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Title: Separated fringe packet observations with the Chara Array. II. ω Andromeda, HD 178911, and ξ Cephei

Abstract

When observed with optical long-baseline interferometers, components of a binary star that are sufficiently separated produce their own interferometric fringe packets; these are referred to as separated fringe packet (SFP) binaries. These SFP binaries can overlap in angular separation with the regime of systems resolvable by speckle interferometry at single, large-aperture telescopes and can provide additional measurements for preliminary orbits lacking good phase coverage, help constrain elements of already established orbits, and locate new binaries in the undersampled regime between the bounds of spectroscopic surveys and speckle interferometry. In this process, a visibility calibration star is not needed, and the SFPs can provide an accurate vector separation. In this paper, we apply the SFP approach to ω Andromeda, HD 178911, and ξ Cephei with the CLIMB three-beam combiner at the CHARA Array. For these systems we determine component masses and parallax of 0.963 ± 0.049 M {sub ☉} and 0.860 ± 0.051 M {sub ☉} and 39.54 ± 1.85 mas for ω Andromeda, for HD 178911 of 0.802 ± 0.055 M {sub ☉} and 0.622 ± 0.053 M {sub ☉} with 28.26 ± 1.70 mas, and masses of 1.045 ± 0.031 M {sub ☉} and 0.408 ± 0.066 M {submore » ☉} and 38.10 ± 2.81 mas for ξ Cephei.« less

Authors:
; ; ; ;  [1]; ;  [2];  [3];  [4];  [5]
  1. The CHARA Array, Mount Wilson Observatory, Mount Wilson, CA 91023 (United States)
  2. US Naval Observatory, 3450 Massachusetts Avenue NW, Washington, DC 20392-5420 (United States)
  3. Université de Nice Sophia Antipolis, CNRS, Laboratoire J. L. Lagrange, Observatoire de la Côte d'Azur—BP4209, F-06304 Nice Cedex (France)
  4. Instituut Voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven (Belgium)
  5. Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969, Atlanta, GA 30302-3969 (United States)
Publication Date:
OSTI Identifier:
22342266
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astronomical Journal (New York, N.Y. Online); Journal Volume: 148; Journal Issue: 3; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APERTURES; BINARY STARS; CALIBRATION; INTERFEROMETERS; INTERFEROMETRY; MASS; ORBITS; RESOLUTION; TELESCOPES; VISIBILITY

Citation Formats

Farrington, C. D., Ten Brummelaar, T. A., Turner, N. H., Sturmann, L., Sturmann, J., Mason, B. D., Hartkopf, W. I., Mourard, D., Moravveji, E., and McAlister, H. A., E-mail: farrington@chara-array.org, E-mail: theo@chara-array.org, E-mail: nils@chara-array.org, E-mail: sturmann@chara-array.org, E-mail: judit@chara-array.org, E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil, E-mail: denis.mourard@oca.eu, E-mail: Ehsan.Moravveji@ster.kuleuven.be, E-mail: hal@chara.gsu.edu. Separated fringe packet observations with the Chara Array. II. ω Andromeda, HD 178911, and ξ Cephei. United States: N. p., 2014. Web. doi:10.1088/0004-6256/148/3/48.
Farrington, C. D., Ten Brummelaar, T. A., Turner, N. H., Sturmann, L., Sturmann, J., Mason, B. D., Hartkopf, W. I., Mourard, D., Moravveji, E., & McAlister, H. A., E-mail: farrington@chara-array.org, E-mail: theo@chara-array.org, E-mail: nils@chara-array.org, E-mail: sturmann@chara-array.org, E-mail: judit@chara-array.org, E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil, E-mail: denis.mourard@oca.eu, E-mail: Ehsan.Moravveji@ster.kuleuven.be, E-mail: hal@chara.gsu.edu. Separated fringe packet observations with the Chara Array. II. ω Andromeda, HD 178911, and ξ Cephei. United States. doi:10.1088/0004-6256/148/3/48.
Farrington, C. D., Ten Brummelaar, T. A., Turner, N. H., Sturmann, L., Sturmann, J., Mason, B. D., Hartkopf, W. I., Mourard, D., Moravveji, E., and McAlister, H. A., E-mail: farrington@chara-array.org, E-mail: theo@chara-array.org, E-mail: nils@chara-array.org, E-mail: sturmann@chara-array.org, E-mail: judit@chara-array.org, E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil, E-mail: denis.mourard@oca.eu, E-mail: Ehsan.Moravveji@ster.kuleuven.be, E-mail: hal@chara.gsu.edu. Mon . "Separated fringe packet observations with the Chara Array. II. ω Andromeda, HD 178911, and ξ Cephei". United States. doi:10.1088/0004-6256/148/3/48.
@article{osti_22342266,
title = {Separated fringe packet observations with the Chara Array. II. ω Andromeda, HD 178911, and ξ Cephei},
author = {Farrington, C. D. and Ten Brummelaar, T. A. and Turner, N. H. and Sturmann, L. and Sturmann, J. and Mason, B. D. and Hartkopf, W. I. and Mourard, D. and Moravveji, E. and McAlister, H. A., E-mail: farrington@chara-array.org, E-mail: theo@chara-array.org, E-mail: nils@chara-array.org, E-mail: sturmann@chara-array.org, E-mail: judit@chara-array.org, E-mail: bdm@usno.navy.mil, E-mail: wih@usno.navy.mil, E-mail: denis.mourard@oca.eu, E-mail: Ehsan.Moravveji@ster.kuleuven.be, E-mail: hal@chara.gsu.edu},
abstractNote = {When observed with optical long-baseline interferometers, components of a binary star that are sufficiently separated produce their own interferometric fringe packets; these are referred to as separated fringe packet (SFP) binaries. These SFP binaries can overlap in angular separation with the regime of systems resolvable by speckle interferometry at single, large-aperture telescopes and can provide additional measurements for preliminary orbits lacking good phase coverage, help constrain elements of already established orbits, and locate new binaries in the undersampled regime between the bounds of spectroscopic surveys and speckle interferometry. In this process, a visibility calibration star is not needed, and the SFPs can provide an accurate vector separation. In this paper, we apply the SFP approach to ω Andromeda, HD 178911, and ξ Cephei with the CLIMB three-beam combiner at the CHARA Array. For these systems we determine component masses and parallax of 0.963 ± 0.049 M {sub ☉} and 0.860 ± 0.051 M {sub ☉} and 39.54 ± 1.85 mas for ω Andromeda, for HD 178911 of 0.802 ± 0.055 M {sub ☉} and 0.622 ± 0.053 M {sub ☉} with 28.26 ± 1.70 mas, and masses of 1.045 ± 0.031 M {sub ☉} and 0.408 ± 0.066 M {sub ☉} and 38.10 ± 2.81 mas for ξ Cephei.},
doi = {10.1088/0004-6256/148/3/48},
journal = {Astronomical Journal (New York, N.Y. Online)},
number = 3,
volume = 148,
place = {United States},
year = {Mon Sep 01 00:00:00 EDT 2014},
month = {Mon Sep 01 00:00:00 EDT 2014}
}