2 0 0 3MNRAS.343. .192R 2 12,3 1 *E-mail: [email protected](JR);[email protected] (JKK);[email protected]. believed tobelightfromtheobscured BLRreflectedintoourline- region (BLR)arevisible,whileinSeyfert2(Sy2)galaxiesthetorus Accepted 2003March23.Received17;inoriginalform2002October28 European SouthernObservatory,Karl-Schwarzschild-Str2,D-85748GarchingbeiMünchen,Germany Mon. Not.R.Astron.Soc.343,192-208(2003) tion ofpolarizedbroadlinesinmanySy2s(e.g.Moranetal.2000), nucleus. InSeyfert1(Syl)galaxiesthenucleusandbroadline In thecurrentlyfavouredunifiedmodelsofactivegalacticnuclei ^Max-Planck-Institut fürAstronomie,Königstuhl17,D-69117Heidelberg,Germany J. Reunanen,*K.KotilainenandM.A.Prieto Near-infrared spectroscopyofnearbySeyfertgalaxies-II.Molecular de(MAP) obscures thenucleusandBLRonlynarrowlineregion content andcoronalemission (NLR) isvisible.Evidencefortheunifiedmodelsincludesdetec- (AGN; e.g.Antonucci1993),athickmoleculartorussurroundsthe 1 INTRODUCTION Tuorla Observatory,UniversityofTurku,Väisäläntie20,FIN-21500Piikkiö,Finland © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem blueshifted which,togetherwiththehighBry/[Fe11]ratios,suggestsshocksasdominant range from<20to^300pc,andarelargerthanthepredictedsizesformoleculartorus(1- parallel toitin6/8(75percent)galaxies,agreementwiththeunifiedmodelsofactive We presentsubarcsecnear-infrared1.5-2.5yimmoderateresolutionlong-slitspectraofeight medium. most plausibly,byshockexcitationduetothejetorsuperwindinteractingwithinterstellar two objectswithnoevidenceforahiddenpolarizedbroadlineregion.Thishighdetectionrate it. ThesespectracomplementsimilardataonsixSeyferts,presentedinReunanen,Kotilainen nearby Seyfertgalaxies(z<0.01),bothparalleltotheionizationconeandperpendicular ABSTRACT Key words:galaxies:active-nucleiSeyfertinfrared:galaxies. direction paralleltothecone.Thiscouldbeexplainedbyastronglycollimatedradiationfieldor, in ~60percentofthegalaxies.Inthreegalaxiescoronallinesareextendedonly excitation mechanisminSeyfertgalaxies. directly fromthetorus. galactic nuclei.Thefullwidthathalfmaximum(FWHM)sizesofthenuclearH2emission excited H2andtheexcitationmechanismsofinterstellargas. Seyfert type.ThespatialextentoftheHemissionislargerperpendiculartoconethan & Prieto,andareusedtostudythespatialextentoflineemission,integratedmasses stresses theimportanceofextinctioneffectsasmaincauseforSeyfertdichotomy. 100 pc).Thustheemissionprobablyarisesfrommaterialsurroundingtorusratherthan 2 Bright coronalemissionlines[Sivi]andvu]arecommoninSeyferts,astheydetected Bry and[Fe11]correlatebothspatiallykinematically.Nuclearemissionisgenerally Broad BrywasdetectedinnearlyhalfoftheopticallyclassifiedSeyfert2galaxies,including Large concentrationsofmoleculargas(H2)arepresentinthenucleusregardless been madeatonlymoderatespatial resolution(Veilleuxetal.1997: imized contaminationfromcircumnuclearstarformation,canbe tion tosearchformaterialassociatedwiththetorus,amin- Tsvetanov 1996),almostinvariablyalignedwiththeradiojets. 250; Sosa-Britoetal.2001:1arcsec, R—1100),and/orwithonly of the[Om]emission(e.g.Storchi-Bergmann etal.1999),and one slitpositionangle(PA)along theradioaxisormajor 3-arcsec aperture,R=1400;Winge etal.2000:7-8arcsec,R= able. However,untilrecentlysuchNIRspectroscopicstudieshave achieved inthenear-infrared(NIR;e.g.Veilleux,Goodrich&Hill of-sight, andcone-like[Oin]structures(e.g.Mulchaey,Wilson& 1997), whereawealthofemissionandabsorptionlinesareavail- 1 to100pc(e.g.Pier&Krolik1993).Adequatespatialresolu- The predictedsizeofthemoleculartorusinAGNrangesfrom © 2003RAS 2 0 0 3MNRAS.343. .192R -1 -1 red grismwithresolutionR=980andslitwidth1.0arcsec.The rized. InSection3theresultsforindividualgalaxiesarediscussed, both typeswithanionizationcone.Inthispaper,wecomplement the sample,incomparisonwithnon-Seyfertspirals. molecular gasinthecentralregions.Inforthcomingpublications, trace thespatialdistribution,dynamicsandexcitationofmolecular the sizeoffinalsampleis14Seyferts.Thesedataareusedto these resultswithsimilardataoneightadditionalSeyferts,thus in oursampleofnearby(0.0018redshift,scale,inclination,PA Peletier etal.(1999)andMulchaey,Regan&Kundu(1997),respec- The averageseeingduringtheobservationswas~0.9arcsecfull nology Telescope(NTT),usingthe1024xpixelSOFIcamera Paper I.Hereonlyabriefsummaryisgiven.EightnearbySeyferts The observationsanddatareductionaredescribedindetail AND METHODSOFANALYSIS 2 OBSERVATIONS,DATAREDUCTION g =0.5areassumed. Galaxy Table 1.Observationalpropertiesofthegalaxies. cept forNGC1068and3783,whichweusedtheimagesfrom wavelength rangecoveredis1.5-2.5pmandtheusefulslitlength width athalfmaximum(FWHM).Thespectraweretakenwiththe were observedin2000Decemberwiththe3.5-mESONewTech- data reductionandmethodsusedintheanalysisarebrieflysumma- we shallstudythestellarpopulationsandstarformationhistoriesof emission. and nebulargas,todeterminethemassofhot(T>1000K) © 2003RAS,MNRAS 343,192-208 are giveninTable1. of themajoraxis,morphology,AGN type),thePAsofslit, of 14galaxies.Throughoutthispaper,H=15kmsMpcand and inSection4wepresenttheconclusionsbasedonfullsample ~2 arcmin.Shortbroad-bandJHKsimageswerealsoobtained,ex- (Lidman, Cuby&Vanzi2000)withpixelscale0.288arcsec. 1.5-2.5 \immoderateresolutionspectroscopyofthefirstsixgalaxies 0 0 The long-slitspectraweretaken both parallelandperpendic- This paperisorganizedasfollows.InSection2theobservations, In Reunanenetal.(2002,hereafterPaperI),wepresentedlong-slit © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem 0.00540 0.00973 0.00795 0.00771 0.00544 0.00779 0.00546 0.00379 0.00179 0.00194 0.00382 0.00483 0.00289 0.00425 -1 (pcarcsec) (°) Scale iPA 107 192 157 152 108 154 108 94 56 75 74 82 19 19 46 42 65 78 56 28 74 65 27 72 53 57 39 32 158 141 157 160 158 135 157 43 25 22 70 30 30 32 / (R^SABO^bc (Ri)SAB(r)0/a Morphology (R'^SBO^b (R)SB(s)ab 1 SB(s)cd: sp SAB(s) pec (R)SA(rs)b (ROSB(s)b (R')SB(r)a - SA:(1)0+ SB(s)0+ SABO SO pec Sa pec 1 -L85 1 Inc., undercooperativeagreementwith theNationalScienceFoundation. regions (e.g.Colina1993).X-rayexcitationcanalsoproducelower UV pumping(fluorescence;e.g.Black&vanDishoeck1987).The mal (collisional)excitationbyshocks(e.g.Hollenbach&McKee The extinctionforthecentralregionisgiveninTable2and up toA=0.02inNGC2992.Wehaveassumedtheextinctionlaw the nuclearemissionlinesincontinuumcoloursisnegligible, ies (H—K=0.22;Huntetal.1997).Althoughthiscontinuum from thespectrawithcoloursofnormal,unobscuredspiralgalax- used. binned together.Forthefaintestemission,evenlargerbinsizeswere In ordertotracetheextendedemission,threepixelswereusually tainties of1-0S(3)and[Sivi]arelarger;20-40percenttheflux. All thespectraofagivengalaxywerecombinedandcentral lines, dividedbyanatmosphericstandardstar,andfluxcalibrated. wavelength calibrationfromOHskylinesandXearclamp.The flatfielding usingdomeflats,badpixelandcosmicrayremoval, are operatedbytheAssociationofUniversities forResearchinAstronomy, citation mechanisms.Forexample,theH2lineratio2-1S(l)/l-0 emission lineratioscanbeusedtodistinguishbetweentheseex- unlikely tobelarge,asdiscussedinPaperI.Theeffectofincluding extinction maynotbecorrectforthelineemission,differenceis except 3aforupperlimits.Becauseoftelluricresiduals,theuncer- errors aregenerallydominatedbythecontinuumfitting,and1 [Fe ii]/BryishigherinX-rayorshock-excitedregionsthanH11 100. TheHlineratios2-1S(l)/l-0 S(l)and1-0S(0)/l-0S(2) 1989), ultraviolet(UV)radiationindenseclouds(e.g.Sternberg 1.5-arcsec (5-pixel)spectrumwasextracted,withinaneffective k A 2 Possible mechanismsfortheH2emissioningalaxiesarether- Extinction wasestimatedbycomparingtheintegratedcolours NIR spectroscopyofnearbySeyferts-II193 Syl.5 Syl.8 Type Sy2 Sy2 Sy2 Sy2 Syl Sy2 Syl Sy2 Syl Sy2 Sy2 Sy2 15,54 -64 -42 -20 -60 -50 -55 PA y -3 (°) 50 64 75 15 12 1 -36, -75 PA -40 -75 -89 -26 -15 -78 ± (°) 48 40 26 70 30 35 87 2 x32,48 48, 80 48, 64 48, 64 48, 40 48, 48 48, 48 56, 40 64, 56 32, 64 32, 32 32, 32 32, 32 16, 48 (min) tint Resolution (arcsec) 0.9 0.9 0.8 0.9 0.8 0.8 0.9 0.7 0.9 1.0 1.0 1.1 1.0 1.0 2 0 0 3MNRAS.343. .192R 15-2 Á dependingonwavelength).Decompositionintotwocomponents:(a)28±4(5percentofthetotalflux)and1636Â,(b)333(10cent)178 been obtainedbymeasuringthelinefluxineachcolumnacross Bry He i Nucleus Line nuclear spectrainFig.2.Thespatial extentofthemainemission The nuclear30xarcsecTGband imagesofthegalaxies,with 3 RESULTS the nuclearregionandarecorrectedforseeing.Thenumberof nucleus. However, 1-0S(l)emissionislikelytobebiasedtowardswarmer fraction ofHinthei;=1,/3energyleveldecreasesrapidly the mass,ifrealtemperatureis>1500K.Below1500K mal equilibrium,andaregiveninTable3.If7\.isunknown,it the rotationaltemperatureT,respectively. 2- 1S(l) 20 Á,(c)42.6±4(6percent)and1856(d)4710(72227(e)33.91.1(92055À. are inunitsof10“ergcmandtheGaussianFWHMs(secondrow)A.Thewidthlineshasnotbeencorrectedforinstrumentalprofile(30-32 Table 2.Observedemissionlinefluxeswithinthenuclear1.4arcsecdiameteraperture,afteraddingalldatafromdifferentslitPAs.The(firstrow) columns fittedwaschosentoincludethenuclearknotandexclude gas, becauseTapper=6950Kforthei;1,/3level.Wehave was derivedusingthetransitionprobabilitiesfromWolniewicz, can beusedtoderivethevibrationalexcitationtemperatureTand of thegalaxies. any additionalextendedemission.Thestructuresprobedherecorre- also determinedtheaveragesurfacedensityofexcitedHin and themassisunderestimatedbyafactorof~10if7=1000K. assumed tobe2000K.Thisleadsafactorof~2uncertaintyin Simbotin &Dalgarno(1998),thevibrationtemperatureandther- A* slit positionsoverlaid,areshown in Fig.1andtheH-Æf-band spond tophysicalscalesof100-200pc,dependingonthedistance [Si vu] [Ca vin] [A1 ix] [Si vi] [Fe it] 1-0 Q(3) 1-0 Q(l) 1- 0S(0) 1-0 S(l) 1-0 S(2) 1-0 S(3) 194 J.Reunanen,K.KotilainenandM.A.Prieto 2 ib rol ylh 2 The GaussianFWHMsizesforHand[Fen]inTable3have The massoftheexcitedmolecularhydrogeninnucleus 2 © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem 2.483 2.424 2.407 2.321 2.248 2.224 2.166 2.122 2.058 2.043 2.034 1.964 1.958 1.644 jam k NGC 1068 49.8 ±4.5 74.3 ±8.9 29.1 ±3.2 34.6 ±4.1 36.9 ±8.5 13.2 ±4.0 467 ±75 112 ±18 87± 12 67 ±9 2.49 84.3 <37 <22 Sy2 299 <9 <7 <7 <7 NGC 1365 46.5 ±8.2 90.3 ±3.5 23.2 ±0.8 4.1 ±0.4 6.0 ±0.9 68± 13 Syl.8 <3.3 <1.8 <1.5 <1.3 <0.9 <0.8 <0.8 <1.0 <0.8 1.14 NGC 2110 42.1 ±9.7 40.4 ±1.3 44.1 ±4.8 42.1 ±0.3 53.7 ±6.1 23.4 ±0.2 39.6 ±4.4 4.8 ±0.7 4.4 ±0.3 2.4 ±0.3 3.3 ±0.4 1.2 ±0.2 1.5 ±0.3 <0.3 <0.3 <4.2 <1.4 <0.5 0.85 36.0 Sy2 6.2 b ES0428-G14 44.6 ±0.7 40.3 ±1.1 26.1 ±2.9 26.4 ±7.2 35.2 ±2.6 38.6 ±1.7 37.1 ±0.4 36.3 ±2.9 39.6 ±3.3 0.7 ±0.1 7.9 ±0.1 0.5 ±0.1 3.7 ±0.1 3.1 ±0.2 1.1 ±0.1 1.4 ±0.4 1.0 ±0.1 6.6 ±1 <0.45 <0.2 <0.8 49.3 33.7 0.29 Sy2 9.4 3.1 resembles thatofNGC5128(Paper I),havinganalmostpower- by matchingthefluxofTGbandCOlinesinoff-nuclear(0.7- law likecontinuumshape.The most prominentfeaturesinthe torus. Thisextensioncanalsobe seenintheLM-bands(Marco to 15pcinradius,interpretedastheequatorialplaneofaninclined idenced bythenon-detectionofbroadBra4.05pm(Lutzetal. high extinctionderivedtowardstheBLR(A>50mag),asev- NGC 1068isanearby{z=0.00379;distance15.1Mpc) 3.1 NGC1068 for NGC1068,1365or3783becausethesegalaxieshaveveryweak The nuclear-subtractedspectraareincludedheretobettershowthe nuclear apertureandsubtractingtheresultfromspectra. in Figs6,7and8.Thenuclear-subtractedspectrahavebeenobtained lines inFig.5,andthespectraatdifferentdistancesfromnucleus lines isshowninFigs3and4,velocityfieldsofthemainemission et al.(1998)found/GbandextendedemissionalongPA=102°,up 2000). NGC1068alsoharboursastar-formingringwithdiameter CO lines(COindex~0). weak nuclearemissionlines.Thesubtractedspectraarenotshown & Alloin2000).NGC1068hasan [Om]cone,whichextendsto ~7.5 arcsecatPA=35°(Evanset al.1991). ~15 arcsec(~1.1kpc;e.g.Davies,Sugai&Ward1998).Rouan (R)SA(rs)b galaxy.IthasanextensivelystudiedSy2nucleuswith 1.6 arcsecradiusfromthenucleus)spectrato1.4-arcsecdiameter v The H-andTGbandnuclearspectrum ofNGC1068(Fig.2) NGC 2992 23.7 ±0.5 28.2 ±1.4 33.0 ±2.6 33.6 ±0.4 33.8 ±4.6 32.2 ±1.8 36.8 ±0.5 31.6 ±3.4 11.8 ±0.3 6.5 ±0.1 3.6 ±0.2 8.4 ±0.7 1.5 ±0.2 1.2 ±0.2 1.9 ±0.1 110 ±30 1.2 ±0.2 16 ±5 <0.3 <1.5 41.0 0.95 30.0 Sy2 7.8 6.5 c a NGC 3081 48.2 ±3.9 29.3 ±1.8 29.7 ±5.1 25.5 ±2.7 57.3 ±8.4 33.8 ±1.2 33.1 ±4.8 37.4 ±2.2 35.1 ±2.1 19.9 ±4.7 0.4 ±0.1 0.5 ±0.1 0.9 ±0.1 0.5 ±0.1 7.6 ±0.8 0.7 ±0.2 1.0 ±0.1 1.6 ±0.1 1.4 ±0.1 1.2 ±0.2 <0.3 <0.2 43.1 0.28 36.1 Sy2 3.2 8.1 e 2003RAS,MNRAS 343,192-208 NGC 3783 25.5 ±1.2 23.9 ±0.6 37.8 ±9.6 33.5 ±3.4 38.3 ±7.7 15.3 ±3.1 255 ±33 7.9 ±1.5 2.6 ±0.3 1.1 ±0.3 44± 10 <0.4 <1.6 <0.4 <1.1 <0.8 <0.4 42.0 37.4 1.25 Syl 7.7 2.2 d NGC 7582 47.8 ±9.8 45.4 ±3.9 21.6 ±5.4 34.9 ±1.2 35.6 ±8.0 30.2 ±2.0 2.0 ±0.4 7.1 ±0.4 3.8 ±0.5 <1.9 <1.5 <1.1 <0.8 <0.7 <0.7 <0.8 1.51 Sy2 9.8 58 e 2 0 0 3MNRAS.343. .192R 172 3 perpendicular toit.[Fe11]andBryareextended~4arcsecfromthe Nucleus 106810971365138615662110E428299230813227378349455128 7582 Extent Bry±[pc] Extent Bry||[pc] Extent [Fe11]J_[pc] Extent [Fe11]||[pc] Extent H2-L[pc] Extent H2II[pc] Extent Bry±[arcsec] Extent Bry||[arcsec] Extent [Fe11]J_[arcsec] Extent [Fe11]||[arcsec] Extent H2-L[arcsec] Extent H2II[arcsec] FWHM [Fe11]±[pc] FWHM [Fe11]||[pc] FWHM HJ-[pc] FWHM HII[pc] M(H) ±[M] M(H) II[Mq] N(H) [10cm“] M(H) [Mq] Broad Bry Paper Nucleus extents aregivenoverthewholegalaxyforNGC4945and7582.Star★indicatesthatcentralpeakissignificantlyoff-nuclear. to it(_L).Thenuclearextentgiveninparsecsistheplaneofgalaxyandothervaluesaresky.integratedmassesspatial the ring,andBryisstrongest emissionlineinthering.How- in thestar-formingring~15arcsec(~1.1kpc)fromnucleus. nucleus. Bry,[Fe11],HandHe12.058jamarefurthermoredetected faint. fulness islimitedbytelluricresiduals.NuclearHemission nuclear spectraarethecoronallines[Sivi]1.964jam,[Cavm] He i<0.3 Table 3.ThemassandthecolumndensityofexcitedH2innucleus(1.4-arcsecaperture),nuclearspatialsizecorrectedforseeing(FWHM; et al.2000)orNGC1365(seebelow). ever, generallytheequivalentwidths oftheemissionlinesinring detected inthenucleusare[Fe11]1.644jam,H1-0S(l)2.122jam 2.321 jamand[Sivu]2.483jam.Theotheremissionlines 2- 1S(l)<0.2 Table 4.DereddenedemissionlineratiosrelativetoBry.ThegalaxiesfromPaperIareincludedfacilitatecomparison.ForNGC1386a0.6arcsecslit was used. Section 2)andtheintegratedH2masswithinstar-formingregionsnuclearspatialextentoflines,bothparalleltocone(||)perpendicular © 2003RAS,MNRAS 343,192-208 are smallerthane.g.intheringsof NGC1097(PaperI;Kotilainen and Bry2.166jam.Paar1.876pmisalsoprominent,butitsuse- (300 pc)fromthenucleusparalleltoconeandup~4arcsec 7\ib [10K] [Fen] 4.0>2.2 [Fe ii]isthestrongestemissionline inbetweenthenucleusand [Sivi] 1.964jamisthestrongest emissionlineinthenucleus, [Si vu]7.96 [Cavm] 1.46 [Si vi] 1- 0S(0)<0.3>1.4 1-0 S(l)0.42>4.4 1-0 S(2)<0.3>4.3 2 2 20 2 2 2 2 2 2 1-0 S(l)isthemostextendedlineanddetectedupto5-7arcsec © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem 13.8 Sy2 SylSyl.8Syl.5 2100 2200 <5.3 1800 1068 100* 450 420 450 Sy2 270 320 180 130 4.1 2.3 5.4 5.4 5.4 3.2 no 80 TT <0.12 9.58<0.3 <0.05 2.09<0.06 <0.04 <0.2 <0.04 <0.2 <0.04 1.140.28 <0.04 0.810.05 0.41 <0.2<0.04 0.36 6.840.48 <2.6 1097 1365 Syl Syl.8 340 108 0.9 3.0 1.5 99 60 90 25 80 1 11 6.03 <2.1 <60 430 290 590 yes 4.0 3.0 90 <2.5 1386 <20 <20 <20 410 Sy2 yes 150 150 190 4.2 0.8 0.8 0.8 0.8 3.7 1.0 50 39 30 80 80 17 1 <0.07 0.280.39 <0.8 1.7<2.0 <0.1 <0.2<0.06 <2.7 1566 0.24 <0.20.05 0.30 0.180.06 0.93 0.840.28 0.56 0.230.09 8.34 2.550.93 <30 <30 Syl 280 210 110 yes 100 0.5 0.5 0.5 2.9 2.0 1.1 1.9 42 50 65 90 50 50 82 1 2110 660 730 220 230 220 250 Sy2 300 320 380 100 190 yes 4.1 4.5 4.3 3.3 1.9 1.5 2.66 0.39 11 result ofUVheatingfromOBstars (Puxley,Hawarden&Mountain ratio =0.4isinagreementwiththe starformationoriginforHasa formation modelspredict(e.g.Colina 1993).The1-0SS(l)/Bry inner fewarcsec(Fig.9).SimilarstructureisalsovisibleintheBry material inthejet.Inaddition,paralleltocone[Fe11]hastwo Thus itseemsverylikelythat[Fen]isexcitedbytheoutflowing kinematics ofthe[Fe11]dependsonlyonpositionalongslit. than thatofH.Atlargerradii,[Fe11]seemstofollowmore parallel totheconeismuchsteeperwithininner3arcsec(230pc) velocity componentsandthusthelineprofilechangeswithin closely. Furthermore,withinthesteeppartofvelocitycurve, et al.(2001),basedonHemission.Thevelocitycurveof[Fe11] and coronallines. Schinnerer etal.(2001)basedonCOmillimetrelinesandbyAlloin 1990). Whethertheheatingmechanism isthermalorfluorescence 2 2 2 The nuclear[Fen]/Bryratio=4 (Table3)ishigherthanstar The kinematicsofNGC1068hasbeendiscussedindetailby NIR spectroscopyofnearbySeyferts-II195 E428 <2.6 160* 140^ Sy2 270 530 200 250 300 340 130 150 160 100 180 4.9 2.3 2.8 3.5 1.0 1.9 1.5 no 11 2992 1300 1200 480 470 Sy2 450 250 560 500 900 350 yes 140 120 2.3 6.2 6.7 2.6 8.8 1.9 1.0 1.0 80 11 <0.2 0.04<0.02 0.64 1.470.22 7.33 0.240.46 0.21 0.15<0.02 0.37 <0.020.35 0.91 0.24<0.02 8.73 0.360.42 1.66 <0.010.08 1.60 0.540.21 3081 <2.3 200 240 210 Sy2 250 160 160 110 120 120 0.6 0.6 0.6 1.9 1.0 1.5 1.8 no 90 80 11 Syl.5 3227 600 280 230 230 350 310 860 160 yes 150 2.0 7.5 6.0 2.3 2.0 1.6 1.3 40 50 58 22 84 1 <100 3783 <4.8 270 290 290 Syl 220 yes 130 130 130 130 130 130 0.6 0.6 0.6 0.6 0.6 3.2 1.0 11 <0.2 <0.30.45 <0.1 <0.2<0.03 0.35 <0.2<0.03 0.53 0.34<0.02 0.35 <0.2<0.03 3.10 2.030.07 3.77 14.60.53 1.49 <0.20.11 0.37 4945 1200 1600 420 Sy2 250 270 230 57* 150 4.8 7.8 7.2 2.2 3.1 no 50 50 28 55 36 70 80 17 1 5128 <1.8 <10 <10 Sy2 720 240 0.6 1.1 1.2 1.2 42 44 no 50 30 35 30 30 32 30 30 16 10 1 7582 480 480 480 Sy2 720 580 320 220 340 390 310 yes 160 2.9 6.7 2.3 7.8 3.2 3.6 1.9 1.9 11 2 0 0 3MNRAS.343. .192R 19-2 hydrogen is1.3x10cm(corresponding toM=1800Mq), integrated withinthestar-forming ringastracedbyBry,andthe molecular hydrogenbothinthe nuclear 1.4-arcsecapertureand in thenucleus. is notclear,becauseno2-1S(l)or1-0S(0)emissionwasdetected All imagesareintheZA-bandexceptasmarked.Northisupandeastto left.Slitpositionsareindicatedintheimages,markedwithCforparallelto Figure 1.Thenear-infraredimagesofNGC1068(topleft;//-bandfromPeletier etal.1999),NGC1365(topcentre),2110right),ESO428-G14 cone, onthesidewhereconeisstronger,andPperpendiculartocone. (middle left),NGC2992centre),3081right),3783 (bottomleft;K-bmdfromMulchaeyetal.1997)andNGC7582right). spatial extentofdifferentlines,are giveninTable3.Inthenuclear 1.4-arcsec aperture,thecolumndensity oftheexcitedmolecular 196 J.Reunanen,K.KotilainenandM.A.Prieto H2 The derivedparameters,includingthedensityandmassof © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem 10 0 10 ARA ["] towards north(~2arcsec)than south,inagreementwiththe lines ([Sivi]1.964jam,[Cavm]2.321 pmand[Sivu]2.483pm) the continuum. cannot bemeasuredreliablyastheemissionisweakwithrespectto are resolvedparalleltothecone (Fig. 9),andaremoreextended assuming T=2000K.TheFWHMsizeofthenuclearHemission 1068 (e.g.Oliva&Moorwood1990). Allthedetectedcoronal 2 Several IRcoronallineshavepreviously beendetectedinNGC e 2003RAS,MNRAS 343,192-208 2 0 0 3MNRAS.343. .192R panels. ThemainabsorptionlineshavebeenmarkedinthepanelofNGC2110.Atmosphericfeaturesarewith©. in Fig.2,theextentofmain emission linesinFig.3andthe high-excitation outflowconeofNGC1365(PA=130°;e.g.Kristen is undergoingintensestarburstactivityinitsbarconcentratedinto NGC 1365isanearby(z=0.00546;distance21.7Mpc)SB(s)b 3.2 NGC1365 the two[Fen]velocitycomponents.Extendedcoronallineemis- The velocitycurvesofthecoronallinesresembleweaker NICMOS imageof[Sivi]emissionbyThompsonetal.(2001). NGC 2992,3081,3783and7582.Allthedetectedemissionlineshavebeenlabelledinfirstpanel,markedwitharrowssubsequent Figure 2.ThenuclearH-andÆf-bandspectraina1,4-arcsecaperturefor,fromtoptobottom,NGC1068,1365,2110,ESO428-G14, et al.1997)isparalleltotheradiojet (Sandqvist,Jörsäter&Lindblad galaxy intheFornaxclusterwithaSeyfert1.8nucleus.NGC1365 winds. lar mediumthatareproducedeitherbyajetorAGN-generated © 2003RAS,MNRAS 343,192-208 Kristen etal.1997;Stevens,Forbes&Norris1999).Thehollow a ring-likestructurewithdiameterof~15arcsec(1.6kpc)(e.g. spectra atdifferentdistancesfrom thenucleusinFig.6.Themost sion caninprincipleonlybeexcitedbyshockstheinterstel- 1995). The H-andÆf-bandnuclearspectra ofNGC1365areshown © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem -1 -1 Brackett lines,whicharealsobroad (~1170kms). Bry emissionisblueshiftedby~220 kmswithrespecttothe in thering(Fig.5). Bry, [Fe11]andHeiinthestar-formingring,suggestingacommon the slitinthatdirection.Thereisafaircorrelationbetween1-0S(1), lel toit,astherearenostrongstar-formingregionscoincidentwith narrow componentisseen(Fig.10). is broad,withaFWHMof~1190kms\andnoevidenceforthe Brackett serieslinesandweak[Fe11]1.64pm,aredetected.Bry This maybepartlyduetothestrongnon-stellarcontinuumwhich in oursample,NGC1365doesnotexhibitnuclearH2emission. intriguing featureinthespectraisthatunlikeallothergalaxies where otheremissionlines(e.g.H2andHei)becomevisible. cays smoothlytowardsthestar-formingregions(~6arcsec;600pc), dominates theÆf-bandemission.Infact,onlyHe12.058p.m,several overall velocitycurve.Thisblueshift isalsoobservedinthe//-band origin. Thisisfurthersupportedbythefairlysimilarvelocitycurves [Fe ii]isdetectedperpendiculartotheionizationcone,butnotparal- The velocityfieldofNGC1365is showninFig.5.Thenuclear Bry 2.166pmistheonlyextendednuclearemissionline.Itde- MR spectroscopyofnearbySeyferts-II197 2 0 0 3MNRAS.343. .192R 162 perpendicular totheconeand~90 Mqparalleltoit. been binnedtogethertolowernoise. for 1-0S(l)emissioninthenuclear 1.4-arcsecapertureis8x Figure 3.TheobservedlineemissioninNGC1068(upperleft),1365 (upperright),NGC2110(middleleft),ESO428-G142992 2.1-p.m continuumemissionisindicatedparalleltothecone(short-dashedline) andperpendiculartoit(long-dashedline).Inmostcasesthreecolumnshave dotted lines.Extinctionisplottedinthelowermostpanelofeachsub-figure. Negativedirectionalongtheslithasbeenmarked.Inuppermostpanel, (lower left)andNGC3081right).Opensymbolsindicateparallelto theconeandfilledsymbolsperpendiculartocone.ThePSFisindicatedby of 60Mq.Theintegratedmass theexcitedhydrogenis290Mq 10 ergcms\givinganupper limitinan1.4-arcsecaperture 198 J.Reunanen,K.KotilainenandM.A.Prieto No H2linesaredetectedinthe nucleus. The3crupperlimit © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem -20 -1001020 -10 01020 Position ["] Position ["] lines, Heiand[Fe11],whichtrace starformation,andalsoin1- 0 S(l).Theequivalentwidthof Bry reachesupto70A,much emission regions,thetwoinnermost ofwhichareassociatedwiththe starburst ring.Theseregionsarealso visibleinthe//-bandBrackett Perpendicular totheionizationcone, therearethreeseparateBry -20 -1001020 Position ["] Position ["] e 2003RAS,MNRAS 343,192-208 2 0 0 3MNRAS.343. .192R 1 _1 1 -1 pendicular toitwithnoseparate emissionregions.Surprisingly, but Storchi-Bergmannetal.(1999)didnotdetectthis.Wefoundthe broad componenttotherecombinationlineshasbeenunderdebate respectively) isidenticaltothatbasedonthecontinuumcolour(A NGC 2110isanearby(z=0.00779;distance31.0Mpc)SABO“ 3.3 NGC2110 400 K). the Br10-4/Bryand11-4/Bryratios(A=0.670.69, in thespatiallineemissionprofile.Theextinctionderivedfrom larger thane.g.intheringofNGC1097(Kotilainenetal.2000; in thenucleusandismoreextended paralleltothecone. Bry isnotextended,whichexcludes starformationastheori- from thenucleusparalleltoconeand1.5arcsec(~300pc)per- FWHM ofBrytobe~1550kms,infairagreementwithVeilleux Bry 2.166jam.isratherweak,buthasafaintbroadcomponent in thenucleus,whereotherdetectedlinesarevariousHand the stellarcontinuum.[Feit]1.644jamisbyfarstrongestline ferent fromthemorepowerfulSy2ssuchasNGC1068(thispaper) NGC 2110(Malagutietal.1999)ishighlyabsorbedandindicates gin oftheextended[Fen]emission. Thetotal(nuclear)extentof et al.(1200kms). the NIRbye.g.Storchi-Bergmannetal.(1999).Thepresenceofa extended H1-0S(l)emission,probablyexcitedbycentralX-rays. galaxy withaSy2nucleus.HST[Om]imagingshowsnarrow,1- excited, asthe2-1S(l)/l-0S(l)ratiois0.16±0.05(r=2600 field asevidencedbytheBrackettlines,Happearstobethermally arcsec longjet-likefeature(cone)atPA=340°,andaweaker are noseparateBryknots,buttheringisobservedasaplateau © 2003RAS,MNRAS 343,192-208 as Veilleuxetal.(1997)foundsomeevidenceinPaß1.282jam, and NGC5128(PaperI),appearingtohavemorecontributionfrom an obscuredSylnucleus.Storchi-Bergmannetal.(1999)found at PA=160°(Mulchaeyetal.1994).ThehardX-rayemissionof = 0.68).NotwithstandingtheexistenceofastrongUVradiation ~15 A),implyingrecentstarformation.Paralleltotheconethere ~2 arcsec(300pc)perpendicular to it.[Fen]isspatiallyresolved (FWFTM ~2000kms;Fig.10).Nocoronallinesaredetected. [Fe it]emissionis~4arcsec(0.6 kpc)paralleltothecone,and 1-0 S(l)canonlybetracedupto4-5arcsec(~700pc)distance K K 2 2 vib 2 NGC 2110hasbeenpreviouslyobservedspectroscopicallyin The nuclear//-andX-bandspectrumofNGC2110(Fig.6)isdif- 1-0 S(l)isthemostextendedline,followedby[Fen],buteven © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem Figure 4.TheobservedlineemissioninNGC3783(left)and7582(right).SymbolsareasFig.3. + 5-3 tions (e.g.Knopetal.2001).FurtheroutthevelocitycurvesofH perpendicular toit.Also,bothBry and[Fen]aremoreextended resolved. 1-0S(l)isthemostextended line,extendingupto~7arc- lines, [Sivi]1.964pmandvu] 2.483pm,werealsodetected. Bry 2.166pm,variousHlinesand Hei2.058\im.Twocoronal two-sided jet(Falckeetal.1996). ESO 428-G14isanearby(z=0.00544;distance21.6Mpc) 3.4 ESO428-G14 is largerparalleltotheconethanperpendicularit(320versus to it(220versus190Mq)andtheFWHMofnuclearHemission total integratedMislargerparalleltotheconethanperpendicular likely asthevelocityfieldsof[Fen]andHarequitedifferent. the gasandintensityofradiation,butthisdoesnotseem produced inX-rayexcitedgasdependsstronglyonthedensityof nucleus, HmayalsobeX-rayexcited,asthe1-0S(l)/[Fen]ratio to it,andmoreextendedtowardsnorththansouth.X-rayexcitation NGC 2110ismoreextendedparalleltotheconethanperpendicular images (Weaver2001)andthe[Fen]emission:X-rayemissionin Furthermore, thereisafaircorrelationbetweenChandrasoftX-ray morphologies of[Fen]andBry,it]islikelytobeX-rayexcited. cone areflatterthanthoseparalleltothecone. Olofsson 1986).Ithasabentradiojet(Ulvestad&Wilson1989), 230 pc). energy depositionrateperparticletothegasdensity.Outsideof emission inthenucleus,assumingthatalmostallofgasisdense and [Fen]areinbetteragreement.Thecurvesperpendiculartothe of Hclosetothenucleus,inagreementwithpreviousdetermina- and 7.Thestrongestnuclearlineis[Feit]1.644pm,followedby of ESO428-G14consistsmanythinstrandscloselyrelatedtothe and an[Om]conealongthejet(Wilson&Baldwin1989).TheNLR SA:(1)0 galaxywithaSy2nucleus(Bergvall,Johansson& sec (0.7kpc)paralleltothecone,but onlyupto~2arcsec(210pc) (corresponding toM—250Mq)withinthenuclearaperture.The (n =10cm)andthatthereisahighratioofthelocalX-ray (Maloney, Hollenbach&Helens1996)canalsoexplaintheH sample, and[Fen]/Bry=80.Thus,consideringthedifferent 2 2 2 H2 2 2 2 H2 2 naiTOW 17-2 The dereddened[Feii]/Bryratiois~8,oneofthehighestinour The velocitycurveof[Feit]paralleltotheconeisflatterthanthat The nuclearH,[Fen]andBryemission linesareallspatially The H-andX-bandspectraofESO428-G14areshowninFigs2 Assuming r=2000K,wederiveA4.3x10cm NIR spectroscopyofnearbySeyferts-II199 2 vibH2 2 0 0 3MNRAS.343. .192R -1 row withnodetectablebroadcomponent. parallel tothecone(up~3arcsec; 320pc)thanperpendicu- lar toit(~2arcsec;~200pc).The morphologiesofH,Bryand Figure 5.Theobservedvelocityfieldinunitsofkmsthe1-0S(l)(circles witherrorbars),Bry(squares)and[Fen](triangles)linesforNGC1068 0.5 arcsectothenorth-east(NE) and aseparatepeakisdetected shows thepositionalongslit. (upper left),NGC1365right),2110(middleESO428-G14 (middleright),NGC2992(bottomleft)and7582right).Thex-axis 200 J.Reunanen,K.KotilainenandM.A.Prieto ~1.3 arcsecsouth-west(SW)ofthe continuumnucleus.Bryisnar- [Fe ii]areallsimilarparalleltothecone: thecentralpeakisdisplaced 2 © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem Parallel NGC 299 -5 05 § S Position [arcsec] Position [arcsec] Position [arcsec] * g. @A @. $ ° -1 blueshifted withrespecttoH.Thus itseemsthattheextendedH blueshifted by~70kmsacross thenuclearregion.HandBry clouds. and Bryemissionshareasameorigin, probablyinthestar-forming appear tohavesimilardynamics, but intheNEpeakBryisalso 2 2 2 The velocityfieldofESO428-G14 isshowninFig.5.[Fen] Position [arcsec] e 2003RAS,MNRAS 343,192-208 2 0 0 3MNRAS.343. .192R 17-2 perpendicular toit.TheFWHMsizeofthenuclearHemissionis pendicular toit,[Fe11]islikelybeshock-excitedbythewindsin features at2.0and2.05jj.mareduetoimperfectatmosphericcancellation.Thenuclearsubtractedspectrumwasobtainedasdiscussedinthetext.spectra the fluxinnuclear1.4-arcsecaperture,andspectrawereplacedatuniformintervalstofacilitatecomparisonbetweendifferentregions.Theabsorption Figure 6.The1.5-2.5jj.nispectraof,fromtoptobottom,NGC1068,1365and2110,atdifferentpositionsalongtheslit.K-bmdfluxwasscaledmatch higher thermalbackgroundnoise. The[Sivi]emissionwithinthe the SWthanNE.[Sivu]2.483 jam isalsospatiallyresolvedand the cone.InNE,peakshocksalsoseemtocontributeBry in thenucleusandismoreextendedparalleltoconethanper- mally excitedbyUVradiationfromOBstars.As[Fe11]isblueshifted to theconeup~2arcsecfromnucleus.Perpendicular upper right-handcornerineachpanel. marked withastarhavebeensmoothedthree-pixelboxcarfunction.Thedirectionrespecttotheconehasnextlabelon the Mh —100Mq)withinthenuclearaperture.Theintegratedmass emission. 0 S(l)/Br}/ratioisalsofairlyconstant,0.6-0.9,acrossthenucleus. cone, theratioislower(~1.2)towardsnorth-west(NW).The1- © 2003RAS,MNRAS 343,192-208 of theexcitedhydrogenis200Mqparalleltoconeand160 S(l) ratioisinagreementwiththermalexcitationofH.Assuming similarly extended,thoughitsdetermination suffersfromthemuch solved paralleltothecone(Fig.3), andismoreenhancedtowards similar inbothdirections(~150pc). suggest forstar-formingregions.Theratioisnearlyconstantparallel r =2000K,wederiveA=3.5x10cm(correspondingto 2 2 2 vibH2 No 2-1S(l)isdetected,andtheupperlimittoS(l)/l-0 Based onthevelocityfieldandlineratios,H2ismostlikelyther- The nuclear[FenJ/Bryratio=2.6,whichishigherthanmodels Of thedetectedcoronallines,[Sivi] 1.964jamisspatiallyre- © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem _j ^^^^^^^^^^^^^^^i 1.6 1.822.22.4 Wavelength 15-2- plane ofthegalaxyupto~4kpc(~25arcsec)distanceinSE-NW unusually extensiveconeemergingalmostperpendicularlyfromthe NGC 2993at2.9arcmin(26kpc)distancetowardsSE.Aprominent NGC 2992isanearby(z=0.00771;distance30.6Mpc),almost 3.5 NGC2992 level withflux0.42±0.15x10“ergcms. lying COlines,amarginal[Cavm]2.321-jamlineappearsat2.Sa FWHM~1.6 arcsec(170pc)andanadditional,decayingextended innermost 2arcseciscomposedofaresolvednuclearsourcewith coronal linesandvariousHlines, including2-1S(l)2.248jam. 2.166 jjm.Othernuclearlinesare [Fe 11]1.644jam,He12.058 with aone-sidedextensionalongPA=130°,andatsmallerscales cone. TheradiostructureofNGC2992hasmajoraxisPA=160°, direction (Allenetal.1999),withtheSEconebrighterthanNW dust laneroughlynorth-southalongthemajoraxisofgalaxy edge-on, peculiarSagalaxywithaSy2nucleus,interacting component towardsSW.Furthermore,aftersubtractingtheunder- and 7.Thestrongestemissionline inthenucleusisbroadBry splits thenuclearregionintotwocomponents.NGC2992hasan ‘figure ofeight’shapeatPA=160° (e.g.Ulvestad&Wilson1984). 2 The H-andTGbandspectraofNGC 2992areshowninFigs2 NIR spectroscopyofnearbySeyferts-II201 2 0 0 3MNRAS.343. .192R For symbols,seeFig.6. Figure 7.The1.5-2.5i^mspectraofESO428-G14(top),NGC2992and3081(bottom)perpendiculartotheconeatdifferentpositionsalong slit. 202 J.Reunanen,K.KotilainenandM.A.Prieto Figure 8.The1.5-2.5\imspectraof NGC3783(top)and7582(bottom)atdifferentpositionsalongtheslit. Forsymbols,seeFig.6. © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem _J ^^^^^^L_^^^^I 1.6 1.8 2 2.22.4 1.6 1.822.22.4 Wavelength [¿¿m] Wavelength [/urn] e 2003RAS,MNRAS 343,192-208 2 0 0 3MNRAS.343. .192R -1 become brighterandBryismuch broader (2530kms)thantheir by Gillietal.(2000).Compared to them,theemissionlineshave JHK-bands in1999January,andalso withSOFIanda1-arcsecslit indicated withadottedline.Thetwovelocitycomponentsof[Fen]1.644 Figure 9.Thespatialextent(upperpanel)andvelocityfield(lower NGC 2992hasbeenpreviouslyobserved spectroscopicallyinthe the fitforNGC1365,2110,2992,3783and7582.Thecontinuumhasbeen Figure 10.Decompositionofemissionlinesintonarrow(shortdashedline) and broad(dottedline)componentstheresidual(longdashedof denote paralleltotheconeandfilledsymbolsperpendicularit.PSFis and [Sivu]2.483iumlineemission(squares)inNGC1068.Opensymbols of thecoronal[Sivi]1.964\xm(triangles),[Cavm]2.321(circles) © 2003RAS,MNRAS 343,192-208 subtracted withasecondorderpolynomial. jam areindicatedwithcrosses. © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem 7-2 -1 1 17-2 because BryiskinematicallymorecloselycoupledwithHthan that [Fe11]isexcitedbyshocks.ThenarrowBryemissionmayalso heating. The[Fen]/Bryratiois0.93and=16. from thenucleus,coincidingwithbarorspiralarms(Fig.1). towards theSWHemissionisdetectedassociatedwithbridge Paa. Furthermore,arelativelystrong[A1tx]lineat2.043pmhas nuclear 1.4-arcsecaperture,thegas densityV=1.8x10cm, is 1.6,indicatingthatshocksaretheexcitationmechanismforH H 1-0S-andQ-transitionlines,He12.058pm,narrowBrya The coronal[Cavm]2.321-pmand[A1ix]2.043-pmlines,various by farthestrongestemissionlinesdetectedinnuclearregion. NGC 3081isanearby{z=0.00795;distance31.6Mpc)Sy2 3.6 NGC3081 the linesarespatiallyresolved. FWHM sizeofthenuclearHemissionissmallerparalleltocone The densityoftheexcitedmolecularhydrogenisA^h=8.8x with [Fe11]regions.InadditiontoBry,Heiisalsobroad(2200km Considering that[Fe11]isblueshiftedinthenucleus,itplausible curve ofBryseemstofollowH2morecloselythan[Fe11]. curve of[Feit]isblueshiftedby70kms.However,thevelocity connecting NGC2992to2993.Thisemissionislikelybe corresponding togasmassofonly 110Mq.TheFWHMsizeof 0.13 and0.57,respectively,clearly rulingoutUVfluorescence,and whereas the1-0S(0)/l-0S(l)and 1-0S(2)/l-0S(l)ratiosare width ofthelines(~30-32À).Also[Fe11]isnotspatiallyresolved. 2.122 pm,whichbothextend~2arcsec(310pc;Fig.3).Bry,1-0 weak [Fe11]1.644pmarealsodetected. et al.1996).HezimagingshowsaringofH11regionswiththemajor galaxy withfourrings(e.g.Buta&Purcell1998),alarge-scalebar originate inshocks,asthenarrowBry/1-0S(l)ratiois~0.2,but arc sec(220pc)paralleltoit.BothBryand[Feit]aremoreextended of upto7arcsec(1.1kpc)perpendiculartheconebutonly1 appeared. also. Theupperlimittothenuclear 2-1S(1)/l-0S(l)ratiois0.13, and canbeproducedbystarformation.The1-0S(l)/Bryratio S(l) and[Fe11]areverynarrow,comparabletotheinstrumental and 7.Thecoronallines[Sivi]1.964pm[Sivu]2.484are axis perpendiculartothelarge-scalebar(Storchi-Bergmannetal.). at PA=66°,andanuclearbar=120°(Storchi-Bergmann at the2.5crlevel.ThecoronallinesareweakerthanthoseinNGC appears tobeafairlybroad(80À)[Cavm]2.321-pmlinedetected s“) (Fig.10). separate Bryregionsperpendiculartothecone5arcsec(760pc) shock-excited, as2-1S(l)emissionisnotdetected.Therearealso (~4 arcsec;600pc)paralleltotheconethan1-0S(l).Inaddition, suggesting shockstoberesponsible fortheexcitationofH.In (120 pc)thanperpendiculartoit(250pc). [Fe it],theshockedregionsproducingBryarenotlikelytocoincide [A1 ix]2.043pm)aredetectedinNGC2992.Inaddition,there r =2600K)isinagreementwiththermalexcitationofH. 1068 and3081(thispaper),itisnotpossibletodiscusswhether 10 cm,correspondingtointegratedgasmassof~500Mq.The 2 narrow 2 H2 2 2 2 2 2 vib2 The dereddened2-1S(l)/l-0S(l)ratio0.18(correspondingto The 1-0S(l)/Bryratioisquitelow,0.28,suggestingthermalUV The velocityfieldofNGC2992isshowninFig.5. The mostextendedlineis1-0S(l),whichcanbetracedadistance The [Fen]/Bryratiois0.64,oneofthelowestinsample, The mostextendedlineis[Sivi],followedbyBryand1-0S(l) The H-andTGbandspectraofNGC3081areshowninFigs2 Three coronallines[Sivi]1.964pm,[Sivu]2.483pmand MR spectroscopyofnearbySeyferts-II203 2 0 0 3MNRAS.343. .192R / _ 1 -1 17-2 ring, Bry2.166pmisonlyvisibleaftersmoothingthespectra,and perpendicular toit(160pc).TheintegratedmassofexcitedHis required toconfirmitspresence. pears tobeafaint[A1ix]linedetectedat2.5alevelblended be double-peaked,incontrasttoBry(Fig.10).ThewidthofHei ring (e.g.Mulchaeyetal.1997).NGC3783hasextremelybroad but oneoftheclosestSyls,andthushasbeenextensivelystudied is thebroad(~2630kms^Bry.Otherlinesdetectedare1-0S(l), B aimerandHelineswhichareblueshiftedrelativetothesystemic NGC 3783isan(R’)SB(r)agalaxywithaSylnucleus.Itthemost 3.7 NGC3783 line duetothemuchhigherbackgroundnoisethissuffers. nuclear. Thisextendedemissioncannotbedetectedinthe[Sivu] no emissionlinesfromtheinnerringcanbedetected. the nuclearHemissionislargerparalleltocone(210pc)than NGC 7582isanearby{z=0.00540; distance=20.9Mpc) 3.8 NGC7582 Thus wecannotexcludethecontributionfromfluorescentHemis- 4800 K),whileforfluorescentemissiontheexpectedratiois~0.5. unobscured. lines aredetected(Br10-41.737jam,Br11-41.681pmand faint broadHeilineisdetected(Fig.2).Thisalsoappearsto NGC 3783. nucleus (Fig.4).Thus,nokinematicalanalysiscanbepresentedfor to thecaseofNGC3081,3783isratherdistantandfaint, velocity (Evans1988). distant (z=0.00973;distance38.6Mpc)galaxyinoursample, 200 pc).Perpendiculartotheconeemissionpeakisslightlyoff- clear rings(e.g.NGC1097,1365and4945),thein3081 with thebroadHeiline,buthighersignal-to-noiseratiospectraare and eachlinecanonlybetracedupto~1arcsec(200pc)fromthe of NGC3783(Fig.8).Thestrongestlinewithinthenuclearaperture 6.7 kpc)withstarformationactivitycirclingastrongstellarbar and partiallytheinnerring(~75°;70arcsec,11kpc).Innuclear only thenuclearring(PA~120°;majoraxis~12arcsec,1.9kpc) are notprominentinthespectra.Theeffectiveslitlengthcovers 204 J.Reunanen,K.KotilainenandM.A.Prieto (PA =163°),andthintightlywoundspiralarmsemergingfromthis (e.g. Maranetal.1996).Ithasaninnerring(diameter~35arcsec, (FWHM 2.2arcsec,350pc)thanperpendiculartoit(1.2 80 Mqparalleltotheconeand70perpendicularit. (R)SB(s)ab galaxyintheGrusquartet withaSy2nucleus.Op- significant differencebetweenthedirections.Inaddition,thereap- (corrected fortheinstrumentalresolution)is~0.7arcsecwithno sion isdetected.TheFWHMsizeofthenuclearemissionsource spatially resolvedinthenucleusbutnoadditionalextendedemis- sion. ThedensityoftheexcitedHinnucleusAh—3.2x separated by~1000kms.Inthe//-band,otherBracketttransition (~3700 kms)isbroaderthanthatofBry,andthepeaksare [Ca vin]2.321p.mand[Sivu]2.483pm.vi]areboth [Fe it],HeI,//-bandBrackettlinesandthreecoronallines.Similar 10 cm(correspondingtoM—290Mq). 12-4 1.641pm).TheirratiosagainstBryindicatethattheBLRis 2 2 2 1 2 H2 Three coronallinesaredetectedinNGC3783:[Sivi]1.964pm, The upperlimittothe2-1S(l)/l-0S(l)ratiois~0.3(rb< Non-stellar continuumappearstodominatetheoverallspectrum The coronal[Sivi]lineismoreextendedparalleltothecone In contrastwiththeothergalaxiesinsamplecircumnu- Similar tothecaseofNGC2992,inadditionbroadBry,a vi © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem -1 17-2 -1 below isbasedonthistotalsample. Thestrongestemissionlineis perpendicular toitacrossthegalaxy.ThenuclearHemissionistoo perpendicular tothecone.TheringismoreprominentinBryand perpendicular tothecone(8arcsec,900pc)thanparallelit two-component fit.Twocoronallines([Sivi]and[Sivu])arealso Bry canbedecomposedintobroad(~3000kms)andnarrow nuclear lineisBry,whiletheotherlinesdetectedare1-0S(l) tected bySosa-Britoetal.(2001).Thesharp-edged[Om]outflow is variable,andthebroadhydrogenrecombinationlinehasbeende- the scatteredlightfromnucleus.However,nuclearemission the L-bandnucleusdominates,albeitringremainsvisible nuclear region.IntheNIR,galaxyappearssmoother,andin tical broad-bandimages(e.g.Malkan,Gorjian&Tam1998)show two intermediateSeyferts),[Fen] 1.644pmin21percent(three Bry 2.166pmin43percentofthe galaxies (twoSyls,twoSy2sand We havepresentedNIR1.5-2.5qmlong-slitspectraofeightSeyfert 4 DISCUSSION Bry. the presenceofAGNinNGC7582,asdoesdetectionbroad the excitedhydrogenis320Mqparalleltoconeand480 Assuming r=2000K,thedensityofHis7.8x10cm, than modelspredictforstar-formingregions,butinagreementwith the conevelocitycurvesofvariousemissionlinesarerelatively in agreementwithrelativelyrecentstarformation. larger thantheinstrumentalresolution.Heiisalsostronginring, the cone.Theemissionlinesarenarrow,comparabletoorslightly pc) intheNE,2.5arcsecSWand~2perpendicularto detected. 2.195 pm,whichremainsvisibleaftersubtractingthecontinuum. cone ofNGC7582(PA=250°)wasdetectedbyStorchi-Bergmann does notrevealahiddenBLR(Heisler,Lumnden&Bailer1997), galaxies withanionizationcone.Combinedsimilardataonsix emission region.However,thedetectionofcoronallinessupports weak toaccuratelydeterminetheFWHMsizeofnucleus. corresponding toagasmassof220Mq.Theintegrated with respecttoH.Theratioof[Fen]/narrowBry=3.1islarger flat andsimilartoeachother.[Fen]issystematicallyblueshifted effect oftheringonHemissionisalsonotable,especially additional bluewingandisthereforenotperfectlyfittedbyasimple and otherHlines,[Fen]anunidentifiedemissionfeatureat & Bonatto(1991). and evenhardX-rayemissionisattenuatedbylargecolumndensity a disturbedmorphologywithanopticallyobscurednucleus,red Sy2s), 1-0S(l)2.122pmin14per cent(oneSyl,oneSy2)anda Syls, twointermediateSeyferts and nineSy2s).Thediscussion Seyferts fromPaperI,thetotalsample sizeis14Seyferts(three and itisnotpossibletoreliablymeasurethesizeofcoronal agreement withthermalexcitationofH(r=2900±500K). (420 kms)components(Fig.10).Thebroadcomponenthasan (Warwick etal.1993),indicatingthatanedge-ontorusblockseven (Prieto, Reunanen&Kotilainen2002).Opticalspectropolarimetry star-forming ring(diameter2arcsec)andadustlanecrossingthe shocks orX-rays. (2.5 arcsec,270pc).1-0S(l)emissiondeclinessmoothly,butthe [Fe ii],whicharedetectedparalleltotheconeup4arcsec(430 2 vib2 2 2 2 2vib The H-andZf-bandspectraareshowninFig.8.strongest The coronallines[Sivi]1.964pmandvu]2.483areweak, The ratioof2-1S(l)/l-0S(l)=0.20±0.06inthenucleus The velocityfieldofNGC7582isshowninFig.5.Parallelto 1-0 S(l)isthemostextendedline(Fig.4)andmore e 2003RAS,MNRAS 343,192-208 2 0 0 3MNRAS.343. .192R b) andtheextinctioninnuclearaperture (panelscandd).Theclassifi- polarized emissionbutnotinBry.ThedetectionofbroadBry foreground absorbingmaterialmaybeintheformofstar-forming is likelytobehighenoughcompletelyobscuretheBLR.The torus oraforegrounddustscreenisunknown;thelatterexplanation least luminousinthesample,whilethreehighASy2galaxies have largerextinctionthanSyls(Fig.11).ThetwoSy2swithlow to thelowerextinctionthatnuclearemissionsuffersinNIR mon withTran’ssampleisNGC1068,whereaBLRdetectedin BLR inpolarizedlight(Tran2001).Theonlyothergalaxycom- the sample.Ofthesegalaxies,onlytwowereopticallyclassifiedas The onlygalaxyinthesamplewithnonuclearBry2.166-jamemis- 4.1 Bryemission in NGC1386. line inNGC2110and3227[Sivu]remainsthestrongest line in5/8(62percent)galaxies,while[Fen]remainsthestrongest Figure 11.Thenuclearsurfacedensity ofmolecularhydrogen(panelsand NLR. narrow component.Alternatively,Brymayarisefromthe clear Bryemissionisdetectedin8/14(57percent)galaxies following discussionasSyl,basedontheliterature.Broadnu- cent (threeSy2s).IfabroadBrylineisdetected,itthestrongest coronal line(either[Sivi]1.964jamorvu]2.484jam)in21per detection ofbroadBry(thispaper). cation inpanels(a)and(c)isbasedon literature,andin(b)(d)onthe 75 percent(6/8)ofthegalaxieswhichhavebroadBryalsoa clouds, whichareknownfrequentlytocoexistwiththeAGN(e.g. these galaxies(NGC1386and7582)havenoindicationofahidden Storchi-Bergmann etal.2001).Thisexplanationseemslikely,as A areESO428-G14andNGC3081,bothofwhichamongthe of thehighspatialresolutionandqualitydataused. Syls andtwoasintermediateSeyferts,whiletheremainingfour © 2003RAS,MNRAS 343,192-208 seems moreplausibleastheopticaldepthofmoleculartorus sample. Whethertheobscuringmaterialisrelatedtomolecular (NGC 1068,4945and5128)representthehigh-luminosityendof (Fig. 11).ThehighdetectionrateofbroadBryisalsoaconsequence ~40 percent(4/9)oftheopticallyclassifiedSy2sismainlydue (NGC 1386,2110,2992and7582)wereclassifiedasSy2s.Twoof sion isNGC1097(PaperI),whichwe,however,classifyinthe K k If theclassificationisbasedondetectionofBry,Sy2galaxies 0 123 © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem 17 1819 A [mag] k further outfromthenucleus.Thisextendedemissionisverypatchy, the galaxy.Inmanygalaxiesseparateemissionregionsaredetected the nuclear[Fen]emissionrangesfrom~30pcinNGC5128to 40 pcinNGC3227to~3007582.Thetotalextentof in 57percentofthegalaxies(8/14;oneSyl,twointermediate 4.2 [Feii]emission region thatHeiislocatedin.Theroleofextinctionseemsunlikely, Hei/Bry fluxratio~0.35.Onepossibleexplanationforthenon- broad Hei2.058-pmemissionwasdetected.Inbothofthem,the nuclear apertureandfortheextendedemission, andtheH2/Bryrrwratios Figure 12.Thelogarithmic[Fen]/Brynarrow ratios(panelsaandb)inthe mechanism. However,theBryfluxesusedinthisratioshould line ratios,butthe[Fen]/Bryratioissensitivetoexcitation include shocksandX-rayexcitation. by LyphotonsproducetheNIR[Fen]spectrum.Othersuggestions bination ofcollisionalexcitationanddecaysfromlevelspopulated ies inthewavelengthrange0.8-2.4pm,andsuggestedthatacom- Rodriguez-Ardila etal.(2002)studiedfournarrow-lineSylgalax- models ofstar-formingregions(e.g.Colina1993). weakness ofHeiwithrespecttoBry,ortheatmosphericallypoor detection ofbroadHeiinmostthesamplegalaxiesisintrinsic width ofHeiiscomparabletothatBry,andthebroaddereddened contribute muchtothe[Fen]flux.Theii]/Bryratios exclude thebroadcomponent,becauseBLRisunlikelyto extended emissionarealsogenerallyinagreementwiththeoretical which botharetracersofstarformation.Theoriginthisextended and inmostgalaxiescloselyfollowsthestar-formingcomplexesas Seyferts, andfiveSy2s).Inspatiallyresolvedcases,theFWHM Spatially resolvednuclear[Fen]1.644-pmemissionisdetected aS And—LIABry• (panels candd).TheshadingisasinFig. 11. and supernovae.Thelow[Fen]/Bryratios0.5-2(Fig.12)ofthis size ofthenuclearemissioncorrectedforseeingrangesfrom [Fe it]emissionisthusverylikelyduetostar-formingprocesses [Fe ii]isfairlycorrelatedwithBry2.166pmandHei2.058pm, 1.2 kpcinNGC2110,withaverageextent~300pctheplaneof na0 narrow Additionally, intwogalaxies(SylNGC3783andSy22992) The weaker//-band[Fen]linesaretoofainttoyieldreliable The originofthenuclear[Fen]ishoweverunclear.Recently, NIR spectroscopyofnearbySeyferts-II205 lg(H/Br) 27 2 0 0 3MNRAS.343. .192R 17_29-2 -1 -1 perpendicular toitforthewholesample (uppertwopanels)andseparately range from<20pcinNGC1386to—3002110,andare relation disappears.Thissuggeststhattheopticalclassificationinto but thescatterislarge.Also,whenclassificationintoSeyferttypes the conethanparalleltoitin6/8(75percent)galaxies(Fig.13), FWHM extentofnuclearHemissionislargerperpendicularto in allthegalaxiesexceptparalleltoconeNGC1386.The Bry galaxies. the scatterofN^islargerinnarrowBrygalaxiesthanbroad is basedonthedetection/non-detectionofbroadBryemission,this The surfacedensitiestendtobelargerinSy2sthanSy1s(Fig.11), from 1.5x10cminNGC1097to1.3inNGC1068. NGC 1365.ThesurfacedensitiesoftheexcitedH(Table3)range Nuclear Hemissionwasdetectedinallgalaxiesexcept 4.3 Hemission inantly excitedbyshocksproducedwinds/jetsintheionization high, —3OnlyinNGC3081thisratioislow,0.6,obtainablewith In galaxieswithoutbroadBrythe[Fen]/Bryratioisalsofairly tion betweenX-rayand[Feit]emissionfavoursexcitation. than theinstrumentalprofile,reachinguptoFWHM—700kms, much higherthanstarformationmodelspredict,butcanbepro- for bothSytypes(lowerpanels).Theclassification isbasedonthedetection Figure 13.TheFWHMsizeoftheH emission bothparalleltotheconeand cone. duced byX-rayorshockexcitation.Often,the[Fen]isbroader of broadBry.Differentphysicalscales (pcarcsec)areindicatedwith while infourgalaxiesthenuclearHemissionistooweaktoobtain accurate FWHMsizesandintwogalaxiestheHemissioncentreis Seyfert typesislargelyrelatedtotheextinctioneffects.However, of shockexcitation.InNGC1386and2110thespatialcorrela- and blueshiftedwithrespectofBry.Boththesearesignatures are highinallthegalaxieswithabroadcomponent,rangingfrom 206 J.Reunanen,K.KotilainenandM.A.Prieto shading. significantly off-nuclear.TheFWHMsizescorrectedfortheseeing shocks, photoionizationorstarformation.Thusthe[Fen]ispredom- -3 inNGC3783to-802110(Fig.12).Theseratiosare 2 2 2 2 2 2 2 2 The nuclear1-0S(l)2.122-pmemissionisspatiallyresolved © Royal Astronomical Society •Provided bytheNASA Astrophysics DataSystem 1 1.522.53 Ig FWHM[pc] related withtwomaincomponents:thefirstassociatedstar- plane ofthegalaxy,from—100pcinNGC5128to>1kpc not observedin[Fen]orBry. forming regionsandthesecondasmoothlydecayingdisc,whichis forming regions.Inconclusion,extendedHemissionappearstobe the 1-0S(l)velocitycurves,whicharegenerallywell-ordered.A forms adiscsurroundingthenucleus.Thisisfurthersupportedby in NGC1386and3783.Theoverall1-0S(l)emissionismore from thetorusitself. the molecularmaterial(disc?)surroundingtorusthandirectly Pier &Krolik1993).Thustheemissionismorelikelytoarisefrom larger thanthepredictedsizesformoleculartorus(1-100pc; NE. Furthermore,inNGC3783the coronallinesarespatiallyre- in NGC3081bothsidesaresimilarly extendedandinESO428- In NGC1068theextendedemission isonlyvisibleononeside, in allthreegalaxieswithspatialinformation,i.e.NGC1068,3081 needed toconfirmtheirpresence.Coronallinesaredetectedin2/5 to ourknowledge,onlyinCircinus(Maiolinoetal.1998),andNGC in sevengalaxies.Overall,atleastonecoronallinewasdetected Four coronallinesweredetected:[Sivi]1.964pm,[Alix]2.043 4.4 Coronallineemission UV fluorescenceindensecloudsremainsunclear,althoughshocks Whether thethermalexcitationisproducedbyshocks,X-raysor in theringofNGC1365,whereequivalentwidthBry tent withthermalexcitationofthemolecularH.Thisisvalideven upper limitsareinconsistentwithsignificantfluorescentexcitation, different fromthatofH.Insevengalaxies,separateoff-nuclear1-0 with increasingradius,itseemsprobablethatthemoleculargas 2992 and4945.Asthisextendednuclearemissiondeclinessmoothly 0 S(l)emissioncanbedetecteduptoarangeofphysicalscalesinthe while theoppositeistrueinsevengalaxies.Theextendednuclear1- extended perpendiculartotheconethanparallelitinfivegalaxies, the ionizationcone.Wehavean ongoingfollow-upprogramto G14 theemissionismoreextended towardstheSWthan galaxies (62percent)whereBryisbroad. galaxies (40percent),whereBry2.166pmisnarrow,andin5/8 2992 and3081(thispaper).Inaddition,inafewgalaxieseither[Ca with IRcoronallinedetection,andconfirmstheresultsofPrieto 57 percentofthegalaxies(8/14;oneSyl,intermediateSeyfert was detectedineight,[A1ix]two,[Cavm]fourand[Sivu] 2.166-pm lineis—70A,indicativeofastrongUVradiationfield. 2-1 S(l)emissionisdetectedonlyintwogalaxies,andalsoconsis- are alsodetectedinBryand[Fen]probablyoriginatefromstar- S(l) emissionknotsarealsodetected.InmostcasestheseHpatches as themorphologiesofbothBryand[Fen]emissionaregenerally and ESO428-G14,implyingananisotropicnuclearradiationfield. vm] or[A1ix]wasdetectedat—2.5a-level,andreobservationsare & Viegas(2000),thatcoronallinesarecommonandbrightinthe and sixSy2s).ThissubstantiallyincreasesthenumberofSeyferts are themostlikelyexplanation. and inagreementwiththermalexcitation.Furthermore,off-nuclear starburst originforthissmoothextendedemissionseemsexcluded solved, butthesizeissimilarboth parallelandperpendicularto spectra ofSeyfertgalaxies.The[A1ix]linehasbeendetectedsofar, [Ca vin]2.321pmand[Sivu]2.4833pm.Oftheselines,[Sivi] pm emissionwasdetectedandthe2-1S(l)/l-0S(l)ratioortheir 2 2 2 2 Extended nuclearemissionisdetectedinallthegalaxiesexcept Interestingly, thecoronallinesareextendedparalleltocone Only in36percent(5/14)ofthegalaxies,nuclear2-1S(l)2.244 e 2003RAS,MNRAS 343,192-208 2 0 0 3MNRAS.343. .192R 179-2 -1 _1 -1 related withacircumnuclearring,andnuclearcomponent.Ex- proposed bytheauthor.Weinsteadbelievethathighspatialresolu- preparation). nents aredetected:asmoothlydecayingdiscand(insomecases) range from10tocm.Ingeneral,twoextendedcompo- less oftheSeyferttype.ThenuclearsurfacedensitiesexcitedH2 the future. tion NIRspectroscopywillrevealmorehiddenbroadlineobjectsin non-detection oftheBLRinpolarizedemission(Tran2001)isin- fying AGNintheIR.TheexistenceofgenuineSy2sonbasis Bry, H2.12qm,[Fen]1.64qmandcoronallines[Sivi]1.96yim tial extensionandkinematicsof[Fen],Fh,Brycoronallines, NIR 1.5-2.5\imlong-slitspectroscopywitharesolutionof line tostudythecoronalregionindetail(Prietoetah, lar mediumisthemostplausible originfortheextendedcoronal the nuclearionizingradiationunlessitisstronglycollimated.Thus This clearlysupportsthepresenceofastronganisotropicradiation lines areextendedparalleltotheconebutnotperpendicularit. ies regardlessofthetypenucleus.Inthreegalaxiescoronal lines arecommonandbrightfeaturesinthespectraofSeyfertgalax- mechanism inSeyfertgalaxies. Nuclear [Fen]isinmanygalaxiesblueshiftedandthewidthof tended [Feit]andBryemissionisdetectedinhalfofthesample. Bry and[Fen].Generallytwocomponentsaredistinguished:one is indeeddetectedin6/8(75percent)galaxies. nuclear emissionperpendiculartotheconethanparallelit.This ing theradiationfromAGNshouldbeevidentasmoreextended gether withsimilardataofadditionalsixSeyfertgalaxies(PaperI), 5 CONCLUSIONS emission. Thewidthofthecoronal lines(upto1200kms)also field inthesegalaxies.However,duetothehighionizationpotential cases, confirmingtheresultsofPrieto&Viegas(2000)thatcoronal circumnuclear star-formingring.Whiletheringisprominentalsoin consistent withourdetectionofbroadBryintwothecandidates galaxies, stressingtheimportanceofextinctioneffectsandclassi- diameter aperture.Themainresultsareasfollows. and [Sivn]2.48pm. and thesizesofcentralemittingregionsdownto<0.5arcsec and perpendiculartoit.Thisdatasetallowsusstudythespa- olution ^1arcsecisproducedbothparalleltotheionizationcone a homogenoussampleofhigh-qualityNIRspectrawithspatialres- obtain diffractionlimitedimagesofnearbySeyfertsinthe[Sivn] © 2003RAS,MNRAS 343,192-208 of thecoronallines,extendedemissioncannotbeproducedby of theobjectsand[Cavm][A1ix]arealsodetectedinsome (10-100 pc),andthecentralmolecularcontentwithina1.4-arcsec ~300 kmsofeightnearbySeyfertgalaxiesispresented.To- supports thisscenario. shock excitationcausedbye.g.the jetinteractingwiththeinterstel- [Fe it]andBry,thediscisonlydetectedinH. 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