Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/788/164 Properties of the known Galactic classical novae (Pagnotta+, 2014)

Identifying and quantifying recurrent novae masquerading as classical novae. Pagnotta A., Schaefer B.E. <Astrophys. J., 788, 164 (2014)> =2014ApJ...788..164P (SIMBAD/NED BibCode)
ADC_Keywords: Novae ; Photometry Keywords: novae, cataclysmic variables Abstract: Recurrent novae (RNe) are cataclysmic variables with two or more nova eruptions within a century. Classical novae (CNe) are similar systems with only one such eruption. Many of the so-called CNe are actually RNe for which only one eruption has been discovered. Since RNe are candidate Type Ia supernova progenitors, it is important to know whether there are enough in our Galaxy to provide the supernova rate, and therefore to know how many RNe are masquerading as CNe. To quantify this, we collected all available information on the light curves and spectra of a Galactic, time-limited sample of 237 CNe and the 10 known RNe, as well as exhaustive discovery efficiency records. We recognize RNe as having (1) outburst amplitude smaller than 14.5-4.5xlog(t3), (2) orbital period >0.6 days, (3) infrared colors of J-H>0.7 mag and H-K>0.1 mag, (4) FWHM of Hα>2000 km/s, (5) high excitation lines, such as Fe X or He II near peak, (6) eruption light curves with a plateau, and (7) white dwarf mass greater than 1.2 M. Using these criteria, we identify V1721 Aql, DE Cir, CP Cru, KT Eri, V838 Her, V2672 Oph, V4160 Sgr, V4643 Sgr, V4739 Sgr, and V477 Sct as strong RN candidates. We evaluate the RN fraction among the known CNe using three methods to get 24%±4%, 12%±3%, and 35%±3%. With roughly a quarter of the 394 known Galactic novae actually being RNe, there should be approximately a hundred such systems masquerading as CNe. Description: RNe and CNe have substantial overlap in the observed distributions of their properties. Indeed, this is expected, since many CNe are really RNe. Nevertheless, a variety of properties are greatly different between the CNe and the RNe. For example, most RNe have orbital periods longer than 0.6 days, while most CNe have orbital periods shorter than 0.3 days. Such properties can be used as indicators for recognizing RNe among the CNe. Due to the overlapping distribution of properties, no one property (other than multiple observed nova eruptions) can be used to definitively identify the CN or RN nature of any system. We never prove that a system is an RN by any means other than finding multiple eruptions. The presence of multiple positive indicators, however, especially if none are contrary, can make a strong case for the RN nature of a system. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 185 237 Properties of the Known Galactic Classical Novae refs.dat 153 129 References
See also: II/173 : A REFERENCE CATALOGUE OF GALACTIC NOVAE (Version 1990.0) J/PAZh/34/270 : Photometric parameters of Galactic novae (Burlak+, 2008) J/PAZh/34/278 : Distances and extinction of Galactic novae (Burlak, 2008) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 9 A9 --- ID Nova identifier 11 A1 --- l_Amp [>] Limit flag on Amp 13- 17 F5.2 mag Amp ? Outburst amplitude 19- 20 A2 --- r_Amp Reference for Amp (listed in refs.dat file) 23 A1 --- l_t3 [>] Limit flag on t3 24- 26 I3 d t3 ? Time to decline three magnitudes 28- 30 A3 --- r_t3 Reference for t3 (listed in refs.dat file) 32- 36 F5.2 mag A-A0 ? Distance from the threshold line 38- 47 A10 km/s FWHM FWHM velocity of Hα 49- 55 A7 --- r_FWHM Reference(s) for FWHM (listed in refs.dat file) 57- 59 A3 --- HeII [Yes/No ] Presence of He II? 61- 63 A3 --- r_HeII Reference for HeII (listed in refs.dat file) 65- 72 A8 --- HiFe Highest iron present 74- 78 A5 --- r_HiFe Reference for HiFe (listed in refs.dat file) 80 A1 --- LC Light curve type (2) 82 A1 --- r_LC Reference for LC (listed in refs.dat file) 84- 88 F5.3 d Porb ? Orbital period 89 A1 --- u_Porb [:] Uncertainty flag on Porb 91- 93 A3 --- r_Porb Reference for Porb (listed in refs.dat file) 95-100 F6.3 mag J-H ? The (J-H) color 102-104 A3 --- r_J-H Reference for J-H (listed in refs.dat file) 106-111 F6.3 mag H-K ? The (H-K) color 113-117 A5 --- r_H-K Reference(s) for H-K (listed in refs.dat file) 119-121 A3 --- RG [Yes/No ] Presence of a red giant secondary? 123-131 A9 --- r_RG Reference(s) for RG (listed in refs.dat file) 133-174 A42 --- Com Other relevant comments 176-183 A8 --- r_Com Reference(s) for Com (listed in refs.dat file) 185 A1 --- Cat [BCDEF] Category (1)
Note (1): Category as follows: B = Contains strong recurrent nova (RN) candidates, for which many of our indicators strongly point to the system being recurrent, with only one eruption observed thus far; C = Contains likely RN candidates, for which our evaluation of the characteristics indicates that the probability is ≥50% that the system is recurrent; D = Contains likely classical novae (CNe), despite the system perhaps showing some small number of positive RN indicators; E = Contains systems which are certainly CNe based on the indicators; F = Contains systems for which there is not enough information to determine the status of the system. Note (2): Light curve type as follows: S = Smoothly declining; D = Dust dips; J = Large random jitters from before the peak until the transition phase; O = Periodic oscillations around the transition phase; F = Flat-topped; C = A slow-rising fast-fall cusp around the transition phase; P = Light curves are characterized by a plateau around the transition phase, with this plateau being an interruption of the otherwise smooth decline from peak, at which point the light curve goes nearly flat for a measurable amount of time, then abruptly returns to its steep decline, often at a faster rate than before the plateau phase.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Num [1/129] Reference number 5- 59 A55 --- Ref Reference 63- 81 A19 --- Bibcode Reference bibcode 83-153 A71 --- Com Comment on reference
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 18-Jul-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© Unistra/CNRS