Spectroscopy of southern Galactic disk planetary nebulae. Notes on chemical composition and emission-line stars
aa r X i v : . [ a s t r o - ph . S R ] J u l Astronomy & Astrophysicsmanuscript no. pap7_astro-ph c (cid:13)
ESO 2018January 7, 2018
Spectroscopy of southern Galactic disk planetary nebulae ⋆ Notes on chemical composition and emission-line stars
S.K. Górny
N. Copernicus Astronomical Center, Rabia´nska 8, 87-100 Toru´n, Polande-mail: [email protected]
Received June 2013; accepted June 2014
ABSTRACT
Aims.
We present low resolution spectroscopic observations for a sample of 53 planetary nebulae (PNe) located in the southern skybetween Vela and Norma constellations and pertaining to the Galactic disk with expected Galactocentric distance range of 5 to 10 kpc.
Methods.
We derive nebular chemical composition and plasma parameters with the classical empirical method. For most of theobserved objects this has been done for the first time. We compare our results to published data for PNe of the Galactic bulge and PNein the inner-disk region with expected typical Galactocentric distance of about 3 kpc. We use the spectra to search for emission-linecentral stars in the observed sample.
Results.
The distributions of the chemical abundances of the observed disk sample are generally indistinguishable from Galacticbulge and inner-disk PNe populations. The exceptions are possible di ff erences in the He / H distribution, as compared to bulge PNeand Ne / Ar, as compared to the inner-disk PNe sample. The derived O / H ratios for the observed disk PNe fit to the concept of flatteningof the chemical gradient in the inner parts of the Milky Way. Investigating the spectra, we found six new emission-line central starscomprising examples of all known types: WEL, VL, and [WR]. We confirm that these types represent three evolutionary unconnectedforms of enhanced mass-loss in the central stars of PNe. We note on the problem of high ionisation PNe with nebular C IV emissionthat can mimic the presence of WEL central stars in 1D spectra.
Key words.
ISM: planetary nebulae: general – Galaxy: abundances – stars: Wolf-Rayet
1. Introduction
Planetary nebulae (PNe) are a very short evolutionary phase inthe life of low- and intermediate-mass stars (0.8 – 8 M ⊙ ) thatoccur after they leave the asymptotic giant branch (AGB) andbefore they end their lives as white dwarfs (Iben 1995). Dur-ing the AGB and in particular, at the tip of this phase of evo-lution, stars experience strong winds that e ffi ciently enrich thesurrounding interstellar medium with huge amounts of gas, dust,and molecules from the outer layers of the star (e.g., Herwig2005). When mass loss stops, these stars leave the AGB andrapidly increase their e ff ective temperatures preserving a roughlyconstant luminosity. When the ionisation of the ejected gas bythe central star becomes possible, a new PN emerges composedof the matter formerly expelled from the progenitor.A better knowledge of the PNe phase is necessary for un-derstanding the final fate of stars like the Sun but also to studythe formation and the chemical evolution of the Milky Way andother galaxies. The PNe have several properties that make themvery good tools in this respect. They are good indicators of thechemical composition of the interstellar matter from which theprogenitor stars were born (see, e.g., Chiappini et al. 2009). Dueto the wide mass range of their progenitors, the PNe that we nowobserve have been created by stars that formed at very di ff er-ent epochs. In addition, their narrow emission-line nature makesthem observable at very large distances. ⋆ Based on observations made at the South African Astronomical Ob-servatory
Thanks to a considerable e ff ort, hundreds of new PNe havebeen discovered in the Milky Way in the last two decades (fora review see Parker & Frew 2011). However, published analysisbased on the observed PNe properties still frequently use limitedand biased samples. The first observing bias is the natural con-dition that the most easily accessible objects (brightest or simplynear-by) are first to be observed and analysed. Even if a substan-tial number of such data is collected, it does not necessarily meanthey properly represent the PNe population across the Galaxy.The problem that observational selection e ff ects have to beproperly taken into account has been underlined many times inthe past (e.g., Stasi´nska & Tylenda 1994). Nevertheless, theycan remain one of the major concerns, while investigating theabundance gradients in the Milky Way. By analysing the sam-ples collected by di ff erent authors, it can be noted that they areoften dominated by the relatively close objects.In some cases, selection e ff ects may appear unexpect-edly. For example, Górny et al. (2009) reported that Wolf-Rayet([WR]) type central stars are probably related to the intrinsicallybrightest PNe in a given population. The reason for this is un-known. It is important here that this property remained unno-ticed until a dedicated, su ffi ciently deep search of new [WR] ob-jects was undertaken that also incorporated the fainter Galacticbulge PNe.For this reason, we think it is still necessary to collect newobservational data to further minimise the presence and influ-ence of selection e ff ects in PNe related studies. In this paper,we present low resolution optical spectroscopic observations of53 PNe that are located in the southern sky between Vela and Article number, page 1 of 35 ig. 1.
The distribution of the observed PNe on the sky in galactic co-ordinates, dark circles. Open grey circles mark other PNe catalogued byAcker et al. (1992) and filled grey circles PNe from Parker et al. (2006)and Miszalski et al. (2008).
Fig. 2.
The distribution of the nebular F(H β ) fluxes for PNe observedin this work, dark hatched bars; PNe included in other large spectro-scopic surveys (see text for the references) - grey hatched bars; andother PNe from Acker et al. (1992), as open bars. Norma constellations with an expected Galactocentric distancerange of 5 to 10 kpc. The sample and observations are describedin Sect. 2. The results of the search for new emission-line centralstars is presented in Sect. 3. In Sect. 4, we derive the chemicalcomposition of the observed PNe and compare them briefly withabundance distributions for Galactic bulge and inner-disk PNepopulations. The main results of this work are summarised inSect. 5.
2. Low resolution optical spectra
We present observations of 53 PNe that are located near theplane of the Milky Way disk with Galactic longitude from l = ◦ to 340 ◦ . Their on-sky distribution is presented in Fig. 1.Spectra of these objects were secured with the 1.9-meter tele-scope of the South African Astronomical Observatory in April2003, May 2004, June 2005, and May 2006 as an auxiliaryprogram during observing runs dedicated to the search of newsmall PNe towards the Galactic bulge (Górny 2006) when thatpart of the sky was not accessible. No strict selection cri-teria were employed to choose the targets; however, objectsnot listed in large surveys like de Freitas Pacheco et al. (1991, 1992); Kingsburgh & Barlow (1994); Cuisinier et al. (1996);Milingo et al. (2002); Kwitter et al. (2003) were preferred and,therefore, we have only 13 sources in common with these au-thors. Some additional preference was given to PNe with anunknown type of the central star and without information onmeasured stellar flux. Three additional PNe with Spitzer spectrawere observed in April 2011.In Fig. 2 we present the distribution of total apparent nebularH β fluxes for our observed sample, as seen in the dark hatchedbars. We compare them to the distribution for the PNe located inthe same direction of the sky and presented in above mentionedpapers or included in more recent papers, such as Cavichia et al.(2010); Henry et al. (2010); Milingo et al. (2010). For a refer-ence, the remaining PNe of this region from Strasbourg-ESOCatalogue of Acker et al. (1992) are shown. As a result of our se-lection approach, the sample we observed is composed of fainterPNe. Our targets were also smaller. The median diameter ofPNe we observed was about 8 arcsec, whereas the PNe includedin other papers had a median diameter of 10 arcsec, as comparedto almost 16 arcsec for a general PNe population in that region(238 PNe from Acker et al. 1992).In Table 1, the detailed log of observations is presented. ThePNe are identified by their PN G identifier (Galactic coordinates)and usual names. The typical spectral coverage was 3500-7400Åwith an average resolution of 1000 which allows for detection ofall important nebular lines without serious blending. The slitwidth was usually set to 1.8 arcsec, which is slightly larger thanthe typical seeing conditions at the site. The slit orientation wasalways E-W, and it was positioned directly on the central starif it could be identified or roughly at the geometrical center ofthe nebula. The CCD was read with a 1x2 pre-binning in thespatial direction, which is along the slit. The slit width and itsorientation could in principle lead to some loss of the stellar lightdue to seeing variations and di ff erential atmospheric refraction.The latter e ff ect could have influence on relative line ratios forthe smallest observed PNe. To avoid this, we tried to observe allobjects at their minimum air-masses. Their values are given incolumn 5 of Table 1.The integration time of the observations varied from 20 to90 minutes and was divided into two or three sub-exposures. Inmany cases, additional shorter exposure lasting from 3 minutesto only 15 seconds were executed to ensure unsaturated detectionof the strongest lines: H α , [O III] λ / or [N II] λ ff erent spectroscopic standardstars were observed (LTT 3218, LTT3864, LTT4364, LTT 7987,LTT 9239 CD -32 or Eg 274). Since no order blocking filterswere used, some contamination to the red light of the standardstars is possible from the second order blue continuum. Thespectrograph was, however, characterised by a general low sen-sitivity to blue light. We checked during tests in 2011 and 2012with the same instrument and configuration for stars, LTT 3218and CD -32, that contamination was adding only up to 4% ofadditional light at 7600Å. The e ff ect was linear in wavelength(from about 6000Å upward) but would sometimes disappear de-pending on the sky conditions of a given night. We have there-fore not corrected the measured lines for this e ff ect. In practise,its influences for our PNe would be measurable only for [O II] λ . We anyway correct λ /
30 lines to measurements of their bluecounterpart [O II] λ Table 1.
Log of observations presenting PN G numbers, usual names, year of the observation, exposure time in seconds; mean airmass duringobservation, and nebular diameter in arcsec.
PN G name date exp Z diam PN G name year exp. Z diam268.4 + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + to reduce and calibrate the spectra. These included bias sub-traction, flat-field correction, atmospheric extinction correc-tion, wavelength, and flux calibration and extraction of the 1-dimensional spectra. For the standard stars and most of the ob-served PNe, this was done in the usual manner by summing theappropriate rows of the sky subtracted frames. In the case ofsome PNe, in particular, those located close to the Galactic planein crowded fields a multi-step method similar to the one de-scribed in Górny et al. (2009) had to be applied. In this methodbefore extracting 1D spectra, all the background sources have tobe removed. This includes not only sky continuum emission andtelluric and interstellar lines but also stellar continua, includingthat of the PN central star. Intensities of the nebular lines werefinally measured from the 1-dimensional spectra by employingthe REWIA package , assuming Gaussian profiles and perform-ing multi-Gaussian fits when necessary.The line intensities have been corrected for extinction byadopting the extinction law of Seaton (1979) to reproduce thetheoretical case B of Balmer line ratios at the electron tempera-ture and density derived for the object. The same iterative pro-cedure, as the one described in Górny et al. (2009), was appliedusing the measured H α / H β ratio. As a result the procedure wasusually not giving the theoretically expected ratios of H γ / H β and / or H δ / H β . This can be due to deviations from the adopted ESO-MIDAS is developed and maintained by the European SouthernObservatory REWIA is a data processing program developedby J. Borkowski at Copernicus Astronomical Center ∼ jubork/rewia/ extinction law for individual PNe or higher uncertainty of fluxcalibration in the blue part of the spectra. If the deviations inH δ and / or H γ were systematical in one direction and larger thanexpected from purely observational uncertainties, we applied anadditional correction procedure (Górny et al. 2009) to bring theH γ / H β and H δ / H β ratios to their theoretically expected values.The correction factors typically amounted to 7% and 11% for H γ and H δ lines, respectively. A proportional wavelength dependentcorrection was than applied to all the nearby lines, including theimportant [O iii ] λ ii ] λ , we present the measured anddereddened intensities of all important nebular lines on the scaleof H β =
100 for the observed PNe. In cases when the additionalcorrection described above was necessary, the lines are markedwith "c" in Table B.1.
Figure 4 presents intensity ratios of the [O III] doublet lines λ λ λ λ λ ffi culty All appendices are available online Article number, page 3 of 35 ig. 3.
Illustrative examples of the acquired spectra of low ionisation planetary nebula (top panel) and a high ionisation nebula (bottom panel)in our observing programme. to precisely relate the measured value to the other much fainterlines. In the ratio shown in Fig. 4, the larger source of error isindeed measurements of the λ λ λ λ λ α line sep-arating them. It can be seen in Fig. 5 that the majority of theobserved ratios are well confined between the 5% deviations.There are, however, some outliers, in particular, for cases when[N II] lines are fainter, and it can be noted that the intensity of the λ α line takesplace. However, this has to be a very minor e ff ect on our results,since [N II] λ ff erent references. Wefound instead that our list of targets has 11 objects in commonwith Dopita & Hua (1997), who measured absolute fluxes of se-lected lines for a large sample of southern sky PNe. In Ap-pendix A, we present and discuss the comparison of our mea-surements with those of Dopita & Hua (1997).As a result of all above mentioned evaluations, we concludethat the basic accuracy of all the line measurements from ourspectra can be adopted as roughly 5%. In cases marked with acolon in Table B.1, the uncertainty is estimated around 20%, andin the rare cases of extremely weak lines or lines contaminatedwith sky features or field stars (marked with semicolon), this canbe as high as 40%. Article number, page 4 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Fig. 4.
Intensity ratio of the [O iii ] λ λ iii ] λ β ). The dashed line representsmean value for the presented observations, and the dotted lines are 5%deviations from it. Fig. 5.
Intensity ratio of the [N ii ] λ λ ii ] λ β ). The long dashed linerepresents median value for the presented observations, and the dottedlines are 5% deviations from it.
3. Search for PNe with emisssion-line stars
A large fraction of PNe exhibit emission-line central stars (CSs).As can be inferred from the work of Weidmann & Gamen(2011b), they compose about one third of PNe with classifiedCSs. Two main types of emission-line central stars are widelyrecognised in the literature (Tylenda et al. 1993): the Wolf-Rayettype central stars ([WR]) and weak emission-line CSs (WELs).The spectra of the first group closely resemble those of the gen-uine massive population I Wolf-Rayet stars of the WC spectral subclass with strong and wide emissions of C, O, and He. TheWELs seem to be a less homogeneous group with usually onlynarrow and much fainter C IV doublet λ /
12. Recently, theexistence of a separate third group of PNe with emission-linecentral stars has been proposed by Górny et al. (2009), who in-vestigated a large sample of PNe in the Galactic bulge and inner-disk region. This new class of CSs was named VL or very late type and was found in the low ionisation PNe with a stellar spec-tra represented by C III and C II emission lines, but, again narrowand less strong. In the classical scheme, they could be assignedto [WC 11] subtype. The sample of PNe analysed in the presentwork gave us the possibility to check if VL type of objects arealso present among Galactic disk PNe.We used our acquired data to search for new emission-lineCSs. We checked our reduced 2D and integrated 1D spectrafor the presence of characteristic emission-lines utilised for thespectral classification as listed in Górny et al. (2004) and thecompound of C and N lines around 4650Å, which is usually as-sociated with the WELs type objects (Tylenda et al. 1993).We have found three new WELs, two new [WR]-type, andone new VL PNe. The spectra of the new WELs PNe are pre-sented in Fig. C.1 and of the new [WR] and VL type objects inFig. C.2 in Appendix C. In both figures, the expected locations ofthe characteristic emission lines are indicated with dotted lines,and if positively identified, they are marked with the ion name oftheir origin.In addition, we also registered stellar emission lines in al-most all cases when the previous emission-line classification al-ready existed (Weidmann & Gamen 2011b). The only exceptionwas He 2-63, which is probably due to the short exposure timeof our observation and the NGC 5979 that turned out not to be atrue but a mimic of a WEL object (see below). We hereby con-firmed the [WR]-type nature of two CSs but reclassified threeother objects to be a VL-type PNe. In Fig. C.3, we present spec-tra of the reobserved and confirmed PNe with previously knownemission-line CSs.In Table B.2 in Appendix B, we present a complete list ofnew and previously known emission-line CSs that are presentamong PNe from our observing list. In the first column we givetheir usual names. In column 2, the full width at half maximumof the main stellar emission line is presented but only if it wasexceeding the instrumental width. In practise, these measure-ments in Table B.2 are always referring to C IV λ λ Article number, page 5 of 35 .2. Notes on individualPNe
Objects PB 5, My 60, and He 2-115, whose spectra are shownin Fig. C.1 present good examples of WELs PNe, as defined byTylenda et al. (1993). The C IV lines at λ /
12 are visible asseparate doublet components and are much fainter and narrowerthan in the case of [WR] PNe. Other lines often associated withWELs, such as λ λ λ λ λ λ /
10 of λ λ λ λ λ λ λ λ β . We, therefore, rate this object to the VL-type PNe with emission-line CSs.The objects He 2-131 and He 2-108 are well studiedemission-line objects with CSs models available in litera-ture (Hultzsch et al. 2007; Pauldrach et al. 2004; Kudritzki et al.1997). The object He 2-108 was recently analysed byPottasch et al. (2011) with apparently lacking good optical spec- Fig. 6.
Spectrum of NGC 5979 around 4640Å (left) and 5800Å(right).
Fig. 7.
Spectrum of NGC 3918 around 4640Å (left) and 5800Å(right). tra. We feel both PNe are worth to be included in the sample forat least illustrative purposes how they would be processed andclassified with the kind of spectra we collected.He 2-131 and He 2-108 were first classified as WELs objectsin Tylenda et al. (1993). However, both objects display not nar-row C IV λ /
12 emissions but a C III λ λ λ λ /
12 in absorption. Thecentral star of He 2-131 is surrounded by a low ionisation nebulawith [O III] λ β , whereas thestar is presumably hotter and, therefore, the intensity of [O III]5007 is almost two times larger than H β in the case of He 2-108.We would classify them both, however, as VL type. The WELs type PNe are probably a heterogeneous group of ob-jects that has already been suggested by Tylenda et al. (1993).Recently, it has been proposed by Corradi et al. (2011) that thestellar emission lines of C and N attributed in WELs to the en-hanced mass loss may originate from the irradiated zone in closebinary systems. Miszalski et al. (2011) argue this is actuallythe case of NGC 6326, which they observed both photometri-cally and spectroscopically. In the bottom panel of Fig. C.3,we present our low resolution spectra of NGC 6326. Faint butclearly visible emission lines of C IV at λ /
12 would nor-mally be identified as stellar and clearly would allow us to clas-sify this object as a typical WEL. The C II λ λ /
12 linesalso have the nebular origin in some PNe?The central star of NGC 5979 has been classified byWeidmann & Gamen (2011b) using the low resolution spectrathey acquired as a WEL object. In Fig. 6, we present our fullyreduced 2D spectrum of this PN. In the right panel, we showthe part of the spectrum around 5805Å, and in the left panel,the region centred on 4640Å. The lines of N III, C III, and C IVions are clearly detectable at the expected wavelengths. They allare, however, emitted from the spatially extended region and are,therefore, not of the stellar but nebular origin. The stellar contin-uum emission can also be recognised in the centre of the images.It is broadened in the spatial direction by the seeing but obvi-ously much narrower than the emission lines. If analysed using
Article number, page 6 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Fig. 8.
Nebular surface brightness S H β versus parameter S V as de-fined in an analogous way using stellar V flux. Data presented fordi ff erent types of disk PNe from the observed sample: magenta tri-angles – [WR] PNe, blue squares – WEL PNe, and green circles –VL PNe ([WC 11]-like spectra). Small symbols mark normal PNe with-out emission-line CSs detected. The lines present model calculationsfor central stars of 0.57, 0.60, and 0.64M ⊙ , adopting a simple nebularmodel (see text). only the final summed 1D spectrum, this object would perfectlymimic WEL type spectra.In Fig. 7, we show the same regions of spectrum for theNGC 3918. In the case of this object, the stellar continuum isdetectable only in the blue part. The emission lines of C IV at5801 /
12 and the combination of lines around 4650Å are againclearly not of stellar origin. In the case of the presumed C IVline identified at 4658Å, it can be noticed that the emission hastwo separate spatial components.The objects NGC3918 and NGC5979 are high ionisationPNe. From our line measurements, we derived the ratio of se-lective to total He ++ / He abundance to be 0.38 and 0.81, respec-tively. In Fig. 3, we presented the full spectrum of NGC 5979,where lines of highly ionised ions can be identified. The e ff ectivetemperature of NGC 5979 calculated with Zanstra He method isT ⋆ = ⋆ = ⊙ . In the caseof NGC 3918, those parameters can be derived as 148k K and3.52 L ⊙ . Apparently, in both these PNe some carbon is ionisedup to C + in the large part of the nebula and can give rise to linesthat are otherwise expected to be observed from stellar atmo-spheres. It was noticed by Górny et al. (2001) that there is an impor-tant di ff erence in the distribution of spectral classes among[WR] PNe located in the bulge as compared to the PNe in theGalactic disk. An apparent underpopulation of [WR] CSs inthe [WC5]-[WC7] range for disk objects was observed. In thebulge, on the contrary, [WR] CSs were found to be mostly ofthe intermediate spectral types suggesting that the Wolf-Rayetphenomenon depends on the characteristics of the investigated stellar population giving rise to the observed PNe. The new ob-servations of bulge PNe by Górny et al. (2004) and Górny et al.(2009) did not solve the problem since the comparable searchsurveys for the Galactic disk were not available. Instead, a po-tential new class of emission-line objects (VL) had to be intro-duce (Górny et al. 2009).Recently, Depew et al. (2011) published a list of newly dis-covered [WR] PNe that contains some possible intermediate[WC] class objects in the Galactic disk . Additionally, we foundor reclassified three intermediate [WC] spectral-class objects inour disk sample (see Table B.2). The first important result fromthe present work is therefore that the di ff erence in spectral classdistribution, although still present, may be not that pronounced.Possibly more such objects could be found in a deeper dedicatedsearch. The second piece of information is that the VL objectsare also present in the Galactic disk and not confined only to theinner parts of the Milky Way and its bulge in particular.In Fig. 8, we present the locations of PNe from the observedsample in the S H β versus S V plot, where S H β is the nebular sur-face brightness in H β and S V is defined in an analogous way butusing the stellar flux in the visual V band (see in Górny et al.1997). The evolutionary tracks shown in Fig. 8 have been cal-culated with a simple model of PNe by assuming total nebularmass M neb = ⊙ , a filling factor ǫ = exp = / s for central stars of 0.57, 0.60, and 0.64M ⊙ evolving in agreement with Blöcker (1995) models.It can be seen in Fig. 8 that the locations of VL PNe clearlydi ff er from those of [WR] and WEL objects. In particular, VLPNe cannot be evolutionary predecessors of either of the twoother groups, as first noted by Górny et al. (2009). Because S H β and S V are distance independent, one can directly compare lo-cations of PNe analysed in this work with Fig.11 of Górny et al.(2009), which present bulge and inner-disk emission-line CSsthat they discovered. Analogous locations are occupied in thecase of any of the three groups in both plots. We therefore canconfirm the conclusion of Górny et al. (2009) that [WR], VL,and WELs form three independent types of emission-line CSsphenomenon and that it is also true for the PNe in the Galacticdisk.The rate of occurrence of the di ff erent types of PNe withemission-line CSs is, of course, of a large importance if onewants to discuss the possible evolutionary paths of their creation.At the same time, it is very di ffi cult to be established, as the num-ber of objects that are discovered in a given sample is unavoid-ably subject to serious bias. The bias originates from the ob-servational details, selection e ff ects when choosing targets, andobvious physical constraining factors, such as the distance to thegiven population.A natural sample to compare with the present one wouldbe the 44 Galactic bulge PNe observed by Górny et al. (2004).Both groups have been actually observed with the same instru-ment and almost identical setup, but there are also di ff erences.The Galactic bulge PNe are further away and smaller, whichshould work against e ffi cient discovery of emission-line CSs inthe bulge sample due to the stronger contamination e ff ect fromthe nebulae. On the other hand, the Górny et al. (2004) samplewas preselected by choosing objects with infrared IRAS colourstypical for [WR] PNe (Górny et al. 2001). This could have animportant consequence since no such preselection was active inthe present sample. Nevertheless, taking the numbers of objects Originally, Depew et al. (2011) used di ff erent classification schemesof [WC] and [WO] subclasses, whereas we continue to use the classical[WC] scheme that range from [WC11] to [WC2]Article number, page 7 of 35 nto account discovered from original new observations in bothstudies (i.e., comparing only with sample G of Górny et al. 2004,see column 3 in their Table 4) one findss that seven WELs andtwo [WR] were discovered in the bulge by Górny et al. (2004),as compared to three WEL, two [WR] and one new VL in thepresent sample. Clearly, no final conclusions about the rate ofoccurrence of emission-line phenomenon in both environmentscan be reached in this way.The precise answer to the question of what exactly is therate of occurrence of each type of emission-line phenomenonin di ff erent environments requires constricting a more completesamples in both regions of the Milky Way. Possible selectione ff ects need to be carefully considered but is outside the scopeof the present data paper.
4. Chemical abundances and plasma parameters
We start this section with the description of the method we used.Then we analyse the calculated plasma parameters and presentthe derived chemical abundances. We finalise the result by com-paring them to the abundances of the Galactic bulge and inner-disk PNe populations that were analysed recently.
We use the code ABELION that was developed by G. Stasi´nska,which is based on the classical empirical method to derive theplasma parameters and nebular chemical abundances. The ver-sion of the code is identical with that used by Górny et al. (2009)and Chiappini et al. (2009). We first derive the electron densi-ties from the [S ii ] λ / T e (O iii ) from the [O iii ] λ / / or T e (N ii ) from [N ii ] λ / T e (N ii )to derive abundances of ions with low ionisation potential and T e (O iii ) for hydrogen and lines from other ions with intermedi-ate and high ionisation potentials. If T e (N ii ) was very uncertain(three cases) we used the T e (O iii ) for all the ions instead. If theobservational data did not allow for the stimation of the electrontemperature, the object was rejected from further considerations(five cases).As discussed in detail in Górny et al. (2009), the O + ionicabundances derived from λ λ ff ected by recombination fromO ++ ions, but this does not solve the problem, as checked byGórny et al. (2009). In Fig. C.4, we compare the O + ionic abun-dances derived from λ + from λ ff erence for the presented observations is 0.17 dex, andwe use this value to correct λ T e (N ii ). A weak correlationcan be seen in the sense that the discrepancy between λ λ T e (N ii ). We,however, attempted no fitting to this correlation when correctingthe λ + ionic abundance is a mean of thetwo values weighted by their reversed uncertainties.After the ionic abundances are computed, the elementalabundances are obtained using the ionisation correction factors(ICFs), as in Górny et al. (2009) and based mainly on the schemeof ICFs from Kingsburgh & Barlow (1994). The uncertainties inabundance ratios and other derived parameters were obtained bypropagating uncertainties in the observed emission line intensi- Fig. 9.
The electron temperature derived from [O iii ] λ / ii ] λ / ties using Monte-Carlo simulations by assuming that the princi-ple line intensity errors are of at least 5%, as explained above.In Table B.3 in Appendix B, we give the derived plasma di-agnostics and ionic and elemental abundances for 48 objects or-dered by PN G numbers. For each object, there are three rowsof data. The first row gives the values of parameters computedfrom the nominal values of the observed lines and their ratios.The second and third row give the upper and lower limits ofthese parameters, respectively. Column (1) of Table B.3 givesthe PN G number and Column (2) gives the usual name of theobject; Column (3) gives the electron density deduced from [S ii ] λ / iii ] λ / ii ] λ / T e (N ii ) is in parenthesis, T e (O iii )was chosen for all ions. Column (6) gives the He / H ratio andColumns (7) to (12) the N / H, O / H, Ne / H, S / H, Ar / H, Cl / H ratios,respectively. To avoid dealing with values that are too uncertain,we removed from further consideration any plasma parameter orabundance ratio for which the error (at two-sigma level) is largerthan 0.3 dex. We marked these values with a colon in Table B.3.
In this section, we present the plasma parameters derived for ourobserved disk PNe from Vela-Norma direction and compare itto the Galactic bulge and inner-disk samples of Chiappini et al.(2009) that were computed with exactly the same code and as-sumptions. The inner-disk sample is less well defined and in-cludes PNe that are observed in the direction of the Galacticcentre but do not pertain to the bulge, according to the stan-dard criteria. They can be located at Galactocentric distances
Article number, page 8 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Fig. 10.
The nebular abundance ratios N / O versus O / H for the threeanalysed Galactic PNe samples. The notation of symbols as in Fig. 9. estimated as less than 2 kpc up to almost 7 kpc but the medianGalactocentric distance is about 3 kpc. In Fig. 9, we plot T e (O iii )versus T e (N ii ). First, it can be noted that all disk PNe that weshow here seem to have T e larger than 10 K. Among the bulgeand inner-disk samples, there is a considerable number of objectswith temperatures below that value. From Fig. 9, the correlationbetween T e (O iii ) and T e (N ii ) seems to be at the same level fordisk PNe as for the other two groups but there are two PNe inthis sample that have T e (O iii ) ≫ T e (N ii ). In the bulge PNe sam-ple, on the contrary, there is a group with T e (N ii ) ≫ T e (O iii ).Calculating a median value of log T e (O iii ) for the disk PNe (39objects with useful data) we checked that it is 4.09 and 0.06 dexlarger than for the bulge PNe. The tests indicate the di ff erence isstatistically significant at more than 99% confidence level.Analysing the distributions of the electron density derivedfrom [S ii ] λ / ff erences, although our disksample from Vela-Norma direction seems to have more mem-bers with smaller densities. The median log N e = ++ to to-tal He abundance. The median He ++ / He for the Galactic diskPNe investigated here is 0.11. A similar value have been derivedfor the Galactic inner-disk sample, whereas very few observedPNe have any He ++ ions at all for the bulge PNe.Summarising, we would tentatively describe the disk PNefrom the sample analysed here as more evolved, of higher elec-tron temperature, and also of presumably higher ionisation levelthan the PNe in the other two samples. This is what could beexpected, since it is generally more di ffi cult to observe evolvedPNe at larger distances like the bulge or inner-disk regions. These estimates are based on distances from Cahn et al. (1992). We used Kolmogorov-Smirnov and Wilcoxson tests for all the distri-butions analysed in this work.
Fig. 11.
The nebular abundance ratios He / H versus N / H for the threeanalysed Galactic PNe samples. The notation of symbols as in Fig. 9.
One of the advantages of studding chemical abundances of PNeis that some of them bring information on the nucleosynthesisprocesses occurring in the interiors of their progenitor stars (e.g.nitrogen), whereas others are assumed to remain unchanged dur-ing the life of the star and inform about the primordial chemicalcomposition of the matter that the parent star was born from.In Fig. 10 we show the relation of O / H versus N / O for thePNe included in the sample investigated here as compared toGalactic bulge and inner-disk samples of Chiappini et al. (2009).Similar behaviour can be seen in this plot for the three groupsof PNe. There are also very few outliers. The object with thelowest O / H abundance in the disk PNe group in this plot is He 2-131 that we discussed already in Sect. 3.2 . We derive medianlog O / H = -3.46 and median log N / O = -0.37 for the disk PNe sam-ple analysed here.In Fig. 11, we plot He / H versus N / H for the analysed PNe ofthe three Galactic locations. The median value log He / H = / H > / Hnor N / O distributions, although a very convincing correlation ofHe / H with N / H can be seen in Fig. 11. The low O abundance we calculate is the result of the high T e (O iii ) ≈ λ T e (N ii ) ≈ T e is close to the lat-Article number, page 9 of 35 ig. 12. Distributions of the nebular Ne / Ar abundance ratio for thethree analysed Galactic samples: disk PNe from Vela-Norma direction(top), bulge PNe (middle), and inner-disk PNe (bottom). The medianvalues, the 25 and 75 percentiles are marked with three short verticallines above each histogram. Numbers of objects used are shown in theleft-hand parts of the panels below sample names.
Fig. 13.
The nebular abundance ratio O / H versus Galactocentricdistance for PNe observed in this work.
Figure 12 presents the comparison of Ne / Ar abundance ra-tios for the three samples of PNe. In this case, a gradual increaseof Ne / Ar can be observed from disk sample with the smallestratio through bulge PNe and towards the inner-disk sample. Thedi ff erence between our disk sample and the inner-disk PNe isconfirmed at about 99% significance level. We noticed no statis-tically significant di ff erences in distributions of any other abun-dance ratios comparing the three PNe samples.Although the group of PNe we observed is not numerousenough and, as we mentioned above, a large and properly se-lected samples should be used to study gradients of chemicalabundances in the Milky Way, we present the derived O / H abun- ter value and the preference would be given to O + from λ / H = − would be derived. dances versus the Galactocentric distances of these objects in theFig. 13. This is mostly done to demonstrate the usability of thedata we collected for this and other purposes. We used the dis-tances of Cahn et al. (1992) and found them for 19 of our diskPNe. As in previous cases, we analysed only objects with anO / H ratio errors estimated to be smaller than 0.3 dex. As seenin Fig. 13, the observed PNe are located from about 5 to 10 kpcfrom the Galactic center. Even though the presented sample ofdisk PNe is small, their locations in Fig. 13 clearly support theidea of flattening the chemical gradient in the internal parts ofthe Milky Way.
5. Summary
We presented low resolution optical spectroscopic observationsfor a sample of 53 PNe located in the southern sky between Velaand Norma constellations and pertaining to the Galactic disk.We used the spectra to analyse the chemical composition of PNeand search for new emission-line central stars. Our main resultsare as follows:1. We derived chemical abundances of 48 observed PNe, forthe first time for most of them or allowed abundances of ad-ditional, previously unobserved elements to be measured.2. We compared the nebular chemical abundances in our sam-ple with the results of Chiappini et al. (2009) for Galacticbulge and inner-disk PNe populations. We found no statisti-cally meaningful di ff erences in abundance distributions, ex-cept for He / H, that seems more abundant in the bulge PNeas compared to our disk sample and Ne / Ar with larger ratiosfound in the inner-disk PNe population.3. The oxygen abundances derived for the analysed samplefavour flattening of the O / H gradient within the inner partsof the Galactic disk.4. We performed extensive search for central stars withemission-lines and found three new WEL, two [WR] and oneVL type object. Re-analysing the spectra of previously clas-sified objects additional three members of the VL group havebeen proposed.5. We identify NGC 3918 and NGC 5979 as the possible mim-ics of WEL objects with C IV 5801 /
12 emitted from highlyionised nebulae.6. We confirmed for the first time that the VL type PNe are alsolocated outside the inner parts of the Milky Way. We identi-fied three examples of [WR]-type central stars with interme-diate spectral class [WC5]-[WC6] pertaining to the Galacticdisk.7. We argue WELs, [WR], and VL objects are three evolution-ary unrelated types of emission-line phenomenon in centralstars of PNe.
Acknowledgements.
Part of this work was supported from grant N203 511838 ofthe Science and High Education Ministry of Poland. I wish to thank M. Hajdukwho assisted during observations in June 2005 and A.D. García-Hernández forhis help in selecting targets in 2011.
References
Acker, A., Marcout, J., Ochsenbein, F., et al. 1992, The Strasbourg-ESO Cata-logue of Galactic Planetary Nebulae. Parts I, II.Acker, A. & Neiner, C. 2003, A&A, 403, 659Blöcker, T. 1995, A&A, 299, 755Cahn, J. H., Kaler, J. B., & Stanghellini, L. 1992, A&AS, 94, 399Cavichia, O., Costa, R. D. D., & Maciel, W. J. 2010, Rev. Mexicana Astron.Astrofis., 46, 159
Article number, page 10 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Chiappini, C., Górny, S. K., Stasi´nska, G., & Barbuy, B. 2009, A&A, 494, 591Corradi, R. L. M., Sabin, L., Miszalski, B., et al. 2011, MNRAS, 410, 1349Cuisinier, F., Acker, A., & Koeppen, J. 1996, A&A, 307, 215de Freitas Pacheco, J. A., Maciel, W. J., & Costa, R. D. D. 1992, A&A, 261, 579de Freitas Pacheco, J. A., Maciel, W. J., Costa, R. D. D., & Barbuy, B. 1991,A&A, 250, 159Depew, K., Parker, Q. A., Miszalski, B., et al. 2011, MNRAS, 414, 2812Dopita, M. A. & Hua, C. T. 1997, ApJS, 108, 515García-Rojas, J., Peña, M., Morisset, C., Mesa-Delgado, A., & Ruiz, M. T. 2012,A&A, 538, A54Górny, S. K. 2006, in IAU Symposium, Vol. 234, Planetary Nebulae in ourGalaxy and Beyond, ed. M. J. Barlow & R. H. Méndez, 409–410Górny, S. K., Chiappini, C., Stasi´nska, G., & Cuisinier, F. 2009, A&A, 500,1089Górny, S. K., Stasi´nska, G., Escudero, A. V., & Costa, R. D. D. 2004, A&A, 427,231Górny, S. K., Stasi´nska, G., Szczerba, R., & Tylenda, R. 2001, A&A, 377, 1007Górny, S. K., Stasi´nska, G., & Tylenda, R. 1997, A&A, 318, 256Henry, R. B. C., Kwitter, K. B., Jaskot, A. E., et al. 2010, ApJ, 724, 748Herwig, F. 2005, ARA&A, 43, 435Hultzsch, P. J. N., Puls, J., Méndez, R. H., et al. 2007, A&A, 467, 1253Iben, Jr., I. 1995, Phys. Rep., 250, 2Kingsburgh, R. L. & Barlow, M. J. 1994, MNRAS, 271, 257Kudritzki, R. P., Mendez, R. H., Puls, J., & McCarthy, J. K. 1997, in IAU Sympo-sium, Vol. 180, Planetary Nebulae, ed. H. J. Habing & H. J. G. L. M. Lamers,64Kwitter, K. B., Henry, R. B. C., & Milingo, J. B. 2003, PASP, 115, 80Lee, T.-H., Stanghellini, L., Ferrario, L., & Wickramasinghe, D. 2007, AJ, 133,987Milingo, J. B., Kwitter, K. B., Henry, R. B. C., & Cohen, R. E. 2002, ApJS, 138,279Milingo, J. B., Kwitter, K. B., Henry, R. B. C., & Souza, S. P. 2010, ApJ, 711,619Miszalski, B., Jones, D., Rodríguez-Gil, P., et al. 2011, A&A, 531, A158Miszalski, B., Parker, Q. A., Acker, A., et al. 2008, MNRAS, 384, 525Parker, Q. A., Acker, A., Frew, D. J., et al. 2006, MNRAS, 373, 79Parker, Q. A. & Frew, D. J. 2011, in Asymmetric Planetary Nebulae 5 Confer-encePauldrach, A. W. A., Ho ff mann, T. L., & Méndez, R. H. 2004, A&A, 419, 1111Pottasch, S. R., Surendiranath, R., & Bernard-Salas, J. 2011, A&A, 531, A23Seaton, M. J. 1979, MNRAS, 187, 73PStasi´nska, G. & Tylenda, R. 1994, A&A, 289, 225Tylenda, R., Acker, A., & Stenholm, B. 1993, A&AS, 102, 595Weidmann, W. A. & Gamen, R. 2011a, A&A, 531, A172Weidmann, W. A. & Gamen, R. 2011b, A&A, 526, A6 Article number, page 11 of 35 ppendix A: Comparison with emission-line fluxstandards
In this section, we compare our line measurements with datapublished by Dopita & Hua (1997). We have 11 PNe in commonwith their list of southern emission-line flux standards. They arelisted in Table A.1. In Fig. A.1, we present the comparison forthe lines of [O III] λ α , [N II] λ λ λ +
31, and [Ar III] λ ff erences have been nor-malised separately for each PNe and each line to the error of theline intensity as given by Dopita & Hua (1997).Because our observations are not absolutely flux calibrated,we first had to recalculate values of Dopita & Hua (1997) to thesame scale (H β = β in both our and Dopita & Hua (1997) measurements. Forthe 11 PNe in common with our observations and presented inFig. A.1, the error of the H β flux in Dopita & Hua (1997) variesbetween 1% and 2%.The dashed lines in Fig. A.1 represent the normalised errorlimits of Dopita & Hua (1997) measurements. Our results areshown with black-filled circles. The triangles in Fig. A.1 repre-sent line measurements from the Strasbourg-ESO catalogue ofAcker et al. (1992) and are shown for reference. The latter havebeen derived from the Catalogue’s spectroscopic survey and areof considerably lower sensitivity than our spectra.The panel A of Fig. A.1 presents the comparison of our mea-surement and that of Dopita & Hua (1997) of the [O III] λ ff erent in panel B that presents the com-parison of H α measurements. Although there is no systematicdeviation between our data and Dopita & Hua (1997), the scat-ter is larger than in the previous plot. It cannot be blamed on themeasurement of H β line, which is sometimes 10 times fainterthen the H α line, since it would then have comparable impactin the first panel. We checked that the internal errors of Dopitameasurements for H α / H β line ratio are largest for objects No. 1,6, and 9 (see Table A.1) and reach 4.0, 4.5, and 3.2%, respec-tively. It can be noted that our measurements actually fall withinthe normalised errors in these cases. One possibility is thereforethat the errors of Dopita & Hua (1997) are underestimated forother PNe. The discrepancy of H α / H β ratios between di ff erentauthors are not uncommon. In this case, we can see that they aremostly influenced by H α measurements itself.In panel C of Fig. A.1, we show a comparison for the close[N II] λ In practise, the errors in H β have in practise minor influence on ourfurther calculations since they cancel when ratios of lines are computed,except through the H α / H β ratio used to deredden the observations Table A.1.
List of PNe in common with Dopita & Hua (1997).
No. PN G name1 285.4 + + + + + + This di ff erence in observingtechnique will have smaller influence on ions of higher ionisa-tion potentials, like [O III], since they are naturally concentratedtoward the center of the nebula.In panel D of Fig. A.1, we compare the He I λ α and [N II] measurements beingunderestimated by these authors. However, some influence inwhich we frequently had to use short snapshot spectra to mea-sure such lines cannot be excluded.In panels E and F of Fig. A.1, we compare our results withDopita & Hua (1997) for the lines of another two ions. In thecase of [S II] doublet λ +
31, a similar picture to [N II] isseen strengthening our arguments presented above. For [Ar III] λ ff ects is noticeable in our data. It would systematicallyunderestimate measurements of red lines, like [Ar III] λ ff erent authors canbe a complex function of many factors (wavelength, blending,location of emission zone within the nebula, etc.), and the valuesdo not always converge with increasing line strength. This underestimation have, however, a minor e ff ect on our results,since N / O abundance ratio is derived by comparison to [O II] lines thatorigin from a similar region in the nebula.Article number, page 12 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Fig. A.1.
Comparison of our line intensities with measurements of Dopita & Hua (1997) for 11 PNe in common that are listed in Table A.1. Thedi ff erence for each PNe (identified on horizontal axis) between our measurement and of Dopita & Hua (1997) is marked with a black dot usinga normalised scale (vertical axis). The normalisation was done with the original errors from Dopita & Hua (1997). If the normalised absolutedi ff erence is less than 1 (dashed lines) our measurements agree within the uncertainty given by the latter authors. Open triangles present ananalogous comparison for data from Acker et al. (1992) compared to Dopita & Hua (1997) for the same PNe and are given for reference.Article number, page 13 of 35 ppendix B: Supplementary tables Article number, page 14 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.1.
Main nebular lines on the scale H β = PN G 268.4 + + β ) 1.82 1.41 0.87 0.843727 [O II] 12.1 : 32.52 :c 158.4 252.20 c 54.8 137.91 11.2 ; 18.37 ;c3869 [Ne III] 49.9 118.48 c 73.0 110.57 c 66.2 145.11 58.2 89.73 c4068 [S II] 6.5 : 12.96 :c 8.7 : 12.23 :c p p4102 H I 13.5 26.13 c 17.5 24.27 c 15.2 26.20 19.0 26.46 c4340 H I 28.6 47.17 c 36.9 48.24 c 35.0 47.26 37.3 47.90 c4363 [O III] 13.8 22.39 11.0 14.26 16.4 24.12 15.3 19.464471 He I 4.0 5.82 4.0 4.89 3.0 : 4.05 : 1.5 1.814686 He II 36.0 42.36 25.5 27.83 50.9 58.20 74.5 80.794711 [Ar IV] 3.9 3.04 5.2 ; 4.96 ; 4.8 4.80 9.7 10.144725 [Ne IV] 1.2 ; 1.36 ; 1.8 : 1.93 : 0.9 : 0.96 :4740 [Ar IV] 5.8 6.50 3.2 : 3.40 : 4.0 4.39 8.3 8.784861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 510.3 462.21 477.2 442.06 467.3 445.65 420.6 401.795007 [O III] 1644.5 1422.24 1462.0 1306.84 1442.4 1345.42 1279.4 1196.345200 [N I] 0.7 ; 0.51 ; 6.3 : 4.94 : 1.5 : 1.29 :5515 [Cl III] ? ? 2.4 ; 1.53 ; 1.4 ; 1.06 ; 1.1 : 0.84 :5537 [Cl III] 1.4 0.77 1.4 : 0.88 : 1.1 ; 0.82 ; 0.8 : 0.61 :5755 [N II] 9.5 4.25 13.0 6.98 1.6 : 1.09 :5876 He I 32.7 13.17 29.1 14.41 12.9 8.34 8.9 5.856300 [O I] 37.8 11.42 56.9 22.56 10.4 5.86 ? ?6312 [S III] 10.5 3.15 8.2 3.23 5.4 3.03 3.2 1.836548 [N II] 118.1 30.63 338.4 119.27 39.5 20.68 3.3 1.776563 H I 1092.2 280.79 808.4 283.00 535.8 279.40 524.9 280.146583 [N II] 352.4 89.51 1091.7 378.63 123.4 63.98 8.0 4.256678 He I 13.6 3.28 11.2 3.73 5.1 2.58 3.9 2.026716 [S II] 9.1 2.15 74.1 24.31 13.3 6.66 1.1 0.566730 [S II] 19.9 4.67 118.5 38.67 13.6 6.79 1.5 0.777006 [Ar V] 11.8 2.43 1.3 ; 0.38 ; 2.0 0.94 3.7 1.787136 [Ar III] 94.9 18.39 95.4 26.85 35.7 16.26 22.8 10.687325 [O II] 133.7 23.69 92.1 24.18 12.6 5.50 2.5 1.12 Article number, page 15 of 35 able B.1.
Continued.
PN G 283.8-04.2 285.4 + + β ) 0.44 1.72 0.47 0.133727 [O II] 157.5 261.58 c 26.1 71.42 c 36.63 48.17 14.80 : 18.37 :c3869 [Ne III] 97.9 151.98 c 31.8 76.76 c 51.12 64.97 56.85 69.40 c4068 [S II] 2.5 ; 5.06 ;c 1.11 ; 1.34 ;4102 H I 18.9 26.19 c 13.4 26.30 c 20.75 24.93 21.95 26.07 c4340 H I 38.0 47.24 c 29.0 48.26 42.18 48.45 40.64 47.09 c4363 [O III] 18.2 22.88 4.7 7.67 7.64 8.73 11.26 12.674471 He I 4.0 5.84 4.75 5.274686 He II 71.4 77.33 43.80 45.674711 [Ar IV] 7.1 : 7.60 : 1.0 : 0.35 : 1.25 0.49 2.37 ; 2.46 ;4725 [Ne IV]4740 [Ar IV] 10.9 ; 11.52 ; 0.94 ; 0.97 ; 3.08 ; 3.17 ;4861 H I 100.0 100.00 100.0 100.00 100.00 100.00 100.00 100.004959 [O III] 456.0 445.17 349.3 318.24 287.99 280.78 339.79 337.455007 [O III] 1362.1 1314.91 1082.5 944.27 862.42 830.94 1030.56 1020.175200 [N I] 4.2 : 3.89 : 1.3 : 0.97 : 0.67 : 0.62 :5515 [Cl III] 0.7 : 0.41 : 0.38 0.335537 [Cl III] 1.3 0.74 0.66 0.575755 [N II] 2.8 : 2.30 : 7.2 3.38 1.45 1.185876 He I 7.1 : 5.69 : 40.5 17.22 18.79 14.89 8.76 8.226300 [O I] 15.3 11.44 29.1 9.44 4.64 3.42 1.18 ; 1.09 ;6312 [S III] 3.6 : 2.69 : 6.7 2.16 1.67 1.23 1.22 ; 1.12 ;6548 [N II] 76.5 55.12 130.8 36.74 19.32 13.67 5.53 5.036563 H I 388.9 279.62 1023.4 285.09 401.24 283.37 310.11 282.066583 [N II] 235.3 168.69 418.9 115.38 55.71 39.22 14.44 13.126678 He I 3.7 ; 2.62 ; 17.1 4.49 5.40 3.75 3.89 3.526716 [S II] 21.2 14.94 10.4 2.68 1.14 0.79 2.03 : 1.84 :6730 [S II] 23.1 16.25 20.2 5.17 2.23 1.54 2.47 : 2.23 :7006 [Ar V] 2.0 ; 1.36 ; 1.1 ; 0.25 ;7136 [Ar III] 34.3 23.03 103.8 22.17 14.16 9.30 8.54 7.627325 [O II] 14.0 9.20 133.8 26.26 16.06 10.31 4.12 ; 3.65 ; Article number, page 16 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.1.
Continued.
PN G 291.4 + + + β ) 0.33 0.81 2.16 0.923727 [O II] 44.6 61.45 c 244.7 : 419.46 :c3869 [Ne III] 20.9 : 13.10 :c 85.2 114.90 c 77.1 ; 98.64 ;c 146.3 : 234.49 :c4068 [S II] 5.4 7.05 c4102 H I 31.0 : 26.36 :c 19.9 25.83 c4340 H I 44.4 47.46 c 37.2 47.28 35.8 ; 47.32 ;c 35.9 47.15 c4363 [O III] 10.6 ; 9.71 ; 5.2 6.55 28.2 ; 37.08 ; 26.8 : 34.84 :4471 He I 4.7 5.624686 He II 107.9 104.86 18.9 20.43 49.9 : 55.15 : 76.7 83.784711 [Ar IV] 20.0 : 19.52 : 3.6 3.22 15.2 : 16.40 :4725 [Ne IV]4740 [Ar IV] 17.8 ; 17.46 ; 3.9 4.12 13.9 : 14.79 :4861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 120.4 118.30 407.3 389.82 509.9 453.53 356.9 339.545007 [O III] 358.6 349.44 1242.6 1165.17 1605.8 1352.23 1100.3 1022.695200 [N I] 2.0 1.74 39.5 33.725515 [Cl III] 6.5 : 5.86 : 1.0 0.775537 [Cl III] 1.6 1.235755 [N II] 5.4 3.78 12.7 ; 4.90 ; 40.9 27.275876 He I 25.1 16.78 35.2 12.00 38.6 : 24.42 :6300 [O I] 14.5 8.53 34.2 8.29 83.3 45.586312 [S III] 6.0 3.52 17.4 4.18 16.8 : 9.16 :6548 [N II] 133.8 73.57 128.0 25.91 948.5 480.596563 H I 351.7 276.09 524.7 287.41 1389.6 278.37 544.0 274.436583 [N II] 420.0 228.83 391.5 77.31 3024.5 1516.506678 He I 8.6 4.58 12.5 2.32 p p6716 [S II] 21.4 11.29 8.4 : 1.52 : 209.4 101.276730 [S II] 36.6 19.26 23.1 4.15 180.8 87.127006 [Ar V] 9.1 ; 6.87 ; 36.3 5.587136 [Ar III] p p 64.2 31.03 153.2 21.97 102.8 44.987325 [O II] 20.3 9.43 174.9 18.54 55.5 : 23.21 : Article number, page 17 of 35 able B.1.
Continued.
PN G 294.6 + β ) 0.27 0.33 0.33 1.43727 [O II] 58.7 : 61.84 :c 126.7 153.71 c 26.7 38.90 c 20.8 58.69 c3869 [Ne III] 100.7 106.75 c 2.8 3.32 c 61.7 85.03 c 56.4 139.07 c4068 [S II] 2.1 : 2.24 :c 3.0 : 3.43 :c 2.5 : 3.18 :c 3.0 6.10 c4102 H I 24.4 26.09 c 22.9 26.07 c 20.8 26.10 c 13.2 26.01 c4340 H I 43.0 46.65 c 42.6 46.98 41.1 47.14 c 29.0 47.01 c4363 [O III] 19.4 20.98 1.1 : 1.21 : 9.8 11.49 9.8 15.924471 He I 3.2 3.40 3.7 3.98 4.4 4.98 3.4 4.964686 He II 47.1 48.36 0.3 : 0.31 : 21.0 24.784711 [Ar IV] 7.9 : 7.56 : 0.6 1.1 : 0.36 : 4.7 4.714725 [Ne IV] 1.8 ; 1.84 ; 1.7 ; 1.94 ;4740 [Ar IV] 8.5 : 8.66 : 1.1 : 1.14 : 8.1 : 9.09 :4861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 537.1 529.16 48.6 47.74 279.9 274.99 553.7 513.235007 [O III] 1613.1 1578.26 150.0 146.12 848.0 826.27 1723.9 1542.265200 [N I] 1.0 0.95 0.6 0.57 0.7 0.66 1.1 0.865515 [Cl III] 0.6 0.55 0.2 ; 0.18 ; 0.4 0.36 0.9 0.585537 [Cl III] 0.9 0.82 0.3 0.27 0.5 0.45 1.4 0.885755 [N II] 2.0 1.77 4.0 3.46 2.4 2.08 5.7 3.085876 He I 11.8 10.29 13.7 11.62 18.9 16.06 30.8 15.346300 [O I] 6.5 5.43 4.1 3.30 4.0 3.23 17.2 6.876312 [S III] 3.3 2.75 1.1 0.88 2.5 2.02 8.7 3.456548 [N II] 32.2 26.28 68.5 53.68 25.7 20.19 107.7 38.266563 H I 345.5 281.66 364.5 285.18 358.7 281.35 803.2 283.456583 [N II] 101.2 82.35 212.6 165.98 62.9 49.23 321.7 112.486678 He I 4.0 3.23 3.8 2.94 4.9 3.80 11.7 3.936716 [S II] 3.5 2.82 2.1 1.62 1.9 1.47 14.0 4.636730 [S II] 6.3 5.07 4.5 3.46 3.5 2.70 26.2 8.627006 [Ar V] 2.9 2.29 0.3 0.23 2.9 0.867136 [Ar III] 25.3 19.77 9.1 6.77 14.3 10.66 93.1 26.467325 [O II] 11.3 8.71 42.1 30.80 16.0 11.74 45.4 12.04 Article number, page 18 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.1.
Continued.
PN G 297.4 + + + + β ) 0.89 0.13 0.92 2.423727 [O II] 138.9 234.70 c 170.7 221.26 c 293.7 457.07 c 29.2 : 56.49 :c3869 [Ne III] 75.1 94.48 c 55.5 81.64 c4068 [S II]4102 H I 17.1 : 24.30 :c 21.7 25.97 c 19.3 25.86 c 12.5 25.65 c4340 H I 37.8 49.29 41.2 46.96 c 37.5 46.82 c 23.3 47.74 c4363 [O III] 7.5 : 8.48 :4471 He I 3.4 : 4.14 : 4.4 ; 4.85 ; 5.2 8.874686 He II 14.5 15.15 17.4 18.724711 [Ar IV]4725 [Ne IV]4740 [Ar IV]4861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 12.9 12.29 314.4 312.23 259.4 246.79 26.2 22.985007 [O III] 35.0 32.59 944.5 934.96 797.3 741.09 82.3 67.895200 [N I] 15.6 13.325515 [Cl III]5537 [Cl III] 1.6 ; 1.53 ;5755 [N II] 2.2 ; 1.48 ; 3.0 : 2.84 : 6.8 : 4.54 : 8.7 3.005876 He I 11.6 7.43 14.2 : 13.33 : 23.7 15.00 48.4 14.506300 [O I] 2.3 ; 1.28 ; 5.6 ; 5.15 ; 83.4 45.65 9.7 : 1.98 :6312 [S III] 4.8 ; 2.62 ; 6.5 : 1.32 :6548 [N II] 105.7 54.54 50.3 45.77 210.5 106.70 609.8 101.926563 H I 568.2 291.93 312.5 284.20 567.9 286.59 1763.7 291.406583 [N II] 346.5 176.97 152.1 138.21 660.4 331.25 1941.6 315.706678 He I 5.7 2.84 4.8 : 4.35 : 9.2 4.50 29.9 4.546716 [S II] 8.1 3.99 25.6 23.15 117.4 56.80 34.3 5.076730 [S II] 14.8 7.27 20.0 18.07 96.3 46.42 66.5 9.747006 [Ar V]7136 [Ar III] 11.7 5.23 18.3 16.32 40.1 17.55 114.8 13.047325 [O II] 25.8 11.04 7.6 ; 6.73 ; 37.5 15.69 81.7 8.24 Article number, page 19 of 35 able B.1.
Continued.
PN G 300.4-00.9 300.5-01.1 300.7-02.0 300.8-03.4name He 2- 84 He 2- 85 He 2- 86 ESO 095-1C(H β ) 1.27 1.76 2.00 0.673727 [O II] 91.8 161.37 c 18.5 : 49.45 :c 7.8 37.40 c 134.1 : 161.27 :c3869 [Ne III] 76.2 125.10 c 46.4 108.72 c 21.7 83.58 c 91.2 : 107.46 :c4068 [S II] 1.6 : 4.48 :c4102 H I 16.8 24.61 c 13.8 26.02 c 9.7 25.73 c4340 H I 35.6 47.95 c 29.7 47.03 c 24.9 46.64 c 42.3 47.13 c4363 [O III] 8.4 11.19 9.3 14.81 1.7 : 3.42 : 18.8 ; 20.88 ;4471 He I 5.1 : 6.37 : 2.2 : 3.15 : 4.3 7.414686 He II 25.9 28.52 40.2 47.00 ? ?4711 [Ar IV] 6.5 : 6.29 : 9.6 10.56 1.2 : 0.54 :4725 [Ne IV]4740 [Ar IV] 5.3 : 5.67 : 8.2 9.15 1.5 : 1.77 :4861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 402.0 375.18 505.5 459.55 311.3 279.26 533.6 514.645007 [O III] 1241.5 1121.92 1570.6 1365.70 989.1 843.42 1622.4 1538.565200 [N I] 16.8 13.49 1.0 0.715515 [Cl III] 1.5 ; 0.86 ; 0.9 0.485537 [Cl III] 1.9 : 1.07 : 1.7 0.885755 [N II] 19.8 11.30 3.4 1.57 7.1 2.945876 He I 31.3 16.60 27.1 11.29 55.5 20.466300 [O I] 54.7 23.73 15.7 4.96 13.6 3.66 15.1 9.756312 [S III] 13.7 5.91 9.6 3.01 9.4 2.51 14.5 9.346548 [N II] 439.6 171.48 86.9 23.70 175.5 39.91 40.0 24.436563 H I 731.4 283.57 1046.7 283.06 1285.7 289.60 462.3 281.416583 [N II] 1395.2 536.40 266.4 71.21 538.4 119.68 131.2 79.516678 He I 14.1 5.23 12.2 3.10 25.4 5.336716 [S II] 128.0 46.81 22.0 5.49 11.6 2.38 31.2 18.426730 [S II] 149.0 54.21 36.9 9.14 24.2 4.93 29.5 17.377006 [Ar V] 5.7 : 1.89 : 10.4 2.277136 [Ar III] 100.5 32.00 107.5 22.15 203.8 33.67 52.8 28.997325 [O II] 48.9 14.62 32.3 6.10 55.5 8.31 Article number, page 20 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.1.
Continued.
PN G 302.2 + + + + β ) 1.22 1.23 0.96 0.493727 [O II] 12.8 25.07 c3869 [Ne III] 76.0 ; 10.89 ;c 2.5 4.44 c 20.5 35.26 c 55.9 82.56 c4068 [S II] 1.4 2.16 c4102 H I 17.6 26.57 c 17.6 26.33 c 19.6 26.35 c4340 H I 63.5 ; 46.92 ;c 36.1 47.72 c 35.8 47.63 38.4 47.46 c4363 [O III] 5.3 7.19 8.6 11.32 15.1 18.614471 He I 5.0 6.33 4.6 5.694686 He II 87.8 82.61 101.6 111.45 102.5 110.154711 [Ar IV] 0.8 14.0 14.22 14.1 15.004725 [Ne IV] 2.5 2.694740 [Ar IV] 10.4 11.10 11.4 11.994861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 354.2 331.59 52.2 48.82 154.5 146.64 231.4 225.395007 [O III] 1070.6 971.85 162.6 147.40 475.9 440.80 702.9 676.265200 [N I] 3.9 3.155515 [Cl III] 0.4 : 0.27 :5537 [Cl III] 0.6 0.40 0.7 ; 0.51 ;5755 [N II] 11.4 6.625876 He I 25.2 13.63 1.4 ; 0.87 ;6300 [O I] 1.8 0.806312 [S III] 10.4 4.61 3.5 : 1.85 : 3.4 : 2.47 :6548 [N II] 38.7 15.556563 H I 704.5 284.90 680.8 271.90 566.5 276.66 396.4 276.176583 [N II] 49.0 19.66 96.9 38.39 3.5 1.706678 He I 8.7 3.33 2.8 1.326716 [S II] 0.6 0.23 1.0 ; 0.47 ;6730 [S II] 1.3 0.49 0.7 ; 0.33 ;7006 [Ar V] 13.4 5.82 5.1 : 3.35 :7136 [Ar III] 49.2 16.48 40.7 13.43 13.3 5.60 12.6 8.147325 [O II] 84.8 26.34 Article number, page 21 of 35 able B.1.
Continued.
PN G 309.0 + + β ) 1.78 1.27 3.25 1.053727 [O II] 17.0 : 73.21 :c 91.04 : 122.57 :c 233.9 433.55 c3869 [Ne III] 20.3 : 71.46 :c 78.21 : 102.73 :c 68.1 : 116.88 :c4068 [S II] 2.2 ; 5.77 ;c4102 H I 10.3 25.71 c 19.1 : 28.88 :c4340 H I 25.8 46.60 c 38.68 47.03 c 38.4 52.474363 [O III] 1.6 3.08 13.11 ; 15.85 ; 7.2 ; 9.72 ;4471 He I 3.7 6.164686 He II 14.91 15.91 70.7 : 96.61 : 4.5 ; 4.98 ;4711 [Ar IV] 2.0 ; 1.72 ;4725 [Ne IV]4740 [Ar IV]4861 H I 100.0 100.00 100.00 100.00 100.0 : 100.00 : 100.0 100.004959 [O III] 307.1 278.78 543.11 507.01 534.6 448.22 282.9 267.205007 [O III] 972.0 843.37 1648.96 1490.70 1728.9 1335.03 872.2 802.135200 [N I] 1.1 ; 0.81 ; 5.0 ; 4.17 ;5515 [Cl III] 0.9 : 0.51 :5537 [Cl III] 2.0 : 1.11 :5755 [N II] 4.5 2.05 13.49 : 7.71 : 6.7 : 4.21 :5876 He I 47.8 19.65 31.42 16.70 47.9 : 9.49 : 27.1 16.046300 [O I] 17.2 5.34 54.53 23.74 27.6 ; 3.28 ; 55.3 27.736312 [S III] 7.6 2.34 4.72 ; 2.04 ; 76.3 ; 8.93 ; 18.2 9.086548 [N II] 292.55 114.52 184.1 16.65 193.9 89.026563 H I 1095.0 290.19 727.74 283.16 3217.8 286.55 617.8 282.216583 [N II] 273.0 71.50 908.68 350.61 524.0 45.67 600.5 272.416678 He I 20.4 5.08 10.28 3.83 37.4 ; 2.97 ; 9.8 : 4.31 :6716 [S II] 8.5 2.08 24.43 8.97 68.2 5.23 65.7 28.596730 [S II] 17.2 4.17 34.81 12.71 79.9 6.05 59.9 25.967006 [Ar V] 79.3 : 4.75 :7136 [Ar III] 110.7 22.26 86.42 27.63 419.3 22.58 39.0 15.147325 [O II] 93.5 17.22 65.09 19.55 111.1 : 4.19 : 29.1 10.72 Article number, page 22 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.1.
Continued.
PN G 311.4 + + β ) 1.03 1.31 4.69 0.093727 [O II] 6.6 11.20 c 50.7 132.37 c 75.5 93.26 c3869 [Ne III] 50.9 81.58 c4068 [S II] 2.3 ; 3.40 ;c 4.5 5.17 c4102 H I 17.8 25.94 c 14.1 25.51 c 23.2 26.45 c4340 H I 34.4 46.74 31.1 45.84 43.9 47.57 c4363 [O III] 6.2 8.33 0.3 : 0.33 :4471 He I 3.9 4.90 5.4 7.21 1.6 1.724686 He II 37.1 40.97 2.0 : 2.27 : 0.3 0.314711 [Ar IV] 4.5 4.33 0.34725 [Ne IV]4740 [Ar IV] 4.6 4.934861 H I 100.0 100.00 100.0 100.00 100.0 ; 100.00 ; 100.0 100.004959 [O III] 354.3 334.98 21.2 19.75 1381.2 1070.59 3.1 3.085007 [O III] 1086.8 1000.98 66.7 60.11 4431.6 3049.74 9.5 9.435200 [N I] 0.6 0.595515 [Cl III] 0.9 : 0.65 : 0.1 : 0.10 :5537 [Cl III] 0.5 : 0.36 : 0.2 : 0.19 :5755 [N II] 2.1 : 1.18 : 101.1 ; 12.75 ; 3.0 2.885876 He I 22.3 13.32 39.4 20.54 325.8 31.38 5.7 5.446300 [O I] 342.5 15.73 2.4 2.266312 [S III] 2.3 1.16 1.5 : 0.63 : 122.4 : 5.51 : 0.8 0.756548 [N II] 3.4 1.58 182.5 69.38 1696.0 52.59 89.2 83.266563 H I 614.8 284.81 780.1 294.71 8893.1 269.62 294.0 274.306583 [N II] 8.7 4.00 577.4 216.25 5559.3 163.39 275.7 257.076678 He I 8.4 3.75 15.6 5.63 185.3 : 4.77 : 1.6 1.496716 [S II] 1.5 0.66 7.5 2.67 199.1 : 4.86 :6730 [S II] 1.9 0.84 12.6 4.46 253.4 : 6.08 :7006 [Ar V] 0.2 0.187136 [Ar III] 26.4 10.42 45.7 14.10 1512.9 22.17 3.5 3.227325 [O II] 6.8 2.55 9.6 2.78 1837.4 17.58 10.5 9.61 Article number, page 23 of 35 able B.1.
Continued.
PN G 315.4 + + + β ) 0.89 0.40 0.51 1.083727 [O II] 269.5 529.16 c 82.7 151.31 c 162.8 306.97 c3869 [Ne III] 71.2 128.02 c 284.3 ; 349.68 ; 3.0 : 5.04 :c 52.1 90.77 c4068 [S II] p p 0.5 ; 0.74 ;c4102 H I 16.7 25.95 c 17.8 25.91 c 17.1 : 26.15 :c4340 H I 34.3 46.93 c 37.1 46.88 c 33.0 45.484363 [O III] 6.6 9.04 1.0 ; 1.30 ;4471 He I 5.0 : 6.38 : 5.1 : 6.27 :4686 He II 13.1 14.58 104.8 108.94 3.4 3.73 17.5 19.424711 [Ar IV] 0.8 ; 0.15 ; 0.7 0.064725 [Ne IV]4740 [Ar IV]4861 H I 100.0 100.00 100.0 ; 100.00 ; 100.0 100.00 100.0 100.004959 [O III] 382.6 364.64 405.8 397.02 60.6 58.95 215.6 203.315007 [O III] 1166.8 1087.32 1256.3 1216.63 184.1 176.81 650.6 596.945200 [N I] 6.2 5.32 p p5515 [Cl III] p p 0.5 : 0.43 :5537 [Cl III] p p 0.4 : 0.34 :5755 [N II] 7.4 5.01 0.7 0.56 10.1 6.275876 He I 25.1 16.14 21.6 16.77 29.2 17.036300 [O I] 64.6 36.11 10.4 : 5.12 :6312 [S III] 1.9 : 1.06 : 1.1 0.79 p p6548 [N II] 176.3 91.51 32.0 21.98 301.1 135.296563 H I 551.0 284.80 388.4 287.68 416.8 285.61 639.4 285.816583 [N II] 548.4 281.80 97.6 : 72.10 : 102.1 69.73 940.9 417.576678 He I 8.4 4.21 7.2 4.85 11.9 5.126716 [S II] 37.1 18.41 28.5 : 20.72 : 3.0 2.01 128.3 54.576730 [S II] 39.2 19.38 15.5 : 11.25 : 3.6 2.41 107.0 45.327006 [Ar V]7136 [Ar III] 37.5 16.90 54.4 : 37.85 : 24.3 15.39 63.4 23.977325 [O II] 41.9 18.07 4.5 2.78 28.1 10.07 Article number, page 24 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.1.
Continued.
PN G 319.2 + + + + β ) 1.19 2.70 2.21 1.213727 [O II] 51.1 121.86 c 7.5 32.60 c 16.5 67.93 c 123.9 252.223869 [Ne III] 78.4 165.14 c 14.7 52.57 c 8.4 29.01 c 41.8 ; 77.88 ;4068 [S II] 4.3 : 7.58 :c 2.2 ; 5.98 ;c4102 H I 15.3 26.19 c 9.9 25.66 c 13.3 ; 21.41 ;4340 H I 33.5 47.70 23.2 46.54 c 22.9 46.68 c 35.1 50.294363 [O III] 21.4 30.06 1.1 ; 2.22 ; 1.3 ; 2.58 ; p p4471 He I 3.8 4.94 4.2 7.22 3.3 5.614686 He II 41.2 46.20 1.9 ; 2.40 ; 17.1 19.214711 [Ar IV] 7.2 7.18 p p 1.1 ; 0.53 ;4725 [Ne IV] 1.9 2.084740 [Ar IV] 4.6 4.98 p p 1.0 ; 1.18 ;4861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 598.7 561.24 282.8 244.25 208.5 184.92 260.1 243.555007 [O III] 1852.0 1684.52 894.9 721.78 666.1 558.55 800.2 726.615200 [N I] 3.4 2.77 1.4 ; 0.88 ; 7.5 6.095515 [Cl III] 1.5 1.03 1.2 0.51 1.3 0.645537 [Cl III] 1.7 1.15 2.8 1.15 1.0 0.485755 [N II] 12.6 7.45 11.0 3.36 5.7 2.15 9.1 5.335876 He I 26.8 14.80 85.7 22.30 51.4 17.06 32.4 17.716300 [O I] 21.2 9.70 27.8 4.72 15.2 3.56 42.7 19.286312 [S III] 11.3 5.15 12.6 2.12 6.4 1.48 4.5 ; 2.02 ;6548 [N II] 229.8 95.22 365.9 49.60 123.8 24.09 321.3 131.066563 H I 678.3 279.47 2175.9 291.19 1500.5 288.91 707.8 287.066583 [N II] 727.0 297.18 1134.4 149.12 384.4 72.94 1016.5 408.966678 He I 10.1 3.99 43.9 5.34 23.6 4.20 14.5 5.646716 [S II] 33.1 12.91 30.7 3.63 5.8 1.01 109.5 42.006730 [S II] 48.4 18.79 61.6 7.20 12.5 2.16 100.2 38.257006 [Ar V] 5.8 2.07 1.1 ? 0.16 ?7136 [Ar III] 71.6 24.53 332.4 29.28 120.9 16.53 75.6 25.417325 [O II] 52.1 16.84 108.8 8.39 187.7 23.01 27.5 ; 8.71 ; Article number, page 25 of 35 able B.1.
Continued.
PN G 322.5-05.2 323.9 + + β ) 0.25 1.62 1.71 3.593727 [O II] 7.7 9.17 c 19.1 57.86 c 17.4 : 67.97 :c3869 [Ne III] 54.5 63.74 c 3.7 9.62 c 23.8 : 150.36 :4068 [S II] 1.9 2.16 c4102 H I 23.1 26.20 c 12.7 25.61 c 11.1 25.37 c 5.1 ; 20.91 ;4340 H I 42.7 47.27 c 29.2 47.26 c 27.5 45.61 18.2 52.814363 [O III] 15.8 17.28 2.9 ; 8.08 ;4471 He I 0.8 : 0.86 : 5.7 8.16 1.0 ; 1.46 ; p p4686 He II 101.2 104.344711 [Ar IV] 15.7 15.99 0.4 ; p p4725 [Ne IV] 3.7 : 3.79 :4740 [Ar IV] 13.5 13.79 p p4861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 319.0 314.65 66.1 60.53 467.9 385.085007 [O III] 965.3 946.07 209.0 183.67 3.3 ; 2.88 ; 1574.8 1183.335200 [N I] 1.2 0.91 1.5 ; 1.12 ;5515 [Cl III] 0.6 : 0.55 : 0.8 0.48 p p5537 [Cl III] 0.6 : 0.55 : 1.0 0.59 3.9 : 1.20 :5755 [N II] 0.2 ; 0.18 ; 3.4 1.66 1.9 : 0.90 : 22.2 4.565876 He I 3.1 2.73 52.8 23.52 9.8 4.19 124.8 20.856300 [O I] 3.3 : 1.14 : 4.2 1.37 70.5 6.686312 [S III] 2.5 2.12 2.3 : 0.79 : 0.9 : 0.29 : 27.1 2.536548 [N II] 1.7 1.41 251.6 75.73 277.1 78.47 573.8 40.286563 H I 337.1 279.26 979.1 292.42 1061.5 298.14 4148.7 286.276583 [N II] 3.9 3.23 774.3 228.79 860.4 238.95 1823.7 122.896678 He I 2.1 : 1.72 : 21.1 5.95 4.6 1.22 77.8 4.736716 [S II] 0.8 0.66 19.5 5.41 36.6 9.50 53.8 3.156730 [S II] 0.8 0.65 31.2 8.59 68.0 17.54 109.4 6.317006 [Ar V] 4.3 3.457136 [Ar III] 15.5 12.35 50.6 11.75 7.9 1.70 641.2 25.387325 [O II] 1.1 0.87 10.0 2.14 7.5 : 1.49 : 354.0 9.65 Article number, page 26 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.1.
Continued.
PN G 327.1-01.8 327.8-01.6 330.9 + + β ) 1.94 0.74 1.15 0.953727 [O II] 44.5 : 138.94 :c 97.4 150.06 c3869 [Ne III] 104.9 153.14 c p p 34.0 96.11 c4068 [S II] 3.8 : 5.14 :c4102 H I 14.5 ; 31.09 ;c 19.9 26.58 c 12.8 26.10 c4340 H I 29.2 : 51.94 : 38.3 47.66 c p p 33.4 47.13 c4363 [O III] 20.2 24.93 p p 6.6 10.954471 He I 2.5 : 2.94 : 3.8 5.664686 He II 80.8 86.734711 [Ar IV] 8.9 9.07 1.6 ; 0.11 ;4725 [Ne IV]4740 [Ar IV] 7.6 7.99 2.8 ; 3.18 ;4861 H I 100.0 100.00 100.0 100.00 100.0 100.00 100.0 100.004959 [O III] 17.1 15.39 637.6 612.61 468.3 439.94 293.6 278.875007 [O III] 56.7 48.58 1937.3 1826.93 1350.2 1231.95 878.4 814.495200 [N I] 1.6 ; 1.41 ;5515 [Cl III] 2.6 2.065537 [Cl III] 2.1 1.655755 [N II] 8.9 : 3.78 : 4.4 3.185876 He I 9.7 6.72 33.1 : 18.65 : 23.3 14.526300 [O I] 10.1 2.83 7.4 4.56 0.9 : 0.48 :6312 [S III] 4.4 ; 1.22 ; 12.1 7.44 1.8 0.966548 [N II] 420.6 100.03 97.6 56.586563 H I 1233.8 290.72 487.1 281.38 662.5 281.07 570.7 281.526583 [N II] 1316.6 306.27 300.4 172.69 24.2 : 10.19 : 5.2 2.556678 He I 16.2 3.57 4.3 2.42 8.3 3.966716 [S II] 23.0 4.96 40.3 22.506730 [S II] 48.3 10.33 43.3 24.117006 [Ar V] 2.9 1.537136 [Ar III] 59.4 10.36 69.2 35.66 17.4 6.18 16.1 6.867325 [O II] 62.4 9.89 12.5 6.21 2.8 : 0.94 : Article number, page 27 of 35 able B.1.
Continued.
PN G 338.1-08.3name NGC 6326C(H β ) 0.113727 [O II] 40.5 43.243869 [Ne III] 102.2 108.234068 [S II] 2.1 2.204102 H I 25.2 26.334340 H I 45.0 46.524363 [O III] 13.7 14.144471 He I 3.4 3.484686 He II 51.4 51.954711 [Ar IV] 6.6 6.234725 [Ne IV] 0.7 ; 0.71 ;4740 [Ar IV] 5.2 : 5.24 :4861 H I 100.0 100.004959 [O III] 446.3 443.605007 [O III] 1342.5 1330.615200 [N I] 0.4 : 0.39 :5515 [Cl III] 0.7 0.685537 [Cl III] 0.6 0.585755 [N II] 0.5 0.485876 He I 10.4 9.846300 [O I] 2.5 2.326312 [S III] 2.4 2.236548 [N II] 10.0 9.216563 H I 307.7 283.146583 [N II] 29.8 27.406678 He I 3.5 3.216716 [S II] 5.1 4.676730 [S II] 5.9 5.407006 [Ar V] 1.0 0.917136 [Ar III] 14.1 12.757325 [O II] 3.4 3.06 Article number, page 28 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.2.
New, reobserved, and mis-classified PNe with emission-linecentral stars. Column 3 gives the width of C IV λ name FWHM classificationt.w. WG new WELs:PB 5 WEL -My 60 WEL? -He 2-115 WEL - new [WR]:He 2- 67 43Å [WC 4] -He 2-117 25Å [WC 5-6] -He 2-125 VL - reobserved :Pe 1- 1 45Å [WC 5] [WO 4]He 2- 63 undetect.
WELHe 2- 86 22Å [WC 5-6] [WC 4]He 2-107 VL [WC10-11]He 2-131 VL WELHe 2-108 VL WELHe 2-123 WEL WEL? misclassified / mimics :NGC 6326 WEL?NGC 5979 not stellar WELNGC 3918 not stellar - Article number, page 29 of 35 able B.3.
Plasma parameters and abundances. The first row for each PN gives parameters computed from the nominal values of the observationaldata. The second and third row give the upper and lower limits, respectively, of these parameters. Column (1) gives the PN G number; Column(2) usual name; Column (3) electron density deduced from [S ii ] λ / iii ] λ / ii ] λ / T e (N ii ) is in parenthesis if T e (O iii ) was chosen for all ions. Columns (6) to (12) give the He / H,N / H, O / H, Ne / H, S / H, Ar / H, and Cl / H ratios, respectively.
PN G Main Name n e (S ii ) T e (O iii ) T e (N ii ) He / H N / H O / H Ne / H S / H Ar / H Cl / H268.4 + +
04 (14413) 13362 1.13E-01 1.34E-04 3.06E-04 6.48E-05 4.39E-06 1.77E-06 4.80E-074.43E +
04 (16435) 13737 1.20E-01 1.80E-04 3.76E-04 7.84E-05 5.79E-06 2.03E-06 6.47E-071.12E +
04 ( 8523) 12629 1.08E-01 1.19E-04 2.76E-04 5.67E-05 3.91E-06 1.64E-06 3.62E-07269.7-03.6 PB 3 2.50E +
03 10829 11849 1.23E-01 2.21E-04 4.38E-04 1.02E-04 6.39E-06 2.51E-06 3.57E-073.08E +
03 11190 12267 1.28E-01 2.52E-04 4.88E-04 1.19E-04 7.23E-06 2.77E-06 4.70E-072.11E +
03 10446 11541 1.16E-01 1.89E-04 3.92E-04 9.02E-05 5.57E-06 2.24E-06 2.60E-07279.6-03.1 He 2- 36 5.50E +
02 10793 14481 1.13E-01 6.38E-05 2.89E-04 7.77E-05 2.87E-06 1.25E-06 5.81E-076.42E +
02 12013 14743 1.18E-01 9.13E-05 3.59E-04 9.24E-05 3.74E-06 1.44E-06 9.59E-074.33E +
02 9822 13657 1.08E-01 5.31E-05 2.66E-04 6.56E-05 2.57E-06 1.17E-06 3.63E-07283.8 + +
03 13868 1.10E-01 5.11E-05 3.15E-04 6.02E-05 4.33E-06 1.68E-06 8.33E-062.45E +
03 14412 1.16E-01 6.40E-05 3.80E-04 6.92E-05 5.10E-06 1.86E-06 1.04E-051.05E +
03 13324 1.03E-01 4.17E-05 2.62E-04 5.24E-05 3.66E-06 1.48E-06 6.34E-06283.8-04.2 He 2-39 7.04E +
02 9821 14289 1.09E-01 1.25E-04 4.77E-04 1.38E-04 2.85E-06 2.40E-067.99E +
02 10751 14589 1.18E-01 1.53E-04 6.61E-04 2.01E-04 3.51E-06 3.12E-065.53E +
02 8774 13546 9.90E-02 1.09E-04 4.19E-04 1.19E-04 2.42E-06 1.85E-06285.4 + +
03 12859 10662 1.15E-01 1.13E-04 3.15E-04 7.50E-05 5.44E-06 2.60E-06 1.30E-068.96E +
03 13611 10927 1.23E-01 1.44E-04 3.64E-04 8.28E-05 6.63E-06 2.99E-06 1.82E-064.56E +
03 12264 10301 1.08E-01 1.04E-04 2.81E-04 6.65E-05 4.87E-06 2.38E-06 9.03E-07286.0-06.5 He 2- 41 6.74E +
03 12917 11626 9.68E-02 4.53E-05 2.09E-04 4.53E-05 2.24E-06 9.05E-07 1.02E-061.30E +
04 13591 11976 1.02E-01 5.12E-05 2.48E-04 5.37E-05 2.55E-06 1.03E-06 1.21E-063.76E +
03 10618 11199 9.09E-02 3.73E-05 1.79E-04 4.15E-05 1.88E-06 8.02E-07 7.64E-07289.8 + +
02 12459 9.87E-02 5.30E-05 2.66E-04 4.85E-05 2.61E-06 9.40E-071.93E +
03 12885 1.03E-01 7.64E-05 3.11E-04 5.75E-05 3.62E-06 1.10E-064.38E +
02 12078 9.16E-02 3.46E-05 2.31E-04 4.67E-05 1.70E-06 6.73E-07291.4 + + +
03 10228 9552 1.34E-01 4.86E-04 5.94E-04 1.85E-04 1.67E-05 4.71E-06 2.16E-063.80E +
03 10637 9774 1.41E-01 5.60E-04 6.95E-04 2.26E-04 1.98E-05 5.23E-06 2.77E-062.50E +
03 9825 9258 1.27E-01 3.90E-04 5.27E-04 1.76E-04 1.41E-05 4.25E-06 1.65E-06293.1-00.0 BMPJ1128-61 1.00E +
05 9416 15416 1.10E-01 1.15E-04 3.33E-04 5.25E-05 4.75E-06 1.26E-061.00E +
05 12660 21593 1.28E-01 2.68E-04 8.59E-04 1.58E-04 1.06E-05 2.27E-062.03E +
04 7917 10081 9.74E-02 6.97E-05 1.49E-04 2.06E-06 7.29E-07293.6 + +
02 11118 20203 2.71E-01 2.59E-04 1.78E-04 9.05E-05 4.32E-06 1.85E-063.64E +
02 11571 24121 3.14E-01 2.99E-04 2.24E-04 1.37E-04 5.02E-06 2.16E-061.72E +
02 10777 18398 2.32E-01 1.99E-04 1.45E-04 6.28E-05 3.14E-06 1.35E-06294.6 + +
03 11286 12728 1.08E-01 1.64E-04 4.04E-04 7.24E-05 4.55E-06 2.48E-06 9.27E-076.07E +
03 11744 13093 1.13E-01 1.95E-04 4.55E-04 8.59E-05 5.22E-06 2.97E-06 1.18E-063.52E +
03 10861 12253 1.02E-01 1.33E-04 3.61E-04 6.60E-05 3.83E-06 2.15E-06 7.16E-07294.9-04.3 He 2- 68 1.49E +
04 9666 10614 7.57E-02 4.57E-05 2.27E-04 1.49E-05 1.94E-06 8.00E-07 1.31E-076.42E +
04 10402 11330 8.06E-02 7.18E-05 6.44E-04 4.49E-05 3.72E-06 1.02E-06 2.25E-078.86E +
03 8135 9485 7.01E-02 3.79E-05 1.68E-04 1.09E-05 1.56E-06 6.75E-07 8.94E-08
Article number, page 30 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.3.
Continued.
PN G Main Name n e (S ii ) T e (O iii ) T e (N ii ) He / H N / H O / H Ne / H S / H Ar / H Cl / H295.3-09.3 He 2- 62 4.93E +
03 16469 12945 1.03E-01 7.38E-05 1.41E-04 3.81E-05 3.18E-06 8.37E-07 1.00E-066.64E +
03 17364 13389 1.11E-01 8.62E-05 1.64E-04 4.39E-05 3.75E-06 9.30E-07 1.30E-063.85E +
03 15468 12481 9.64E-02 5.64E-05 1.22E-04 3.35E-05 2.57E-06 7.42E-07 6.44E-07296.3-03.0 He 2- 73 5.05E +
03 12601 11580 1.22E-01 2.56E-04 4.15E-04 1.04E-04 8.50E-06 3.42E-06 1.40E-067.13E +
03 13090 11942 1.28E-01 3.09E-04 4.74E-04 1.17E-04 9.78E-06 3.85E-06 1.50E-064.00E +
03 11929 11241 1.16E-01 2.12E-04 3.59E-04 9.25E-05 7.16E-06 3.04E-06 1.30E-06297.4 + +
03 7847 5.13E-02 7.43E-05 4.75E-04 5.63E-06 1.34E-065.17E +
03 9025 5.44E-02 1.14E-04 1.23E-03 8.98E-06 2.05E-062.89E +
03 6680 4.78E-02 5.39E-05 2.68E-04 4.26E-06 1.00E-06299.0 + +
02 11854 11144 1.15E-01 1.18E-04 3.07E-04 8.77E-05 7.15E-06 1.74E-06 1.76E-061.82E +
02 13232 11899 1.33E-01 1.67E-04 4.10E-04 1.23E-04 8.93E-06 2.15E-06 3.17E-066.35E +
01 10822 10167 8.58E-02 8.21E-05 2.48E-04 7.03E-05 5.92E-06 1.45E-06 1.01E-06299.5 + +
02 9922 1.27E-01 1.53E-04 5.45E-04 1.83E-04 9.25E-06 2.44E-062.24E +
02 10627 1.35E-01 1.87E-04 7.66E-04 2.47E-04 1.33E-05 3.06E-061.13E +
02 9225 1.18E-01 1.29E-04 3.85E-04 1.12E-04 6.06E-06 1.96E-06300.2 + +
03 8019 9.98E-02 1.49E-04 2.72E-04 9.28E-06 3.13E-067.57E +
03 8294 1.06E-01 1.76E-04 3.63E-04 1.24E-05 3.68E-064.18E +
03 7595 9.34E-02 1.29E-04 2.38E-04 7.19E-06 2.79E-06300.4-00.9 He 2- 84 8.06E +
02 11855 11504 1.46E-01 4.30E-04 3.51E-04 1.09E-04 1.27E-05 3.57E-069.53E +
02 12431 12048 1.54E-01 5.22E-04 3.93E-04 1.30E-04 1.45E-05 3.94E-066.71E +
02 11378 11169 1.38E-01 3.52E-04 2.94E-04 9.92E-05 1.06E-05 3.10E-06300.5-01.1 He 2- 85 3.01E +
03 11663 11815 1.16E-01 2.00E-04 4.03E-04 8.86E-05 7.36E-06 3.28E-06 1.54E-063.80E +
03 12094 12198 1.23E-01 2.42E-04 4.64E-04 9.50E-05 8.47E-06 3.63E-06 2.30E-062.51E +
03 11204 11406 1.09E-01 1.62E-04 3.55E-04 7.56E-05 6.17E-06 2.94E-06 9.97E-07300.7-02.0 He 2- 86 9.96E +
03 11073 8659 1.39E-01 4.25E-04 5.42E-04 1.82E-04 1.96E-05 6.54E-06 6.36E-061.45E +
04 11741 9033 1.49E-01 5.88E-04 7.52E-04 2.58E-04 3.07E-05 8.27E-06 1.40E-056.77E +
03 9808 8045 1.30E-01 3.35E-04 4.59E-04 1.34E-04 1.57E-05 5.77E-06 4.04E-06300.8-03.4 ESO 095-12 3.76E +
02 12902 9.41E-05 2.76E-04 5.05E-05 1.35E-05 2.29E-064.78E +
02 14770 1.40E-04 4.74E-04 9.93E-05 2.66E-05 3.46E-062.93E +
02 10436 6.60E-05 1.77E-04 2.65E-05 8.22E-06 1.62E-06305.1 + +
04 24953 5.25E-02 3.78E-06 8.88E-06 5.53E-07 6.93E-07 3.76E-07 3.96E-071.00E +
05 25828 6.09E-02 7.98E-06 1.39E-05 7.40E-07 1.01E-06 4.74E-07 5.84E-077.21E +
03 21122 5.15E-02 2.94E-06 8.26E-06 4.86E-07 6.32E-07 3.36E-07 3.33E-07307.3 + +
01 17216 1.06E-01 2.07E-04 3.84E-05 1.32E-066.48E +
02 18192 1.13E-01 3.69E-04 5.98E-05 1.49E-063.00E +
01 16303 9.83E-02 1.61E-04 3.08E-05 1.14E-06308.2 + + +
03 12410 8444 1.35E-01 1.73E-04 6.05E-04 1.78E-04 1.91E-05 4.63E-06 1.18E-051.22E +
04 13139 8564 1.43E-01 2.22E-04 7.86E-04 2.40E-04 2.55E-05 5.28E-06 1.85E-055.93E +
03 11439 8068 1.27E-01 1.41E-04 5.71E-04 1.43E-04 1.68E-05 4.33E-06 7.46E-06309.5-02.9 MaC 1- 2 1.63E +
03 11936 11754 1.32E-01 3.55E-04 3.94E-04 7.51E-05 4.10E-06 2.63E-061.96E +
03 13156 13256 1.39E-01 6.42E-04 7.09E-04 1.53E-04 8.03E-06 4.03E-061.38E +
03 10827 9507 1.23E-01 2.17E-04 2.76E-04 4.27E-05 1.97E-06 1.96E-06
Article number, page 31 of 35 able B.3.
Continued.
PN G Main Name n e (S ii ) T e (O iii ) T e (N ii ) He / H N / H O / H Ne / H S / H Ar / H Cl / H310.7-02.9 He 2-103 3.08E +
02 10404 12355 1.27E-01 8.98E-05 2.76E-04 1.08E-04 1.06E-05 1.30E-063.60E +
02 11348 13745 1.34E-01 1.88E-04 4.72E-04 1.66E-04 2.62E-05 2.16E-062.24E +
02 9488 9873 1.17E-01 7.86E-05 2.02E-04 4.72E-05 7.40E-06 1.03E-06311.4 + +
03 10812 1.31E-01 2.10E-05 3.52E-04 8.33E-05 4.30E-06 2.02E-06 6.10E-061.29E +
03 11135 1.37E-01 2.50E-05 4.08E-04 9.62E-05 5.01E-06 2.27E-06 7.52E-068.21E +
02 10507 1.24E-01 1.90E-05 3.01E-04 7.47E-05 3.80E-06 1.82E-06 4.88E-06312.6-01.8 He 2-107 2.49E +
03 7015 1.42E-01 1.51E-04 4.69E-04 8.80E-06 5.06E-063.09E +
03 7371 1.51E-01 1.92E-04 7.18E-04 1.24E-05 6.40E-061.98E +
03 6396 1.32E-01 1.26E-04 3.20E-04 6.37E-06 4.12E-06315.1-13.0 He 2-131 8918 20404 3.20E-02 3.22E-05 6.71E-05 1.64E-07 1.18E-079197 24008 3.49E-02 3.87E-05 8.08E-05 2.53E-07 1.55E-078729 17216 2.86E-02 2.57E-05 5.22E-05 9.84E-08 9.17E-08315.4 + +
02 11001 10816 1.32E-01 1.36E-04 4.80E-04 1.64E-04 2.85E-06 1.93E-066.53E +
02 11237 11032 1.39E-01 1.58E-04 5.50E-04 1.86E-04 3.39E-06 2.16E-064.72E +
02 10605 10506 1.24E-01 1.20E-04 4.42E-04 1.48E-04 2.27E-06 1.71E-06316.1 + +
02 8083 10396 1.26E-01 2.80E-05 1.91E-04 1.62E-05 1.67E-06 1.92E-06 4.16E-071.06E +
03 8463 11712 1.33E-01 3.78E-05 2.80E-04 2.67E-05 3.21E-06 2.85E-06 1.03E-067.45E +
02 7592 9057 1.17E-01 2.19E-05 1.39E-04 1.00E-05 1.06E-06 1.36E-06 1.89E-07318.3-02.5 He 2-116 1.75E +
02 10299 1.44E-01 1.95E-04 3.52E-04 1.59E-04 1.64E-05 3.05E-062.37E +
02 10641 1.54E-01 2.32E-04 4.27E-04 2.31E-04 1.86E-05 3.63E-061.17E +
02 9872 1.35E-01 1.76E-04 3.17E-04 1.19E-04 1.54E-05 2.74E-06319.2 + +
03 12685 14422 1.40E-01 2.67E-04 2.93E-04 7.20E-05 5.29E-06 1.74E-06 5.26E-072.41E +
03 13103 15135 1.47E-01 3.16E-04 3.24E-04 7.66E-05 5.98E-06 1.87E-06 6.16E-071.60E +
03 12124 14126 1.31E-01 2.21E-04 2.54E-04 5.94E-05 4.40E-06 1.54E-06 4.05E-07320.9 + +
03 11101 8090 1.53E-01 5.92E-04 6.02E-04 1.58E-04 2.42E-05 6.85E-06 8.95E-061.03E +
04 11727 8978 1.64E-01 9.02E-04 9.99E-04 2.70E-04 4.78E-05 9.91E-06 2.66E-054.74E +
03 10264 7080 1.42E-01 3.69E-04 3.96E-04 8.86E-05 1.20E-05 4.96E-06 3.19E-06321.3 + +
04 11453 8926 1.17E-01 8.25E-05 3.71E-04 6.33E-05 7.15E-06 2.96E-06 4.43E-062.30E +
04 12391 9618 1.24E-01 1.20E-04 8.64E-04 1.39E-04 1.23E-05 4.12E-06 1.01E-057.90E +
03 7178 7803 1.08E-01 5.87E-05 2.63E-04 4.23E-05 4.44E-06 2.27E-06 1.68E-06321.8 + +
02 9709 1.47E-01 2.88E-04 4.54E-04 1.51E-04 8.43E-06 3.72E-063.70E +
02 10064 1.55E-01 3.49E-04 5.27E-04 2.53E-04 1.09E-05 4.17E-062.20E +
02 9419 1.39E-01 2.17E-04 3.81E-04 9.30E-05 5.92E-06 3.25E-06322.5-05.2 NGC 5979 5.09E +
02 (22456) 14604 1.11E-01 6.70E-05 3.44E-04 5.75E-05 5.32E-06 2.27E-06 9.30E-068.49E +
02 (27308) 15206 1.17E-01 7.62E-05 4.06E-04 6.59E-05 5.92E-06 2.48E-06 1.13E-052.40E +
02 ( 8121) 14049 1.05E-01 5.62E-05 2.87E-04 5.13E-05 4.62E-06 2.03E-06 6.87E-06323.9 + +
03 7687 1.64E-01 2.44E-04 2.92E-04 5.82E-05 7.67E-06 3.19E-06 1.33E-062.51E +
03 7859 1.74E-01 2.83E-04 3.31E-04 7.26E-05 8.75E-06 3.58E-06 1.58E-061.75E +
03 7507 1.55E-01 2.22E-04 2.57E-04 4.16E-05 6.04E-06 2.79E-06 1.02E-06324.2 + +
03 6158 2.80E-02 2.38E-04 5.37E-04 1.34E-05 9.45E-075.83E +
03 6492 3.03E-02 3.24E-04 9.27E-04 2.09E-05 1.20E-063.13E +
03 5763 2.63E-02 1.74E-04 2.89E-04 8.83E-06 7.39E-07324.8-01.1 He 2-133 7.82E +
03 14361 10072 1.40E-01 4.88E-04 4.28E-04 1.65E-04 1.25E-05 3.39E-06 4.67E-061.32E +
04 15328 11171 1.49E-01 7.56E-04 6.82E-04 2.89E-04 2.19E-05 4.63E-06 1.07E-055.42E +
03 13180 8719 1.29E-01 3.14E-04 2.88E-04 1.02E-04 7.20E-06 2.57E-06 1.61E-06
Article number, page 32 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Table B.3.
Continued.
PN G Main Name n e (S ii ) T e (O iii ) T e (N ii ) He / H N / H O / H Ne / H S / H Ar / H Cl / H327.1-01.8 He 2-140 1.06E +
04 8254 1.27E-04 2.86E-04 8.14E-06 2.29E-063.07E +
04 8906 2.65E-04 1.08E-03 2.54E-05 3.92E-066.60E +
03 7375 9.05E-05 1.39E-04 4.28E-06 1.74E-06327.8-01.6 He 2-143 6.37E +
02 11164 12925 1.24E-01 3.53E-04 6.11E-04 1.34E-04 1.26E-05 3.22E-06 1.76E-067.70E +
02 11580 13468 1.30E-01 4.10E-04 6.91E-04 1.52E-04 1.45E-05 3.52E-06 2.15E-065.43E +
02 10822 12544 1.17E-01 2.83E-04 5.28E-04 1.18E-04 1.03E-05 2.87E-06 1.28E-06336.9 + +
02 10845 11766 1.16E-01 9.76E-05 4.11E-04 9.24E-05 5.75E-06 1.94E-06 1.38E-069.61E +
02 11721 12174 1.22E-01 1.24E-04 4.82E-04 1.07E-04 7.05E-06 2.25E-06 1.92E-066.84E +
02 9864 11392 1.11E-01 6.99E-05 3.66E-04 8.18E-05 4.53E-06 1.73E-06 8.83E-07
Article number, page 33 of 35 ppendix C: Supplementary figures
Fig. C.1.
Spectra of the new PNe with WELs stars. Dotted lines markpossible locations of stellar emission-lines identified with the ion nameif the line was detected.
Fig. C.2.
Spectra of the possible new PNe with Wolf-Rayet typecentral stars.Article number, page 34 of 35.K. Górny: Spectroscopy of southern Galactic disk planetary nebulae
Fig. C.3.
Spectra of the reobserved PNe with known and misclassifiedemission-line central stars.
Fig. C.4.
Ratio of O + ionic abundances derived from λ λ Fig. C.5.
Ratio of O + ionic abundances derived from λ λ T e (N iiii