A new implementation of the infrared flux method using the 2MASS catalogue

By J. I. González Hernández, P. Bonifacio, Jonay I. Gonzalez-Hernandez, obspm Fr. 2009

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Context. The effective temperature scale of FGK stars, especially at the lowest metallicities remains a major problem in the chemical abundance analysis of metal-poor stars. Aims. We present a new implementation of the infrared flux method (I RFM) using the 2MASS catalogue. Methods. We computed the theoretical quantities in the 2MASS JHKs filters by integrating theoretical fluxes computed from ATLA S models, and compare them directly with the observed 2MASS JHKs magnitudes. This is the main difference between our imple- mentation of the IRFM and that of Ram´ irez & Melendez (2005, ApJ, 626, 446; hereafter RM05), since to introduce new stars at the lowest metallicities they transform the 2MASS JHKs magnitudes into the TCS photometric system. We merge in our sample the stars from Alonso et al. (1996, AA hereafter AAM96; 1999, AA hereafter AAM99), and other studies to appropriately cover a wide range of metallicities, endin g up with 555 dwarf and subgiant field stars and 264 giant field s tars. We derived a new bolometric flux calibration using the availabl e Johnson-Cousins U BV(RI)C and the 2MASS JHKs photometry. We also computed new Teff versus colour empirical calibrations using our extended sample of stars. Results. We derived effectives temperatures for almost all the stars in the AAM96 and AAM99 samples and find that our scales of temperature are hotter by ∼ 64 K (σT = 104 K, N = 332 dwarfs) and∼ 54 K with aσT = 131 K (N = 202 giants). The same comparison with the sample of RM05 for stars with (Fe/H)<−2.5 provides a difference of∼ −87 K (σT = 194 K, N = 12 dwarf stars) and∼ 61 K (σT = 62 K, N = 18 giant stars). Conclusions. Our temperature scale is slightly hotter than that of AAM96 and RM05 for metal-rich dwarf stars but cooler than that of RM05 for metal-poor dwarfs. We have performed an fully self-consistent IRFM in the 2MASS photometric system. For those who wish to use 2MASS photometry and colour-temperature calibrations to derive effective temperatures, especially for metal-poor stars, we recommend our calibrations over others available in the literature. In our implementation we avoid the transf ormation of the 2MASS JHKs magnitudes to a different photometric system and thus fully exploit the excellent internal consistency of the 2MASS photometric system.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d329151cb50e38ad1742043c2b46b39f17dd28d6

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Citations in the corpus

The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “This sample allows to compare empirically determined Teff values (calibrated on the González Hernández & Bonifacio 2009, temperature scale) with theoretical models of the appropriate chemical composition, that are very sensitive to the treatment of the superadiabatic layers, hence the calibration…”
APOGEE Data Releases 13 and 14: Data and Analysis (2018, methodology): “However, Figure 29 shows the difference between the spectroscopic temperature and photometric temperatures derived from the González Hernández & Bonifacio (2009) photometric calibration, as applied to a low-reddening sample that includes all APOGEE stars with b > 30 and E(B − V ) < 0.02, where…”
Confirmation of the Gaia DR2 Parallax Zero-point Offset Using Asteroseismology and Spectroscopy in the Kepler Field (2018, methodology): “The spectroscopic Teffvalues from APOGEE that we use are calibrated to be in agreement with the infrared flux method (IRFM) photometric scale of González Hernández & Bonifacio (2009) for targets in low-extinction fields.”
The PASTEL catalogue: 2016 version (2016, background): “They mainly come from less reliable determinations in the earliest bibliographic references, or from the most uncertain determinations in González Hernández & Bonifacio (2009) who sometimes quote errors of several hundred K.”
The Solar Twin Planet Search. I. Fundamental parameters of the stellar sample (2014, methodology): “The classic example of the relationship between stellar abundances and planets is the observed higher frequency of giant planets around stars of higher metallicity (e.g., Gonzalez1997; Santos et al. 2004; Valenti & Fischer 2005; Ghezzi et al. 2010).”
A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS (2014, methodology): “Flagstaff, Arizona: Lowell Observatory Giclas, H. L., Burnham, R., Jr., & Thomas, N. G. 1978, Lowell Observatory Bulletin, 8, 89 Gilroy, K. K., Sneden, C., Pilachowski, C. A., & Cowan, J. J. 1988, ApJ, 327, 298 Giridhar, S., Lambert, D. L., Gonzalez, G., & Pandey, G. 2001, PASP, 113, 519 González H”
The Payne: Self-consistent ab initio Fitting of Stellar Spectra (2018, methodology): “For this comparison we only consider giants that have small line-ofsight extinction, i.e., E(B−V )<0.02 from the SFD map (Schlegel et al. 1998), avoid the Galactic disk ( > b 30∣ ∣ ), and have color 0.1<J−K < 0.9 following González Hernández & Bonifacio (2009).”
A Guide to Realistic Uncertainties on the Fundamental Properties of Solar-type Exoplanet Host Stars (2020, methodology): “An example of this “calibration pyramid” is the infrared color-Teff relation by González Hernández & Bonifacio (2009), which is used to calibrate temperatures for hundreds of thousands of giants in large spectroscopic surveys such as APOGEE (Majewski et al. 2017), but hinges on a handful of…”
The PASTEL catalogue of stellar parameters (2010, unknown): “…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 (2009) 814 3745 - 7489 IRFM + colour calibrations a ratio higher than 100, although it is possible that some results…”
THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, methodology): “The Teff Calibration The ASPCAP spectroscopic effective temperatures were compared with photometric ones using calibrations by González-Hernández & Bonifacio (2009), hereafter GHB09, using 2MASS J − Ks colors (Skrutskie et al. 2006).”
STELLAR DIAMETERS AND TEMPERATURES. III. MAIN-SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS (2013, methodology): “Figure 20 shows the results of this comparison, displaying side-by-side the effective temperatures using the Casagrande et al. (2010) and González Hernández & Bonifacio (2009) relations (left and right, respectively).”
Red giant masses and ages derived from carbon and nitrogen abundances (2015, unknown): “As an exception to the rule generally used in this paper, we do not use here the raw ASPCAP values of T eff , but use instead the values that are calibrated to match the photometric temperatures calculated from the 2MASS J − K s colour (as in Gonz´alez Hern´andez & Bonifacio 2009).”
A non-LTE study of neutral and singly-ionized iron line spectra in 1D models of the Sun and selected late-type stars ? (2011, methodology): “For HD 84937 the infrared flux method (IRFM) temperatures of Alonso et al. (1996); Meléndez & Ramírez (2004); González Hernández & Bonifacio (2009), and Casagrande et al. (2010), Teff = 6330 K, 6345 K, 6333 K, and 6408 K, respectively, are consistent within 1σ.”
Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18 (2019, methodology): “In fact, to remove systematics with respect to the temperature scale defined by the infra-red flux method (González Hernández & Bonifacio 2009), for DR14 and following releases a metallicity- and temperature dependent calibration was applied to the raw ASPCAP results (Holtzman et al. 2018; Jönsson…”
An absolutely calibrated T eff scale from the infrared flux method. Dwarfs and subgiants (2010, methodology): “Finally, we suspect that the trend forTeff 5000 K is due to the absence of (RI)C colours in González Hernández & Bonifacio (2009) (Section 2.2, bottom panel of Figure 2).”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “The determinations by González Hernández & Bonifacio (2009) and Casagrande et al. (2011) are both based on the IRFM with 2MASS colour indices.”