Optical Calibrator Stars
Stars with high-resolution optical spectroscopy and published parameters and/or abundances
An object whose
APOGEE_TARGET1 value includes one or more of the bitmasks in the following table was targeted for spectroscopy as part of this ancillary target program. See SDSS bitmasks to learn how to use these values to identify objects in this ancillary target program.
|APOGEE_HIRES||20||star with parameters and/or abundances derived from high-resolution optical spectroscopy|
In addition to the stellar parameter and abundance calibrators targeted in well-studied clusters and the bulge, One ancillary program is targeting a number of field stars that have been the subject of optical high-resolution spectroscopic studies. The program goals include: comparing abundances and atmospheric parameters derived using APOGEE’s IR spectra with those in the literature; testing advanced 3D stellar model atmospheres (e.g., Fabbian et al. 2010, 2012) as a complement to observations of even closer stars with well-determined angular diameters and very accurate parallaxes; and establishing kinematical and chemical memberships in the Galactic thin/thick disks or halo.
|Instituto de Astrofisica de Canarias|
|damian -at- iac.es|
Carlos Allende Prieto, Katia Cunha, Verne Smith
Target Selection Details
The target list for this program comprises stars from the IRTF “Cool Stars” Spectral Library (Rayner et al. 2009) and stars observed by Reddy et al. (2003) and Reddy et al. (2006) at McDonald Observatory, limited to those with H < 12.5 mag (Vega) falling within APOGEE’s existing disk and halo fields at the time of the first call for ancillary programs.
Fabbian, D., Khomenko, E., Moreno-Insertis, F., & Nordlund, Å. 2010, ApJ, 724, 1536
Fabbian, D., Moreno-Insertis, F., Khomenko, E., & Nordlund, Å. 2012, A&A, 548, A35
Rayner, J. T., Cushing, M. C., & Vacca, W. D. 2009, ApJS, 185, 289
Reddy, B. E., Tomkin, J., Lambert, D. L., & Allende Prieto, C. 2003, MNRAS, 340, 304
Reddy, B. E., Lambert, D. L., & Allende Prieto, C. 2006, MNRAS, 367, 1329