THE 3.3 ㎛ PAH FEATURE AS A SFR INDICATOR: PROBING THE INTERPLAY BETWEEN SF AND AGN ACTIVITIES

We utilize AKARI’s slitless spectroscopic capability to detect the 3.3 „m polycyclic aromatic hydrocarbons (PAHs) emission and measure star formation (SF) activity for various AKARI programs. First, we obtain 2»5 „m spectra of 20 flux-limited galaxies with mixed SED classes in order to calibrate the 3.3 „m PAH luminosity (LPAH3:3) as a star formation rate (SFR) indicator. We find that LPAH3:3 correlates with LIR as well as with the 6.2 „m PAH luminosity (LPAH6:2). The correlations does not depend on SED classes. We find that ULIRGs deviate from the correlation between PAH luminosities and LIR, while they do not for the correlation between PAH luminosities. We suggest possible eects to cause this deviation. On the other hand, how AGN activity is linked to SB activity is one of the most intriguing questions. While it is suggested that AGN luminosity of quasars correlates with starburst (SB) luminosity, it is still unclear how AGN activity is connected to SF activity based on host galaxy properties. We are measuring SFRs for the LQSONG sample consisting of reverberation mapped AGNs and PG-QSOs. This is an extension of the ASCSG program by which we investigated the connection between SB and AGN activities for Seyferts type 1s at z » 0.36. While we found no strong correlation between LPAH3:3 and AGN luminosity for these Seyferts 1s, LPAH3:3 measured from the central part of galaxies correlates with AGN luminosity, implying that SB and AGN activities are directly connected in the nuclear region.

[1]  A. Pollo,et al.  CLASSIFICATION SCHEMES AND PROPERTIES OF INFRARED GALAXIES , 2012 .

[2]  T. Nakagawa,et al.  Near-Infrared High-Resolution Spectroscopy of the Obscured AGN IRAS 01250+2832 , 2012 .

[3]  E. Wright,et al.  INFRARED LUMINOSITIES AND AROMATIC FEATURES IN THE 24 μm FLUX-LIMITED SAMPLE OF 5MUSES , 2010, 1009.1633.

[4]  T. Nakagawa,et al.  AKARI IRC INFRARED 2.5–5 μm SPECTROSCOPY OF A LARGE SAMPLE OF LUMINOUS INFRARED GALAXIES , 2010, 1008.1585.

[5]  M. Elitzur,et al.  DETECTIONS OF WATER ICE, HYDROCARBONS, AND 3.3 μm PAH IN z ∼ 2 ULIRGs , 2009 .

[6]  Ralf Bender,et al.  THE ASTROPHYSICAL JOURNAL Preprint typeset using L ATEX style emulateapj v. 10/09/06 THE M–σ AND M–L RELATIONS IN GALACTIC BULGES, AND DETERMINATIONS OF THEIR INTRINSIC SCATTER , 2008 .

[7]  H. Netzer.  RADIATION PRESSURE FORCE AND BLACK HOLE MASS DETERMINATION IN LOW-REDSHIFT TYPE-I AND TYPE-II ACTIVE GALACTIC NUCLEI , 2008, 0811.3251.

[8]  Takashi Onaka,et al.  Systematic Infrared 2.5—5μm Spectroscopy of Nearby Ultraluminous Infrared Galaxies with AKARI , 2008, 0808.0363.

[9]  D. Ballantyne.  Obscuring Active Galactic Nuclei with Nuclear Starburst Disks , 2008, 0806.2863.

[10]  P. Andreani,et al.  Star Formation in the Hosts of High-z QSOs: Evidence from Spitzer PAH Detections , 2008, 0805.2669.

[11]  Mario Schweitzer,et al.  Spitzer Quasar and ULIRG Evolution Study (QUEST). II. The Spectral Energy Distributions of Palomar-Green Quasars , 2007, 0706.0818.

[12]  L. Armus,et al.  Mid-Infrared Galaxy Classification Based on Silicate Obscuration and PAH Equivalent Width , 2006, astro-ph/0611918.

[13]  T. Treu,et al.  Cosmic evolution of black holes and galaxies to z=0.4 , 2006, Proceedings of the International Astronomical Union.

[14]  T. Treu,et al.  Cosmic Evolution of Black Holes and Spheroids. I. The MBH-σ Relation at z = 0.36 , 2006, astro-ph/0603648.

[15]  M. Imanishi,et al.  Comparison of Nuclear Starburst Luminosities between Seyfert 1 and 2 Galaxies Based on Near-Infrared Spectroscopy , 2004, astro-ph/0408422.

[16]  Hans-Walter Rix,et al.  On the Black Hole Mass-Bulge Mass Relation , 2004, astro-ph/0402376.

[17]  M. Umemura,et al.  Why Are Massive Black Holes Small in Disk Galaxies? , 2003, astro-ph/0312207.

[18]  Brazil.,et al.  Hidden starbursts in Seyfert 1 galaxies , 2003, astro-ph/0302327.

[19]  John Kormendy,et al.  Inward Bound—The Search for Supermassive Black Holes in Galactic Nuclei , 1995 .