The Astronomical Journal

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2017

Karen A. Collins, Department of Physics & Astronomy, Vanderbilt University, Nashville, TN 37235, USA; [email protected]; Department of Physics, Fisk University, Nashville, TN 37208, USA; Department of Physics & Astronomy, University of Louisville, Louisville, KY 40292, USA
John F. Kielkopf, Department of Physics & Astronomy, University of Louisville, Louisville, KY 40292, USA
Keivan G. Stassun, Department of Physics & Astronomy, Vanderbilt University, Nashville, TN 37235, USA; [email protected]; Department of Physics, Fisk University, Nashville, TN 37208, USA
Frederic V. Hessman Inst. f. Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
The Astronomical Journal, Journal Year: 2017, Volume and Issue: 153(2), P. 1 - 1

Published: Jan. 1, 2017

ImageJ is a graphical user interface (GUI) driven, public domain, Java-based, software package for general image processing traditionally used mainly in life sciences fields. The image processing capabilities of ImageJ are useful and extendable to other scientific fields. Here we present AstroImageJ (AIJ), which provides an astronomy specific image display environment and tools for astronomy specific image calibration and data reduction. Although AIJ maintains the general purpose image processing capabilities of ImageJ, AIJ is streamlined for time-series differential photometry, light curve detrending and fitting, and light curve plotting, especially for applications requiring ultra-precise light curves (e.g., exoplanet transits). AIJ reads …

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Branimir Sesar, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
Nina Hernitschek, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
Sandra Mitrović, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
Željko Ivezić, University of Washington, Department of Astronomy, P.O.Box 351580, Seattle, WA 98195-1580, USA; [email protected]
Hans-Walter Rix, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
Judith G. Cohen, Division of Physics, Mathematics and Astronomy, Caltech, Pasadena, CA 91125, USA
Edouard J. Bernard, Université Côte d’Azur, OCA, CNRS, Lagrange, France
Eva K. Grebel, Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12–14, D-69120 Heidelberg, Germany
Nicolas F. Martin, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany; Observatoire astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l’Université, F-67000 Strasbourg, France
Edward F. Schlafly, Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany; Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA
William S. Burgett, GMTO Corporation, 251 S. Lake Avenue, Suite 300, Pasadena, CA 91101, USA
Peter W. Draper, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK
Heather Flewelling, Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI 96822, USA
Nick Kaiser, Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI 96822, USA
Rolf P. Kudritzki, Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI 96822, USA
Eugene A. Magnier, Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI 96822, USA
Nigel Metcalfe, Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI 96822, USA
John L. Tonry, Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI 96822, USA
Christopher Waters Institute for Astronomy, University of Hawai’i at Manoa, Honolulu, HI 96822, USA
The Astronomical Journal, Journal Year: 2017, Volume and Issue: 153(5), P. 1 - 1

Published: May 1, 2017

RR Lyrae stars may be the best practical tracers of Galactic halo (sub-)structure and kinematics. The PanSTARRSl (PSI) Зтг survey offers multi-band, multi-epoch, precise photometry across much of the sky, but a robust identification of RR Lyrae stars in this data set poses a challenge, given PSl’s sparse, asynchronous multi-band light curves (<12 epochs in each of five bands, taken over a 4.5 year period). We present a novel template fitting technique that uses well-defined and physically motivated multi-band light curves of RR Lyrae stars, and demonstrate that we get accurate period estimates, precise to 2 s in >80% of cases. We augment these light-curve fits with other features from photometric time-series and provide them to progressively more detailed machine- learned classification models. From these models, we are able to select the widest (three-fourths of the sky) and deepest (reaching 120 kpc) sample of RR …

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