Ultraviolet and X-ray Light-Curves of Novae Observed by the Neil Gehrels Swift Observatory
Abstract
:1. Introduction
2. Observations
3. Analysis and Results
3.1. Light-Curve Descriptions
3.1.1. V2491 Cyg
3.1.2. U Sco
3.1.3. V407 Cyg
3.1.4. T Pyx
3.1.5. V959 Mon
3.1.6. V339 Del
3.1.7. V745 Sco
3.1.8. V1534 Sco
3.1.9. V1535 Sco
3.1.10. V3890 Sgr
3.1.11. V1674 Her
3.1.12. RS Oph
3.2. Normalised Break Times
4. Discussion
4.1. Individual Novae
4.2. Comparing the Sample as a Whole
4.3. Populations
4.3.1. Classical Novae
4.3.2. Recurrent Novae
4.3.3. Symbiotic-like Novae
4.4. Comparison with Previous Work
5. Summary
Supplementary Materials
Author Contributions
Funding
Data Availability Statement
Conflicts of Interest
1 | While most novae are first discovered at optical wavelengths, V959 Mon was initially detected in -rays by the Large Area Telescope onboard Fermi, when too close to the Sun for ground-based telescopes to observe [5,6]. Models of nova eruptions also predict there should be a brief, soft X-ray flash after hydrogen ignition, before the optical emission is detectable. This was finally observed for the first time in 2020 by eROSITA (extended Roentgen Survey with an Imaging Telescope Array) for the nova YZ Ret [7]. |
2 | It is, however, possible for the nuclear burning to cease before the ejecta fully clear, in which case the soft X-rays may fade away before they can be detected. In the case of V745 Sco [8], it was suggested that only the cooling, tail-end of the SSS emission was seen, with the actual hydrogen burning having ended very quickly, placing it close to this `unobservable region’. |
3 | See details at https://www.swift.ac.uk/analysis/uvot/, accessed on 20 November 2022. |
4 | V959 Mon is the exception, with observations starting some time after the actual nova eruption, because of its location with respect to the Sun at outburst (see footnote 1). |
5 | Over the years, distance estimates to novae have changed. We use the most recent derivations by [40], using parallax data from the third Gaia data release (DR3) among other methods, for all our sample bar V407 Cyg, which was not included in this catalogue. |
6 | The SSS phase of V339 Del ended during the solar observing constraint, when no observations could be performed. However, an extrapolation backwards of the decline once observations restarted suggests the X-ray fading began around the same time as the constraint. |
7 | U Sco was observed at a particularly high cadence when trying to map the 1.23-day eclipses. |
8 | https://swift.gsfc.nasa.gov/analysis/uvot_digest/redleak.html, accessed on 20 November 2022. |
9 | V1534 Sco is a possible exception, as previously noted. |
10 | As noted in Table 3, V1534 Sco does not show an obvious SSS phase, with day 7 actually corresponding to the time when the X-ray emission peaked due to the decrease of the absorption. This nova has therefore be omitted from this range. |
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Nova | Alternative Name | Eruption Date UT | P | E(B−V) | Symbiotic? | Distance (kpc) | References |
---|---|---|---|---|---|---|---|
V2491 Cyg | Nova Cyg 2008 No. 2 | 2008-04-10.73 | 2.3 h | 0.23 | 4.8 | [40,41,42,43,44] | |
U Sco | — | 2010-01-28.44 | 1.23 d | 0.20 | 6.3 | [11,40,45,46] | |
V407 Cyg | — | 2010-03-10.80 | 43 y | 0.5 | Y | 3.9 | [47,48,49,50] |
T Pyx | — | 2011-04-14.24 | 1.83 h | 0.25 | 3.6 | [11,40,51,52] | |
V959 Mon | Nova Mon 2012 | 2012-06-22 | 7.1 h | 0.38 | 2.9 | [5,6,40,53,54,55] | |
V339 Del | Nova Del 2012 | 2013-08-14.58 | 0.163 d | 0.18 | 1.6 | [40,56,57] | |
V745 Sco | — | 2014-02-06.69 | 2440 d | 1.00 | Y | 8.0 | [11,40,58,59] |
V1534 Sco | Nova Sco 2014 | 2014-03-26.85 | 520 d | 1.11 | ? | 8.2 | [40,49,60,61,62,63] |
V1535 Sco | Nova Sco 2015 | 2015-02-11.84 | 50 d | 0.80 | Y | 7.8 | [40,49,63,64,65,66,67] |
V3890 Sgr | — | 2019-08-27.87 | 747.6 d | 0.59 | Y | 8.5 | [11,40,68,69,70,71] |
V1674 Her | Nova Her 2021 | 2021-06-12.19 | 0.153 d | 0.50 | 3.2 | [40,72,73,74] | |
RS Oph | — | 2021-08-09.54 | 453.6 d | 0.73 | Y | 2.7 | AAVSO ; [11,40,75,76,77] |
Nova | Filter | T | T | T | T | T | ||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|
(day) | (day) | (day) | (day) | (day) | ||||||||
V2491 | 1.93 | 40.2 | 4.60 | 55.1 | 2.91 | 124 | 1.5 | |||||
Cyg | ||||||||||||
U Sco | 0.54 | 4.4 | 3.0 | 12.52 | −0.28 | 24.19 | 4.99 | 44.51 | −2.85 | 52.28 | 8.34 | |
0.44 | 3.9 | 3.20 | 12.53 | 0.02 | 25.15 | 5.61 | 41.8 | −0.33 | 52.34 | 7.56 | ||
V407 | 0.35 | 41.4 | 4.39 | 63 | 2.23 | |||||||
Cyg | ||||||||||||
T Pyx | 6.54 | 113.90 | 1.27 | 142.59 | 7.03 | 150.2 | 4.05 | 268.7 | 1.38 | |||
V959 | 2.02 | 212 | 5.33 | |||||||||
Mon | 1.83 | 205 | 4.91 | |||||||||
2.07 | 205 | 5.29 | ||||||||||
V339 | — | — | 1.1 | 138 | 2.4 | 258 | 1.5 | |||||
Del | 3.0 | 81 | 0.8 | 129 | 2.17 | 266 | 1.7 | |||||
— | — | 0.94 | 133 | 2.96 | 264 | 2.1 | ||||||
V745 | 0.68 | 6.3 | 3.01 | 15.7 | 1.45 | |||||||
Sco | 0.53 | 5.5 | 2.4 | 18 | 1.40 | |||||||
0.73 | 7.8 | 3.62 | 15.5 | 1.46 | ||||||||
V1534 | 0.75 | 9.5 | 3.65 | 22 | 1.1 | |||||||
Sco | 0.5 | 4.9 | 1.7 | — | — | |||||||
0.43 | 9.4 | 3.7 | — | — | ||||||||
V1535 | 0.71 | 16.2 | 5.20 | 19.0 | 2.0 | 31.4 | 3.7 | 44.4 | −1.32 | 67 | 5.00 | |
Sco | 0.85 | 16.0 | 6.4 | 18.2 | 2.2 | — | — | — | — | — | — | |
V3890 | 0.88 | 13 | 1.4 | 21.6 | 4.7 | 30.2 | 2.9 | 41 | 2.1 | |||
Sgr | ||||||||||||
V1674 | — | — | 2.2 | 30 | 2.1 | 77 | 1.2 | |||||
Her | 2.1 | 12.3 | 1.96 | 32 | 2.02 | 86 | 0.80 | |||||
1.6 | 15 | 2.6 | 30 | 2.2 | — | — | ||||||
RS | uvm2 | 0.99 | 27 | 1.70 | 76 | 3.6 | ||||||
Oph | uvw2 | 1.1 | 40 | 1.8 | 68 | 2.6 |
Nova | T–T | Filter | T | T | T | T | T |
---|---|---|---|---|---|---|---|
(day) | (norm.) | (norm.) | (norm.) | (norm.) | (norm.) | ||
V2491 Cyg | 33–43 | 0.9 | 1.3 | 2.9 | |||
U Sco | 12–33 | 0.1 | 0.4 | 0.7 | 1.4 | 1.6 | |
0.1 | 0.4 | 0.8 | 1.3 | 1.6 | |||
V407 Cyg | 12–40 | 1.0 | 1.6 | ||||
T Pyx | 123–180 | 0.6 | 0.79 | 0.83 | 1.5 | ||
V959 Mon | 150–200 | 1.1 | |||||
1.0 | |||||||
1.0 | |||||||
V339 Del | 60–144 | — | 0.9 | 1.8 | |||
0.6 | 0.9 | 1.8 | |||||
— | 0.9 | 1.8 | |||||
V745 Sco | 3–6 | 1.1 | 2.6 | ||||
0.9 | 3.2 | ||||||
1.3 | 2.6 | ||||||
V1534 Sco | 7 | 1.4 | 3.2 | ||||
0.7 | — | ||||||
1.2 | — | ||||||
V1535 Sco | 12–25 | 0.6 | 0.8 | 1.3 | 1.8 | 2.7 | |
0.6 | 0.7 | — | — | — | |||
V3890 Sgr | 8–20 | 0.7 | 1.1 | 1.5 | 2.1 | ||
V1674 Her | 19–45 | — | 0.7 | 1.7 | |||
0.3 | 0.7 | 1.9 | |||||
0.3 | 0.7 | — | |||||
RS Oph | 21–62 | 0.4 | 1.2 | ||||
0.6 | 1.1 |
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Page, K.L.; Kuin, N.P.M.; Osborne, J.P. Ultraviolet and X-ray Light-Curves of Novae Observed by the Neil Gehrels Swift Observatory. Universe 2022, 8, 643. https://doi.org/10.3390/universe8120643
Page KL, Kuin NPM, Osborne JP. Ultraviolet and X-ray Light-Curves of Novae Observed by the Neil Gehrels Swift Observatory. Universe. 2022; 8(12):643. https://doi.org/10.3390/universe8120643
Chicago/Turabian StylePage, Kim L., N. Paul M. Kuin, and Julian P. Osborne. 2022. "Ultraviolet and X-ray Light-Curves of Novae Observed by the Neil Gehrels Swift Observatory" Universe 8, no. 12: 643. https://doi.org/10.3390/universe8120643