To find and download HEASARC data in the cloud, you can use astroquery.heasarc or download our new tool, hark.
The HEASARC and NuSTAR teams are greatly saddened by the sudden passing of Katja Pottschmidt. Most recently Katja was the lead scientist for the NuSTAR Guest Observer Facility (GOF), a role she had supported for many years. During her science career she worked on many other high energy astrophysics missions and played an integral role in advancing our knowledge of the universe. She was a wonderful colleague and friend and will be keenly missed by all who knew her.
Next: cph, vcph, bcph, bvcph: Up: Additive Model Components Previous: compTT: Comptonization, Titarchuk Contents
coolflow, vcoolflow, bcoolflow, bvcoolflow: cooling flow, mekal
A cooling flow model after Mushotzky & Szymkowiak (1988). This one differs from cflow in setting the emissivity function to be the inverse of the bolometric luminosity. Abundance ratios are set by the abund command. Redshift is converted to distance using the cosmology set by the cosmo command. The switch parameter determines whether spectrum is calculated by running the mekal code, by interpolating on a pre-calculated mekal table, using the AtomDB data, or using the SPEX data. If the last two of these options are selected then see the documentation on the cie model for a list of the xset options which can be used to change the behaviour of the code.
Velocity broadening can only be used with switch=2 or switch=3.
For the coolflow model the parameters are:
| par1 | low temperature (keV) |
| par2 | high temperature (keV) |
| par3 | abundance relative to Solar |
| par4 | redshift |
| par5 | switch (0 = calculate using mekal, 1 = interpolate using mekal, 2 = use AtomDB data), 3 = SPEX data |
| norm | Mass accretion rate (solar mass/yr) |
For the vcoolflow variant the parameters are:
| par1 | low temperature (keV) |
| par2 | high temperature (keV) |
| par3–par16 | Abundances for He, C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Fe, Ni wrt Solar |
| par17 | Redshift |
| par18 | switch (0 = calculate using mekal, 1 = interpolate using mekal, 2 = use AtomDB data, 3 = SPEX data) |
| norm | Mass accretion rate (solar mass/yr) |
For the bcoolflow model the parameters are:
| par1 | low temperature (keV) |
| par2 | high temperature (keV) |
| par3 | abundance relative to Solar |
| par4 | redshift |
| par5 | gaussian sigma for velocity broadening (km/s) (switch=2 or 3 only) |
| par6 | switch (0 = calculate using mekal, 1 = interpolate using mekal, 2 = use AtomDB data, 3 = SPEX data) |
| norm | Mass accretion rate (solar mass/yr) |
For the bvcoolflow variant the parameters are:
| par1 | low temperature (keV) |
| par2 | high temperature (keV) |
| par3–par16 | Abundances for He, C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Fe, Ni wrt Solar |
| par17 | Redshift |
| par18 | gaussian sigma for velocity broadening (km/s) (switch=2 or 3 only) |
| par19 | switch (0 = calculate using mekal, 1 = interpolate using mekal, 2 = use AtomDB data, 3 = SPEX data) |
| norm | Mass accretion rate (solar mass/yr) |
Next: cph, vcph, bcph, bvcph: Up: Additive Model Components Previous: compTT: Comptonization, Titarchuk Contents