Nova KT Eri 2009: infrared studies of a very fast and small amplitude He/N nova

Raj, Ashish; Banerjee, D. P. K.; Ashok, N. M.

doi:10.1093/mnras/stt946

Cited by 14 publications

(10 citation statements)

References 40 publications

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“…6 indicates that we can only realistically expect to detect novae in γrays for mR < 12 and d ≤ 8 kpc, with the majority of these within 6 kpc. These figures be used to explain that the non detection of Nova KT Eri (distance 6.3 ± 0.1 kpc (Raj et al 2013), mV = 8.1 (Yamaoka & Itagaki 2009)) is as a result of the nova being less luminous in γ-rays that those discovered. Raj et al (2013) also discusses the possibility of KT Eri being a recurrent nova, and hence may not belong to the same class of objects.…”

Section: Discussionmentioning

confidence: 98%

Gamma-ray novae: rare or nearby?

Morris

Cotter

Brown

et al. 2016

Mon. Not. R. Astron. Soc.

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Classical Novae were revealed as a surprise source of γ-rays in Fermi LAT observations. During the first 8 years since the LAT was launched, 6 novae in total have been detected to > 5σ in γ-rays, in contrast to the 69 discovered optically in the same period. We attempt to resolve this discrepancy by assuming all novae are γ-ray emitters, and assigning peak one-day fluxes based on a flat distribution of the known emitters to a simulated population. To determine optical parameters, the spatial distribution and magnitudes of bulge and disc novae in M31 are scaled to the Milky Way, which we approximate as a disc with a 20 kpc radius and elliptical bulge with semi major axis 3 kpc and axis ratios 2:1 in the xy plane. We approximate Galactic reddening using a double exponential disc with vertical and radial scale heights of r d = 5 kpc and z d = 0.2 kpc, and demonstrate that even such a rudimentary model can easily reproduce the observed fraction of γ-ray novae, implying that these apparently rare sources are in fact nearby and not intrinsically rare. We conclude that classical novae with m R ≤ 12 and within ≈ 8 kpc are likely to be discovered in γ-rays using the Fermi LAT.

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Section: Discussionmentioning

confidence: 98%

Gamma-ray novae: rare or nearby?

Morris

Cotter

Brown

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Such a profile structure is typical of a bipolar flow and has been seen in quite a few novae viz. RS Oph ), KT Eri 2009 (Ribeiro et al , 2013;Raj et al 2013), T Pyx . From our own data, indication for an asymmetrical ejecta flow also comes from the velocity profiles of the Paγ 1.094µm, Paβ 1.2818µm and Brγ 2.1656µm lines shown in Fig 10. Here a weak blue component is seen in each of the profiles, separated from the principal profile, by -650, -765, -690 kms −1 for Paγ, Paβ and the Br γ lines respectively.…”

Section: Evidence For a Shock From The Evolution Of The Line Profilesmentioning

confidence: 99%

Near-infrared studies during maximum and early decline of Nova Cephei 2014 and Nova Scorpii 2015

Srivastava¹,

Ashok²,

Banerjee³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present multi-epoch near-infrared photo-spectroscopic observations of Nova Cephei 2014 and Nova Scorpii 2015, discovered in outburst on 2014 March 8.79 UT and 2015 February 11.84 UT respectively. Nova Cep 2014 shows the conventional NIR characteristics of a Fe II class nova characterized by strong CI, HI and O I lines, whereas Nova Sco 2015 is shown to belong to the He/N class with strong He I, HI and OI emission lines. The highlight of the results consists in demonstrating that Nova Sco 2015 is a symbiotic system containing a giant secondary. Leaving aside the T CrB class of recurrent novae, all of which have giant donors, Nova Sco 2015 is shown to be only the third classical nova to be found with a giant secondary. The evidence for the symbiotic nature is three-fold; first is the presence of a strong decelerative shock accompanying the passage of the nova's ejecta through the giant's wind, second is the Hα excess seen from the system and third is the spectral energy distribution of the secondary in quiescence typical of a cool late type giant. The evolution of the strength and shape of the emission line profiles shows that the ejecta velocity follows a power law decay with time (t −1.13±0.17 ). A Case B recombination analysis of the H I Brackett lines shows that these lines are affected by optical depth effects for both the novae. Using this analysis we make estimates for both the novae of the emission measure n 2 e L, the electron density n e and the mass of the ejecta.

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“…Radio observations were obtained by O'Brien et al (2010) and X-ray observations by Bode et al (2010), Beardmore et al (2010), and Ness et al (2010). Raj et al (2013) discussed early infrared photometric and spectroscopic evolution, while the line profiles and their temporal evolution were modeled in detail by Ribeiro et al (2013). Jurdana-Šepić et al (2012) searched the Harvard plate archive and measured the progenitor of the nova on 1012 plates dating from 1888 to 1962.…”

Section: Introductionmentioning

confidence: 99%

The narrow and moving HeII lines in nova KT Eridani

Munari

Mason

Valisa³

2014

A&A

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We present outburst and quiescence spectra of the classical nova KT Eri and discuss the appearance of a sharp HeII 4686 Å emission line, whose origin is a matter of discussion for those novae that showed a similar component. We suggest that the sharp HeII line, when it first appeared toward the end of the outburst optically thick phase, comes from the wrist of the dumbbell structure characterizing the ejecta. When the ejecta turned optically thin, the already sharp HeII line became two times narrower and originated from the exposed central binary. During the optically thin phase, the HeII line displayed a large change in radial velocity that had no counterpart in the Balmer lines (both their narrow cores and the broad pedestals). The large variability in radial velocity of the HeII line continued well into quiescence, and it remains the strongest emission line observed over the whole optical range.

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Nova KT Eri 2009: infrared studies of a very fast and small amplitude He/N nova

Cited by 14 publications

References 40 publications

Gamma-ray novae: rare or nearby?

Gamma-ray novae: rare or nearby?

Near-infrared studies during maximum and early decline of Nova Cephei 2014 and Nova Scorpii 2015

The narrow and moving HeII lines in nova KT Eridani

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