Novae in M31 discovered with wide-field telescopes in Crimea and Latvia. The maximum magnitude versus rate of decline relation for Novae in M31

Sharov, A. S.; Alksnis, A.

doi:10.1007/bf00644569

Cited by 8 publications

(7 citation statements)

References 16 publications

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“…The reanalysis of archival plates makes it possible to tap the full potential of long-term databases. Rosino (1964, 1973, 1989), ShAl = Sharov & Alksnis (1991, 1992, and SI2001 = Shafter & Irby (2001). • 7 × 2 .…”

Section: Discussionmentioning

confidence: 99%

“…There have been various systematical surveys of novae in M 31 for more than 80 years starting with the pioneering work of Hubble (1929) and Arp (1956). Among the many other contributors, we refer here only to the work of Rosino et al (1964Rosino et al ( , 1973Rosino et al ( , 1989, Ciardullo and co-workers (e.g., 1987), Sharov & Alksnis (1991, 1992, and Shafter and co-workers (e.g., Shafter & Irby 2001). More recent efforts include, in particular, the AGAPE project (Ansari et al 2004), the POINT-AGAPE project (Darnley et al 2004), and the WeCAPP project (Fliri et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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A systematic search for novae in M 31 on a large set of digitized archival Schmidt plates

Henze¹,

Meusinger²,

Pietsch

2007

A&A

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Aims. This paper reports on the detection of optical novae in our neighbour galaxy M 31 based on digitized historical Tautenburg Schmidt plates. The accurate positions of the detected novae lead to a much larger database when searching for recurrent novae in M 31. Methods. We conducted a systematic search for novae on 306 digitized Tautenburg Schmidt plates covering a time span of 36 years from 1960 to 1996. From the database of both ∼3 × 10 5 light curves and 10 6 detections on only one plate per colour band, nova candidates were efficiently selected by automated algorithms and subsequently individually inspected by eye. Results. We report the detection of 84 nova candidates. We found 55 nova candidates from the automated analysis of the light curves. Among these, 22 were previously unknown, 12 were known but not identified on Tautenburg Schmidt plates before, and 21 novae had been discovered previously on Tautenburg plates. An additional 29 known novae could be confirmed by the detailed investigation of single detections. One of our newly discovered nova candidates shows a high position coincidence with a nova detected about 30 years earlier. Therefore, this object is likely to be a recurrent nova. Furthermore, we re-investigated all 41 nova candidates previously found on Tautenburg plates and confirm all but two. Positions are given for all nova candidates with a typical accuracy of ∼0 . 4. We present light curves and finding charts as online material. Conclusions. The analysis of the plates has shown the wealth of information still buried in old plate archives. Extrapolating from this survey, digitization of other historical M 31 plate archives (e.g. from the Mount Wilson or Asiago observatories) for a systematic nova search looks very promising.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A systematic search for novae in M 31 on a large set of digitized archival Schmidt plates

Henze¹,

Meusinger²,

Pietsch

2007

A&A

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“…M31N 1982-08b was discovered in the outskirts of M31 as nova #27 in the survey of Sharov & Alksnis (1992). A likely recurrence (nominally located ∼ 3 away) was discovered by Shafter & Irby (2001), who reported a nova discovered on 1996 August 12.…”

Section: M31n 1982-08bmentioning

confidence: 99%

Recurrent Novae in M31

Shafter

Henze

Rector

et al. 2015

ApJS

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The reported positions of 964 suspected nova eruptions in M31 recorded through the end of calendar year 2013 have been compared in order to identify recurrent nova candidates. To pass the initial screen and qualify as a recurrent nova candidate two or more eruptions were required to be coincident within 0.1 , although this criterion was relaxed to 0.15 for novae discovered on early photographic patrols. A total of 118 eruptions from 51 potential recurrent nova systems satisfied the screening criterion. To determine what fraction of these novae are indeed recurrent the original plates and published images of the relevant eruptions have been carefully compared. This procedure has resulted in the elimination of 27 of the 51 progenitor candidates (61 eruptions) from further consideration as recurrent novae, with another 8 systems (17 eruptions) deemed unlikely to be recurrent. Of the remaining 16 systems, 12 candidates (32 eruptions) were judged to be recurrent novae, with an additional 4 systems (8 eruptions) being possibly recurrent. It is estimated that ∼4% of the nova eruptions seen in M31 over the past century are associated with recurrent novae. A Monte Carlo analysis shows that the discovery efficiency for recurrent novae may be as low as 10%

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“…Light-curve data, when available, often only cover Hα or the R band where the relationship between fade rate and peak luminosity is weak or absent (e.g., Ciardullo et al 1990b). As mentioned earlier, available broad-band nova data come largely from the photographic surveys of Arp (1956), Rosino (1964Rosino ( , 1973, and Sharov & Alksnis (1992). As noted above, the observation by Arp (1956) that the apparent magnitude distribution for M31 appeared to be bimodal, with peaks corresponding to M B ≈ −8.5 and M B ≈ −7.0 mag at the distance of M31, was later taken as evidence for the existence of two nova populations (e.g., Capaccioli et al 1989).…”

Section: Spatial Distribution Of Nova Speed Classmentioning

confidence: 99%

“…As shown by Ciardullo et al (1990b) the Hα light curves are not simply correlated with the peak luminosity as are the broad-band light curves. Moreover, most of the broadband light-curve data for M31 novae come from the early photographic studies of Arp (1956) and Rosino (1964Rosino ( , 1973, as summarized by Capaccioli et al (1989), and from observations in Crimea and Latvia during the period between 1977 and 1990 (Sharov & Alksnis 1992).…”

Section: Introductionmentioning

confidence: 99%

A Spectroscopic and Photometric Survey of Novae in M31

Shafter

Darnley

Hornoch

et al. 2011

ApJ

158

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We report the results of a multi-year spectroscopic and photometric survey of novae in M31 that resulted in a total of 53 spectra of 48 individual nova candidates. Two of these, M31N 1995-11e and M31N 2007-11g, were revealed to be long-period Mira variables, not novae. These data double the number of spectra extant for novae in M31 through the end of 2009 and bring to 91 the number of M31 novae with known spectroscopic classifications. We find that 75 novae (82%) are confirmed or likely members of the Fe II spectroscopic class, with the remaining 16 novae (18%) belonging to the He/N (and related) classes. These numbers are consistent with those found for Galactic novae. We find no compelling evidence that spectroscopic class depends sensitively on spatial position or population within M31 (i.e., bulge vs. disk), although the distribution for He/N systems appears slightly more extended than that for the Fe II class. We confirm the existence of a correlation between speed class and ejection velocity (based on line width), as in the case of Galactic novae. Follow-up photometry allowed us to determine light-curve parameters for a total of 47 of the 91 novae with known spectroscopic class. We confirm that more luminous novae generally fade the fastest, and that He/N novae are typically faster and brighter than their Fe II counterparts. In addition, we find a weak dependence of nova speed class on position in M31, with the spatial distribution of the fastest novae being slightly more extended than that of slower novae.

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Novae in M31 discovered with wide-field telescopes in Crimea and Latvia. The maximum magnitude versus rate of decline relation for Novae in M31

Cited by 8 publications

References 16 publications

A systematic search for novae in M 31 on a large set of digitized archival Schmidt plates

A systematic search for novae in M 31 on a large set of digitized archival Schmidt plates

Recurrent Novae in M31

A Spectroscopic and Photometric Survey of Novae in M31

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