TY - JOUR
T1 - Multiwavelength monitoring of a very active dwarf nova AX J1549.8-5416 with an unusually high duty cycle
AU - Zhang, G.
AU - Gelfand, J.
AU - Russell, D.
AU - Lewis, F.
AU - Masetti, N.
AU - Bernardini, F.
AU - Andruchow, I.
AU - Zibecchi, L.
PY - 2017/10/1
Y1 - 2017/10/1
N2 - We present new optical, UV and X-ray observations of a highly variable
dwarf nova(DN) AX J1549.8-5416. The multiwavelength analysis of three
mini-outbursts and one normal outburst represent one of the most
complete multiwavelength studies of a DN and help to refine the
relationship between the X-ray, UV and optical emission in this
system. We find that the UV emission is delayed the optical (1.0-5.4
days) during the rising phase of the outburst. The X-ray emission is
suppressed during the peak of the optical outburst and recovers
during the end of the outburst. We also analyse archival Swift, Chandra
and XMM-Newton observations of the source. Our estimated high duty
cycle suggests the X-ray luminosity of this source should be larger
than 10E32 erg/s in quiescence. We find a roughly anti-correlation
between X-ray and UV flux. The X-ray spectra of XMM-Newton and Chandra
can be well described either by a single temperature thermal plasma
model or by an isobaric cooling flow model when its X-ray flux is high.
AB - We present new optical, UV and X-ray observations of a highly variable
dwarf nova(DN) AX J1549.8-5416. The multiwavelength analysis of three
mini-outbursts and one normal outburst represent one of the most
complete multiwavelength studies of a DN and help to refine the
relationship between the X-ray, UV and optical emission in this
system. We find that the UV emission is delayed the optical (1.0-5.4
days) during the rising phase of the outburst. The X-ray emission is
suppressed during the peak of the optical outburst and recovers
during the end of the outburst. We also analyse archival Swift, Chandra
and XMM-Newton observations of the source. Our estimated high duty
cycle suggests the X-ray luminosity of this source should be larger
than 10E32 erg/s in quiescence. We find a roughly anti-correlation
between X-ray and UV flux. The X-ray spectra of XMM-Newton and Chandra
can be well described either by a single temperature thermal plasma
model or by an isobaric cooling flow model when its X-ray flux is high.
M3 - Article
SP - 245
JO - The X-ray Universe 2017, Proceedings of the conference held 6-9 June, 2017 in Rome, Italy. Edited by J.-U. Ness and S. Migliari
JF - The X-ray Universe 2017, Proceedings of the conference held 6-9 June, 2017 in Rome, Italy. Edited by J.-U. Ness and S. Migliari
ER -