© Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 M´exico. Astrof´ısica Astronom´ıa y de Mexicana Revista ino neatn n egn ytm,adtheo- and systems, merging and frac- interacting significant of a of show Studies tion universe early galaxies. the elliptical in transformation galaxies into complete galaxies the spiral nu- even of galactic perhaps in and activity quasar-like forma- clei of star onset of bursts the intense tion, in properties resulting the galaxies, on of impact profound quite a inter- have interact These can actions can companions. nearby they found their and with are strongly groups, galaxies and isolation, clusters in in evolving of Instead https://doi.org/10.22201/ia.01851101p.2020.56.01.09 c 2 1 00 nttt eAtoo´a nvria ainlAtooad M´exico Aut´onoma de Nacional Astronom´ıa, Universidad de Instituto 2020: nttt eAtoo´a NM iddd M´exico, de Ciudad UNAM, Astronom´ıa, de France.Instituto Marseille, LAM, CNES, CNRS, Univ, Marseille Aix H α IEAISO H SLTDITRCIGGLX PAIR GALAXY INTERACTING ISOLATED THE OF KINEMATICS nNC69 ihtoeotie napeiu iia ieai nlsso the of analysis results kinematic our pairs. similar of galaxy previous these comparison a between The in differences great obtained highlighted literature. those Antennae the with comparing by from 6090 NGC results perturbations results our on the of kinematic of consistency some with the parameters, analysed verified them We kinematic also We several encounter. their curve. obtained by H rotation we induced its the 6090 and interferometer, NGC in field Fabry-Perot velocity in observations scanning its galaxy the present each with we kinematic For acquired pairs, and PUMA. 6090 NGC galaxy morphology of both gas, line of hydrogen emission pair. behaviour ionized galaxy dynamic of 4038/39) (NGC and distribution Antennae the the compare to To features similar displays 6090) (NGC iia rvopr a nea etcogadsdfrniseteetsprsde pares estos Words: entre an´alisisKey cinem´atico diferencias un destac´o grandes de Antenas los las con galaxias. para 6090 NGC previo de similar encuentro. resultados literatura. su los la comparaci´on de por de rotaci´on. obtuvieron los compar´andolosLa inducidas con resultados de se estos perturbaciones curva de 6090 las verific´o consistencia NGC su Se la de en y algunas velocidades galaxia analizaron de Adem´as, cada se campo Para par´ametros cinem´aticos, su PUMA. varios barrido, de Antenas Fabry-Perot ob- emisi´on Las l´ınea presentan H de la se en galaxias galaxias, servaciones com- morfolog´ıa de de y ionizado, pares gas ambos din´amico distribuci´on cinem´atico par entre del y portamiento la comparar al Para similares caracter´ısticas 4038/39). (NGC muestra 6090), (NGC .INTRODUCTION 1. notcliae,tebrl tde sltditrcigglx arKG486 KPG pair galaxy interacting isolated studied barely the images, optical In ni´gnsdl´pio lprd aaisasaopc suid,KG486 KPG estudiado, poco aislado galaxias de par ´optico, el im´agenes del En ieaisaddnmc ehd:dt nlss—techniques: — analysis data galaxies: methods: — interactions — interferometric dynamics galaxies: — and 6090 kinematics NGC individual: galaxies: .M Sardaneta M. M. eevdMrh1 09 cetdDcme 72019 17 December accepted 2019; 19 March Received P 8 NC6090) (NGC 486 KPG 1 .Rosado M. , , 56 ABSTRACT α RESUMEN 18 (2020) 71–85 , eNC69 durdscne interfer´ometro el con adquiridas 6090 NGC de 2 n .S´anchez-Cruces M. and , rvttoa neato ihaohrglx a be dis- may galaxy another are the with interaction that gravitational galaxies established (1972), simulations, Toomre of numerical & through Toomre bodies 1986). (Schweizer the torted structures commonly, spiral and increased and, and/or bridges bars large stellar are in tails, there Morphologically, galaxies interacting effects. the gravitational by erned population 2000). galaxy (Mihos the general of in evolution the shaping pro- rare dominant cess the inter- being be may than strong interactions Rather galaxy of events, lifetime. form their some during had action have galaxies that indicate most formation structure cosmological of ries h vlto n neato fglxe sgov- is galaxies of interaction and evolution The 1 α 71 © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 ytm ti motn ooti h ieai in- kinematic the obtain to perturbed important on asymmetric is points an it few for system, a However, only galaxy. to the information restrict- cer- 2016), kinematic al. along ing G¨unthardt et spectroscopy (e.g. positions long-slit tain been using has out galaxies interacting carried on work kinematic the al. et Torres-Flores 2003; al. 2014). et lead (Amram always and merging not may misalignments to that collisions axes suggest hand, tails major tidal other gaseous the and On stellar mergers. or galaxy- strong interactions imply galaxy curves rotation veloc- between the of discrepancies sides disturbed com- both amplitude gas highly high kinematic and In double ponents, nuclei, double 2007; 2010). fields, 2004, ity mem- al. al. the et et (Fuentes-Carrera of effect Repetto pair each the on the of have understanding can bers for interaction the useful that is galaxies ing 1987). evolu- (Karachentsev the galaxies of the of properties tion about and formation information of important galaxies conditions Gabbasov double with 2011; on us research al. provides Systematic et 2014). Rosado al. 2004; (Fuentes-et al. other each et gravita- between Carrera the exerted to effects relative nearest tional neglected their close be of can so effect are gravitational neighbours located which the that galaxies pairs, space two galaxy in of isolated composed of systems that to is 2002). used actions al. features et main Combes the 1981; (Bosma of bar one a is identify along axis curve minor contour isovelocity the central the incli- of the nation Hence, contour symmetrically. deformed isovelocities are the curves orbits; non-circular ellipti- and in to cal very observable corresponding shows clearly dynamics characteristics, is gas distinctive bar the Martin a component, 2014; stellar When al. the 2016). et Gabbasov Soto 1992; 1999; & Hernquist al. & star- et (Barnes trigger region Dinshaw nuclear to of the amounts acts to large bar gas funnelling rapidly The by activity 2015). burst perturbed 2000a,b; al. a Laurikainen et of & disc Renaud Salo the 1987; in trig- (Noguchi bar galaxy a galaxy of companion formation a the S from ger & forces ROSADO SARDANETA, tidal merger, 2001). Karachentsev al. 1966; deformations et Vorontsov-Velyaminov Arp these other 1987; (e.g. surveys several for several and in responsible tails seen solely thin ‘tidal and is large called gravity of they also thus, but which tails’; structures, structure, spiral filamentary of the only not source the 72 rmteosrainlpito iw otof most view, of point observational the From interact- from information kinematic Obtaining inter- galaxy of process the in case simplest The a during that show simulations Numerical els h eea aaeeso G 00which 6090 NGC 1 of Table parameters In general 2017). the al. list et we Cortijo-Ferrero 1999; (Dinshaw discussion al. under and po- et still is the bar, nucleus galaxy; its stellar irregular of distorted an sition a a like of looks has SW evidence 6090 NE NGC 6090 and NGC structure follows: 6090 spiral NGC as up the seen make identifi- In are that an galaxies 2011). has the al. system near-infrared, et (Miralles-Caballero galaxy bridge the nuclei able two tails, its merging a tidal of of addition as and in stage defined because, intermediate been pre-merging an or also in al. has et system 6090 Chisholm NGC galaxy by But merger a as (2015). defined was it shows (Wang kinematics on the 2004). based of al. any system et to the belong in to galaxies appear not gas of molecular does the one component and on 1999) than Scoville & rather (Bryant nuclei them radio the between peak of or is The 2004) length disc 2000). that al. al. of et et angle (Wang Sugai position 1999; disc of Scoville & rotating direction (Bryant a ring the as along nuclei ap- aligned the gas and molecular wings elongated Meanwhile, curved pears 1991). enormous al. with et with and (Martin arcsec, contact 0.14 in by nuclei separated spirals interacting of arcmin. 6090 field NGC a 4 in of of (DSS) view image Survey Fig- of Sky optical of Digitized the the panel from shows upper taken which the This 1 in observed 1999). ure Scoville be & can Bryant feature 1999; 1993; al. Boroson et & Dinshaw Mazzarella 1991; al. al. et et Hummel Martin 1972; 1987; Toomre An- & (The Toomre system system (e.g. galaxy galaxy tennae) 4038/39 NGC this the wavelengths, like looks optical At tidal long 1999). two 486 nuclei KPG and of double disc a tails pair asymmetric as an with described galaxy system been has interacting 6090) (NGC isolated The 2008). al. 2004, et al. Epinat lost et 2015; (Fuentes-Carrera is interaction galaxy that, each the of fact during symmetry the axial to of the addition members sometimes in the system, process of each interacting interaction on the the produced been determine has us informa- which kinematic help extended can the tion way, this spec- In field interferometer(FP). Fabry-Perot integral scanning a ob- as with using troscopy such disc, the techniques of servational portions large from formation ANCHEZ-CRUCES ´ u oteitrcineiec htNC6090 NGC that evidence interaction the to Due pair a as appears 6090 NGC radio-wavelengths In ≈ ≈ 0kci egh(..Dnhwe al. et Dinshaw (e.g. length in kpc 60 3 . rsc h Osuc per to appears source CO the arcsec; 4 1.1 . G 6090 NGC ≈ 60 ◦ ihamjraxis major a with © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 o ahmme.Lsl,w omn norre- compare our and literature, on the comment in we found those Lastly, and sults obtained member. curves each rotation the for as galax- well of as pair 6090, the NGC of ies map H velocity the dispersion and of field analysis the present andaF aacb pcrlycnrddo the on centreded spectrally ob- we cube data H 6090, NGC FP system a galaxy tained the of dynamic and behaviour kinematic and morphology, the gas, gen galac- single a for system. only tic reported been have hitherto 6090. NGC on online. centred viewed view be of can field figure arcsec color The 28 a in H the SPM shown is red, in perposed the on Telescope Multi-Object Space Camera Hubble 2.22 Near-Infrared the Observa- Bottom: from M´exico). the age California, from Baja M´artir, telescope OAN- Pedro SPM, m San 2.1 in Astron´omico Nacional the torio at mode sys- image galaxy shown 86 is the of red, on FWHM in centred superposed H view which, the of over field 6090 NGC (DSS) arcmin Survey tem Sky 4 Digitized a the from in Image Top: 1. Fig. α oivsiaetedsrbto finzdhydro- ionized of distribution the investigate To msinln ftesse.I hspprwe paper this In system. the of line emission α ietiae ae iha6819 a with taken image, direct otie rmtePM nisdirect its in PUMA the from (obtained A ˚ NCO/S)oe hc,su- which, over (NICMOS/HST) α ietiaefo OAN- from image direct α H mg,tevelocity the image, α IEAISO P 8 NC69)73 6090) (NGC 486 KPG OF KINEMATICS le iha with filter A ˚ µ im- m oia etrso G 00osre rmisH its from maps; observed continuum and 6090 NGC monochromatic of features and logical parameters in observational process; the reduction the of overview an is Am- by (1992). made al. Antennae system et the ram galaxy of those the with of 6090 NGC characteristics kinematic the s km 70 ** s km 75 * h g f e d c Administra- Space b and https://ned.ipac.caltech.edu/). Aeronautics tion. National contract Labora- under the Technology, Propulsion with of Jet Institute the by California tory, operated is (NED) Base a csaPld ta.(1996). al. et Acosta-Pulido rat&Soil (1999). Scoville & Bryant (1987). Karachentsev Distance (2015). al. et Chisholm Data Extragalactic (NASA/IPAC (2014) NASA/IPAC otj-err ta.(2017). al. et Cortijo-Ferrero (1990). al. et Condon http://leda.univ-lyon1.fr/). (HyperLeda: HyperLeda itne(p)122 8906 L (Mpc) Distance s (km velocity Radial heliocentric Mean system 6090 NGC (J2000) Coordinates Parameters eaain(rsc 5.4 (arcsec) Separation nuclear Photometric D m Pair G 486 KPG type Morphological names Other itneotie from obtained Distance AAEESO H AAYSYSTEM GALAXY THE OF PARAMETERS IR 25 b hsppri raie sflos in follows: as organized is paper This / ( 2 L − − aci)4.36 (arcmin)

1 1 Mpc Mpc 3 ) D − − 1 1 = . . v/H AL 1 TABLE G 6090 NGC − 1 8855 ) 0 § z epeettemorpho- the present we 3 optdusing computed egr obenucleus double Merger, 0 = δ α utpegalaxy Multiple +52 = 16 = G 10267 UGC . G 6090 NGC 23 with 02930 r 496 Mrk 127.7 Merger 123.3 128 14.36 × h ◦ 10 § 11 g,** 27 d,* sdevoted is 4 h,** e 1f 11 e,* b m b a a 0 a g a,c a § 40.7 24 a a H there 2 00 . H b 0 s a 0 e = = α © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 reseta ag f19 of has range it In- spectral system; (Queensgate free Fabry- servostabilization ET-50 a an a and is with used struments) images FP cosmical The obtain emission sources. extended to of Astronom´ıa- interferometry used de Perot Instituto and the a at is UNAM PUMA built 1995). reducer al. focal et inter- (Rosado Fabry-Perot PUMA scanning ferometer, the M´exico using California, M´artir,(OAN-SPM) Baja Pedro San in Astron´omico Observatorio cional Na- the in at telescope the performed m 2.1 with were 2015 6090 NGC July of observations Our 6090. NGC for Mpc 118 of distance a adopted and e reseta ag hog 8dffrn equally different 48 through range spectral free ter H in (19 resolution is spectral PUMA sampling a of plies finesse effective The H in in presented given is each are of discussion conclusions mass A the of galaxy. computation the including map ysis, dispersion velocity system; the the of motions through non-circular galaxy the each system analyse of galaxy we the and of associated 6090 member NGC the data. each fields, of FP curve velocity our rotation derived from the made show analysis We kinematic the to S & ROSADO SARDANETA, 74 eetrSt3CCD Site3 2048 PUMA sampling ET-50 Spectral H at range spectral Value Free H SPM) at (OAN, order m interference 2.1 FP Finesse interferometer FP Scanning 4 (binning scale Image size Detector Detector Instrument Telescope Parameter vrg eig16 arcsec 1.67 6717 min 72 6819 seeing Average line Calibration time exposure Total filter Interference .OSRAIN N AAREDUCTIONS DATA AND OBSERVATIONS 2. 0 . NTUETLADOBSERVATIONAL AND INSTRUMENTAL nti ae,w considered we paper, this In 5k s km 75 = ms km 0 eouina H at resolution − 1 civdb cnigteinterferome- the scanning by achieved ) − § 1 sddctdt h yaia anal- dynamical the to dedicated is 5 Mpc PARAMETERS α − AL 2 TABLE f/ 1 × α 7 )12 arcsec/pix 1.27 4) § . asganfcsa the at focus Cassegrain 5 α Cno ta.1990) al. et (Condon 7. . 9 99k s km (909 A ˚ 0.97 19 . FH 86 = (FWHM A ˚ 9 4. ms km (44.1 A ˚ 99k s km (909 A ˚ ≈ × ≈ 330 4wihim- which 24 (Ne) A ˚ § 08pix 2048 10 α ,adour and 6, − f0 of 1 tH at ) . − − 414 1 1 ) ) A) ˚ α A ˚ . h bet swl stevlct fteinzdgas. ionized the of velocity the as well as object, H the at emitting gas (ion- ized emission contains monochromatic process pro- the about scanning intensity information the the using throughout Thus, pixel found each file wave- cube. at data in profile calibration calibration each each the The for for fixed level steps. was pixel scanning length at 48 units the arbitrary of in Python value own flux our used we analysis com- scripts. To data and 6090. NGC the of data plete maps resulting our the of to (WCS) seeing average mscsetwcs the determine to IRAF applied We cube. spectral a with of smoothing application Gaussian and 1962) al. and at et rays lines Krassovsky sky cosmic OH of the 6828 removal of subtraction subtraction, cube: bias the to rections ADHOCw the observa- 2. and Table in instrumental listed The are parameters tional pixel. obtain observed to each profile line order inside the of in for wavelength cube end reference calibration the the com- the was at map from phase cube puted parabolic calibration The observation. a whose the obtain lamp Ne to a length used data we 6717 the at So, calibrate line to wavelength. necessary in is it cube layers FP the of channel). per s (90 utes H 6819 86 at of centred FWHM with filter interference an line emission 1 of of pixel arcmin. seeing per 10 sampling of spatial view final 1 of a 512 field obtained a we a So, obtaining of inside signal, window the pixel enhance to 0 ning of scale pixel cube 0 of data tion this for finesse was measured the of the during However, particularly 6090, mirrors observations, NGC the FP for the 1995). acquisition of data parallelism al. the et to due (Rosado channels spaced iraf.noao.edu/. Boulesteix. J. by oped . α 7ace hc ssihl etrta h average the than better slightly is which arcsec 27 ANCHEZ-CRUCES ´ 4 3 eue 2048 a used We h Psann rcs losu ooti a obtain to us allows process scanning FP The used we analysis and reduction data the For dependence wavelength phase avoid to order In IRAF: devel- http://cesam.lam.fr/fabryperot/index/softwares aacb ihattlepsr ieo 2min- 72 of time exposure total a with cube data ≈ . 5 0wihlast apigseta resolu- spectral sampling a to leads which 10 ,6842 A, ˚ . 97 IaeRdcinadAayi Facility” Analysis and Reduction “Image . 7ace.T slt h esitdH redshifted the isolate To arcsec. 67 scoet h esitdnblrwave- nebular redshifted the to close is A ˚ (44 A ˚ oadteWrdCodnt System Coordinate World the add to . 3 2 . 1 rscadw e 4 a set we and arcsec 317 otaet aetesadr cor- standard the make to software n 6863 and A ˚ . a sd hs eotie an obtained we Thus, used. was A ˚ ms km 1 × α ,tecniumeiso of emission continuum the ), 08CDdtco iha with detector CCD 2048 − 4 1 σ ak uhas such tasks tH at ) . 7k s km 57 = 9 Cabran1961; (Chamberlain A ˚ α . − 1 imexamine ntedata the in × bin- 4 http:// × 512 A ˚ α © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 ahpxlwt nacrc o h eta velocities H central the the for of of accuracy an profile with the pixel of each barycentre the ing for profile line pixel. the each of value maximum H the the monochromatic integrating of the intensity C´ardenas-Mart´ınez For the Repetto 2013; image, al. 2018). 2004; Vollmer Fuentes-Carrera et al. (e.g. Rosado & et 2010; cube Fuentes-Carrera al. the et 2000; of channels al. inten- 48 lowest et 3 the the of of sities average was continuum the the considering of made image the of computation The fNC69 Eare NE 6090 NGC of su- were 6090 image. NGC NICMOS/HST of the emissions on panel) (Fig- perposed monochromatic right and 2 panel) ure left H 2 the of (Figure contours uum the show data PUMA results. the our matches view of field of arcsec 2.22 22 panel NICMOS/HST whose the bottom show the we 6090 1 NGC In Figure of antennae. area the central disregarding the to analysis kinematic is H 6090 in NGC system s galactic km 1 8885 the = for pix determined 1 we where side, per side, arcsec per 0 20.32 pixels has 16 which i.e. object, the at of emitting area gas H ionized direct The H the PUMA. with superimposed we obtained panel (upper 1) 6090 Figure NGC of of image optical DSS the On an with filter, same seconds. 90 the of with time and exposure path optical the in H 4 rect to down system from galaxy pixels. range the external the most of the in centre were the values in ratio ra- whose 24 signal-to-noise the pixel, the masked each on of and based field field velocity profiles velocity dial velocity resulting radial the the on superimposed 6090. NGC we to of part corresponding Then, the map contains velocity that radial area the rectangular a only ing G 00N ecnosreta h oie gas ionized the that observe can we at NE 6090 NGC occurs 16 emission monochromatic δ J2000 . α 2 p.Tema eicnrcrda eoiythat velocity radial heliocentric mean The kpc. 726 h ± .MNCRMTCADCONTINUUM AND MONOCHROMATIC 3. 11 DOwcluae h ailvlct ed us- fields velocity radial the calculates ADHOCw h oriae ftecniummaximum continuum the of coordinates The that 6090 NGC of morphology the visualize To di- a obtained we cube, data the to addition In htw eetdwsfudwti h central the within found was detected we that α ms km 5 m ntetdltis(nene,s elmtdour limited we so (antennae), tails tidal the in +52 = α 40 mg fNC69 aigteF u of out FP the having 6090 NGC of image . − 8 − 1 s 1 eddntdtc oie a emitting gas ionized detect not did We . , emse h eoiyfil includ- field velocity the masked We . ◦ 27 δ J2000 0 27 00 . 2 n h aiu H maximum the and 32, IMAGES +52 = α J2000 α iewsotie by obtained was line H ◦ α 16 = 27 IEAISO P 8 NC69)75 6090) (NGC 486 KPG OF KINEMATICS 0 27 . 00 . 7ace = arcsec 27 α .For 0. h µ α J2000 11 α image m α iefor line m contin- image 40 . 8 = s α , nacutrcokiedrcinadwoevleis value north whose the and to ' direction respect counter-clockwise with a continuum ma- in the the of of angle axis the is jor photomet- which contin- (PA), the angle the to position respect of ric with isophotes In symmetrical the are east. that uum the note towards we presence the addition, greater But a pop- has stellar galaxy. the ulation that companion show continuum its the of towards isophotes i.e. west, H in emitting ae ftepooercmxmmare maximum photometric 16 the of nates bar. stellar a of presence h svlct otu uvso h ico the kine- of the to disc respect the with symmetric of not curves are galaxy contour that isovelocity shows NE, 6090 the NGC for 3 s of km Figure radius Furthermore, 9143 a to to up 8799 ordered field from velocity range the in lie s km 8919 a reaches which field, of velocity radius ordered its within ties galaxies. both of veloc- mainly side outside, each northern the Also, the towards toward distortions has maxima. field photometric ity each its on of roughly 6090 NGC ordered one fields i.e. velocity galaxies, veloc- two independent the presents two notice of to field possible ity is it 2.22 superposed) the image and 6090 NGC curves contour of isovelocities field its velocity (with In the shows match. which exactly 3, will Figure photomet- parameters the all kinematic that and expect betweenric not consequence interaction do the we a galaxies, to As the due phenomenon, emission. this continuum of the as ionized ogy the H that at shown emitting was gas it section previous the In SW. 6090 NGC of nuclei the of literature position the the the in of about controversy centre created photometric has this the than galaxy; 1999) al. 2.22 et the shaw litera- of the maximum in the described as knot ture the the to nearer is imum H the that H note we its Moreover, towards of accumulated direction its is opposite of it the that side also opposite and the companion, south, greater the a towards has continuum presence the that note we galaxy, this H α the of ordinates J2000 h 0 11 o h aayNC69 W h coordi- the SW, 6090 NGC galaxy the For o G 00N,tevle fterda veloci- radial the of values the NE, 6090 NGC For ◦ h atr fteiohtssget h likely the suggests isophotes the of pattern The . m 16 = 40 R − . 4 1 s 5 = o G 00S,terda velocities radial the SW, 6090 NGC For . h .KNMTCRESULTS KINEMATIC 4. , 11 α δ . J2000 m rsc i nternefo 73to 8783 from range the in lie arcsec, 6 a rae rsnetwrsthe towards presence greater a has 4.1 43 α α eoiyFields Velocity . osnthv h aemorphol- same the have not does . 3 +52 = s oohoai aiu are maximum monochromatic , δ J2000 ◦ α 27 α +52 = oohoai max- monochromatic 0 aiu emission. maximum µ 22 mg eg Din- (e.g. image m 00 . 1adteco- the and 21 R ◦ 27 − 4 = 1 0 23 ihnits within α . arcsec. 5 J2000 00 . .For 0. µ m = © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 cie ntepeiu eto,sget h pres- the suggests section, de- previous contours mor- the continuum the in the to scribed added by feature, indicated This phology axis. minor matic s online. km s viewed km 8810 in from labelled starting spaced is 10 linearly locity of are in factor which centred a galaxy by each view of the of contours firstly, locity overlaid, field are arcsec field 2.22 velocity NICMOS/HST 26 the On a 6090. interferom- NGC in H FP PUMA, the scanning with eter, the acquired with field obtained Velocity observation 3. Fig. online. viewed be H 2.22 can NICMOS/HST the H figure the the of on from overlaid contours obtained PUMA, ADU 2.22 Right: with 10000 NICMOS/HST to the 1500 6090. on NGC from overlaid spaced on PUMA, linearly continuum interferometer, the FP of scanning contours Left: 2. Fig. S & ROSADO SARDANETA, 76 µ mg n,scnl,teisove- the secondly, and, image m − 1 nt.Teclrfiuecnbe can figure color The units. − α 1 ahisove- Each . oohoai mg ierysae rm40 o200 D obtained ADU 240000 to 4000 from spaced linearly image monochromatic α aacube data µ mg na2 rscfil fve ete nNC69.Tecolor The 6090. NGC on centred view of field arcsec 22 a in image m oriaesses( is systems that coordinate inclined axis is which angle an plane an about galactic the rotates disc to system well-defined perpendicular the a that has galaxy and each (1981). Binney that & Supposing Mihalas by proposed assumptions aycnr fteH the the using of pixel single centre every bary radial in galaxies the the computes of kine- velocity which using the software, observations from ADHOCw FP our the obtained rotation with was the acquired way, data galaxy this matic be each In can of galaxy. that curve disc motion a basic which in most 6090, assumed NGC the in to the galaxy studying corresponds each started of We motion the circular destroyed. otherwise be the as effects, of would order discs to such second kind are perpendicular this disc, motions, galactic motions In radial or the inflows/outflows that system. systems inside argue galactic galaxies interacting can 6090 independent NGC we two the detected sections, have previous we de- in features kinematic scribed and morphological the From criteria the with agreement (1981). Bosma in by bar, proposed stellar a of ence ANCHEZ-CRUCES ´ ndigs,w s h emti n kinematic and geometric the use we so, doing In i µ otepaeo h k;w s h polar the use we sky; the of plane the to mg na2 rscfil fve centred view of field arcsec 22 a in image m 4.2 oainCurves Rotation . α ,θ R, rfieosre nec pixel. each in observed profile ntepaeo h galaxy the of plane the in ) α aacb ythe by cube data © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 e sawoe(hti,o t eteo mass); of centre its of is, (that whole a as tem V supinta hr sailsmer bu the about galaxy, symmetry of axial centre is there that as- assumption we generally galaxies, is disc rotation in sume motion that of Given form dominant plane. the the to ular and respectively, plane, and ρ the in V ( lies velocity axis radial ( the rotation at sky; the the where of color point plane The the at bars. gin with indicated ( galaxy; is each and sector right for same the ordered the In is field within below. velocity pixels SW the 6090 of NGC where online. value and to viewed averaged above up be NE the obtained 6090 can galaxy, NGC with figure each galaxy: associated of each curves dispersion major of rotation the the 2.22 curve the represents line NICMOS/HST shown rotation solid are the the the panels map, of superposed each was computation on kinematic then, the maps the pair; for these galactic indicates the On which in axis components view. galaxy kinematic of of position field the H arcsec for the reference 22 with acquired a maps velocity in the PUMA, show panels Left 4. Fig. h agnilvlct ntepaeo h galaxy the of plane the in ( velocity tangential the V 2 sys Θ (cos Θ ( ,θ R, a bandwt h ailvelocity radial the with obtained was ) ,φ ρ, V h enhloeti ailvlct ftesys- the of velocity radial heliocentric mean the ,φ ρ, Θ V 2 r φ is ) r h ailadtneta eoiisi the in velocities tangential and radial the are cos ) and sec + ntepaeo h k,lctn h ori- the locating sky, the of plane the in ) V θ obs V sin 2 z ( i qa ozr.Mroe,udrthe under Moreover, zero. to equal ,φ ρ, sin i V Θ + 2 = ) φ ildpn nyon only depend will V n tan and ) z V ( V z ,θ R, sys stevlct perpendic- velocity the is + cos ) V φ H r α sec = ( i where , ,θ R, IEAISO P 8 NC69)77 6090) (NGC 486 KPG OF KINEMATICS V obs sin ) i measured ) tan R A P θ Thus, . V θ R obs sin n h ahdlnsrpeettesco nl htwsconsidered was that angle sector the represent lines dashed the and , with , 2 k i V of + = r α where naglrsco ln h ieai ao axis major kinematic within the pixels along the to curves sector rotation associated angular the dispersions an of strong points avoid curves. the to observed rotational order the of In with points average the this on to bars distance associated indi- same axis, dispersion major the the the cating at along centre are kinematic that the from pixels the of velocity observations. FP our with obtained was the to corresponds ρ quantities: the aacb bandwt h cnigF interferometer, FP scanning the with obtained cube data k and h DOwsfwr vrgstemeasured the averages software ADHOCw The k hrgo nteglx ntrso observable of terms in galaxy the on region th R φ k k and fthe of θ V k Θ r ie ntrso h coordinates the of terms in given are ( k R hglx eino h k which sky the on region galaxy th k k hpxlo h eoiyfil that field velocity the of pixel th = ) V cos obs k θ µ k − mg safaeof frame a as image m sin V sys i , (1) © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 twihtesatri oaincrei minimized, is curve rotation in are centre scatter photometric the the which around at position the de- 4. centre, as Figure kinematic rived of the panel of left coordinates sec- physical upper The angular the in an marked as within galaxy 30 field with of velocity obtained tor was the 4 in Figure of pixels panel right upper the the curves. in rotation points symmetric of scattered instead in curves rotation result would in values obtained changes these observations; we our which from curves values with rotation listed the values The those galaxy. to each correspond of curve rotation the centre. kinematic own its agreement of in velocity is radial galaxy the that each with considered of velocity we Finally, systemic the images. ellipses these isophotal on the traced from galaxies 2.22 the of the inclination to IRAF of task apparent with by plane would puted sky it the on inclination lengths has axis ellipse its galaxy an to panels each like due left that look disc, assuming in well-defined Then, shown a as 4. 2010) 2004, Figure al. al. of et et Repetto Fuentes-Carrera 2007; (e.g. considered were S & ROSADO SARDANETA, 78 eemndta h eicnrcdsac othis to distance heliocentric the that determined of inside i curve sym- scattered most radius least the the and us smooth give metric, the that software, cen- parameters ADHOCw photometric Using kinematic the arcsec. 0.4 matches within rotation galaxy tre the this compute in to curve used centre kinematic The OAINCREPRMTR N ASRNEO AHGLX NTENC69 PAIR 6090 NGC THE IN GALAXY EACH OF RANGE MASS AND PARAMETERS CURVE ROTATION 13 = h oaincreo G 00N rsne in presented NE 6090 NGC of curve rotation The calculate to used parameters the contains 3 Table α aaee G 00N G 00SW 6090 NGC NE 6090 NGC (J2000) Coordinates Parameter itne(p)18118 118 s (km velocity rotation Max. s (km velocity Systemic (Mpc) Distance ais(p)322.6 4.5 3.2 5.6 ( Mass (kpc) Radius (arcsec) Radius ( Inclination Kinematic J2000 . 9 ◦ ◦ i 16 = rudteknmtcmjrai fthe of axis major kinematic the around ± R M cos = a

0 and 5 = h . 0.76 ) ,and 5, A P 11 ◦ − 13.9 ) m 1 b . rscare arcsec 6 ( o t nlnto a ecom- be can inclination its so, ; ( 40 b/a ◦ 150 ) . 84 .W ple the applied We ). V s µ sys , mg oetmt the estimate to image m δ − J2000 80k s km 8880 = 1 808890 8880 ) − A P +52 = 1 130 ) 150 = ◦ 27 − ellipse 1 0 We . ◦ 26 ± 00 . 94. δ AL 3 TABLE 3, α +52 = × 16 = 10 10 h ◦ l ntevlct edwti naglrsco of pix- sector with angular an obtained within was field velocity 60 4) the Figure in els of panel right centre. kinematic its from south the rotational the to maximum in Its of while reaches away. side velocity moves us, north gas approaches the the gas south in of the north i.e. NE the 6090 blue-shifted, NGC that is shows galaxy (Hubble curve law the rotation Hubble The the through 1936). Mpc 118 is galaxy h hsclcodntso h ieai eteare centre kinematic α the of coordinates physical The s ailvlct au,adtepxla h south- the at pixel the rotation low- and the the value, with velocity in point radial the velocities est considered radial hence, and the frame- curve draw the considered the to centre field; work kinematic velocity the the of on pixels pixel dispersion two com- high only velocities using a radial puted the with of average side the receding to associated the on point centre. a kinematic its from north the the to arcsec as is 2 well ve-at SW 6090 NGC rotational as of maximum blue-shifted locity The is galaxy. side northeastern is north shows SW SW 6090 the 6090 NGC NGC of that curve of rotation The distance Mpc. 118 heliocentric obtained have the we NE, that 6090 NGC for distance centric V case, radius this of in inside were, curve parameters scatter rotation and the kinematic asymmetry in The the significantly cen- reduce arcsec. photometric that the 0.77 matches within rotation galaxy tre the this compute in to curve used centre kinematic The o1.26 to 11 ± 27 ± ± J2000 sys ANCHEZ-CRUCES ◦ m ´ . 64.8 0.5 132 5 26 3 h oaincreo G 00S (bottom SW 6090 NGC of curve rotation The ntertto uv fNC69 Wteeis there SW 6090 NGC of curve rotation the In 0 40 rudteknmtcmjrai ftegalaxy. the of axis major kinematic the around 80k s km 8890 = 26 . 84 × 00 16 = . 94 10 s 10 h 11 V m − Θ A P 1 40 uta ecluae h helio- the calculated we as Just . max . 42 26 = 0.63 s 130 = , δ α δ V +52 = ◦ × J2000 Θ 16 = ± 10 max ± 3, 10 ms km 5 i h ◦ +52 = o1.05 to 11 64 = 132 = ± ± ± 27 m 0.5 3 5 R 0 40 − . 8 1 22 4 = . ◦ 42 × ◦ ± t3arcsec 3 at 00 ± . 27 10 21 s . ms km 5 0 arcsec 5 0 10 . 22 ,and 5, 00 . 21. − 1 © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 ete hn nissronig h eoiydis- is velocity it the where surroundings is its range persion in Then, centre. a onierto eetdwt UAadmainly and PUMA with detected ratio, sig- noise low noticed to a nal with were profiles velocity profiles radial double broader through galaxies, both tween maximum s dispersion km 85 galaxies. velocity the is the between SW, 6090 bridge NGC a In like look might what s km from 75 59 gradually to increases dispersion ≈ velocity NE 6090 NGC with the In 6090 dis- overlaid. NGC image 5 of NICMOS/HST Figure map the dispersion system. velocity galaxy the plays the of map of dispersion profile velocity H the (FWHM) to the maximum fitted half functions Gaussian at of width full the Through this of curve rotation the of south. view the only toward better point galaxy this a sys- use get entire to decided the to we of that, field Despite radial velocity tem. highest the the of with value centre velocity kinematic the of west online. viewed be galaxy. can each figure of color centre photometric The the 6090 the NGC represent using on ‘+’ centred 2.22 bols obtained view NICMOS/HST of the map field on arcsec superposed dispersion 22 a Velocity in PUMA 5. Fig. 45 ntenrhsd fteglx ytmadbe- and system galaxy the of side north the In − α − − 5k s km 55 iei ahpxlw bandtevelocity the obtained we pixel each in line 1 6k s km 66 − nisnrhwsensia r erto near arm spiral north-western its in 1 4.3 ≈ ett h oiino t photometric its of position the to next 9k s km 69 eoiyDseso Field Dispersion Velocity . − 1 − ≈ 1 nteesensd ftegalaxy, the of side eastern the in 0k s km 40 ntecnr,adte pto up then and centre, the in − 1 . − 1 nraigt h north, the to increasing H α IEAISO P 8 NC69)79 6090) (NGC 486 KPG OF KINEMATICS µ mg.Sym- image. m o xswl elwro h ersd Bne & the (Binney in galaxy side each mi- near for way, apparent the this on its In lower the along 1987). be Tremaine of distance will brightness given axis surface nor a the at then bulge pass- it, starlight the through dusty, of is ing fraction disc significant inner a the absorbs more if it that declines means one This profile the smoothly. surface-brightness being side out- the far centre the nu- where the axis, minor the from the unequally of along of ward off brightness criterion falls apparent region gradient the clear the followed (1985): we Pasha 6090 NGC trail, in galaxies or the closer if lead is determine to galaxy Thus, the of us. trails, to side or which leads determine must galaxy we given disks. a thin whether in determine spirals To trailing and leading themselves distinguish by cannot measurements Radial-velocity work. this in them consider not to the do signal not of we low do ratio their computation noise given they the Moreover, that in curves. point so rotation ordered any galaxy, the at each contribute of of outside with field are pixels velocity interac- profiles Those an velocity galaxies. has double its disper- 6090 between NGC velocity bridge that the tion indicates of field feature early- sion This in shocks mergers. of consequence stage a profiles as broader interpreted (2017) Those al. and et Cortijo-Ferrero by zone. detected already bridge were the in located online. viewed The be analysis. can kinematic figure our one. of color from eastern orientation derived 3D the NE schematic is 6090 a NGC 6090 the shows NGC panel of be top-right near- observer would The the the galaxy Therefore, to the side smoothly. est of of more decreases side map that far one of continuum the criterion gradient (1985), the galac- the Pasha the Following of on centre. centred phometric axis profile minor tic the Intensity along NE 6090 NGC 6. Fig. 4.4 h oainSneof Sense Rotation The . G 00NE 6090 NGC © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 is R is ro- maximum velocity the curve, tation rotation SW 6090 NGC the is is obtained range galaxy this of of velocity V rotation maximum respectively.the halo, spherical a massive by a dominated by being or disc galaxy flat the to correspond (0 ues range coefficient the the in constant and a constant gravitational the of a range is galax- as the spiral galaxy in the the of is mass or ies the disc Thus, flat system. a of spherical as mass galaxy the evaluate the to galaxies: cases extreme two considers calculating in velocity consists tion approach This mass the 2010). Repetto 2007; al. al. et et Fuentes-Carrera 1992; Am- al. (e.g. et galaxies been ram the of pairs has studying using as when before calculated (1983), done Lequeux was by system described approach galaxy 6090 NGC each of the mass the in for values possible of range A arms. spiral of 2.22 structure of the image mark the clearly addition, not its In along emission axis. continuum minor low with the pixels to of due which sense, number rotation through its result determine might accurate we an obtain to possible trailing a in- in can rotating we arms its 1), direction. has of Figure galaxy structure of this arms that panel fer the right (see trace us galaxy which availing this lanes and, dust blue-shifted gas the is the of side that northern indicates the curve on rotation consid- Then, the galaxy. that the S ob- of ering & the side ROSADO to eastern SARDANETA, the nearest is side server the that in photomet- indicates profile 2 minor This Figure its (see from axis continuum ric the of profile one. each of sense rotation the order in determine axis to minor their continuum along the obtained of was emission profile intensity the pair 6090 NGC 80 ohmse hnbt aaisaedmntdby is dominated halo are spherical galaxies massive both a when masses both n hnbt aaisaedmntdb a disc, flat by dominated is mass are the galaxies both when and NE M .MS SIAE SN DYNAMICAL USING ESTIMATES MASS 5. 1 = R hs rmteNC69 Ertto curve, rotation NE 6090 NGC the from Thus, not was it SW 6090 NGC for hand, other the On intensity the extracted we NE, 6090 NGC For SW 3 ms km 130 = 2 = . 7ace.Frti aaytems range mass the galaxy this For arcsec. 97 1 = M . ( M 7ace.Frti aaytemass the galaxy this For arcsec. 47 . R 05 V flat pt eti aisweeterota- the where radius certain a to up ) ( κ R × − a enmaue.Temethod The measured. been has ) 1 = M 1 V 10 SW M NE hc srahda radius a at reached is which ANALYSIS . 10 39 ( R M § 1 = . × 3 ms km 132 = 6 = )

) ssoni iue6. Figure in shown as 3), , 10 M hrfr,tesmof sum the Therefore, . 1 . 26 . sph 10 κRV ) hs iiigval- limiting whose 0), κ M 2 = ×

2 ( . 10 R . − 31 10 ) 1 /G × M ece at reached where ,

10 µ From . does m 10 M κ

G is , etdo h k plane, line sky the the in on jected projected velocity sight, the of of difference velocity become the a they quantities, with observable orbit into transformed circular a components in V move the pair that the assuming This of of components. consists the of method motion orbital by relative from proposed the mass method the the calculates is which (1987), galaxies Karachentsev of pair a of value spherical a by dominated are halo. galaxies case both disc the which dismiss flat of in to dynamics necessary a be the by would on encounter dominated of this study possi- are further state is a they active but it that individually, the 6090 infer NGC to in to due galaxies ble Thus, the of 2010). interaction 1987; al. Tremaine & et Binney Mo (e.g. merge to for galaxies energy and the orbital friction sufficient dynamical to remove until interactions expected halo tidal are common galaxies a the in form Then, orbit to halo. merge common may a halos extended their encounter, hrfr,tettlms ftepi is: pair the of mass Karachentsev total motion, factor the circular projection Therefore, For the galax- obtained between both pair. (1987) angle connecting the line the of the Ω and ies and sight sky, of the line the of plane the and where rto ewe h ulu fec aay For have, galaxy. we each 6090 NGC of system nucleus and the the galaxies, between aration the of ties where is separation plane the sky and the sight of on line projected the on projected 1 and ity = plane Ω in sky results which the galaxies, on projected the nuclei D connecting the line of the tance sin and = Ω sight is pair of line the plane of tween without orbital inclination method the an this that has assumed with we obtain generality, mass of to of loss order limit in upper function, the sinusoidal a on depend where suigacrua ri,tettlms ol be: would mass total the orbit, circular a Assuming 12 ANCHEZ-CRUCES ´ 133 = eodidpnetwyo bann h mass the obtaining of way independent second A an have mass equal roughly of galaxies two When n pta separation spatial a and G i V steagebtentepaeo h orbit the of plane the between angle the is . 12 y p stesz fteln oncigthe connecting line the of size the is kpc 1 stegaiainlcntn.As constant. gravitational the is = stedffrnebtenteveloci- the between difference the is V − 12 M 1 ( sin orbital L/D M i o ,adtesprto pro- separation the and Ω, cos = i ,where ), = 90 = 3 32 X π 3 32 π r y X = ◦ r G V r hn h nl be- angle the Then, . stepoetdsep- projected the is When . r L . y 2 76 (1 G , 4 = 12 ≈ ◦ − V hs h veloc- the Thus, . 2 V 12 , sin . p stedis- the is kpc 1 12 V h 2 0k s km 10 = η 12 and i i sin and 3 = y 2 X and Ω) π/ r ≈ 1 are (2) (3) 32. / − X r 2 1 . , © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 and M iiulmse fteglxe nteAtna are Antennae the in in- 2 galaxies the approximately the that of found of masses (1992) mass al. dividual et the Amram using measure galaxies, to Finally, the method (1983) profiles. Lequeux detected velocity the a no double of were with there behaviour pixels Additionally, the show disc. none galaxies rotating system; component the throughout its ordered of not is 2.2 field ity at unam- com- observations matched its with nuclei from Antennae biguously farthest the part Then, its panion. toward emissions the grow that to but tend emission, continuum its H with at emitting gas ionized nae, 6090 NGC for the done paper. have of this we analysis in as Antennae, kinematic the a of performed disc (1992) Amram Therefore, al. zone. et central H the at in in emitting detected gas only i.e. ionized tails, systems of tidal galaxy their emission both sys- in was galaxy detected Antennae, neither hydrogen the In ionized and (1992). 6090 been NGC al. tem, has et Amram Antennae another by the with FP obtained pair observations through galaxy studied the H of The matics PUMA. studied interferometer, we Fabry-Perot galaxies, own H kine- their produced the of studying systems interaction of the both goal by between the similarities With matic Bryant Maz- 1999). 1999; 1991; al. Scoville (e.g. et al. & Dinshaw Antennae) et 1993; Boroson Martin (the & 1972; zarella 4038/39 Toomre NGC & described to Toomre been (tidal has similar system antennas galaxy as curved this two that so with tails), system dou- a nuclei as appears ble 6090 NGC wavelengths, optical At velocity projected the that fact the the to of difference value due low by individ- is this proposed that the mass think method We of the (1983). with sum Lequeux obtained the masses than ual smaller magnitude h Icniummxm eotdb odne al. et Condon by nu- reported the maxima continuum of HI 2.22 the positions lagging at The is reported direction. clei population opposite stellar the com- old in its galaxy, the to each near while within situated panion, is but gas hydrogen continuum; ionized the the of H that in to emitting gas ionized of orbital ma ta.(92 eotdta nteAnten- the in that reported (1992) al. et Amram o G 00 in 6090, NGC For r α 4 = ieaiso G 00uigtescanning the using 6090 NGC of kinematics 3 = V 12 . . p.Teeoe h ria asis mass orbital the Therefore, kpc. 1 23 sqiesmall. quite is × × .DISCUSSION 6. 10 10 8 10 M § µ yDnhwe l (1999), al. et Dinshaw by m entdta h intensity the that noted we 3 M

hc stoodr of orders two is which ,

. α α slwrwt respect with lower is sdfiin compared deficient is H α µ IEAISO P 8 NC69)81 6090) (NGC 486 KPG OF KINEMATICS .Teveloc- The m. α α kine- was h eoiydseso aiu.Temxmmof maximum 2.22 The the maximum. dispersion velocity the δ +52 is monochro- continuum the Thus, of δ position is north. maximum the emission the matic maximum SW, 6090 the in NGC while is for south, emission the max- to monochromatic photometric located the that the is so imum towards south, hydrogen the than presents ionized north galaxy of This emissions NE. 6090 NGC greater in ionized those the as tion of H in observations emitting our gas emis- from monochromatic derived the and sions continuum the of ima and literature minimal. the are in results reported our the galaxy of this position of we the nucleus 7 between Figure differences the In that arcsec). show 0.4 (within centre the match kinematic and coincide completely ob- almost PUMA servations the of continuum and monochromatic the 7. marked Figure are in paper image NICMOS/HST this the in on obtained H we continuum that and maxima monochromatic the and (1990), online. viewed be can figure color H image the ( this (O), emissions In continuum maximum the the of 6090. of NGC positions at the marked centered have 2.22 arcsec we at 16 image of NICMOS/HST view 7. Fig. 4 J2000 J2000 ,terdocnium()adteifae ( infrared the and (X) continuum radio the ), oee,frteglx G 00S h max- the SW 6090 NGC galaxy the for However, of maxima the that found we NE, 6090 NGC For ◦ 27 H α +52 = 0 22 +52 = µ msini at is emission m 00 . hc ac h ieai eteand centre kinematic the match which , α ◦ J2000 27 ◦ 27 α 0 23 0 r o eryi h aeposi- same the in nearly not are cont 23 00 . 00 . Dnhwe l 99,and 1999), al. et (Dinshaw 16 = n h aiu fthe of maximum the and , α α α h J2000 oohoai emission monochromatic 11 J2000 m H 40 α 16 = . 16 = µ 4 fafil of field a of m s , δ h h J2000 11 11 2 m m .The ). cont 40 40 . . 3 3 = s s α , , © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 oiylre hntedseso rrsda velocity residual or ve- dispersion rotational the than maximum system. larger have 6090 locity NGC curves the rota- in rotation the galaxy The compute each to of curves us tion allowed which fields locity in 4 is nuclei is its 6090 between NGC distance system the mem- galaxy Mpc, 118 two the of the 7 distance of is average nuclei 6090 NGC the of of bers determined separation we galaxy, the southwest that the H of the nucleus of the SW. maximum 6090 NGC the of taking Thus, maximum detected and dispersion centre we velocity kinematic where the the near south- maximum, peak, continuum is infrared the maximum the continuum of the ward of that position obtained the (2017) al. et Cortijo-Ferrero However, their 7100 2.22 to of of 3700 knot lines from range absorption the main in observations the (2017), that al. argued et who Cortijo-Ferrero by pos- supported This is itself. sibility component a the it is for maximum galaxy Therefore, infrared southwestern H the 6090. that redshifted NGC concluded of be the may observations of our not maximum of could the line star as field a detected of field be a emission galaxy; be the could However, this peak star. infrared of the that radio-continuum proposed they the 2.22 of the in maximum point brightest the 1990). at al. et Condon is 1987; continuum radio 16 maximum the S & ROSADO SARDANETA, 82 h § ASSO H AAYSSE G 00FUDI H IEAUEA DIFFERENT AT LITERATURE THE IN FOUND 6090 NGC SYSTEM GALAXY THE OF MASSES 11 eadn h eoiyfil fNC69,w said we 6090, NGC of field velocity the Regarding of position the compared (1999) al. et Dinshaw . htti aaysse a w ree ve- ordered two has system galaxy this that 4.1 m 40 umle l 18)H 3.9 5.02 4.2 H Mass MIR HI MIR 3650 the of Phase H H work This (2017) al. et Cortijo-Ferrero (2017) al. et Cortijo-Ferrero (2016a) al. et Chisholm (1987) al. et Hummel (1999) Scoville & Bryant (1991) al. et Sanders Author . 8 s µ , aetesm esita h galaxy. the as redshift same the have m δ J2000 A EEGH OPRDWT H NSFUDI HSWORK THIS IN FOUND ONES THE WITH COMPARED WAVELENGTHS +52 = . 1ace.Asmn htthe that Assuming arcsec. 11 ◦ 27 0 27 µ mg ihthe with image m 00 . Hme tal. et (Hummel α otnu as continuum α J2000 tthe at A ˚ . kpc. 1 AL 4 TABLE = α H H Mosre [ observed IM oorrsls h ag ftesmo indepen- rota- of the sum from the paper this of in range estimated The masses dent results. our compared wavelengths to the different for at literature system the 6090 in NGC reported masses the of values merger. a to previous stage interaction stage an sys- advanced in both are less although tems a Antennae, the in than system interaction a of conclude is inter- to 6090 NGC us an allow that signals galaxies, that between field bridge behaviour action dispersion the velocity and its contin- maps, of fields, monochromatic velocity and dis- ordered have uum two we that its In features about the interaction. cussed 6090, NGC of of the stage case up advanced the make an that in galaxies is the Antennae of encounter the optical that at and paper) (2017). al. al. their et et of Cortijo-Ferrero Dinshaw by 2 wavelengths by figure infrared (see the in (1999) in structure made bar a galaxy of this the presence confirmed the we about NE, 6090 assumption NGC in detected motions isove- we non-circular that the asymmetric and the curves, contour with locities observations, our from velocities. rotational maxima values their these than even less but veloc- were disc, maximum the their outside reach dispersion ity galaxies Both disc. the range the in maximum dispersion a locity has SW velocity 6090 NGC rotational meanwhile disc; range its rota- the in maximum is a dispersion has velocity galaxy tional northeast the fields: α α α H u a disc flat sum u p halo sph sum orbital ANCHEZ-CRUCES ´ − (dyn) 2 eadn h asvle,Tbe4cnan the contains 4 Table values, mass the Regarding concluded (1992) al. et Amram paper, their In obtained map continumm the with Furthermore, (gas) 2 6950 2 6.8 A ˚ V NE V SW 3 ms km 130 = 3 ms km 132 = ≈ 45 ≈ − 40 M − 6k s km 66 1 −

0.032 2.31 2.29 0.46 1.39 1.4 × n t velocity its and − 9k s km 69 1 10 ihisve- its with , 10 − 1 ] − nieof inside 1 inside © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 utfiihn nitrcinwt h eta molecu- In central were gas. the lar clouds with gas interaction NE an molecular 6090 finishing NGC of the just the trailing, if arm arms that its spiral from inferred had northwestern They offset the NE. 6090 NGC regions to nuclei in galactic occurring starbursts the and NE. 6090 tails NGC nortweast- of tidal the arm by two ern defined the well them, note similar between have We bridge which 6090, NGC values. happen- of mass is galaxies phenomenon the This to ing 2002). al. et two (Combes into drawn are bridge, arms tennae a external form two to similar, the up or join while equal arms spiral are internal two galaxies masses the interacting the two when the the if galaxies; of arms disc four are the of companions formation of two the symmetry an- allows the the action form general, tidal that in tails Therefore, tidal the tennae. long always two obtain feature: They same star merger. of the formation during the clusters or 2008, morphology al. its et fea- either Renaud 2015), 1972; 2010; different Toomre al. et & Teyssier Toomre model 1988; (e.g. Barnes Antennae to the of conditions tures initial similar companion. its of around move- SW 6090 the NGC of of conse- assumptions ment be geometrical can our mass an to orbital of quence the difference in The magnitude reliable. of we are order Hence, work ob- we this halo. that in spherical parameters tained kinematic a the or that argue disc can flat dom- and is a (1991) galaxy by each al. if inated both et (1999), Scoville Sanders & with by Bryant coincide determined also value mass-to-light They the the wavelengths. from other acquired at magni- ratio masses of the order same as the tude of is velocity rotation mum smaller Scov- & magnitude (1999). Bryant by ille of estimated mass order the dynamic the than an than smaller and magnitude values, of former orders Karachentsev two by is cal- proposed (1987) system method 6090 NGC the ra- the with mass-to-light which of culated mass the 1991), the of However, al. means tio. et by 2017) determined (Martin al. were continuum et Cortijo-Ferrero radio 1999; 2016a; and Scoville al. & in- Bryant et the 1991; in Chisholm al. authors et other (Sanders magnitude by frared of estimated order masses same the the as of method is the (1983) with Lequeux obtained of galaxy each of curves tion ial,Sgie l 20)osre young observed (2004) al. et Sugai Finally, assumed have simulations numerical the of Most maxi- the from computed masses the of sum The hc eanfroeo w ilo years billion two or one for remain which § . esoe httesia rsi the in arms spiral the that showed we 4.4 H α IEAISO P 8 NC69)83 6090) (NGC 486 KPG OF KINEMATICS an- h ieo h msinae htwsdetected. was that area emission the to of due size galaxy star. the southwestern morphologi- the field the of study a characteristics to be cal able cannot not were therefore we However, and galaxy, the of of H 2.22 maximum at the emitting which gas Furthermore, wavelengths, ionized infrared inconsistent. and were radio those from of different location reported a in is galaxy southwest di- trailing a in arms rotate the galaxy that conclude rection. NE 6090 stellar NGC to a possible the has also of was galaxy It field axis, this minor velocity that bar. the the suggests to again bar; respect which stellar with symmetry contin- a no the of shows of signs isophotes show the galaxy, uum characteristics this specific In observe therein. to galaxy northeast effects. projection this to that the due conclude from We is magnitude difference masses. individual of 6090, NGC the orders of of two sum mass by orbital differs the which ad- obtained In we wavelengths. dition, different the with for obtained ratio with literature, mass-to-light consistent the in indi- is found the calculated masses of the we sum that The masses system. galaxy vidual and the galaxy, of each mass of the mass the velocity, rotation mum pair. curve the rotation of the galaxy each computed of contour we isovelocity which ordered from 6090 NGC curves with of regions field two velocity shows The maps. dispersion ity at emitting obtained H of gas we (ionized area observations emission monochromatic central our the Through the in system. solely the detected This was the PUMA. emission with interferometer, out the Fabry-Perot carried of scanning 486) (KPG observations H 6090 NGC our at galaxies present emitting we gas ionized paper this In interaction. the during pressure have ram by could which formed their SW, been H 6090 of NGC high 1 in of Figure dispersion region locity a (see with band coincides UV which the paper), Chisholm in by north- (2016b) detected the al. SW at 6090 et NGC outflow of the side be eastern arms could trailing NE 6090 the NGC of of the- consequence this likely favoring Another ory. trailing, are galaxy north-eastern α ,tecnium h eoiyfil n h veloc- the and field velocity the continuum, the ), ecnlddta h htmti eteo the of centre photometric the that concluded We the in detected was emission enough addition, In maxi- the obtained we curves rotation the Using µ onie ofimn htti nti part is knot this that confirming coincide, m .CONCLUSIONS 7. α α n h aiu fthe of maximum the and fteioae arof pair isolated the of α ve- © Copyright 2020: Instituto de Astronomía, Universidad Nacional Autónoma de México DOI: https://doi.org/10.22201/ia.01851101p.2020.56.01.09 rat .M cvle .Z 99 J 1,2632 117, AJ, 1999, ApJ, Z. 2018, N. I. Scoville, C´ardenas-Mart´ınez, Fuentes-Carrera, & & M. dynamics, N. 1825 P. 86, Bryant, Galactic AJ, 1981, 1987, A. Bosma, S. 705 Tremaine, 30, & ARA&A, 1992, J. L. C., Hernquist, Binney, & 699 E. Oliveira, 331, J. ApJ, Barnes, 1988, de E. 1 J. 14, Barnes, Mendes ApJS, 1966, H. H., Arp, Plana, P., Coarer, Le & Amram, J., al. Boulesteix, et M., J., Marcelin, R. P., Amram, Laureijs, U., Klaas, A., J. Acosta-Pulido, institutions. these form of digital permission compressed the present with were the plates into The Telescope. processed Schmidt UK the Moun- and Palomar tain on Telescope Schmidt us- Oschin these obtained the data of ing photographic images on based The are Gov- surveys W-2166. U.S. NAG under Grant Institute ernment Science Telescope Space obtain observations. to us our helping and facilitating for OAN-SPM at M´exico.California, M´artir Baja Pedro (OAN-SPM), Astron´omico San Na- Sierra Observatorio on cional the interferom- at Fabry-Perot PUMA, scanning eter, the with formed Technol- through and paper this CY-109919. Science financing project for for (CONACYT) Council ogy National ican IN109919. UNAM-DGAPA-PAPIIT gram in galaxies the of that than a Antennae. in earlier the are merger of galaxies up of analysis these stage make that kinematic concluded that the we the 6090 galaxies Through NGC to the due systems. of mainly these con- interaction are to of S differences us wavelengthstage & their allowed ROSADO SARDANETA, same the that This clude the discussed instruments. have at similar we with made systems observations paper galaxy as this from these defined between In differences been Antennae kinematic has the merger. it to also a similar while is 4038/39), system (NGC the 6090, NGC 84 6,141 868, Press University Princeton : N.J. Princeton, 865 402, A&A, 2003, J. Boulesteix, & C., Balkowski, 106 266, A&A, 1992, E. 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