A Spectroscopic and Photometric Survey of Novae in M31
A. W. Shafter, M. J. Darnley, K. Hornoch, A. V. Filippenko, M. F. Bode, R. Ciardullo, K. A. Misselt, R. A. Hounsell, R. Chornock, T. Matheson
aa r X i v : . [ a s t r o - ph . GA ] A p r A Spectroscopic and Photometric Survey of Novae in M31
A. W. Shafter , M. J. Darnley , K. Hornoch , A. V. Filippenko , M. F. Bode , R.Ciardullo , K. A. Misselt , R. A. Hounsell , R. Chornock , , and T. Matheson ABSTRACT
We report the results of a multi-year spectroscopic and photometric surveyof novae in M31 that resulted in a total of 53 spectra of 48 individual novacandidates. Two of these, M31N 1995-11e and M31N 2007-11g, were revealedto be long-period Mira variables, not novae. These data double the number ofspectra extant for novae in M31 through the end of 2009 and bring to 91 thenumber of M31 novae with known spectroscopic classifications. We find that 75novae (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 findno compelling evidence that spectroscopic class depends sensitively on spatialposition or population within M31 (i.e., bulge vs. disk), although the distributionfor He/N systems appears slightly more extended than that for the Fe II class. Weconfirm the existence of a correlation between speed class and ejection velocity(based on line width), as in the case of Galactic novae. Follow-up photometryallowed us to determine light-curve parameters for a total of 47 of the 91 novaewith known spectroscopic class. We confirm that more luminous novae generallyfade the fastest, and that He/N novae are typically faster and brighter than theirFe II counterparts. In addition, we find a weak dependence of nova speed class onposition in M31, with the spatial distribution of the fastest novae being slightlymore extended than that of slower novae. Department of Astronomy, San Diego State University, San Diego, CA 92182, USA Astrophysics Research Institute, Liverpool John Moores University, Birkenhead CH41 1LD, UK Astronomical Institute, Academy of Sciences, CZ-251 65 Ondˇrejov, Czech Republic Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Lab, Uni-versity Park, PA 16802, USA Steward Observatory, University of Arizona, Tucson, AZ, 85721, USA Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719-4933, USA
Subject headings: galaxies: stellar content — galaxies: individual (M31) — stars:novae, cataclysmic variables
1. Introduction
Classical novae form a subclass of the cataclysmic variable stars. They are semidetachedbinary star systems where a late-type Roche-lobe-filling star transfers mass to a white dwarfcompanion (e.g., Warner 1995, 2008). If the mass accretion rate onto the white dwarf issufficiently low to allow the accreted gas to become degenerate, a thermonuclear runaway(TNR) will eventually ensue in the accreted envelope, leading to a nova eruption. Theseeruptions can reach an absolute magnitude as bright as M V ≈ −
10 (e.g., Starrfield et al.2008), making them among the most luminous explosions in the Universe. Their high lumi-nosities and rates ( ∼
50 yr − in a galaxy like M31; Shafter & Irby 2001; Darnley et al. 2006)make novae powerful probes of the properties of close binaries in different (extragalactic)stellar populations. The most thoroughly studied extragalactic system is M31, where morethan 800 novae have been discovered over the past century (e.g., see Pietsch et al. 2007e;Shafter 2008, and references therein).Despite this large number of novae discovered, very few follow-up studies of their pho-tometric, or particularly their spectroscopic, properties have been attempted. Most recentM31 surveys have been undertaken through narrow-band filters in order to take advantageof the fact that novae fade more slowly in H α than they do in the continuum (e.g., Ciar-dullo et al. 1987; Shafter & Irby 2001). Such observations are ideal for determining the rateand spatial distribution of novae within a galaxy, but not for characterizing the nova lightcurves. As shown by Ciardullo et al. (1990b) the H α light curves are not simply correlatedwith the peak luminosity as are the broad-band light curves. Moreover, most of the broad-band light-curve data for M31 novae come from the early photographic studies of Arp (1956)and Rosino (1964, 1973), as summarized by Capaccioli et al. (1989), and from observationsin Crimea and Latvia during the period between 1977 and 1990 (Sharov & Alksnis 1992).Similarly, spectroscopic data for M31 novae have, until recently, also been limited. Thedearth of available spectra is not surprising given that novae in M31 are by definition tran-sient, and relatively faint, reaching peak brightnesses in the range m V ≈
18 to m V ≈
15 magbefore fading back to quiescence. Furthermore, since their eruptions are not predictable inadvance, spectroscopic observations require not only timely access to large telescopes, butcoordination with a photometric survey dedicated to discovering suitable targets. Humason(1932) was the first to report spectroscopic observations of classical novae in M31, and it wasnot until more than half a century later that Ciardullo et al. (1983) published the spectra 3 –of four H α emission-line sources, which they identified as classical novae in eruption. Thenumber of nova spectra has increased dramatically in recent years thanks to greater accessto queue scheduling on large telescopes, such as the Hobby-Eberly Telescope (HET).In order to better understand the spectroscopic properties of novae in M31, and to studyany variation with spatial position in the galaxy, we began a multi-year M31 nova survey inthe Fall of 2006 using the HET. The program was motivated in large part by the work ofWilliams (1992), who realized that the spectra of Galactic novae (taken within a few weeksof eruption) can be divided into one of two principal spectroscopic types: Fe II and He/N.These types are believed to be related to fundamental properties of the progenitor binarysuch as the white dwarf mass. As part of our HET program, we have measured the spectraof 26 M31 novae (representing ∼ /
2. Observations2.1. Spectroscopy
During the early part of our survey, optical spectra were obtained primarily with the Lick3-m Shane reflector using the Kast double spectrograph (Miller & Stone 1993), although theobservation of M31N 1990-10b was taken with the older UV Schmidt spectrograph (Miller& Stone 1987). Most spectra were acquired in one of two basic instrument configurations.One used the D55 dichroic beamsplitter to split the spectrum over ∼ ∼ ∼ . ′′ -wide slit giving a spectral resolution of ∼ ∼
11 ˚A (6 ˚A) in the red. The other setup removed the beamsplitter and all light was sent toa 600/5000 grating on the red side, providing ∼ ∼ , and the data were extracted IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Associ- g ′′ slit and the GG385 order-blockingfilter, covering 4275–7250 ˚A at a resolution of R ≈ g ′′ slit andthe GG385 filter. This choice increased our wavelength coverage to 4150–11000 ˚A whileyielding a resolution of R ≈ g λ ∼ < ation for Research in Astronomy, Inc. under cooperative agreement with the National Science Foundation. To complement our spectroscopic survey, we were able to amass sufficient photomet-ric observations to produce light curves for many of the novae in our survey. Our primarymotivation was to measure nova fade rates ( t ) that could then be correlated with other prop-erties, such as spectroscopic class. The photometric data consist both of targeted (mostly B and V -band) observations, which were obtained primarily with the Liverpool Telescope(LT; Steele et al. 2004) and the Faulkes Telescope North (FTN; Burgdorf et al. 2007), andsurvey images (mainly R band), taken over the years with a variety of telescopes. The LTand FTN data were reduced using a combination of IRAF and Starlink software, calibratedusing standard stars from Landolt (1992), and checked against secondary standards fromMagnier et al. (1992), Haiman et al. (1994), and Massey et al. (2006).Our extensive R -band observations were taken largely from the photometric databasecompiled by one of us (K.H.) as part of an ongoing program to monitor nova light curvesin M31. These data include both survey and targeted images taken with various telescopeswith diameters of 0.26–6 m. Most of the images come from the 0.65-m telescope of theOndˇrejov Observatory (operated partly by the Charles University, Prague) and the 0.35-mtelescope in the private observatory of K.H. at Lelekovice. Standard reduction proceduresfor raw CCD images were applied (bias and dark-frame subtraction and flat-field correction)using the SIMS and Munipack programs. Reduced images of the same series were coaddedto improve the signal-to-noise ratio; the total exposure time of these series varied from afew minutes up to about one hour. To facilitate nova detection, the gradient of the galaxybackground was flattened by the spatial median filter using SIMS. Photometric and astro-metric measurements of the novae were then performed using “Optimal Photometry” (basedon fitting of point-spread function profiles) in GAIA and APHOT (a synthetic aperturephotometry and astrometry software package developed by M. Velen and P. Pravec at theOndˇrejov Observatory; see Pravec et al. [1994]), respectively. Five to ten comparison starswere used for individual brightness measurements. B , V , and R magnitudes for comparisonstars located in the M31 field were taken from Massey et al. (2006). Finally, in the caseof images taken using the Sloan Digital Sky Survey (SDSS) g ′ and r ′ filters, we computed g ′ and r ′ magnitudes for comparison stars from BV RI magnitudes taken from Massey etal. (2006) using empirical color transformations between the SDSS ugriz system and theJohnson-Cousins
U BV RI system published by Jordi et al. (2006). A summary of all of our http://ccd.mii.cz/ http://munipack.astronomy.cz/
3. Nova Populations3.1. Background
It has been conjectured, based both on Galactic and extragalactic observations, thatthere may exist more than one population of novae (e.g., Della Valle et al. 1992; DellaValle & Livio 1998; Shafter 2008; Kasliwal et al. 2011, and references therein). Initially,Galactic observations suggested that novae associated with the disk were on average moreluminous and faded more quickly than novae thought to be associated with the bulge (e.g.,Duerbeck 1990; Della Valle et al. 1992). However, the interpretation of Galactic nova datais complicated by the need to correct for interstellar extinction, which can be significant andvaries widely with the line of sight to a particular nova. Furthermore, extinction hampers thediscovery of a significant fraction of objects: although Galactic novae occur at an estimatedrate of ∼ − (Shafter 1997, 2002), only about one in five of these are discovered andsubsequently studied in any detail. Consequently, although much has been learned fromthe study of Galactic novae, it is clear that these data are not ideal for establishing thepopulation characteristics of novae.Nova eruptions are luminous enough to be detected as far away as the Virgo cluster.However, despite the considerable data amassed in recent years, evidence for distinct novapopulations in extragalactic systems is conflicting. Ciardullo et al. (1990b) argued that agalaxy’s nova rate was independent of the galaxy’s Hubble type, and therefore independentof the galaxy’s dominant stellar population. A few years later, based largely on the samedata, but with different assumptions regarding the luminosity normalization, Della Valleet al. (1994) proposed that nova rates and light-curve properties (e.g., rate of decline frommaximum light) did in fact vary between galaxies of differing Hubble types, with late-typesystems such as M33 and the Magellanic Clouds having generally faster fading novae andhigher luminosity-specific nova rates. However, subsequent studies (e.g., Shafter et al. 2000;Ferrarese et al. 2003; Shafter & Williams 2004) have questioned these results, arguing that(given the considerable uncertainties that plague the determination of luminosity-specific 7 –nova rates) the available data are insufficient to establish any significant correlation. Further,the broader implications of the argument by Della Valle & Duerbeck (1993) that novae inthe Large Magellanic Cloud (LMC) generally were brighter and faded faster than those seenin the older stellar populations of the Galaxy or M31’s bulge, has been called into questionby Ferrarese et al. (2003) who showed that novae in M49, the first-ranked Virgo ellipticalgalaxy, generally faded at least as fast as novae in the LMC. The nearby Sb spiral, M31, is by far the most thoroughly studied extragalactic system,with observations of novae going back to Hubble (1929). Spanning ∼ ∼ ′ of the nucleus, and (3) the frequency distribution of nova maximum magnitudes isbimodal, with peaks m pg ≈ . m pg ≈ . α imaging confirmed that the novaspatial distribution is more centrally concentrated than the background light; in fact thedistribution was consistent with a purely bulge population. The central “hole” in the novadistribution noted by Arp was not seen in the H α data, and was assumed to be an artifactof the poor contrast against the bright nuclear background in Arp’s photographic images.Several more recent studies of the spatial distribution of M31 novae have confirmedthe association with M31’s bulge population (e.g., Capaccioli et al. 1989; Shafter & Irby2001; Darnley et al. 2004, 2006), but a major uncertainty in these studies is whether asignificant fraction of disk novae are being missed due to internal extinction within thegalaxy (see also Hatano et al. 1997). Taken at face value, the association of novae with M31’sbulge population came as a surprise given that Galactic novae have long been recognized tohave a significant disk population (e.g., Duerbeck 1984, 1990). To address this discrepancy,Ciardullo et al. (1987) proposed the idea that a significant fraction of the novae in M31’s bulgecould have been formed in the dense cores of the galaxy’s globular clusters and subsequentlybeen ejected into the bulge through three-body interactions within the clusters, through tidaldisruption of some clusters, or a combination of both processes. 8 – A promising new approach for studying nova populations is to consider the characterof a nova’s spectrum within a few weeks after maximum light. When analyzing a largesample of Galactic nova spectra, Williams (1992) realized that the novae could be naturallysegregated into two principal spectroscopic classes (Fe II and He/N) based on the emissionlines in their spectra. Novae displaying prominent Fe II emission (the Fe II novae) usuallyshow P Cygni absorption profiles, evolve more slowly, have lower expansion velocities, andshow lower levels of ionization, compared to novae with strong lines of He and N (theHe/N novae). Complicating this division is the fact that a small fraction of novae initiallyexhibit Fe II emission lines along with broad (full width at half-maximum intensity [FWHM] ∼ > − ) Balmer emission before going on to develop spectra typical of the He/Nnovae. Such systems are referred to as either hybrid or Fe IIb novae. Both Fe II andHe/N novae (although more often the He/N systems) occasionally go on to develop strongNe emission in their post-outburst spectra, which suggests that the higher-mass ONe whitedwarfs may be found in both classes of novae.Della Valle & Livio (1998) analyzed the spatial distribution of a sample of 22 Galacticnovae with data suitable for determining their spectroscopic class. By restricting their sampleto novae with well-determined distances (i.e., from expansion parallax), they were able to usethe observed positions to estimate the distance of each nova from the Galactic plane. Theydiscovered that the fastest and brightest novae were primarily associated with the He/Nspectroscopic class, and that the progenitors were preferentially located close to the Galacticplane (i.e., z ∼ <
100 pc). Fainter and dimmer novae, on the other hand, were more typicallymembers of the Fe II class, and were found at much greater heights (up to z ∼ >
4. The M31 Nova Survey4.1. Spectroscopic Class
Through the end of 2009, a total of 837 nova candidates have been discovered in M31since the observations of Hubble (1929) began nearly a century ago.(Pietsch et al. 2007e) Of these, spectra are now available for a total of 91 M31 novae, including the 46 fromour present survey. As described above, novae spectra are, in principle, divisible into one ofthree primary classes: Fe II, He/N, and hybrid (or Fe IIb) novae. In practice, however, it isoften difficult to make an unambiguous classification. Spectra are taken at different timesafter eruption, and the signal-to-noise ratio can vary widely from spectrum to spectrum. Inaddition, a nova can, on occasion, show characteristics of more than one class. For example,during the course of our spectroscopic survey, we have identified three novae (M31N 2007-10a,2007-10b, and 2007-11b) that might have been traditionally classified as He/N or hybrid, butwhich do not share all of the characteristics of those classes. These spectra are dominated byprominent but narrow (FWHM < − ) lines of H, He I, and He II, with weaker N IIIand Fe II emission features occasionally seen. In the basic scheme of Williams (1992), suchnovae would be difficult to classify. Henceforth, we will refer to these objects as narrow-lineHe/N, or He/Nn, novae.The spectra of all novae included in our survey (see Figs. 1–12) were examined andsubsequently classified into one of six groups: Fe II, likely Fe II (Fe II:), He/N, likely He/N(He/N:), He/Nn, and hybrid (also known as broad-lined Fe II or Fe IIb novae). We found atotal of 30 Fe II novae ( ∼ ∼ ∼ ∼ ∼ ∼ Whenall 91 novae with measured spectra are considered (see Table 4), the relative percentagesremain similar with ∼
74% (67 novae), ∼
8% (7 novae), ∼
11% (9 novae), ∼
7% (6 novae), and ∼
1% (one nova) representing the Fe II, Fe II:, He/N, He/N: (including the He/Nn systems), ∼ m31novae/opt/m31/index.php Most, perhaps all, novae that are classified as He/N appear to display some weak Fe II emission nearmaximum light, and are therefore technically members of the hybrid class. Rather than referring to allof these novae as hybrid objects, we reserve the hybrid classification for those novae with prominent Fe IIemission early on (e.g., M31N 2006-10b).
10 –and hybrid classes, respectively. Thus, when all the data are considered, approximately 4out of 5 ( ∼ ∼
40% of novae in his Galactic sample belonged to the He/N class. Simi-larly, Della Valle & Livio (1998) found that as many as 10 out of 27 (37%) in their sampleof novae with well-determined distances (from expansion parallax) were He/N or Fe IIb sys-tems. More recently, however, Shafter (2007) has reviewed all available spectroscopic datafor Galactic novae, finding that only 20 out of the 94 systems ( ∼ The apparent concentration of He/N and hybrid/Fe IIb novae toward the disk of theGalaxy (Della Valle & Livio 1998) is an intriguing finding, and it would be of considerableinterest if it could be confirmed in M31. While it is not possible to determine the height of agiven nova above M31’s galactic plane, we can explore differences in the spatial distributionsbetween the different spectroscopic classes. Based on the Galactic results of Della Valle &Livio (1998), one might expect that the He/N and related systems would be preferentiallyassociated with the disk of M31, while the Fe II systems would perhaps display a morecentrally concentrated, bulge-like distribution.In Figure 21 we have plotted the projected positions of the 91 M31 novae with knownspectroscopic class. Despite the expectation that the He/N nova distribution might be moreextended compared to the Fe II systems, there appears to be no obvious dependence ofspectroscopic type with spatial position in the galaxy. This impression can be misleading,however, since the high inclination of M31 to the plane of the sky ( i ≈ ◦ ) makes it difficultto assign an unambiguous position within M31 to a given nova. This is particularly truefor novae near the center of M31 where the foreground disk is superimposed on the galacticbulge. On the other hand, novae observed at a large galactocentric radius ( ∼ > ′ ) are likelyto be associated with the disk of the galaxy. In order to approximate the true position of a 11 –nova within M31, we have assigned each nova an isophotal radius, defined as the length ofthe semimajor axis of an elliptical isophote [computed from the R -band surface photometryof Kent (1987)] that passes through the observed position of the nova.In Figure 22 we show the cumulative distributions of the Fe II and He/N (and hybrid)novae plotted as a function of their isophotal radius. Although it appears that the He/N-hybrid distribution may be slightly more extended than the Fe II distribution, a Kolmogorov-Smirnov (KS) test reveals that the distributions would be expected to differ by more thanthat observed 81% of the time if they were drawn from the same parent population. Whenonly a subset of the novae with well-established spectroscopic types are considered, thisprobability decreases slightly to 73%.The interpretation of these results is complicated by the fact that our spectroscopic dataare drawn from a sample of M31 novae that may not be spatially complete. As mentionedearlier, although the CCD surveys conducted in H α are essentially complete in the innermostregions of the galaxy, they did not typically cover the full disk of M31. In recent years thesituation has improved with the availability of wide-field surveys, such as the ROTSE-IIIbprogram, which have provided good coverage over most of the galaxy. Given the nature ofthe M31 surveys, we suspect that our spectroscopic sample may be biased somewhat towardnovae at smaller galactocentric radii (where, historically, the galaxy has been more frequentlymonitored), and thus may favor one spectroscopic class over the other. Nevertheless, such abias should not affect the distributions of Figure 22 in a differential sense: both Fe II andHe/N novae are detectable throughout the galaxy. Another potential source of bias involvesthe fact that the He/N novae are on average brighter and faster fading than the Fe II systems(see § One of the defining properties of the He/N spectroscopic class is that the emission-linewidths are considerably broader than those seen in the Fe II novae. Specifically, Williams(1992) found that the emission lines of Galactic novae in the He/N class are characterized bya half-width at zero intensity (HWZI) > − . Empirically, we have found that for 12 –most nova line profiles, the HWZI roughly equals the FWHM; since the latter is the moreeasily measured quantity, we have adopted it to characterize the spectra in our survey. Thevalues of the FWHM and the equivalent widths of H α and H β in our nova spectra are givenin Table 5.Although the emission-line width is expected to be correlated with the expansion velocityof the nova ejecta, the FWHM does not necessarily yield the expansion velocity directly. Inan idealized nova, the broad emission features typically seen in an He/N system are believedto be formed mainly in a discrete, optically thin shell ejected at relatively high velocity fromnear the white dwarf’s surface. In this case, the line profiles are expected to be flat-toppedand nearly rectangular in appearance, with the FWHM closely approximating the ejectionvelocity of the shell. In the Fe II systems, however, the lines are mainly produced in awind, which originates at a distance above the surface of the white dwarf that varies as theoutburst evolves. Thus, the escape velocity for this wind is smaller than that at the whitedwarf’s surface. As a result, the expansion velocity (and hence line width) may depend onthe time elapsed since eruption.When comparing the emission-line widths of the novae in our sample, it must be kept inmind that our spectroscopic data were obtained at varying times after eruption, and thus donot necessarily reflect the relative expansion velocities accurately. Nevertheless, as Figure 23illustrates, a clear difference between the ejection velocities of the two principal classes ofnovae (Fe II and He/N) is apparent. Without exception, the novae belonging to the He/Nclass are characterized by H α FWHM > − , while the Fe II systems all have H α FWHM less than this value. Interestingly, although He/Nn novae display prominent lines ofhelium as do the standard He/N novae, they are narrow-line objects that resemble a typicalFe II nova at times (e.g., see M31N 2007-11b in Fig. 8). In addition, they often do notdisplay prominent lines of nitrogen as do the typical He/N systems.
To further explore the properties of the novae in our survey, whenever possible we haveaugmented our spectroscopic data with available photometric observations. Few light curvesare available for the novae in our spectroscopic sample that erupted prior to the start of ourHET survey in 2006. Nevertheless, when the entire set of spectroscopic novae is considered,we have sufficient photometric data to estimate decline rates for half of the sample.A convenient and widely used parameterization of the decline rate is t , which repre-sents the time (in days) for a nova to decline 2 mag from maximum light. According to the 13 –criteria of Warner (2008), novae with t ∼ <
25 days are considered “fast” or “very fast,” withthe slowest novae characterized by t values of several months or longer. Rates of decline,and corresponding values of t , have been measured (for all novae with sufficient photometriccoverage) by performing weighted linear least-squares fits to the declining portion of the lightcurves that extend up to 3 mag below peak. In an attempt to account for systematic errorsin the individual photometric measurements, the weights used in the fits were composed ofthe sum of the formal errors on the individual photometric measurements plus a constantsystematic error estimate of 0.1 mag. The net effect of including the systematic error com-ponent was a reduction of the relative weighting of points with small formal errors and acorresponding increase in the formal errors of the best-fit parameters and in the uncertaintiesin t derived from them.Because our photometric observations do not always begin immediately after discovery,and the date of discovery does not always represent the date of eruption, we have made twomodifications to our photometric data in order to better estimate the light-curve parameters.First, when available, we have augmented our light-curve data with the discovery dates andmagnitudes given in the catalog of Pietsch et al. (2007e). Second, for some novae we havemodified (brightened) the peak magnitude slightly through an extrapolation of the decliningportion of the light curve up to 2.5 days pre-discovery in cases where upper flux limits (within5 days of discovery) are available. The light-curve parameters resulting from our analysisare given in Table 6.
If we adopt a distance modulus for M31 of µ = 24 .
38 mag (Freedman et al. 2001) anda foreground reddening, E ( B − V ) = 0 .
062 mag (Schlegel et al. 1998), we can compute theabsolute magnitude at maximum light, and thereby produce calibrated maximum-magnitudeversus rate-of-decline (MMRD) relations. The MMRD relations (the peak absolute magni-tude vs. log t ) for the B , V , and R light curves are shown in Figures 24, 25, and 26,respectively. These plots illustrate not only that the peak nova luminosity is correlated withthe rate of decline (i.e., the brightest novae generally fade the fastest), as was first studiedextensively by McLaughlin (1945) for Galactic novae, but that the He/N systems are typi-cally among the brightest and fastest novae. Weighted, linear least-squares fits to our B , V , ∼ m31novae/opt/m31/index.php
14 –and R -band data yield M B = − . ± .
11 + (1 . ± . t , (1) M V = − . ± .
10 + (1 . ± . t , (2)and M R = − . ± .
12 + (2 . ± . t , (3)respectively. The peculiar He/Nn object M31N 2007-10b, which has particularly scanty light-curve coverage, has a relatively large uncertainty in the peak magnitude. For comparison, inFigure 24 we show the theoretical M B vs. log t relation of Livio (1992), while in Figure 25we include the Galactic M V relation from Downes & Duerbeck (2000): M V = − . ± .
44 + (2 . ± .
32) log t . (4)The slope of our M31 V -band MMRD relation is shallower than that for the Galacticdata, and the M31 data are also systematically fainter than expected from the best-fittingGalactic relations. The latter discrepancy, in particular, as well as some of the scattergenerally seen in the MMRD relations, is likely due to the fact that we have only correctedthe M31 data for Galactic foreground extinction, not for extinction internal to M31. Basedon these comparisons, it appears that the M31 nova sample perhaps suffers as much as0.5 mag of extinction from within M31 itself, especially in the disk of the galaxy. This valueis consistent with an estimate of A ( r ′ ) = 0 . r ≤ ′ and those with r > ′ , we find that the latter sample is slightly fainter at peakby an average of ∼ . . ± . . ± . The R -band MMRD relation includes r ′ -band data for novae where R -band observations are not available.When both R and r ′ observations are available for a given nova, only the more extensive data set is used.
15 –although our sample is dominated by Fe II systems, three of the four fastest novae are He/Nor related (He/Nn) systems. On the other hand, with the exception of the He/Nn nova M31N2007-10b, we do not find strong evidence for a significant population of fast, but relativelyfaint, novae that apparently do not follow the classic MMRD relation. As discussed byKasliwal et al. (2011), it is possible that these novae arise from progenitors containing high˙ M (hot) and relatively massive white dwarfs, similar to what is expected for recurrent novae.Perhaps such novae are related to the class of He/Nn novae described earlier.Given that the He/N novae generally fade more quickly than the Fe II systems, and thatHe/N novae have significantly higher expansion velocities based on their emission-line widths,the expansion velocity should be inversely correlated with the light-curve parameter, t . InFigure 27 we have plotted the measured t value (based on the V band when possible) versusthe measured H α FWHM for the 25 novae in our survey where it is possible to measure bothparameters. As expected, there is a clear trend of faster novae exhibiting higher expansionvelocities. The one exception is the He/Nn nova, M31N 2007-10a, which apparently evolvedquite quickly despite its relatively slow expansion velocity. Based on these data (excludingM31N 2007-10a), a weighted linear least-squares fit yields the following:log t (d) = 6 . ± . − (1 . ± .
02) log [H α FWHM (km / s)] . (5)This relation can be compared with a similar one for Galactic novae found by McLaughlin(1960). A major factor in the discrepancy between the two may arise because in McLaughlin’srelation the expansion velocities are derived from the absorption-line minima (P Cyg profiles)measured near maximum light. Typically, such velocities are only 20% to 50% of thoseinferred from the emission-line FWHM. The scatter in our data, particularly for the slowernovae, is probably due in part to the time dependence of the derived velocities, as referredto in § The question of whether the photometric properties of novae in M31 (e.g., peak bright-ness, fade rate) vary with spatial position in the galaxy (and possibly with stellar population)has yet to be thoroughly studied. Most recent surveys, which have concentrated primarilyon the discovery of novae either for the purpose of measuring the spatial distribution, theoverall rate, or both, lack the high cadence required to produce useful nova light curves.Light-curve data, when available, often only cover H α or the R band where the relationshipbetween fade rate and peak luminosity is weak or absent (e.g., Ciardullo et al. 1990b). As 16 –mentioned earlier, available broad-band nova data come largely from the photographic sur-veys of Arp (1956), Rosino (1964, 1973), and Sharov & Alksnis (1992). As noted above, theobservation by Arp (1956) that the apparent magnitude distribution for M31 appeared to bebimodal, with peaks corresponding to M B ≈ − . M B ≈ − . t for a total of 74 novae. Ofthese, 35 (approximately half the total) are characterized by t ≤
25 days, and were cat-egorized as either “fast” or “very fast” according to the definition in Warner (2008). Forour purposes we simply refer to this group as the “fast” novae. We refer to the remaining35 novae with t >
25 days as “slow” novae. Given the uncertainties involved in accuratelymeasuring t , we did not restrict our sample of fade rates to any particular color or bandpass;however, when data were available in multiple colors, we chose the t values based on B -bandobservations to be as consistent as possible with data from earlier surveys.In Figure 28 we have plotted separately the spatial distributions of the “fast” and“slow” novae. It appears that the slower novae (red circles) are perhaps more centrallyconcentrated than the fast sample (blue squares). This impression is confirmed when weconsider the cumulative distributions shown in Figure 29. A KS test reveals that the twodistributions would be expected to differ by more than they do 23% of the time if they weredrawn from the same parent distribution. Thus, our data are consistent with the notion that“faster” novae, both in the Galaxy (Duerbeck 1990; Della Valle et al. 1992) and in M31, aremore associated with the disk population than are the slower novae. We caution, however,that selection effects could potentially complicate the interpretation of this result. As waspointed out earlier in our discussion of spectroscopic class, our nova sample is not likelyto be spatially complete. It is possible that we may be preferentially missing faster novaein the outer regions of the galaxy where the temporal sampling of the surveys has perhapsbeen less frequent. If so, our conclusion that the faster novae appear to be more spatiallyextended would actually be strengthened. Taken at face value, our results suggest that thephotometric characteristics of novae are likely affected by changes in the underlying stellarpopulation. 17 – Below we highlight several individual novae of particular significance. These objectshave either have been detected as a super-soft X-ray source (SSS), or have been observed ex-tensively, both photometrically and spectroscopically, or have some peculiarity that warrantsfurther discussion.
As part of a program of follow-up spectroscopy of Local Group transients, one of us(A.V.F.) obtained spectra of two novae in the bulge of M31 on 1993 Nov. 8 and 17 (UTdates are used throughout this paper). The positions of the two objects are near that oftwo novae discovered in the survey by Shafter & Irby (2001), M31N 1993-10g and 1993-11c,which are separated by ∼ ′′ . Unfortunately, the original observing logs are no longeravailable, so we are unable to make an unambiguous connection between the two spectraand the two novae. Based on approximate coordinate information in the FITS header forthe spectrum taken on 1993 Nov. 17, we have made the tentative assignments indicated inFigures 1 and 2. The spectrum we have associated with M31N 1993-11h is clearly that of anFe II nova, while that of 1993-11c is less certain but consistent with an Fe II classification.Both novae have been identified as possible recurrent nova candidates by Shafter & Irby(2001). The position of M31N 1993-10g is coincident with 1964-01a to within 9 . ′′ , whilethat of 1993-11c is within 3 . ′′ and 6 . ′′ of 1967-12a and 1923-02a, respectively. Given thatthe coordinates for novae discovered on photographic plates are not known precisely in manycases, these both appear to be plausible recurrent nova candidates. However, both novaeare located only ∼ ′ from the nucleus of M31 where the nova density is high, increasing theprobability of a chance positional coincidence. For a given observed separation s , we cancompute the probability of a chance coincidence, P C , by considering the nova density in anannulus of area A , centered at the position of each nova. Specifically, P C = 1 − exp h n − X i=1 ln(1 − ix) i , (6)where n is the number of novae in the annulus, and x = πs /A . In both cases of interesthere, we find that P C ∼ > .
95, making it highly likely that the two outbursts were a chancecoincidence from separate objects, and therefore not from a recurrent nova. 18 –
M31N 1995-11e was identified during the nova survey of Shafter & Irby (2001), whofirst recorded the object on 1995 Nov. 28 at m Hα = 18 . m Hα = 17 . m ≈ . m ≈
18 mag on Sep. 09. Our spectrum presented here (see Fig. 12) and originally reportedby Shafter et al. (2008) clearly shows that the object is a long-period red variable star (i.e.,a Mira variable), and not a nova.
M31N 2001-10a was discovered as part of the POINT-AGAPE (Darnley et al. 2004)and the Naini Tal microlensing surveys (Joshi et al. 2004). Our spectroscopic data and r ′ -band photometry show that M31N 2001-10a was a relatively slowly evolving Fe II novacharacterized by t = 73 days. X-ray observations reported by Henze et al. (2010, 2011)show the nova to be a long-lived SSS that was still detectable more than 7 yr post outburst.The long duration of the SSS phase is indicative of prolonged burning on the surface of thewhite dwarf. This is expected for the relatively large accreted mass associated with slowlyevolving outbursts on a low-mass white dwarf. M31N 2005-01a, discovered by Hornoch (2005) on 2005 Jan. 07.89, was a particularlyluminous nova that was well covered photometrically near maximum light, reaching R =15 .
04 mag (see Fig. 14). Our spectrum (see Fig. 4), taken 8 days post discovery when thenova was near R = 15 . M ∼ < − . M31N 2005-07a, discovered by K.H. on Jul 2005 27.909 at R = 18 . R = 17 . ∼ α emission and a numberof extremely weak features that may include He and N emission. We tentatively classify theobject as an Fe II: system, but it is possibly related to the He/Nn novae. M31N 2005-09b was discovered in the outskirts of M31 by Quimby et al. (2005) onSep. 1.23 using the 0.45-m ROTSE-IIIb telescope at the McDonald Observatory. The novareached m = 16 . α : FWHM ≈ − , HWZI ≈ − ), Fe II, Na D, and He I emission features. The nova isconsistent with membership in the Fe II spectroscopic class; however, the emission-line widthis at the high end of what is normally seen in Fe II novae, and the nova could be plausiblyincluded in the Fe IIb or hybrid class. M31N 2006-09c was discovered independently by Quimby (2006), K. Itagaki, P. Kuˇsnir´ak,and K.H. on 2006 Sep. 18. It was detected ∼
150 days post discovery by both the IRACand IRS instruments on the
Spitzer Space Telescope as part of an infrared survey of selectedM31 novae recently conducted by Shafter et al. (2011). No evidence of an infrared excesscharacteristic of dust formation was apparent at the time of these observations. The novawas also detected as a weak SSS by Henze et al. (2011) and originally classified as a Fe IInova by Shafter et al. (2006). Our R -band photometry shows that t = 26 days, indicatinga moderate rate of decline typical of the Fe II class. M31N 2006-10a was a relatively faint nova discovered at R = 18 . Our observations (see Figs. 5 and 14) reveal the object to be a slowly evolvingFe II nova. It was also observed by Shafter et al. (2011) ∼
110 days post discovery as part of ∼ m31novae/opt/m31/M31 table.html
20 –their
Spitzer survey. M31N 2006-10a showed the clearest evidence of the 10 novae observedby
Spitzer for a near-infrared excess (in this case peaking at λ ≈ µ m), suggestive of dustformation. They went on to estimate the total mass of dust formed to be ∼ × − M ⊙ under the assumption that the dust was carbon based. Henze et al. (2011) found no evidenceof X-ray emission from this nova during the time of their observations. M31N 2006-10b was discovered independently by K. Itagaki on 2006 Oct. 31.583 and byR. Quimby and F. Castro at m ≈ . The time of maximum light is well constrained by Itagaki’s image from Oct. 30.530 (limitingmag 20.0), which shows no evidence of the nova. Although the light curve is not completenear maximum light, the available evidence suggests that the nova faded quite rapidly, withestimates of t ( B ) = 21 days and t ( V ) = 11 days.We obtained two spectra of the nova, the first ∼ ∼ Spitzer
IRS and IRAC, respectively, but not detected with either instrument.
M31N 2006-11a is a typical Fe II nova (see Fig. 6) that was discovered by K. Itagaki at m = 17 . The object was observed by Shafter etal. (2011) as part of their
Spitzer survey. It was marginally detected by the IRAC, but notwith the IRS, 86 and 77 days after discovery, respectively.
21 –
This nova was discovered by one of us (K.H.) on 2007 Feb. 03. It was classified asa likely hybrid nova by Pietsch et al. (2007a) based on possible He and N emission in thespectrum. Our spectrum, taken on 2007 Feb. 10.06, suggests the object is an Fe II system(see Fig. 7), although there appears to be a broader component in the H α and (possibly)the H β emission lines that is often seen in the hybrid systems. The light curve measured inthe R band yields t ( R ) = 35 days, which is typical of an Fe II nova but would be somewhatslow for a hybrid system. The object was also detected as a SSS by Henze et al. (2011), andwas still detectable 2 yr after eruption. Such a long active SSS phase is characteristic of arelatively large accreted mass. We conclude that the object was likely an Fe II nova. M31N 2007-06b was discovered by Quimby et al. (2007) as part of the ROTSE IIIbprogram at McDonald Observatory on 2007 Jun 19.4 at m = 16 . ∼ t ∼ <
18 days. Spectroscopic observations by Shafter& Quimby (2007) revealed the nova to be a member of the He/N spectroscopic class. Theobject was subsequently detected as a SSS by Pietsch et al. (2007b).
M31N 2007-07f was a slowly evolving nova discovered in the outskirts of M31 as partof the ROTSE-IIIb program by Yuan et al. (2007), and is apparently a member of the Fe IIspectroscopic class (Quimby 2007, private communication). The object exhibited a slow riseto maximum light, reaching m = 17 . ± . Spitzer survey of Shafter et al. (2011) and detected bythe IRAC. As discussed by Shafter et al. (2011), 2007-07f showed evidence (although moremarginal than for M31N 2006-10a) for a weak infrared excess, consistent with that expectedfrom dust grains formed in the ejecta.
22 –
This object was discovered by Pietsch et al. (2007c) at R = 18 . t ≈
63 days. The nova was included in the Shafter et al. (2011)
Spitzer survey and marginally detected with the IRAC, but not the IRS, about 158 and 183days post discovery, respectively.
M31N 2007-10a was discovered K. Itagaki on Oct. 5.606 and independently by Pietschet al. The spectrum was classified by Gal-Yam & Quimby (2007) as an Fe II nova, butour spectrum (see Fig. 7) reveals narrow Balmer, He I λλ λ t ( B ) ≈ t ( V ) ≈ Spitzer survey of Shafter et al. (2011).
M31N 2007-10b is the best example from our survey of a faint but fast nova similar tothe class of novae discovered by Kasliwal et al. (2011). The nova was discovered by Burwizet al. (2007) at R = 17 . The nova fadedunusually quickly: our B , V , and R light curves suggest t ≈ ∼ α = 1450 ±
100 km s − )for this class. Based on the available photometric and spectroscopic data, we suggest thatthe object is a member of our proposed He/Nn class. Consistent with its rapid evolution,the object was detected by Henze et al. (2011) as a SSS with an X-ray duration of less than100 days.
23 –
M31N 2007-11b, our third example of an He/Nn nova, was discovered by Pietsch etal. (2007d) and independently by E. Ovcharov and A. Valcheva. Although our spectrum(see Fig. 8) appears to be quite similar to that of an Fe II nova (albeit with weak Fe IIemission), subsequent spectra by Rau (2007) and Barsukova et al. (2007b) showed that theobject quickly developed prominent, narrow (FWHM H α = 1430 ±
100 km s − ) Balmer, He I,and He II emission lines. Unlike the other He/Nn systems (M31N 2007-10a and 2007-10b),the light-curve evolution of 2007-11b was not particularly fast, with t ( B ) = 25 days and t ( V ) = 45 days, respectively. M31N 2007-11d was an unusually bright and slowly rising nova discovered by K. Nishiyamaand F. Kabashima on Nov. 17.57, and subsequently studied extensively by Shafter et al.(2009). The early spectrum was that of a classic Fe II system: narrow Balmer and Fe IIemission lines flanked to the blue by pronounced P-Cyg absorption features. Another spec-trum obtained ∼ α = 2260 km s − ) with weak He I and O I emission (see Fig. 8). The nova fadedmoderately rapidly ( t [ V ] = 9 . Spitzer
IRS (Shafter et al. 2011).
M31N 2007-11g was discovered by Ovcharov et al. (2007) on 2007 Nov 28.716 at R ≈ . M31N 2007-12b was a relatively bright and rapidly evolving He/N nova. It was dis-covered on 2007 Dec. 9.53 by K. Nishiyama and F. Kabashima1 at m = 16 .
24 –(unfiltered), and independently by K.H. on Dec. 10.73 at R = 17 . Subsequent spec-troscopic observations revealed the object to be a rapidly declining ( t = 8 . B ] , . V ] days)He/N system (see Fig. 9 and Table 6). Initially, the object was thought to be a recurrent novagiven its close proximity to the position of M31N 1969-08a; however, subsequent astrometryestablished that the two novae were, in fact, distinct objects.Archival Hubble Space Telescope observations of the pre-outburst location of M31N 2007-12b (Bode et al. 2009) revealed the presence of a coincident stellar source with magnitudeand color very similar to those of the Galactic recurrent nova RS Ophiuchi, where the redgiant secondary star dominates the light at quiescence. This discovery, coupled with therapid photometric evolution and the object’s detection by the
Swift satellite (Burrows et al.2005) as an SSS (Kong & Di Stefano 2008), were interpreted by Bode et al. (2009) as strongevidence that M31N 2007-12b is, nevertheless, a recurrent nova system.
M31N 2007-12d was discovered independently by Henze et al. (2007) and by K. Nishiyama& F. Kabashima on 2007-Dec. 17.57. Although no detailed light-curve data exist, Henzeet al. (2011) estimated a rapid decline with t ≈ α ≈ − ) indicating a high expansion velocity. The nova was detected briefly( <
20 days) as an SSS by Henze et al. (2011).
M31N 2009-10b was discovered by K.H. and P. Kuˇsnir´ak on 2009 Oct. 9.986 (Hornoch2009), and independently by K. Itagaki on Oct. 11.414. . It was an unusually brightnova that reached R = 14 . t ≈
10 days in B and V ). Spectroscopic observations by Di Mille et al. (2009b) andBarsukova et al. (2009b) show conclusively that the nova belongs to the Fe II spectroscopicclass, making it quite similar to M31N 2007-11d.
25 –
5. Conclusions
Whether there exist two distinct populations of classical novae is an important butunanswered question. In an attempt to gain further insight, we have conducted a majorspectroscopic survey of novae in the nearby galaxy M31. These data have allowed us todetermine spectroscopic classes for a total of 46 novae, more than doubling the numberpreviously available. Specifically, after combining our data with published spectra, we havenow been able to compile a list of spectroscopic classes for a total of 91 novae that eruptedprior to 2010. In addition, we have undertaken photometric observations of many of therecent novae in this group in order to measure their light curves (i.e., their peak brightnessand rate of decline). Whenever possible, we have augmented our photometric observationswith light-curve data from the literature.Our combined spectroscopic and photometric survey has allowed us to explore the spatialdistribution of novae in M31 to a greater extent than has been possible previously. Ananalysis of these data has enabled us to arrive at the following conclusions. • As part of this survey we have found that ∼
80% of the M31 novae with available spectrabelong to the Fe II class. The remaining ∼
20% are composed of novae whose spectra arecharacterized by H, He, and N emission lines, with Fe II emission features either weak orabsent. Usually these latter systems display relatively broad (FWHM ∼ > − ) linestypical of the He/N spectroscopic class; however, a small fraction of these systems (e.g.,M31N 2007-10a, 2007-10b, and 2007-11b) are characterized by relatively narrow line widths(FWHM ∼ < − ). We refer to the latter systems as narrow-line He/N, or He/Nn,novae. The relative percentages of Fe II and He/N (and related) novae are similar to thosefound for Galactic novae (Shafter 2007; Della Valle & Livio 1998). • We have presented photometric observations with sufficient coverage to determine light-curve parameters (peak brightness and rate of decline) for most of the novae in our spec-troscopic survey, and for approximately half of all novae with known spectroscopic classifi-cations. These data have allowed us to confirm that novae in the He/N and He/Nn classeshave generally faster light-curve evolution than the more common Fe II objects. When thelight-curve parameters for the entire sample are considered, we find that the brighter novaegenerally fade the fastest; they are consistent with an MMRD relation. Similarly, we findthat the ejection velocities inferred from line widths are higher for the faster novae, as is thecase for their Galactic counterparts. • Under the assumption that there exist two separate populations of novae (bulge and diskpopulations), it is believed that the disk population, with their generally more massive whitedwarfs, should produce novae that are on average brighter and faster than their counterparts 26 –in the bulge population (Duerbeck 1990; Della Valle et al. 1992). To test this predictionfurther, we have explored the photometric behavior (specifically t ) of novae as a function ofspatial position in M31. After supplementing photometric data from our survey with declinerates from the “high quality” light-curve sample given by Capaccioli et al. (1989), we wereable to generate a sample of 74 M31 novae with well-determined fade rates. This samplewas subsequently divided into two groups: those with t ≤
25 days (the “fast” sample) andthose with t >
25 days (the “slow” sample). A comparison of the spatial distributions forthe two samples shows that the fast novae are in fact more spatially extended from the coreof M31 than the slow novae, as expected in the two-population scenario. • We have also explored the possibility that the spectroscopic class of M31 novae varieswith spatial position in the galaxy, as would be expected if the He/N and related novaecontain more massive white dwarfs. Surprisingly, as shown in Figures 21 and 22, the spatialdistribution shows only a hint that Fe II objects may be more centrally concentrated (i.e.,associated with the bulge of M31), and there is no compelling evidence for a dependence onspectroscopic class. Specifically, a KS test shows a 81% probability that the Fe II and He/Ndistributions would differ more than what is observed if they were drawn from the sameoverall distribution. This result suggests that the average white dwarf mass in nova systemsmay not be as strongly dependent on spatial position (and hence stellar population) in M31as suggested by the photometric data.Taken together, our spectroscopic and photometric data do not provide compelling ev-idence in support of the hypothesis that there exist two populations of novae in M31. Nev-ertheless, our light-curve data can be interpreted as mildly suggestive of a weak dependenceof nova-speed class on spatial position (stellar population) within the galaxy. Furthermore,our spectra are not inconsistent with the possibility that spectroscopic type may be sensitiveto stellar population. Whatever sensitivity there may be, however, appears to be weak, if itexists at all.A major step forward in the understanding of nova populations generally, and the spec-troscopic classification specifically, will likely require additional spectra and light-curve datafor novae erupting in galaxies spanning a range of morphological types. For example, a sam-ple of light curves and spectra from novae arising in the extreme Population II environmentof an elliptical galaxy will be particularly instructive. The Large Synoptic Survey Telescope,when it becomes operational, will generate a large sample of Virgo cluster nova light curvesthat will undoubtedly shed new light on the question of nova populations. Spectra of novaein Virgo cluster galaxies can then be obtained with low-resolution spectrographs currentlyavailable on 10-m class telescopes. 27 –The work presented here was made possible through observations obtained from facilitiesbased throughout the world. Spectra were obtained with the Lick Observatory Shane 3-mtelescope operated by the University of California and with the Marcario Low-ResolutionSpectrograph on the Hobby-Eberly Telescope, which is operated by McDonald Observa-tory on behalf of the University of Texas at Austin, the Pennsylvania State University,Stanford University, the Ludwig-Maximillians-Universit¨at, Munich, and the George-August-Universit´at, G¨ottingen. Photometric observations were made using the Liverpool Telescope,which is operated on the island of La Palma by Liverpool John Moores University (LJMU)in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica deCanarias with financial support from the UK Science and Technology Facilities Council.Faulkes Telescope North (FTN) is operated by the Las Cumbres Observatory Global Tele-scope network. Data from FTN were obtained as part of a joint programme between LasCumbres Observatory and the LJMU Astrophysics Research Institute. Photometric observa-tions were also obtained at the Centro Astron´omico Hispano Alem´an (CAHA) Observatoryat Calar Alto, operated jointly by the Max-Planck Institut f¨ur Astronomie and the Institutode Astrof´ısica de Andaluc´ıa (CSIC), with the 6-m telescope of the Special AstrophysicalObservatory (SAO) of the Russian Academy of Sciences (RAS), operated under the financialsupport of the Science Department of Russia (registration number 01-43), with the VaticanAdvanced Technology Telescope (the Alice P. Lennon Telescope and the Thomas J. BannanAstrophysics Facility), with the 1.3-m McGraw-Hill and the 2.4-m Hiltner telescopes at theMDM Observatory, with the 2.5-m Isaac Newton Telescope operated on the island of LaPalma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachosof the Instituto de Astrofsica de Canarias, with the 2.1-m telescope of the Kitt Peak NationalObservatory, National Optical Astronomy Observatory, which is operated by the Associa-tion of Universities for Research in Astronomy (AURA), Inc., under cooperative agreementwith the National Science Foundation, and with the 0.84-m telescope of the ObservatorioAstron´omico Nacional, San Pedro M´artir. We wish to thank the staff of all these facilitiesfor their assistance in obtaining the observations reported here.Finally, we would like to thank the following individuals for contributing images ofM31: V. L. Afanasiev, Z. Bardon, M. Burleigh, P. Cagaˇs, S. Casewell, S. N. Dodonov, T.Farnham, A. Gal´ad, J. Gallagher, P. Garnavich, J. Gorosabel, T. Henych, M. Jel´ınek, A.Karska, C. Kennedy, R. Khan, P. Kub´anek, P. Kuˇsnir´ak, D. Mackey, K. Morhig, B. Mueller,O. Pejcha, J. Prieto, N. Samarasinha, L. ˇSarounov´a, P. ˇSedinov´a, O. N. Sholukhova, K.Thorne, B. Tucker, M. Tukinsk´a, A. Valeev, M. Wolf, and P. Zasche. We are also gratefulto the following for assistance with the Lick spectroscopic observations and reductions: A.Coil, R. J. Foley, M. Ganeshalingam, S. Jha, L. C. Ho, J. Hoffman, D. C. Leonard, W. Li,M. Papenkova, F. J. D. Serduke, J. C. Shields, and J. M. Silverman. Photometric reduction 28 –software was kindly provided by P. Cagaˇs (SIMS), F. Hroch (Munipack), and M. Velenand P. Pravec (Aphot). This research has made use of the SIMBAD database, operated atCDS, Strasbourg, France, and of NASA’s Astrophysics Data System Bibliographic Services.A.V.F.’s group at UC Berkeley is grateful for the financial support of the National ScienceFoundation (most recently through grant AST-0908886) and the TABASGO Foundation.A.W.S. is grateful to the University of Victoria for hospitality during a recent sabbaticalleave while this work was being completed, and to the NSF for financial support throughgrants AST-0607682 and AST-1009566. 29 –
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This preprint was prepared with the AAS L A TEX macros v5.2.
36 –Fig. 1.— Spectra of the M31 novae M31N 1990-10b, 1993-06a, 1993-08a, 1993-11c (IDuncertain; see text), and 1998-09d, taken 19, 25, 37, 9, and 9 days post discovery, respectively.All are Fe II systems with the possible exception of M31N 1993-08a, which has a broad H α emission line characteristic of the He/N novae. 37 –Fig. 2.— Spectra of the M31 novae M31N 1992-11b, 1993-10g (ID uncertain, see text), 2001-10a, 2002-08a, and 2004-08b obtained 10, 21, 17, 40, and 34 days post discovery, respectively.All are Fe II systems with the possible exception of 2002-08a, which was observed well pastmaximum light and has a spectrum similar to that of an He/Nn nova. 38 –Fig. 3.— Spectra of the M31 novae M31N 1999-06a, 1999-08f, 1999-10a, 2001-12a, and 2002-01b, taken 75, 19, 6, 58, and 35 days post discovery, respectively. All are Fe II novae withthe exception of 1999-08f, where the type is uncertain, and 2002-01b, where the broad H α line suggests that the object may be a He/N system. 39 –Fig. 4.— Spectra of the M31 novae M31N 2004-09a, 2004-11a, 2004-11b, 2005-01a, and2005-07a taken 8, 14, 14, 8, and 2 days post discovery, respectively. All are Fe II novae withthe possible exception of 2004-11b, which has a spectrum characterized by relatively broadBalmer and N III emission similar to that of an Fe IIb, or hybrid nova, and M31N 2005-07a,which might be a He/Nn system. 40 –Fig. 5.— Spectra of the M31 novae M31N 2006-09c, 2006-10a, and two observations of2006-10b taken 7, 8, 2, and 24 days post discovery, respectively. Both M31N 2006-09c andM31N 2006-10a are typical Fe II novae, while M31N 2006-10b (observed twice) is an exampleof a hybrid or Fe IIb nova. By the time of the second spectrum, M31N 2006-10b had evolvedinto a classic He/N nova. 41 –Fig. 6.— Spectra of the M31 novae M31N 2006-11a, 2006-12a, 2006-12b, and 2007-02a,taken 4, 24, 18, and 3 days post discovery, respectively. All four novae are typical membersof the Fe II class. 42 –Fig. 7.— Spectra of the M31 novae M31N 2007-02b, 2007-06b, 2007-08d and 2007-10a, taken7, 37, 21, and 14 days post discovery, respectively. M31N 2007-02b is likely to be an Fe IIsystem, although the broad component in the Balmer lines is often seen in hybrid novae.M31N 2007-06b is a He/N nova that originated in the M31 globular cluster Bol 111 (Shafter& Quimby 2007). M31N 2007-08d is a Fe II system. M31N 2007-10a is an unusual novadisplaying prominent Balmer and He I lines. The nova is not typical of either the Fe II class(no Fe II lines) or the He/N class (the lines are narrow and there is no sign of nitrogen lines).This is the prototype of our new class of the narrow-lined He novae (He/Nn). 43 –Fig. 8.— Spectra of the M31 novae M31N 2007-11b, 2007-11c, and 2007-11d (two spectra),taken 11, 5, 5, and 18 days post discovery, respectively. All are Fe II novae. M31N 2007-11dwas observed twice, shortly after eruption when the P Cyg line profiles were clearly evident,and roughly two weeks later after the continuum had faded considerably. 44 –Fig. 9.— Spectra of the M31 novae M31N 2007-11e, 2007-12a, 2007-12b, and 2007-12d,taken 8, 10, 6, and 4 days post discovery, respectively. M31N 2007-11e and M31N 2007-11aare typical Fe II novae, while M31N 2007-12b and M31N 2007-12d are both examples ofHe/N novae. 45 –Fig. 10.— Spectra of the M31 novae M31N 2008-08d (two spectra), 2008-09a, 2008-09c, and2008-10a, taken 14, 57, 10, 6, and 11 days post discovery, respectively. All four novae are ofthe Fe II spectral type. 46 –Fig. 11.— Spectra of the M31 novae M31N 2008-10b (two spectra), 2009-01a, and 2009-02a, taken 15, 20, 6, and 2 days, respectively. M31N 2008-10b is a Fe II nova that wasobserved twice. The first spectrum of M31N 2008-10b and the spectra of and M31N 2009-01a and M31N 2009-02a display P Cyg profiles indicating that they were observed shortlyafter eruption. 47 –Fig. 12.— Spectra of the M31 nova M31N 2008-11a, a classic He/N nova, taken 4 and 22 dayspost discovery. The final two objects, M31N 2007-11g and M31N 1995-11e, are examples oflong-period variable stars that were mistakenly classified as novae. 48 –Fig. 13.— Nova light curves. The uncertainties in the photometric measurements are shownas vertical bars with the following colors representing the different bandpasses: B – blue; V – green; R – dark grey; r ′ – red; i ′ – black; z ′ – light grey. Upper flux limits are indicatedby downward facing arrows. 49 –Fig. 14.— Nova light curves (continued). See Fig. 13 for details. 50 –Fig. 15.— Nova light curves (continued). See Fig. 13 for details. 51 –Fig. 16.— Nova light curves (continued). See Fig. 13 for details. 52 –Fig. 17.— Nova light curves (continued). See Fig. 13 for details. 53 –Fig. 18.— Nova light curves (continued). See Fig. 13 for details. 54 –Fig. 19.— Nova light curves (continued). See Fig. 13 for details. 55 –Fig. 20.— Nova light curves (continued). See Fig. 13 for details. 56 – -60-40-200204060 ∆ RA cos δ (arc min)-60-40-200204060 ∆ δ ( a r c m i n ) Fig. 21.— The spatial distribution of the 91 M31 novae with known spectroscopic class (seeTable 4). The Fe II and Fe II: novae are indicated by filled and open red circles, respectively.The He/N and He/N: novae are represented by filled and open blue squares, respectively.The gray ellipses represent elliptical isophotes from the surface photometry of Kent (1987). 57 – C u m u l a ti v e F r ac ti on He/NFe II0 20 40 60 80 100 120Isophotal Radius (arc min)00.20.40.60.81 C u m u l a ti v e F r ac ti on He/NFe II
Fig. 22.— The cumulative distributions of Fe II novae compared with that for He/N and re-lated novae. The top panel shows the Fe II and Fe II: systems (red) compared with the He/N+ hybrid and He/N: systems (blue). The bottom panel compares only the well-establishedFe II and He/N + hybrid novae. A KS test indicates a 81% (73% for bottom panel) prob-ability that the distributions would differ by more than they do if both distributions comefrom the same parent population. 58 –Fig. 23.— The distribution of H α emission-line FWHM values from the novae in our sample.The novae classified as He/N (cross-hatched blue histogram) are clearly segregated fromtheir Fe II counterparts (red open histogram), with the latter systems having FWHM ∼ < − . Notable exceptions are two peculiar novae classified as He/Nn for which wehave FWHM measurements that are represented by the filled region. 59 – Log [t (days)] -10-9-8-7-6-5 M B Fe IIHe/NHe/Nn
M31N 2007-10b M31N 2007-11bM31N 2007-10aM31N 2009-10bM31N 2007-11d
Fig. 24.— The B -band maximum-magnitude vs. rate-of-decline relation (MMRD) from ourphotometric survey. The Fe II, He/N, and He/Nn novae are represented by filled red circles,filled blue squares, and open blue squares, respectively. The solid line represents the best-fitrelation determined from a weighted linear least-squares analysis (Equation 1), while thedashed line represents the theoretical relation from Livio (1992). Despite the considerablescatter, the data follow the expected trend with the brightest novae generally fading thefastest. 60 – Log [t (days)] -10-9-8-7-6-5 M V Fe IIHe/NHe/Nn
M31N 2007-10b M31N 2007-11bM31N 2007-10a M31N 2009-10bM31N 2007-11d
Fig. 25.— The V -band MMRD relation from our photometric survey. The symbols have thesame meaning as in Fig. 24. The solid line is the best-fit relation given by Equation 2, whilethe dashed line represents the Galactic V -band relation from Downes & Duerbeck (2000). 61 – Log [t (days)] -10-9-8-7-6-5 M R Fe IIHe/NHe/Nn
M31N 2007-10b M31N 2007-11bM31N 2009-10bM31N 2007-11d M31N 2005-01a
Fig. 26.— The R -band MMRD relation. The symbols have the same meaning as in Fig. 24.The best-fit relation is given by Equation 3. Note the tight group of luminous Fe II novae(M31N 2005-01a, 2007-11d, and 2009-10b) with M V ∼ < − α FWHM (km/s)0.511.522.5 l og t M31N 2007-10a
Fig. 27.— The dependence of the light-curve parameter t on nova expansion velocity (asreflected by the FWHM of H α ). With the exception of M31N 2007-10a, there is a cleartrend of decreasing t with increasing H α emission-line width. The red filled circles representFe II novae, while the filled (open) blue squares represent He/N (He/Nn and He/N:) novae,respectively. The dashed line reflects the best-fit relation given in Equation 5, while thedotted line gives the Galactic relation of McLaughlin (1960). 63 – -60-40-200204060 ∆ RA cos δ (arc min)-60-40-200204060 ∆ δ ( a r c m i n ) Fig. 28.— The spatial distribution of the 47 M31 novae with measured decline rates fromour survey supplemented by 27 decline rates from the “high quality” light-curve sample fromthe Hubble, Arp, and Rosino surveys Capaccioli et al. (1989). The “very fast” and “fast”novae ( t ≤
25 days) are indicated by blue squares, with the slower novae ( t >
25 days)are indicated by red circles. The gray ellipses represent elliptical isophotes from the surfacephotometry of Kent (1987). 64 – C u m u l a ti v e F r ac ti on t < 25 dt > 25 d Fig. 29.— The cumulative distributions of the two nova samples from Figure 28. The bluedistribution represents “very fast” and “fast” novae ( t ≤
25 days), with the red distribution(broken lines) representing slower novae ( t >
25 days). A KS test indicates a 23% probabilitythat the distributions would differ by more than they do if both distributions come from thesame parent population. Thus, it appears possible that the faster novae are more extendedcompared with the slower declining systems. 65 –Table 1. Summary of Lick Spectroscopic Observations aR.A. Decl. CoverageNova (J2000.0) (J2000.0) UT Date (˚A)M31N 1990-10b 00 h m . s ◦ ′ . ′′
11 Nov. 1990 3900–7100M31N 1992-11b 00 42 36.2 41 11 54.0 18 Nov. 1992 3500–9500M31N 1993-06a 00 42 49.2 41 17 27.5 28 Jun. 1993 4200–7100M31N 1993-08a 00 42 45.1 41 14 27.0 12 Sep. 1993 3500–9500M31N 1993-10g b
00 42 47.7 41 18 01.0 08 Nov. 1993 3500–9500M31N 1993-11c b
00 42 50.1 41 17 28.0 17 Nov. 1993 4300–7100M31N 1998-09d 00 42 46.6 41 14 49.2 20 Sep. 1998 4300–7000M31N 1999-06a 00 42 49.7 41 15 05.6 10 Sep. 1999 4300–7000M31N 1999-08f 00 42 41.1 41 19 12.2 17 Sep. 1999 4300–7000M31N 1999-10a 00 42 49.7 41 16 32.0 08 Oct. 1999 4300–7000M31N 2001-10a 00 43 03.3 41 12 11.5 20 Oct. 2001 3500–9500M31N 2001-12a 00 42 41.4 41 16 24.5 11 Feb. 2002 3300–7900M31N 2002-01b 00 42 33.9 41 18 23.9 11 Feb. 2002 3300–7900M31N 2002-08a 00 42 30.92 41 06 13.1 13 Sep. 2002 3500–9500M31N 2004-08b 00 43 26.84 41 16 40.8 10 Sep. 2004 3500–9500M31N 2004-09a 00 42 40.27 41 14 42.5 10 Sep. 2004 3500–9500M31N 2004-11a 00 42 42.81 41 18 27.9 19 Nov. 2004 3500–9500M31N 2004-11b 00 43 07.45 41 18 04.7 19 Nov. 2004 3500–9500M31N 2005-01a 00 42 28.39 41 16 36.2 16 Jan. 2005 3500–9500M31N 2005-07a 00 42 50.79 41 20 39.8 01 Aug. 2005 3500–9500M31N 2008-08d 00 45 48.25 43 02 22.2 08 Sep. 2008 3500–9500 a All observations obtained with the Shane 3-m reflector. b Due to ambiguity in the data logs from November 1993, it is possible thatthe dates of observation (and thus the spectra) for these two novae are reversed.
66 –Table 2. Summary of HET Spectroscopic Observations
R.A. Decl. Exp. CoverageNova (J2000.0) (J2000.0) UT Date (sec) (˚A) WeatherM31N 1995-11e 00 h m s ◦ ′ . ′′
67 –Table 3. Photometric Observations
JD(2 , , a M31N 1999-08f1427.686 17 . ± . r ′ (29)1427.690 17 . ± . r ′ (29)1428.444 17 . ± . r ′ (29)1428.452 17 . ± . r ′ (29)1429.452 17 . ± . r ′ (29)1429.456 17 . ± . r ′ (29)1430.467 18 . ± . r ′ (29)1430.471 18 . ± . r ′ (29)1432.686 18 . ± . r ′ (29)1432.690 18 . ± . r ′ (29)1433.678 18 . ± . r ′ (29)1433.686 18 . ± . r ′ (29)1449.467 19 . ± . r ′ (29)1449.471 19 . ± . r ′ (29)1450.463 19 . ± . r ′ (29)1450.467 19 . ± . r ′ (29)1451.475 19 . ± . r ′ (29)1452.491 19 . ± . r ′ (29)1454.374 19 . ± . r ′ (29)1454.389 19 . ± . r ′ (29)1455.538 19 . ± . r ′ (29)1456.495 19 . ± . r ′ (29)1456.499 19 . ± . r ′ (29)1457.495 19 . ± . r ′ (29)1457.499 19 . ± . r ′ (29)1458.506 19 . ± . r ′ (29)1461.510 19 . ± . r ′ (29)1461.514 19 . ± . r ′ (29)1462.530 19 . ± . r ′ (29)1462.534 19 . ± . r ′ (29)1462.561 19 . ± . r ′ (29)1463.549 20 . ± . r ′ (29)1463.557 19 . ± . r ′ (29)1484.499 20 . ± . r ′ (29)1484.502 20 . ± . r ′ (29)1486.456 20 . ± . r ′ (29)1426.694 19 . ± . i ′ (29)1426.702 19 . ± . i ′ (29)1427.690 19 . ± . i ′ (29)1427.698 19 . ± . i ′ (29)1428.702 19 . ± . i ′ (29)
68 –Table 3—Continued
JD(2 , , a M31N 2001-10a2191.616 17 . ± . r ′ (29)2191.620 17 . ± . r ′ (29)2194.620 17 . ± . r ′ (29)2194.624 17 . ± . r ′ (29)2195.640 17 . ± . r ′ (29)2195.643 17 . ± . r ′ (29)2196.382 18 . ± . r ′ (29)2196.386 18 . ± . r ′ (29)2197.628 18 . ± . r ′ (29)2197.632 18 . ± . r ′ (29)2199.452 17 . ± . r ′ (29)2199.456 17 . ± . r ′ (29)2227.339 18 . ± . r ′ (29)2271.405 20 . ± . r ′ (29)2271.409 20 . ± . r ′ (29)2292.429 20 . ± . r ′ (29)2295.343 20 . ± . r ′ (29)2295.350 20 . ± . r ′ (29)2194.612 16 . ± . i ′ (29)2194.620 16 . ± . i ′ (29)2197.620 17 . ± . i ′ (29)2197.624 17 . ± . i ′ (29)2198.636 17 . ± . i ′ (29)2198.640 17 . ± . i ′ (29)2199.382 17 . ± . i ′ (29)2199.386 17 . ± . i ′ (29)2200.628 17 . ± . i ′ (29)2200.632 17 . ± . i ′ (29)2202.448 17 . ± . i ′ (29)2202.456 17 . ± . i ′ (29)2230.331 18 . ± . i ′ (29)M31N 2002-08a2490.523 17 . ± . R (2)2504.452 17 . ± . R (2)2512.360 18 . ± . R (2)2513.344 17 . ± . R (2)2516.506 18 . ± . R (32)2517.368 18 . ± . R (2)2517.560 18 . ± . R (32)
69 –Table 3—Continued
JD(2 , , a . ± . R (2)2521.433 18 . ± . R (2)2522.414 18 . ± . R (2)2524.358 18 . ± . R (32)2525.417 19 . ± . R (2)2529.435 18 . ± . R (2)2530.438 18 . ± . R (2)2530.637 18 . ± . R (32)2547.365 19 . ± . R (2)2548.505 19 . ± . R (2)M31N 2004-08b3241.563 17 . ± . V (32)3220.474 > . R (32)3221.460 19 . ± . R (2)3222.401 18 . ± . R (2)3224.497 17 . ± . R (32)3225.405 17 . ± . R (2)3225.482 17 . ± . R (32)3226.570 17 . ± . R (32)3227.505 18 . ± . R (2)3228.393 18 . ± . R (2)3228.456 17 . ± . R (2)3229.557 18 . ± . R (32)3233.443 17 . ± . R (2)3235.370 17 . ± . R (2)3236.410 17 . ± . R (2)3236.586 17 . ± . R (32)3237.375 17 . ± . R (2)3240.429 17 . ± . R (2)3241.402 17 . ± . R (2)3241.560 17 . ± . R (32)3246.342 18 . ± . R (2)3246.399 18 . ± . R (2)3249.415 18 . ± . R (2)3249.464 18 . ± . R (2)3251.518 18 . ± . R (32)3252.312 18 . ± . R (2)3252.368 18 . ± . R (2)3253.319 19 . ± . R (2)3253.558 19 . ± . R (32)3254.362 19 . ± . R (2)3255.430 19 . ± . R (2)
70 –Table 3—Continued
JD(2 , , a . ± . R (2)3257.453 18 . ± . R (2)3257.571 18 . ± . R (32)3258.363 18 . ± . R (2)3258.393 18 . ± . R (2)3259.384 18 . ± . R (2)3259.413 18 . ± . R (2)3260.385 18 . ± . R (32)3262.453 18 . ± . R (2)3265.332 19 . ± . R (2)3265.352 19 . ± . R (2)3266.335 19 . ± . R (2)3270.330 19 . ± . R (2)3275.290 19 . ± . R (2)3279.356 19 . ± . R (32)3282.281 19 . ± . R (2)3283.619 19 . ± . R (32)3288.272 19 . ± . R (2)3289.828 20 . ± . R (33)3301.408 20 . ± . R (32)M31N 2004-09a3241.560 > . R (32)3246.399 > . R (2)3249.415 18 . ± . R (2)3249.438 18 . ± . R (2)3249.452 17 . ± . R (2)3251.518 17 . ± . R (32)3252.312 17 . ± . R (2)3252.368 17 . ± . R (2)3253.319 18 . ± . R (2)3253.341 18 . ± . R (2)3253.441 18 . ± . R (2)3253.558 18 . ± . R (32)3254.362 18 . ± . R (2)3254.400 18 . ± . R (2)3255.430 18 . ± . R (2)3257.429 18 . ± . R (2)3257.453 18 . ± . R (2)3257.571 18 . ± . R (32)3258.363 18 . ± . R (2)3258.393 18 . ± . R (2)3259.384 18 . ± . R (2)3259.413 18 . ± . R (2)
71 –Table 3—Continued
JD(2 , , a . ± . R (32)3262.453 18 . ± . R (2)3262.472 18 . ± . R (2)3265.332 18 . ± . R (2)3265.352 18 . ± . R (2)3266.335 19 . ± . R (2)3270.330 18 . ± . R (2)3270.351 19 . ± . R (2)3275.290 19 . ± . R (2)3279.356 19 . ± . R (32)3279.398 19 . ± . R (2)3282.257 19 . ± . R (2)3283.619 19 . ± . R (32)3288.272 19 . ± . R (2)3288.292 20 . ± . R (2)3289.802 20 . ± . R (33)M31N 2004-11a3301.408 > . R (2)3315.347 16 . ± . R (2)3315.390 16 . ± . R (2)3317.352 17 . ± . R (2)3321.404 18 . ± . R (2)3324.305 18 . ± . R (2)3325.218 18 . ± . R (2)3334.218 19 . ± . R (2)3335.273 19 . ± . R (2)3339.296 19 . ± . R (2)3339.318 19 . ± . R (2)3342.192 19 . ± . R (32)3344.192 19 . ± . R (2)3344.214 19 . ± . R (2)3357.568 19 . ± . R (37)3358.260 20 . ± . R (32)M31N 2004-11b3381.253 19 . ± . V (32)3301.408 > . R (2)3315.347 16 . ± . R (2)3315.390 16 . ± . R (2)3317.352 17 . ± . R (2)3321.404 17 . ± . R (2)
72 –Table 3—Continued
JD(2 , , a . ± . R (2)3325.218 17 . ± . R (2)3334.218 17 . ± . R (2)3335.273 17 . ± . R (2)3339.296 17 . ± . R (2)3339.318 17 . ± . R (2)3342.172 18 . ± . R (32)3344.192 18 . ± . R (2)3344.214 18 . ± . R (2)3346.410 18 . ± . R (2)3347.344 18 . ± . R (2)3347.370 18 . ± . R (2)3348.359 18 . ± . R (2)3357.568 19 . ± . R (37)3358.260 19 . ± . R (32)3360.236 19 . ± . R (2)3361.324 19 . ± . R (2)3370.230 19 . ± . R (2)3370.267 19 . ± . R (2)3373.321 19 . ± . R (32)3377.266 19 . ± . R (32)3378.391 19 . ± . R (2)3380.426 19 . ± . R (2)3381.249 19 . ± . R (32)3381.276 19 . ± . R (2)3381.417 19 . ± . R (2)3382.219 19 . ± . R (2)3382.246 19 . ± . R (32)3384.212 19 . ± . R (2)3387.231 19 . ± . R (32)3387.400 20 . ± . R (2)3388.224 19 . ± . R (32)M31N 2005-01a3381.253 15 . ± . V (32)3382.251 15 . ± . V (32)3384.333 15 . ± . V (32)3386.305 15 . ± . V (32)3387.237 15 . ± . V (32)3388.233 15 . ± . V (32)3373.321 > . R (32)3377.266 19 . ± . R (32)3377.293 19 . ± . R (2)
73 –Table 3—Continued
JD(2 , , a . ± . R (2)3380.224 15 . ± . R (2)3380.253 15 . ± . R (2)3380.437 15 . ± . R (2)3381.249 15 . ± . R (32)3381.266 15 . ± . R (2)3381.286 15 . ± . R (2)3381.306 15 . ± . R (2)3381.408 15 . ± . R (2)3381.426 15 . ± . R (2)3382.219 15 . ± . R (2)3382.246 15 . ± . R (32)3382.257 15 . ± . R (2)3384.212 15 . ± . R (2)3384.252 15 . ± . R (2)3384.326 15 . ± . R (32)3384.405 15 . ± . R (2)3386.202 15 . ± . R (2)3386.228 15 . ± . R (2)3386.300 15 . ± . R (32)3386.424 15 . ± . R (2)3387.212 15 . ± . R (2)3387.231 15 . ± . R (32)3387.249 15 . ± . R (2)3387.400 15 . ± . R (2)3388.224 15 . ± . R (32)3390.287 15 . ± . R (2)3390.327 15 . ± . R (2)3394.234 15 . ± . R (2)3398.274 16 . ± . R (2)3401.212 17 . ± . R (2)3405.273 19 . ± . R (32)3405.633 19 . ± . R (20)3406.326 20 . ± . R (32)3407.231 > . R (2)3407.283 > . R (2)3509.952 21 . ± . R (33)3411.257 > . R (32)3532.699 21 . ± . R (38)3534.701 21 . ± . R (38)3535.681 21 . ± . R (38)3538.697 21 . ± . R (38)3541.718 21 . ± . R (38)3651.821 22 . ± . R (35)3702.638 > . R (33)
74 –Table 3—Continued
JD(2 , , a . ± . R (36)3996.839 > . R (37)3384.315 14 . ± . I (2)M31N 2005-07a3564.493 > . R (32)3575.429 > . R (2)3579.409 18 . ± . R (2)3581.419 17 . ± . R (2)3584.404 19 . ± . R (2)3587.509 19 . ± . R (32)3588.415 18 . ± . R (2)3594.390 19 . ± . R (32)3651.862 19 . ± . R (32)3702.638 20 . ± . R (33)3710.730 21 . ± . R (36)3760.586 21 . ± . R (36)3771.346 21 . ± . R (21)M31N 2006-06a3771.264 > . R (2)3771.346 > R (21)3869.565 > . R (1)3892.518 17 . ± . R (3)3899.502 18 . ± . R (1)3899.540 17 . ± . R (1)3900.502 18 . ± . R (1)3911.522 18 . ± . R (2)3921.464 19 . ± . R (2)M31N 2006-09c4256.677 > . B (30)4260.700 > . B (30)4260.705 > . V (30)3892.967 > . R (14)3991.566 > . R (4)3993.376 > . R (2)3996.404 18 . ± . R (3)3999.609 17 . ± . R (3)
75 –Table 3—Continued
JD(2 , , a . ± . R (2)4000.590 17 . ± . R (4)4001.360 17 . ± . R (2)4002.302 17 . ± . R (2)4002.329 17 . ± . R (2)4005.312 17 . ± . R (2)4007.312 17 . ± . R (2)4014.295 19 . ± . R (2)4017.258 19 . ± . R (2)4019.319 18 . ± . R (2)4024.383 19 . ± . R (2)4026.330 19 . ± . R (2)4026.364 19 . ± . R (2)4034.312 19 . ± . R (2)4260.690 > . r ′ (30)4260.695 21 . ± . i ′ (30)M31N 2006-10a4044.337 18 . ± . B (30)4050.589 19 . ± . B (30)4056.585 18 . ± . B (30)4062.606 18 . ± . B (30)4069.484 19 . ± . B (30)4071.549 19 . ± . B (30)4074.575 19 . ± . B (30)4077.542 19 . ± . B (30)4084.460 19 . ± . B (30)4092.454 19 . ± . B (30)4099.407 20 . ± . B (30)4101.393 19 . ± . B (30)4114.372 > . B (30)4120.432 > . B (30)4254.685 > . B (30)4044.334 17 . ± . V (30)4050.586 19 . ± . V (30)4056.582 18 . ± . V (30)4062.604 18 . ± . V (30)4069.481 19 . ± . V (30)4071.546 19 . ± . V (30)4074.572 19 . ± . V (30)4077.539 19 . ± . V (30)
76 –Table 3—Continued
JD(2 , , a . ± . V (30)4092.451 19 . ± . V (30)4099.404 19 . ± . V (30)4101.391 19 . ± . V (30)4114.370 > . V (30)4120.429 > . V (30)4254.692 > . V (30)3771.346 > R (21)4019.319 > . R (2)4024.383 > . R (2)4026.330 > . R (2)4031.251 19 . ± . R (2)4034.312 18 . ± . R (2)4034.470 18 . ± . R (3)4035.360 18 . ± . R (2)4043.331 17 . ± . R (2)4047.288 19 . ± . R (2)4048.324 19 . ± . R (2)4055.296 18 . ± . R (2)4055.262 18 . ± . R (23)4070.308 19 . ± . R (6)4071.385 18 . ± . R (3)4078.308 18 . ± . R (2)4078.343 18 . ± . R (2)4080.306 18 . ± . R (2)4084.212 18 . ± . R (2)4093.174 19 . ± . R (2)4096.325 19 . ± . R (2)4097.222 19 . ± . R (2)4115.194 > . R (2)4121.381 > . R (2)4122.331 > . R (2)4122.377 > . R (2)4254.671 > . r ′ (30)M31N 2006-10b4044.388 18 . ± . B (30)4049.501 19 . ± . B (30)4057.534 20 . ± . B (30)4063.463 20 . ± . B (30)4069.445 20 . ± . B (30)4072.440 > . B (30)
77 –Table 3—Continued
JD(2 , , a > . B (30)4084.411 21 . ± . B (30)4099.438 > . B (30)4106.415 > . B (30)4114.383 > . B (30)4120.458 > . B (30)4248.704 > . B (30)4049.498 20 . ± . V (30)4054.317 > . V (30)4057.531 20 . ± . V (30)4063.460 21 . ± . V (30)4069.442 > . V (30)4072.437 > . V (30)4075.470 > . V (30)4084.408 > . V (30)4099.436 > . V (30)4102.385 > . V (30)4106.412 > . V (30)4108.486 > . V (30)4114.380 > . V (30)4120.455 > . V (30)4248.709 > . V (30)4248.693 > . r ′ (30)4248.699 > . i ′ (30)M31N 2006-11a4141.368 20 . ± . B (30)4141.372 20 . ± . V (30)3771.346 > R (21)4048.324 > . R (2)4055.296 > . R (2)4070.263 16 . ± . R (6)4070.308 16 . ± . R (6)4078.308 16 . ± . R (2)4078.343 16 . ± . R (2)4080.306 16 . ± . R (2)4084.212 16 . ± . R (2)4093.174 17 . ± . R (2)4096.325 17 . ± . R (2)
78 –Table 3—Continued
JD(2 , , a . ± . R (2)4115.194 18 . ± . R (2)4121.381 18 . ± . R (2)4122.331 19 . ± . R (2)4122.377 19 . ± . R (2)4126.289 19 . ± . R (2)4126.339 19 . ± . R (2)4128.275 19 . ± . R (2)4135.298 19 . ± . R (2)4135.334 19 . ± . R (2)4141.362 19 . ± . R (2)4146.295 19 . ± . R (2)4149.273 19 . ± . R (2)4166.247 19 . ± . R (1)4167.366 20 . ± . R (1)4170.264 20 . ± . R (1)4173.269 19 . ± . R (25)4174.268 > . R (2)4175.267 > . R (4)4240.561 > . R (1)4141.356 19 . ± . r ′ (30)4141.362 20 . ± . i ′ (30)M31N 2006-12a3771.346 > R (21)4078.343 > . R (2)4080.306 > . R (2)4084.212 > . R (2)4093.174 17 . ± . R (2)4096.325 17 . ± . R (2)4096.357 17 . ± . R (2)4097.222 17 . ± . R (2)4097.241 17 . ± . R (2)4115.194 18 . ± . R (2)4115.226 18 . ± . R (2)4121.381 18 . ± . R (2)4122.331 19 . ± . R (2)4122.377 19 . ± . R (2)4126.289 > . R (2)4126.339 > . R (2)4128.275 19 . ± . R (2)
79 –Table 3—Continued
JD(2 , , a M31N 2007-02b3771.346 > R (21)4128.275 > . R (2)4135.298 16 . ± . R (2)4141.362 17 . ± . R (2)4146.295 17 . ± . R (2)4149.273 17 . ± . R (2)4162.295 18 . ± . R (1)4164.263 18 . ± . R (1)4166.274 18 . ± . R (1)4170.274 19 . ± . R (1)4174.268 18 . ± . R (2)4175.267 19 . ± . R (4)4238.560 > . R (1)M31N 2007-07c3771.346 > R (21)4288.506 > . R (1)4327.469 19 . ± . R (1)4330.344 19 . ± . R (1)M31N 2007-07e3771.346 > R (21)4288.506 > . R (1)4327.469 17 . ± . R (1)4330.344 18 . ± . R (1)4343.487 18 . ± . R (4)4353.409 18 . ± . R (1)4356.430 19 . ± . R (1)4357.473 19 . ± . R (1)4358.284 19 . ± . R (1)4365.319 19 . ± . R (3)M31N 2007-08d3771.346 > R (21)4380.401 18 . ± . R (24)4380.424 18 . ± . R (24)4382.235 19 . ± . R (24)4387.219 > . R (24)4387.231 19 . ± . R (24)4387.561 19 . ± . R (1)
80 –Table 3—Continued
JD(2 , , a . ± . R (24)4388.626 19 . ± . R (1)4389.233 19 . ± . R (24)4389.646 20 . ± . R (1)M31N 2007-10a4383.529 17 . ± . B (30)4384.398 18 . ± . B (30)4387.398 18 . ± . B (30)4389.384 19 . ± . B (30)4390.355 19 . ± . B (30)4392.486 20 . ± . B (30)4393.714 21 . ± . B (30)4394.448 21 . ± . B (30)4395.553 > . B (30)4396.352 > . B (30)4397.375 > . B (30)4398.367 > . B (30)4399.380 > . B (30)4400.693 > . B (30)4402.606 > . B (30)4405.649 > . B (30)4406.679 > . B (30)4407.573 > . B (30)4410.416 > . B (30)4383.860 18 . ± . B (31)4384.846 18 . ± . B (31)4385.970 19 . ± . B (31)4386.811 18 . ± . B (31)4387.869 19 . ± . B (31)4388.786 19 . ± . B (31)4389.991 17 . ± . B (31)4390.773 19 . ± . B (31)4391.745 20 . ± . B (31)4392.739 20 . ± . B (31)4393.971 > . B (3)4394.793 > . B (31)4383.532 17 . ± . V (30)4384.401 18 . ± . V (30)4387.403 18 . ± . V (30)4389.386 19 . ± . V (30)4390.358 19 . ± . V (30)
81 –Table 3—Continued
JD(2 , , a . ± . V (30)4393.717 20 . ± . V (30)4394.451 20 . ± . V (30)4395.555 > . V (30)4396.355 > . V (30)4397.378 > . V (30)4398.370 > . V (30)4399.383 > . V (30)4400.696 > . V (30)4402.609 > . V (30)4405.652 > . V (30)4406.682 > . V (30)4407.576 > . V (30)4410.419 > . V (30)4383.862 17 . ± . V (31)4384.849 18 . ± . V (31)4385.973 18 . ± . V (31)4386.813 18 . ± . V (31)4387.872 18 . ± . V (31)4388.789 19 . ± . V (31)4389.994 18 . ± . V (31)4390.777 19 . ± . V (31)4391.748 19 . ± . V (31)4392.742 20 . ± . V (31)4393.975 > . V (31)4394.796 > . V (31)3771.346 > R (21)4388.644 18 . ± . R (1)4383.535 17 . ± . i ′ (30)4384.404 18 . ± . i ′ (30)4389.389 19 . ± . i ′ (30)4390.361 19 . ± . i ′ (30)4392.492 19 . ± . i ′ (30)4393.720 20 . ± . i ′ (30)4394.453 20 . ± . i ′ (30)4395.558 > . i ′ (30)4396.358 > . i ′ (30)4397.381 > . i ′ (30)4398.373 > . i ′ (30)4399.386 > . i ′ (30)4400.698 > . i ′ (30)4402.612 > . i ′ (30)
82 –Table 3—Continued
JD(2 , , a > . i ′ (30)4406.685 > . i ′ (30)4407.578 > . i ′ (30)4410.422 > . i ′ (30)4383.857 18 . ± . i ′ (31)4384.844 18 . ± . i ′ (31)4385.967 18 . ± . i ′ (31)4386.808 18 . ± . i ′ (31)4387.835 19 . ± . i ′ (31)4387.866 19 . ± . i ′ (31)4388.783 19 . ± . i ′ (31)4389.988 18 . ± . i ′ (31)4390.771 19 . ± . i ′ (31)4391.743 19 . ± . i ′ (31)4392.736 20 . ± . i ′ (31)4393.968 20 . ± . i ′ (31)4394.790 > . i ′ (31)4395.810 > . i ′ (31)M31N 2007-10b4389.507 19 . ± . B (30)4392.397 > . B (30)4393.519 > . B (30)4394.436 > . B (30)4395.483 > . B (30)4389.504 19 . ± . V (30)4392.394 > . V (30)4393.516 > . V (30)4394.433 > . V (30)4395.480 > . V (30)3771.346 > R (21)4382.235 > . R (1)4387.219 18 . ± . R (24)4387.561 18 . ± . R (1)4388.227 19 . ± . R (24)4388.626 19 . ± . R (1)4389.233 19 . ± . R (24)4389.646 19 . ± . R (1)4405.318 > . R (28)4409.388 > . R (1)4410.204 > . ± . R (27)
83 –Table 3—Continued
JD(2 , , a > . ± . R (27)4389.501 20 . ± . i ′ (30)4390.406 20 . ± . i ′ (30)4392.391 > . i ′ (30)4393.513 > . i ′ (30)4394.430 > . i ′ (30)4395.477 > . i ′ (30)M31N 2007-11b4418.534 19 . ± . B (30)4420.510 19 . ± . B (30)4421.434 19 . ± . B (30)4431.597 21 . ± . B (30)4432.478 20 . ± . B (30)4438.431 20 . ± . B (30)4444.422 20 . ± . B (30)4419.872 19 . ± . B (31)4421.846 19 . ± . B (31)4422.762 20 . ± . B (31)4427.856 > . B (31)4418.537 19 . ± . V (30)4420.513 19 . ± . V (30)4421.437 19 . ± . V (30)4431.602 20 . ± . V (30)4432.481 20 . ± . V (30)4438.434 20 . ± . V (30)4441.433 19 . ± . V (30)4444.424 20 . ± . V (30)4419.874 19 . ± . V (31)4421.849 19 . ± . V (31)4422.765 19 . ± . V (31)4427.859 20 . ± . V (31)3771.346 > . R (21)4415.446 18 . ± . R (1)4416.223 18 . ± . R (1)4453.263 19 . ± . R (1)4418.540 19 . ± . i ′ (30)4420.516 19 . ± . i ′ (30)
84 –Table 3—Continued
JD(2 , , a . ± . i ′ (30)4431.607 19 . ± . i ′ (30)4432.484 19 . ± . i ′ (30)4438.437 19 . ± . i ′ (30)4441.436 19 . ± . i ′ (30)4444.427 20 . ± . i ′ (30)4419.877 19 . ± . i ′ (31)4421.852 19 . ± . i ′ (31)4422.768 19 . ± . i ′ (31)4427.862 19 . ± . i ′ (31)4428.758 19 . ± . i ′ (31)4430.869 19 . ± . i ′ (31)4436.765 19 . ± . i ′ (31)M31N 2007-11c4419.883 16 . ± . B (31)4420.536 16 . ± . B (30)4421.447 16 . ± . B (30)4421.858 16 . ± . B (31)4422.774 17 . ± . B (31)4427.868 > . B (31)4430.875 > . B (31)4432.385 18 . ± . B (30)4436.771 19 . ± . B (30)4438.418 19 . ± . B (30)4441.397 19 . ± . B (30)4443.534 > . B (30)4449.347 20 . ± . B (30)4419.886 16 . ± . V (31)4420.539 16 . ± . V (30)4421.450 17 . ± . V (30)4421.860 17 . ± . V (31)4422.776 17 . ± . V (31)4427.870 > . V (31)4428.767 > . V (31)4429.766 18 . ± . V (31)4430.878 18 . ± . V (31)4432.388 18 . ± . V (30)4436.773 19 . ± . V (31)4438.421 19 . ± . V (30)4441.400 19 . ± . V (30)4443.537 > . V (30)
85 –Table 3—Continued
JD(2 , , a . ± . V (30)3771.346 > . R (21)4415.475 > . R (1)4416.387 19 . ± . R (1)4417.547 17 . ± . R (1)4445.234 19 . ± . R (1)4419.888 17 . ± . i ′ (31)4420.542 17 . ± . i ′ (30)4421.453 17 . ± . i ′ (30)4421.863 17 . ± . i ′ (31)4422.779 17 . ± . i ′ (31)4427.873 > . i ′ (31)4429.769 19 . ± . i ′ (31)4432.391 19 . ± . i ′ (30)4438.424 19 . ± . i ′ (30)4443.540 > . i ′ (30)4449.352 > . i ′ (30)M31N 2007-11d4427.880 16 . ± . B (30)4428.780 16 . ± . B (30)4429.770 16 . ± . B (30)4432.470 16 . ± . B (31)4436.580 17 . ± . B (31)4436.780 17 . ± . B (30)4439.370 20 . ± . B (31)4443.330 21 . ± . B (31)4427.880 16 . ± . V (30)4428.780 16 . ± . V (30)4429.780 16 . ± . V (30)4432.470 16 . ± . V (31)4436.590 17 . ± . V (31)4436.780 17 . ± . V (30)4439.370 20 . ± . V (31)4443.340 21 . ± . V (31)4427.880 15 . ± . i ′ (30)4428.780 15 . ± . i ′ (30)4429.780 16 . ± . i ′ (30)4432.470 16 . ± . i ′ (31)4436.590 17 . ± . i ′ (31)
86 –Table 3—Continued
JD(2 , , a . ± . i ′ (30)4439.380 18 . ± . i ′ (31)4443.340 20 . ± . i ′ (31)4449.340 20 . ± . i ′ (31)M31N 2007-12a4449.415 18 . ± . B (30)4451.434 17 . ± . B (30)4455.392 17 . ± . B (30)4459.390 18 . ± . B (30)4460.344 18 . ± . B (30)4461.386 18 . ± . B (30)4463.473 18 . ± . B (30)4466.335 18 . ± . B (30)4467.367 18 . ± . B (30)4468.388 18 . ± . B (30)4469.432 19 . ± . B (30)4471.343 19 . ± . B (30)4473.862 19 . ± . B (31)4474.413 19 . ± . B (30)4474.732 19 . ± . B (31)4474.741 19 . ± . B (31)4449.418 17 . ± . V (30)4451.437 17 . ± . V (30)4455.395 17 . ± . V (30)4459.393 18 . ± . V (30)4460.347 18 . ± . V (30)4461.389 18 . ± . V (30)4463.476 18 . ± . V (30)4466.338 18 . ± . V (30)4467.370 18 . ± . V (30)4468.391 18 . ± . V (30)4469.435 19 . ± . V (30)4471.346 19 . ± . V (30)4473.865 19 . ± . V (31)4474.416 19 . ± . V (30)4474.734 19 . ± . V (31)4474.744 19 . ± . V (31)4449.421 17 . ± . i ′ (30)4451.439 17 . ± . i ′ (30)4455.398 17 . ± . i ′ (30)4459.396 17 . ± . i ′ (30)
87 –Table 3—Continued
JD(2 , , a . ± . i ′ (30)4461.392 17 . ± . i ′ (30)4463.479 18 . ± . i ′ (30)4466.341 18 . ± . i ′ (30)4467.373 18 . ± . i ′ (30)4468.394 18 . ± . i ′ (30)4469.437 18 . ± . i ′ (30)4471.349 18 . ± . i ′ (30)4473.868 18 . ± . i ′ (31)4474.419 18 . ± . i ′ (30)4474.747 18 . ± . i ′ (31)M31N 2007-12b4449.440 19 . ± . B (30)4452.350 19 . ± . B (30)4455.400 20 . ± . B (30)4459.400 20 . ± . B (30)4460.390 21 . ± . B (30)4461.510 > . B (30)4464.520 21 . ± . B (30)4467.350 > . B (30)4468.400 > . B (30)4469.460 > . B (30)4470.440 > . B (30)4472.480 > . B (30)4449.450 19 . ± . V (30)4452.350 19 . ± . V (30)4455.410 20 . ± . V (30)4459.410 20 . ± . V (30)4460.390 > . V (30)4461.510 > . V (30)4464.520 > . V (30)4467.350 > . V (30)4468.400 > . V (30)4469.470 > . V (30)4470.450 > . V (30)4472.480 > . V (30)3771.346 > . R (21)4417.547 > . R (1)4445.234 17 . ± . R (1)4450.392 18 . ± . R (1)4450.402 18 . ± . R (1)
88 –Table 3—Continued
JD(2 , , a . ± . R (1)4449.450 18 . ± . i ′ (30)4452.360 19 . ± . i ′ (30)4455.410 > . i ′ (30)4459.410 > . i ′ (30)4460.390 > . i ′ (30)M31N 2007-12d3771.346 > . R (21)4453.238 17 . ± . R (1)M31N 2008-05c4528.246 > . R (1)4601.558 > . R (28)4617.523 17 . ± . R (1)4617.549 17 . ± . R (1)4619.529 17 . ± . R (1)4619.554 17 . ± . R (1)4620.543 17 . ± . R (1)4628.541 18 . ± . R (3)4645.550 19 . ± . R (1)4646.535 19 . ± . R (1)4647.492 19 . ± . R (1)4648.557 19 . ± . R (1)4655.567 19 . ± . R (3)4675.581 19 . ± . R (3)4677.432 19 . ± . R (1)4678.562 19 . ± . R (1)4679.551 19 . ± . R (1)4682.379 19 . ± . R (1)4682.574 19 . ± . R (1)4683.562 19 . ± . R (1)4685.548 20 . ± . R (1)4692.616 > . R (28)4697.573 20 . ± . R (3)4706.362 19 . ± . R (1)4712.608 > . R (1)M31N 2008-06b4505.226 > . R (1)4620.542 > . R (1)
89 –Table 3—Continued
JD(2 , , a > . R (3)4644.498 16 . ± . R (5)4645.489 16 . ± . R (1)4645.529 16 . ± . R (1)4645.550 16 . ± . R (1)4646.535 16 . ± . R (1)4647.492 16 . ± . R (1)4648.557 16 . ± . R (1)4652.560 17 . ± . R (3)4655.567 17 . ± . R (3)4675.581 18 . ± . R (3)4677.432 18 . ± . R (1)4678.562 18 . ± . R (1)4679.551 19 . ± . R (1)4681.370 19 . ± . R (1)4682.379 19 . ± . R (1)4682.574 19 . ± . R (1)4683.562 19 . ± . R (1)4685.548 19 . ± . R (1)4692.616 > . R (28)4697.573 20 . ± . R (3)4706.362 > . R (1)M31N 2008-07a5095.981 21 . ± . > . R (1)4617.523 > . R (1)4619.529 19 . ± . R (1)4620.542 18 . ± . R (1)4628.541 19 . ± . R (3)4645.488 19 . ± . R (1)4646.535 19 . ± . R (1)4647.492 18 . ± . R (1)4648.557 19 . ± . R (1)4655.567 19 . ± . R (3)4675.581 19 . ± . R (3)4677.432 18 . ± . R (1)4678.562 18 . ± . R (1)4679.551 18 . ± . R (1)4681.370 19 . ± . R (1)4682.379 19 . ± . R (1)4682.574 19 . ± . R (1)4683.562 19 . ± . R (1)
90 –Table 3—Continued
JD(2 , , a . ± . R (1)4685.548 18 . ± . R (1)4692.616 18 . ± . R (28)4697.573 19 . ± . R (3)4706.362 19 . ± . R (1)4708.387 18 . ± . R (1)4709.613 19 . ± . R (1)4710.589 19 . ± . R (1)4711.310 18 . ± . R (1)4712.291 19 . ± . R (1)4712.337 18 . ± . R (1)4712.608 18 . ± . R (1)4713.343 19 . ± . R (1)4715.330 18 . ± . R (1)4716.334 18 . ± . R (1)4718.378 19 . ± . R (3)4719.299 19 . ± . R (3)4738.221 18 . ± . R (3)4744.604 19 . ± . R (1)4745.257 19 . ± . R (1)4748.472 19 . ± . R (7)4748.485 19 . ± . R (7)4754.400 19 . ± . R (3)4760.628 19 . ± . R (3)4763.219 19 . ± . R (1)4765.545 19 . ± . R (1)4772.448 19 . ± . R (1)4774.545 19 . ± . R (1)4776.228 19 . ± . R (1)4777.215 19 . ± . R (1)4779.283 19 . ± . R (1)4779.318 19 . ± . R (1)4800.301 19 . ± . R (1)4801.226 18 . ± . R (1)4809.285 19 . ± . R (1)4982.972 > . R (9)5095.968 20 . ± . R (13)M31N 2008-07b4505.226 > . R (1)4655.567 > . R (3)4675.581 18 . ± . R (3)4677.432 18 . ± . R (1)4677.448 18 . ± . R (1)
91 –Table 3—Continued
JD(2 , , a . ± . R (1)4679.551 18 . ± . R (1)4681.370 19 . ± . R (1)4682.379 19 . ± . R (1)4682.550 19 . ± . R (1)4682.574 19 . ± . R (1)4683.562 19 . ± . R (1)4684.525 19 . ± . R (1)4685.548 19 . ± . R (1)4685.564 19 . ± . R (1)4685.577 19 . ± . R (1)4692.616 19 . ± . R (28)4697.573 20 . ± . R (3)4706.362 20 . ± . R (1)4708.424 20 . ± . R (1)4710.323 > . R (1)4711.335 20 . ± . R (1)4712.608 20 . ± . R (1)4713.343 20 . ± . R (1)4715.330 20 . ± . R (1)M31N 2008-08a4685.548 > . R (1)4692.616 16 . ± . R (28)4697.573 17 . ± . R (3)4706.362 18 . ± . R (1)4706.627 18 . ± . R (1)4708.387 18 . ± . R (1)4709.613 18 . ± . R (1)4710.589 19 . ± . R (1)4711.310 18 . ± . R (1)4712.291 19 . ± . R (1)4712.608 19 . ± . R (1)4713.343 18 . ± . R (1)4715.330 18 . ± . R (1)M31N 2008-08b4685.548 > . R (1)4692.616 17 . ± . R (28)4697.573 19 . ± . R (3)M31N 2008-09a
92 –Table 3—Continued
JD(2 , , a . ± . R (1)M31N 2008-10a4778.655 19 . ± . B (30)4778.727 19 . ± . B (31)4779.967 > . B (31)4779.637 20 . ± . B (30)4780.463 20 . ± . B (30)4781.491 > . B (30)4782.449 19 . ± . B (30)4783.360 > . B (30)4785.451 19 . ± . B (30)4786.404 > . B (30)4787.479 19 . ± . B (30)4788.455 19 . ± . B (30)4789.403 19 . ± . B (30)4778.658 19 . ± . V (30)4778.732 19 . ± . V (31)4779.641 19 . ± . V (30)4779.972 19 . ± . V (31)4780.466 20 . ± . V (30)4780.900 18 . ± . V (31)4781.495 > . V (30)4782.453 19 . ± . V (30)4783.364 19 . ± . V (30)4785.456 19 . ± . V (30)4786.407 19 . ± . V (30)4787.483 19 . ± . V (30)4788.458 19 . ± . V (30)4789.406 19 . ± . V (30)4775.921 17 . ± . r ′ (31)4777.861 17 . ± . r ′ (31)4778.644 18 . ± . r ′ (30)4778.712 18 . ± . r ′ (31)4779.626 18 . ± . r ′ (30)4779.952 18 . ± . r ′ (31)4780.452 18 . ± . r ′ (30)4780.877 18 . ± . r ′ (31)4781.480 17 . ± . r ′ (30)4782.438 18 . ± . r ′ (30)4783.349 18 . ± . r ′ (30)4785.440 18 . ± . r ′ (30)
93 –Table 3—Continued
JD(2 , , a . ± . r ′ (30)4787.468 18 . ± . r ′ (30)4788.444 18 . ± . r ′ (30)4789.392 18 . ± . r ′ (30)M31N 2008-10b4716.407 > . R (1)4748.479 19 . ± . R (4)4754.419 19 . ± . R (3)4763.218 18 . ± . R (1)4765.546 19 . ± . R (1)4772.448 19 . ± . R (1)4774.571 19 . ± . R (1)4776.228 18 . ± . R (1)4777.229 18 . ± . R (1)4779.283 19 . ± . R (1)4795.192 19 . ± . V (1)4798.431 18 . ± . V (5)4799.199 18 . ± . R (1)4800.301 18 . ± . R (1)4801.267 18 . ± . R (1)4809.285 18 . ± . R (1)4829.183 19 . ± . R (1)4760.472 18 . ± . B (30)4761.514 17 . ± . B (30)4764.549 19 . ± . B (30)4777.584 18 . ± . B (30)4778.441 19 . ± . B (30)4779.485 19 . ± . B (30)4780.429 19 . ± . B (30)4781.435 19 . ± . B (30)4782.461 > . B (30)4783.401 > . B (30)4785.495 18 . ± . B (30)4786.422 18 . ± . B (30)4787.370 19 . ± . B (30)4788.467 19 . ± . B (30)4789.418 18 . ± . B (30)4790.383 19 . ± . B (30)4760.793 17 . ± . B (31)4761.793 17 . ± . B (31)4762.894 > . B (31)
94 –Table 3—Continued
JD(2 , , a . ± . B (31)4763.740 19 . ± . B (31)4763.793 19 . ± . B (31)4764.919 > . B (31)4771.889 19 . ± . B (31)4772.862 19 . ± . B (31)4773.835 19 . ± . B (31)4774.842 19 . ± . B (31)4777.843 18 . ± . B (31)4779.922 19 . ± . B (31)4780.835 > . B (31)4760.476 18 . ± . V (30)4761.517 17 . ± . V (30)4764.553 19 . ± . V (30)4777.588 18 . ± . V (30)4778.444 18 . ± . V (30)4779.487 19 . ± . V (30)4780.433 19 . ± . V (30)4781.438 19 . ± . V (30)4782.465 19 . ± . V (30)4783.405 > . V (30)4785.499 18 . ± . V (30)4786.426 18 . ± . V (30)4787.374 19 . ± . V (30)4788.471 19 . ± . V (30)4789.421 18 . ± . V (30)4790.387 19 . ± . V (30)4760.796 17 . ± . V (31)4761.796 17 . ± . V (31)4762.895 17 . ± . V (31)4763.730 18 . ± . V (31)4763.743 18 . ± . V (31)4763.796 19 . ± . V (31)4764.923 > . V (31)4771.892 19 . ± . V (31)4772.865 20 . ± . V (31)4773.837 19 . ± . V (31)4774.845 19 . ± . V (31)4777.846 18 . ± . V (31)4779.925 19 . ± . V (31)4780.838 > . V (31)4760.478 18 . ± . r ′ (30)
95 –Table 3—Continued
JD(2 , , a . ± . r ′ (30)4764.556 19 . ± . r ′ (30)4777.591 18 . ± . r ′ (30)4778.448 19 . ± . r ′ (30)4779.492 19 . ± . r ′ (30)4780.437 19 . ± . r ′ (30)4781.442 > . r ′ (30)4782.469 > . r ′ (30)4783.409 > . r ′ (30)4785.503 18 . ± . r ′ (30)4786.430 18 . ± . r ′ (30)4787.378 19 . ± . r ′ (30)4788.474 19 . ± . r ′ (30)4789.425 18 . ± . r ′ (30)4790.391 19 . ± . r ′ (30)4760.799 18 . ± . r ′ (31)4761.799 17 . ± . r ′ (31)4762.898 18 . ± . r ′ (31)4763.733 18 . ± . r ′ (31)4763.799 18 . ± . r ′ (31)4764.925 19 . ± . r ′ (31)4771.895 19 . ± . r ′ (31)4772.868 19 . ± . r ′ (31)4773.841 19 . ± . r ′ (31)4774.848 19 . ± . r ′ (31)4777.850 18 . ± . r ′ (31)4779.928 19 . ± . r ′ (31)4780.841 18 . ± . r ′ (31)M31N 2008-11a4778.400 19 . ± . B (30)4779.472 19 . ± . B (30)4779.891 19 . ± . B (31)4780.486 19 . ± . B (30)4780.907 20 . ± . B (31)4782.418 20 . ± . B (30)4783.496 > . B (30)4785.529 20 . ± . B (30)4786.490 > . B (30)4787.404 20 . ± . B (30)4788.428 20 . ± . B (30)4789.503 20 . ± . B (30)4794.344 20 . ± . B (30)
96 –Table 3—Continued
JD(2 , , a > . B (30)4796.581 > . B (30)4799.384 21 . ± . B (30)4800.470 > . B (30)4802.396 > . B (30)4805.339 > . B (30)4805.395 > . B (30)4778.404 18 . ± . V (30)4779.476 19 . ± . V (30)4779.896 19 . ± . V (31)4780.489 19 . ± . V (30)4780.912 > . V (31)4781.472 19 . ± . V (30)4782.422 19 . ± . V (30)4783.499 > . V (30)4785.532 20 . ± . V (30)4786.494 > . V (30)4787.407 20 . ± . V (30)4788.432 20 . ± . V (30)4789.508 20 . ± . V (30)4794.348 21 . ± . V (30)4795.482 20 . ± . V (30)4796.585 > . V (30)4799.387 20 . ± . V (30)4800.474 > . V (30)4800.498 > . V (30)4802.400 21 . ± . V (30)4805.399 > . V (30)4744.340 > . R (1)4775.218 16 . ± . R (1)4776.217 17 . ± . R (1)4779.260 18 . ± . R (1)4780.234 18 . ± . R (1)4800.310 > . R (1)4778.389 17 . ± . r ′ (30)4779.461 18 . ± . r ′ (30)4779.901 18 . ± . r ′ (31)4780.475 18 . ± . r ′ (30)4780.917 18 . ± . r ′ (31)4782.407 18 . ± . r ′ (30)4783.485 18 . ± . r ′ (30)4785.518 19 . ± . r ′ (30)
97 –Table 3—Continued
JD(2 , , a . ± . r ′ (30)4787.393 19 . ± . r ′ (30)4788.418 19 . ± . r ′ (30)4789.492 20 . ± . r ′ (30)4790.412 19 . ± . r ′ (30)4794.333 20 . ± . r ′ (30)4795.467 20 . ± . r ′ (30)4796.570 > . r ′ (30)4799.373 20 . ± . r ′ (30)4800.403 20 . ± . r ′ (30)4800.459 20 . ± . r ′ (30)4802.385 21 . ± . r ′ (30)4803.398 > . r ′ (30)4805.328 21 . ± . r ′ (30)4805.384 21 . ± . r ′ (30)4778.393 18 . ± . i ′ (30)4779.465 18 . ± . i ′ (30)4779.906 18 . ± . i ′ (31)4780.478 19 . ± . i ′ (30)4780.922 19 . ± . i ′ (31)4782.411 19 . ± . i ′ (30)4783.489 > . i ′ (30)4785.521 20 . ± . i ′ (30)4786.483 > . i ′ (30)4787.396 20 . ± . i ′ (30)4788.421 20 . ± . i ′ (30)4789.497 21 . ± . i ′ (30)4790.415 20 . ± . i ′ (30)4794.337 20 . ± . i ′ (30)4795.471 20 . ± . i ′ (30)4796.574 > . i ′ (30)4799.376 21 . ± . i ′ (30)4800.464 20 . ± . i ′ (30)4802.389 21 . ± . i ′ (30)4803.401 > . i ′ (30)4805.331 > . i ′ (30)4805.388 > . i ′ (30)4778.396 17 . ± . z ′ (30)4779.468 18 . ± . z ′ (30)4780.482 18 . ± . z ′ (30)4781.465 > . z ′ (30)4782.414 19 . ± . z ′ (30)4783.492 19 . ± . z ′ (30)
98 –Table 3—Continued
JD(2 , , a . ± . z ′ (30)4786.486 > . z ′ (30)4787.400 > . z ′ (30)4788.425 20 . ± . z ′ (30)4789.499 20 . ± . z ′ (30)4790.419 > . z ′ (30)4794.340 > . z ′ (30)4795.474 > . z ′ (30)4796.578 > . z ′ (30)M31N 2008-12b4842.404 17 . ± . B (30)4846.474 17 . ± . B (30)4851.347 17 . ± . B (30)4856.441 18 . ± . B (30)4859.377 19 . ± . B (30)4842.408 17 . ± . V (30)4846.478 17 . ± . V (30)4851.351 17 . ± . V (30)4856.444 18 . ± . V (30)4859.381 19 . ± . V (30)4829.183 > . R (1)4840.253 17 . ± . R (4)4848.217 17 . ± . R (11)4851.394 17 . ± . R (1)4842.394 17 . ± . r ′ (30)4846.464 17 . ± . r ′ (30)4851.337 17 . ± . r ′ (30)4856.430 18 . ± . r ′ (30)4859.366 19 . ± . r ′ (30)4842.397 17 . ± . i ′ (30)4846.467 17 . ± . i ′ (30)4851.340 17 . ± . i ′ (30)4856.433 18 . ± . i ′ (30)4859.370 18 . ± . i ′ (30)4842.400 16 . ± . z ′ (30)4846.471 16 . ± . z ′ (30)4851.344 17 . ± . z ′ (30)4856.437 17 . ± . z ′ (30)
99 –Table 3—Continued
JD(2 , , a . ± . z ′ (30)M31N 2009-01a4872.241 > . R (11)M31N 2009-02a4872.254 16 . ± . R (11)M31N 2009-08a5053.724 17 . ± . B (30)5057.516 18 . ± . B (30)5058.498 18 . ± . B (30)5059.719 18 . ± . B (30)5060.533 18 . ± . B (30)5061.484 18 . ± . B (30)5061.562 18 . ± . B (30)5062.507 18 . ± . B (30)5063.485 18 . ± . B (30)5064.630 17 . ± . B (30)5065.739 17 . ± . B (30)5066.525 17 . ± . B (30)5067.474 17 . ± . B (30)5069.678 18 . ± . B (30)5070.586 18 . ± . B (30)5071.746 > . B (30)5072.526 18 . ± . B (30)5073.467 18 . ± . B (30)5075.501 18 . ± . B (30)5076.459 18 . ± . B (30)5077.718 18 . ± . B (30)5077.487 18 . ± . B (30)5078.572 17 . ± . B (30)5079.469 17 . ± . B (30)5114.306 19 . ± . B (17)5053.729 17 . ± . V (30)5057.520 18 . ± . V (30)5058.501 18 . ± . V (30)5059.723 18 . ± . V (30)5060.536 18 . ± . V (30)5061.488 18 . ± . V (30)5061.566 18 . ± . V (30)
100 –Table 3—Continued
JD(2 , , a . ± . V (30)5063.489 18 . ± . V (30)5064.633 18 . ± . V (30)5065.742 17 . ± . V (30)5066.528 17 . ± . V (30)5067.478 18 . ± . V (30)5069.681 18 . ± . V (30)5070.590 19 . ± . V (30)5071.749 > . V (30)5072.529 18 . ± . V (30)5073.470 18 . ± . V (30)5074.483 18 . ± . V (30)5075.504 18 . ± . V (30)5076.463 18 . ± . V (30)5077.721 18 . ± . V (30)5077.490 18 . ± . V (30)5078.575 18 . ± . V (30)5079.472 17 . ± . V (30)5092.525 18 . ± . V (17)5095.981 18 . ± . V (13)5114.308 20 . ± . V (17)4985.974 > . R (9)4988.527 > . R (1)5055.923 18 . ± . R (8)5063.605 18 . ± . R (22)5073.441 18 . ± . R (1)5074.366 18 . ± . R (1)5075.384 18 . ± . R (1)5076.478 17 . ± . R (1)5080.413 17 . ± . R (1)5081.393 18 . ± . R (1)5083.357 18 . ± . R (1)5084.267 18 . ± . R (1)5094.451 18 . ± . R (3)5095.968 18 . ± . R (13)5114.304 19 . ± . R (17)5114.486 19 . ± . R (3)5124.491 19 . ± . R (3)5135.632 19 . ± . R (12)5140.546 19 . ± . R (1)5141.359 19 . ± . R (1)5148.536 19 . ± . R (1)5162.281 19 . ± . R (5)5168.173 19 . ± . R (7)
101 –Table 3—Continued
JD(2 , , a . ± . R (1)5181.226 19 . ± . R (1)5184.717 19 . ± . R (19)5199.299 20 . ± . R (12)5227.345 20 . ± . R (12)5228.383 20 . ± . R (12)5050.721 18 . ± . r ′ (30)5052.551 18 . ± . r ′ (30)5052.556 18 . ± . r ′ (30)5052.570 18 . ± . r ′ (30)5052.585 18 . ± . r ′ (30)5052.591 18 . ± . r ′ (30)5052.605 18 . ± . r ′ (30)5052.620 18 . ± . r ′ (30)5052.626 18 . ± . r ′ (30)5052.640 18 . ± . r ′ (30)5052.652 18 . ± . r ′ (30)5052.660 18 . ± . r ′ (30)5052.682 18 . ± . r ′ (30)5052.711 18 . ± . r ′ (30)5052.721 18 . ± . r ′ (30)5052.728 18 . ± . r ′ (30)5053.716 18 . ± . r ′ (30)5053.505 18 . ± . r ′ (30)5053.509 18 . ± . r ′ (30)5053.514 18 . ± . r ′ (30)5053.528 18 . ± . r ′ (30)5053.532 18 . ± . r ′ (30)5053.537 18 . ± . r ′ (30)5053.541 18 . ± . r ′ (30)5054.478 18 . ± . r ′ (30)5056.718 18 . ± . r ′ (30)5057.510 18 . ± . r ′ (30)5058.491 18 . ± . r ′ (30)5059.713 18 . ± . r ′ (30)5060.526 18 . ± . r ′ (30)5061.478 18 . ± . r ′ (30)5061.555 18 . ± . r ′ (30)5062.501 18 . ± . r ′ (30)5063.479 18 . ± . r ′ (30)5064.623 18 . ± . r ′ (30)5065.733 18 . ± . r ′ (30)5066.518 18 . ± . r ′ (30)5067.468 18 . ± . r ′ (30)
102 –Table 3—Continued
JD(2 , , a . ± . r ′ (30)5070.580 19 . ± . r ′ (30)5072.519 18 . ± . r ′ (30)5073.460 18 . ± . r ′ (30)5074.733 18 . ± . r ′ (30)5075.495 18 . ± . r ′ (30)5077.712 18 . ± . r ′ (30)5078.566 18 . ± . r ′ (30)5078.515 18 . ± . r ′ (30)5079.463 18 . ± . r ′ (30)5210.587 20 . ± . r ′ (16)5211.600 20 . ± . r ′ (16)M31N 2009-08b5061.546 18 . ± . B (30)5063.625 18 . ± . B (30)5064.662 18 . ± . B (30)5066.594 19 . ± . B (30)5067.459 19 . ± . B (30)5069.600 19 . ± . B (30)5070.567 19 . ± . B (30)5071.522 19 . ± . B (30)5072.496 19 . ± . B (30)5073.554 19 . ± . B (30)5074.717 19 . ± . B (30)5075.517 19 . ± . B (30)5076.485 19 . ± . B (30)5077.471 20 . ± . B (30)5078.492 20 . ± . B (30)5079.523 20 . ± . B (30)5061.549 18 . ± . V (30)5063.628 18 . ± . V (30)5064.665 18 . ± . V (30)5066.596 18 . ± . V (30)5067.462 19 . ± . V (30)5069.603 19 . ± . V (30)5070.570 19 . ± . V (30)5071.523 19 . ± . V (30)5072.499 19 . ± . V (30)5073.556 19 . ± . V (30)5074.719 19 . ± . V (30)5075.520 20 . ± . V (30)5076.487 20 . ± . V (30)
103 –Table 3—Continued
JD(2 , , a . ± . V (30)5078.494 20 . ± . V (30)5079.526 20 . ± . V (30)5061.541 17 . ± . r ′ (30)5063.620 18 . ± . r ′ (30)5064.657 18 . ± . r ′ (30)5066.588 18 . ± . r ′ (30)5067.454 18 . ± . r ′ (30)5069.595 18 . ± . r ′ (30)5070.562 18 . ± . r ′ (30)5071.516 18 . ± . r ′ (30)5072.491 18 . ± . r ′ (30)5073.548 18 . ± . r ′ (30)5074.711 19 . ± . r ′ (30)5075.512 19 . ± . r ′ (30)5076.479 19 . ± . r ′ (30)5077.466 19 . ± . r ′ (30)5078.487 19 . ± . r ′ (30)5079.518 19 . ± . r ′ (30)5061.544 18 . ± . i ′ (30)5063.622 18 . ± . i ′ (30)5064.659 18 . ± . i ′ (30)5066.591 18 . ± . i ′ (30)5067.456 18 . ± . i ′ (30)5069.598 18 . ± . i ′ (30)5070.564 18 . ± . i ′ (30)5071.517 18 . ± . i ′ (30)5072.494 19 . ± . i ′ (30)5073.551 19 . ± . i ′ (30)5074.714 19 . ± . i ′ (30)5075.514 19 . ± . i ′ (30)5076.482 19 . ± . i ′ (30)5077.469 19 . ± . i ′ (30)5078.489 19 . ± . i ′ (30)5079.521 19 . ± . i ′ (30)M31N 2009-08d5061.639 17 . ± . B (30)5063.650 17 . ± . B (30)5064.648 17 . ± . B (30)5065.724 17 . ± . B (30)5066.555 18 . ± . B (30)
104 –Table 3—Continued
JD(2 , , a . ± . B (30)5069.658 18 . ± . B (30)5070.656 18 . ± . B (30)5071.730 > . B (30)5072.510 18 . ± . B (30)5073.509 18 . ± . B (30)5075.531 18 . ± . B (30)5076.514 18 . ± . B (30)5077.512 18 . ± . B (30)5078.478 18 . ± . B (30)5079.494 18 . ± . B (30)5061.641 17 . ± . V (30)5063.653 17 . ± . V (30)5064.651 17 . ± . V (30)5065.727 18 . ± . V (30)5066.558 18 . ± . V (30)5067.502 > . V (30)5069.661 > . V (30)5070.659 > . V (30)5072.513 18 . ± . V (30)5073.512 > . V (30)5079.497 19 . ± . V (30)5095.981 19 . ± . V (13)4985.974 > . R (9)4988.527 > . R (1)5055.923 17 . ± . R (8)5063.605 18 . ± . R (22)5076.478 > . R (1)5095.968 19 . ± . R (13)5061.633 17 . ± . r ′ (30)5063.644 18 . ± . r ′ (30)5064.643 17 . ± . r ′ (30)5065.719 18 . ± . r ′ (30)5066.550 18 . ± . r ′ (30)5067.494 > . r ′ (30)5069.653 > . r ′ (30)5070.651 > . r ′ (30)5072.505 18 . ± . r ′ (30)5073.504 18 . ± . r ′ (30)5075.526 > . r ′ (30)5077.507 > . r ′ (30)5078.472 > . r ′ (30)
105 –Table 3—Continued
JD(2 , , a . ± . r ′ (30)M31N 2009-08e5114.306 19 . ± . B (17)5129.835 20 . ± . B (15)5092.543 19 . ± . V (17)5095.981 19 . ± . V (13)5114.308 19 . ± . V (17)5129.824 20 . ± . V (15)5055.923 > . R (8)5063.605 > . R (22)5073.441 17 . ± . R (1)5074.366 18 . ± . R (1)5075.384 18 . ± . R (1)5076.478 17 . ± . R (1)5080.413 18 . ± . R (1)5081.393 18 . ± . R (1)5083.357 18 . ± . R (1)5084.267 18 . ± . R (1)5094.451 18 . ± . R (3)5095.968 18 . ± . R (13)5114.304 18 . ± . R (17)5114.486 18 . ± . R (3)5124.491 18 . ± . R (3)5129.829 19 . ± . R (15)5135.632 19 . ± . R (12)5140.546 18 . ± . R (1)5141.359 19 . ± . R (1)5148.536 18 . ± . R (1)5157.316 18 . ± . R (24)5162.281 19 . ± . R (5)5173.177 19 . ± . R (1)5181.226 > . R (1)5184.717 19 . ± . R (19)5199.299 20 . ± . R (12)5227.345 20 . ± . R (12)5228.383 20 . ± . R (12)M31N 2009-09a5092.506 19 . ± . V (17)
106 –Table 3—Continued
JD(2 , , a . ± . R (1)5081.393 17 . ± . R (1)5083.357 18 . ± . R (1)5092.506 18 . ± . R (17)5095.993 18 . ± . R (13)5148.578 18 . ± . R (1)5162.513 19 . ± . R (5)5173.203 19 . ± . R (1)5226.321 19 . ± . R (12)5227.306 19 . ± . R (12)5228.284 19 . ± . R (12)M31N 2009-10a5114.341 18 . ± . B (17)5117.718 18 . ± . B (30)5117.501 18 . ± . B (30)5118.647 18 . ± . B (30)5119.495 18 . ± . B (30)5120.389 19 . ± . B (30)5127.496 19 . ± . B (30)5128.375 19 . ± . B (30)5129.515 20 . ± . B (30)5130.468 20 . ± . B (30)5131.408 20 . ± . B (30)5132.359 > . B (30)5114.361 18 . ± . V (17)5117.721 18 . ± . V (30)5117.505 18 . ± . V (30)5118.650 18 . ± . V (30)5119.498 18 . ± . V (30)5120.392 19 . ± . V (30)5127.499 19 . ± . V (30)5128.378 19 . ± . V (30)5129.518 20 . ± . V (30)5130.472 20 . ± . V (30)5131.412 > . V (30)5114.340 17 . ± . R (17)5162.549 > . R (5)M31N 2009-10b5117.487 16 . ± . B (30)
107 –Table 3—Continued
JD(2 , , a . ± . B (30)5118.603 15 . ± . B (30)5119.488 15 . ± . B (30)5120.370 15 . ± . B (30)5124.457 16 . ± . B (18)5127.489 18 . ± . B (30)5128.368 18 . ± . B (30)5129.500 18 . ± . B (30)5130.475 18 . ± . B (30)5131.393 18 . ± . B (30)5132.352 19 . ± . B (30)5134.341 19 . ± . B (30)5135.354 19 . ± . B (30)5136.461 19 . ± . B (30)5137.400 19 . ± . B (30)5138.449 > . B (30)5139.652 19 . ± . B (30)5140.529 20 . ± . B (30)5142.515 19 . ± . B (30)5143.620 > . B (30)5146.507 > . B (30)5117.714 15 . ± . V (30)5117.490 16 . ± . V (30)5118.606 15 . ± . V (30)5119.491 15 . ± . V (30)5120.374 15 . ± . V (30)5124.458 16 . ± . V (18)5127.493 18 . ± . V (30)5128.371 18 . ± . V (30)5129.503 18 . ± . V (30)5129.824 18 . ± . V (15)5130.479 18 . ± . V (30)5131.397 18 . ± . V (30)5132.355 18 . ± . V (30)5134.345 19 . ± . V (30)5135.357 19 . ± . V (30)5136.465 18 . ± . V (30)5137.403 18 . ± . V (30)5138.452 19 . ± . V (30)5139.656 19 . ± . V (30)5140.532 19 . ± . V (30)5142.519 19 . ± . V (30)5143.623 > . V (30)5144.343 > . V (30)
108 –Table 3—Continued
JD(2 , , a > . R (9)4988.527 > . R (1)5105.262 > . R (3)5114.486 18 . ± . R (3)5124.460 15 . ± . R (18)5124.491 15 . ± . R (26)5129.829 17 . ± . R (15)5129.835 18 . ± . B (15)5135.257 17 . ± . R (3)5135.632 17 . ± . R (12)5140.546 18 . ± . R (1)5141.359 18 . ± . R (1)5148.536 18 . ± . R (1)5157.316 18 . ± . R (24)5162.281 18 . ± . R (5)5173.177 19 . ± . R (1)5181.226 19 . ± . R (1)5199.299 19 . ± . R (12)5227.345 20 . ± . R (12)5228.383 20 . ± . R (12)M31N 2009-10c5114.306 18 . ± . B (17)5117.725 17 . ± . B (30)5117.494 17 . ± . B (30)5118.654 17 . ± . B (30)5119.471 16 . ± . B (30)5120.382 17 . ± . B (30)5127.511 16 . ± . B (30)5128.361 16 . ± . B (30)5129.507 15 . ± . B (30)5130.461 16 . ± . B (30)5131.401 16 . ± . B (30)5132.366 16 . ± . B (30)5134.356 17 . ± . B (30)5135.340 16 . ± . B (30)5136.476 16 . ± . B (30)5137.340 16 . ± . B (30)5138.469 17 . ± . B (30)5139.574 17 . ± . B (30)5140.627 17 . ± . B (30)5142.540 17 . ± . B (30)5143.613 18 . ± . B (30)
109 –Table 3—Continued
JD(2 , , a > . B (30)5145.520 > . B (30)5146.619 > . B (30)5147.498 18 . ± . B (30)5114.308 17 . ± . V (17)5117.728 17 . ± . V (30)5117.497 17 . ± . V (30)5118.657 17 . ± . V (30)5119.475 17 . ± . V (30)5120.385 17 . ± . V (30)5127.515 16 . ± . V (30)5128.364 17 . ± . V (30)5129.511 16 . ± . V (30)5130.464 16 . ± . V (30)5131.404 17 . ± . V (30)5132.369 16 . ± . V (30)5134.359 17 . ± . V (30)5135.343 16 . ± . V (30)5136.479 17 . ± . V (30)5137.343 17 . ± . V (30)5138.472 > . V (30)5139.578 17 . ± . V (30)5140.630 18 . ± . V (30)5142.543 18 . ± . V (30)5143.616 > . V (30)5144.328 > . V (30)5114.304 17 . ± . R (17)5114.486 17 . ± . R (3)5124.491 16 . ± . R (3)5135.257 16 . ± . R (3)5135.632 17 . ± . R (12)5140.546 17 . ± . R (1)5141.359 17 . ± . R (1)M31N 2009-11a5142.606 18 . ± . B (30)5142.522 18 . ± . B (30)5143.606 18 . ± . B (30)5144.311 18 . ± . B (30)5145.513 19 . ± . B (30)5146.498 19 . ± . B (30)5147.477 19 . ± . B (30)
110 –Table 3—Continued
JD(2 , , a . ± . B (30)5150.410 19 . ± . B (30)5151.559 19 . ± . B (30)5154.592 19 . ± . B (30)5155.334 19 . ± . B (30)5156.309 19 . ± . B (30)5157.572 19 . ± . B (30)5159.438 19 . ± . B (30)5161.539 20 . ± . B (30)5164.398 21 . ± . B (30)5168.433 > . B (30)5169.522 > . B (30)5142.609 18 . ± . V (30)5143.609 18 . ± . V (30)5144.315 18 . ± . V (30)5145.516 18 . ± . V (30)5146.501 18 . ± . V (30)5147.480 18 . ± . V (30)5149.361 19 . ± . V (30)5150.413 19 . ± . V (30)5151.563 19 . ± . V (30)5154.595 19 . ± . V (30)5155.338 19 . ± . V (30)5156.312 19 . ± . V (30)5157.575 19 . ± . V (30)5159.441 19 . ± . V (30)5161.542 20 . ± . V (30)5164.401 20 . ± . V (30)5168.436 > . V (30)5169.525 19 . ± . V (30)5140.463 17 . ± . R (1)5141.221 17 . ± . R (5)5148.564 18 . ± . R (1)5162.534 19 . ± . R (5)5160.803 19 . ± . r ′ (10)5209.656 21 . ± . r ′ (16)5160.806 20 . ± . g ′ (10)M31N 2009-11b (recurrent nova)5154.412 19 . ± . B (30)5156.323 19 . ± . B (30)
111 –Table 3—Continued
JD(2 , , a . ± . B (30)5162.503 20 . ± . B (30)5168.480 > . B (30)5169.340 > . B (30)5170.551 19 . ± . B (30)5171.365 19 . ± . B (30)5172.330 19 . ± . B (30)5154.415 20 . ± . V (30)5156.326 19 . ± . V (30)5159.409 19 . ± . V (30)5162.507 20 . ± . V (30)5168.483 > . V (30)5169.343 19 . ± . V (30)5170.554 19 . ± . V (30)5171.368 19 . ± . V (30)5172.333 19 . ± . V (30)5148.536 18 . ± . R (1)5135.632 18 . ± . R (12)5162.281 19 . ± . R (5)5162.513 19 . ± . R (5)5173.177 19 . ± . R (1)5173.203 19 . ± . R (1)5181.226 19 . ± . R (1)5199.299 20 . ± . R (12)5227.306 20 . ± . R (12)5228.284 20 . ± . R (12)5209.616 20 . ± . g ′ (16)5207.591 21 . ± . g ′ (16)5207.599 20 . ± . r ′ (16)5209.621 20 . ± . r ′ (16)M31N 2009-11c5145.323 19 . ± . B (30)5146.516 18 . ± . B (30)5147.487 18 . ± . B (30)5148.383 17 . ± . B (30)5149.503 18 . ± . B (30)5150.403 18 . ± . B (30)5154.422 18 . ± . B (30)5156.337 18 . ± . B (30)
112 –Table 3—Continued
JD(2 , , a . ± . B (30)5162.535 18 . ± . B (30)5168.457 19 . ± . B (30)5169.333 > . B (30)5170.584 19 . ± . B (30)5171.373 19 . ± . B (30)5172.363 19 . ± . B (30)5173.509 19 . ± . B (30)5145.326 18 . ± . V (30)5146.519 17 . ± . V (30)5147.490 17 . ± . V (30)5148.386 16 . ± . V (30)5149.506 18 . ± . V (30)5150.406 18 . ± . V (30)5154.425 17 . ± . V (30)5156.340 18 . ± . V (30)5161.549 18 . ± . V (30)5162.538 18 . ± . V (30)5168.461 18 . ± . V (30)5169.336 18 . ± . V (30)5170.587 19 . ± . V (30)5171.375 18 . ± . V (30)5172.366 19 . ± . V (30)5173.512 19 . ± . V (30)5135.632 > . R (12)5140.463 > . R (1)5141.359 19 . ± . R (1)5148.536 17 . ± . R (1)5154.424 17 . ± . R (7)5157.316 17 . ± . R (24)5158.542 17 . ± . R (1)5161.164 18 . ± . R (7)5162.281 18 . ± . R (5)5162.513 18 . ± . R (5)5168.173 18 . ± . R (7)5169.202 18 . ± . R (1)5173.177 18 . ± . R (1)5173.192 18 . ± . R (1)5173.203 18 . ± . R (1)5181.226 18 . ± . R (1)5184.717 19 . ± . R (19)5227.306 > . R (12)
113 –Table 3—Continued
JD(2 , , a . ± . g ′ (10)5156.759 18 . ± . r ′ (10)5209.631 > . r ′ (16)M31N 2009-11d5156.330 17 . ± . B (30)5157.579 18 . ± . B (30)5159.445 18 . ± . B (30)5161.532 18 . ± . B (30)5168.464 > . B (30)5169.515 19 . ± . B (30)5170.529 20 . ± . B (30)5171.358 20 . ± . B (30)5172.556 19 . ± . B (30)5173.365 19 . ± . B (30)5176.376 > . B (30)5156.333 17 . ± . V (30)5157.582 18 . ± . V (30)5159.448 18 . ± . V (30)5161.535 18 . ± . V (30)5168.468 > . V (30)5169.518 20 . ± . V (30)5170.532 20 . ± . V (30)5171.361 19 . ± . V (30)5172.559 20 . ± . V (30)5173.368 20 . ± . V (30)5176.378 20 . ± . V (30)5157.299 17 . ± . R (24)5158.560 17 . ± . R (1)5162.525 17 . ± . R (5)5168.505 18 . ± . R (7)5173.192 18 . ± . R (1)5227.379 > . R (12)5156.787 16 . ± . g ′ (10)5207.619 21 . ± . g ′ (16)5156.785 16 . ± . r ′ (10)5207.626 21 . ± . r ′ (16)M31N 2009-11e
114 –Table 3—Continued
JD(2 , , a . ± . B (30)5162.524 17 . ± . B (30)5168.445 17 . ± . B (30)5169.326 17 . ± . B (30)5170.572 17 . ± . B (30)5171.379 16 . ± . B (30)5172.355 16 . ± . B (30)5173.411 18 . ± . B (30)5176.408 18 . ± . B (30)5161.578 18 . ± . V (30)5162.528 17 . ± . V (30)5168.448 17 . ± . V (30)5169.329 17 . ± . V (30)5170.575 17 . ± . V (30)5171.382 17 . ± . V (30)5173.415 19 . ± . V (30)5176.412 19 . ± . V (30)5148.536 > . R (1)5157.316 17 . ± . R (24)5158.542 17 . ± . R (1)5161.164 17 . ± . R (7)5162.281 17 . ± . R (5)5162.513 17 . ± . R (5)5168.173 17 . ± . R (7)5169.202 17 . ± . R (1)5173.177 18 . ± . R (1)5173.203 18 . ± . R (1)5181.226 18 . ± . R (1)5184.717 18 . ± . R (19)5186.730 18 . ± . R (20)5199.299 19 . ± . R (12)5227.345 19 . ± . R (12)5228.383 19 . ± . R (12)5157.691 17 . ± . g ′ (10)5158.715 17 . ± . g ′ (10)5207.591 19 . ± . g ′ (16)5210.592 19 . ± . g ′ (16)5157.688 17 . ± . r ′ (10)5158.713 17 . ± . r ′ (10)5207.599 18 . ± . r ′ (16)
115 –Table 3—Continued
JD(2 , , a . ± . r ′ (16) a Observers: (1) K. Hornoch, Ondˇrejov 0.65-m; (2) K. Hornoch, Lelekovice 0.35-m; (3) P.Kuˇsnir´ak, Ondˇrejov 0.65-m; (4) M. Wolf, Ondˇrejov0.65-m; (5) K. Hornoch & M. Wolf, Ondˇrejov 0.65-m; (6) M. Wolf i& P. Zasche, Ondˇrejov 0.65-m;(7) K. Hornoch & P. Zasche, Ondˇrejov 0.65-m; (8)P. Zasche, San Pedro M´artir 0.84-m; (9) O. Pe-jcha, MDM 1.3-m; (10) O. Pejcha, MDM 2.4-m;(11) K. Hornoch & P. ˇSedinov´a, Ondˇrejov 0.65-m; (12) P. Kub´anek, J. Gorosabel i& M. Jel´ınek,Calar Alto 1.23-m; (13) P. Kub´anek, MDM 2.4-m; (14) P. Garnavich & A. Karska, MGIO 1.83-mVATT; (15) P. Garnavich, K. Thorne & K. Morhig,MGIO 1.83-m VATT; (16) J. Prieto & R. Khan,MDM 2.4-m; (17) A. Valeev & O. Sholukhova,SAO 6-m; (18) V. L. Afanasiev & S. N. Dodonov,SAO 6-m; (19) T. Farnham & B. Mueller, KPNO2.1-m; (20) N. Samarasinha & B. Mueller, KPNO2.1-m; (21) M. Burleigh & S. Casewell, La Palma2.5-m INT; (22) A. Gal´ad, AGO Modra 0.60-m;(23) P. Cagaˇs, Zl´ın 0.26-m; (24) K. Hornoch &P. Kuˇsnir´ak, Ondˇrejov 0.65-m; (25) P. Kuˇsnir´ak& T. Henych, Ondˇrejov 0.65-m; (26) P. Kuˇsnir´ak& Z. Bardon, Ondˇrejov 0.65-m; (27) K. Hornoch& M. Tukinsk´a, Ondˇrejov 0.65-m; (28) P. Zasche& Ondˇrejov, 0.65-m; (29) Darnley et al. 2004;La Palma 2.5-m INT; (30) La Palma 2.0-m LT;(31) Mt. Haleakala 2.0-m FTN; (32) P. Kuˇsnir´ak,L. ˇSarounov´a & M. Wolf, Ondˇrejov 0.65-m; (33)P. Garnavich, MGIO 1.83-m VATT; (34) P. Gar-navich & B. Tucker, MGIO 1.83-m VATT; (35) P.Garnavich & C. Kennedy, MGIO 1.83-m VATT;(36) P. Garnavich & J. Gallagher, MGIO 1.83-mVATT; (37) P. Garnavich, KPNO 3.5-m WIYN;(38) D. Mackey, La Palma 2.5-m INT.
116 –Table 4. Full Spectroscopic Sample of M31 Novae ∆ α cosδ ∆ δ a DiscoveryNova ( ′ ) ( ′ ) ( ′ ) mag (Filter) Type References a M31N 1981-09a − . − .
89 5.67 16.4(H) Fe II 1M31N 1981-09b − .
65 2.10 2.96 14.9(H) Fe II 1M31N 1981-09c 0.78 2.87 3.43 15.0(H) Fe II 1M31N 1981-09d 4.11 − .
16 8.07 15.8(H) Fe II 1M31N 1986-08a − . − .
64 4.98 16.3(H) Fe II 2M31N 1987-09a 7.80 2.13 10.57 19.4(B) Fe II 2M31N 1987-10a − .
33 1.75 2.28 18.4(B) Fe II 2M31N 1989-08a 6.47 − .
29 10.36 17.9(B) He/N 2M31N 1989-08b − .
01 0.00 1.10 19.3(B) Fe II 2M31N 1989-08c − . − .
41 6.84 17.9(B) Fe II 2M31N 1989-09a 2.15 4.05 5.06 15.5(H) Fe II 2M31N 1989-10a 0.36 3.10 3.91 17.6(B) Fe II 2M31N 1990-10b − . − .
32 5.44 17.6(B) Fe II 3M31N 1992-11b 3.07 − .
49 5.04 17.2(V) Fe II 3M31N 1993-06a 0.91 1.31 1.64 15.8(R) Fe II: 3M31N 1993-08a 0.14 − .
70 1.64 15.8(R) He/N: 3M31N 1993-10g 0.63 1.87 2.17 16.7(H) Fe II 3M31N 1993-11c 1.08 1.32 1.73 15.8(H) Fe II: 3M31N 1998-09d 0.43 − .
33 1.78 16.5(B) Fe II 3M31N 1999-06a 0.97 − .
05 1.89 17.8(R) Fe II 3M31N 1999-08f − .
61 3.04 4.44 17.0(w) Fe II: 3M31N 1999-10a 1.00 0.39 1.10 17.5(w) Fe II: 3M31N 2001-10a 3.56 − .
96 10.81 17.0(R) Fe II 3M31N 2001-12a − .
55 0.26 0.68 15.5(R) Fe II 3M31N 2002-01b − .
97 2.25 4.60 16.8(R) He/N: 3M31N 2002-08a − . − .
93 14.01 17.1(R) Fe II: 3M31N 2004-08b 7.98 0.54 12.60 17.3(R) Fe II 3M31N 2004-09a − . − .
44 1.72 17.5(R) Fe II 3M31N 2004-11a − .
29 2.32 3.03 16.5(R) Fe II 3M31N 2004-11b 4.34 1.93 4.97 16.6(R) He/N: 3M31N 2005-01a − .
00 0.46 3.98 15.0(R) Fe II 3M31N 2005-06d 26.35 17.61 44.21 15.7(w) He/N 4M31N 2005-07a 1.21 4.52 5.85 17.4(R) FeII: 3M31N 2005-09a 1.48 3.84 4.76 16.7(R) Fe II 4M31N 2005-09b − . − .
00 71.73 16.5(w) Fe II b − . − .
34 66.76 16.0(w) Fe II 5M31N 2006-06a 5.16 − .
40 11.09 17.5(R) Fe II 4M31N 2006-09c − . − .
39 11.61 16.8(w) Fe II 3M31N 2006-10a − . − .
36 17.31 18.7(R) Fe II 3M31N 2006-10b − . − .
81 63.14 16.4(w) Hy 3M31N 2006-11a 2.35 − .
84 20.46 17.3(w) Fe II 3M31N 2006-12a − . − .
39 5.11 17.8(R) Fe II 3M31N 2006-12b − . − .
41 10.88 18.0(R) Fe II 3M31N 2007-02a − . − .
22 40.21 16.3(w) Fe II 3M31N 2007-02b − . − .
57 21.34 16.7(R) Fe II: 3,6
117 –Table 4—Continued ∆ α cosδ ∆ δ a DiscoveryNova ( ′ ) ( ′ ) ( ′ ) mag (Filter) Type References a M31N 2007-06b − . − .
71 26.20 16.8(w) He/N 3,7M31N 2007-07b 0.29 1.92 2.26 17.7(R) Fe II 8M31N 2007-07c 3.56 − .
26 5.55 15.8(R) He/N 8,9M31N 2007-07e − .
20 1.59 2.00 18.1(R) Fe II 8M31N 2007-07f − . − .
95 81.74 17.4(w) Fe II 10M31N 2007-08a − . − .
25 30.49 17.6(w) Fe II: 8M31N 2007-08d − . − .
74 59.56 18.1(R) Fe II 3M31N 2007-10a 2.19 − .
78 27.57 16.0(w) He/Nn 3,11M31N 2007-10b 8.48 1.09 12.91 17.8(w) He/Nn 12M31N 2007-11b 12.94 − .
52 59.72 18.6(R) He/Nn 3,13,14M31N 2007-11c 3.72 − .
24 4.77 17.4(R) Fe II 14,15M31N 2007-11d 24.34 21.60 34.03 14.9(w) Fe II 3,16M31N 2007-11e 34.06 46.07 57.52 16.4(w) Fe II 3,17M31N 2007-12a 14.79 22.57 28.53 17.8(w) Fe II 3M31N 2007-12b 6.70 − .
37 14.79 16.1(w) He/N 3,18M31N 2007-12c 27.26 4.08 66.22 16.4(w) Fe II 19M31N 2007-12d − . − .
35 11.92 17.2(R) He/N 3M31N 2008-05c 5.20 3.12 6.18 17.0(R) Fe II 20M31N 2008-06b − . − .
34 3.56 15.9(R) He/N 21M31N 2008-07a − .
87 2.12 4.34 18.3(R) Fe II 22M31N 2008-07b 8.08 − .
08 26.01 19.0(g) Fe II 23M31N 2008-08a 0.12 0.98 1.09 16.8(R) Fe II 24,25M31N 2008-08b 1.51 0.07 1.69 16.4(R) He/N 24,25M31N 2008-08c − .
72 10.15 18.72 16.8(R) Fe II 25M31N 2008-08d 33.62 106.41 109.45 18.1(w) Fe II 26M31N 2008-09a − . − .
26 14.26 18.1(g) Fe II 3M31N 2008-09c 1.33 − .
25 30.22 17.6(g) Fe II 3M31N 2008-10a 9.51 38.60 65.42 17.1(w) Fe II 3M31N 2008-10b 3.40 − .
98 6.19 18.3(R) Fe II 25,27M31N 2008-11a − . − .
11 18.51 16.5(R) He/N 3M31N 2008-12b 3.85 1.72 4.43 16.8(w) Fe II 28M31N 2009-01a 22.44 7.39 48.17 18.5(w) Fe II 3M31N 2009-02a 11.11 20.52 26.38 16.8(w) Fe II 3M31N 2009-08a 2.57 1.35 3.00 17.2(H) Fe II 29M31N 2009-08b 15.93 32.73 45.52 17.1(w) Fe II 30M31N 2009-08d 0.45 − .
52 0.81 17.2(R) Fe II 31M31N 2009-08e − .
54 1.89 3.54 17.8(w) Fe II 32M31N 2009-09a − . − .
13 17.38 17.6(w) Fe II 33M31N 2009-10a 27.78 48.61 61.67 17.1(w) Fe II 34M31N 2009-10b − .
43 0.60 6.17 14.7(R) Fe II 35M31N 2009-10c 0.26 − .
19 0.37 17.2(H) Fe II 36M31N 2009-11a 3.81 24.99 48.41 17.6(R) Fe II 37M31N 2009-11b − . − .
09 10.56 18.4(R) Fe II 23,38M31N 2009-11c 4.91 − .
83 12.92 17.0(R) Fe II 39M31N 2009-11d 17.37 2.79 35.48 16.4(r) Fe II 40
118 –Table 4—Continued ∆ α cosδ ∆ δ a DiscoveryNova ( ′ ) ( ′ ) ( ′ ) mag (Filter) Type References a M31N 2009-11e − . − .
16 3.86 17.4(R) Fe II 41 a REFERENCES: (1) Ciardullo et al. (1983); (2) Tomaney & Shafter (1992); (3)this work; (4) Pietsch et al. (2005); (5) Hatzidimitriou et al. (2007); (6) Pietsch etal. (2007a); (7) Shafter & Quimby (2007); (8) Barsukova et al. (2007); (9) Rau etal. (2007a); (10) Quimby (2007, private communication); (11) Gal-Yam & Quimby(2007); (12) Rau et al. (2007b); (13) Rau (2007); (14) Barsukova et al. (2007b); (15)Ciroi (2007); (16) Shafter et al. (2009); (17) Di Mille et al. (2007); (18) Bode et al.(2009); (19) Rau & Cenko (2007); (20) Rau et al. (2008) (21) Reig et al. (2008); (22)Barsukova et al. (2008); (23) Kasliwal et al. (2011); (24) Di Mille et al. (2008a); (25)Di Mille et al. (2010); (26) Chornock et al. (2008); (27) Di Mille et al. (2008b); (28)Kasliwal et al. (2008); (29) Valeev et al. (2009); (30) Rodr´ıguez-Gil et al. (2009); (31)Di Mille et al. (2009a); (32) Medvedev et al. (2000); (33) Barsukova et al. (2009a);(34) Fabrika et al. (2009a); (35) Barsukova et al. (2009b); (36) Fabrika et al. (2009b);(37) Hornoch et al. (2009a); (38) Kasliwal (2009); (39) Hornoch et al. (2009b); (40)Hornoch et al. (2009c); (41) Hornoch et al. (2009d) b The line with of 4400 km s − reported by D. C. Leonard referred to an estimateof the full width at zero intensity, not the FWHM. Analysis of the original spectrumreveals the object to be a classic Fe II nova
119 –Table 5. Balmer Emission-Line Properties
EW (˚A) FWHM (km s − )Nova H β H α H β H α M31N 1990-10b − −
541 1600 1550M31N 1992-11b − − − −
392 1840 1770M31N 1993-08a . . . . . . . . . 4350M31N 1993-10g a − −
324 1630 1680M31N 1993-11c a − −
828 1450 1560M31N 1998-09d − −
323 1720 1840M31N 1999-06a − − − −
704 1640 1690M31N 1999-10a − −
565 1780 1930M31N 2001-10a − −
945 1540 1540M31N 2001-12a . . . − −
760 . . . 3430M31N 2002-08a − −
470 1360 1320M31N 2004-08b − −
410 1970 1830M31N 2004-09a − −
250 2000 1880M31N 2004-11a − −
830 1230 1580M31N 2004-11b − − − −
107 1810 1680M31N 2005-07a . . . −
120 . . . 1100M31N 2006-09c − −
470 1910 1920M31N 2006-10a − −
90 950 810M31N 2006-10b − −
102 3330 3090 − − − −
57 1420 1120M31N 2006-12a − −
330 1850 1760M31N 2006-12b − −
226 1230 1020M31N 2007-02a − −
61 1530 1310M31N 2007-02b − −
304 1460 1910M31N 2007-06b − −
168 2940 2870M31N 2007-08d − −
284 1160 1180M31N 2007-10a − −
154 470 500M31N 2007-11b − −
535 1480 1290M31N 2007-11c − −
137 1950 1700M31N 2007-11d − −
16 1630 1550 − − − −
306 1750 1600M31N 2007-11g − −
13 340 300M31N 2007-12a − −
309 2050 1850M31N 2007-12b − −
990 4070 4080M31N 2007-12d − − − −
440 1150 1050 − −
634 1360 1480M31N 2008-09a − −
262 1540 1460M31N 2008-09c − −
23 1590 1010
120 –Table 5—Continued
EW (˚A) FWHM (km s − )Nova H β H α H β H α M31N 2008-10a − −
300 1390 1270M31N 2008-10b − . −
19 660 640 − −
95 1220 950M31N 2008-11a − −
636 4510 4350 − −
370 1460 3160M31N 2009-01a − −
25 560 550M31N 2009-02a − −
15 1280 1410 a Due to ambiguity in the data logs from November1993, it is possible that the data for these two novae arereversed.
121 –Table 6. Light-Curve Parameters
Nova Filter M max Fade Rate (mag day − ) t (days)M31N 1999-08f r ′ − . ± .
11 0 . ± .
002 31 . ± . r ′ − . ± .
11 0 . ± .
004 50 . ± . R − . ± .
20 0 . ± .
005 45 . ± . R − . ± .
25 0 . ± .
002 52 . ± . R − . ± .
20 0 . ± .
006 35 . ± . R − . ± .
25 0 . ± .
010 19 . ± . R − . ± .
20 0 . ± .
002 47 . ± . R − . ± .
17 0 . ± .
009 19 . ± . R − . ± .
25 0 . ± .
003 120 . ± . R − . ± .
11 0 . ± .
006 67 . ± . R − . ± .
14 0 . ± .
006 23 . ± . B − . ± .
11 0 . ± .
002 56 . ± .
1. . . V − . ± .
11 0 . ± .
002 57 . ± .
1. . . R − . ± .
20 0 . ± .
005 94 . ± . B − . ± .
11 0 . ± .
018 7 . ± .
4. . . V − . ± .
11 0 . ± .
018 5 . ± . R − . ± .
20 0 . ± .
006 28 . ± . R − . ± .
25 0 . ± .
007 34 . ± . R − . ± .
20 0 . ± .
006 34 . ± . R − . ± .
35 0 . ± .
010 45 . ± . R − . ± .
11 0 . ± .
003 80 . ± . B − . ± .
11 0 . ± .
013 9 . ± .
5. . . V − . ± .
11 0 . ± .
013 7 . ± .
4. . . i ′ − . ± .
13 0 . ± .
010 8 . ± . B − . ± .
15 0 . ± .
067 3 . ± .
5. . . V − . ± .
56 0 . ± .
065 2 . ± .
3. . . R − . ± .
44 0 . ± .
085 3 . ± . B − . ± .
11 0 . ± .
004 36 . ± .
6. . . V − . ± .
11 0 . ± .
003 45 . ± .
5. . . R − . ± .
25 0 . ± .
012 43 . ± .
0. . . i ′ − . ± .
14 0 . ± .
006 74 . ± . B − . ± .
24 0 . ± .
006 14 . ± .
6. . . V − . ± .
27 0 . ± .
007 12 . ± .
6. . . i ′ − . ± .
18 0 . ± .
013 11 . ± . B − . ± .
11 0 . ± .
009 14 . ± .
9. . . V − . ± .
11 0 . ± .
009 12 . ± .
7. . . r ′ − . ± .
11 0 . ± .
009 13 . ± .
8. . . i ′ − . ± .
11 0 . ± .
011 9 . ± . B − . ± .
12 0 . ± .
005 25 . ± .
6. . . V − . ± .
11 0 . ± .
004 24 . ± .
4. . . i ′ − . ± .
11 0 . ± .
004 29 . ± . B − . ± .
11 0 . ± .
034 4 . ± .
3. . . V − . ± .
11 0 . ± .
033 3 . ± .
2. . . R − . ± .
11 0 . ± .
043 5 . ± . R − . ± .
11 0 . ± .
002 53 . ± . R − . ± .
11 0 . ± .
005 24 . ± .
122 –Table 6—Continued
Nova Filter M max Fade Rate (mag day − ) t (days)M31N 2008-07a R − . ± .
11 0 . ± .
001 410 . ± . R − . ± .
20 0 . ± .
006 40 . ± . R − . ± .
20 0 . ± .
011 21 . ± . B − . ± .
11 0 . ± .
003 37 . ± .
2. . . V − . ± .
11 0 . ± .
003 38 . ± .
2. . . r ′ − . ± .
11 0 . ± .
003 67 . ± . B − . ± .
12 0 . ± .
003 98 . ± .
9. . . V − . ± .
12 0 . ± .
003 117 . ± .
5. . . R − . ± .
25 0 . ± .
015 63 . ± .
2. . . r ′ − . ± .
11 0 . ± .
003 73 . ± . B − . ± .
11 0 . ± .
029 3 . ± .
2. . . V − . ± .
11 0 . ± .
024 4 . ± .
2. . . R − . ± .
11 0 . ± .
044 5 . ± .
6. . . r ′ − . ± .
11 0 . ± .
013 7 . ± .
4. . . i ′ − . ± .
13 0 . ± .
006 16 . ± .
8. . . z ′ − . ± .
12 0 . ± .
017 8 . ± . B − . ± .
11 0 . ± .
006 36 . ± .
1. . . V − . ± .
11 0 . ± .
006 30 . ± .
9. . . r ′ − . ± .
11 0 . ± .
006 27 . ± .
2. . . i ′ − . ± .
15 0 . ± .
012 24 . ± .
6. . . z ′ − . ± .
12 0 . ± .
011 45 . ± . B − . ± .
11 0 . ± .
001 351 . ± .
5. . . V − . ± .
11 0 . ± .
001 190 . ± .
5. . . R − . ± .
11 0 . ± .
001 142 . ± .
0. . . r ′ − . ± .
11 0 . ± .
001 142 . ± . B − . ± .
11 0 . ± .
005 18 . ± .
8. . . V − . ± .
11 0 . ± .
005 17 . ± .
8. . . r ′ − . ± .
11 0 . ± .
004 23 . ± .
2. . . i ′ − . ± .
12 0 . ± .
006 26 . ± . B − . ± .
24 0 . ± .
017 27 . ± .
5. . . V − . ± .
11 0 . ± .
008 31 . ± .
9. . . R − . ± .
20 0 . ± .
008 36 . ± .
2. . . r ′ − . ± .
11 0 . ± .
019 25 . ± . R − . ± .
11 0 . ± .
001 121 . ± . R − . ± .
25 0 . ± .
001 163 . ± . B − . ± .
11 0 . ± .
007 16 . ± .
9. . . V − . ± .
11 0 . ± .
006 15 . ± . B − . ± .
11 0 . ± .
007 8 . ± .
2. . . V − . ± .
11 0 . ± .
005 8 . ± .
2. . . R − . ± .
11 0 . ± .
010 12 . ± . B − . ± .
13 0 . ± .
008 14 . ± .
8. . . V − . ± .
14 0 . ± .
011 16 . ± .
4. . . R − . ± .
25 0 . ± .
020 30 . ± . B − . ± .
11 0 . ± .
007 21 . ± .
6. . . V − . ± .
11 0 . ± .
005 21 . ± .
2. . . R − . ± .
11 0 . ± .
009 20 . ± .
123 –Table 6—Continued
Nova Filter M max Fade Rate (mag day − ) t (days)M31N 2009-11b B − . ± .
11 0 . ± .
004 92 . ± .
6. . . V − . ± .
11 0 . ± .
004 74 . ± .
6. . . R − . ± .
11 0 . ± .
002 88 . ± . B − . ± .
11 0 . ± .
003 42 . ± .
7. . . V − . ± .
14 0 . ± .
005 32 . ± .
4. . . R − . ± .
11 0 . ± .
004 43 . ± . B − . ± .
11 0 . ± .
007 11 . ± .
4. . . V − . ± .
11 0 . ± .
025 7 . ± .
7. . . R − . ± .
11 0 . ± .
013 16 . ± . R − . ± .
20 0 . ± .
002 55 ..
002 55 .. ± ..