TY - JOUR
T1 - SEARCH for GAMMA-RAY EMISSION from AE AQUARII with SEVEN YEARS of FERMI LAT OBSERVATIONS
AU - Li, Jian
AU - Torres, Diego F.
AU - Rea, Nanda
AU - Wilhelmi, Emma De Oña
AU - Papitto, Alessandro
AU - Hou, Xian
AU - Mauche, Christopher W.
PY - 2016/11/20
Y1 - 2016/11/20
N2 - © 2016. The American Astronomical Society. All rights reserved. AE Aquarii (AE Aqr) is a cataclysmic binary hosting one of the fastest rotating (Pspin = 33.08 s) white dwarfs (WDs) known. Based on seven years of Fermi Large Area Telescope (LAT) Pass 8 data, we report on a deep search for gamma-ray emission from AE Aqr. Using X-ray observations from ASCA, XMM-Newton, Chandra, Swift, Suzaku, and NuSTAR, spanning 20 years, we substantially extend and improve the spin ephemeris of AE Aqr. Using this ephemeris, we searched for gamma-ray pulsations at the spin period of the WD. No gamma-ray pulsations were detected above 3δsignificance. Neither phase-averaged gamma-ray emission nor gamma-ray variability of AE Aqr is detected by Fermi LAT. We impose the most restrictive upper limit to the gamma-ray flux from AE Aqr to date: 1.3 × 10-12 erg cm-2 s-1 in the 100 MeV-300 GeV energy range, providing constraints on models.
AB - © 2016. The American Astronomical Society. All rights reserved. AE Aquarii (AE Aqr) is a cataclysmic binary hosting one of the fastest rotating (Pspin = 33.08 s) white dwarfs (WDs) known. Based on seven years of Fermi Large Area Telescope (LAT) Pass 8 data, we report on a deep search for gamma-ray emission from AE Aqr. Using X-ray observations from ASCA, XMM-Newton, Chandra, Swift, Suzaku, and NuSTAR, spanning 20 years, we substantially extend and improve the spin ephemeris of AE Aqr. Using this ephemeris, we searched for gamma-ray pulsations at the spin period of the WD. No gamma-ray pulsations were detected above 3δsignificance. Neither phase-averaged gamma-ray emission nor gamma-ray variability of AE Aqr is detected by Fermi LAT. We impose the most restrictive upper limit to the gamma-ray flux from AE Aqr to date: 1.3 × 10-12 erg cm-2 s-1 in the 100 MeV-300 GeV energy range, providing constraints on models.
KW - gamma rays: stars
KW - novae, cataclysmic variables
KW - X-rays: individual (AE Aquarii)
U2 - 10.3847/0004-637X/832/1/35
DO - 10.3847/0004-637X/832/1/35
M3 - Article
VL - 832
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 35
ER -