Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México

Riesgo, H.; López, J. A. H 2-12, A Misidentified Planetary Nebula in Kepler SNR Revista Mexicana de Astronomía y Astrofísica, vol. 41, núm. 1, abril, 2005, pp. 57-60 Instituto de Astronomía Distrito Federal, México

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How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative © Copyright 2005: Instituto de Astronomía, Universidad Nacional Autónoma de México vn msinlnsadln-ltehlesetafrom spectra echelle long-slit and lines emission evant remnants. supernova e.g., with nebulae, excited sample shock that [N in values [S with and objects ratios, the line highest among the is L´ 2–12 & (Riesgo-Tirado H [N ratios high line with emission PNe of program at the Kohoutek in by (1994;1997). included published dates not PNe later PN is misclassified PNe 2–12 probable of galactic H list or of true 004.5+06.8). Catalogue a (PNG al. ESO-Strasbourg plan- as et the misclassified again Acker in a it on as later include works However, it (1992) these (PN). list of nebula (1987) consequence etary al. super- a et Kepler’s as of Acker Probably remnant nebular the nova. in bright- the knot Bond as but est it describe 1) catalogue (1978) 4+6 Kohoutek (1967) and (PK (1976) Kohoutek nebulae planetary & galactic Perek in- of was the object in The cluded 1952). (Haro objective observations through prism camera Schmidt Tonantzintla the eit eiaad Astronom´ de Mexicana Revista eew rsn epnro-adiaeyi rel- in imagery narrow-band deep present we Here observing an of part as 2–12 H studied have We with Haro Guillermo by discovered was 2–12 H –2 IIETFE LNTR EUAI ELRSNR KEPLER IN NEBULA PLANETARY MISIDENTIFIED A 2–12, H ii] /H α lmnslctdo h etr ieo elrssproarmat Therefore, nebula. planetary remnant. misclassified supernova a Words: Kepler’s as Key the noted of However, and be side knots must nebula. brightest western 2–12 the planetary of the H true part on actually a is located as object filaments this classified that been shows here has presented nebula data This 2–12. H err´ clasificaci´ como la considerada tanto, ser lo debe Por planetaria Sin nebulosa Kepler. una planetaria. de m´ supernova nebulosa filamentos de una y remanente como nudos clasificada los sido aqu´de ha presentados nebulosa datos los Esta embargo, 2–12. H de .0smlrt hs xetdfrom expected those to similar 0.90 = .INTRODUCTION 1. arwbn ietiae n ogsi,ehlesetaaepeetdfor presented are spectra echelle long-slit, and images direct Narrow-band im´ Presentamos nvria ainlAut´ Nacional Universidad YRDNMC S:IDVDA H21)— 2–12) (H INDIVIDUAL ISM: — HYDRODYNAMICS LE—IM UENV REMNANTS SUPERNOVA NEB- ISM: PLANETARY ISM: — — ULAE OUTFLOWS AND JETS ISM: eevd20 oebr1;acpe 04Dcme 6 December 2004 accepted 18; November 2004 Received ii] ayAstrof´ y ıa /H gnsd ad not seto cel ernialarga rendija de echelle espectros y angosta banda de agenes α ii] n [S and /H pz2002). opez .Reg n .A L´ A. J. and Riesgo H. ısica sbilne oaiao nl at cietld la de occidental parte la en localizados brillantes as nttt eAstronom´ de Instituto α =2.89 ii] nm eM´ de onoma , /H 41 ABSTRACT usrnqeet beoe nraia parte realidad en es objeto este que muestran ı RESUMEN 76 (2005) 57–60 , α /.,21 eecp fteOsraoi As- Observatorio the of telescope m tron´ 2.12 f/7.9, super- Kepler’s fila- of and side remnant. knots western nova bright the in the located of planetary ments part true rather a not but is observa- nebula nebula These this that nebula. confirm tions the across positions several fH21 ntelgto [O images of The light the 27. in June 2–12 2000 H on of MEX- wheel the filter with MAN obtained were images narrow-band ( rme n iie ytercrepnigflat- corresponding 1–1. between their varied Seeing by fields. divided were and they rays; standard trimmed cosmic by and reduced bias were removing techniques images The detector. the AHPBW),H˚ ntueto 00Jn 9 hsiae hw in shown image, This 29. June 2000 on instrument racnee nH2–12. H on centered area ie ee10 o ahiae IECCD SITE A image. each for 1024 s with 1800 were times 54 evtos h mgsi i.1cvra1 a cover 1 Fig. in images The servations. xc,Esnd,B . M´ C., B. Ensenada, exico, λ c ohiae n pcr eeotie tthe at obtained were spectra and images Both nH An PW r hw nFgr .Exposure 1. Figure in shown are HPBW) A ˚ mc ainli a er M´ Pedro San in Nacional omico 6585 opez .OSRAIN N RESULTS AND OBSERVATIONS 2. ıa α ,10 A, ˚ × onea. mg a lootie ihtesame the with obtained also was image 04 24 1024, α ( AHPBW)and[S˚ λ nd –2como 2–12 H de on c 6565 µ m( ,11 A, ˚ exico ≡ 0. iii] )sur ieswas pixels square 3) uigteeob- these during 5 AHPBW),[N˚ ( λ ii] c 5009 ri.The artir. ( λ c . 6726 4 ,52 A, ˚ × 1 A, ˚ 57 ii] . 4 © Copyright 2005: Instituto de Astronomía, Universidad Nacional Autónoma de México × oaihi ersnaini iue2 oesa2 a covers 2, Figure in representation logarithmic nH21.I oesa rao 1 of area an covers centered It images 2–12. negative logarithmic H of on mosaic A 1. Fig. L & RIESGO 58 2 . raadsoscerytermral large remarkable the clearly shows and area 8 30" .
4 × [O N] [N 1 [S . H
4. III II II α ] ] . 8 hs ein r hw ntesm figure. same the in shown are regions these [N corresponding uiu bet(ureo V´ this to (Guerrero, resemblance L´ some object (e.g., bears curious 1–17 structures Pe complex Only with peculiar, 2000). highly PNe is for morphology even its However, PN. lar mn h N nw oteauthors. the to known PNe the among oaino h ltpstosaeidctdi Fig- in indicated H logartithmic are a positions over 3 slit posi- The ure the slit spectrum. of the calibration a all of location by for times followed obtained Integration each were tions, nebula. duration across the s obtained of 1800 was body positions slit main seven the of set A W. cuayaantaT/raclm.Tespectral The s lamp. km 10 arc was Th/Ar resolution a against accuracy f2 of H Logarithmic 2. Fig. h k.Tesetawr airtdto calibrated were spectra The sky. the adit a sdt slt h 7hodrcon- order H 87th the 90 the isolate This of taining to filter used 2003). was A bandwidth al. A cross-dispersion. ˚ et no Meaburn has 1984; spectrometer SPM al. at et Spectrometer (Meaburn Echelle Manchester the with 2–12. H of neighborhood the in structure scale rldmnin.Cneunl,52iceet,each increments, 0 512 Consequently, spec- and dimensions. spatial tral Two both in above. employed described was binning CCD times SITE same the used We OPEZ ´ . 0ln,gv oa rjce ltlnt f5 of length slit projected total a gave long, 60 . tfis lne –2rsmlsakot,bipo- knotty, a resembles 2–12 H glance, first At h ogsi cel pcr eeobtained were spectra echelle long-slit The
8 × 2 .
.Nrhi padadEs st h etside. left the to is East and upward is North 8. α +[N ii] .DISCUSSION 3. 3.1 α 54ln rfie xrce from extracted profiles line 6584 Morphology . mg fH21 oeiga area an covering 2–12 H of image ii] − 1 h ltwsoine – E oriented was slit The . 58 54eiso lines. emission 6584 6548, α zuz L´ & azquez, mg fH21.The 2–12. H of image ± pz1999) opez . ms km 1.0 . 2on 12 opez − 1 © Copyright 2005: Instituto de Astronomía, Universidad Nacional Autónoma de México mg.Alsisaeoine –.Te[N The E–W. oriented are slits All image. xiainseis(e i.1.A diinlpuz- H additional the An in apparent 1). structure, high Fig. zling and (see low species in bright excitation are curved knots and elongated These an morphology. follow that knots distinct of eelalkl addt stecr fteputative the of not core does the nebula. as images planetary candidate the likely of Further- a inspection reveal apparent. detailed is nebula a the more, of side other counter-part be the No on hardly outflow. can collimated which a cavity perimeter with or identified the filament bent structure defining circular remarkably this a if and 2) of as extended Fig. north-east, very (see the be towards scale, to larger north- noted a the is towards On of center extends the and east. from nebula) (not bright structure the knotty sec- the northern of the from tion emerge to seems that filament nsa,ee o N ihhg-eoiyoutflows high-velocity with L´ PNe (e.g., for even unusual, ue msini eetdoe –2 nylocalized only 2–12, H over detected is emission fuse, i.3 e fsvnln-ltehlesetaotie cosH21.Si oiin r niae vralgrtmcH logarithmic a over indicated are positions Slit 2–12. H across obtained spectra echelle long-slit seven of Set 3. Fig. oiinvlct diagrams. position-velocity -400 -2000 h anbd fH21 sfre yagroup a by formed is 2–12 H of body main The h iepolsfo h nt fH21 r very are 2–12 H of knots the from profiles line The V pze l 97 L´ 1997; al. et opez Hel [ kms] -1 3.2 Kinematics . 2 1 3 pz20) ogoa,dif- global, No 2002). opez 30" 30" α mg,i long a is image, -2 IIETFE N59 PN MISIDENTIFIED A 2-12, H ii] λ c 6585 iepolsetatdfo hs ltpstosaesonas shown are positions slit these from extracted profiles line A ˚ evdt oenal ihacmo ihveloc- high ob- common is a 2–12 with H nearly of move structure to knotty served whole the Thus, ih.Ol nteeteesi oiin n 7 and 1 V positions between blueshifted, values predominantly slit be with extreme to seems the of even material line in the sense, the Only other to any respect sight. with in tilts nor extreme nebula, considering the of out- center the in signs bipolar no flowofanykindofsymmetrywithrespecttothe a are to there correspond pro- Furthermore, line not the outflow. do PN, knots bipolar these a from as files However, interpreted is clumps. 2–12 dense H with if wind interac- at stellar the the though of from 1998), tion originate (1996; which al. speeds lower et much Meaburn by 78 Abell [O the to airglow. to corresponds 3 Fig. in grams tnearly at (V eoiysie oeigarneof range a narrow covering by characterized spikes are velocity kinematics knot The individual 3). each Fig. of (see knots the from emission hel h iepolsi –2aesmwa similar somewhat are 2–12 H in profiles line The ∼ 4 0to iii] W − E E 0 ms km 300 eoiysie dnie nAel3 and 30 Abell in identified spikes velocity − 0 ms km 400 7 6 5 4 3 2 1 N − 1 hel ln h lti h Vdia- PV the in slit the along − ∼− 1 -400 -2000 .Teeiso located emission The ). 5 to 350 V Hel [ kms] ∼ − 5 ms km 150 0 ms km 400 -1 7 6 5 − − 1 α 1 . © Copyright 2005: Instituto de Astronomía, Universidad Nacional Autónoma de México 0REG L & RIESGO 60 r oeai otoeepce rmcollisionally from expected regions. those shocked to excited akin [N more high are the the morphology, symmetry, [S expanding overall regions, apparent emission any odd of localized lack highly the and speeds high extended an from expected region. be shocked would as pattern, ity .Reg n .AbroL´ Alberto J. and Riesgo H. respectively. 32214-E, and sup- IN112103 through grants CONACYT continuous and DGAPA-UNAM from acknowledges port JAL CONACYT. PN. misclassified a as noted Kepler’s be bright- then of should the edge and is western to SNR the It on corresponds structure knotty 2–12 investigation. est, H this that motivated concluded PNe of in survey released recently sup- opti- remnant, is http://chandra.harvard.edu/photo/2004/kepler/. supernova (Chandra), interpretation X-ray Kepler This combined ( the cal shocked passage blast. by the radiative SNR ported after as the cooling behaving of and now expanding form are regions, rem- that 2–12 knots the dense in are H the originated where profiles environment having line nant as velocity understood high thus localized, peculiar, Kohoutek. by PNe misidentified the and of catalogue the lists ESO-Strasbourg in the unnoticed e.g., field, gone PN SNR; had Kepler’s connection of part this known however, well a have as (1991) 2–12 Vancura H studied & Long, Blair, (1991); Pritchet of number a Furthermore papersinthefieldofSNR(e.g.,VandenBergh& with SNR. 2–12 Kepler’s H Oph, identified V843 finding already had na- nabulae, (1976) planetary its Bond of explore that realm to the us beyond prompted ture PN, a to responding ii] h euirln rfie nH21 ihtheir with 2–12 H in profiles line peculiar The M´ from scholarship posgraduate a acknowledges HR our in found 2–12 H of ratios line unsual The and ratios, line morphology, anomalous The cor- not 2–12, H of characteristics unusual The /H HST xc hiso [email protected]). (hriesgo, exico α ierto n h rgt[O bright the and ratios line n nrrd(pte)iae fthe of images (Spitzer) infrared and ) .TENTR FH2–12 H OF NATURE THE 4. pz nttt eAstronom´ de Instituto opez: iii] ii] /H emission α and a NM po otl87 20 neaa .C., B. Ensenada, 22800 877, Postal Apdo. UNAM, ıa, a e eg,S,&Pice,C 91 AP 0,194 103, PASP, 1991, C. Pritchet, & S., Bergh, den Van L´ & H., Galac- Riesgo-Tirado, of Catalogue 1967, L. Kohoutek, & L., Perek, ootk .17,i A yp 6 lntr Nebulae, Planetary 76, Symp. IAU in 1978, L. Kohoutek, ce,A,Ohebi,F,Sehl,B,Tlna R., Tylenda, B., Stenholm, F., Ochsenbein, A., Acker, L´ ebr,J,L´ J., Meaburn, ao .15,Bl b.Tnnznl auaa 1, Tacubaya, y Tonantzintla Obs. Bol. 1952, G. Haro, ureo .A,V´ A., 192 M. 88, PASP, Guerrero, 1976, E. 366, H. ApJ, Bond, 1991, O. Vancura, & S., K. Long, P., W. Blair, Stenholm, & R., S. Pottasch, M., Chopinet, A., Acker, ebr,J,L´ J., Meaburn, L´ F., & D. 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