To investigate AGN outflows as a tracer of AGN feedback on star-formation, we perform integral-field spectroscopy of 20 type 2 AGNs at z<0.1, which are luminous AGNs with the [O III] luminosity >10 41.5 erg s −1 , and exhibit strong outflow signatures in the [O III] kinematics. By decomposing the emission-line profile, we obtain the maps of the narrow and broad components of [O III] and Hα lines, respectively. The broad components in both [O III] and Hα represent the non-gravitational kinematics, i.e., gas outflows, while the narrow components, especially in Hα, represent the gravitational kinematics, i.e., rotational disk. By using the integrated spectra within the flux-weighted size of the narrow-line region, we estimate the energetics of the gas outflows. The ionized gas mass is 1.0-38.5×105 M , and the mean mass outflow rate is 4.6±4.3 M yr −1 , which is a factor of ∼260 higher than the mean mass accretion rate 0.02±0.01 M yr −1 . The mean energy injection rate of the sample is 0.8±0.6% of the AGN bolometric luminosity, while the momentum flux is (5.4±3.6)×L bol /c on average, except for two most kinematically energetic AGNs with low L bol , which are possibly due to the dynamical timescale of the outflows. The estimated outflow energetics are consistent with the theoretical expectations for energy-conserving outflows from AGNs, yet we find no supporting evidence of instantaneous quenching of star formation due to the outflows.
We present a Chandra, Suzaku and Rosat study of the hot Intra Group Medium (IGrM) of the relaxed fossil group/ poor cluster RXJ 1159+5531. This group exhibits an advantageous combination of flat surface brightness profile, high luminosity and optimal distance, allowing the gas to be detected out to the virial radius (R vir ≡ R 108 =1100 kpc) in a single Suzaku pointing, while the complementary Chandra data reveal a round morphology and relaxed IGrM image down to kpc scales. We measure the IGrM entropy profile over ∼3 orders of magnitude in radius, including 3 data bins beyond ∼ 0.5R 200 that have good azimuthal coverage (>30%). We find no evidence that the profile flattens at large scales (>R 500 ), and when corrected for the enclosed gas fraction, the entropy profile is very close to the predictions from self-similar structure formation simulations, as seen in massive clusters. Within R vir , we measure a baryon fraction of 0.17 ± 0.02, consistent with the Cosmological value. These results are in sharp contrast to the gas behaviour at large scales recently reported in the Virgo and Perseus clusters, and indicate that substantial gas clumping cannot be ubiquitous near R vir , at least in highly evolved (fossil) groups.
Using archival Chandra observations of 19 LINERs, we explore the X-ray properties of their inner kiloparsec to determine the origin of their nuclear X-ray emission, to investigate the presence of an AGN, and to identify the power source of the optical emission lines. The relative numbers of LINER types in our sample are similar to those in optical spectroscopic surveys. We find that diffuse, thermal emission is very common and is concentrated within the central few hundred parsecs. The average spectra of the hot gas in spiral and elliptical galaxies are very similar to those of normal galaxies. They can be fitted with a thermal plasma (kT $ 0:5 keV ) plus a power-law ( photon index of 1.3-1.5) model. There are on average three detected point sources in their inner kiloparsec with 10 37 ergs s À1 < L 0:5 -10 keV < 10 40 ergs s À1 . The average cumulative luminosity functions for sources in spiral and elliptical galaxies are identical to those of normal galaxies. In the innermost circle of 2B5 radius in each galaxy we find an AGN in 12 of the 19 galaxies. The AGNs contribute a median of 60% of the 0.5-10 keV luminosity of the central 2B5 region, and they have luminosities of 10 37 -10 39 ergs s À1 ( Eddington ratios of 10 À8 to 10 À5 ). The ionizing luminosity of the AGNs is not enough to power the observed optical emission lines in this particular sample. Thus, we suggest that the lines are powered either by the mechanical interaction of an AGN jet (or wind) with the circumnuclear gas or by stellar processes, such as photoionization by post-AGB stars from an old or intermediate-age population (in most cases) or by young stars (in a few cases).
We present a compilation of spectral energy distributions (SEDs) of 35 weak active galactic nuclei (AGNs) in low-ionization nuclear emission region (LINERs) using recent data from the published literature. We make use of previously published compilations of data, after complementing and extending them with more recent data. The main improvement in the recent data is afforded by high-spatial resolution observations with the Chandra X-Ray Observatory and high-spatial resolution radio observations utilizing a number of facilities. In addition, a considerable number of objects have been observed with the Hubble Space Telescope in the near-IR through near-UV bands since the earlier compilations were published. The data include upper limits resulting from either non-detections or observations at low spatial resolution that do not isolate the AGN. For the sake of completeness, we also compute and present a number of quantities from the data, such as optical-to-X-ray spectral indices (α ox ), bolometric corrections, bolometric luminosities, Eddington ratios, and the average SED. We anticipate that these data will be useful for a number of applications. In a companion paper, we use a subset of these data ourselves to assess the energy budgets of LINERs.
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