The AGN properties of the starburst galaxy NGC 7582

NGC 7582 was identified as a Starburst galaxy in the optical \cite[(Veron et al. 1981)]{Veron et al.(1981)} but its X-Ray emission is typical of a Seyfert 1 galaxy \cite[(Ward et al. 1978)]{Ward et al.(1978)}. We analyzed a datacube of this object obtained with the GMOS-IFU on the Gemini-South telescope. After a subtraction of the stellar component using the {\sc starlight} code \cite[(Cid Fernandes et al. 2005)]{Cid Fernandes et al. (2005)}, we looked for optical signatures of the AGN. We detected a broad $H\alpha$ component (figure \ref{fig1}) in the source where \cite[Bianchi et al.(2007)]{Bianchi et al.(2007)} identified the AGN in an HST optical image. We also found a broad $H\beta$ feature (figure \ref{fig2}), but its emission reveals a extended source. We suggest that it is the light of the AGN scattered in the ionization cone. We propose that NGC 7582 is a Seyfert 1 galaxy. A number of other "hot-spots" and Wolf-Rayet features were also identified.Comment: 1 page, 2 figures, to be published in the Proceedings of the IAU Symposium no. 26

Biodégradation anaérobie de l'acide crotonique par une biomasse bactérienne spécialisée dans la dégradation de l'acide butyrique

La connaissance, actuellement très limitée, du métabolisme des bactéries acétogènes intervenant dans la biodégradation anaérobie de l'acide butyrique et d'un de ses sous-produits, l'acide crotonique, est à l'origine de cette étude.Après avoir mis au point un réacteur anaérobie à biomasse fixée, cette dernière a, dans un premier temps, été adaptée à la biodégradation exclusive du butyrate. La dégradation du crotonate a ensuite été étudiée, selon différents protocoles expérimentaux (pulses de crotonate en alimentation continue avec du butyrate puis alimentation continue avec du crotonate). Des injections de crotonate ont également été effectuées en circuit fermé, avec une biomasse adaptée dans un premier temps à la dégradation d'un mélange d'AGV, le réacteur étant ensuite alimenté avec du propionate puis du butyrate seuls.Contrairement à ce que laissait penser la bibliographie, il a été constaté que les bactéries adaptées à la dégradation exclusive du butyrate sons très rapidement à même de dégrader le crotonate.Les résultats obtenus permettent d'approcher les spécificités bactériennes, la voie catabolique suivie par le crotonate, son mode de régulation enzymatique et les équilibres qui la gouvernent. C'est ainsi qu'il est possible de proposer un modèle explicatif relativement simple du mécanisme de biodégradation du crotonate.Volatile Fatty Acids (VFAs) are intermediate metabolites formed in the anaerobic biodegradation of organic matter. They are commonly found in sewage, municipal sanitary landfill leachate and effluents from agricultural and food-processing industries. A good knowledge of the microorganisms involved in VFA biodegradation is necessary to operate satisfactory biotreatment of those effluents.The objective of the present study is to better understand the metabolism of the anaerobic bacteria responsible for the degradation of butyric acid and one of its metabolites (crotonic acid), which is still poorly known.Syntrophomonaswolfei is one of the few butyrate-degrading acetogenic bacteria that bas been documented. First studios have shown that this microorganism is not capable of degrading crotonic acid (MCINERNEY et al., 1979, 1981). This is surprising since crotonyl-Coenzyme A, in its activated form, is an intermediate metabolite of n-butyrate ß-oxidation, which is the most common mechanism of butyrate biodegradation. In addition, ß-oxidatlon of crotonate is thermodynamically possible, even under standard conditions.These observations are al the origin of the present study, which investigates the anaerobic biodegradation of crotonate. Other Investigators have followed a similar approach and isolated S. wolfei in pure culture on crotonate.The degradation of crotonate was studied in a bench-scale up-flow anaerobic filter of twenty liters, operated in the dark, at 35 °C.A first set of experiments was carried out with a biomass exclusively adapted to the biodegradation of butyrate. Heat-expansed vermiculite was used as a packing medium. Various experimental protocols were successive followed. First, pulses of crotonate were injected into the reactor under conditions of continuous feeding with butyrate, and then, the reactor was continuously fed with crotonate. The objective was to determine whether a bacterial population exclusively adapted to butyrate biodegradation would be capable of degrading crotonate.It was found that crotonate was actually biodegraded in the reactor. Woth the first protocol, when pulses of crotonate were injected into the reactor, crotonate was totally removed in 55 hours (fig. 3). Butyrate and acetate concentrations increased as crotonate was degraded, but no significant increase in biogas production was observed. On the other hand, under the same conditions, it was found that iso-butyrate was not degraded, which is consistent with other published data (MCINERNEY et al., 1979, 1981 ; STIEB and SCHINK, 1985,1989).With the second protocol (continuous feeding with crotonate at 5.2 gg/l), crotonate was totally biodegraded in 48 hours after a 24 hours lag period. This biodegradation resulted in the accumulation of acetate and, in a lower extend, butyrate (fig.4).Following this stage, the reactor was fed with a higher crotonate concentration (12 g/l), and it was observed that crotonate was totally degraded in 20 hours, without any lag period (fig. 5).These results showed that butyrate-degrading bacteria were capable of degrading crotonate effectively after a short period of adaptation.Further experiments were conducted with a biomass previously adapted to the degradation of a mixture of VFAs (acetate, propionate, iso-butyrate, butyrate and caproate). Berl saddles were used as a support for bacterial growth. The reactor was operated in a recirculated batch mode and spiked with crotonate. Finally, the reactor was successively fed for four weeks with propionate and for two weeks with butyrate, before being spiked with crotonate.In all these experiments, crotonate biodegradation was observed, but, in contrast to the results obtained with the “vermiculite reactor”, no butyrate accumulation occured (fig.6).These results show that a bacterial population adapted to the degradation of a mixture of VFAs or to the degradation of individual VFAs such as propionate and n-butyrate, is capable of degrading crotonate.Based on the present study and on literature data, the following mechanism can be proposed for the biodegradation of crotonate (fig.7). The first stage is the activation of crotonate into crotonyl-Coenzyme A by an acetyl-CoA/crotonyl-CoA transferase, as recently isolated from S. wolfei (BEATY and MCINERNEY, 1987). When present at low concentrations, crotonate is probably directly degraded into acetate, as shown by the results obtained with the “selles de Berl reactor”, in which no intermediate metabolite has been detected. At higher concentrations, enzymatic sites may be saturated and an equilibrium be established with butyrate, which is then released into the medium. This has been shown by the accumulation of butyrate under conditions of continuous feeding with crotonate. In addition, another intermediate metabolite has been formed, which has not been identified in the present study. This product is most probably poly-ß-hydroxy-butyrate, which has been found in S.wolfei (MCINERNEY et al, 1979) although if is not very common in chemiotrophic bacteria

Probing the Ionizing Continuum of Narrow-Line Seyfert 1 Galaxies. I.Observational Results

We present optical spectra and emission-line ratios of 12 Narrow-Line Seyfert 1 (NLS1) galaxies that we observed to study the ionizing EUV continuum. A common feature in the EUV continuum of active galactic nuclei is the big blue bump (BBB), generally associated with thermal accretion disk emission. While Galactic absorption prevents direct access to the EUV range, it can be mapped by measuring the strength of a variety of forbidden optical emission lines that respond to different EUV continuum regions. We find that narrow emission-line ratios involving [OII]3727, Hbeta, [OIII]5007, [OI]6300, Halpha,[NII]6583, and [SII]6716,6731 indicate no significant difference between NLS1s and Broad-Line Seyfert 1 (BLS1) galaxies, which suggests that the spectral energy distributions of their ionizing EUV - soft X-ray continua are similar. The relative strength of important forbidden high ionization lines like [NeV]3426 compared to HeII4686 and the relative strength of [FeX]6374 appear to show the same range as in BLS1 galaxies. However, a trend of weaker F([OI]6300)/F(Halpha) emission-line ratios is indicated for NLS1s compared to BLS1s. To recover the broad emission-line profiles we used Gaussian components. This approach indicates that the broad Hbeta profile can be well described with a broad component (FWHM = 3275 +- 800 km/s) and an intermediate broad component (FWHM = 1200 +- 300 km/s). The width of the broad component is in the typical range of normal BLS1s. The emission-line flux that is associated with the broad component in these NLS1s amounts to at least 60% of the total flux. Thus it dominates the total line flux, similar to BLS1 galaxies.Comment: 34 pages, 9 figures. accepted for publication in the Astrophys.Journa

Fabry Perot Halpha Observations of the Barred Spiral NGC 3367

We report the gross properties of the velocity field of the barred spiral galaxy NGC 3367. The following values were found: inclination with respect to the plane of the sky, i=30 deg; position angle (PA) of receding semi major axis PA=51 and systemic velocity V(sys)=3032 km/s. Large velocity dispersion are observed of upt o 120 km/s in the nuclear region, of up to 70 km/s near the eastern bright sources just beyond the edge of the stellar bar where three spiral arms seem to start and in the western bright sources at about 10 kpc. Deviations from normal circular velocities are observed from all the disk but mainly from the semi circle formed by the string of south western Halpha sources. An estimate of the dynamical mass is M(dyn)=2x10^11 Msolar.Comment: Accepted to be published in May 2001 issue in the A.J. 19 pages, 7 figure

The Central Engines of 19 LINERs as Viewed by Chandra

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 parsec. The average spectra of the hot gas in spirals and ellipticals 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 3 detected point sources in their inner kiloparsec with L(0.5-10 keV)~10^37-10^40 erg/s. The average cumulative luminosity functions for sources in spirals and ellipticals are identical to those of normal galaxies. In the innermost circle of 2.5" 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 2.5" region, they have luminosities of 10^37-10^39 erg/s (Eddington ratios 10^-8 to 10^-5). 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, e.g. photoionization by post-AGB stars or young stars.Comment: Accepted by Ap.J. 23 pages, 8 figures, emulatepj format, images of fig 1 not included, for complete PDF preprint see http://www.astro.psu.edu/users/mce/preprints

The Nature of LINERs

We present $J$-band ($1.15-1.35 \mu$m) spectroscopy of a sample of nine galaxies showing some degree of LINER activity (classical LINERs, weak-[O {\sc i}] LINERs and transition objects), together with $H$-band spectroscopy for some of them. A careful subtraction of the stellar continuum allows us to obtain reliable [Fe {\sc ii}]$1.2567 \mu$m/Pa$\beta$ line ratios. We conclude that different types of LINERs (i.e., photoionized by a stellar continuum or by an AGN) cannot be easily distinguished based solely on the [Fe {\sc ii}]$1.2567 \mu$m/Pa$\beta$ line ratio. The emission line properties of many LINERs can be explained in terms of an aging starburst. The optical line ratios of these LINERs are reproduced by a model with a metal-rich H {\sc ii} region component photoionized with a single stellar temperature $T_* = 38,000$K, plus a supernova remnant (SNR) component. The [Fe {\sc ii}] line is predominantly excited by shocks produced by SNRs in starbursts and starburst-dominated LINERs, while Pa$\beta$ tracks H {\sc ii} regions ionized by massive young stars. The contribution from SNRs to the overall emission line spectrum is constrained by the [Fe {\sc ii}]$1.2567 \mu$m/Pa$\beta$ line ratio. Although our models for aging starbursts are constrained only by these infrared lines, they consistently explain the optical spectra of the galaxies also. The LINER-starburst connection is tested by predicting the time dependence of the ratio of the ionizing luminosity ($L_{\rm ion}$) to the supernova rate (SNr), $L_{\rm ion}$/(SNr). We predict the relative number of starbursts to starburst-dominated LINERs (aging starbursts) and show that it is in approximate agreement with survey findings for nearby galaxies.Comment: Accepted in ApJ (19 pages, 8 figures, uses emulateapj.sty

U B V R I Photometry of Stellar Structures throughout the Disk of the Barred Galaxy NGC 3367

We report new detailed surface U, B, V, R, and I photometry of 81 stellar structures in the disk of the barred galaxy NGC 3367. The images show many different structures indicating that star formation is going on in the most part of the disk. NGC 3367 is known to have a very high concentration of molecular gas distribution in the central regions of the galaxy and bipolar synchrotron emission from the nucleus with two lobes (at 6 kpc) forming a triple structure similar to a radio galaxy. We have determined the U, B, V, R, and I magnitudes and U - B, B - V, U - V, and V - I colors for the central region (nucleus), a region which includes supernovae 2003 AA, and 79 star associations throughout NGC 3367. Estimation of ages of star associations is very difficult due to several factors, among them: filling factor, metallicity, spatial distribution of each structure and the fact that we estimated the magnitudes with a circular aperture of 16 pixels in diameter, equivalent to $6''.8\sim1.4$ kpc. However, if the colors derived for NGC 3367 were similar to the colors expected of star clusters with theoretical evolutionary star tracks developed for the LMC and had a similar metallicity, NGC 3367 show 51 percent of the observed structures with age type SWB I (few tens of Myrs), with seven sources outside the bright surface brightness visible disk of NGC 3367.Comment: Accepted for publication (abr 2007) in The Astronomical Journal (July 2007 issue

HST Observations of the Optical Jets of PKS 0521-365, 3C371, and PKS 2201+044

HST observations have led to the discovery of the optical counterpart of the radio jet of PKS 2201+044, and to a detailed analysis of the optical jets of PKS 0521-365 and 3C371. At HST spatial resolution these jets are well resolved, displaying knotty morphologies. When compared with radio maps of appropriate resolution, a clear one-to-one correspondence between optical and radio structures is found, showing that all detected optical structures are indeed related to the radio synchrotron emission. Photometry of the brightest knots shows that the radio-to-optical spectral index and the derived intensity of the equipartition magnetic field are approximately constant along the jet. Thus, present observations suggest that the electron energy distribution does not change significantly all along the jet.Comment: Accepted for publications on the Astrphysical Journal. Contains 14 pages and 5 figure

Elusive Active Galactic Nuclei

A fraction of active galactic nuclei do not show the classical Seyfert-type signatures in their optical spectra, i.e. they are optically "elusive". X-ray observations are an optimal tool to identify this class of objects. We combine new Chandra observations with archival X-ray data in order to obtain a first estimate of the fraction of elusive AGN in local galaxies and to constrain their nature. Our results suggest that elusive AGN have a local density comparable to or even higher than optically classified Seyfert nuclei. Most elusive AGN are heavily absorbed in the X-rays, with gas column densities exceeding 10^24 cm^-2, suggesting that their peculiar nature is associated with obscuration. It is likely that in elusive AGN, the nuclear UV source is completely embedded and the ionizing photons cannot escape, which prevents the formation of a classical Narrow Line Region. Elusive AGN may contribute significantly to the 30 keV bump of the X-ray background.Comment: accepted for publication in MNRAS Letters, 6 pages, 3 figures, typos and references correcte