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Direct detection of SDSS J0926+3624 orbital expansion with ARCONS

Szypryt, P. and Duggan, G. E. and Mazin, B. A. and Meeker, S. R. and Strader, M. J. and van Eyken, J. C. and Marsden, D. and O'Brien, K. and Walter, A. B. and Ulbricht, G. and Prince, T. A. and Stoughton, C. and Bumble, B. (2014) Direct detection of SDSS J0926+3624 orbital expansion with ARCONS. Monthly Notices of the Royal Astronomical Society, 439 (3). pp. 2765-2770. ISSN 0035-8711. doi:10.1093/mnras/stu137.

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AM Canum Venaticorum (AM CVn) stars belong to a class of ultra-compact, short period binaries with spectra dominated largely by helium. SDSS J0926+3624 is of particular interest as it is the first observed eclipsing AM CVn system. We observed SDSS J0926+3624 with the \textbf{Ar}ray \textbf{C}amera for \textbf{O}ptical to \textbf{N}ear-IR \textbf{S}pectrophotometry (ARCONS) at the Palomar 200" telescope. ARCONS uses a relatively new type of energy-resolved photon counters called Microwave Kinetic Inductance Detectors (MKIDs). ARCONS, sensitive to radiation from 350 to 1100 nm, has a time resolution of several microseconds and can measure the energy of a photon to ∼10. We present the light curves for these observations and examine changes in orbital period from prior observations. Using a quadratic ephemeris model, we measure a period rate of change P˙=(3.07±0.56)×10−13. In addition, we use the high timing resolution of ARCONS to examine the system's high frequency variations and search for possible quasi-periodic oscillations (QPOs). Finally, we use the instrument's spectral resolution to examine the light curves in various wavelength bands. We do not find any high frequency QPOs or significant spectral variability throughout an eclipse.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Duggan, G. E.0000-0002-9256-6735
van Eyken, J. C.0000-0003-2192-5371
Prince, T. A.0000-0002-8850-3627
Additional Information:© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 January 16. Received 2014 January 16. In original form 2013 September 13. First published online February 17, 2014. The MKID detectors used in this work were developed under NASA grant NNX11AD55G, and the readout was partially developed under NASA grant NNX10AF58G. SRM was supported by a NASA Office of the Chief Technologist's Space Technology Research Fellowship, NASA grant NNX11AN29H. This work was partially supported by the Keck Institute for Space Studies. Fermilab is operated by Fermi Research Alliance, LLC under Contract no. De-AC02-07CH11359 with the United States Department of Energy. The authors would like to thank Shri Kulkarni, Director of the Caltech Optical Observatories for facilitating this project, as well as the excellent staff of the Palomar Observatory. This project also greatly benefitted from the support of Mike Werner, Paul Goldsmith, and Jonas Zmuidzinas at JPL.
Group:Keck Institute for Space Studies
Funding AgencyGrant Number
NASA Space Technology Research FellowshipNNX11AN29H
Keck Institute for Space Studies (KISS)UNSPECIFIED
Department of Energy (DOE)DE-AC02-07CH11359
Subject Keywords:binaries: close – binaries: eclipsing – stars: individual: SDSS J0926+3624 – cataclysmic variables – white dwarfs
Issue or Number:3
Record Number:CaltechAUTHORS:20160307-110122581
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Official Citation:P. Szypryt, G. E. Duggan, B. A. Mazin, S. R. Meeker, M. J. Strader, J. C. van Eyken, D. Marsden, K. O'Brien, A. B. Walter, G. Ulbricht, T. A. Prince, C. Stoughton, and B. Bumble Direct detection of SDSS J0926+3624 orbital expansion with ARCONS MNRAS (April 11, 2014) Vol. 439 2765-2770 doi:10.1093/mnras/stu137 first published online February 17, 2014
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65115
Deposited By: Colette Connor
Deposited On:09 Mar 2016 19:27
Last Modified:10 Nov 2021 23:40

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