<i>Swift</i>X‐Ray Observations of Classical Novae

Ness, J. U.; Schwarz, Guenter; Retter, A.; Starrfield, S.; Schmitt, J. H. M. M.; Gehrels, N.; Burrows, D. N.; Osborne, J. P.

doi:10.1086/518084

Cited by 68 publications

(93 citation statements)

References 30 publications

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“…Ness et al 2007a;Orio et al 2001) are similar to those of optical surveys. In our galaxy, the investigation of the whole nova population is hampered by the large area (namely the whole sky) to be scrutinised and by our unfavourable position close to the Galactic Plane.…”

Section: Introductionsupporting

confidence: 82%

“…In our galaxy, the investigation of the whole nova population is hampered by the large area (namely the whole sky) to be scrutinised and by our unfavourable position close to the Galactic Plane. As Ness et al (2007a) pointed out, the detectability of a SSS is highly dependent on its foreground absorption, which is affecting the supersoft X-rays much stronger than harder photons. Note that Orio et al (2001) analysed 350 archival ROSAT observations and found SSS emission for only three Galactic novae.…”

Section: Introductionmentioning

confidence: 99%

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X-ray monitoring of classical novae in the central region of M 31

Henze

Pietsch

Haberl

et al. 2010

A&A

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Context. Classical novae (CNe) have recently been reported to represent the major class of supersoft X-ray sources (SSSs) in the central region of our neighbour galaxy M 31. Aims. We carried out a dedicated monitoring of the M 31 central region with XMM-Newton and Chandra in order to find SSS counterparts of CNe, determine the duration of their SSS phase and derive physical outburst parameters. Methods. We systematically searched our data for X-ray counterparts of CNe and determined their X-ray light curves and spectral properties. Additionally, we determined luminosity upper limits for all novae from previous studies which are not detected anymore and for all CNe in our field of view with optical outbursts between May 2005 and March 2007. Results. We detected eight X-ray counterparts of CNe in M 31, four of which were not previously known. Seven sources can be classified as SSSs, one is a candidate SSS. Two SSSs are still visible more than nine years after the nova outburst, whereas two other nova counterparts show a short SSS phase of less than 150 days. Of the latter sources, M31N 2006-04a exhibits a short-time variable X-ray light curve with an apparent period of (1.6 ± 0.3) h. This periodicity could indicate the binary period of the system. There is no X-ray detection for 23 out of 25 CNe which were within the field of view of our observations and had their outburst from about one year before the start of the monitoring until its end. From the 14 SSS nova counterparts known from previous studies, ten are not detected anymore. Additionally, we found four SSSs in our XMM-Newton data without a nova counterpart, one of which is a new source. Conclusions. Out of eleven SSSs detected in our monitoring, seven are counterparts of CNe. We therefore confirm the earlier finding that CNe are the major class of SSSs in the central region of M 31. We use the measured SSS turn-on and turn-off times to estimate the mass ejected in the nova outburst and the mass burned on the white dwarf. Classical novae with short SSS phases seem to be an important contributor to the overall population.

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Section: Introductionsupporting

confidence: 82%

Section: Introductionmentioning

confidence: 99%

X-ray monitoring of classical novae in the central region of M 31

Henze

Pietsch

Haberl

et al. 2010

A&A

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“…The spectral model consists of a soft and a hard component, so the 2Y10 keV luminosity should be somewhat lower. The remainder of classical novae are taken from the Swift survey of classical novae ( Ness et al 2007). As the focus of this paper is the supersoft component, they do not provide luminosities or the conversion factor appropriate for the shell X-rays.…”

Section: Novae As X-ray Transientsmentioning

confidence: 99%

Novae as a Class of Transient X‐Ray Sources

Mukai

Orio

Valle

2008

ApJ

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Motivated by the recently discovered class of faint (10 34 Y10 35 ergs s À1 ) X-ray transients in the Galactic center region, we investigate the 2Y10 keV properties of classical and recurrent novae. Existing data are consistent with the idea that all classical novae are transient X-ray sources with durations of months to years and peak luminosities in the 10 34 Y10 35 ergs s À1 range. This makes classical novae a viable candidate class for the faint Galactic center transients. We estimate the rate of classical novae within a 15 0 radius region centered on the Galactic center (roughly the field of view of XMM-Newton observations centered on Sgr A*) to be $0.1 yr À1 . Therefore, it is plausible that some of the Galactic center transients that have been announced to date are unrecognized classical novae. The continuing monitoring of the Galactic center region carried out by Chandra and XMM-Newton may therefore provide a new method to detect classical novae in this crowded and obscured region, where optical surveys are not, and can never hope to be, effective. Therefore, X-ray monitoring may provide the best means of testing the completeness of the current understanding of the nova populations.

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“…X-ray telescope (XRT) data were extracted and processed using the standard Swift tools 24 , specifically xrtpipeline v0.11.3. We used event grades 0-12 and extracted events using a 24 arcsec radius region around the nova (Ness et al 2007). Table 2 for line identifications in the 0.8-4.5 μm region).…”

Section: Observationsmentioning

confidence: 99%

“…In Table 4 we list the observation day, exposure time, count rate, and hardness ratio. The count rates were obtained as described in the Appendix in Ness et al (2007). We also extracted spectra from the recorded photon energies; however, the number of photons was insufficient to obtain a well exposed spectrum.…”

Section: Swift X-ray Telescope Observationsmentioning

confidence: 99%

NOVA V2362 CYGNI (NOVA CYGNI 2006):SPITZER,SWIFT, AND GROUND-BASED SPECTRAL EVOLUTION

Lynch

Woodward

Gehrz

et al. 2008

The Astronomical Journal

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Nova V2362 Cygni has undergone a number of very unusual changes. Ground-based spectroscopy initially revealed a normal sequence of events: the object faded and its near-infrared emission lines gradually shifted to higher excitation conditions until about day 100 when the optical fading reversed and the object slowly brightened. This was accompanied by a rise in the Swift X-ray telescope flux and a sudden shift in excitation of the visible and IR spectrum back to low levels. The new lower excitation spectrum revealed broad line widths and many P-Cygni profiles, all indicative of the ejection of a second shell. Eventually, dust formed, the X-ray brightnessapparently unaffected by dust formation-peaked and then declined, and the object faded at all wavelengths. The Spitzer dust spectra revealed a number of solid-state emission features that, at this time, are not identified.

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SwiftX‐Ray Observations of Classical Novae

Cited by 68 publications

References 30 publications

X-ray monitoring of classical novae in the central region of M 31

X-ray monitoring of classical novae in the central region of M 31

Novae as a Class of Transient X‐Ray Sources

NOVA V2362 CYGNI (NOVA CYGNI 2006):SPITZER,SWIFT, AND GROUND-BASED SPECTRAL EVOLUTION

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