A <i>NuSTAR</i> observation of the fast symbiotic nova V745 Sco in outburst

Orio, Marina; Rana, V.; Page, K. L.; Sokoloski, J. L.; Harrison, Fiona A.

doi:10.1093/mnrasl/slu195

Cited by 34 publications

(53 citation statements)

References 28 publications

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“…Interestingly, our N H values are quite similar to those measured for 2 recurrent novae known to have red giant companions: V745 Sco and RS Oph. In RS Oph, the values for N H were ∼ 10 23 cm −2 just 0.16 days after eruption, but fell to ∼ 10 22 cm −2 by Day 3.23 and were ∼ 8 × 10 21 cm −2 by Day 10 (Orio et al 2015). In RS Oph, Nelson et al (2008) reported N H ∼ 10 22 cm −2 14 days after eruption.…”

Section: X-raysmentioning

confidence: 97%

The Peculiar Multiwavelength Evolution Of V1535 Sco

Linford

Chomiuk

Nelson

et al. 2017

ApJ

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We present multi-wavelength observations of the unusual nova V1535 Sco throughout its outburst in 2015. Early radio observations were consistent with synchrotron emission, and early X-ray observations revealed the presence of high-energy (>1 keV) photons. These indicated that strong shocks were present during the first ∼2 weeks of the nova's evolution. The radio spectral energy distribution was consistent with thermal emission from week 2 to week 6. Starting in week 7, the radio emission again showed evidence of synchrotron emission and there was an increase in X-ray emission, indicating a second shock event. The optical spectra show evidence for at least two separate outflows, with the faster outflow possibly having a bipolar morphology. The optical and near infrared light curves and the X-ray N H measurements indicated that the companion star is likely a K giant.

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Section: X-raysmentioning

confidence: 97%

The Peculiar Multiwavelength Evolution Of V1535 Sco

Linford

Chomiuk

Nelson

et al. 2017

ApJ

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“…Model parameter estimation was undertaken using the XSPEC fitting engine, applying isothermal APEC models attenuated by a variable absorption component representing the circumstellar environment combined with a fixed interstellar absorption corresponding to a neutral hydrogen column density of 5.6 × 10 21 cm −2 . A metallicity of 0.51 times the solar abundances of Anders & Grevesse (1989) was adopted, following Orio et al (2015). Unfortunately, during the SSS phase there was insufficient signal at higher energies above that of the SSS signal with which to constrain the plasma temperature; consequently, there is a gap in the Swift temperatures between days 4 and 12.…”

Section: Swift Xrt Observationsmentioning

confidence: 99%

“…The explosion triggered observing campaigns over the entire electromagnetic spectrum, including radio (Rupen et al 2014;Kantharia et al 2016), infrared (Banerjee et al 2014), optical (Anupama et al 2014;Mróz et al 2014), X-ray Drake et al 2014;Mukai et al 2014;Page et al 2015), hard X-ray (Rana et al 2014;Orio et al 2015), and γ-ray (Cheung et al 2014(Cheung et al , 2015 wavelengths. Page et al (2015) present a detailed summary of the various observations.…”

Section: Introductionmentioning

confidence: 99%

COLLIMATION AND ASYMMETRY OF THE HOT BLAST WAVE FROM THE RECURRENT NOVA V745 Sco

Drake

Delgado

Laming

et al. 2016

ApJ

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The recurrent symbiotic nova V745 Sco exploded on 2014 February 6 and was observed on February 22 and 23 by the Chandra X-ray Observatory Transmission Grating Spectrometers. By that time the supersoft source phase had already ended, and Chandra spectra are consistent with emission from a hot, shock-heated circumstellar medium with temperatures exceeding 10 7 K. X-ray line profiles are more sharply peaked than expected for a spherically symmetric blast wave, with a full width at zero intensity of approximately 2400 km s −1 , an FWHM of 1200 ± 30 km s −1 , and an average net blueshift of 165 ± 10 km s −1 . The red wings of lines are increasingly absorbed toward longer wavelengths by material within the remnant. We conclude that the blast wave was sculpted by an aspherical circumstellar medium in which an equatorial density enhancement plays a role, as in earlier symbiotic nova explosions. Expansion of the dominant X-ray-emitting material is aligned close to the plane of the sky and is most consistent with an orbit seen close to face-on. Comparison of an analytical blast wave model with the X-ray spectra, Swift observations, and near-infrared line widths indicates that the explosion energy was approximately 10 43 erg and confirms an ejected mass of approximately 10 −7 M e . The total mass lost is an order of magnitude lower than the accreted mass required to have initiated the explosion, indicating that the white dwarf is gaining mass and is a Type Ia supernova progenitor candidate.

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“…To date, at least 14 Galactic novae (including three confirmed and one suspected RN) have been observed with a decline time  t 4 2 days (see Hounsell et al 2010;Strope et al 2010;Munari et al 2011;Orio et al 2015), and these are summarized in Table 5. M31N 2008-12a resides at the faster end of this rapidly declining sample, exhibiting decline times very similar to those of the RN USco (marginally slower to t 2 but faster to t 3 , assuming V-band luminosities), and exhibits the only known decline with < t 3 3 days.…”

Section: Initial Decline (Day 1-4)mentioning

confidence: 99%

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

Darnley

Henze

Bode

et al. 2016

ApJ

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The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of =  P 351 13 rec days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground-and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swiftobservatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28±0.12 UT. The 2013-2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities ∼13,000 km s −1 ,

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A NuSTAR observation of the fast symbiotic nova V745 Sco in outburst

Cited by 34 publications

References 28 publications

The Peculiar Multiwavelength Evolution Of V1535 Sco

The Peculiar Multiwavelength Evolution Of V1535 Sco

COLLIMATION AND ASYMMETRY OF THE HOT BLAST WAVE FROM THE RECURRENT NOVA V745 Sco

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

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