DOI: 10.24378/exe.63
title: What can the SEDs of first hydrostatic core candidates reveal about their nature? (dataset)

description: This is the dataset that was used to produce the associated paper, published in MNRAS. It contains the output from each of the SPH simulations, including dump files, model SED files and scripts used for the photometry and SED fitting. To view the paper follow the DOI or linked handle.
description: The file ModelSEDs_Scripts.zip contains the model SEDs used for fitting the observations, the other SEDs shown in the paper, python scripts for fitting model SEDs to observations and the instrument data necessary for the latter. The model SEDs are text files (.dat) and are named according to the model. e.g. 1MB09BK_FC00068_10um_inc045.dat “1M” = 1solar mass “B09” rotation rate beta=0.09 “FC00068” number of dump file: see SEDsTable.pdf for which snapshot this refers to. “10um” max grain size of 10 micron Grain type: “amc” or “sil”. If none specified, the model used silicates. “inc045” inclination The dump file numbers corresponding to each snapshot for the SEDs used in fitting are given in SEDsTable.pdf in ModelSEDs_Scripts. In the PythonScripts directory that is in ModelSEDs_Scripts, model_phot_list.py generates photometry for a list of model SEDs and uses the module phot.py and the instrument data (filter profiles and the index file intruments.txt). Instructions are included in the script. Fconvert.py converts a filter profile in frequency format to wavelength format. The FitThisSED_phot.py script scales and compares a list of synthetic SEDs generated by model_phot_list.py to a chosen observed SED. This output can be plotted with PlotFits.py. Again, instructions are given in the python scripts. The file plot_radial_profiles.ipynb is a Jupyter notebook to plot the radial intensity profiles shown in Fig.5. The output from the SPH calculations can be found in the remaining zip files. The files containing radiation hydrodynamical calculations are labelled using RHD1 or RHD2, “1M”/“2M” … for 1 solar mass / 2 solar mass and “B01”/“B05”… for beta= 0.01, beta=0.05 etc for the initial ratio of rotational to gravitational potential energy. If the mass is not given, the mass was 1 solar mass. For the RHD1 files, the initial temperature is given (7K/10K/15K). Files that include a string like “BD1e20…” refer to the calculations that had an additional boundary column density (e.g. 1e20 H2 molecules). Calculations that employed different radii cores include a string such as “radii_R3e16”, that refers to an initial core radius of 3e16cm. The zip files labelled MU5_BKRT_B005_[a-d] contained the output from the Mu=5 Beta=0.005 RHD2 radiation magnetohydrodynamical calculation, including the dump shown in the density snapshot (BMHD127). The SPH dump files are provided for all of the calculations discussed in the paper - a summary is shown in Table 1. These are Fortran binary files, written in big endian format and generated by the sphNG code. They can be read and visualised using the free, publicly available SPLASH visualisation code written by Daniel Price. SPLASH can be downloaded from http://users.monash.edu.au/~dprice/splash/ . The files besphere* and be_mhd* that may be contained within each of the calculation zip files contain a summary of the dumps including times, maximum densities and temperatures.
description: The article associated with this dataset is located in ORE at: http://hdl.handle.net/10871/30603