AT 2017fvz: a nova in the dwarf irregular galaxy NGC 6822

Healy, M. W.; Darnley, M. J.; Copperwheat, C. M.; Filippenko, A. V.; Henze, M.; Hestenes, Julia; James, P. A.; Page, K. L.; Williams, S. C.; Zheng, W.

doi:10.1093/mnras/stz1108

Cited by 3 publications

(2 citation statements)

References 73 publications

(95 reference statements)

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“…Recently, individual novae have been studied in detail in IC 1613 (Williams et al, 2017) and NGC 6822 (Healy et al, 2019), both hosts are dwarf irregular galaxies in the Local Group and, like the Magellanic Clouds, provide further examples of novae in low metallicity environments (see the discussion within Orio, 2013).…”

Section: Beyond Andromedamentioning

confidence: 99%

On a century of extragalactic novae and the rise of the rapid recurrent novae

Darnley

Henze

2020

Advances in Space Research

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Novae are the observable outcome of a transient thermonuclear runaway on the surface of an accreting white dwarf in a close binary system. Their high peak luminosity renders them visible in galaxies out beyond the distance of the Virgo Cluster. Over the past century, surveys of extragalactic novae, particularly within the nearby Andromeda Galaxy, have yielded substantial insights regarding the properties of their populations and sub-populations. The recent decade has seen the first detailed panchromatic studies of individual extragalactic novae and the discovery of two probably related sub-groups: the 'faint-fast' and the 'rapid recurrent' novae. In this review we summarise the past 100 years of extragalactic efforts, introduce the rapid recurrent sub-group, and look in detail at the remarkable faint-fast, and rapid recurrent, nova M31N 2008-12a. We end with a brief look forward, not to the next 100 years, but the next few decades, and the study of novae in the upcoming era of wide-field and multi-messenger time-domain surveys.

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Section: Beyond Andromedamentioning

confidence: 99%

On a century of extragalactic novae and the rise of the rapid recurrent novae

Darnley

Henze

2020

Advances in Space Research

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“…A search for potential progenitor/quiescent systems was performed following the procedure set out in Bode et al (2009), and then further refined by Williams et al (2014) and more recently Healy et al (2019). Astrometric solutions were computed between each V-and i -band LT observation and the corresponding CFHT V-and I-band stack, and the GALEX data, to define the progenitor search region with those data.…”

Section: Archival Datamentioning

confidence: 99%

AT 2016dah and AT 2017fyp: the first classical novae discovered within a tidal stream

Darnley

Newsam

Chinetti

et al. 2020

Monthly Notices of the Royal Astronomical Society

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AT 2016dah and AT 2017fyp are fairly typical Andromeda galaxy (M 31) classical novae. AT 2016dah is an almost text book example of a ‘very fast’ declining, yet uncommon, Fe ii‘b’ (broad-lined) nova, discovered during the rise to peak optical luminosity, and decaying with a smooth broken power-law light curve. AT 2017fyp is classed as a ‘fast’ nova, unusually for M 31, its early decline spectrum simultaneously shows properties of both Fe ii and He/N spectral types – a ‘hybrid’. Similarly, the light curve of AT 2017fyp has a broken power-law decline but exhibits an extended flat-topped maximum. Both novae were followed in the UV and X-ray by the Neil Gehrels Swift Observatory, but no X-ray source was detected for either nova. The pair were followed photometrically and spectroscopically into their nebular phases. The progenitor systems were not visible in archival optical data, implying that the mass donors are main-sequence stars. What makes AT 2016dah and AT 2017fyp particularly interesting is their position with respect to M 31. The pair are close on the sky but are located far from the centre of M 31, lying almost along the semiminor axis of their host. Radial velocity measurements and simulations of the M 31 nova population leads to the conclusion that both novae are members of the Andromeda Giant Stellar Stream (GSS). We find the probability of at least two M 31 novae appearing coincident with the GSS by chance is $\sim \!1{{\ \rm per\ cent}}$. Therefore, we claim that these novae arose from the GSS progenitor, not M 31 – the first confirmed novae discovered in a tidal steam.

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AT 2023prq: A Classical Nova in the Halo of the Andromeda Galaxy

Healy-Kalesh,

Perley

2023

Res. Notes AAS

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The classical nova, AT 2023prq, was discovered on 2023 August 15 and is located at a distance of 46 kpc from the Andromeda galaxy (M31). Here we report photometry and spectroscopy of the nova. The “very fast” ( t 2 , r ′ ∼ 3.4 days) and low luminosity ( M r ′ ∼ − 7.6 ) nature of the transient along with the helium in its spectra would indicate that AT 2023prq is a “faint-and-fast” He/N nova. Additionally, at such a large distance from the center of M31, AT 2023prq is a member of the halo nova population.

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AT 2017fvz: a nova in the dwarf irregular galaxy NGC 6822

Cited by 3 publications

References 73 publications

On a century of extragalactic novae and the rise of the rapid recurrent novae

On a century of extragalactic novae and the rise of the rapid recurrent novae

AT 2016dah and AT 2017fyp: the first classical novae discovered within a tidal stream

AT 2023prq: A Classical Nova in the Halo of the Andromeda Galaxy

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