CMDfit Bolometric Corrections
Most of the bolometric corrections provided we have calculated ourselves by folding spectra through the appropriate filter responses. In addition, by reddening the spectra before folding them through the resposes, we produce extinction tables. The atmospheres we have used are the BT-Settl (Allard et al, 2011) and the Kurucz (Castelli & Kurucz, 2004) new opacity, microturbulance 2km/s models. The optical filter resposes we have are Bessell, INT-WFC, IPHAS/UVEX and SDSS. In many cases we provide both photon counting and energy integrating versions, the former being suitable for CCD detectors, the latter for photomultiplier tubes. In the IR we have the 2MASS and UKIDSS filters. The extinctions are calculated using the Fitzpatrick (1999) curve, since Yuan el al (2013) show this reproduces the observed extinctions in the optical and near IR well. The references for the system responses are as follows.
Bessell. The UBVRI Johnson-Cousins system defined in Bessell & Murphy (2012).
INT-WFC. The UgriZ system with an AB zeropoint described in Bell et al (2012).
IPHAS/UVEX. Bolometric corrections for the IPHAS and UVEX ugri surveys with the INT. Created using the system responses in Bell et al (2012), but with the zero point set to be Vega.
SDSS. The ugriz system with an AB zeropoint defined in Doi et al (2010).
2MASS. The JHKs system described in Cohen, Wheaton & Megeath (2003).
In addition we provide the following sets of published tables of bolometric corrections.
The Bell et al (in prep) tuning to the Pleiades or Praesepe is noted in the options as "BT-Settl/Bell". It is only available for certain interior models. The tuning (which is for temperatures cooler than about 4000K) is based on the BT-Settl model atmospheres. Above about 4000K the tables are either the BT-Settl BCs (for temperatures less than 8000K), or the Kurucz BCs (temperatures greater than 8000K).
Jeffries/Naylor. These are available on request (since we believe they are superceded by Bell et al). The bolometric corrections are derived from fitting observations for cool low-mass stars, and from Bessell, Castelli & Plez (1998) for the the hooter stars. The technique is outlined in Naylor et al (2002). In one case the bolometric correction is from Flower (1996). The conversions from effective temperature are derived from fitting the Pleiades ("Pleiades tuning") and is described in Jeffries et al (2001).
Bessell Tycho: Bolometric corrections and effective temperature to colour conversions into the Hipparcos Tycho system from Bessell (2000). Currently there are no extinctions available.
Kenyon & Hartmann (1995). The emprical tables from Kenyon & Hartmann (1995).
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