PoS(Seyfert 2012)009 http://pos.sissa.it/ 4 square arcsec. × , [Fe II]) and analyze these to disentangle 2 ,H γ , Br α † ∗ ´ c is member of the International Max Planck Research School (IMPRS) for Astronomy and Astro- ´ c [email protected] [email protected] [email protected] [email protected] [email protected] Speaker. Semir Smaji We detect several emission lines ([Si VI], Pa The NIR is less influenced by dust extinctionthrough than optical dusty light. regions. This enables In us addition, to look itcombination to is of an sensitive extent NIR to imaging the and mass-dominating spectroscopygives stellar of us population. the the The VLT opportunity integral field tostellar spectrograph analyze SINFONI population several and emission ionization and mechanisms absorption over lines a and field to of investigate view the (FOV) of 4 the ionization mechanisms and theI, kinematics CO(6-3) of and the CO(2-0) gas. and thesynthesis. We large We use wavelength fit the range a stellar, of absorption dust H+K-band and features forto power-law of contribution a the together Si thorough with H+K-band an continuum emission. extinction component Theand extinction result information presents over regions the dominated full FOV. by the different contributors ∗ † Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

physics at the MPIfR and the Universities of Bonn and Cologne. Nuclei of Seyfert and QSOsNovember - 6-8, Central 2012 engine & conditionsMax-Planck-Insitut of für Radioastronomie formation (MPIfR), Bonn, Germany Monica Valencia-S. I. Physikalisches Institut, Universität zu Köln,Max-Planck-Insitut Germany für Radioastronomie (MPIfR), Bonn, Germany E-mail: Andreas Eckart I. Physikalisches Institut, Universität zu Köln,Max-Planck-Insitut Germany für Radioastronomie (MPIfR), Bonn, Germany E-mail: Jens Zuther I. Physikalisches Institut, Universität zu Köln,E-mail: Germany Semir Smaji Sebastian Fischer I. Physikalisches Institut, Universität zu Köln,E-mail: Germany The central kpc of edge-on AGN I. Physikalisches Institut, Universität zu Köln,Max-Planck-Insitut Germany für Radioastronomie (MPIfR), Bonn, Germany E-mail: PoS(Seyfert 2012)009 ´ c ]. 6 Semir Smaji 4 square arcsec centered on the nucleus. The × 2 ]. 11 ). Observations of this cover a wavelength range ]. This evolutionary component is supposed to bring together 1(b) ]. There are attempts to extend the UM by adding an evolu- 5 4 ]. Polarized observations were not able to detect broad emission lines 13 ]. We have spectral and spatial information over the H+K-band ranging from ]. 12 10 m at a field of view (FOV) of 4 µ ]. 3 ]. In addition, Seyfert 2 galaxies show very disturbed morphologies similar to HII and 9 , ] and references therein) and most likely every galaxy harbors a massive black hole (MBH), 8 m to 2.4 2 µ We will present two individual results from our study of a nearby Seyfert 2 sample selected The data for this work was obtained with SINFONI the Very Large Telescope (VLT) integral NGC 7172 is an edge-on early-type at a of about 0.0087 and is a member The Unified Model (UM) explains the different types of active galaxies with regard to their Most galaxies with a significant bulge component harbor a super massive black hole (SMBH) ]. The last problem is supported by the finding that Seyfert 2 galaxies tend to be edge-on ori- 7 , 1 from radio over MIR, NIRX-ray and source optical H2158-321 to [ X-ray observations. NGC 7172 was identified with the from the Veron-Cetty & Veron catalogue [ field spectrograph [ ented [ starburst galaxies [ 1.1 The Data 1.45 of the Hickson Compactregion Group from 90 east (HCG90). to west It (see has Fig. a prominent dustlane crossing its nuclear Another possible bias is thathost of galaxy, Seyfert not 2 the galaxies dustyhence beeing ’torus’, classifying biased provides these by the galaxies Seyfert wrongly dust as 1 screenhelp Seyfert galaxies that to 2 where look galaxies. prevents the "behind" us Observations of the from polarized toruswill seeing light usually by the can not detecting BLR work the with scattered dust andon obscuration reflected large by broad galactic the emission scales host lines. and because[ far This this away dust from obscuration the often nucleus occurs where the broad emission lines are excited two galaxies discussed here are NGCsample. 7172 and NGC 289 both Seyfert 2 galaxies chosen from our orientation towards the observer [ tionary component to the scenario [ the orientation phenomena of the UM,line Seyfert 1 region and (NHBLR) Seyfert galaxies 2 galaxies, andlyzing with narrow the the extending line non-hidden models broad Seyfert statistically 1for there (NLS1) a is galaxies. biased the sample important However, are issue whencombined NLS1 of easily ana- galaxies biases. into that A one show class topical several of different example objects characteristics seperate which from cannot Seyfert be 1 galaxies, see more on this in [ (e.g., [ i.e. the black hole atactive the galaxies center where of the the SMBH interacts Milky heavily Way.ways, with The on the evolution the host of galaxy. one SMBHs This hand interaction can gas works(e.g., be from both nuclear studied the bars best inter and in stellar spirals) mediumphotons (ISM) and into feeds on the the the ISM central other via SMBH outflows hand via (e.g.,is the inflow jets not active and fully SMBH shocks). understood, blows In out i.e. which gas wayin the these and the effect two ISM radiates of phenomena [ outflows work which can disrupt but also trigger star formation The central kpc of edge-on AGN 1. Introduction PoS(Seyfert 2012)009 ´ c ]. 17 Semir Smaji ). A several 1(a) m on). All these features µ ] (see also Fig. 16 (b) NGC 7172 3 ]. 15 shows nuclear spectra of our objects overlayed with the different 2 ). 1 (a) NGC 289 The images were taken with the HST F606W filter. Both images were overscaled to show the full In the following we show that, although the nuclear regions of these galaxies look similar, a The continuum of galaxies tells us a lot about their properties. From color-color diagrams we We use our own idl routine with an AMOEBA minimization to get information on the different These two galaxies show several similarities. Both are interacting, NGC 7172 as part of NGC 289 is a at a redshift of 0.0054 interacting with its dwarf companion ]. However, short term variability measured in the X-ray suggests that there is a BLR around 14 components. Both spectra, the very redof spectrum of NGC NGC 289, 7172 and show the(e.g., flat stellar Si dominated residuals. I spectrum and NGC CO(6-3)) and 289 K-band shows (e.g., the strong CO stellar band absorption heads from features 2.29 in H-band closer and better resolved look shows significant differences. 2.1 Continuum Synthesis are able to determine theadditional amount spectral of information stellar we light can andwill do the give us a extinction more of sophisticated information our and about objects. the thorough composition continuum Since of synthesis we the that have light emittedemitting by components the that the dominate nuclear nuclear regions. region. Fora our stellar analysis we component fit a and (hot)spectra dust a of component, power-law our component objects. multiplied Figure by an extinction component to the million years old starburst is supposed to have occurred in the nuclear region of NGC 289 [ 2. Results HCG90 and NGC 289 withdust its patterns dwarf companion. close to From the opticalstarburst nuclear images (see regions both Fig. and galaxies both show strong galaxies do not show strong signs of an active The central kpc of edge-on AGN [ the active nucleus of NGC 7172 [ Figure 1: extent of the host galaxy. Inlinear both brightness images scale. the The detail details in show the our upper observations left FOV. corner shows the nuclear region using a Arp 1981. It has a dustlane crossing its red nuclear region [ PoS(Seyfert 2012)009 . ´ c λ 1 2 m, H µ Semir Smaji we determine 1.56 1 λ − m) and [Fe II] in the µ , [Fe II] γ , Br (b) NGC 7172 α . The extinction for NGC 7172 follows V 1.959, 2.12, 2.23 λ 2 m. Due to the detection of the [Si VI] coronal and a FWHM of 5700 km s µ line. The spectrum of NGC 7172 surprisingly 1 , a typical width for Seyfert 1 galaxies. With the − 1 γ 4 − of more than 11 in the central region. . This black hole mass is similar to other literature line is also detected. The full width at half maximum

V 1.962 erg s γ λ M 8 , which is situated in the band gap between and H- and 41 α 10 10 line we are able to determine a black hole mass of the SMBH × × α 1.0) =9.1 ± α Pa =(4.5 BH (a) NGC 289 ]. We also detect the narrow emission lines of Pa 21 , m and the coronal line [Si VI] µ 20 , The spectra are extracted from the nuclei of NGC 289 and NGC 7172. Overplotted is the contin- 19 The nuclear spectrum of NGC 289 shows several narrow emission lines. In particular strong ]. With a luminosity of L . Our extinction fit traces the dust clouds seen in the (HST) images 18 line we are sure that we are looking at the position of the SMBH. Because of the high ionization 1.959, 2.12 shows broad H-recombination lines. Pa H-band. We also detect a rather faint narrow Br [ K-band, is clearly visible. A fainter broad(FWHM) Br of both broad lines isluminosity about and 5700 the km FWHM s of the Pa 3 molecular hydrogen emission in the K-band (e.g., H The extinction values for NGCexactly 289 the range opaque up dustlane to and 1 reaches mag an A A 2.2 Line Emission The central kpc of edge-on AGN Figure 2: uum synthesis fit (green) andare the the components: residua. Note (blue), that power-law the (yellow), residuum dust of (red). NGC The 7172 is flat moved spectra fromare 0 flux fitted to well 5 for by displayingemission our reasons. is stellar coming template from takenstellar evolved from contribution stars, a is either red about from 70% supergiant. of AGBcomponent all stars which Hence, the makes or the emission up old in main 30% H+K-band. main of7172 continuum In shows the sequence a addition, emission stars. strong we and red fit an continuum The a almostthe emission power-law negligible which sublimation dust can temperature only component. of be NGC about attributedcontinuum to 1200K. emission very The on hot dust dust the close emission nucleus. to makesare The up filled stellar more up absorption features than and are diluted 80%eligible still by of for visible, less the the however, than strong they 20% dust of all emission.in the NGC continuum Due contribution. 7172 to However, the the and total strongnegligible NGC stellar contributions for dust 289 NGC component are 7172. stars in are The the extinction component same fit order worked of very well magnitude. as can The be power-law seen component in is figure a black hole mass ofvalues M [ PoS(Seyfert 2012)009 . ´ c α 4 from these ). We used ∗ Semir Smaji σ 2(a) lines is centered 2 (b) NGC 7172 ) and the LOSVD in the H- and (h) , 4(g) are slightly offset to the south-west. Pa ). The flux peak of the H ), the stellar LOSV and the stellar LOSVD. . An off nuclear spectrum shows the stellar α 2 2.1 4(c) 5 . The LOSV dispersion (LOSVD) does not show any 1 − 0.81 the main contribution of the stellar light comes from evolved 0.72 2.1 0.63 0.54 0.45 0.36 (a) NGC 289 0.27 m are also detected along the galactic plane (east-west direction). The line of sight 0.18 µ 0.09 . The images show the fitted extinction maps of NGC 289 and NGC 7172. Extinction values are V 2.12 emission origin from a starburst with an NLR origin if the emission is located close to the λ γ 2 As already seen in section equivalent width (EW) and H-band luminosity. But, one has to be careful as not to confuse γ and H velocity (LOSV) maps of theseshifted) two with lines velocities indicate of a up rotationspecific to increase from 150 or east km decrease (blue s which shifted) would be to indicative west of (red an outflow or an inner disks, see Fig. the Br nucleus. This is exactly the casea in the stellar nuclear population region synthesis. of From NGC 7172.about our the continuum Hence, scale we synthesis were of we not the were able total still to stellar able do emission to (section get information on the position of the SMBH, whereas [Si VI] and Pa 2.3 Stellar Content stars with typical absorptionstars features and (e.g., old stars CO(6-3),CO(2-0)). lookabsorption features very The in similar problem the with NIR. here respect ThereBr is to are still their that possibilities spectral AGB to energy identify distribution starburts in (SED) the and NIR, i.e. the K-band using the CO(6-3) andblue CO(2-0) absorption shift features. in Again the wethe east see emission and a lines red rotation but pattern similar. shift with At in the the same west. time we determine The the velocities stellar are dispersion not equal to the velocities of We show an example of aabsorption nuclear features spectrum that in figure are also visible in the NGC 289 nuclear spectrum (Fig. potential of more than 150accreting eV SMBH. for The [Si coronal VI] lineline this region region (NLR) line (CLR) and can BLR. is The only supposedsame occurrence be direction. of to excited a The be CLR by 8 situated is the cm sometimes between[Si VLA radiation connected VI] map the to from line shows an narrow an an indicating outflow in elongation a the into possible the outflow south-west (see similar Fig. to that of the Figure 3: given in A these features to determine the LOSV maps (see Fig. The central kpc of edge-on AGN PoS(Seyfert 2012)009 . ´ c 1 − Semir Smaji and we conclude

M 8 (c) SiVI flux 10 (f) SiVI LOSV (i) SiVI LOSVD × 1.0) ± . We can compare the upper limit of , the velocity maps are in units of kms =(4.5 1 1 − − BH m µ 2 − m LOSV µ 200 km s Wm 6 12 . ∼ narrow LOSV 16 2 − ∗ α λ 2 σ (h) CO(6-3) LOSV (b) Pa (e) H ]. The LOSVD is not corrected for instrumental broadening. m flux 1 µ 12 to our prior calculated BH mass of M . narrow flux 2

λ α 2 M 8 (g) CO(2-0) LOSV (a) Pa (d) H 10 The flux maps are shown in units of 10 × =4 ↓ We presented two similar ’looking’ galaxies that, at a closer look, are not that similar. NGC BH 3. Summary and Conclusions Figure 4: Subfigures taken from [ The central kpc of edge-on AGN features. The stellar dispersion enablesthe us to measured estimate stellar an velocity upper dispersion limitM of for the black hole massthat using these are in good agreement. PoS(Seyfert 2012)009 ´ c and α Semir Smaji ]. 1 7 ´ c, S., Fischer, S., Zuther, J., & Eckart, A. 2012, A&A, 544, A105 From this result we can conclude that Seyfert 2 galaxies are intrinsically the same as Seyfert recombination lines are a direct proof of a BLR and the strong hot dust in the center show γ [2] Ho, L. C. 2008, ARA&A, 46,[3] 475 Schawinski, K., Thomas, D., Sarzi, M.,[4] et al.Antonucci, 2007, R. MNRAS, 1993, 382, ARA&A, 1415 31, 473 [5] Zhang, E.-P., & Wang, J.-M. 2006, ApJ,[6] 653, 137 Valencia-S., M. et al., this proceedings [7] Antonucci, R. 2012, Astronomical and Astrophysical[8] Transactions, 27,Shen, 557 S., Shao, Z., & Gu,[9] M. 2010,Lagos, ApJ, C. 725, D. L210 P., Padilla, N. D., Strauss, M. A., Cora, S. A., & Hao, L. 2011, MNRAS, 414, 2148 [1] Smaji [10] Hunt, L. K., & Malkan, M.[11] A. 2004,Véron-Cetty, ApJ, M.-P., 616, & 707 Véron, P. 2006, A&A,[12] 455, 773 Eisenhauer, F., Abuter, R., Bickert, K., et[13] al. 2003,Marshall, SPIE, F. 4841, E., 1548 Boldt, E. A.,[14] Holt, S. S.,Lumsden, et S. al. L., 1979, Heisler, C. ApJS, A., 40,[15] Bailey, 657 J. A.,Guainazzi, Hough, M., J. Matt, H., G., & Antonelli, Young, L. S.[16] A., 2001, et MNRAS,Carollo, al. 327, C. 1998, 459 M., MNRAS, Stiavelli, 298, M., 824 Seigar, M., de Zeeuw, P. T., & Dejonghe, H. 2002, AJ, 123, 159 1 galaxies. The obscuration ofa NGC Seyfert 7172 2 by galaxy. the Still, dust the leadsobserver UM due to to proposes a the that misclassification obscuration Seyfert of of 1 the NGCthe nuclear and 7172 obscuration region Seyfert as takes by 2 place the galaxies in dusty the torus are galactic but differentlane in plane to crossing the due the case the to of the central NGC edge-on region 7172 viewing of anglewith a and the similar the galaxy. orientation thick The and dust amount question of thatare dust arises Seyfert that are is: 1 misclassified galaxies? Are as There Seyfert there 2 is otheris galaxies a galaxies not but bias actually clear of and Seyfert a 2 galaxies thoroughfrom by investigation orientation Seyfert in and 1 this dust galaxies field coverage. though is Only the needed then extent to models ensure that a want statistical to independence extendReferences the UM can be proved. that NGC 7172 is Seyfertstellar 1 velocity galaxy, dispersion according in our to FOV we thefor are UM. able NGC Using to 7172 determine the from two broad independent out BH emissionvalues. data. mass lines estimates Both We and estimates show the are that in theoptical, agreement NIR even with the is each polarized, far light. other more and For potent more with information in literature on discovering NGC the 7172 true see nature [ of AGN than the The central kpc of edge-on AGN 7172 and NGC 289characteristics are of inhabiting both a BLR, classified NGC 7172 asand does. broad NGC Seyfert H-recombination 7172 2 shows lines. a galaxies, very The redof red however, nuclear the spectrum spectrum as dusty originates NGC torial from structure 289 theBr which hot shows is dust no supposed of the to inner surround part an active SMBH. The broad Pa PoS(Seyfert 2012)009 ´ c Semir Smaji 8 The central kpc of edge-on AGN [17] Bendo, G. J., & Joseph, R.[18] D. 2004,Kim, AJ, D., 127, Im, 3338 M., & Kim,[19] M. 2010,Longo, ApJ, G., 724, Busarello, 386 G., Lorenz, H.,[20] Richter, G.,Awaki, & H., Zaggia, Murakami, S. H., 1994, Ogawa, A&A, Y., & 282,[21] Leighly, 418 K.Winter, M. L. 2006, M., ApJ, Mushotzky, 645, R. 928 F., Reynolds, C. S., & Tueller, J. 2009, ApJ, 690, 1322