A new extensive library of PHOENIX stellar atmospheres and synthetic spectra

By T. Husser, S. W. Berg, S. Dreizler, Derek Homeier, A. Reiners, Travis S. Barman, Peter Hauschildt. 2013

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Aims. We present a new library of high-resolution synthetic spectra based on the stellar atmosphere code PHOENIX that can be used for a wide range of applications of spectral analysis and stellar parameter synthesis. Methods. The spherical mode of PHOENIX was used to create model atmospheres and to derive detailed synthetic stellar spectra from them. We present a new self-consistent way of describing micro-turbulence for our model atmospheres. Results. The synthetic spectra cover the wavelength range from 500 A to 5.5 μm with resolutions of R = 500 000 in the optical and near IR, R = 100 000 in the IR and Δλ = 0.1 A in the UV. The parameter space covers 2300 K ≤ Teff ≤ 12 000 K, 0.0 ≤ log g ≤ +6.0, −4.0 ≤ [Fe/H] ≤ +1.0, and −0.2 ≤ [α/Fe] ≤ +1.2. The library is a work in progress and we expect to extend it up to Teff = 25 000 K.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/792b1fa0ca8b0ab9deb56792aa3e89b05b8a8fc7

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Citations in the corpus

The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument (2022, methodology): “The radial velocities of stars in the MWS are determined by chi-square fitting of the spectra by interpolated templates (Koposov et al. 2011) from the PHOENIX stellar library (Husser et al. 2013) using the rvspecfit8 code (Koposov 2019).”
Atmospheric characterization of Proxima b by coupling the Sphere high-contrast imager to the Espresso spectrograph (2016, methodology): “We simulate the high-resolution spectrum of Proxima using the PHOENIX stellar spectral library (Husser et al. 2013).”
A detached stellar-mass black hole candidate in the globular cluster NGC 3201 (2018, methodology): “After the extraction of point sources, the individual spectra of the 20 visits are fitted against our Göttingen Spectral Library (Husser et al. 2013) of synthetic PHOENIX spectra to determine the stellar effective temperature and metallicity as well as radial velocities and the telluric absorption ”
ZODIACAL EXOPLANETS IN TIME (ZEIT). III. A SHORT-PERIOD PLANET ORBITING A PRE-MAIN-SEQUENCE STAR IN THE UPPER SCORPIUS OB ASSOCIATION (2016, methodology): “We applied a prior on limb darkening derived from the Husser et al. (2013) atmospheric models, calculated using the LDTK toolkit (Parviainen & Aigrain 2015), which enabled us to account for errors in stellar parameters and finite grid spacing.”
ExoMol molecular line lists – XXXIII. The spectrum of Titanium Oxide (2019, methodology): “13 shows a comparison between synthetic spectra generated using the present TOTO line list data with Plez-2012, a PHOENIX stellar photosphere model that uses a previous version of the Plez line list (Husser et al. 2013), and the HARPS observation of GL 581.”
The hidden giant: discovery of an enormous Galactic dwarf satellite in Gaia DR2 (2018, background): “0 spectral library (Husser et al. 2013) that spans a large range of metallicities (from [Fe/H] =−4 to [Fe/H] = 1, [α/Fe] between −0.2 and 1.2) and stellar atmospheric parameters.”
The Transit Light Source Effect: False Spectral Features and Incorrect Densities for M-dwarf Transiting Planets (2017, methodology): “Both model grids are based on the stellar atmosphere code PHOENIX (Hauschildt & Baron 1999), with the DRIFT-PHOENIX model grids including additional physics describing the formation and condensation of mineral dust clouds (Woitke & Helling 2003, 2004; Helling & Woitke 2006; Helling et al. 2008a,b; W”
The CARMENES search for exoplanets around M dwarfs (2018, methodology): “The photospheric parameters of the stars were determined as in Passegger et al. (2018) using the latest grid of PHOENIX-ACES model spectra (Husser et al. 2013) and the method described in Passegger et al. (2016).”
The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure (2018, methodology): “The most prominent zones of avoidance (nodding) for the PHOENIX grid occur at Teff∼3900, 5000, 5200, and 5700 K (Figure 3).”
A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone (2013, methodology): “The adjustment consists of matching the observed spectrum to a grid of synthetic spectra from the newest PHOENIX/ACES grid (see Husser et al. 2013)).”
FRIENDS OF HOT JUPITERS. I. A RADIAL VELOCITY SEARCH FOR MASSIVE, LONG-PERIOD COMPANIONS TO CLOSE-IN GAS GIANT PLANETS (2013, methodology): “…of our contrast curves from separations in arc seconds to projected physical distances in AU We convert our contrast curves from delta magnitudes in either Ks or Kp bands to mass limits for stellar companions using the latest version of the PHOENIX stellar atmosphere models (Husser et al. 2013).”
They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, methodology): “Our approach was to estimate the distribution of reddening Er−J for the entire giant star catalog by comparing the observed r − J color with that synthesized by the PHOENIX stellar atmosphere model (Husser et al. 2013) for the known Teff and asteroseimically determined log g.”
Limb darkening and exoplanets: testing stellar model atmospheres and identifying biases in transit parameters (2015, methodology): “In §2 we detail our methodology for obtaining LDCs from ATLAS9 (Kurucz 1979) and PHOENIX (Husser et al. 2013) stellar model atmospheres, and compare our results with the literature in order to try understand the discrepancy between previously published tables.”
On the Cool Side: Modeling the Atmospheres of Brown Dwarfs and Giant Planets (2014, methodology): “Some atmospheric models, most notably the PHOENIX models (Allard & Hauschildt 1995; Barman et al. 2001), add a ‘micro-turbulent velocity’ to the thermal velocity, where the former is taken to scale with the characteristic convective velocity, w (see Section 4.2) (Husser et al. 2013).”
The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “For the low Teff and high gravity regime, we use spectra from the Göttingen Spectral Library (Husser et al. 2013).”
THE MUSCLES TREASURY SURVEY. I. MOTIVATION AND OVERVIEW (2016, methodology): “…atmosphere models considering only the photosphere (e.g., the PHOENIX models) are able to reproduce the peak and Rayleigh-Jeans tail of the stellar SED given the correct prescription for the effective temperature and abundances of atoms and molecules (Allard & Hauschildt 1995; Husser et al. 2013).”
Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies (2018, methodology): “For each mask, we first fit the broadband photometry of the slit star with the PHOENIX theoretical star models (Husser et al. 2013) to estimate its intrinsic spectrum.”