PMAS-PPAK integral-field spectroscopy of nearby Seyfert and normal spiral galaxies I. The central kiloparsecs of NGC 4138 Bartakov´ a´ T.1, Jungwiert B.2,3,Sanchez´ S. F.4,5, Stoklasova´ I.2, Emsellem E.6, Ferruit P.7, Jahnke K.8, Mundell C.9, Tacconi-Garman L. E.6, Vergani D.10, Wisotzki L.11 1 Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Brno, Czech Republic; 2 Astronomical Institute, Academy of Science of the Czech Republic, Prague, Czech Republic; 3 Astronomical Institute of the Charles University in Prague, Czech Republic; 4 Centro de Estudios de F´ısica del Cosmos de Aragon´ (CEFCA), Teruel, Spain; 5 Centro Astronomico´ Hispano-Aleman,´ Calar Alto, Almer´ıa, Spain; 6 European Southern Observatory, Garching, Germany; 7 CRAL-Observatoire de Lyon, Saint-Genis-Laval, France; 8 Max-Planck-Institut fur Astronomie, Heidelberg, Germany; 9 Astrophysics Research Institute, Liverpool John Moores University, United Kingdom; 10 INAF-Osservatorio Astronomico di Bologna, Italy; 11 Astrophysical Institute Potsdam, Germany. email: [email protected] Project overview These peculiarities are suspected to be related to a minor merger, however they could also be related to a destroyed Ratio Ha/Hb |2.5/*| Ratio [SII]6717/[SII]6731 |1.15/2.0| We study properties of ionized gas, gas/stellar kinematics bar, or a combination of both. New studies are necessary 30 6 30 2 5.5 1.9 and stellar populations in central regions (a few inner 20 20 to understand the galaxy history and mass transfer within 1.8 5 kiloparsecs) of four pairs of nearby Seyfert (NGC 5194, 10 10 1.7 the inner kiloparsecs. Our new data bring, for the first 4.5 1.6 0 0 NGC 4579, NGC 4151, NGC 4138) and normal spiral time, the 2D spectroscopic coverage of the whole region 4 1.5 -10 -10 galaxies (NGC 5505, NGC 3351, NGC 2985, NGC 3245). encompassed by the ring. DE offset [arcsec] 3.5 DE offset [arcsec] 1.4 1.3 -20 3 -20 1.2 -30 2.5 -30 While the key to the AGN fuelling and growth of the cen- -30 -20 -10 0 10 20 30 -30 -20 -10 0 10 20 30 We modelled the absorption features and slope of the RA offset [arcsec] RA offset [arcsec] tral supermassive black holes lies certainly closer to the spectra using the synthetic library of Bruzual & Charlot nucleus than 1 kpc, establishing the connection between (2003) to derive LOS stellar velocities and continuum flux Ratio [NII]6583/Ha (log scale) Ratio [OIII]5007/Hb |*/0.8| (log scale) 100 1 0.4 0.8 pc and kpc scale is one of unavoidable preliminary and to make correction for stellar absorption. Emission 30 30 0.3 0.6 steps: the velocity field at 100 pc can be very complex 20 20 lines were fitted by simple Gaussian functions to obtain 0.2 0.4 10 0.1 10 and its modeling requires a prior understanding of larger 0.2 line intensities, mean LOS velocities and velocity disper- 0 0 0 0 scales. Also, signatures of past inflow can be expected -0.1 sions. See Figs. 2. – 4. We also show spectral diagnostic -0.2 -10 -0.2 -10 DE offset [arcsec] DE offset [arcsec] in the kpc-scale radial gradients of stellar age, metallicity diagrams in Fig.5. to constrain ionization sources. -0.3 -0.4 -20 -20 and velocity dispersion. Our main goals are to: 1. look -0.4 -0.6 -30 -0.5 -30 -0.8 for systematic differences in central stellar populations -30 -20 -10 0 10 20 30 -30 -20 -10 0 10 20 30 RA offset [arcsec] RA offset [arcsec] and stellar/gaseous kinematics between Seyfert and non- Intensity in stellar continuum (log scale) [10-16erg/s/cm2/arcsec2] Stellar velocities |-300/300| [km/s] 30 4.5 30 300 active galaxies; 2. estimate inflow/outflow to/from the 200 Figure 4: Top left: Map of Hα/Hβ intensity ratio tracing 20 4 20 central kpc; 3. put constraints on the central kpc fuelling 10 10 100 the interstellar redenning: the highest extinction follows 3.5 via stellar mass-loss. The sample is intended as a pilot 0 0 0 the ring. Top right: Map of [SII]6717/[SII]6731 ratio, 3 study to demonstrate the efficacy of using the PMAS- -10 -10 -100 DE offset [arcsec] DE offset [arcsec] which is related to electron density distribution: highest 2.5 PPAK integral field spectrograph for the study of active -20 -20 -200 ratio values correspond to lowest electron densities. -30 2 -30 -300 and inactive galaxies over a uniquely wide range of size -30 -20 -10 0 10 20 30 -30 -20 -10 0 10 20 30 Bottom left and right: Maps of [NII]/Hα and OIII/Hβ scales. RA offset [arcsec] RA offset [arcsec] ratios show that gas in the inner region is most probably ionized by the AGN, while stars dominate the ionization Intensity in Ha (log scale) [10-16erg/s/cm2/arcsec2] Velocity in Ha |-200/200| [km/s] of the ring. Observations 30 2.5 30 200 150 20 2 20 NGC4138 Diagnostic diagram [OIII]/Hb vs. [NII]/Ha, S/N > 3 100 1.5 10 1.5 10 Eight nearby (0.001 <z< 0.005) galaxies were observed 50 SEYFERT with PMAS-PPAK IFU at the Calar Alto 3.5 m telescope 0 1 0 0 1.0 -50 ′′ ′′ -10 0.5 -10 74 × 64 DE offset [arcsec] DE offset [arcsec] -100 with FOV of (see Fig.1) and spatial sampling 0.5 -20 0 -20 of 2.68′′, i.e. ∼ 100 − 260 pc. Our data were obtained -150 -30 -0.5 -30 -200 3600 − 7000 ˚ -30 -20 -10 0 10 20 30 -30 -20 -10 0 10 20 30 0.0 HII in two setups: 1. range A with resolution RA offset [arcsec] RA offset [arcsec] 10 7 ˚ 6200 6900 ˚ LINER of ∼ . A (FWHM); 2. range − A with -0.5 log ([OIII]5007 / Hbeta) integrated FOV resolution of ∼ 2.77 A.˚ Figure 2: Intensity and mean LOS velocity of stars (top) the brightest spaxel Ho et al. (1997) -1.0 Dopita et al. (2000) and in Hα line (bottom). One can see very different Kewley et al. (2001) Kauffmann et al. (2003) Stasinska et al. (2005) The spectra contain stellar absorption features, e. g. morphologies – smooth stellar light, gaseous ring -1.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 Balmer lines, MgI, Fe lines, CaII H and K lines, use- surrounding a gaseous mini-bar – and rotation in log ([NII]6583 / Halpha) NGC4138 Diagnostic diagram [OIII]/Hb vs. [SII]/Ha, S/N > 3 ful to constrain stellar populations and kinematics, as opposite directions. 1.5 well as emission lines including Hα, Hβ, [OI], [OII], [OIII], [NI], [NII], [SII] for deriving gas kinematics and 1.0 SEYFERT Intensity in [NII] (log scale) [10-16erg/s/cm2/arcsec2] Intensity in [SII] (log scale) [10-16erg/s/cm2/arcsec2] ionization sources, extinction, electron density and star 30 2.5 30 2 0.5 6200 − 6900 ˚ 2 formation rate. The range A centered on Hα 20 20 1.5 0.0 was chosen to get more precise gas kinematics. 10 1.5 10 1 HII 0 1 0 -0.5 0.5 log ([OIII]5007 / Hbeta) -10 0.5 -10 LINER DE offset [arcsec] DE offset [arcsec] 0 integrated FOV -20 0 -20 -1.0 the brightest spaxel Ho et al. (1997) Dopita et al. (2000) -30 -0.5 -30 -0.5 Kewley et al. (2001) -30 -20 -10 0 10 20 30 -30 -20 -10 0 10 20 30 -1.5 RA offset [arcsec] RA offset [arcsec] -2.0 -1.5 -1.0 -0.5 0.0 0.5 log ([SII]6717 + [SII]6731 / Halpha) Figure 5: Spatialy resolved diagnostic diagrams; Intensity in Hb (log scale) [10-16erg/s/cm2/arcsec2] Intensity in [OII] (log scale) [10-16erg/s/cm2/arcsec2] ≤ 10′′ 30 2 30 2 central spaxels with R are red, those with 10′′ ≤ 25′′ 20 1.5 20 1.5 <R are green and spaxels ′′ 10 10 with R> 25 are black. 1 1 0 0 0.5 0.5 -10 -10 DE offset [arcsec] DE offset [arcsec] Acknowledgments 0 0 Figure 1: PPAK layout: 331 object fibers surrounded -20 -20 -30 -0.5 -30 -0.5 This project is supported by grants No. 205/08/H005 (Czech Science by 36 sky fibers. The black circles are just -30 -20 -10 0 10 20 30 -30 -20 -10 0 10 20 30 Foundation), AV0Z10030501 (Academy of Sciences of the Czech Republic), RA offset [arcsec] RA offset [arcsec] LC06014 (Center for Theoretical Astrophysics, Czech Ministry of Education) and protective buffers. From Kelz el al. (2006). MUNI/A/0968/2009 (Masaryk University in Brno). The data were obtained under the EU Opticon Access Program following a proposal (PI: B. Jungwiert) submitted Intensity in [OIII] (log scale) [10-16erg/s/cm2/arcsec2] Velocity in [OIII] |-200/200| [km/s] in the framework of the EU Research Training Network. “Euro3D - Promoting 3D 2.5 200 30 30 Spectroscopy in Europe”. 2D maps of NGC4138 150 20 2 20 100 10 1.5 10 Here we present 2D maps for a Seyfert 1.9 galaxy 50 References ′′ 0 1 0 0 NGC 4138 (d ∼ 16 Mpc, 1 ∼ 80 pc). While it is mor- -50 -10 0.5 -10 [1] Afanasiev V. L. & Silchenko O. K., 2002, ApJ 124, 706 + DE offset [arcsec] DE offset [arcsec] -100 phologically classified as SA(r)0 and looks very regu- -20 0 -20 -150 [2] Bruzual G.