PoS(GOLDEN 2017)050 https://pos.sissa.it/ ´ ´ ´ ´ íso, Chile íso, Chile íso, Chile íso, Chile ´ c ∗ [email protected] [email protected] [email protected] [email protected] [email protected] [email protected] [email protected] ˇ ckovi Speaker. In order to investigate the luminosityproject to and reobserve expansion the evolution novae of collected novaties. in shells, the In we Downes the et have present al. started article, (2001) a wea catalogue discuss first, on very potential shell preliminary, problems luminosi- analysis of of the the Downes expansion et evolution of al. our work first and set conduct of shell data. ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). The Golden Age of Cataclysmic Variables11-16 and September, Related 2017 Objects IV Palermo, Italy E-mail: E-mail: V. A. R. M. Ribeiro Univeridade de Aveiro, Portugal E-mail: M. Vu N. Vogt Instituto de Física y Astronomía, Universidad de Vapara A. Ederoclite Centro de Estudios de Física delE-mail: Cosmos de Aragón, Teruel, Spain Instituto de Física y Astronomía, Universidad de Vapara L. Schmidtobreick European Southern Observatory, Santiago, Chile E-mail: C. Tappert Instituto de Física y Astronomía, UniversidadE-mail: de Vapara E. Arancibia Instituto de Física y Astronomía, UniversidadE-mail: de Vapara The evolution of nova shells PoS(GOLDEN 2017)050 ] lu- III ]. Thus, C. Tappert 15 , 19 , ) and [O ] and Downes & β 18 1 , 17 and H α 1300 yr, 400 yr, 120 yr and 580 yr, ≥ for a given nova; for DK Lac, two very different ], and the probable intermediate polar J17014 3 t ]). On the other hand, a number of searches for 17 1 24 post-novae detected shells in roughly 50% of their , spun by the data points of an individual nova in DDD01. t 22 ∆ known 3 yr. While this study represents a valuable step in the right . In particular, they find two different relations per speed class, ) ≤ t ( t L ≤ ]). 28 in which the nova declines by two and three magnitudes after maximum ] (hereafter DDD01) investigated the hydrogen (H 3 t ], the nova-like V1315 Aql [ 5 23 ]. The smoking gun for establishing a CV as a former nova is the presence of , and 29 21 2 , t ] in their investigations on 8 4 Left: Histogram of the time range ]. The ages of these shells have been determined to 16 Downes et al. [ In order to study the long-term effect of the nova eruption on the underlying cataclysmic , 25 in the form of a slowtypically early at and a a shell steep age latedirection, 100 decline, and, d with in the fact, breakpoint remains betweenshells the the to only date, two there comprehensive relations are work a on number the of brightness potential evolution problems of associated with nova it. brightness, respectively. They derive several nominalfunction relations of time for after the eruption, luminosity of the lines as a minosities of a large sample ofto nova shells, the distinguishing times novae of different speed class according The five novae with thethose largest five time novae. range are The labelled.values numbers are Right: state reported (DDD01, the Comparison [ decline of time the luminosity evolution of Figure 1: shells signatures in a total of slightly more than 110 CVs were unsuccessful [ Duerbeck [ a nova shell. Inand the AT recent Cnc years, [ such shells have been detected around the dwarf novae Z Cam binary (CV), it is importantpopulation to compare [ the properties of post-novae with those of the general CV Nova shells 1. Introduction [ respectively (for Z Cam and AT Cnc, see [ either those CVs arethe much four older cases (in above, the or their sense shells of became time undetectable after muchtargets. the Which, faster. then, nova Cohen are eruption) the [ parameters post-novaedetected? that determine than for how long a nova shell can be reasonably 2. The luminosity evolution of nova shells PoS(GOLDEN 2017)050 t – L (3.1) C. Tappert the initial 1 c from different ) t ( L being the dominant ]). 3 t emission in slow novae, 24 α 2 t ]). It is thus very reasonable to assume 2 c 13 0), the behaviour appears to be consistent 5 0 the initial size of the shell, . > 0 narrow-band photometry of all novae in the t = + 0 α t c 1 2 , c t we compare the behaviour of the five novae with + 1 0 c on-band (#692) as well as an off-band (#698) narrow-band ) = α t ( r . However, a number of other parameters come to mind that are 3 t the decline rate of novae is roughly correlated with the ejection energy the deceleration parameter. He used this ansatz to fit the expansion data on 2 not all speed classes count with a sufficiently even distribution of data points depends on c ) the data set predominantly consists of novae with one single measurement of the t ] parametrized the expansion of the nova shell as ( 6 L , left). shows the resulting difference (on-band minus off-band) images for the nova shells of 1 2 being the radius of the shell at time ) t ( novae of the same speed class (see point 2), depends critically on for all novae, regardless of this parameter. A single parameter: also likely to affect the brightness ofmedium, the shell, or e.g. dust the formation structure in of the the surrounding shell interstellar material. The validity of deriving and thus the velocity of thethat ejected also material (e.g., [ parameter. In thethe right largest plot time of range Fig. Nevertheless, in especially at DDD01. the later This stages (log includes systems of very different speed classes. Sample size: Grouping: along the age axis. Thewhich most is significant dominated example by is the behaviour that of of a the single, H extragalactic, nova (figure 10 in DDD01). shell luminosity. Only five novae(Fig. have a data point distribution that spans more than 20 yr r From July 23 to 25, 2017, we observed a sample of classical novae from DDD01 on La Silla Our main purpose is to extend the DDD01 data. This will yield a second data point in the Duerbeck [ 3. 1. 2. with filter. Fig. four classical novae and found significant deceleration for all four of them. Observatory, using the New Technology Telescope (NTT) withand the Camera ESO (EFOSC2). Faint We Object used an Spectrograph H diagram for all novae invidual DDD01, systems, and instead thus of allow having for toby an rely a analysis on specific of fitting the a parameter. sample shelladditional of decline However, phenomena, different rate the e.g. systems the for nature grouped evolution indi- of together ofdetermination the our of expansion. novae, observations as This allows well bears as for importance for an for the the investigation age-dating distance ancient of novae (e.g., [ expansion rate, and V842 Cen (Nova Cen 1986), HR Del (Nova Del 1967) and FH Ser (Nova Ser 1970). The gist of the pointsOur above is plan that of it attack appears desirable is to the extend following: and re-analyse first, the DDD01 take data. H DDD01 paper to checkmeasure for emission line the fluxes, presence and of second,above analyse mentioned extended parameters. the shells data with and respect flux-calibrated to possible spectroscopy correlations to of 3. First preliminary results: deceleration Nova shells PoS(GOLDEN 2017)050 C. Tappert in time. t ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] with respect to the discrepancy of 26 27 9 4 4 14 2 20 7 27 3 11 10 4 30 12 4 ] with their own data and those of other authors. [arcsec] reference r 3 27 [yr] 29.83 4.3530.84 4.934.58 8 [ [ 14.44 1.85 [ 23.52 3.5 [ 27.20 3.5 [ [ 26.12 5.7529.45 3.78 [ [ 49.99 7.7(3) this work 19.50 2.6526.05 4.5 [ 47.40 7.0(6) [ this work 11.33 3.025.22 3.630.66 5.2(5) [ 25.01 [ this 2.75 work [ t for the three novae at a given point r V842 Cen 8.25 0.8 [ FH Ser 12.46 2.0 [ object HR Del 13.76 1.85 [ Shell radii data on the classical novae V842 Cen (left), HR Del (middle) and FH Ser (right). α Table 1: EFOSC H When talking about the size of a shell, one has to define which part of the surface brightness Figure 2: Such ambiguity can becan resolved be once followed the more precisely, shell but this shows only localized becomes inhomogeneities, feasible at whose the motion later stages of the expansion. distribution is to be measured.as The one general sigma consensus above the seems sky todepends background. be on However, that the this quality the also of limiting is the value not data. is without This taken problems, is, as e.g., it discussed strongly in [ the shell size derived in the high-quality data of [ Nova shells PoS(GOLDEN 2017)050 ]. The ] finds 6 6 C. Tappert 5.2(1) arcsec, × . It is evident that (a) DQ 1 4 . For a first rough test, we compare the distribution of 3 ) in Fig. ]. 6.2(3) arcsec, for V842 Cen, HR Del and FH Ser, respectively, 1 for the three observed novae and data on DQ Her taken from [ 6 t × ] with respect to the presentation of the deceleration parameters (or the braking 6 versus time r ] of previous data yields much less scatter than for our systems. In conclusion, 6 Shell radii 6.6(4) arcsec and 7.0(6) × Note that there is a mistake in [ In order to check for a possible deceleration, we plot our values of the major semi-axes together 1 we note that while ourexpansion result velocity is show consistent smaller deceleration, with a thenecessary. more tendency thorough that analysis nova of shells all with the a available data slower is initial in his data thatwe the also deceleration show is the inversely datawhich related for consequently the also to counts nova the with with the expansion theHer smallest velocity. slowest deceleration has parameter expansion a For in significantly the comparison, higher Duerbecknot expansion sample, consistent rate DQ with than Her, a the linear otherre-analysis expansion, three by but novae, [ and require (b) deceleration. that We the also data remark are that the careful parameter that he usesdeceleration in equation his are table positive. This, 2), however, in yields acceleration. that both the deceleration parameter and the sign of the second term in the the data with a linear expansion,data. as defined Clearly, by within the the zero point scatter, (0,0) all and data the are result consistent from with our EFOSC2 zero deceleration. Duerbeck [ dashed lines represent a linear evolutionthe from deceleration the fit zero to point DQ to Her the from final [ data point. The solid line represents In our preliminary analysisrion. on the In three this novae, way, we we7.7(3) find used the the shell one sizes sigma corresponding above to background the semi-axes crite- to 5.2(5) Figure 3: with those of other authors (Table with the errors reflecting the differencescentral of star. the measurements of the semi-axes to both sides of the Nova shells PoS(GOLDEN 2017)050 , 196 , , Acta C. Tappert , 90 , MNRAS 292 , 1151 , , , 175 , 6 Astroph. Space 325 7 ApJ , , , , 314 , , 1219 , 516 A&A , 344 393 , , MNRAS , ApJ , narrow-band images show the MNRAS α , Study of nova shells. II. FH Serpentis Journ. Astron. Data , , 1541 , 689 Luminosities of [O III] and Hydrogen 138 , 268 , AJ , , 2007 ApJ 5 , 120 , AJ , Optical Imaging of Nova Shells and the Maximum Nova shells Hubble Space Telescope imaging and ground-based spectroscopy Deep optical imaging of nova remnants: a southern sky sample Hubble Space Telescope imaging and ground-based spectroscopy of HR Del Remnant Anatomy Using Two-Dimensional Spectral Data and The nebular expansion parallax and the luminosity of nova FH Ser The interaction of nova shells with the interstellar medium these proceedings Direct photography of the nebular remnant of Nova Delphini 1967 Nova shells. II - Calibration of the distance scale using novae Classical novae and the extragalactic distance scale , 221 , 85 300 , 461 42 , , 131 , Three-Dimensional Photoionization Shell Models Astron. MNRAS of old nova shells - II. The bipolar shell of the slow nova HR Del old nova shells - I. FH Ser, V533 Her, BT Mon, DK Lac and V476 Cyg Sci. P87 Balmer lines in nova shells years and decades after outburst Magnitude-Rate of Decline Relationship 1970 and QU Vulpeculae 1984, nebular expansion, parallax and luminosity CT, EA, MV and NV acknowledge support by Fondecyt project 1170566. We have presented the outline of a project to investigate the luminosity evolution of nova [8] A. Ederoclite, et al., [9] D. J. Harman, T. J. O’Brien, 2003, [7] H. W. Duerbeck, 1992, [6] H. W. Duerbeck, 1987, [4] R. A. Downes, H. W. Duerbeck, 2000, [5] R. A. Downes, H. W. Duerbeck, C. E. Delahodde, 2001, [3] M. della Valle, R. Gilmozzi, A. Bianchini, H. Esenoglu, 1997, [2] J. G. Cohen, A. J Rosenthal, 1983, [1] J. G. Cohen, 1985, [14] M. Moraes, M. Diaz, 2009, [10] C. D. Gill, T. J. O’Brien, 1998, [11] C. D. Gill, T. J. O’Brien, 2000, [12] L. Kohoutek, 1981, [13] M. Livio, 1992, References resolved shells of the novaeyields V842 the sizes Cen, of the HR shells. Del Inin and comparison either with FH previous of Ser. data we the find Adifferent no three preliminary evidence sources for systems. analysis impedes deceleration of the the We detectionbe data suspect comparatively of small. that deceleration, A the which, careful scatterdetermination as re-analysis of in of we shell previous the sizes. argue, data radii is will be data also needed expected taken for to from a more several uniform Acknowledgments shells. As an example of the first data taken in this project, H Nova shells 4. Summary PoS(GOLDEN 2017)050 , , 458 , , 739 MNRAS , 465 C. Tappert , , p.71 , 1371 MNRAS , 462 , MNRAS , MNRAS , On the absence of nova When does an old nova become , 4692 SALT observations of southern 473 in: RS Ophiuchi (1985) and the , , Searching for nova shells around Life after eruption - VI. Recovery of the old Proper-motion age dating of the progeny of , 107 MNRAS 756 , ]. All physics are hidden in the parameters of An ancient nova shell around the dwarf nova Z , 6 The Inter-eruption Timescale of Classical Novae Catalog of 93 Nova Light Curves: Classification ApJ 6 AT Cnc: A Second Dwarf Nova with a Classical Nova A deep optical imaging study of the nebular remnants The Structure of the Remnant of HR Delphini , should be calculated accordingly. ) t An Atlas of Nova Shells ( Discovery of spin-modulated circular polarization from IGR r , 2863 , 558 451 , 353 548 , , Non-detection of nova shells around asynchronous polars , 159 276 , 446 , Nature , 34 MNRAS , , A119 , , 2215 140 MNRAS , 576 What exactly is the acceleration or deceleration equation you are using? Note We use a simple parametrized acceleration / deceleration equation in the form , Nature , 449 AJ , , 121 , , A&A 758 , , MNRAS ApJ , , , L55 post-novae Nova Scorpii AD 1437 266 Shell of classical novae and Properties novae EL Aql, V606 Aql, V908 Oph, V1149 Sgr, V1583 Sgr and V3964 Sgr a dwarf nova? Kinematics and age of the nova shell of the dwarf nova AT Cancri shells Recurrent Nova Phenomenon, Proceedings, M. F. Bode (ed.), Utrecht: VNU Science Press cataclysmic variables J17014-4306, the remnant of Nova Scorpii 1437 AD 1833 from Expansion of the Z Camelopardalis Shell Camelopardalis this equation, which will have toobserved be expansion compared rates to is proper available. models once a sufficiently large sample of that you have first an energydown phase and and momentum a conserving radiative free phase, expansion the phase followed by a slow DISCUSSION SOLEN BALMAN: CLAUS TAPPERT: of a polynomial of second order, as introduced by [ [27] A. J. Slavin, T. J. O’Brien, J. S. 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