NOVA LIGHT CURVES FROM THE SOLAR MASS EJECTION IMAGER (SMEI). II. THE EXTENDED CATALOG

Classical novae (CNe) belong to the cataclysmic variable (CV) class of objects. These are interacting close binary systems in which mass is transferred from a donor star to the surface of an accreting compact companion, leading to a variety of behaviors, the most noticeable of which is an eruption (see Bode & Evans 2008; Bode 2010, for reviews).

A typical CN system consists of a white dwarf (WD) primary and a cooler, lower-mass main-sequence secondary star (spectral type ranging from F to M; Darnley et al. 2012). As the secondary evolves, it fills its Roche lobe, allowing hydrogen-rich material to transfer at a rate of 10⁻¹¹–10⁻⁹ ${M}_{\odot }$ yr⁻¹ via the inner Lagrangian point (L1) toward the WD and form an accretion disk. Material is deposited from the disk onto the surface of the WD, causing the bottom of the accreted layer on the WD to become electron degenerate. Within this degenerate layer hydrogen burning ensues, leading to a thermonuclear runaway (TNR) and ultimately the CN eruption. The total radiant output of a single CN eruption is in the range of 10⁴⁵–10⁴⁶ erg, with TN-outburst amplitudes of approximately 10−20 mag and absolute V-band magnitudes of ${M}_{V}=-10.7$ at maximum for the fastest and most luminous CNe (Shafter et al. 2009 and references therein). The resulting energy released is sufficient to expel the accreted envelope and drive mass loss (10⁻⁵–10⁻⁴ M_⊙; Goss et al. 2011) at velocities of a few hundred to several thousand kilometers per second⁻¹. All CNe are thought to have repeat eruptions (although for some this may take up to ${10}^{4}/{10}^{5}$ yr; Hernanz 2005); however, a CN observed in TN outburst more than once is reclassified as a recurrent nova (RN); observed recurrence times range from 1 to 100 yrs (Darnley et al. 2014, 2015), or even as short as 6 months (Henze et al. 2015), with TN-outburst amplitudes typically smaller than CNe (≈5–6 mag if the secondary is giant, 10–15 if a main-sequence star). The basic triggering and explosion mechanism of an RN is the same as for a CN, but there are some distinct differences in the physical properties of this subgroup. In order to reconcile the short quiescence period of an RN with a TNR, the WDs within these systems are believed to be hotter, more massive (close to the Chandrasekhar 1931, limit), and have higher mass accretion rates (∼10⁻⁸–10⁻⁷ M_⊙ yr⁻¹) than CNe (see Yaron et al. 2005; Wolf et al. 2013). The majority of RN systems also harbor evolved secondary stars rather than the typical main-sequence star of a CN system (see, e.g., Darnley et al. 2012).

As with most transients, CNe are traditionally classified according to their photometric and spectroscopic properties. Each nova has its own unique optical light curve. However, they do share a common idealized nova light curve (McLaughlin 1960). Most novae tend to rise rapidly to peak within 1–3 days. Owing to the transient nature of a nova, this initial rise has rarely been observed well enough to establish any classification regime, but the subsequent decline from maximum has. Novae tend to be classified according to the number of days that they take to decline n magnitudes from maximum; thus, they are divided into "speed classes." These classes were first introduced by Gaposchkin (1957), and often declines of two or three magnitudes are quoted (t₂ and t₃, respectively).

During the initial rise, novae are thought to experience a pre-maximum halt (PMH) approximately one to two magnitudes below maximum (McLaughlin 1960). The duration of this halt appears to be related to the speed class of the nova, lasting a few hours for fast novae and a few days for slow novae. Until recently the PMH had only been observed for a few slow novae such as DQ Her, V450 Cyg (Gaposchkin 1957), V723 Cas, V463 Sct (Hachisu & Kato 2004, who present a new interpretation of the observed long PMHs), and V5558 Sgr (Tanaka et al. 2011), with no strong evidence to suggest that it was also present for the faster speed classes. Hounsell et al. (2010b, hereafter Paper I), however, found from Solar Mass Ejection Imager (SMEI) observations that for all very fast/fast novae (classical and recurrent) studied in detail in that paper, a PMH was detected with a duration consistent with their speed class. The PMHs of the very fast novae observed in Paper I consisted of three to four SMEI data points in which a temporary reversal of the light curve was suggested and its duration was calculated as the time between the first and third change in gradient of the slope. The PMH of the one fast nova detected (V1280 Sco) was represented by a plateau in the light curve and made up of seven SMEI data points. Here the PMH duration was taken as the time between the first and second change of gradient. If a slower nova were to have been detected within the SMEI data, we might expect a similar plateau.

Although there is now evidence for the existence of this phase of evolution in the nova light curve, no physical explanation for the PMH is currently accepted, although several theories exist. Williams (2012) suggests that a PMH lasting a day or more may be caused by an enhancement of mass loss from the secondary star, which then dominates over the initial WD ejecta. This changeover in the dominance of the two mass-loss sources could be the cause of the halt. Other work by Hillman et al. (2014) has used nova evolution simulations (via a hydrodynamic Lagrangian code) to create detailed light curves, and find that halts of long or short duration occur naturally within the burst. Examining the evolution of nova effective temperature (${T}_{{\rm{eff}}}$), luminosity, and radius, they find that at a point just before expansion and mass loss occur, the ${T}_{{\rm{eff}}}$ deceases and the rising luminosity halts. Their work also found that this halt would in many cases be accompanied by a dip in the total luminosity. Such a dip is due to a temporary drop in the energy flux as convection in the expanding and thinning envelope ceases to be efficient near the envelope surface. Because of the decreasing opacity of the envelope, radiation soon dominates over convection, thus reversing the dip. Work by both Hillman et al. (2014) and Williams (2012) is WD mass dependent.

The majority of Galactic novae are still discovered by the amateur community. Over the past century various surveys have attempted to measure the Galactic rate; however, results are greatly affected by temporal and spatial coverage, selection effects, and interstellar extinction. Based on an extrapolation of the observed nova rates in the solar neighborhood (assumed complete to m < 2), Shafter (1997) estimated a Galactic nova rate of approximately 35 yr⁻¹; this is supported by Darnley et al. (2006), with a value of ${34}_{-12}^{+15}$ yr⁻¹. Of these, an average of roughly one CN per year has been observed to reach ${m}_{V}$ = 8 or brighter (see Figure 2 of Shafter 2002). It is well known that novae with the highest peak bolometric luminosity fade the most rapidly and are thus often missed; historical observations are therefore clearly incomplete at m_V = 8, and the actual number of novae reaching this brightness is expected to be significantly higher (∼5 yr⁻¹; see Shafter 2002; Warner et al. 2008, and discussion in Paper I).

With the advent of all-sky imaging facilities, both ground and space based, there is new hope for detecting a more complete sample of Galactic novae. Although the detection of transient events may not be the original science objective of these missions, their archives hold a wealth of data on many events. These observations may contain great detail and provide data on many previously poorly examined and understood phases of evolution. Examination of these archives is therefore exceptionally important. One such space-based all-sky mission is the SMEI; its usefulness in observing novae was well documented in Paper I, Hounsell et al. (2010a, 2011, 2012), Surina et al. (2014), and Darnley et al. (2013).

SMEI is a high-precision white-light differential photometer (Buffington et al. 2006, 2007) based on board the Coriolis solar satellite. SMEI was in operation from 2003 January (Eyles et al. 2003; Jackson et al. 2004) until 2011 September. The instrument consists of three baffled CCD cameras each with a $60^\circ \quad \times \quad$ 3° field of view, combining to sweep out nearly the entire sky with each 102-minute orbit of the spacecraft (Hick et al. 2007). The peak throughput of the instrument is at approximately 700 nm with an FWHM ∼ 300 nm. SMEI is able to reliably detect brightness changes in point sources down to at least 8th magnitude.

SMEI was originally designed to map out large-scale variations in heliospheric electron densities by observing the Thomson-scattered sunlight from solar wind electrons (Jackson et al. 2004). In order to isolate the faint Thomson-scattered sunlight, the much larger white-light contributions from the zodiacal dust cloud, the sidereal background, and individual point sources (bright stars and planets) were determined and removed (see Hick et al. 2007, for further details). Thus, brightness determination of point sources is a routine step in the SMEI data analysis and as such has led to the production of detailed light curves for many bright objects including variables (see, e.g., Buffington et al. 2006; Spreckley & Stevens 2007; Tarrant et al. 2007, 2008a, 2008b, 2008c; Clover et al. 2011; Goss et al. 2011; Surina et al. 2014; Paper I).

This paper presents results from the examination of nine additional Galactic novae observed by SMEI. These novae are fainter than the four presented in Paper I and indicate the limit of SMEI's ability to detect brightness changes at fainter magnitudes and in crowded regions. In Section 2 we explain how data were obtained and analyzed. Section 3 presents our results, and a discussion are conclusions are provided in Section 4.

The SMEI database contains a catalog with the names, co-ordinates, and discovery magnitudes of 62 Galactic CNe and 3 RNe, with eruptions dating between 2003 and 2011. The photometry of each nova in this paper was obtained using this catalog and an extended iterative least-squares fit of the point-spread function (PSF) as described in Hick et al. (2005, 2007) and Section 2 of Paper I. Zodiacal and sidereal background light contributions were also considered during the fitting stage. The remaining 51 novae not examined as part of this paper, Surina et al. (2014), or Paper I either were too faint for detection or resided in fields far too crowded for reliable results to be obtained.

As noted in Paper I, the SMEI PSF has a full width of approximately 1° and is highly asymmetric with a "fish-like" appearance. Owing to this large size, an object of interest is considered crowded when it lies less than one PSF width from another bright object (typically 6th magnitude or brighter); such crowding within the SMEI data is commonplace. To combat this issue, simultaneous fitting of multiple objects can be initiated where possible (stellar separation >075) and contamination of the object of interest reduced.

In order to achieve the best fit and produce the most reliable nova light curve, the surrounding region of each object required assessment for levels of potential contamination due to crowding, cosmic-ray hits, and finally their proximity to the sunward and antisunward masks (see Buffington et al. 2006, 2007, for a description of these masks). If the nova was in a crowded field, a simultaneous fit was conducted and the area used to sample the surrounding stellar region (wing radius) from the PSF centriod reduced. The reduction of the wing radius also reduces errors if the object is located near a masked region. For these reasons multiple light curves were generated for each nova using an auto_wing¹¹ radius and wing radii of 12, 13, and 14. The resulting photometry files were then assessed on several criteria: (1) correlation of the fitted PSF to the model, via the sample Pearson correlation coefficient ( r ); (2) the number of pixels used to define the PSF fitting area, which is often an indictor of masks or image defects ( npsf ); (3) variation of the background fitted value; (4) deviation of the R.A. and decl. from the catalog position, where jumps can be an indication of the fitting of a residual from the poor subtraction of a neighboring star; this becomes more of an issue as the nova fades.

Within Paper I, points possessing r ≥ 0.5 were deemed reliable. However, as the novae presented here are much fainter, a less stringent cutoff of 0.4 was found to be acceptable. A 1σ threshold was applied to the other selection criteria listed above (in some cases a 3σ cutoff was applied if the object was detected only a few times by the instrument, or if the initial R.A. and decl. were uncertain). Using the filtered file that possessed the highest number of "valid" points, the flux of the nova was then converted into an unfiltered SMEI apparent magnitude (${m}_{\mathrm{SMEI}}$) and its error contribution calculated from photon counting statistics.

As noted above, the novae presented in this paper are much fainter than those given in Paper I, all of which possessed a peak ${m}_{{\rm{SMEI}}}$ < 5.5. The objects within this paper have peak magnitudes between 6 and 8; fainter than this detection is unreliable. The light curves derived, although more noisy than those in Paper I, have nonetheless provided precise measurements of peak time, eruption magnitude, and in many cases a value for t₂. Table 1 summarizes our main findings, and the individual novae are discussed below. Novae that possess the most interesting data are presented first, with the remaining given in order of eruption date. Where possible a light curve for each nova has been presented, with a legend for all data given in Figure 1. An Appendix tabulating the available photometry for each nova examined is included at the end of the paper.

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Table 1.  Derived Light-curve Parameters of 14 Novae Using Data from the Solar Mass Ejection Imager

Name	Time of	Peak	t2	Speed	Pre-max	Pre-max	${\rm{\Delta }}{m}_{{\rm{SMEI}}}$	${\rm{\Delta }}t$ From	Wing
	Maximum	SMEI	(days)	Classa	Duration	Mean	From Halt	Halt to	Radius
	(yyyy/mm/dd)	Magnitude			(days)b	Magnitude	to Peakc	Peak (days)	(deg)
V1187 Sco	2004/08/3.77${}_{-0.04}^{+0.07}$	6.95 ± 0.04	10.10${}_{-0.39}^{+0.43}$ d	Very fast	⋯	⋯	⋯	⋯	1.3
V2467 Cyg	2007/03/16.56 ± 0.04	6.30 ± 0.03	${5.68}_{-0.53}^{+0.61}$ d	Very fast	⋯	⋯	⋯	⋯	1.3
V458 Vul	2007/08/13.66 ± 0.04	7.94 ± 0.07	⋯	Fast	⋯	⋯	⋯	⋯	auto-wing
V597 Pup	2007/11/14.68${}_{-0.35}^{+0.04}$	6.91 ± 0.04	2.81${}_{-0.90}^{+1.0}$ d	Very fast	0.21	8.07 ± 0.14	1.16	0.96	1.3
V459 Vul	2007/12/28.11${}_{-0.07}^{+0.11}$	6.59 ± 0.04	∼19.4e	Fast	⋯	⋯	⋯	⋯	1.2
V2491 Cyg	2008/04/10.89 ± 0.04	7.36 ± 0.05	⋯	Very fast	⋯	⋯	⋯	⋯	1.2
QY Mus	2008/09/28.63 ± 0.2	6.93 ± 0.04	⋯	Moderately fast	⋯	⋯	⋯	⋯	1.2
V5580 Sgr	2008/11/30.85	7.01 ± 0.04	⋯	⋯	⋯	⋯	⋯	⋯	auto-wing
V5583 Sgr	2009/08/7.08 ± 0.04	6.94 ± 0.05	⋯	Very fast	0.21	7.64 ± 0.03	0.71	1.10	1.4
T Pyxf	2011/05/12.22 ± 0.04	6.33 ± 0.03	⋯	Slow	∼10	∼8.1	∼1.8	14.6	⋯
RS Oph	2006/02/12.94 ± 0.04	3.87 ± 0.01	7.9	Very fast	0.14	4.50 ± 0.05	0.63	0.49	1.25
V1280 Sco	2007/02/16.15 ± 0.04	4.00 ± 0.01	21.3	Fast	0.42	5.231 ± 0.003	1.23	0.49	1.25
V598 Pup	2007/06/6.29 ± 0.04	3.46 ± 0.01	4.3	Very fast	0.28	5.2 ± 0.1	1.74	2.19	1.4
KT Eri	2009/11/14.67 ± 0.04	5.42 ± 0.02	6.6	Very fast	0.14	6.04 ± 0.07	0.63	0.71	1.25

Notes. The last five novae listed represent objects reported within Hounsell et al. (2012), Surina et al. (2014), and Paper I. Novae in this paper tend to be fainter than those in Paper I, and as such we were unable to obtain in most cases all parameters listed in the table.

^aV1187 Sco—Lynch et al. (2006), V2467 Cyg—Lynch et al. (2009), V458 Vul—Wesson et al. (2008), V597 Pup—Naik et al. (2009), V459 Vul—Poggiani (2010), V2491 Cyg—Munari et al. (2011) and Darnley et al. (2011), QY Mus—Schwarz et al. (2011), V5583 Sgr—Schwarz et al. (2011). ^bHere the duration of the halt is taken to be the time between the first and third change in gradient of the rising light curve for very fast novae. For fast and moderately fast it is the first and second change. ^c ${\rm{\Delta }}{m}_{{\rm{SMEI}}}$ from halt to peak is calculated using the mean magnitude of the PMH. ^dBased on a linear fit of the initial decline data from the SMEI nova light curve (see text for further details). ^eUsing linear extrapolation between the first and last data point of the SMEI light curve (see text for further details). ^fHere all data have been taken from Surina et al. (2014). Within this work the PMH was suggested to have lasted for ≈10 days with magnitudes varying between 7.7 and 8.5; hence, a mean magnitude of 8.1 was quoted in the above table. The time between halt and peak was also taken, in this case, from the end of the PMH phase.

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3.1. V597 Puppis

Nova V597 Pup (α = ${08}^{{\rm{h}}}{16}^{{\rm{m}}}18\buildrel{\rm{s}}\over{.} 01,\$ δ = $-34^\circ 15^{\prime} 24\buildrel{\prime\prime}\over{.} 1$; J2000) was discovered in TN outburst by Pereira et al. (2007) at a visual magnitude of 7.0 on 2007 November 14.23 UT (MJD 54,418.23), reaching a peak visual magnitude of ${m}_{V}$ = 6.4 on 2007 November 14.48 UT (MJD 54,418.48, green cross within Figure 2). The nova then declined rapidly with a ${t}_{{\rm{2}}}$ = 2.5 days (Naik et al. 2009), making it one of the fastest novae recorded. Naik et al. (2009) classified the nova as an He/N-type with a WD close to the Chandrasekhar limit. A pre-eruption detection is found within the Digitized Sky Survey (Pereira et al. 2007) with a source at V ∼ 20, which coincides with the nova position. Continued monitoring of the object by Warner & Woudt (2009) revealed the nova as an intermediate polar (IP) in the orbital period gap (${P}_{{\rm{orb}}}$ = 2.67 hr), with a rotational period of 8.7 minutes. Observation of the object a year after eruption also revealed the presence of a deep secondary eclipse caused by the passage of the optically thick accretion disk in front of the irradiated side of the secondary star. The object is considered unique as it is the first CV found to have this deep an eclipse.

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Table 2.  SMEI Light-curve Data for Nova V1187 Sco

Date-Obs MJD	SMEI Mag	SMEI Error	r
53,215.68	7.47	0.05	0.73
53,217.52	7.49	0.05	0.72
53,217.66	7.62	0.05	0.70
53,217.80	7.59	0.05	0.71
53,218.01	7.67	0.05	0.71
53,218.08	7.73	0.06	0.69
53,218.30	7.66	0.05	0.70
53,218.37	7.78	0.06	0.76
53,218.86	7.87	0.06	0.74
53,219.92	7.37	0.05	0.63
53,219.99	7.17	0.04	0.64
53,220.06	7.29	0.05	0.64
53,220.13	7.26	0.05	0.63
53,220.20	7.07	0.04	0.66
53,220.27	7.20	0.04	0.61
53,220.34	7.02	0.04	0.65
53,220.41	7.03	0.04	0.63
53,220.48	7.03	0.04	0.64
53,220.55	7.01	0.04	0.64
53,220.62	7.12	0.04	0.64
53,220.70	7.04	0.04	0.62
53,220.77	6.95	0.04	0.63
53,220.91	7.09	0.04	0.57
53,220.98	7.06	0.04	0.60
53,221.26	6.97	0.04	0.61
53,221.33	7.11	0.04	0.58
53,221.40	7.15	0.04	0.58
53,221.47	7.20	0.04	0.54
53,221.54	7.29	0.05	0.57
53,221.61	7.32	0.05	0.57
53,221.68	7.33	0.05	0.57
53,221.75	7.43	0.05	0.55
53,221.82	7.29	0.05	0.55
53,221.89	7.25	0.04	0.56
53,221.96	7.52	0.05	0.53
53,222.04	7.54	0.05	0.52
53,222.18	7.50	0.05	0.51
53,222.25	7.46	0.05	0.52
53,222.32	7.53	0.05	0.50
53,222.39	7.63	0.05	0.50
53,222.53	7.41	0.05	0.51
53,222.60	7.54	0.05	0.49
53,222.67	7.63	0.05	0.47
53,222.81	7.53	0.05	0.50
53,222.88	7.60	0.05	0.48
53,222.95	7.52	0.05	0.49
53,223.02	7.49	0.05	0.49
53,223.09	7.53	0.05	0.49
53,223.23	7.49	0.05	0.47
53,223.80	7.70	0.06	0.46
53,223.87	7.57	0.05	0.45
53,223.94	7.81	0.06	0.43
53,224.01	7.60	0.05	0.44
53,224.29	7.94	0.06	0.40
53,224.36	7.70	0.05	0.44
53,224.43	7.52	0.05	0.44
53,224.50	7.91	0.06	0.41
53,224.57	7.84	0.06	0.43
53,224.64	7.74	0.06	0.42
53,224.71	7.81	0.06	0.41
53,224.79	7.85	0.06	0.40
53,224.86	7.77	0.06	0.42
53,224.93	7.79	0.06	0.41
53,225.00	7.81	0.06	0.42
53,225.21	7.91	0.06	0.42
53,225.28	7.56	0.05	0.48
53,225.35	7.83	0.06	0.44
53,225.42	7.91	0.06	0.42
53,225.49	7.94	0.06	0.42
53,226.20	7.84	0.06	0.44
53,226.27	7.95	0.06	0.43
53,226.34	8.05	0.06	0.42
53,226.48	8.30	0.07	0.39
53,226.55	8.48	0.08	0.38
53,226.62	8.08	0.07	0.38
53,226.83	8.42	0.08	0.35
53,226.90	8.46	0.08	0.35
53,226.97	8.38	0.07	0.33
53,227.04	8.08	0.07	0.35
53,227.26	8.77	0.09	0.31
53,227.33	8.42	0.08	0.36
53,227.40	8.31	0.07	0.34
53,227.54	8.37	0.07	0.33
53,229.45	8.42	0.08	0.33
53,229.94	8.38	0.07	0.36
53,230.01	8.47	0.08	0.31
53,230.79	8.69	0.09	0.37
53,231.21	9.49	0.12	0.35
53,231.28	9.37	0.12	0.34
53,231.91	9.08	0.10	0.31

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Table 3.  SMEI Light-curve Data for Nova V2467 Cyg

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,160.88	13.07	0.67	0.31
54,161.38	10.30	0.19	0.30
54,167.16	10.63	0.22	0.42
54,170.27	9.10	0.11	0.54
54,173.52	10.26	0.19	0.55
54,173.80	9.14	0.11	0.57
54,173.87	8.85	0.10	0.56
54,173.94	9.85	0.15	0.58
54,174.01	8.78	0.09	0.55
54,174.08	7.90	0.06	0.53
54,174.15	7.77	0.06	0.52
54,174.22	7.77	0.06	0.58
54,174.43	7.14	0.04	0.58
54,174.50	7.06	0.04	0.57
54,174.57	7.12	0.04	0.63
54,174.64	6.80	0.04	0.59
54,174.71	6.83	0.04	0.60
54,174.79	6.80	0.04	0.62
54,174.86	6.75	0.04	0.61
54,174.93	6.64	0.04	0.68
54,175.00	6.65	0.04	0.65
54,175.07	6.48	0.03	0.67
54,175.14	6.55	0.03	0.62
54,175.21	6.61	0.04	0.63
54,175.28	6.60	0.03	0.55
54,175.42	6.61	0.04	0.56
54,175.49	6.50	0.03	0.67
54,175.56	6.30	0.03	0.70
54,175.63	6.40	0.03	0.67
54,176.48	7.21	0.05	0.35
54,176.55	7.20	0.05	0.39
54,176.62	7.46	0.05	0.32
54,176.69	7.20	0.05	0.37
54,176.76	7.15	0.05	0.37
54,176.83	7.22	0.05	0.35
54,176.90	7.27	0.05	0.35
54,181.77	9.32	0.12	0.38
54,182.26	9.29	0.12	0.43
54,182.48	9.18	0.11	0.37
54,182.55	9.60	0.14	0.42
54,182.62	9.86	0.15	0.44
54,182.69	8.55	0.08	0.43
54,182.76	9.38	0.12	0.45
54,182.83	8.89	0.10	0.46
54,182.90	8.44	0.08	0.43
54,183.46	10.53	0.21	0.38
54,183.54	9.43	0.13	0.46
54,183.61	10.44	0.20	0.40
54,183.75	8.78	0.09	0.50
54,183.82	8.97	0.10	0.48
54,184.03	7.73	0.06	0.33
54,184.10	7.71	0.06	0.43
54,184.17	7.93	0.06	0.38
54,184.59	7.66	0.06	0.31
54,184.73	8.19	0.07	0.38
54,184.80	7.86	0.06	0.33
54,184.88	8.17	0.07	0.37
54,184.95	7.81	0.06	0.33

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The light curve created using the SMEI data set covers the latter part of the initial rise, peak, and early decline (see Figure 2). There does appear to be one data point on 2007 November 7.04 UT (MJD 54,407.04) at ${m}_{{\rm{SMEI}}}$ = 9.57 ± 0.13; however, the r of this point is only 0.34 and thus not reliable. All data after this point and up to the initial rise possess an r less than 0.3 and are therefore omitted from Figure 2 and further discussion. Examination of the initial rise hints at the possibility of a PMH starting on 2007 November 13.63 UT (MJD 54,417.63) and lasting several hours with a mean ${m}_{{\rm{SMEI}}}$ = 8.07 ± 0.14 (defined as the mean magnitude over the duration of the halt; quoted error is the rms scatter). As in Paper I, the duration of the halt for this object is taken to be the time between the first and third changes in gradient of the rising light curve and is appropriate for the speed class of the nova. It should be noted, however, that the first two points of this halt have r < 0.4 (actual values are 0.39 and 0.35, respectively; this lower r is due in part to the limiting magnitude of SMEI), and as such the reality of this PMH can not be confirmed. There is then a gap in the data lasting several hours due to the SMEI weekly calibration, after which the nova is seen to reach its maximum intensity of ${m}_{{\rm{SMEI}}}=6.91\pm 0.04$ on 2007 November ${14.68}_{-0.35}^{+0.04}$ UT (MJD 54,418.68). This coincides better with the R-band magnitude of 6.7 on 2007 November 14.48 UT (MJD 54,418.48) given in Pereira et al. (2007; red cross within Figure 2) than the V-band data quoted above. Note, however, that it is possible that the peak nova brightness actually occurred in the data gap caused by the weekly calibration. This uncertainty has been included in the quoted time of maximum. The decline of the nova is shown by SMEI to be exceptionally fast, but given the scatter off the data around 8/9 magnitude, a direct measurement of ${t}_{{\rm{2}}}$ could not be made. However, assuming that the data can be modeled by a simple linear decline (as is often seen in the early stages of nova light curves), we derived an approximate ${t}_{{\rm{2}}}$ time of ${2.81}_{-0.9}^{+1.0}$ days (error quoted is statistical only and was obtained using the uncertainties of the fitted gradient and intercept). This is similar to the value given by Naik et al. (2009), confirming the very fast classification. Within Figure 2, the SMEI light curve is also compared to AAVSO data (V band) and data (B, V, R, and I band) from the STONY BROOK/SMARTS Atlas of (mostly) Southern Novae¹² (hereafter referred to as the Nova Atlas; see Walter et al. 2012, for a full description) within the same time frame.

Table 4.  SMEI Light-curve Data for Nova V458 Vul

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,321.22	8.57	0.10	0.40
54,321.86	8.06	0.08	0.62
54,321.93	8.04	0.07	0.66
54,322.00	8.15	0.08	0.65
54,322.07	8.16	0.08	0.65
54,322.14	8.40	0.09	0.60
54,322.35	8.56	0.09	0.55
54,322.49	8.36	0.09	0.53
54,322.70	8.20	0.08	0.58
54,322.91	8.39	0.09	0.52
54,322.98	8.38	0.09	0.53
54,323.12	8.36	0.09	0.51
54,323.48	8.30	0.08	0.49
54,323.55	8.33	0.09	0.49
54,323.62	8.45	0.09	0.44
54,323.83	8.38	0.09	0.49
54,323.90	8.45	0.09	0.47
54,324.04	8.47	0.09	0.46
54,324.11	8.56	0.09	0.49
54,324.18	8.20	0.08	0.56
54,324.25	8.18	0.08	0.54
54,324.46	8.41	0.09	0.50
54,324.54	8.50	0.09	0.47
54,324.61	8.47	0.09	0.46
54,324.75	8.31	0.08	0.51
54,324.82	8.51	0.09	0.47
54,324.96	8.23	0.08	0.53
54,325.10	8.17	0.08	0.57
54,325.17	8.14	0.08	0.58
54,325.24	8.29	0.08	0.54
54,325.31	8.15	0.08	0.58
54,325.38	8.11	0.08	0.56
54,325.45	8.17	0.08	0.58
54,325.52	8.13	0.08	0.64
54,325.59	8.07	0.08	0.64
54,325.66	7.94	0.07	0.68
54,325.73	7.98	0.07	0.70
54,325.80	8.00	0.07	0.67
54,325.88	7.98	0.07	0.71
54,325.95	8.07	0.08	0.69
54,326.02	8.13	0.08	0.67
54,326.09	8.14	0.08	0.67
54,326.23	8.34	0.09	0.61
54,326.30	8.43	0.09	0.55
54,326.58	8.26	0.08	0.54
54,326.65	8.32	0.09	0.52
54,326.72	8.47	0.09	0.48
54,326.86	8.63	0.10	0.48
54,327.43	8.51	0.09	0.43
54,327.57	8.57	0.10	0.48
54,328.06	8.87	0.11	0.42
54,328.13	8.64	0.10	0.44
54,328.20	8.31	0.08	0.47
54,328.34	8.57	0.10	0.47
54,328.41	8.44	0.09	0.52
54,328.63	8.84	0.11	0.48
54,328.70	8.87	0.11	0.43

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Table 5.  SMEI Light-curve Data for Nova V597 Pup

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,407.04	9.57	0.13	0.34
54,416.43	10.48	0.20	0.43
54,416.50	10.30	0.18	0.31
54,417.34	9.56	0.13	0.40
54,417.48	8.79	0.09	0.37
54,417.62	8.34	0.07	0.39
54,417.70	7.97	0.06	0.35
54,417.84	7.89	0.06	0.40
54,417.91	7.76	0.06	0.41
54,417.98	7.69	0.06	0.41
54,418.54	7.02	0.04	0.61
54,418.61	6.96	0.04	0.64
54,418.68	6.91	0.04	0.66
54,418.75	7.03	0.04	0.63
54,418.82	7.17	0.04	0.55
54,418.89	7.23	0.05	0.55
54,418.96	7.24	0.05	0.58
54,419.04	7.17	0.04	0.59
54,419.11	7.22	0.04	0.56
54,419.18	7.33	0.05	0.58
54,419.25	7.33	0.05	0.55
54,419.32	7.42	0.05	0.52
54,419.39	7.51	0.05	0.52
54,419.53	7.73	0.06	0.49
54,419.60	7.76	0.06	0.45
54,419.67	8.05	0.07	0.44
54,419.74	7.87	0.06	0.47
54,419.81	7.93	0.06	0.45
54,419.88	7.75	0.06	0.44
54,419.95	7.80	0.06	0.44
54,420.23	8.28	0.07	0.47
54,420.30	8.70	0.09	0.47
54,420.45	8.45	0.08	0.44
54,420.52	8.59	0.08	0.46
54,420.66	8.30	0.07	0.49
54,420.94	8.50	0.08	0.46
54,421.01	8.95	0.10	0.42
54,421.22	8.96	0.10	0.47
54,421.29	8.78	0.09	0.45
54,421.36	8.72	0.09	0.46
54,421.65	8.69	0.09	0.50
54,421.72	8.75	0.09	0.48
54,421.79	8.72	0.09	0.49
54,422.00	9.10	0.11	0.43
54,422.07	8.87	0.10	0.55
54,422.28	9.38	0.12	0.44
54,422.42	9.22	0.11	0.48
54,422.56	8.99	0.10	0.50
54,422.63	8.86	0.09	0.50
54,422.78	9.07	0.10	0.51
54,422.85	9.31	0.12	0.50
54,422.92	8.97	0.10	0.51
54,422.99	9.12	0.11	0.45
54,423.06	8.98	0.10	0.46
54,423.20	8.70	0.09	0.45
54,423.34	9.61	0.13	0.55
54,423.48	10.89	0.24	0.54
54,423.76	9.82	0.15	0.50
54,424.12	10.29	0.18	0.48
54,424.19	9.32	0.12	0.43
54,424.33	9.54	0.13	0.52
54,424.96	8.81	0.09	0.48
54,426.73	10.38	0.19	0.49
54,426.80	9.00	0.10	0.51
54,426.87	8.98	0.10	0.45
54,427.36	9.43	0.12	0.52
54,427.43	10.06	0.16	0.48
54,427.64	10.35	0.19	0.47
54,427.71	10.20	0.17	0.45
54,427.86	10.73	0.22	0.44
54,428.07	11.35	0.29	0.30
54,428.14	9.49	0.13	0.40
54,428.35	9.15	0.11	0.46
54,428.42	9.54	0.13	0.47
54,428.70	9.43	0.12	0.46
54,428.77	9.32	0.12	0.46
54,428.84	9.00	0.10	0.46
54,428.91	10.19	0.17	0.49
54,429.41	12.00	0.40	0.48
54,429.62	11.19	0.27	0.44
54,429.97	10.49	0.20	0.48
54,430.25	11.65	0.34	0.44
54,430.61	11.13	0.27	0.48
54,430.82	10.74	0.22	0.50
54,430.89	11.66	0.34	0.52
54431.03	11.25	0.28	0.47
54,433.00	10.73	0.22	0.45
54,433.22	9.78	0.14	0.52
54,434.91	12.96	0.61	0.52
54,435.12	9.82	0.15	0.47
54,435.19	11.63	0.33	0.50
54,435.41	11.07	0.26	0.50
54,436.11	11.71	0.35	0.50
54,436.89	11.87	0.37	0.44
54,437.24	11.02	0.25	0.44
54,437.80	11.36	0.30	0.50
54,438.58	10.46	0.20	0.47
54,438.65	10.05	0.16	0.42
54,439.85	11.55	0.32	0.49
54,439.92	12.96	0.61	0.49
54,441.12	10.28	0.18	0.40
54,441.54	11.81	0.36	0.45
54,441.61	10.86	0.24	0.46
54,441.82	9.37	0.12	0.46
54,442.04	10.84	0.23	0.38
54,442.18	10.28	0.18	0.38
54,442.67	11.42	0.30	0.48
54,442.74	9.50	0.13	0.44
54,442.88	12.91	0.60	0.33
54,443.09	10.21	0.18	0.37
54,443.66	10.35	0.19	0.48
54,443.87	9.69	0.14	0.37
54,444.08	9.98	0.16	0.35
54,444.36	10.13	0.17	0.43
54,444.58	10.44	0.19	0.34
54,444.72	9.67	0.14	0.35
54,444.86	10.52	0.20	0.45
54,445.07	11.79	0.36	0.44
54,445.14	10.24	0.18	0.41
54,445.21	10.78	0.23	0.35
54,445.92	9.39	0.12	0.34
54,446.41	10.21	0.18	0.42
54,446.62	9.49	0.13	0.42
54,446.98	10.21	0.18	0.47
54,447.05	10.10	0.17	0.39
54,447.19	9.53	0.13	0.45
54,447.26	9.74	0.14	0.45
54,447.33	9.31	0.12	0.41
54,447.54	9.01	0.10	0.40
54,447.68	9.13	0.11	0.40

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3.2. V5583 Sagittarii

Nova V5583 Sgr ($\alpha ={18}^{{\rm{h}}}{07}^{{\rm{m}}}07\buildrel{\rm{s}}\over{.} 67,\ \delta =-33^\circ 46^{\prime} 33\buildrel{\prime\prime}\over{.} 9$; J2000) was observed by both SMEI and the Solar TErrestrial RElations Observatory (STEREO) Heliospheric Imager (Eyles et al. 2009). A review of STEREO observations for this object can be found in Holdsworth et al. (2014).

Table 6.  SMEI Light-curve Data for Nova V597 Pup Continued

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,447.75	9.06	0.10	0.40
54,447.82	9.72	0.14	0.39
54,448.04	9.43	0.12	0.35
54,448.11	9.71	0.14	0.42
54,448.25	8.95	0.10	0.49
54,448.46	9.43	0.12	0.39
54,449.02	9.21	0.11	0.39
54,449.52	9.44	0.12	0.37
54,449.59	9.79	0.14	0.41
54,449.66	9.45	0.12	0.40
54,449.87	9.38	0.12	0.40
54,450.01	9.88	0.15	0.39
54,450.15	9.73	0.14	0.49
54,450.36	9.48	0.13	0.42
54,450.50	10.29	0.18	0.45
54,450.57	10.01	0.16	0.44
54,450.64	11.04	0.26	0.42
54,450.86	10.09	0.17	0.54

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V5583 Sgr is a very fast CN that was discovered by Nishiyama et al. (2009) at a magnitude of 7.7 on 2009 August 6.49 UT (MJD 55,049.49); it then rose to maximum on 2009 August 7.57 UT (MJD 55,050.57) at m_V = 7.43. An approximate ${t}_{{\rm{2}}}$ time of 5 days is given by Schwarz et al. (2011).

Table 7.  SMEI Light-curve Data for Nova V459 Vul

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,431.27	9.79	0.15	0.45
54,431.91	9.02	0.11	0.41
54,449.05	8.18	0.07	0.41
54,459.85	7.06	0.04	0.49
54,459.99	6.86	0.04	0.48
54,461.54	6.88	0.04	0.47
54,461.61	6.85	0.04	0.47
54,461.68	6.79	0.04	0.52
54,461.89	6.65	0.04	0.56
54,461.96	6.65	0.04	0.56
54,462.11	6.59	0.04	0.58
54,462.32	6.86	0.04	0.49
54,462.39	6.88	0.04	0.49
54,462.46	7.52	0.05	0.44
54,462.53	6.93	0.04	0.53
54,462.67	7.11	0.04	0.43
54,462.74	7.00	0.04	0.43
54,462.88	6.89	0.04	0.48
54,462.95	6.99	0.04	0.46
54,463.02	6.88	0.04	0.53
54,463.16	6.96	0.04	0.48
54,463.23	6.87	0.04	0.52
54,463.45	6.84	0.04	0.50
54,463.52	6.82	0.04	0.51
54,463.73	6.82	0.04	0.57
54,463.94	6.94	0.04	0.50
54,464.08	6.95	0.04	0.50
54,464.29	7.05	0.04	0.50
54,464.43	7.07	0.04	0.54
54,464.50	7.11	0.04	0.52
54,464.57	7.19	0.05	0.51
54,464.64	7.13	0.04	0.49
54,464.79	7.18	0.05	0.51
54,464.93	7.46	0.05	0.47
54,465.21	7.15	0.05	0.45
54,465.28	7.14	0.04	0.47
54,465.35	7.14	0.04	0.50
54,466.20	7.12	0.04	0.47
54,466.34	7.06	0.04	0.52
54,466.41	7.15	0.05	0.48
54,466.55	7.09	0.04	0.44
54,466.90	7.10	0.04	0.49
54,466.97	7.14	0.05	0.54
54,467.40	7.36	0.05	0.46
54,467.54	7.25	0.05	0.50
54,470.79	7.27	0.05	0.48
54,477.70	8.20	0.07	0.52

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The nova was detected by SMEI on 2009 August 1.16 UT (MJD 55,044.16) at ${m}_{\mathrm{SMEI}}=8.60\pm 0.10$. There is then a gap in the data due to a combination of low r and npsf values lasting until August 5.67 UT (MJD 5,548.67), after which it then rises (Figure 3) to a peak magnitude of ${m}_{\mathrm{SMEI}}\;=6.94\pm 0.05$ on 2009 August 7.08 ± 0.04 UT (MJD 55,050.08). The timing of this peak coincided nicely with that presented in Holdsworth et al. (2014; the STEREO peak is given as ${m}_{{\rm{H}}{\rm{I}}}$ = 7.18 ± 0.06 on 2009 August 7.04 ± 0.17 UT, MJD 55,050.04); however, the timing of both the SMEI and STEREO peaks is earlier than that given by Nishiyama et al. (2009), suggesting that the maximum was previously missed.

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Table 8.  SMEI Light-curve Data for Nova V2491 Cyg

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,566.61	7.46	0.05	0.43
54,566.68	7.46	0.05	0.45
54,566.75	7.42	0.05	0.45
54,566.82	7.37	0.05	0.44
54,566.89	7.36	0.05	0.41
54,566.96	7.54	0.05	0.46
54,567.03	7.56	0.05	0.45
54,567.10	7.89	0.06	0.42
54,567.17	7.90	0.06	0.40
54,567.24	7.63	0.05	0.49
54,567.59	8.64	0.09	0.44
54,567.66	10.67	0.22	0.31
54,567.88	12.85	0.58	0.40

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Table 9.  SMEI Light-curve Data for Nova QYMus

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,705.26	7.89	0.06	0.97
54,705.40	7.89	0.06	0.97
54,705.47	7.56	0.05	0.97
54,705.54	7.87	0.06	0.97
54,705.61	8.33	0.08	0.97
54,705.68	7.75	0.06	0.97
54,708.01	7.83	0.06	0.96
54,708.36	7.95	0.07	0.97
54,708.79	7.86	0.06	0.94
54,709.63	8.77	0.09	0.96
54,710.05	8.12	0.07	0.97
54,710.20	7.81	0.06	0.97
54,710.27	7.66	0.06	0.97
54,710.62	8.29	0.08	0.97
54,713.09	8.05	0.07	0.97
54,713.16	7.92	0.06	0.97
54,713.44	7.92	0.06	0.97
54,713.51	8.02	0.07	0.97
54,713.58	8.18	0.07	0.97
54,713.65	7.82	0.06	0.97
54,713.72	7.93	0.06	0.97
54,714.36	7.93	0.06	0.98
54,714.43	7.67	0.06	0.97
54,714.50	7.58	0.06	0.97
54,714.57	7.36	0.05	0.97
54,714.64	7.57	0.05	0.97
54,714.71	7.84	0.06	0.97
54,715.06	7.32	0.05	0.97
54,715.20	7.32	0.05	0.97
54,715.27	7.61	0.06	0.97
54,715.34	7.27	0.05	0.97
54,715.41	7.59	0.06	0.97
54,715.48	7.27	0.05	0.97
54,715.55	7.48	0.05	0.97
54,715.62	7.35	0.05	0.97
54,715.70	7.43	0.05	0.97
54,715.77	7.50	0.05	0.96
54,716.05	7.43	0.05	0.97
54,716.12	7.87	0.06	0.97
54,716.19	7.77	0.06	0.97
54,716.26	8.18	0.07	0.97
54,716.33	7.81	0.06	0.97
54,716.40	7.74	0.06	0.97
54,716.47	7.83	0.06	0.97
54,716.54	7.46	0.05	0.97
54,716.61	7.98	0.07	0.97
54,716.68	7.70	0.06	0.97
54,716.75	7.81	0.06	0.97
54,717.04	7.43	0.05	0.97
54,717.11	7.37	0.05	0.97
54,717.18	7.28	0.05	0.97
54,717.25	7.48	0.05	0.97
54,717.32	7.28	0.05	0.97
54,717.39	7.61	0.06	0.98
54,717.46	7.51	0.05	0.97
54,717.53	7.39	0.05	0.97
54,717.60	7.29	0.05	0.97
54,717.74	7.55	0.05	0.96
54,718.02	7.96	0.07	0.97
54,718.16	7.63	0.06	0.97
54,718.23	7.62	0.06	0.97
54,718.38	7.45	0.05	0.97
54,718.45	7.66	0.06	0.97
54,718.52	7.50	0.05	0.97
54,718.59	7.46	0.05	0.97
54,718.73	7.55	0.05	0.97
54,719.22	8.26	0.08	0.97
54,719.29	7.81	0.06	0.97
54,719.36	8.05	0.07	0.97
54,719.43	7.86	0.06	0.97
54,719.50	8.05	0.07	0.97
54,719.58	7.72	0.06	0.98
54,719.65	7.94	0.06	0.97
54,720.07	8.36	0.08	0.97
54,720.14	8.04	0.07	0.97
54,720.21	7.84	0.06	0.97
54,720.28	8.16	0.07	0.97
54,720.42	8.26	0.08	0.97
54,720.49	8.12	0.07	0.97
54,720.56	7.77	0.06	0.97
54,720.63	8.32	0.08	0.97
54,720.70	8.17	0.07	0.97
54,720.78	7.51	0.05	0.95
54,720.99	7.65	0.06	0.96
54,721.06	7.80	0.06	0.97
54,721.13	8.05	0.07	0.97
54,721.20	7.63	0.06	0.97
54,721.27	7.51	0.05	0.97
54,721.34	7.89	0.06	0.97
54,721.41	8.20	0.07	0.97
54,721.48	7.83	0.06	0.97
54,721.62	8.15	0.07	0.97
54,721.69	8.40	0.08	0.97
54,721.76	8.54	0.09	0.95
54,722.05	8.24	0.07	0.97
54,722.12	8.60	0.09	0.97
54,722.19	8.20	0.07	0.97
54,722.33	8.80	0.10	0.97
54,722.40	8.43	0.08	0.97
54,722.47	8.06	0.07	0.97
54,722.54	8.09	0.07	0.97
54,722.61	7.89	0.06	0.97
54,722.68	8.97	0.10	0.97
54,722.75	8.28	0.08	0.97
54,723.03	8.03	0.07	0.97
54,723.10	8.14	0.07	0.97
54,723.18	8.49	0.08	0.97
54,723.32	8.17	0.07	0.97
54,723.39	9.98	0.16	0.97
54,723.53	7.87	0.06	0.97
54,723.60	7.90	0.06	0.97
54,723.67	8.29	0.08	0.97
54,723.74	8.33	0.08	0.96
54,724.16	7.47	0.05	0.97
54,724.23	7.56	0.05	0.97
54,724.30	7.63	0.06	0.97
54,724.45	7.92	0.06	0.97
54,724.52	7.63	0.06	0.97
54,724.59	7.90	0.06	0.97
54,725.08	7.99	0.07	0.97
54,725.22	7.97	0.07	0.97
54,725.29	7.76	0.06	0.97
54,725.50	8.54	0.09	0.97
54,727.76	7.28	0.05	0.97
54,728.39	7.88	0.06	0.97
54,729.03	7.58	0.06	0.97
54,729.24	7.79	0.06	0.97
54,731.07	7.20	0.05	0.97
54,731.36	7.58	0.06	0.97
54,733.61	8.03	0.07	0.97
54,735.09	7.59	0.06	0.97
54,737.21	7.26	0.05	0.97
54,737.63	6.93	0.04	0.97
54,738.06	6.94	0.04	0.97
54,738.13	7.00	0.04	0.97
54,738.20	7.09	0.04	0.97

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A PMH may be present in the SMEI data around 2009 August 5.98 UT (MJD 55,048.98) at an average ${m}_{\mathrm{SMEI}}=7.64\quad$± 0.03 (defined as the mean magnitude over the duration of the halt; quoted error is the rms scatter). Unfortunately, the feature is derived from data with a much lower r than optimal (r values are 0.23, 0.26, and 0.26, respectively) and is therefore unreliable. However, it should be noted that Holdsworth et al. (2014) also find evidence of PMHs around this time. Holdsworth et al. (2014) define a PMH as a decrease in the brightness during the rise phase of the nova eruption and detect three possible events, the first on MJD 55,048.88 ± 0.08 at ${m}_{{\rm{H}}{\rm{I}}}$ = 8.38 ± 0.09, the second on MJD 55,049.13 ± 0.08 at ${m}_{{\rm{H}}{\rm{I}}}$ = 8.05 ± 0.10 (which, when taking into consideration timing definitions, coincides with the SMEI PMH), and the third on MJD 55,049.29 ± 0.08 at ${m}_{{\rm{H}}{\rm{I}}}$ = 7.89 ± 0.08 (see Figure 4). This third halt is also seen in the SMEI light curve at an average ${m}_{\mathrm{SMEI}}=7.18$. However, it is only ∼0.25 mag below maximum and is not within the range that has generally been proposed for a PMH.

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Table 10.  SMEI Light-curve Data for Nova QYMus Continued

Date-Obs MJD	SMEI Mag	SMEI Error	r
54,738.34	6.95	0.04	0.97
54,738.55	7.16	0.05	0.97
54,739.54	7.13	0.04	0.97
54,739.68	7.29	0.05	0.97
54,743.63	8.24	0.07	0.97
54,745.11	8.52	0.08	0.97
54,745.39	7.96	0.07	0.95
54,745.54	8.18	0.07	0.97
54,746.38	8.50	0.08	0.97
54,747.23	8.65	0.09	0.97
54,748.14	8.28	0.08	0.97
54,748.50	9.03	0.11	0.97
54,748.64	10.54	0.21	0.97
54,748.78	8.27	0.08	0.97
54,749.48	8.19	0.07	0.97
54,749.70	9.04	0.11	0.96
54,750.05	8.02	0.07	0.97
54,750.26	9.45	0.13	0.97
54,750.68	8.20	0.07	0.96
54,751.04	8.25	0.07	0.97
54,751.11	9.76	0.15	0.97
54,751.25	8.20	0.07	0.97
54,751.32	7.69	0.06	0.97
54,751.39	10.00	0.17	0.97
54,751.74	8.24	0.07	0.97
54,751.81	7.95	0.07	0.96
54,752.02	7.72	0.06	0.97
54,752.30	9.00	0.11	0.97
54,752.66	8.65	0.09	0.96
54,752.73	9.57	0.14	0.97
54,753.01	8.51	0.08	0.97
54,753.08	9.11	0.11	0.97
54,753.15	8.24	0.07	0.97
54,753.22	8.03	0.07	0.97
54,753.29	8.59	0.09	0.97
54,753.36	9.41	0.13	0.97
54,753.58	8.68	0.09	0.97
54,754.56	8.84	0.10	0.97
54,754.63	8.59	0.09	0.97
54,754.85	7.48	0.05	0.92
54,755.13	9.01	0.11	0.97
54,755.34	9.61	0.14	0.97
54,755.48	11.97	0.41	0.97
54,755.69	8.93	0.10	0.96
54,755.76	8.78	0.10	0.96
54,756.40	10.11	0.17	0.96
54,756.54	9.01	0.11	0.96
54,756.61	8.74	0.09	0.96
54,756.68	12.22	0.46	0.96
54,756.75	8.60	0.09	0.97
54,757.03	8.60	0.09	0.97
54,757.17	8.35	0.08	0.97
54,757.32	9.82	0.15	0.96
54,757.39	8.96	0.10	0.96
54,760.84	11.27	0.30	0.95
54,761.27	8.50	0.08	0.97
54,761.34	8.13	0.07	0.97
54,761.41	9.00	0.11	0.97
54,761.48	8.81	0.10	0.97
54,761.55	9.64	0.14	0.97
54,761.62	9.11	0.11	0.97
54,761.76	9.11	0.11	0.97
54,761.83	11.87	0.39	0.96
54,762.04	11.77	0.37	0.97
54,762.18	9.29	0.12	0.97
54,762.25	9.08	0.11	0.97
54,762.32	11.02	0.26	0.97
54,762.54	8.60	0.09	0.97
54,762.75	9.76	0.15	0.96
54,762.82	9.31	0.12	0.97
54,763.03	9.77	0.15	0.97
54,763.59	9.16	0.11	0.97
54,763.66	9.68	0.14	0.97
54,763.73	9.20	0.12	0.97
54,764.09	7.64	0.06	0.97
54,764.16	8.36	0.08	0.97
54,764.30	8.60	0.09	0.97
54,764.65	10.05	0.17	0.97
54,771.70	9.59	0.14	0.96
54,772.06	8.38	0.08	0.96
54,772.41	8.43	0.08	0.97
54,772.48	11.49	0.33	0.97
54,772.62	9.13	0.11	0.97
54,772.76	9.08	0.11	0.96
54,772.83	8.36	0.08	0.96
54,772.90	10.83	0.24	0.94
54,773.05	8.04	0.07	0.96
54,773.12	9.00	0.11	0.96
54,773.19	8.15	0.07	0.97
54,773.26	9.58	0.14	0.97
54,773.33	8.68	0.09	0.96
54,773.40	8.10	0.07	0.96
54,773.47	8.18	0.07	0.96
54,773.54	7.86	0.06	0.96
54,773.61	8.03	0.07	0.96
54,773.68	9.28	0.12	0.96
54,773.75	8.22	0.07	0.96
54,773.82	10.59	0.22	0.96
54,773.89	8.35	0.08	0.92
54,774.03	8.25	0.07	0.96
54,774.10	8.54	0.09	0.96
54,774.18	8.00	0.07	0.96
54,774.25	9.53	0.13	0.96
54,774.32	7.91	0.06	0.96
54,774.39	8.31	0.08	0.96
54,774.46	8.35	0.08	0.97
54,774.53	9.67	0.14	0.97
54,774.88	11.53	0.33	0.95
54,774.95	9.23	0.12	0.92

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Approximately 1 day after maximum, the object then seems to enter a "plateau" phase that lasts for 1.6 days with an average ${m}_{\mathrm{SMEI}}=7.56$, after which it declines. Again it should be noted that these data have a correlation coefficient much less than optimal (0.1 ≤ r < 0.3) and are less reliable. The discrepancy between the SMEI and STEREO light curves especially at late times is clearly evident and due to the reduced quality of the SMEI data (r < 0.3) throughout the nova eruption. Therefore, the r < 0.3 SMEI data are less reliable and complementary to the STEREO data when obtained simultaneously.

Table 11.  SMEI Light-curve Data for Nova V5583 Sgr

Date-Obs MJD	SMEI Mag	SMEI Error	r
55,044.16	8.60	0.10	0.23
55,044.23	8.29	0.08	0.19
55,044.37	8.21	0.08	0.21
55,044.44	8.65	0.10	0.23
55,044.58	9.88	0.17	0.20
55,048.67	8.01	0.07	0.24
55,048.74	7.83	0.07	0.24
55,048.81	7.77	0.07	0.21
55,048.88	7.64	0.06	0.23
55,048.96	7.60	0.06	0.26
55,049.10	7.69	0.06	0.26
55,049.24	7.48	0.06	0.29
55,049.31	7.67	0.06	0.33
55,049.38	7.32	0.05	0.31
55,049.45	7.28	0.05	0.31
55,049.66	7.20	0.05	0.36
55,049.73	7.18	0.05	0.37
55,049.87	7.17	0.05	0.38
55,049.94	7.04	0.05	0.39
55,050.01	7.08	0.05	0.38
55,050.08	6.94	0.05	0.44
55,050.16	7.03	0.05	0.40
55,050.23	6.98	0.05	0.42
55,050.44	7.13	0.05	0.39
55,050.72	7.28	0.05	0.34
55,050.79	7.34	0.05	0.32
55,051.00	7.37	0.06	0.31
55,051.14	7.57	0.06	0.27
55,051.21	7.55	0.06	0.28
55,051.29	7.65	0.06	0.24
55,051.36	7.58	0.06	0.27
55,051.43	7.57	0.06	0.28
55,051.50	7.54	0.06	0.27
55,051.57	7.62	0.06	0.26
55,051.64	7.58	0.06	0.26
55,051.71	7.61	0.06	0.26
55,051.78	7.53	0.06	0.24
55,051.85	7.58	0.06	0.23
55,051.92	7.63	0.06	0.25
55,051.99	7.55	0.06	0.25
55,052.06	7.56	0.06	0.24
55,052.13	7.62	0.06	0.24
55,052.20	7.62	0.06	0.23
55,052.27	7.44	0.06	0.26
55,052.34	7.53	0.06	0.25
55,052.41	7.56	0.06	0.25
55,052.48	7.56	0.06	0.27
55,052.55	7.48	0.06	0.28
55,052.70	7.50	0.06	0.29
55,052.77	7.50	0.06	0.30
55,053.26	7.91	0.07	0.29
55,053.33	7.84	0.07	0.28
55,053.40	7.93	0.07	0.27
55,053.47	7.98	0.07	0.25
55,053.54	7.91	0.07	0.25
55,053.61	7.91	0.07	0.24
55,053.68	8.00	0.07	0.21
55,053.75	8.11	0.08	0.20
55,053.82	7.90	0.07	0.19
55,053.89	8.12	0.08	0.17
55,053.96	8.29	0.08	0.14
55,054.04	8.09	0.08	0.16
55,054.11	7.92	0.07	0.18
55,054.18	8.34	0.09	0.15
55,054.25	8.19	0.08	0.16
55,054.32	8.05	0.08	0.19
55,054.39	7.88	0.07	0.22
55,054.53	7.85	0.07	0.24
55,054.60	8.34	0.09	0.24
55,054.67	8.21	0.08	0.26

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Table 12.  SMEI Light-curve Data for Nova RS Oph

Date-Obs MJD	SMEI Mag	SMEI Error
53,775.77	7.79	0.06
53,775.84	7.42	0.05
53,776.26	7.07	0.04
53,778.03	6.18	0.03
53,778.10	5.66	0.02
53,778.17	5.30	0.02
53,778.24	4.93	0.02
53,778.31	4.59	0.01
53,778.38	4.44	0.01
53,778.45	4.46	0.01
53,778.52	4.36	0.01
53,778.59	4.20	0.01
53,778.66	4.09	0.01
53,778.73	3.97	0.01
53,778.80	3.93	0.01
53,778.87	3.93	0.01
53,778.94	3.87	0.01
53,779.01	3.93	0.01
53,779.09	3.98	0.01
53,779.16	4.03	0.01
53,779.23	4.12	0.01
53,779.30	4.16	0.01
53,779.37	4.23	0.01
53,779.44	4.26	0.01
53,779.51	4.29	0.01
53,779.58	4.39	0.01
53,779.65	4.38	0.01
53,779.72	4.46	0.01
53,779.79	4.47	0.01
53,779.86	4.51	0.01
53,779.93	4.56	0.01
53,780.00	4.59	0.01
53,780.07	4.59	0.01
53,780.14	4.59	0.01
53,780.21	4.63	0.01
53,780.28	4.63	0.01
53,780.36	4.62	0.01
53,780.43	4.67	0.01
53,780.50	4.67	0.01
53,780.57	4.66	0.01
53,780.64	4.73	0.01
53,780.71	4.72	0.01
53,780.78	4.73	0.01
53,780.85	4.71	0.01
53,780.92	4.73	0.01
53,781.27	4.91	0.02
53,781.34	4.88	0.02
53,781.41	4.85	0.02
53,781.48	4.90	0.02
53,781.55	4.96	0.02
53,781.63	4.99	0.02
53,781.70	4.95	0.02
53,781.77	5.00	0.02
53,781.84	5.00	0.02
53,781.91	4.93	0.02
53,781.98	5.02	0.02
53,782.05	5.00	0.02
53,782.12	5.11	0.02
53,782.19	5.06	0.02
53,782.26	5.13	0.02
53,782.75	5.19	0.02
53,782.82	5.26	0.02
53,782.90	5.25	0.02
53,782.97	5.30	0.02
53,783.04	5.29	0.02
53,783.11	5.30	0.02
53,783.18	5.33	0.02
53,783.25	5.32	0.02
53,783.32	5.36	0.02
53,783.39	5.27	0.02
53,783.53	5.34	0.02
53,783.60	5.33	0.02
53,783.67	5.35	0.02
53,783.74	5.38	0.02
53,783.81	5.36	0.02
53,783.88	5.38	0.02
53,783.95	5.38	0.02
53,784.02	5.37	0.02
53,784.10	5.47	0.02
53,784.17	5.47	0.02
53,784.24	5.38	0.02
53,784.31	5.56	0.02
53,784.38	5.45	0.02
53,784.45	5.46	0.02
53,784.52	5.48	0.02
53,784.59	5.51	0.02
53,784.66	5.53	0.02
53,784.73	5.53	0.02
53,784.80	5.59	0.02
53,784.87	5.60	0.02
53,784.94	5.67	0.02
53,785.01	5.60	0.02
53,785.08	5.71	0.02
53,785.15	5.65	0.02
53,785.22	5.72	0.02
53,785.29	5.72	0.02
53,785.37	5.66	0.02
53,785.44	5.66	0.02
53,785.51	5.67	0.02
53,785.58	5.72	0.02
53,785.65	5.72	0.02
53,785.72	5.63	0.02
53,785.79	5.64	0.02
53,785.86	5.59	0.02
53,785.93	5.63	0.02
53,786.00	5.73	0.02
53,786.07	5.75	0.02
53,786.14	5.75	0.02
53,786.21	5.77	0.02
53,786.28	5.77	0.02
53,786.35	5.75	0.02
53,786.42	5.74	0.02
53,786.49	5.79	0.02
53,786.56	5.78	0.02
53,786.78	5.77	0.02
53,786.85	5.83	0.02
53,786.92	5.80	0.02
53,786.99	5.84	0.02
53,787.06	5.80	0.02
53,787.20	5.82	0.02
53,787.27	5.88	0.03
53,787.34	5.93	0.03
53,787.41	5.91	0.03
53,787.48	5.98	0.03
53,787.55	5.89	0.03
53,787.69	6.00	0.03
53,787.76	6.09	0.03
53,787.83	5.95	0.03
53,787.91	6.08	0.03
53,787.98	6.00	0.03
53,790.16	6.24	0.03
53,790.37	6.11	0.03
53,790.45	6.21	0.03
53,794.47	6.23	0.03
53,794.68	6.05	0.03
53,794.75	6.10	0.03
53,794.82	6.46	0.03
53,794.89	6.48	0.03
53,794.96	6.15	0.03

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3.3. V1187 Scorpii

Nova V1187 Sco ($\alpha ={17}^{{\rm{h}}}{29}^{{\rm{m}}}18\buildrel{\rm{s}}\over{.} 81,\ \delta =-31^\circ 46^{\prime} 01\buildrel{\prime\prime}\over{.} 5$; J2000) was discovered prior to peak at ${m}_{V}$ = 9.9 on 2004 August 2.07 UT (MJD 53,219.07) using data from the All Sky Automated Survey (ASAS)-3 patrol (Pojmanski et al. 2005). It subsequently rose to a maximum magnitude of ${m}_{V}$ = 7.42 on 2004 August 3.58 UT (MJD 53,220.58; Yamaoka 2004; this is the peak of the V-band AAVSO light curve given in Figure 5). The initial decline gave ${t}_{2}$ = 8.7 and ${t}_{3}$ = 15 days (Lynch et al. 2006), classifying V1187 Sco as a very fast nova. Near-IR spectroscopic observations of the object by Lynch et al. (2006) indicated the development of a nova explosion on an O Ne WD, which did not form dust before entering its nebular phase. The emission lines found within the spectra had complex, double-peaked profiles. Using the H i double emission lines, the nova ejecta were modeled as a ring or partial sphere-like emitting region. An extinction of ${A}_{V}$ = 4.68 ± 0.24 was derived also using O i lines in combination with the optical spectra.

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Table 13.  SMEI Light-curve Data for Nova V1280 Sco

Date-Obs MJD	SMEI Mag	SMEI Error
54,144.61	6.19	0.03
54,144.68	6.18	0.03
54,144.75	6.20	0.03
54,144.82	6.19	0.03
54,144.89	6.16	0.03
54,144.96	6.16	0.03
54,145.24	6.14	0.03
54,145.31	6.20	0.03
54,145.38	6.10	0.03
54,145.52	6.02	0.03
54,145.59	5.89	0.02
54,145.66	5.81	0.02
54,145.73	5.70	0.02
54,145.80	5.59	0.02
54,145.88	5.48	0.02
54,145.95	5.37	0.02
54,146.02	5.30	0.02
54,146.09	5.27	0.02
54,146.23	5.23	0.02
54,146.30	5.24	0.02
54,146.37	5.23	0.02
54,146.44	5.22	0.02
54,146.51	5.24	0.02
54,146.58	5.22	0.02
54,146.65	5.23	0.02
54,146.72	5.14	0.02
54,146.79	4.75	0.01
54,146.86	4.37	0.01
54,146.93	4.12	0.01
54,147.00	4.05	0.01
54,147.07	4.00	0.01
54,147.15	4.00	0.01
54,147.22	4.02	0.01
54,147.29	4.04	0.01
54,147.36	4.14	0.01
54,147.43	4.13	0.01
54,147.50	4.19	0.01
54,147.57	4.25	0.01
54,147.64	4.41	0.01
54,147.71	4.54	0.01
54,147.78	4.68	0.01
54,147.85	4.79	0.01
54,147.92	4.85	0.02
54,148.06	4.85	0.02
54,148.13	4.73	0.01
54,148.27	4.35	0.01
54,148.34	4.23	0.01
54,148.41	4.24	0.01
54,148.49	4.25	0.01
54,148.56	4.29	0.01
54,148.63	4.33	0.01
54,148.70	4.41	0.01
54,148.77	4.49	0.01
54,148.84	4.56	0.01
54,148.91	4.64	0.01
54,148.98	4.68	0.01
54,149.05	4.71	0.01
54,149.12	4.71	0.01
54,149.19	4.74	0.01
54,149.26	4.76	0.01
54,149.33	4.79	0.01
54,149.40	4.81	0.01
54,149.47	4.80	0.01
54,149.54	4.77	0.01
54,149.61	4.74	0.01
54,149.68	4.70	0.01
54,149.76	4.64	0.01
54,149.83	4.56	0.01
54,149.90	4.46	0.01
54,149.97	4.34	0.01
54,150.04	4.25	0.01
54,150.11	4.16	0.01
54,150.18	4.13	0.01
54,150.25	4.13	0.01
54,150.32	4.15	0.01
54,150.39	4.22	0.01
54,150.53	4.44	0.01
54,150.60	4.57	0.01
54,150.67	4.74	0.01
54,150.74	4.92	0.02
54,150.81	4.94	0.02
54,150.88	4.89	0.02
54,150.95	4.85	0.02
54,151.03	4.81	0.01
54,151.10	4.81	0.01
54,151.17	4.86	0.02
54,151.24	4.85	0.02
54,151.31	4.86	0.02
54,151.38	4.80	0.01
54,151.45	4.73	0.01
54,151.52	4.68	0.01
54,151.59	4.67	0.01
54,151.66	4.68	0.01
54,151.73	4.71	0.01
54,151.80	4.71	0.01
54,151.87	4.71	0.01
54,151.94	4.69	0.01
54,152.22	4.78	0.01
54,152.30	4.75	0.01
54,152.37	4.77	0.01
54,152.44	4.77	0.01
54,152.51	4.73	0.01
54,152.58	4.65	0.01
54,152.65	4.70	0.01
54,152.72	4.75	0.01
54,152.79	4.80	0.01
54,152.86	4.87	0.02
54,152.93	4.89	0.02
54,153.00	4.92	0.02
54,153.07	4.90	0.02
54,153.14	4.85	0.02
54,153.21	4.77	0.01
54,153.28	4.77	0.01
54,153.35	4.77	0.01
54,153.42	4.80	0.01
54,153.49	4.83	0.02
54,153.56	4.84	0.02
54,153.64	4.86	0.02
54,153.71	4.85	0.02
54,153.78	4.86	0.02
54,153.85	4.88	0.02
54,153.92	4.87	0.02
54,154.06	4.84	0.02
54,154.13	4.84	0.02
54,154.20	4.83	0.02
54,154.27	4.83	0.02
54,154.34	4.87	0.02
54,154.41	4.88	0.02
54,154.48	4.86	0.02
54,154.55	4.87	0.02
54,154.62	4.86	0.02
54,154.69	4.87	0.02
54,154.76	4.89	0.02
54,154.83	4.93	0.02
54,154.91	4.98	0.02
54,154.98	4.97	0.02
54,155.05	4.98	0.02
54,155.12	5.00	0.02
54,155.19	4.98	0.02
54,155.26	4.96	0.02
54,155.33	4.97	0.02
54,155.40	4.98	0.02
54,155.47	5.02	0.02
54,155.54	5.04	0.02
54,155.61	5.06	0.02
54,155.68	5.08	0.02
54,155.75	5.10	0.02
54,155.82	5.09	0.02
54,155.89	5.05	0.02
54,155.96	5.07	0.02
54,156.03	5.03	0.02
54,156.10	5.03	0.02
54,156.18	5.04	0.02
54,156.25	5.03	0.02
54,156.32	5.03	0.02
54,156.74	5.04	0.02
54,156.81	5.03	0.02
54,157.16	5.04	0.02
54,157.23	5.06	0.02
54,157.30	5.11	0.02
54,157.37	5.14	0.02
54,157.45	5.15	0.02
54,157.52	5.15	0.02
54,157.59	5.16	0.02
54,157.66	5.20	0.02
54,157.73	5.22	0.02
54,157.80	5.25	0.02
54,157.87	5.25	0.02
54,157.94	5.29	0.02
54,158.01	5.30	0.02
54,158.08	5.32	0.02
54,158.15	5.35	0.02
54,158.22	5.40	0.02
54,158.29	5.42	0.02
54,158.36	5.44	0.02
54,158.43	5.48	0.02
54,158.50	5.49	0.02
54,158.57	5.53	0.02
54,158.64	5.51	0.02
54,158.72	5.53	0.02
54,158.79	5.57	0.02
54,158.86	5.55	0.02
54,158.93	5.60	0.02
54,159.28	5.63	0.02
54,159.35	5.73	0.02
54,159.42	5.81	0.02
54,159.49	5.87	0.02
54,159.56	5.92	0.02
54,159.63	5.95	0.03
54,159.70	5.94	0.03
54,159.77	5.95	0.03
54,159.84	5.99	0.03
54,159.98	6.00	0.03
54,160.13	6.07	0.03
54,160.27	6.19	0.03
54,160.41	6.17	0.03
54,160.48	6.18	0.03
54,160.55	6.22	0.03
54,160.62	6.23	0.03
54,160.69	6.24	0.03
54,160.76	6.26	0.03

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The SMEI data give the peak brightness of nova V1187 Sco as ${m}_{\mathrm{SMEI}}=6.95\pm 0.04$ on 2004 August ${3.77}_{-0.04}^{+0.07}$ UT (MJD 53,220.77). This is 0.47 mag brighter and 0.19 days later than the V-band peak given in the lower time resolution results of Yamaoka (2004). Within Figure 5, the SMEI light curve is compared to V-band AAVSO data and I-band data from the Nova Atlas within the same time frame.

Table 14.  SMEI Light-curve Data for Nova V1280 Sco Continued

Date-Obs MJD	SMEI Mag	SMEI Error
54,160.83	6.25	0.03
54,160.90	6.27	0.03
54,160.97	6.34	0.03
54,161.04	6.39	0.03
54,161.11	6.42	0.03
54,161.18	6.35	0.03
54,161.40	6.45	0.03
54,161.47	6.49	0.03
54,161.54	6.53	0.03
54,161.61	6.63	0.03
54,161.68	6.66	0.03
54,161.75	6.61	0.03
54,161.82	6.69	0.04
54,161.89	6.79	0.04
54,161.96	6.95	0.04
54,162.03	6.96	0.04
54,162.10	7.03	0.04
54,162.17	7.10	0.04
54,162.24	7.12	0.04
54,162.31	7.20	0.04
54,162.38	7.14	0.04
54,162.45	7.20	0.04
54,162.52	7.30	0.05
54,162.60	7.32	0.05
54,162.67	7.42	0.05
54,162.74	7.55	0.05
54,162.81	7.55	0.05
54,162.88	7.55	0.05
54,162.95	7.57	0.05
54,163.02	7.80	0.06
54,163.09	7.60	0.05
54,163.16	7.69	0.06
54,163.23	7.79	0.06
54,163.30	7.61	0.05
54,163.37	8.21	0.07
54,163.44	8.19	0.07
54,163.51	8.04	0.06
54,163.58	8.29	0.07
54,163.65	8.10	0.07
54,163.72	8.22	0.07
54,163.79	8.31	0.07
54,163.87	8.69	0.09
54,163.94	9.08	0.10
54,164.01	8.86	0.09
54,164.08	9.78	0.14
54,164.15	9.41	0.12
54,164.22	10.02	0.16
54,164.29	9.72	0.14
54,164.36	11.18	0.27
54,164.43	10.21	0.17
54,164.71	10.70	0.22

Download table as:  ASCIITypeset images: 1 2

Table 15.  SMEI Light-curve Data for Nova V598 Pup

Date-Obs MJD	SMEI Mag	SMEI Error
54,248.82	9.60	0.14
54,254.47	7.54	0.05
54,254.61	6.36	0.03
54,254.68	6.06	0.03
54,254.75	5.88	0.03
54,254.82	5.57	0.02
54,254.96	4.94	0.02
54,255.03	5.08	0.02
54,255.10	5.24	0.02
54,255.17	5.13	0.02
54,255.24	5.05	0.02
54,255.31	4.77	0.02
54,255.38	4.72	0.01
54,255.45	4.62	0.01
54,255.52	4.49	0.01
54,255.59	4.34	0.01
54,255.67	4.38	0.01
54,255.74	4.29	0.01
54,255.81	4.04	0.01
54,255.88	4.06	0.01
54,255.95	3.90	0.01
54,256.02	3.97	0.01
54,256.09	3.92	0.01
54,256.16	3.87	0.01
54,256.23	3.68	0.01
54,256.30	3.62	0.01
54,256.65	3.49	0.01
54,256.72	3.50	0.01
54,256.79	3.67	0.01
54,256.94	3.48	0.01
54,257.29	3.46	0.01
54,257.36	3.57	0.01
54,257.43	3.48	0.01
54,257.50	3.52	0.01
54,257.57	3.53	0.01
54,257.64	3.57	0.01
54,257.71	3.62	0.01
54,257.78	3.61	0.01
54,257.99	3.81	0.01
54,258.06	3.82	0.01
54,258.13	3.84	0.01
54,258.20	3.84	0.01
54,258.28	3.89	0.01
54,258.35	3.95	0.01
54,258.42	3.99	0.01
54,258.49	4.04	0.01
54,258.56	4.19	0.01
54,258.63	4.08	0.01
54,258.70	4.10	0.01
54,258.77	4.15	0.01
54,258.98	4.27	0.01
54,259.05	4.28	0.01
54,259.12	4.33	0.01
54,259.19	4.34	0.01
54,259.26	4.41	0.01
54,259.33	4.43	0.01
54,279.71	7.04	0.04
54,279.79	7.07	0.04
54,279.86	6.87	0.04
54,280.07	7.10	0.04
54,280.14	7.19	0.05
54,280.21	7.13	0.04
54,280.28	6.98	0.04
54,280.35	7.19	0.05
54,280.42	7.18	0.05
54,280.49	7.32	0.05
54,280.56	7.19	0.05
54,280.63	7.27	0.05
54,280.70	7.31	0.05
54,280.77	7.39	0.05
54,280.84	7.14	0.04
54,281.34	7.23	0.05
54,281.41	7.81	0.06
54,281.48	7.91	0.06
54,281.55	8.20	0.07
54,281.62	7.84	0.06
54,281.69	7.54	0.05
54,281.76	7.88	0.06
54,282.04	9.53	0.13
54,282.18	8.63	0.09
54,282.32	10.65	0.22
54,282.54	9.38	0.12
54,282.68	9.57	0.14
54,282.82	9.28	0.12
54,282.89	11.51	0.33
54,283.38	7.16	0.05
54,283.45	7.19	0.05
54,283.52	8.90	0.10
54,283.59	10.36	0.19
54,283.66	7.03	0.04
54,283.73	7.18	0.05
54,283.80	6.85	0.04
54,286.84	7.40	0.05
54,286.91	7.55	0.05
54,287.05	7.75	0.06
54,287.12	8.43	0.08
54,287.19	7.96	0.07
54,287.26	8.24	0.07
54,287.33	8.02	0.07
54,287.40	8.23	0.07
54,287.47	8.27	0.08
54,287.54	8.02	0.07
54,287.61	9.09	0.11
54,287.68	8.16	0.07
54,287.75	8.21	0.07
54,288.18	7.97	0.07
54,288.25	7.95	0.06
54,288.32	7.64	0.06
54,288.46	7.50	0.05
54,288.53	8.01	0.07
54,288.60	8.94	0.10
54,288.67	8.71	0.09
54,288.74	7.76	0.06
54,288.81	7.72	0.06
54,288.88	7.64	0.06
54,288.95	7.92	0.06
54,289.16	8.46	0.08
54,289.23	8.36	0.08
54,289.31	8.52	0.08
54,289.38	7.90	0.06

Download table as:  ASCIITypeset images: 1 2

A substantial portion of the initial nova rise is missing from the SMEI light curve; however, some data before peak are presented. As the nova is of the very fast classification, one would expect the rise to maximum to also be fast; however, within the SMEI data we are finding the opposite effect. This apparent slow rise is most likely due to contamination of the data from several close bright neighboring stars, despite the conduction of simultaneous fitting and the fitting of additional bright stars in the larger surrounding region. The apparent plateau/dip before the final rise to peak may therefore not be a PMH; instead, it is probably residual light from a neighboring star. Data points between July 29 and 31 (MJD 53,215–53,217) were removed owing to large variations in the R.A. and decl. on fitting, suggesting a fit of residuals rather than the nova. However, the gap seen around the 2nd of August (MJD 53,219) is due to an SMEI anomaly during which the instrument was forced to shut down and restart.¹³ The noisiness of the light curve especially during decline is also likely due to contamination from neighboring bright stars. However, there does appear to be some structured oscillation that may be real.

Table 16.  SMEI Light-curve Data for Nova V598 Pup Continued

Date-Obs MJD	SMEI Mag	SMEI Error
54,289.45	8.44	0.08
54,289.52	8.73	0.09
54,289.66	8.12	0.07
54,289.73	7.96	0.07
54,289.80	7.81	0.06
54,289.87	8.31	0.08
54,289.94	7.99	0.07
54,290.01	7.67	0.06
54,290.08	7.73	0.06
54,290.15	7.76	0.06
54,292.90	8.37	0.08
54,292.97	7.67	0.06
54,293.04	7.73	0.06
54,293.11	7.72	0.06
54,293.18	7.69	0.06
54,293.25	7.83	0.06
54,293.33	7.32	0.05
54,293.40	7.81	0.06
54,293.47	7.77	0.06
54,293.54	7.78	0.06
54,293.61	7.48	0.05
54,293.68	7.53	0.05
54,293.75	7.93	0.06
54,293.82	7.89	0.06
54,293.89	7.55	0.05
54,293.96	8.06	0.07
54,297.06	12.19	0.45
54,297.84	7.82	0.06
54,297.91	7.41	0.05
54,297.98	8.18	0.07
54,298.05	8.76	0.09
54,298.12	7.53	0.05
54,298.19	7.23	0.05
54,298.26	12.24	0.46
54,298.33	7.75	0.06
54,298.40	7.92	0.06
54,298.47	7.97	0.07
54,298.54	7.92	0.06
54,298.62	6.70	0.04
54,298.76	8.19	0.07
54,298.83	7.06	0.04
54,303.20	13.64	0.86
54,306.73	7.77	0.06
54,306.80	9.09	0.11
54,306.87	7.95	0.06
54,306.94	8.17	0.07
54,307.01	8.71	0.09
54,307.15	9.80	0.15
54,307.22	9.41	0.13
54,307.29	9.06	0.11
54,307.36	8.29	0.08
54,307.43	9.76	0.15
54,307.50	8.76	0.09
54,307.57	9.11	0.11
54,307.64	9.55	0.13
54,307.71	10.08	0.17
54,307.78	9.05	0.11
54,308.00	10.45	0.20
54,308.07	8.37	0.08
54,308.14	7.68	0.06
54,308.28	9.97	0.16
54,308.35	7.61	0.06
54,308.42	7.39	0.05
54,308.49	10.21	0.18
54,308.56	7.47	0.05
54,308.63	9.67	0.14
54,308.70	6.45	0.03
54,308.84	8.93	0.10
54,308.92	7.53	0.05
54,308.98	7.94	0.06
54,309.27	8.23	0.07
54,309.34	8.28	0.08
54,309.41	8.00	0.07
54,309.48	7.79	0.06
54,309.55	7.87	0.06
54,309.62	7.84	0.06
54,309.69	10.94	0.25
54,309.76	7.68	0.06
54,309.83	8.33	0.08
54,309.90	8.21	0.07
54,309.97	8.68	0.09
54,310.04	8.58	0.09
54,310.11	8.65	0.09
54,310.18	8.61	0.09
54,310.25	8.31	0.08
54,310.32	9.13	0.11
54,310.39	8.73	0.09
54,310.47	9.05	0.11
54,310.61	9.08	0.11
54,310.68	8.04	0.07
54,310.75	9.22	0.12
54,310.82	11.30	0.30
54,310.89	9.57	0.14
54,310.96	7.92	0.06
54,311.17	8.71	0.09
54,311.31	8.49	0.08
54,311.38	9.26	0.12
54,311.45	7.49	0.05
54,311.52	8.81	0.10
54,311.59	11.19	0.28
54,311.74	14.67	1.38
54,311.81	8.37	0.08
54,311.88	5.97	0.03
54,312.02	8.84	0.10
54,312.09	7.17	0.05
54,312.16	8.24	0.07
54,312.23	6.06	0.03
54,312.30	6.15	0.03
54,312.37	7.36	0.05
54,312.44	6.40	0.03
54,312.51	5.95	0.03
54,312.58	5.97	0.03
54,312.65	5.91	0.03
54,312.72	5.90	0.03
54,312.79	6.40	0.03
54,312.86	6.40	0.03
54,312.93	6.02	0.03
54,313.29	9.20	0.11
54,313.36	6.45	0.03
54,313.43	6.29	0.03
54,313.50	7.06	0.04
54,313.57	7.43	0.05
54,313.78	7.84	0.06
54,313.85	8.40	0.08
54,313.92	7.28	0.05
54,313.99	8.49	0.08
54,314.06	7.90	0.06
54,314.13	8.64	0.09
54,314.20	7.08	0.04
54,314.27	11.04	0.26
54,314.35	8.41	0.08
54,314.42	8.35	0.08
54,314.49	7.53	0.05
54,314.63	7.54	0.05
54,314.70	7.92	0.06
54,314.77	8.38	0.08
54,314.84	7.59	0.06
54,314.91	8.91	0.10
54,314.98	8.69	0.09
54,315.05	7.53	0.05
54,315.12	7.93	0.06
54,315.19	9.62	0.14
54,315.40	15.13	1.71
54,315.54	8.31	0.08
54,315.61	8.73	0.09
54,315.76	10.90	0.25
54,315.83	9.13	0.11
54,315.90	8.61	0.09
54,315.97	9.68	0.14
54,316.04	8.39	0.08
54,316.11	9.14	0.11
54,316.18	8.06	0.07
54,316.25	7.62	0.06
54,316.32	8.47	0.08
54,316.39	8.95	0.10
54,316.53	8.38	0.08
54,316.60	8.39	0.08
54,316.67	8.67	0.09
54,316.74	8.33	0.08
54,316.81	8.64	0.09
54,316.88	8.35	0.08
54,317.10	9.54	0.13
54,317.31	10.29	0.19
54,317.38	10.89	0.25
54,317.45	8.62	0.09
54,317.52	7.82	0.06
54,317.59	9.60	0.14
54,317.66	8.23	0.07
54,317.73	8.28	0.08
54,317.80	7.75	0.06
54,317.87	9.46	0.13
54,317.94	8.10	0.07
54,318.01	7.95	0.06
54,318.08	8.17	0.07
54,318.15	7.26	0.05
54,318.22	11.12	0.27
54,318.30	8.48	0.08
54,318.44	8.41	0.08
54,318.51	13.05	0.66
54,318.58	9.05	0.11
54,318.65	8.41	0.08
54,318.72	8.69	0.09
54,318.79	11.58	0.34
54,318.86	8.96	0.10
54,318.93	7.52	0.05
54,319.00	8.52	0.08
54,319.07	9.98	0.16
54,319.21	8.34	0.08
54,319.35	8.52	0.08
54,319.42	7.46	0.05
54,319.49	8.15	0.07
54,319.57	11.33	0.30
54,319.64	8.42	0.08
54,319.71	7.40	0.05
54,319.78	6.81	0.04
54,319.85	8.53	0.08
54,319.92	8.36	0.08
54,319.99	8.22	0.07
54,320.27	8.90	0.10
54,320.34	8.23	0.07
54,320.41	8.18	0.07
54,320.48	7.79	0.06
54,320.55	8.14	0.07
54,320.62	8.51	0.08
54,320.69	8.67	0.09
54,320.76	8.32	0.08
54,320.84	9.45	0.13
54,320.91	8.72	0.09
54,321.12	8.64	0.09
54,321.19	7.80	0.06

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The SMEI data shown in Figure 5 do not cover the magnitude range required for the determination of a ${t}_{{\rm{2}}}$ time. However, on application of a liner fit to the initial decline of the nova using all data where r is greater than 0.3, a ${t}_{{\rm{2}}}$ of ${10.10}_{-0.39}^{+0.43}$ days was derived (error quoted is statistical only and obtained using the uncertainties of the fitted gradient and intercept). This is slightly larger than the result presented in Lynch et al. (2006), but agrees (within errors) with the very fast nova classification.

Table 17.  SMEI Light-curve Data for Nova V598 Pup Continued

Date-Obs MJD	SMEI Mag	SMEI Error
54,321.26	8.26	0.07
54,321.47	8.56	0.09
54,321.54	8.73	0.09
54,321.61	9.40	0.13
54,321.68	9.08	0.11
54,321.75	9.88	0.16
54,321.82	9.48	0.13
54,321.89	6.84	0.04
54,321.96	9.38	0.12
54,322.10	8.04	0.07
54,322.18	11.40	0.31
54,322.25	8.53	0.08
54,322.32	9.09	0.11
54,322.39	7.61	0.06
54,322.46	6.88	0.04
54,322.53	7.10	0.04
54,322.60	8.16	0.07
54,322.67	7.18	0.05
54,322.74	7.73	0.06
54,322.95	7.65	0.06
54,323.23	8.04	0.07
54,323.37	9.96	0.16
54,323.45	9.68	0.14
54,323.59	8.15	0.07
54,323.66	6.88	0.04
54,323.73	9.08	0.11
54,323.80	7.46	0.05
54,323.87	7.86	0.06
54,323.94	7.62	0.06
54,324.01	7.97	0.07
54,324.08	8.34	0.08
54,324.15	7.64	0.06
54,324.29	7.98	0.07
54,324.57	7.95	0.06
54,324.64	7.37	0.05
54,324.72	7.43	0.05
54,324.79	7.56	0.05
54,324.86	8.51	0.08
54,324.93	9.02	0.11
54,325.14	7.23	0.05
54,325.21	7.67	0.06
54,325.28	10.04	0.17
54,325.35	9.85	0.15
54,325.42	7.43	0.05
54,325.63	8.67	0.09
54,325.70	8.47	0.08
54,325.77	7.99	0.07
54,325.84	9.75	0.15
54,325.91	8.30	0.08
54,325.98	8.70	0.09
54,326.06	9.49	0.13
54,326.20	6.47	0.03
54,326.27	8.20	0.07
54,326.34	10.41	0.20
54,326.41	8.53	0.08
54,326.48	9.59	0.14
54,326.55	7.47	0.05
54,326.62	9.28	0.12
54,326.76	8.02	0.07
54,326.83	8.39	0.08
54,326.90	9.02	0.11
54,326.97	8.01	0.07
54,327.25	8.02	0.07
54,327.33	9.54	0.13
54,327.40	9.27	0.12
54,327.47	7.47	0.05
54,327.54	9.75	0.15
54,327.61	9.44	0.13
54,327.68	9.20	0.11
54,327.75	7.76	0.06
54,327.82	9.19	0.11
54,327.89	9.00	0.10
54,327.96	9.17	0.11
54,328.03	8.78	0.09
54,328.10	8.19	0.07
54,328.17	8.40	0.08
54,328.24	8.58	0.09
54,328.31	8.39	0.08
54,328.45	10.60	0.22
54,328.67	9.57	0.14
54,328.74	9.56	0.13
54,328.81	8.16	0.07
54,328.88	8.27	0.08
54,328.95	9.24	0.12
54,329.02	7.62	0.06
54,329.09	8.58	0.09
54,329.16	8.87	0.10
54,329.23	9.06	0.11
54,329.37	8.51	0.08
54,329.44	10.23	0.18
54,329.51	8.49	0.08
54,329.58	9.00	0.10
54,329.65	8.43	0.08
54,329.72	9.09	0.11
54,329.79	9.20	0.11
54,329.87	11.10	0.27
54,329.94	8.55	0.09
54,330.01	8.21	0.07
54,330.08	11.81	0.38
54,330.15	8.35	0.08
54,330.29	8.54	0.09
54,330.36	8.33	0.08
54,330.43	7.37	0.05
54,330.50	7.79	0.06
54,330.57	9.18	0.11
54,330.64	8.78	0.09
54,330.71	7.83	0.06
54,330.85	9.85	0.15
54,330.99	8.70	0.09

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