Effective temperature scale and bolometric corrections from 2MASS photometry

By Eduard Masana, C. Jordi, I. Barcelona, I. D. E. D. Catalunya. 2006

168 citations recorded by the source corpus.

We present a method to determine effective temperatures, angular semi-diameters and bolometric corrections for population I and II FGK type stars based on V and 2MASS IR photometry. Accurate calibration is accomplished by using a sample of solar analogues, whose average temperature is assumed to be equal to the solar effective temperature of 5777 K. By taking into account all possible sources of error we estimate associated uncertainties to better than 1% in effective temperature and in the range 1.0–2.5% in angular semi-diameter for unreddened stars. Comparison of our new temperatures with other determinations extracted from the literature indicates, in general, remarkably good agreement. These results suggest that the effective temperaure scale of FGK stars is currently established with an accuracy better than 0.5%–1%. The application of the method to a sample of 10 999 dwarfs in the Hipparcos catalogue allows us to define temperature and bolometric correction (K band) calibrations as a function of (V − K), [m/H ]a nd logg. Bolometric corrections in the V and K bands as a function of Teff ,[ m/H] and log g are also given. We provide effective temperatures, angular semi-diameters, radii and bolometric corrections in the V and K bands for the 10 999 FGK stars in our sample with the corresponding uncertainties.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4d19dce9cedf7956e451f747b3b339d171d6f9ef

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In Astronomy and Astrophysics

1. J. Southworth
2. J. Winn
3. D. Charbonneau
4. Debra A. Fischer
5. J. Johnson
6. G. Marcy
7. I. Ramírez
8. Eric Mamajek

In Instrumentation

1. J. Southworth
2. J. Winn
3. Eric Mamajek
4. G. Marcy
5. J. Johnson
6. D. Charbonneau
7. I. Ramírez
8. Luca Casagrande

Citations in the corpus

• The Stellar Populations of Praesepe and Coma Berenices (2007, methodology): “We estimated absolute bolometric magnitudes for each model using the bolometric corrections of Masana et al. (2006).”
• The Transit Light Curve Project. V. System Parameters and Stellar Rotation Period of HD 189733 (2006, methodology): “Ultimately, Bakos et al. (2007) adopted the value 0:758 0:016 R based on a calibration of 2MASS photometry by Masana et al. (2006).”
• THE ARAUCARIA PROJECT. THE DISTANCE TO THE SMALL MAGELLANIC CLOUD FROM LATE-TYPE ECLIPSING BINARIES (2013, unknown): “…several calibrations between colors and effective temperatures (di Benedetto 1998; Alonso et al. 1999; Houdashelt et al. 2000; Ramı́rez & Meléndez 2005; Masana et al. 2006; González H. & Bonifacio 2009; Casagrande et al. 2010; Worthey & Lee 2011) to set new temperatures for the primaries.”
• A BCool magnetic snapshot survey of solar-type stars (2013, background): “…−0.000 X 1.7+0.2 −0.2 +0.307+0.017 −0.013 1 References: 1: Valenti & Fischer (2005), 2: Takeda et al. (2007a), 3: Boyajian et al. (2012), 4: Wu et al. (2011), 5: Herrero et al. (2012), 6: Delfosse et al. (1998), 7: do Nascimento Jr (private communication), 8: Holmberg et al. (2009), 9:…”
• Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first Super-Earth with measured radius (2009, unknown): “Using Exodat (Deleuil et al. 2009) and 2MASS photometry, the Masana et al. (2006) calibration yields Teff = 5300± 70 K.”
• XHIP: An extended hipparcos compilation (2011, methodology): “Luminosities are also computed based on V with a bolometric adjustment applied from correction figures supplied by Masana et al. (2006) when available, otherwise (when B-V < 1.6) from the B-V indexed tables of Flower (1996).”
• HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, methodology): “As a check on Teff , we collected all available photometry for HD 147506 in the Johnson, Cousins, 2MASS, and Tycho systems, and applied a number of color-temperature calibrations (Ramı́rez & Meléndez 2005; Masana et al. 2006; Casagrande et al. 2006) using 7 different color indices.”
• Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “The highest value of ∼5900 K is given by Masana et al. (2006), who used a spectral energy distribution fit method with V and 2MASS photometry.”
• The PASTEL catalogue of stellar parameters (2010, unknown): “…IRFM di Benedetto (1998) 533 3846 - 10021 surface brightness+ V-K calibration Kovtyukh et al. (2003, 2004, 2006) 645 3700 - 6118 Line Depth Ratios Masana et al. (2006) 10999 3748 - 7987 SED fit+ V-K calibration Ramı́rez & Meléndez (2005) 754 3535 - 9233 IRFM González Hernández & Bonifacio…”
• Accurate fundamental parameters for lower main‐sequence stars (2006, methodology): “Interestingly, an offset of 0.075 mag in the H band zero-point given by the 2MASS has also been claimed by Masana et al. (2006) to constrain a set of solar analogues to have just the same temperature of the Sun.”
• Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, methodology): “Masana et al. (2006) have also found a difference of 100 K with the IRFM Teff scale using their spectral energy distribution fit method.”
• An absolutely calibrated T eff scale from the infrared flux method. Dwarfs and subgiants (2010, methodology): “This rationalec n be extended to other physical properties, namely using the solar effective temperatureTeff,⊙ = 5777 K as the average value for solar-type stars (e.g. Masana et al. 2006).”
• INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, methodology): “Therefore we attempt to infer the effective temperatures by simultaneously fitting the observed photometry to synthetic models (the “Spectral Energy Distribution Fitting” (SEDF) method, see Masana et al. 2006).”