To appear in Ap. J. A long-lasting quiescence phase of the eruptive variable V1118 Ori D.Lorenzetti1, S.Antoniucci1, T.Giannini1, A. Harutyunyan2, A.A.Arkharov3, V.M.Larionov3,4,5, F.Cusano6, A.Di Paola1, G.Li Causi1, B.Nisini1, R.Speziali1, and 5 1 F.Vitali1. 0 2 n ABSTRACT a J 1 2 V1118 Ori is an eruptive variable belonging to the EXor class of Pre-Main ] Sequence stars whose episodic outbursts are attributed to disk accretion events. R Since 2006, V1118 Ori is in the longest quiescence stage ever observed between S . two subsequent outbursts of its recent history. We present near-infrared photom- h p etry of V1118 Ori carried out during the last eight years, along with a complete - o spectroscopic coverage from 0.35 to 2.5 µm. A longterm sampling of V1118 Ori r t in quiescence has never been done, hence we can benefit from the current cir- s a cumstance to determine the lowest values (i.e. the zeroes) of the parameters to [ be used as a reference for evaluating the physical changes typical of more active 1 phases. A quiescence mass accretion rate between 1–3 × 10−9 M yr−1 can be v (cid:12) 7 derived and the difference with previous determinations is discussed. From line 8 2 emission and IR colors analysis a visual extinction of 1-2 mag is consistently 5 derived, confirming that V1118 Ori (at least in quiescence) is a low-extinction 0 . T Tauri star with a bolometric luminosity of about 2.1 L . An anti-correlation 1 (cid:12) 0 5 1 1INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio, Italy, dario.lorenzetti, : v simone.antoniucci, teresa.giannini, andrea.dipaola, gianluca.licausi, brunella nisini, roberto.speziali, i X [email protected] r a 2Fundaci´onGalileoGalilei INAF,TelescopioNazionaleGalileo, 38700SantaCruzdelaPalma, Tenerife, Spain, [email protected] 3Central Astronomical Observatory of Pulkovo, Pulkovskoe shosse 65, 196140 St.Petersburg, Russia, [email protected] 4Astronomical Institute of St.Petersburg University, Russia, [email protected] 5Isaac Newton Institute of Chile, St.Petersburg branch 6INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy, fe- [email protected] – 2 – exists between the equivalent width of the emission lines and the underlying continuum. We searched the literature for evaluating whether or not such a be- haviour is a common feature of the whole class. The anti-correlation is clearly recognizable for all the available EXors in the optical range (Hβ and Hα lines), while it is not as much evident in the infrared (Paβ and Brγ lines). The observed anti-correlation supports the accretion-driven mechanism as the most likely to account for continuum variations. Subject headings: Stars: pre-main sequence – variable – emission lines – Physical Data and Process: accretion disks – infrared: stars – individual: – individual: V1118 Ori 1. Introduction After the accumulation of most of their final mass, young stellar objects (YSOs) of low-to-intermediate mass (0.5-8 M ) appear as pre-main sequence objects while the mass (cid:12) accretion process continues at a lower rate. In this phase the source is expected to accrete from its circumstellar disk: matter moves through the viscous disk and eventually falls onto the star surface following the magnetic interconnection lines (Shu et al. 1994). Observations show that the disk accretion process takes place through rapid and intermittent outbursts, usually detected at optical and near-IR wavelengths, which can be related to a sudden in- crease of the mass accretion rate by orders of magnitude (e.g. Hartmann & Kenyon 1985, Antoniucci et al. 2008). An in-depth study of these accretion events is crucial to understand: (i) how the process eventually halts (thus determining the observed Initial Mass Function); (ii) how the bursts substantially alter the physical and chemical properties of the circum- stellar disk, with major effects on the formation of proto-planetary systems; and (iii) the mechanism(s) at the origin of such outbursts. Albeit a small and irregular photometric variations (typically 0.2-1 mag) caused by disk accretion variability is a defining feature of all classical T Tauri stars (CTTSs), several young sources display powerful outbursts of much larger intensity (up to 4-5 mag). Depending on different properties (burst duration, recurrence time between subsequent bursts, accretion rate, presence of absorption or emission lines), these objects are usually classified as FUors (Hartmann & Kenyon 1985) and EXors (Herbig 1989). These latter are more suitable for an observational monitoring, since their variations typically occur on shorter times: outbursts duration from some months to one year superposed to longer quiescence periods (years); moreover, they present accretion rates of the order of (10−6-10−7 M yr−1), and emission (cid:12) line spectra (e.g. Lorenzetti et al. 2009, Sicilia-Aguilar et al. 2012, Ko´sp´al et al. 2011). The – 3 – reader is also referred to the excellent review by Audard (2014) who gives a complete view of the EXor properties. Indeed, the nature of EXors is still very uncertain: no detailed analysis or modeling of their disk structure has been performed so far, so the mechanism responsible for the onset of the accretion outbursts is not known. Proposed scenarios involve thermal instability in the disk or gravitational instability triggered by a close companion (or planet). The latter alternative seems less probable, since in that case subsequent outbursts should occur with some periodicity instead of repeating at irregular time intervals. The very uncertain picture of EXor events stems not only from the small number of known EXor objects (around two dozen, e.g. Lorenzetti et al. 2012; Audard et al 2014), but especially from the lack of a proper multi-wavelength monitoring of their photometric and spectroscopic properties, which prevented the construction of a comprehensive database of information for these objects. For this reason, we started an observational program dubbed EXORCISM (EXOR OptiCal and In frared Systematic Monitoring - Antoniucci et al. 2013) that is intended to perform a photometric and spectral monitoring in the range 0.5-2.5 µm of about 20 objects identified as known eruptive variables (EXor) or candidates. In the framework of such a project, we present here optical and near-IR data of the typical source V1118 Ori collected during a quiescence phase in different dates from September 2006 to October 2014. During its recent history V1118 Ori underwent five documented outbursts, each lasting a couple of years (1982-84, 1988-90, 1992-94, 1997-98, 2004-06). Account for the first four events is given in Parsamian et al. 1993, Garc´ıa Garc´ıa & Parsamian 2000, Herbig 2008 and references therein. For a complete view of the V1118 Ori properties shown during its last eruption, see Audard et al. 2005, 2010; Lorenzetti et al. 2006, 2007. Recently, Reipurth et al. (2007) discovered the binary nature of V1118 Ori, finding a close companion separated by 0.18 arcsec and about a factor 1.4 fainter in the Hα filter (∼ 0.4 mag). Typically, outburst phases of EXors are monitored more frequently than quiescence ones, although these latter have exactly the same relevance (e.g. Sipos et al. 2009). In fact, only during these phases the lowest values (the zeroes) of the different parameters can be accurately evaluated so allowing one to compute the physical changes, once the outburst values are obtained. Moreover, because of their longer duration, the quiescence phases can be observationally traced more easily than outbursting ones. Unfortunately, the quiescence status of V1118 Ori has never been thoroughly sampled, and in this paper we try to fill this gap. In Sect.2 optical and near-IR observations are presented; the results are analysed in Sect.3, while our concluding remarks are given in – 4 – Sect.4. 2. Observations 2.1. Near-IR imaging Near-IR data were obtained at the 1.1m AZT-24 telescope located at Campo Imper- atore (L’Aquila - Italy) equipped with the imager/spectrometer SWIRCAM (D’Alessio et al. 2000), which is based on a 256×256 HgCdTe PICNIC array. Photometry was performed with broad band filters J (1.25 µm), H (1.65 µm), and K (2.20 µm). All the observations were obtained by dithering the telescope around the pointed position. The raw imaging data were reduced by using standard procedures for bad pixel removal, flat fielding, and sky subtraction. Photometric data are listed in Table 1 while the derived light curves are depicted in the three panels of Figure 1 for the J, H, and K band, respectively. In the bottom panel (J band) we evidence two groups of activity phases: a long-term quiescence state (blue dots) and a short period of moderate activity (red dots). These states have been arbitrarily identified with a J-band magnitude greater (less) than 12.4, respectively. We will discuss these phases in deeper detail in Sect.3.1. Near-IR data cover a period lasting eight years from September 2006 to October 2014; they have been collected without a systematic cadence and with no monitoring for long periods (of about one year), during which, however, no sign of outburst was reported (from both AAVSO circulars and Astronomer’s Telegrams). Signs of modest activity (about 0.4 mag peak to peak) and short duration are superposed to such a long quiescence state (see Figure 1) that follows the last outburst, whose complete photometry is given elsewhere (Audard et al. 2010; Lorenzetti et al. 2006, 2007). 2.2. Optical spectroscopy Opticalspectraweretakenontwodifferentoccasions(2014March25andAugust12, JD 2456741 and 2456881, respectively). The first was obtained with the 8.4m Large Binocular Telescope (LBT) using the Multi-Object Double Spectrograph (MODS - Pogge et al. 2010). The dual grating mode (Blue + Red channels) was used for a total integration time of 20 min to cover the 0.35 - 0.95 µm spectral range with a 0.6 arcsec slit (resolution ∼ 2000). The second spectrum was obtained with the 3.6 m Telescopio Nazionale Galileo (TNG) using the Device Optimized for the LOw RESolution (DOLORES) instrument. The low resolution red (LR-R) grism was used for a total integration time of 30 min to cover the – 5 – 0.50-0.95 µm spectral range with a resolution of ∼ 700. In both cases (LBT and TNG) images were bias and flat-field corrected using standard procedures. After removing sky background, the two-dimensional spectra were extracted and collapsed to one dimension. For both spectra, wavelength calibration was achieved through available lamp exposures, while spectral calibration was obtained from observations of spectro-photometric standards. TheopticalspectraofV1118Oriaredepictedindifferentcolors(blackforLBT,redforTNG) in Figure 2. These are the only quiescence spectra at a high level of sensitivity comparable with that of Herbig (2008) data. Both spectra show an extraordinary degree of repeatability concerning the continuum shape, whereas the derived line fluxes present variations of less than20%. Suchanoccurrencemightbetheresultoftheextremesteadinessofthisquiescence state, that, as such, can be considered very suitable for deriving the parameters of the object in its low state. 2.3. Near-IR spectroscopy A low resolution spectrum (R ∼ 500, slit width 1 arcsec) was obtained on 2014 August 26 with NICS at TNG with two IR grisms IJ (0.90 - 1.45 µm) and HK (1.40 - 2.50 µm),in two subsequent exposures of 20 and 25 min, respectively. The standard ABB(cid:48)A(cid:48) mode was exploited within a long slit oriented at a position angle of 40◦ in order to minimize the flux of a close field star entering the slit. The spectral images were flat-fielded, sky- subtracted,andcorrectedfortheopticaldistortioninboththespatialandspectraldirections. Telluric features were removed by dividing the extracted spectra by that of a normalized telluric standard star, once corrected for its intrinsic spectral features. Wavelength and flux calibration were obtained from arc lamps and from our photometric data taken in the same period, respectively. InFigure3bothportions(IJandHK)oftheresultingnear-IRspectrum are given, labelling the relevant features identified. 3. Results and analysis 3.1. Near-IR photometry Our images are not able to resolve the companion and no other high-angular resolution observations exist in other bands, hence we cannot precisely evaluate how the companion properties affect the quiescence parameters of V1118 Ori. Therefore, until this case will not be solved by future observations, we will not perform any (highly hypothetical) correction to the observed values derived for V1118 Ori, also considering that if a difference of 0.4 mag – 6 – maintains over the entire spectral range, such correction would be marginal. In Figure 4 the near-IR two-colors plot is presented based on the photometric data given in Table 1. Data points are depicted with different colors (blue and red) to indicate the two different levels of activity evidenced in Figure 1 (see Sect.2.1). From the inspection of the two-colors plot, two considerations can be retrieved. First, all the data roughly cluster in the locus typical of T Tauri stars of a late spectral type and very low extinction. In particular, a valueofA (cid:39)1-2magcanreasonablyaccountforthedatadistribution. Second, aseparation V between the color of the quiescence phase (blue) and that of the moderate activity occurred during years 2008-2009 (points in red) is recognizable. In particular, we depicted with black filled dots the median values of the two distributions (considering 1σ error). The same trend (i.e. that different colors are associated even with modest continuum variations) has been found analysing also the light-curves of different EXors (Giannini et al. in preparation). Indeed, more significant decreases occurring in both the colors (i.e. a blueing effect) are commonly associated to the outburst phases of EXors (Lorenzetti et al. 2007, Audard et al. 2010; see e.g. Fig.1 of Lorenzetti et al. 2012). In this latter paper it is discussed how these variations cannot be accounted for simply by extinction, but rather by an additional thermal component of the emission. Such a circumstance seems to be confirmed also for the moderate activity presented here, since the red points are located fairly orthogonal to the extinction curve rather than along it. Taking into account the lowest photometric values even detected, Audard et al. (2010) provided a plot of the quiescence Spectral Energy Distribution (SED) (their Figure 15- left) and an estimate of 2.0 L for the bolometric luminosity. By substituting their JHK (cid:12) photometry with our values taken on 2007 Mar 12, and by applying the on-line fitting procedure1 (Robitaille et al. 2006, 2007), we obtain practically the same value of bolometric luminosity (2.1 L ). Moreover, the output parameters (such as T = 4080 K and M = 0.7 (cid:12) (cid:63) (cid:63) M ) are well compatible with the known physical parameters of V1118 Ori (T (cid:39) 3700 K; (cid:12) (cid:63) M = 0.4 M - Hillenbrand 1997). (cid:63) (cid:12) 3.2. Optical and near-IR spectroscopy The emission lines detected in the spectrum of the target are among those commonly observedinactiveyoungsources. AlistoftheselinesisgiveninTable2. Themostprominent emission features are the HI recombination lines of the Balmer and Paschen series, which are commonly associated with flows of accreting gas (e.g. Calvet et al. 2000, 2004). Balmer 1Available at http://caravan.astro.wisc.edu/protostars/sedfitter.php – 7 – lines are clearly visible up to H15 in the MODS spectrum, but no significant Balmer jump can be spotted at the end of the series, suggesting a fairly weak Balmer continuum. The spectrum shows also many permitted transitions of He I in the optical range and the He I line at 1.08 µm, which is indicative of stellar winds (e.g. Edwards et al. 2006). Other permitted lines are those of Ca II (H and K line doublet at 0.39 µm and the triplet at 0.85-0.87µm) and the OI line at 0.845 µm. Weak forbidden emission lines of [O I] at 0.630 µm and [S II] at 0.636 µm (which are typical tracers of shocks driven by jets, see e.g. Giannini et al. 2008) are not detected in the spectrum of the source, although they are present as strong nebular contribution eliminated by the sky emission subtraction. This circumstance and the non-detection of [Fe II] (e.g. lines at 0.71-0.74, 1.25, and 1.64 µm) and H (2.12 µm) transitions indicate that, at least in 2 the current quiescence state, there is no significant outflow activity from the source. This result is supported by the H images of the Catalogue of Molecular Hydrogen Emission-Line 2 Objects (MHOs - Davis et al. 2010), where some H filamentary structures are present in 2 the field, but unrelated with V1118 Ori. From the observed emission lines we derived an estimate of the mass accretion rate ˙ (M ) of the quiescent phase of V1118 Ori. For that we employed the set of empirical acc relationships that connect line and accretion luminosity (L ) derived by Alcala´ et. al acc (2014) in a sample of young active T Tauri stars in Lupus. By adopting a distance of 400 pc, we computed the accretion luminosity from 24 different tracers, avoiding blended lines. The L valuesthusinferredwerethenconvertedtomassaccretionratesbyusingtherelationship acc (e.g. Gullbring et al. 1998): L R (cid:18) R (cid:19)−1 ˙ acc ∗ ∗ M = 1− , (1) acc GM R ∗ in where we assumed M = 0.4M , R = 1.29R (Hillenbrand 1997, Stassun et al. 1999), ∗ (cid:12) ∗ (cid:12) ˙ and a typical inner radius R = 5R . The M values that we derive by adopting a visual in ∗ acc extinction A = 1 are reported in Table 2. These are comprised in the interval 2 ×10−10 V and 4 ×10−9, with a median M˙ of about 1 ×10−9 M yr−1and a 1σ dispersion of 7 ×10−10 acc (cid:12) M yr−1. By assuming A = 2 instead, we obtain a median accretion rate of about 3 ×10−9 (cid:12) V M yr−1with a dispersion of 1.6 ×10−9 M yr−1. The single accretion rates derived in both (cid:12) (cid:12) cases from all 24 lines are shown in Fig. 5. ˙ We note that our M estimates are much lower than the previously estimated qui- acc escence M˙ of 2.5 ×10−7M yr−1 that was derived by Audard et al. (2010) from SED acc (cid:12) modelling; a further discussion on this aspect is given in Sect. 3.3. – 8 – 3.3. Comparison with the outburst phase We perform here a comparison between our inferred quiescence parameters and those derived during more active phases. Bolometric luminosity L - From the SED fitting, a value of 2.0 L is given (Audard bol (cid:12) et al. 2010 and confirmed in Sect.3.1) for the quiescent luminosity. Different estimates are given for the outburst luminosity: 25.4 L (Lorenzetti et al. 2006) and 7.4 L (Audard et (cid:12) (cid:12) al. 2010). These values refer to two different outbursts that likely exhibit different levels of brightness, nevertheless a substantial increase of the luminosity certainly occurs, related to the appearance of the spot onto the stellar surface and to the thermal disk contribution. Visual extinction A - From the near IR two-colors plot (Figure 4) and from line V emission analysis, A values of about 1-2 mag are consistently obtained. The extinction V does not seem to change in the outburst during which Audard et al. (2010) derived, from X-rays column density, A values of 1.7+0.8 mag or 1.4+0.6 mag, for R equal to 3.1 or 5.5, V −0.6 −0.5 V respectively. A constant extinction suggests that changes of other physical parameters are not attributable to significant amounts of intervening dust (see also Audard et al. 2010; Lorenzetti et al. 2009). Mass accretion rate M˙ - In Sect. 3.2 M˙ values of 1 or 3 ×10−9 M yr−1 were acc (cid:12) derived, depending on the assumed A , 1 or 2 mag, respectively. This value is two orders of V magnitude lower than the previously estimated quiescence M˙ of 2.5 ×10−7M yr−1 derived acc (cid:12) by Audard et al. (2010) from SED modelling. This discrepancy is likely related to the different methods employed for the computation of the accretion rate. Accretion estimates from the emission lines are to be regarded as more reliable, since the lines are believed to trace the accretion columns or the strong accretion-related winds from the object. Moreover, the empirical accretion luminosity-line luminosity relationships, which are widely used as a ˙ proxyforderivingM , aredirectlycalibratedfrommeasurementsoftheUVexcessemission acc from the accretion shock (e.g. Alcala´ et al. 2014, Muzerolle et al. 1998). Finally, we note ˙ that the M values we find for the quiescence of V1118 Ori are completely consistent with acc the accretion rates measured in most T Tauri objects (e.g. Natta et al. 2006, Alcala´ et al. 2008, Biazzo et al. 2012, Antoniucci et al. 2011, 2014). ˙ For a comparison, we applied the emission line method to compute M to our 2006 acc ˙ data (note that at that time the relationships for deriving M from line fluxes were not acc ˙ available yet). From three bright Pashen lines (Paβ, Paγ, and Paδ) we get M value ∼ acc 1.0 ×10−7M yr−1 namely around 2 orders of magnitude higher than the quiscence value. (cid:12) Notably, this value is lower not only than the outburst value of Audard et al. (2010) of 1.0 ×10−6M yr−1 but even than their quiescence value of 2.5 ×10−7M yr−1 . While the (cid:12) (cid:12) – 9 – difference between the two outburst values could be ascribed to the different outburst phases sampled in Lorenzetti et al. (2006) and in Audard et al. (2010), the inconsistency between our outburst value and the quiescence one by Audard et al. can only be a result of the ˙ different computation methods. Finally, we note that our outburst determination of M / acc ˙ M is within the range (roughly 2-20) predicted by jet launching models (Shu et al. 2000, loss ˙ Ko¨nigl & Pudritz 2000, Ferreira, Dougados & Cabrit, 2006), if we take the value of M = loss 4.0 ×10−8M yr−1 obtained from the HI recombination lines. (cid:12) Emission lines - As listed in Table 2 the optical-IR quiescence spectrum of V1118 Ori is dominated by HI and He I recombination lines. Very few and faint metallic lines are also present. Such a situation is the same reported by Herbig (2008), who observed the source twice, one in outburst and one in a fading phase. While in the former phase he noticed the prominence of H I, He I, Ca II, Fe I, Fe II, and other neutral and ionized metals, when the star was much fainter the spectrum had changed radically: only HI and He I emission lines remained strong. Also our near-IR spectrum, taken during the last outburst (Lorenzetti et al. 2006) showed metallic (e.g. Na I) and CO emission features, now completely disappeared, even if we observed at higher sensitivity. In particular, CO emission is usually associated with large amounts of warm gas (T∼3000 K) in the inner regions of the circumstellar disc, which is indicative of an active phase of accretion (Najita et al. 1996; Lorenzetti et al. 2009; Ko´sp´al et al. 2011). During a similar quiescence phase, Herbig (2008) observed also TiO absorption bands and the Li I 6707 absorption line. While TiO bands are clearly observed in our spectrum, Li I is absent, possibly because of a superposition of emission and absorption, both recurrent on different activity stages of V1118 Ori (Herbig 2008). However, we should have been able to detect a faint Li I feature similar to that observed by Herbig at just a 3σ level ((cid:39) 7 ×10−17 erg s−1 cm−2) over the continuum. In our quiescence spectrum Ca II emission lines are also present, but no comparison can be made with the Herbig (2008) spectrum that did not cover this spectral range. However, the presence of Ca II lines cannot be considered a peculiarity, as they are quite ubiquitous in T Tauri systems. 3.4. Equivalent widths and continuum In the general context of the debate on whether the EXor events are accretion or ex- tinction driven, it is worthwhile to analyse the relationship between lines and continuum emission. In particular, we aim at comparing the line emission behaviour in phases charac- terized by a different level of activity, i.e. how the EW varies with the increasing underlying continuum. First of all we notice that the only member of the EXor class analyzed in this respect – 10 – (PVCep) shows a clear correlation (typical regression coefficient ≥ 0.9) between line and continuum flux (Lorenzetti et al. 2013). Since HI-recombination lines are considered as good tracersoftheaccretionrate(e.g. Muzerolleetal. 1998)theobservedcorrelationsupportsthe idea that accretion-driven mechanism is the most likely to account for continuum variations. Noticethataccretionormasslossprocessesarebothcompatiblewiththeobservedbehaviour, ˙ ˙ since their ratio M / M is roughly in the range 2-20. Although line and continuum acc loss fluxes are correlated, we can provide a more quantitative information by directly comparing the line EW and the continuum itself. Literature data concerning the EW variations of prominent emission lines and those of their underlying continua are taken starting from the list of EXors and candidates (Loren- zetti et al. 2012, their Table 1). We report in Tables 3 and 4 only the data that refer to simultaneous observations of HI recombination lines Hβ and Hα and the continuum in the bands B and R, respectively. Providing that intra-day or day time-scale variations are usually expected to be modest, in few occasions, the values of EW and continuum have been assigned to the same date (within a maximum distance of 3-4 days), even if not strictly si- multaneous. In Figure 6 the results of our literature search are depicted. The same exercise was done for the near-IR recombination lines Paβ, Brγ and the relative photometry in the J, K bands, respectively. For the sake of compactness, near-IR data are not listed in a Table, but are also presented in the same Figure 6 and discussed below. The anti-correlation, evident for V1118, occurs also for the majority of other sources when the optical lines (Hβ and Hα) are considered, while for the near-IR lines (Paβ and Brγ) the anti-correlation is not as much evident, being ascertainable only for about 50% of the presented cases. However, if we take into account only the most significant variations, namely those with ∆EW ≥ 100%, or ∆mag ≥ 2, the total percentage (considering both optical and near-IR lines) of anti-correlations increases to about 80%. In conclusion, the existence of an anti-correlation can be reasonably confirmed as a general property of the EXor class of objects: a result already supported by previous investigations on individual objects (e.g. Cohen et al. 1981, Magakian & Movsessian 2001, Acosta-Pulido et al. 2007). The anti-correlation indicates that the continuum presents larger (likely faster) varia- tionsthanthoseofthelines, whichmeansthatcontinuumandlinesdonotobeytoacommon mechanism of heating and cooling. Such a circumstance tends to rule out the variable ex- tinction as cause of the observed variability, since in that case a constant value of EW should be expected for any continuum fluctuation. Even a selective obscuration can be ruled out: dust should be located at the dust condensation zone, very close to the star and, as such, it should obscure the stellar photosphere more than the accretion columns and the wind regions.