exception if a file already exists in order not to accidentally overwrite files. In single parameter mode LTIR can be replaced with some other parameter: Mdust, Mstar, SFR, sSFR, or Z. Spectra averaged in LTIR, Mdust, Mstar, and SFR are in absolute luminosity, whereas the ones in sSFR and Z are normalized to 1 Lsun. Parameters are in log for all the properties except for Z, which is in 12+log O/H. In two parameter mode (e.g., bosa-templates LTIR 10 11 12 sSFR -10 -9.5) code produces LTIR-sSFR.fits with 6 spectra in this case.
The output files have wavelength in units of nm and nuLnu in units of solar luminosities.
This routine estimates LTIR and the SFR based on one of more (up to four) fluxes as an input. One column must contain redshifts and be named redshift and one must be named sSFR and it should contain log sSFR if known, or some placeholder values if not. Fluxes are specified using column names:
spitzer.irac.ch4spitzer.mips.24herschel.pacs.70herschel.pacs.100herschel.pacs.160herschel.spire.PSWherschel.spire.PMWherschel.spire.PLWjwst.miri.F770Wjwst.miri.F1000Wjwst.miri.F1130Wjwst.miri.F1280Wjwst.miri.F1500Wjwst.miri.F1800Wjwst.miri.F2100Wjwst.miri.F2550WWISE3WISE4
Output includes LTIR in Lsun and SFR in Msun/year calculated based on each filter individually and L(TIR) parameterized templates, also on L(TIR)+sSFR parameterized templates, and finally based on all flux points simultaneously. In order not to accidentally erase data, the script will refuse to run if columns of that name are already present in the file.
Questions and suggestions are welcome and can be sent to Médéric Boquien, [email protected].