UBVJHK synthetic photometry of Galactic O stars

By Fabrice Martins, B. A. M. Garching, Graal Montpellier. 2006

250 citations recorded by the source corpus.

Aims. The development of powerful infrared observational technics enables the study of very extincted objects and young embedded star forming regions. This is especially interesting in the cont ext of massive stars which form and spend a non negligible fraction of their life still enshrouded in their parental molecular cloud. Spectrophotometric calibrations are thus necessary to constrain the ph ysical properties of heavily extincted objects. Methods. Here, we derive UBVJHK magnitudes and bolometric corrections from a grid of atmosphere models for O stars. Bessel passbands are used. Bolometric corrections (BC) are derived as a function of Teff and are subsequently used to derive BC− spectral type (S T) and Absolute Magnitudes−S T relations. Results. Infrared magnitudes and, for the first time, bolometric corr ections are given for the full range of spectral types and luminosity classes. Infrared colors are essentially constant. ( H− K)0 is 0.05 mag bluer than previously proposed. Optical calibrations are also provided and are similar to previous work, except for (B− V)0 which is found to be at minimum -0.28 for standard O stars, slightly larger (0.04 mag) than commonly accepted. Conclusions. We present a consistent set of photometric calibrations of optical and infrared magnitudes and bolometric corrections for Galactic O stars as a function of Teff and spectral type based on non-LTE atmosphere models including winds and line-blanketing.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/16dd89b416eb06e0c1bd7f7f0c2b9ff3db573409

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, result): “V )o colors of O9/B0 dwarfs are -0.32 to -0.31 (among the calibrator stars e.g. 10 Lac, σ Sco, τ Sco, and υ Ori), in agreement with Johnson’s classic work (e.g. Johnson & Morgan 1953; Johnson 1966, but at odds with the recent work of Martins & Plez (2006) who claim that (B–”
The relation between the most-massive star and its parental star cluster mass (2009, background): “It is based on Martins et al. (2005) and Martins & Plez (2006) who provide two new transformations of O-star spectral types into masses, which are both rather similar.”
SOUTHERN MASSIVE STARS AT HIGH ANGULAR RESOLUTION: OBSERVATIONAL CAMPAIGN AND COMPANION DETECTION (2014, methodology): “We used the absolute H-band magnitude of O stars listed in Martins & Plez (2006) to estimate the maximum distance at which an isolated O star can be located for its apparent magnitude to be brighter than our cut-off of H = 7.5.”