Star formation driven galactic winds in UGC 10043

1.8 MB·

by  C. López-Cobá

MNRAS000,1–14(2016) Preprint9January2017 CompiledusingMNRASLATEXstylefilev3.0
Star formation driven galactic winds in UGC 10043
C. López-Cobá1, S. F. Sánchez1, A. V. Moiseev2, D. V. Oparin2, T. Bitsakis3,
I. Cruz-González1, C. Morisset1, L. Galbany4,5, J. Bland-Hawthorn6,
M. M. Roth7, R.-J. Dettmar8, D. J. Bomans8, Rosa M. González Delgado9, M. Cano-Díaz10,
R. A. Marino11, C. Kehrig12, A. Monreal Ibero13 and V. Abril-Melgarejo14
1InstitutodeAstronomía,UniversidadNacionalAutónomadeMéxico,A.P.70-264,C.P.04510,México,D.F.,Mexico
2SpecialAstrophysicalObservatory,RussianAcademyofSciences,NizhniiArkhyz369167,Russia
7
3CONACYTResearchFellow-InstitutodeRadioastronomíayAstrofísica,UniversidadNacionalAutónomadeMéxico,C.P.58190,Morelia,Mexico
1
4PittsburghParticlePhysics,Astrophysics,andCosmologyCenter(PITTPACC),USA.
0
5PhysicsandAstronomyDepartment,UniversityofPittsburgh,Pittsburgh,PA15260,USA.
2
6SydneyInstituteforAstronomy,SchoolofPhysics,UniversityofSydney,NSW2006,Australia

n 7Leibniz-InstitutfürAstrophysikPotsdam(AIP),AnderSternwarte16,D-14482Potsdam,Germany
a 8AstronomischesInstitut,Ruhr-UniversitätBochum,Universitätsstr.150,D-44801Bochum,Germany
J 9InstitutodeAstrofísicadeAndalucía(IAA/CSIC),GlorietadelaAstronomías/nAptdo.3004,E-18080Granada,Spain
6 10CONACYTResearchFellow-InstitutodeAstronomía,UniversidadNacionalAutónomadeMéxico,ApartadoPostal70-264,MéxicoD.F.,04510Mexico
11DepartmentofPhysics,InstituteforAstronomy,ETHZu¨rich,CH-8093Zu¨rich,Switzerland
] 12InstitutodeAstrofísicadeAndalucía(CSIC),GlorietadelaAstronomías/nAptdo.3004,18080,Granada,Spain
A 13GEPI,ObservatoiredeParis,PSLResearchUniversity,CNRS,UniversitéParis-Diderot,SorbonneParisCité,PlaceJulesJanssen,92195Meudon,France
14DepartamentodeFísica,UniversidaddelosAndes,Cra.1No.18A–10,EdificioIp,A.A.4976Bogotá,Colombia
G
.
h
p AcceptedXXX.ReceivedYYY;inoriginalformZZZ
-
o
r
t ABSTRACT
s
a
[ We study the galactic wind in the edge-on spiral galaxy UGC 10043 with the combi-
nation of the CALIFA integral field spectroscopy data, scanning Fabry-Perot interferometry
1
(FPI), and multiband photometry. We detect ionized gas in the extraplanar regions reaching
v
a relatively high distance, up to ∼ 4 kpc above the galactic disk. The ionized gas line ra-
5 tios ([Nii]/Hα, [Sii]/Hα and [Oi]/Hα) present an enhancement along the semi minor axis,
9
incontrastwiththevaluesfoundatthedisk,wheretheyarecompatiblewithionizationdue
6
1 toHii-regions.Thesedifferences,togetherwiththebiconicsymmetryoftheextra-planarion-
0 izedstructure,makesUGC10043aclearcandidateforagalaxywithgasoutflowsionizatedby
. shocks.Fromthecomparisonofshockmodelswiththeobservedlineratios,andthekinemat-
1
icsobservedfromtheFPIdata,weconstrainthephysicalpropertiesoftheobservedoutflow.
0
Thedataarecompatiblewithavelocityincreaseofthegasalongtheextraplanardistancesup
7
to<400kms−1 andthepreshockdensitydecreasinginthesamedirection.Wealsoobserve
1
: adiscrepancyintheSFRestimatedbasedonHα (0.36M(cid:12) yr−1)andtheestimatedwiththe
v
CIGALE code, being the latter 5 times larger. Nevertheless, this SFR is still not enough to
i
X drive the observed galactic wind if we do not take into account the filling factor. We stress
thatthecombinationofthethreetechniquesofobservationwithmodelsisapowerfultoolto
r
a exploregalacticwindsintheLocalUniverse.
Keywords: galaxies:individual:UGC10043.–galaxies:ISM:.–galaxies:kinematicsand
dynamics–ISM:jetsandoutflows.
1 INTRODUCTION themassmetallicityrelation(e.g.Tremontietal.2004;Finlator&
Davé 2008; Peeples & Shankar 2011), (ii) the shape of the stel-
larmassfunction(e.g.Nakanoetal.1995;Elmegreen2001)and
Galacticwindsdrivenbyacombinationofsupernovaeexplosions
(iii) the enrichment of the intergalactic medium with metals (e.g.
andstellarwindsfrommassivestarshavebeenproposedasareg-
Aguirreetal.2001;Oppenheimer&Davé2008).
ulatingmechanismintheformationandevolutionofgalaxies(e.g.
Silk&Rees1998;Springeletal.2005;Ciardi2008).Theycanalso Sincethediscoveryofthecentral-starburstdrivenwindinM
explaintheoriginofsomeglobalpropertiesofgalaxiessuchas(i) 82(Lynds&Sandage1963),therehavebeenseveralworksaiming
(cid:13)c 2016TheAuthors
2 C.López-Cobáetal
Table1.ParametersofUGC10043.References:(1)NASA/IPACExtra-
galacticDatabase;(2)HyperLeda;(3)Matthews&deGrijs(2004)
30
Parameter UGC10043 References
Morphology Sbc 1
20
z 0.007208 1
α(J2000) 15h48m41.2s 1
ec) 10 δD(isJt2a0n0c0e)[Mpc] 3+42.19d9552m09.8s 21
cs m−M[mag] 32.72 2
C (ar 0 θ iP.[Ade.g[d]eg] 19501.5 33
E
D hz[pc] 395 3
∆ 10 LHα[ergs−1] 4.5×1040 Thispaper
log(M∗/M(cid:12)) 9.79 Thispaper
20
Starburstgalaxiesarecommonlyobservedtohostsupernovae-
30
driven galactic scale winds (e.g. Heckman et al. 1990; Heckman
2003).Agalacticwindisproducedwhenthekineticenergyejected
30 20 10 0 10 20 30
bysupernovaeandstellarwinds,producedbymassivestarforma-
∆ RA (arcsec) tion,isefficientlythermalized.Thismeansthatthekineticenergy
ofthewindisconvertedintothermalenergyviashocks,withalit-
tlelossofenergybyradiationduetothehightemperaturesandlow
Figure 1. True-color image of UGC 10043 extracted from the CALIFA densities.Thejointeffectofsupernovaeandstellarwindscreatesa
datacube,wherebluecorrespondsto4450Å,greento5500Å andredto
bubbleofhotgas(T∼108K)insidethestar-formingregionwitha
6580Å.Itisappreciatedthedustabsorptionlinealongthegalacticdisk,
pressuregreaterthanitsenvironment(e.g.Heckmanetal.1990).
thatismoreevidentinthecentralregions.Thewhitecontourindicatesthe
detectionlimitofthefluxintensityofthe[Nii]λ6584emissionline.The Asthebubbleexpandsandsweepsitsenvironment,itquickly
dashedlinesindicatethepotentialbi-conicalstructureoftheionizedgas turns into a radiative phase. If the environment is stratified, like
emission,withanapertureangleofθ≈80◦tracedbyeyeatthemaximum in the case of galactic disks, the bubble will expand faster in the
extensionoftheemissionlineintensity. verticaldirectionofthepressuregradient.Thevelocityofthishot
gasisexpectedtobeintherangeofafewthousandskms−1 (e.g.
Heckman 2003). Once the bubble reaches a certain scale height,
tounderstandtheprocessthatdrivegalacticwindsinactivegalac- the expansion will accelerate and break into fragments. This will
ticnuclei(AGN),starburstandmerginggalaxies(Heckmanetal. allow the gas to expand freely into the halo and the intergalactic
1990;Richetal.2010,2011;Sturmetal.2011;Wildetal.2014). mediumfollowsabipolarcollimatedoutflowgeometry.Thisisthe
Theunderstandingoffeedbackprocessesbyoutflowsplaysanim- so-calledblow-outphasewhenthebubbleturnsintoasuper-wind.
portantroleinthestudyofgalaxyevolutionsincetheymayaffect TheopticalandX-rayemissionintheblow-outphasecomesfrom
stronglythepropertiesoftheinterestellarmedium:i.e.theenergy obstacles(clouds,fragmentedshells)thatareimmersedinthegas
released by star formation (SF, hereafter), and AGN activity into andareshock-heatedbytheoutflow.Thisscenariowasexplained
the halo can heat the gas, preventing its cooling and as a conse- indetailbyHeckmanetal.(1990).
quencesuppressingtheSFinlow-massgalaxies(e.g.Scannapieco Hugeadvantagesoverclassicallongslitspectroscopyareob-
etal.2000;Hopkinsetal.2012).Suchprocessesmayhaveasignif- tainedbytheuseofIntegralFieldSpectroscopy(IFS)tostudythe
icantimpactontheevolutionofthehostgalaxybyregulatingthe spatially resolved properties of galaxies. IFS provides with spa-
amountofcoldgasavailableforSF.Inaddition,thegalacticwinds tiallyresolvedspectraofacompleteField-of-View(FoV),allow-
canreducethenumberofexistingdwarfgalaxies,sincethekinetic ingthestudyofdifferentcomponentsofagalaxyinasimultane-
energy from supernovae ejects halo gas, thus suppressing the SF ousway.ThecombinationofimageandspectroscopythroughIFS
(e.g.Dekel&Silk1986). providesabetterunderstandingofthepropertiesofgalaxies.Sev-
Super-windsarephenomenologicallycomplexsincetheyare eralworkshaveimplementedtheuseofthistechniquetostudythe
comprised of multiple gas phases moving at different velocities ionizationbyshocksand/oroutflowsofgalacticwinds(e.g.Rich
(e.g. Bland-Hawthorn 1995; Heckman et al. 2000; Veilleux et al. etal.2010,2011,2014;Hoetal.2014;Wildetal.2014;Biketal.
2005; Strickland & Heckman 2009). The mass released by star- 2015;Mahonyetal.2016).However,toourknowledge,thereare
burst superwinds can range from tens to thousands of M(cid:12) yr−1 nodetailedstudiesofthefrequencyofoutflowsingalaxies(seefor
with velocities of ∼ 100 km s−1 for the cool component, mean- exampleDahlemetal.1998;Heckmanetal.2000;Heckman2003;
whileinAGN-drivenoutflowsthevelocitiesexceeds500kms−1. Hoetal.2016).
Themechanismthatdrivesoutflowsinstarburstsisthemechanical Inourcurrentpaper,wepresentthestudyofthespatiallyre-
energy supplied by supernovae explosions and stellar winds (e.g. solved properties of the ionized gas in UGC 10043 based on the
Leitherer&Heckman1995).Itisknownthatsuper-windsathigh datafromtheCalar-AltoLegacyIntegralFieldArea(CALIFA)sur-
scalesareverycommoningalaxieswithSFsurfacedensitylarger vey(Sánchezetal.2012),focusingontheanalysisofthedetected
than0.1M yr−1 kpc−2,bothinthelocalUniverse(Dahlemetal. galacticwind.Thisisapilotstudywhichultimategoalistheex-
(cid:12)
1998;Lehnert&Heckman1996)andathighredshift(Pettinietal. plorationofthefrequencyandphysicalconditionsofsuchoutflows
2001). inthecompletesampleofCALIFA.Thepaperisorganizedasfol-
MNRAS000,1–14(2016)
GalacticwindsinUGC10043 3
lows:wepresentthemainpropertiesofUGC10043in§2;thedata inGarcía-Benitoetal.(2015).Theprocedurecomprisestheusual
are described in §3, and the conducted analysis in §4. Section 5 stepsinreductionofIFSdata,asdescribedinSánchez(2006):bias
describestheanalysisofobservationswithascanningFabry-Perot anddarksubtraction,cosmic-rayremoval,CCDflat-fielding,spec-
interferometerattheRussian6-mtelescope;whilethemainresults tratracingandextraction,wavelengthandfluxcalibration,andfi-
arepresentedin§6.Finally,wepresentthemainconclusionsand nallycubereconstruction.Thefinalproductofthedatareduction
discussion in §7. Throughout the paper, we adopted the standard isaregular-griddata-cube,withxandycoordinatesindicatingthe
LCDMcosmology,withparametersH =70.4kms−1Mpc−1,Ω rightascensionanddeclinationofthetargetandzacommonstep
0 m
=0.268andΩΛ=0.732. inwavelength.TheCALIFApipelinealsoprovideswiththepropa-
gatederrorcube,apropermaskcubeofbadpixels,andaprescrip-
tionofhowtohandletheerrorswhenperformingspatialbinning
(duetocovariancebetweenadjacentpixelsafterimagereconstruc-
2 MAINPROPERTIESOFUGC10043
tion).
UGC10043isanedge-onspiralgalaxy(i∼90◦)locatedatadis- These data were complemented with multi-band, aperture
tance of ∼ 35 Mpc (see Table 1). It is found close to MD2004 matched, photometry extracted from the Galaxy Evolution Ex-
dwarf, a companion galaxy located 84(cid:48)(cid:48)to the NW. Matthews & plorer (GALEX; Martin et al. 2005), Sloan Digital Sky Survey
deGrijs(2004)suggestedapossibleinteractionwithUGC10043 (SDSS;Yorketal.2000),andWide-FieldInfraredSurveyExplorer
whichmayexplaintheobservedtidalwarpinitsdisk.UGC10043 (WISE;Wrightetal.2010)surveys,extractedfollowingtheproce-
presents a very thin disk and a prominent large and bright bulge duresdescribedinBitsakisetal.(inprep.).Toestimatethephysical
(Fig.1).Opticalimagesrevealaverypronounceddustlanealong propertiesofthisgalaxy,theseauthorsprovidedaspectralenergy
its disk. Matthews & de Grijs (2004), using Hubble Space Tele- distribution(SED)modelling,usingCIGALE(Nolletal.2009).
scope (HST) narrow band observations in Hα + [Nii] found evi- We also use Fabry-Pérot Interferometer (FPI) observations
denceofstar-formationinitsnucleus.TheyalsofoundHα emis- obtained at the prime focus of the 6-m telescope of Special
sionperpendiculartothediskfollowinganapproximatelybi-conic Astrophysical Observatory Russian Academy of Sciences (SAO
structureresultingfromapossiblegalacticwind.Theseauthorses- RAS)in2014May24/25.ThescanningFPIwasmountedinside
timatethevelocityofthewindin∼100kms−1reachingadistance theSCORPIO-2multi-modefocalreducer(Afanasiev&Moiseev
of3.5kpcoverthedisk.Aguirreetal.(2009)mappedUGC10043 2011).Theoperatingspectralrangearoundthe[Nii]λ6584emis-
withtheVLA.TheyarguedthatUGC10043isunderinteraction sionlinewascutbyanarrowbandpassfilterwithaFWHM≈21Å
withMCG+04−37−035(located2.5(cid:48)totheW;z=0.007398)evi- bandwidth. The interferometer provides a free spectral range be-
dencedbyanobservedHi bridgebetweenthetwogalaxies. tweentheneighbouringinterferenceorders∼35Å withaFWHM
oftheinstrumentalprofile∼1.7Å (R∼3860).Duringthescanning
process,wehaveconsecutivelyobtained40interferograms,eachof
1800sexposure,atdifferentdistancesbetweentheFPIplates,un-
3 DATA derseeingconditionsof1.7−2.1(cid:48)(cid:48).TheFoVwas6.(cid:48)1×6.(cid:48)1witha
InourworkweareusingtheIFSobservationsofUGC10043from samplingof0(cid:48).(cid:48)7perpixel.Thedatawerereducedusingalgorithms
the first and second CALIFA data releases (e.g. Husemann et al. and programs described by Moiseev & Egorov (2008) and Moi-
2013; García-Benito et al. 2015). The CALIFA survey is a re- seev(2015).Thus,eachspaxelinthereduceddatacubecontainsa
centlycompletedprojectthatcomprisesthreedatareleases(DR1, 40-channelspectrum.
DR2 and DR3), the last one delivered in 2016 (Sánchez et al.
2016a).TheaimofCALIFAwastoobtainspatiallyresolvedspec-
troscopyofmorethan600galaxiesattheLocalUniverse(0.005< 4 ANALYSIS
z < 0.03) covering a wide range of morphological and stellar
4.1 ContinuumSubtraction
masses.Theobservationscovertheopticalsizeofthegalaxiesup
to2.5effectiveradiiusingthewide-fieldIntegralFieldUnit(IFU) To study the properties of the ionized gas we need to uncouple
PmasfiberPAcK(PPAK;Kelzetal.2006)ofthePotsdamMulti- thecontinuumfromeachspectraofthedata-cube.Therearesev-
ApertureSpectrophotometerinstrument(PMAS;Rothetal.2005). eralroutinesfocusedintheanalysisofthestellarpopulations(e.g.
ThePPAKfiberbundleconsistsof331fibersof2.7(cid:48)(cid:48)diametereach STARLIGHT,pPXF,CidFernandesetal.2011a;Cappellari&Em-
onecoveringatotalhexagonalFoVof74(cid:48)(cid:48)×64(cid:48)(cid:48)withafillingfac- sellem 2004). Here we adopted Pipe3D, a pipeline developed to
tor of ∼ 60%. In order to guarantee a complete coverage of the analyseIFSdata-cubes(Sánchezetal.2016c, S16hereafter)using
FoV,threeditheringpointingswereappliedtoobtain993indepen- thefittingpackageFIT3D(Sánchezetal.2016b, S15hereafter).
dentspectraforeachobject.Thefinalspatialresolutionis∼1kpc Generally the continuum spectra show a wide range of sig-
at the redshift of the sample. This allows to resolve spatially the naltonoiseratios(S/N)thatarehigherinthecentralregionsand
spectroscopicpropertiesfromthemostrelevantcomponentsofthe graduallydecreasingoutwardfromthegalacticcentre.Fromsimu-
galaxies (Hii regions, bars, spiral arms, bulges). Each galaxy of lationstestedinS15,weobservedthataminimumS/N isrequired
theCALIFAsamplewasobservedintwodifferentconfigurations, ineachspectrumtoobtainanaccuratemodelofthecontinuumand
oneoflowresolution(V500,R∼850)coveringtheopticalrange thereforetoderivethepropertiesoftheionizedgas.Inordertoin-
3750–7500Å andanotheroneofintermediateresolution(V1200, creasetheS/Nineachspectrumweperformaspatialbinningofthe
R∼1650)thatcoversthebluepartoftheopticalrangeofthespec- cubeintheopticalrangeselectingasagoalvalueaS/N∼50.In
tra 3700–4800Å. Along this article we use the data of the V500 Fig.3weshowtheresultofthistessellationprocedure.Thistessel-
set-upforUGC10043. lationhasoneadvantagecomparedtoothermethods,suchasthe
The data were reduced using version 1.5 of the CALIFA Voronoi one (Cappellari & Copin 2003), that the performed seg-
pipeline,whosemodificationswithrespecttotheonepresentedin mentation follows the morphology of the galaxy and at the same
Sánchez et al. (2012) and Husemann et al. (2013), are described timeincreasestheS/N,asdescribedinS16.
MNRAS000,1–14(2016)
4 C.López-Cobáetal
35
17
16 [OIII]5007
30 15 Hβ
14 [OIII]4959
13
12
11
25 10
1] 9
4860 4960 5060
Å
2
m20 Hα
c
1
s
g
er15
16
0
1
ux [10 [NII]6584
Fl
[SII]6717
5 Hβ [OIII]5007 [SII]6731
[NII]6548
[OIII]4959 [OI]6300
0
4000 4500 5000 5500 6000 6500 7000
Wavelength [Å]
Figure2.ExampleofthefittingprocedureofthestellarpopulationusingFIT3Dforonespectrumderivedbyintegrating25spaxelsaroundthecentralregion
ofUGC10043.TheoriginalspectrumisshowninblackandinyellowisthebestfitoftheSSP.Theredcorrespondtothebestcombinationofthestellar
populationsandemissionlinesthatdescribethedata.Ingreenisthestellarpopulationaftertheremovalofthefittedemissionlines.Oneoftheresultsofthe
fitisaspectrumwithoutthestellarpopulationincludingtheemissionlinesoftheionizedgas.Inbluewepresenttheemissionlinesafterremovingthefitted
stellarpopulationandinbrowntheresidualofthesubtractionofthebestfitincludingthestellarpopulationsandtheemissionlinemodel.Theinsightpanel
showsanenlargementaroundHβandtheoxygendoublet[Oiii]ofthefit,theyaxishasthesameunitsinbothplots.
Oncethetessellationisperformed,allthespectrawithineach extendsperpendiculartothediskandisclearlyvisibleinHα,[Sii],
spatial bin are co-added and treated as a single spectrum. Then, and[Nii] maps.
wederiveastellarpopulationmodelforeachofthosespectraby
performingamultiSyntheticStellarPopulation(SSP)fit.Finally,
werecoveramodelofthestellarcontinuumforeachspaxelbyre- 4.3 Spatialvariationoftheemissionlineratios
scalingthemodelwithineachspatialbintothecontinuumfluxin-
Theionizationstageofaphotoionizednebulaismainlydetermined
tensityinthecorrespondingspaxel.Thestellarpopulationmodelis
bythreeparameters:theionizationparameterU1,thehardnessof
thensubtractedtocreateapuregasdata-cubecomprisingonlythe
theionizingradiation(dependingontheeffectivetemperatureand
ionizedemissionlines(alsoincludingthenoiseandtheresiduals
metallicityofthestar,ortheageandmetallicityofthecluster,or
ofthestellarpopulationmodelling).Thestrongestemissionlines
the characteristics of the AGN), and the optical depth at the Ly-
withintheconsideredwavelengthrangearefittedspaxelbyspaxel
mancontinuum(matterboundedregionshavinghigherionization
forthepuregascube,adoptingasingleGaussianfunctionforeach
stages).Furthermore,theionizationstageofshockedregionsisde-
consideredemissionline.Bydoingso,wederivetheircorrespond-
terminedbythecharacteristicsoftheshock(speed,magneticfield,
ingfluxintensityandthepropagatederrors.Finally,wecanextract
densities).
asetof2Dmapscomprisingthespatialdistributionofthefluxin-
Theemissionlineratiosinvolvingthestronglines[Nii],[Sii],
tensitiesforeachanalysedemissionline.InFigure2,weshowthe
[Oiii],[Oi]andtheBalmerlines(HαandHβ)havebeenproposed
resultsofthefittingprocedureforonesinglespectrumtoillustrate
asamethodtoclassifybetweenregionsionizedbyAGNandsofter
thefullprocess.
ionizingsourcesasHiiregions(seeVeilleux&Osterbrock1987).
With the use of IFS, we are able to spatially resolve the location
4.2 Ionizedgasemission ofdifferentionizationsourcesbyanalysingtheirlineratios.Asa
firststep,westudythespatialdistributionofthestrongestemission
InFigure4weshowtheintensitymapsfortheemissionlinesHα, lineratiosandinvestigateifthereisanycorrespondencewiththe
[Nii]λ6584, [Oiii]λ5007, Hβ, [Sii]λλ6731,6716 and [Oi]λ6300 populationproperties.
with a cut in S/N > 3. This cut decreases the number of useful Figure 5 shows line ratio maps of [Nii]/Hα, [Sii]/Hα,
spaxelsineachmapbutnotsignificantly.Fromthesemapsweob-
servethatmostofthecontributiontotheionizedgasislocatedina
narrowregionassociatedtothedisk.Thereisanotherevidentcom- 1 U=Q0/4πr2Nec,whereQ0isthenumberofionizingphotonsemittedby
ponent of ionized gas that is uncoupled from the disk, located in thesourcepersecond,risthedistancebetweenthesourceandthenebula,
the extraplanar regions. This extraplanar emission of ionized gas Neistheelectrondensityandcthelightspeed.
MNRAS000,1–14(2016)
GalacticwindsinUGC10043 5
diagram, Baldwinetal.1981),toseparatetheemissionfromsoft
ionizingsources,likeHiiregions,andobjectswithahigherioniz-
ingpower,asAGNs.However,theselineratiosarelessaccurateto
distinguishamongobjectsoflowionization,likeweakAGNs,ex-
30
citationbyshocks,planetarynebulaeandionizationbypost–AGB
stars(e.g.Binetteetal.1994;Morisset&Georgiev2009;Binette
20
etal.2009;CidFernandesetal.2011b;Kehrigetal.2012;Singh
etal.2013).Subsequently,Veilleux&Osterbrock(1987)extended
10 thisschemeincorporatingthediagnosticdiagramsforthe[Sii]/Hα
ec) and[Oi]λ6300/Hαlineratios.Bothlineratiosaresensitivetoion-
s
arc 0 izationbyshocks,being[Oi]/Hαthemostsensitive.
C ( Differentdemarcationlineshavebeenproposedforthesethree
E
D diagnostic diagrams. The most frequently used ones are those by
∆ 10 Kewley et al. (2001) and Kauffmann et al. (2003). The most re-
centonesRichardsonetal.(2014)andRichardsonetal.(2016)are
20 showninFig. 6.TheKewleyetal.(2001)curvewasdeterminedby
meansofphotoionizationmodels.Itisthemaximumenvelopethat
30 canbereachediftheionizationisproducedbyasingleormulti-
pleburstsofstarformation.TheKauffmannetal.(2003)curvewas
obtainedempiricallyfromgalaxiesoftheSloanDigitalSkySurvey
30 20 10 0 10 20 30
(SDSS). It traces the approximate upper limit of the sequence of
∆ RA (arcsec)
theSFregioninthisdiagram.Thetwocurvesarefrequentlyused
to distinguish from SF regions (below the Kauffmann curve) and
Figure3. Tessellationpatternperformedfortheanalysisofstellarpopula-
AGNs(abovetheKewleycurve).Theintermediateregionbetween
tion.Theadoptedbinningprocedureensuresthatthespatialbinsfollowthe
thetwocurvesisusuallyinterpretedasacompositezoneduetoa
shapeofthegalaxy.
combinationofdifferentionizationsources.However,thiscanalso
bepopulatedbyionizationduetostarburstgalaxieswithcontinu-
[Oiii]/Hβand[Oi]/Hα.Thelineratios[Nii]/Hαand[Oiii]/Hβare ousSF(e.g.Kewleyetal.2001),post-AGBstars(seeCidFernan-
insensitive to dust extinction, as the emission lines are close in desetal.2011b;Papaderosetal.2013;Sánchezetal.2014),shock
wavelength.Theotheremissionlineratiosarealsocloseinwave- ionization(e.g.Richetal.2010;Hoetal.2014;Alataloetal.2016),
length,excluding[Oi]/Hα.Weincludethe[Oi]/Hαemissionline orevenclassicalHiiregionsinevolvedareasofgalaxies(e.g.Oey
inouranalysisdespitetheweaknessof[Oi],becauseitisagood &Kennicutt1993;Sánchezetal.2015).
discriminatorbetweenphotoionizationbyhardionizingpower-law InFig.6,weshowtheclassicalBPTdiagramfortheindivid-
sourcesandOBstars,andalsobecauseitisagoodtracerofshock ualspaxels.Accordingtothespatialdistributionoflineratiosob-
excitation(e.g.Richetal.2010;Farageetal.2010). servedinFig.5,ourinterpretationisthattheextraplanaremission
Afirstinspectionofthelineratiomapsrevealsaremarkable is not likely due to photoionization by young stars. These points
increaseinalllineratiosfromthedisktowardtheextraplanarre- arespreadovertheregiondominatedbystarformationtowardsthe
gions,beingmoreevidentinthe[Nii]/Hαand[Sii]/Hαmaps.Ifwe regionclassicallydominatedbyAGN.Sofarthereisnoevidence
assumethatHαtracestheextensionofthediskasseeninFig.4, ofthepresenceofanAGNinthisgalaxy,whichisalsoconsistent
thenweobservethatthelineratioschangestartsattheedgeofthe withitssmallmassandbulge.Therefore,wediscardAGNasthe
disk. possibleionizationsourceforUGC10043.
The[Oiii]/Hβlineratiocoversasmallerareaduetoourcut Due to the shape and geometry of the extraplanar emission,
inS/NinHβ,sinceHβ is∼3timesweakerthanHα.Ontheother thedistributionoflineratiosfromthestarformingregiontowards
hand,the[Oi]/Hαmapislesspopulatedbecause[Oi]isaweakline theintermediateAGNarea,andthelackofevidenceofanAGN,
comparedto[Nii]and[Sii].Thelineratiosatthediskregioninthe weconsiderthattheextraplanaremissionisrelatedtoshockion-
[Nii]/Hαmapareconsistentwiththemaximumratio(log[Nii]/Hα ization induced by a galactic wind created by a central SF event.
< −0.25) observed in star forming regions (e.g. Kauffmann et al. From Figs. 4 and 5 we observe a symmetrical distribution of the
2003).The[Oiii]/Hβlineratioismoreorlessconstantthroughout extraplanargaswithrespecttothegalacticdisk.Ifweassumethat
thegalaxy.Theincreaseinthelineratios[Nii]/Hα,[Sii]/Hαand theburstofSFwasinthenuclearregionofthegalaxy,andassum-
[Oi]/Hαfarawayfromthegalacticdiskhasalsobeenobservedin inganidealbiconicaldistributionoftheionizedgas(e.g.Heckman
thecaseofextraplanardiffuseionizedgas(DIG)inedge-ongalax- etal.1990)wecantracethelimitoftheoutflowingregionbased
ies,inwhichtheionizationatkiloparsecscalesisproducedbyhot onthedistributionofemissionlines.Theexpectedconicstructure
oldstarsinthehalowithelectrondensitiesintheextraplanarregion wasalreadyshowninFig.1
lower than 10−1 cm−3 (e.g. Tüllmann et al. 2000; Flores-Fajardo We will try to confirm the suspicion of shock ionization by
etal.2011). comparingthepropertiesoftheemissionlineswiththepredictions
byphotoionizationandshockmodels.
4.4 DiagnosticDiagrams
4.5 Photoionionizationmodels
Inordertounderstandchangesinlineratiosacrossthefieldofview,
we explore the so-called diagnostic diagrams. Baldwin, Phillips In Fig. 7 we compare the observed line ratios with the predicted
andTerlevichproposedadiagramthatcomparesthelineintensity onesbyphotoionizationmodelsalongthediagnosticdiagramsde-
ratios [Oiii]λ5007/Hβ versus [Nii]λ6583/Hα (known as the BPT scribed in previous sections: [Nii]/Hα, [Sii]/Hα, [Oi]/Hα versus
MNRAS000,1–14(2016)
6 C.López-Cobáetal
Hα Hβ [OIII]λ5007
30 30 30
20 20 20
ec) 10 ec) 10 ec) 10
s s s
c c c
r r r
a 0 a 0 a 0
C ( C ( C (
E E E
D 10 D 10 D 10
∆ ∆ ∆
20 20 20
30 30 30
30 20 10 0 10 20 30 30 20 10 0 10 20 30 30 20 10 0 10 20 30
∆ RA (arcsec) ∆ RA (arcsec) ∆ RA (arcsec)
-1.80 -1.50 -1.20 -0.90 -0.60 -0.30 0.00 0.30 0.60 -1.05 -0.90 -0.75 -0.60 -0.45 -0.30 -0.15 0.00 -1.75 -1.50 -1.25 -1.00 -0.75 -0.50 -0.25 0.00 0.25
[NII]λ6584 [SII]λ6716+6731 [OI]λ6300
30 30 30
20 20 20
ec) 10 ec) 10 ec) 10
s s s
c c c
r r r
a 0 a 0 a 0
C ( C ( C (
E E E
D 10 D 10 D 10
∆ ∆ ∆
20 20 20
30 30 30
30 20 10 0 10 20 30 30 20 10 0 10 20 30 30 20 10 0 10 20 30
∆ RA (arcsec) ∆ RA (arcsec) ∆ RA (arcsec)
-1.60-1.40-1.20-1.00-0.80-0.60-0.40-0.20 0.00 -1.40 -1.20 -1.00 -0.80 -0.60 -0.40 -0.20 0.00 0.20 -1.20 -1.10 -1.00 -0.90 -0.80 -0.70 -0.60 -0.50 -0.40
Figure4.Exampleofemissionlineintensitymapsinlogscale.Thegreencontourencloses70%ofthefluxintheV-bandandtheblackcontouristhedetection
limitoftheNitrogenemission(i.e.forthosespaxelswithS/N>5,log[Nii]=1.25).Thesetwocontoursdemarcatetheemissionofthedisk+bulgeandthe
extraplanaremission.Thecolourbarsrepresenttheintensityinlogscaleoftheemissioninunitsof10−16ergs−1cm−2Å−1.
[Oiii]/Hβ. The points are color–coded by their distance from the 4.6 Shockmodels
galaxy disk. The three panels include the predicted values from
InFigs.6and7,wedescribedtwomaincomponentsintheioniza-
theMAPPINGS-IIIphotoionizationmodels(Allenetal.2008),for
continuousSFbursts,andusingthePEGASE2syntheticstellarli- tion mechanism, one produced by young stars at the disk and an
extraplanar emission that is not reproduced by the analysed pho-
brary,asdescribedbyDopitaetal.(2000)andKewleyetal.(2001).
Eachlinecorrespondstoadifferentstellarabundance(Z/Z(cid:12)=0.5, toionizationmodels.Mostprobably,thisextraplanarionizationcan
beproducedbyradiativeshocksduringthewarmphase(T∼104
1,1.5and2).Foreachofthemtheionizationchangesfromhigh-
K) of a galactic wind as described above. The observed ionized
ionization(top-left)tolow-ionization(bottom-right).Inallcasesan
averageelectrondensityofn = 350cm−3 isassumed.Wewould gascanbelocatedoverthewallsoftheconicstructureorinfila-
e
mentary structures from the nuclear region. Shock ionization can
liketostressherethatthefartheraregionislocatedfromthedisk
thestrongertheionizationitpresents(outto∼4kpc). belocatedinthediagnosticdiagramsinareasdistributedfromthe
classicallocationofHiiregionstowardsareaswhereAGNioniza-
Thususingacontinuousstarburstphotoionizationmodelwe
tionisdominant(e.g.Daviesetal.2014).
canreproducethelineratiosthatliebelowtheKewleyetal.(2001)
curves, whose spatial location is in the disk of the galaxy. These Thesignaturesofshockscanbeseenasdoublepeaksorbroad
regionsaremostprobablyassociatedwithstarformingregionsas componentsinthevelocitydispersionprofilesduetothedifferent
wesuspected,neverthelessionizationbyshockscoverpartofthe kinematiccomponentsalongthelineofsightandthemorphology
star forming region, as we will see later. Furthermore, there are oftheionizedgas.DuetothelowspectralresolutionoftheCAL-
severallineratiosinthediagnosticdiagramsthatarenotcovered IFAdata,wearenotabletoseparatethedifferentkinematiccom-
withintheparametersspaceofthesephotoionizationmodels. ponentsinthevelocitydispersionprofiles,andthereforeuncouple
andanalysethemseparately.AtthewavelengthofHα theinstru-
mental resolution of our data is σ ∼ 116 km s−1, which exceeds
thetypicalvelocitydispersionofHiiregions(<100kms−1,Yang
etal.(1996);Moiseevetal.(2015)).Thus,itisnotenoughtodis-
tinguishdifferentkinematiccomponentsoftheorderexpectedby
2 http://www2.iap.fr/pegase/pegasehr/ shocks(e.g.Lehnert&Heckman1996).Moreover,evenFPIdata
MNRAS000,1–14(2016)
GalacticwindsinUGC10043 7
30 log([NII]/Hα) 0.45 30 log([SII]/Hα) 0.45
20 0.30 20 0.30
c) 10 0.15 c) 10 0.15
e e
s s
arc 0 0.00 arc 0 0.00
EC ( 0.15 EC ( 0.15
D 10 D 10
∆ 0.30 ∆
0.30
20 20
0.45
0.45
30 0.60 30
0.60
30 20 10 0 10 20 30 30 20 10 0 10 20 30
∆ RA (arcsec) ∆ RA (arcsec)
0.6
30 log([OIII]/Hβ) 0.60 30 log([OI]/Hα)
0.3
0.45
20 20
0.0
0.30
sec) 10 0.15 sec) 10 0.3
c c
r r
C (a 0 0.00 C (a 0 0.6
E E
D 10 0.15 D 10 0.9
∆ ∆
0.30 1.2
20 20
0.45
1.5
30 30
0.60
1.8
30 20 10 0 10 20 30 30 20 10 0 10 20 30
∆ RA (arcsec) ∆ RA (arcsec)
Figure 5. 2D line ratio maps for [Nii]/Hα, [Sii]/Hα, [Oiii]/Hα , and [Oi]/Hα. [Sii] represent the sum of the doublet Sulfur ions [Sii] = [Sii]λ6731 +
[Sii]λ6717.Thegreencontourencloses70%ofthefluxintheV-band.TheblackcontourrepresentsthesamedetectionlimitshowninFig.1,illustratingthe
bi-conicstructureoftheoutflowinthe[Nii]map.
takenwithasignificanthigherspectralresolution(σ∼33kms−1) AGN.Thenewdemarcationisabisectorlinewhichseparatesthe
did not resolve a multicomponent structure of the [Nii] emission ionizationbyshocksfromAGNestimatedfromtwofiducialclear
lineprofile,andonlylinebroadeningandasymmetricprofileswere objectsofthiskindofionizationusingIFSdataaccordingtoSharp
observed (see Sec. 5). Broadening profiles in regions outside the & Bland-Hawthorn (2010). In addition to the shown models, we
galacticdiskhasalsoobservedinstarburst–drivengalacticwinds haveexploredmanydifferentcombinationsofmagneticfieldsand
(e.g. Westmoquette et al. 2010). The presence of broad line pro- pre-shockdensities,alongwiththepossiblepresenceofaprecur-
filessuggeststhatcomplexkinematicscomponentscouldexistthat sor. However, noneof them reproduce theobserved line ratios in
arestillunresolvedatthespectralresolutionofourFPdata.There- thethreediagramssimultaneously,aswellasthemodelsthatare
fore,weneedtocomparetheobservedlineratioswiththepredic- presentedinFig.8.
tionsfromshockionizationmodelstodetermineiftheionizationis
drivenbyshocks,andifso,deriveitsphysicalconditions. The shock models in the [Nii]/Hα and [Sii]/Hα diagrams
cover areas frequently associated with continuous SF (e.g. Kew-
WeadoptgridsofshockmodelsfromtheMAPPINGSIIIli- ley et al. 2001; Sánchez et al. 2015) and low ionization nuclear
brary of fast radiative shock models (Dopita & Sutherland 1995, emission–line regions (LINER) (e.g. Gomes et al. 2016). We ob-
1996;Dopitaetal.2005;Allenetal.2008).Weselectedashock servethatthemajorityofthepointsabovetheKewleycurvesare
velocity(v)rangeof100to400kms−1 inintervalsof25kms−1 located at the right side of the bisector line towards the locus of
s
and a transverse magnetic field flux density of 5 µG. For the gas shockexcitationandthereforeintheextraplanarregion.Forthese
component, we explored a range including both solar and supra- diagramswemakeadistinctionbetweentheregionsthatlieinthe
solarabundances,andpre-shockdensitiesof1,10,100and1000 diskandthoseinthebi-conesaccordingtoourdemarcationshown
cm−3,respectively.InFig.8,weplotthediagnosticdiagramsforthe inFig4.Thereisionizationspatiallylocatedatthebi-conesbelow
differentlineratiosexploredinFig.5,togetherwiththevaluespre- theKauffmanncurve,mostprobablyduetothelowshockveloci-
dictedbytheadoptedshockmodelswithoutprecursor.Inthisplot ties components in the emission lines. Our selected shock model
wehaveaddedadifferentdemarcationfromtheclassicalLINER– describes pretty well the line ratios for the outflow zone in the
MNRAS000,1–14(2016)
8 C.López-Cobáetal
intensitymapof[Nii]λ6584,itsline-of-sightvelocityfield,andits
1.0
AGN locus line-of-sightvelocitydispersion(σ)determinedbybroadeningof
emission line. The maps are masked using a S/N > 3 threshold
LINER in the flux intensity. In the first panel we also plot the spectrum
ofkeyregionsinthegalaxy,showingtworegionswithinthedisk,
0.5 andothertwointheareasofmaximumvelocitydispersionlocated
SF locus
) along the semi-minor axis within the outflow cone. We observe
β
H broadandasymmetricprofileswithoutaremarkableseparationof
7/
0 doubleormultiplecomponents,typicallyfoundingalacticwinds
0
5 driven by SF in these two latter regions (e.g. van Eymeren et al.
λ 0.0
I] 2009).
I
O I Attheouterpartsofthediskweobservealowvelocitydisper-
([ sion(10-40kms−1),whichisthetypicalvalueforgiantHiiregions
g
o ingalaxies(e.g.Moiseevetal.2015).Whileinthewindbi-cones
l
0.5 σ exceeds 100 km s−1, increasing towards larger distances from
the galactic disk, reaching vales ∼ 300 km s−1 probably because
athigherdistancesfromthediskthedensityoftheISMislower.
HII Comp Thesevaluesofthevelocitydispersionareroughlyconsistentwith
theshockmodelsdescribedbefore,forwhichtheexpectedveloci-
1.0 tiesareexpectedtobelowerthan400kms−1.
1.0 0.5 0.0 0.5 1.0
log([N II]/Hα) TheFPImapshowsthatthecircularrotationmakesamayor
contributiontotheobservedline-of-sitevelocitieseveninthegalac-
tic wind region. This picture is typical for edge-on disk galaxies
Figure6.BPTdiagnosticdiagram([Nii]/Hαversus[Oiii]/Hβ).Eachgreen with a relatively moderate outflow (e.g., NGC 4460, Oparin &
dotcorrespondstothelineintensityratioatdifferentlocationswithinthe Moiseev2015).Themeanrotationcurvewassubtractedfromthe
galaxyasshowninFig.5.Bluecontoursaredensityprofilesofthedata. observedvelocityfieldwiththeaimtoremovetheregularveloc-
Thelargestcontourencloses90%ofthedata,whiletheotheronesenclose itygradient.Weuseamodelofatransparentrotatingcylinderthat
75,55and35percentofthetotaldata,respectively.Thedashedandsolid providesagoodapproximationofvelocityfieldsinedge-onrotat-
blacklinesrepresenttheKauffmannetal.(2003)andKewleyetal.(2001)
ingdiskgalaxiesasdescribedindetailin(Moiseev2015).Inshort,
curves,respectively.Theblackdottedlinerepresentthedemarcationline
therotationcurvewascalculatedfromaveragingpointsacrossthe
fromLINERandSeyfertfrom(Kauffmannetal.2003)Theyellowtrian-
galaxy major axis, the amplitude of ionized gas rotation in UGC
gleisthelocationofthecentralspectrumofUGC10043fromthefitting
10043reaches150kms−1.Themeanrotationcurvewasextrapo-
procedureshowninFig.2.Theredandyellowlinesrepresentthelocusof
AGNandSFrespectively,resultingfromreconstructedemissionlinefluxes lated outside the galactic mid-plane to create a model of galactic
basedonmeanfieldindependentanalysis(MFICA)fromRichardsonetal. rotation.Theresidualline-of-sightvelocitiesafterthecircularro-
(2014)andRichardsonetal.(2016).Thegreycoderepresentsthedensity tationsubtractionareshowninthelastpanelofFig.9.Thismap
ofpoints.Wenoteabifurcationofthepointsfromtheregionclassicallyas- reveals a dozen “spots” inside the outflow bi-cones with typical
sociatedwithionizationbystarstowardregionsclassicallyassociatedwith residualvelocities±30kms−1.Thesymmetricaldistributionofthe
AGNionization. residualsrelativetothemajoraxisimpliesthatweareabletoob-
serverealregulardeviationsofline-ofsight-velocitiesfromthecir-
[Nii]/Hα and[Sii]/Hα diagramsandcoverspartiallytheobserved cularrotationproducedbythewindoutflow.
lineratiosfor[Oi]/Hα.Theshockmodelsdescribetheoutflowre-
gionforawindwithapre-shockdensitydecreasingtowardlarger 5.2 Outflowvelocities
extraplanardistanceswithanincreaseofvelocityupto<400km
s−1inthesamedirection. We translated the observed line-of-sight residual velocities into
windoutflowvelocitiesintheframeworksofasimplegeometrical
modelpresentedbyOparin&Moiseev(2015).Thewindnebulaeis
describedbyfrustumrotatingbi-cones.Thematterejectedfromthe
5 FABRY-PÉROTINTERFEROMETERDATAONGAS galacticcircumnuclearregionformsasinglelargeshell.Whilethe
KINEMATICS innerhotgashereistransparentatvisiblewavelengths,thewalls
of the bi-cones could be observed in optical recombination lines.
5.1 Kinematicmaps
From the velocity dispersion map shown in Fig. 9 it is clear that
The Fabry-Pérot Interferometer data provide information about theshockedionizedgasfollowsaconicaldistribution,withalow
ionized gas kinematics with velocity resolution four times better velocitydispersionatthecentralregions(<100kms−1),andatthe
than that of the PPAK/V500 data, in a significantly larger field- edgesofthecone.Followingthiskinematicstructureweestimate
of-view, but with a shallower depth. The observed profiles of the theopeningangleasθ ∼45◦(asmarkedinFig.9),tracedbyeye
kin
[Nii] line were fitted with a Voigt function, which is a convolu- atthelocationofthemaximumgradientinthevelocitydispersion.
tionofaLorentzianandaGaussianfunctioncorrespondingtothe Thisapertureangleissmallerthantheoneoneestimatedfromthe
FPIinstrumentalprofileandbroadeningofobservedemissionlines, morphologyoftheionizedgasemissionbasedontheCALIFAdata.
respectively (Moiseev & Egorov 2008). The emission-line spec- Thisismostprobablybecausetheformertracesthelocationofthe
trum is very well described by a single-component Voigt profile observedchangeinthevelocitydispersion,whichthelattertraces
withoutdoubleormulti-componentsstructures.Fig.9showstwo- the largest extension of the ionized gas. We note that according
dimensional maps derived from the fitting process, including the toobservationsofwindsinothergalaxies,likeM82,conewalls
MNRAS000,1–14(2016)
GalacticwindsinUGC10043 9
1.0 Seyfert LINER Seyfert LINER1.0 Seyfert LINER 4.0 pc]
k
3.5 h [
0.5 Z=1.0 0.5
)β 3.0
H
7/ Z=0.5
0 2.5
50λ 0.0 Z=1.5 0.0
O III] 2.0
g([ Z=2.0 1.5
lo 0.5 0.5
1.0
0.5
1.0 1.0
0.0
1.0 0.5 0.0 0.5 0.8 0.6 0.4 0.2 0.0 0.2 0.4 2.0 1.5 1.0 0.5 0.0
log([N II]/Hα) log([S II]/Hα) log([O I]λ6300/Hα)
Figure7.Diagnosticdiagramsforthe[Nii]/Hα,[Oiii]/Hαand[Oi]/Hαlineratiosasafunctionof[Oiii]/Hβ.Eachdotcorrespondstoonespaxel,thecolour
coderepresentstheperpendiculardistancetothedisk,inbothdirections,inunitsofkpc.Thedarknessbluecoloursareregionsclosertothediskandlighterare
thosefurtheraway.Thecolourlinesrepresentthepredictionsofphotoionizationmodelsfromyoungstarswithcontinuous-burstforthedifferentabundances,
indicatedintheplots,coveringarangefromZ=0.5toZ=2,withdifferentionizationstrengthatvariouslocationswithineachcurve.Thedashedlineinthe
[Nii]/Hα diagramistheKauffmannetal.(2003)curveandthesolidlineinthethreepanelsistheKewleyetal.(2001)curveforthoselineratios.Thedotted
linesinthe[Nii]/Hα,[Sii]/Hα and[Oi]/Hβ diagramsarethedemarcationlinesforLINERandSeyfertgalaxiesaccordingtoKauffmannetal.(2003)and
Kewleyetal.(2006).
1.0 bicone
shocks
disk+bulge
0.5 vs=100 kms1 n=1 cm3 n=1 cm3 n=1 cm3
H)β
7/
0
50λ 0.0 n=10 cm3
O III] n=100 cm3 n=1000 cm3
g([ n=300 cm3
o
l 0.5 n=1000 cm3 n=1000 cm3
1.0 HII comp
1.0 0.5 0.0 0.5 1.0 0.5 0.0 0.5 2.5 2.0 1.5 1.0 0.5 0.0 0.5 1.0
log([N II]/Hα) log([S II]/Hα) log([O I]λ6300/Hα)
Figure8.Diagnosticdiagramsforthe[Nii]/Hα,[Oiii]/Hαand[Oi]/Hαlineratiosasafunctionof[Oiii]/Hβ.Reddotsarethoselocatedwithinthebi-conical
structuredescribedbeforeandthebluedotsarethoselocatedinthedisk.EachyellowlinerepresentsashockmodelwiththesamemagneticfieldofB=5
µGanddifferentvelocitiesincreasingattherightofeachpanelfrom100to400kms−1.Theblackdashedlinesconnectmodelswithequalvelocities.Yellow
dotsareinterpolationsofthemodelsofn=100cm−3 andn=1000cm−3 atn=300cm−3.Ineachplot,wehaveaddedademarcationfromtwoclearest
examplesofAGNphotoinizationandshockionizationaccordingtoSharp&Bland-Hawthorn(2010).Thisgreendashedlinemarksthebisectorbetweenthese
twofiducialtraces,totheleftisthelocusoflineratiosfortheAGN-excitedemissionandtotherightthelocusoflineratiosforshock-excitedemission.
visible in the optical are not homogeneous but consist of several whereV istheresidualline-of-sightvelocityaftersubtractingthe
res
emissionfilaments. purecircularrotation,φistheazimuthanglerelativetotheaxisof
Underthisassumption,theobservedgasbelongstothecone thecone.Withthisequationseveralregionswithalargeamplitude
wallsandmovesalongthemoutofthegalacticdiskwithanoutflow ofV translatedintofastmovingfilamentswithV ≈100–250km
res out
velocityV .Foranedge-ongalaxythepositivevelocitiescorre- s−1,whilethevelocitiesoftheneighbouringpointsaresignificantly
out
spondtothegasonthewallsclosesttous,whilethematterwith smaller. These de-projected outflow velocities are in the range of
negativevelocitiesmovesalongthefarthestwall.Accordingtothe thosefoundinthesurfaceofbipolarstructures(e.g.Heckmanetal.
formula in Oparin & Moiseev (2015) for the galactic inclination 1990; Heckman 2003). Therefore, we confirm the measurements
i=90◦: ofthewindvelocitiesareconsistentwithshocksmodels,asinthe
caseofthedistributionofσ(see§.5.1).
V
V = res , (1)
out sin(θ /2)sinφ
kin
MNRAS000,1–14(2016)
10 C.López-Cobáetal
Flux [10 16 erg s 1 cm 2 Å 1] Velocities [km s 1] σ [km s 1] Vres [km s 1]
1 2 2000 2400 50 100 150 200 250 -40 40
2 1
60
40
20
ec) 2
C (arcs 0 1 4
E
D∆ 3
20
40
3 4
60
40 30 20 10 0 10 20 30 40 40 30 20 10 0 10 20 30 40 40 30 20 10 0 10 20 30 40 40 30 20 10 0 10 20 30 40
∆ RA (arcsec) ∆ RA (arcsec) ∆ RA (arcsec) ∆ RA (arcsec)
Figure9. ResultsoftheFPIobservationsinthe[Nii]emissionline.Fromlefttotheright:[Nii]monochromaticmap,line-of-sightvelocityfield,velocity
dispersionmapfreefrominstrumentalprofileinfluenceandmapoftheline-of-sightvelocitiesaftersubtractionofthemeanrotationcurve.Theinsetsinthe
firstmapareasubsetofFPIspectraextractedatdifferentlocations.Theselocationsaremarkedwithblacksquaresinthefirstpanel,andtheycorrespondsto
aperturesof6.3(cid:48)(cid:48)×6.3(cid:48)(cid:48)
.ThehexagonmarksthefieldmappedwithCALIFA.Thegeometricalmodelusedforthewindoutflowvelocitiesestimationisshownonthelastpanel.
1.0 Seyfert LINER Seyfert LINER 240 1]
m s
210 k
7/H)β 0.5 180 v [disp
0
50λ 0.0 150
O III] 120
og([ 0.5 90
l
60
1.0 30
1.0 0.5 0.0 0.5 0.8 0.6 0.4 0.2 0.0 0.2 0.4 2.0 1.5 1.0 0.5 0.0
log([N II]/Hα) log([S II]/Hα) log([O I]/Hα)
1.0 Seyfert LINER Seyfert LINER 270 1]
240 m s
k
07/H)β 0.5 128100 v [out
0
5λ 0.0 150
O III] 120
og([ 0.5 90
l
60
30
1.0
1.0 0.5 0.0 0.5 0.8 0.6 0.4 0.2 0.0 0.2 0.4 2.0 1.5 1.0 0.5 0.0
log([N II]/Hα) log([S II]/Hα) log([O I]/Hα)
Figure10.DiagnosticdiagramssimilartoFig.7,butthecolourcoderepresentstheionizedgasvelocitydispersionσ(toppanels),andVout(bottompanels)
accordingFPIdata.Onlypointsbelongingtothebi-conewindnebulaemarkedontheFig.9areshown.
MNRAS000,1–14(2016)