ABSTRACTS OF INIVITED TALKS TITLE : Prof VNAME : William NNAME : Brandt TITLE OF PAPER : Observational Similarities and Potential Theoretical Connections Between Ultrasoft Narrow-Line Seyfert 1s and BAL QSOs Abstract : In addition to their unusually narrow permitted lines, ultrasoft Narrow-Line Seyfert 1s (NLS1) often show weak [O III] emission and strong optical Fe II emission. These properties place them toward the `negative' end of the primary eigenvector of Boroson & Green (1992), and they may be characterized by a relatively high mass accretion rate relative to the Eddington rate. Many Broad Absorption Line QSOs (BAL QSOs), particularly those with low-ionization absorption lines, also show weak [O III] and strong optical Fe II. These similarities, particularly if [O III] is isotropic, suggest that BAL QSOs and luminous NLS1 may be related objects characterized by a large covering factor of outflowing gas interior to the Narrow Line Region. They may even be the same basic type of object viewed perhaps from different orientations. Accretion at high rates is likely to drive significant mass outflow that could be observed as BALs and in the ultraviolet spectra of NLS1. We have been analyzing archival and proprietary data to examine this hypothesis, and we report our recent results relevant to this issue. In particular, we report results from a systematic study of soft X-ray weakness in all the z < 0.5 Bright Quasar Survey QSOs. We also discuss additional ways to test the potential NLS1/BAL QSO connection. TITLE : Dr VNAME : Bradley NNAME : Peterson TITLE OF PAPER : Reverberatioin Mapping of NLS1s and the AGN Mass-Luminosity Relationship Abstract : Reverberation mapping of the broad-line region can be used to obtain virial masses of AGN. This has been done for one NLS1 already, and another experiment is in the planning stages. We show how these objects fit into the general AGN mass-luminosity relationship and describe how and why they are different from other AGNs. TITLE : Dr VNAME : Thomas NNAME : Boller TITLE OF PAPER : ROSAT results on NLS1 Abstract : ROSAT observations have greatly advanced our knowledge on the spectral and timing properties of NLS1. ROSAT observations have estabilished the existence of an extremely soft X-ray excess in NLS1. A correlation between the strength of the soft X-ray excess and the optical line width of the $\rm H\beta$ line is detected. A similar relation is detected between the hard 2$-$10 keV continuum slope and the $\rm H\beta$ line width. One possible explanation for the relation at soft X-rays may be the ratio of the accretion rate to the square of the black hole mass. The most extreme X-ray variability is seen to date in the narrow emission line, radio-quiet active galaxies IRAS 13224$-$3809 and PHL 1092. The most probable explanation is that relativistic Doppler boosting effects in the inner accretion disk cause the extreme variability. The implications for the next generation of X-ray telescopes will also be discussed. TITLE : Prof VNAME : Hagai NNAME : Netzer TITLE OF PAPER : Optical UV and X-ray lines in NLS1 Abstract: The extreme properties of the ionizing continuum in NLS1 are likely to produce unusual spectral features. The analysis of the spectrum can thus provide a unique tool for studying several important issues such as the energy budget problem and the role of thin accretion disks. In particular, the UV emission line spectrum is predicted to be softer than in broad line AGN and there uncommon expected properties of X-ray lines. The evidence for such features, as well as theoretical predictions relevant to the coming Chandra and XMM observations, will be reviewed and discussed. TITLE : Dr VNAME : Andrea NNAME : Comastri TITLE OF PAPER : The BeppoSAX survey of Narrow Line Seyfert 1. Abstract : The results of broad band (0.1--10 keV) BeppoSAX observations of a selected sample of NLS1 will be presented. The relatively large effective area of the MECS detectors onboard BeppoSAX above a few keV and the relatively high sensitivity of the PDS instrument for energies > 10 keV have allowed to significantly extend the spectral coverage. In particular I will focus on the iron lines and high energy continuum properties inferred from deep observations of a few bright objects. TITLE : Dr VNAME : Dirk NNAME : Grupe TITLE OF PAPER : The spectrum of NLS1: Statistical properties Abstract : In X-ray selected AGN samples Narrow Line Seyfert 1 galaxies form the mayority of objects. What are their properties in other energy bands? Is there also a high percentage of NLSy1s among radio, infrared, or optically elected AGN? In my talk I will give an overview about what is known about the distribution of NLSy1s over the whole electro-magnetic specrum. TITLE : Dr VNAME : Beverley J. NNAME : Wills TITLE OF PAPER : H$\beta$\ line width, and the UV-X-ray spectra of AGN Abstract : The width of the broad H$\beta$\ emission line is the primary defining characteristic of the NLS1 class. This line width is also an important component of Boroson \& Green's optical `Principal Component 1', which links steeper soft X-ray spectra with narrower H$\beta$ emission, stronger H$\beta$ blue wing, stronger optical Fe\,II emission, and weaker [O\,III]\,$\lambda$5007. In order to understand these relationships we extended spectra into the UV for 22 QSOs with high-quality soft X-ray spectra, and discovered a whole new set of UV relationships that suggest that high accretion rates are linked to dense gas and nuclear starbursts. How do the NLS1s fit into these relationships? TITLE : Dr VNAME : Ari NNAME : Laor TITLE OF PAPER : Optical, UV, and X-ray Clues to the Nature of Narrow Line Quasars Abstract : HST imaging of low z quasars, together with studies of the cores of nearby early type galaxies, suggest that the Hb line width and continuum luminosity of quasars provide a reasonably accurate estimate of the black hole mass. This provides support to the idea that NLQ have a high L/L_Edd, as suggested by the X-ray slope and variability correlations with the Hb line width. I will discuss the observed optical and UV emission line properties of NLQ, in particular those of I Zw 1, the prototype NLQ, how these may be related to a high L/L_Edd, and how this can be further tested. I will summarize with some hints that different types of AGNs may be understood as different combinations of M_BH, L/L_Edd, and inclination. TITLE : Dr VNAME : Karen NNAME : Leighly TITLE OF PAPER : ASCA Observations of NLS1s Abstract : The study of NLS1s using ASCA has many advantages. A representative sample can be studied; to date, observations of more than 30 NLS1s have been made. ASCA observations are conducted contiguously, so their X-ray variability properties can be studied systematically. ASCA detectors have a broad band pass and moderate energy resolution, properties which allow their complex X-ray spectrum to be deconvolved. ASCA observations have revealed that a soft excess extending up to 1 keV is frequently found in the X-ray spectra from NLS1s. The hard X-ray photon index has been shown to be systematically steeper than in Seyfert 1 galaxies with broad optical lines. NLS1s also exhibit larger amplitude variability than broad-line Seyferts of similar hard X-ray luminosity. On occasion, features in the soft X-ray band have been detected that appear to be specific to NLS1s; ionized iron lines have also been observed. These results have been fundamental for building our current picture of the X-ray emission from NLS1s. Many of the properties can be explained if the specific accretion rate is larger in NLS1s than in Seyfert 1 galaxies with broad optical lines. NLS1s may exemplify an extreme state of an intrinsic physical parameter and therefore their study may lead to an enhanced understanding of AGN in general. TITLE : Dr VNAME : Juri NNAME : Poutanen TITLE OF PAPER : Emission processes in AGN Abstract : I will review basic emission processes that are believed to give rise to the X-ray spectra of AGN. Most attention will be payed to the recent advances in theoretical modelling of the emission regions in AGN. Spectral analogies of radio-quiet AGN to the properties of Galactic black hole candidates will be pointed out. TITLE : Dr. VNAME : Suzy NNAME : COLLIN-SOUFFRIN TITLE OF PAPER : The unusual spectrum of FeII in NLS1 Abstract: S. Collin-Souffrin and M. Joly We will review the observations of FeII in NLS1 and in BAL QSOs, with some emphasis on the"extreme FeII emitters". First we will show that they cannot be accounted for in the framework of standard photoionized models. We will then recall several possibilities invoked to explain the large intensities of optical FeII lines, such as non radiative heating, shocks, relativistic electrons, overabundances. In particular we will discuss whether intense FeII lines cannot be linked with the existence of a starburst in the nucleus. TITLE : Dr VNAME : Smita NNAME : Mathur TITLE OF PAPER : UV and X-ray absorption in AGN and its connection to NLS1s. Abstract : I will begin by reviewing the X-ray/UV absorption models and how they offer an unique opprtunity to probe the near nuclear environment of AGN. I will discuss related controversies and argue that all the available data support the unified X-ray/UV absorber scenario. I will elaborate on the X/UV absorption in NLS1s and discuss the implications for models. --------------------------------------------------------------- ABSTRACTS OF CONTRIBUTED TALKS 1. TITLE : Associate Professor VNAME : Richard NNAME : Pogge TITLE OF PAPER : Narrow-Line Seyfert 1s, 15 Years Later Abstract : The spectroscopic properties of the objects that came to be called Narrow-Line Seyfert 1s were first systematically described and named as such 15 years ago by Osterbrock & Pogge (1985). At the time, they were a relatively rare and peculiar subclass of Seyfert galaxies. Their discovery in large numbers in X-ray surveys, however, has elevated them to a role as important members of the AGN family, ones which may hold many keys to understanding the physics of AGN from across the electromagnetic spectrum. My talk will review the spectral classification of the Narrow-Line Seyfert 1s, then and now, and highlight some of the outstanding questions that have arisen, or remained, about this unusual class of objects, many of which will surely be addressed or (or take clearer form) at this meeting. 2. TITLE : Dr VNAME : Robert NNAME : Goodrich CONTRIBUTION : Talk TITLE OF PAPER : FOS Observations of Four NLS1s Abstract : FOS spectra of four NLS1s will be discussed, concentrating on the emission-line diagnostics available in the ultraviolet. 3. TITLE : Prof VNAME : K. NNAME : POUNDS TITLE OF PAPER : X-ray signatures of a high accretion rate in AGN Abstract : Since first indicated in EXOSAT data 10 years ago the importance of X-ray spectral features arising by scattering, absorption and fluorescence (generically termed 'reflection') in dense matter has been well established in the study of X-ray binaries and Active Galactic Nuclei. More recently Narrow Line Seyferts Galaxies have been found to have other distinguishing X-ray features, particularly a steep or 'soft' spectrum and strong variability. By analogy with the 'high state' of Galactic Black Hole Binaries the unusual properties of NLS1 have been attributed to accretion onto the putative central black hole at a significantly higher rate (than for 'normal' Seyferts). New data from ASCA and RXTE have now been analysed to show that additional, unusual spectral features in NLS1 can be understood in terms of 'reflection' from dense matter lying close to the black hole (the putative accretion disc) and which is highly ionised, providing further support for the high accretion rate hypothesis. 4. TITLE : Dr VNAME : Matteo NNAME : Guainazzi TITLE OF PAPER : A study of the X-ray variability properties of PG quasars with RXTE Abstract : We present the X-ray variability properties of a small sample of PG quasars observed with RXTE. The main results are: a) the variability in the 2-5 keV is generally higher than above 5 keV; b) on timescales => 1 day soft X-ray steep QSO are generally more variable than flat ones. The results can be explained in a scenario where steep, narrow-line objects are in a higher accretion rate state. 5. TITLE : Dr VNAME : Edward NNAME : Moran TITLE OF PAPER : New Insights Into the Radio Properties of NLS1s Abstract : While NLS1s have been studied intensively at X-ray and optical wavelengths, comparatively little is known about their characteristics in the radio band. Therefore, we have carried out an investigation of the radio luminosities, source sizes, spectral index distribution, and variability of a large, uniformly selected sample of NLS1s. Our results indicate that, in most respects, the radio properties of NLS1s differ significantly from those of nearby classical Seyfert galaxies. Radio observations of NLS1s may thus provide important clues regarding the origin and nature of the nuclear activity in these objects. 6. TITLE : Mr. VNAME : Alberto NNAME : Rodriguez-Ardila TITLE OF PAPER : The Narrow and Broad Line Region of Narrow-Line Seyfert 1 Galaxies Abstract : This work studies the emission line properties of the broad and narrow line region in the wavelength interval 3700 -- 9500 Angstroms for a sample composed of narrow-line Seyfert 1 galaxies and normal Seyfert 1 galaxies. We have searched for the presence of optically thin gas in the BLR of the galaxies by comparing the broad OI 8446 A and Halpha emission line profiles. Our analysis show that in the NLS1s both profiles are very similar in shape and width. This result rules out the hypothesis of thin gas emission in the high velocity part of the BLR to explain the lack of broad optical permitted lines in these objects. We report the detection of narrow OI 8446 A emission in 6 galaxies of our sample, implying that this line is not restricted to a pure BLR phenomenon. In the narrow line region, we find similar luminosities in the permitted and high ionization forbidden lines of NLS1s and normal Seyfert 1s. However, low ionization lines such as [OI] 6300 A, [OII] 3727 A and [SII] 6717,6731 A are intrinsically less luminous in NLS1s. Physical properties derived from density and temperature sensitive line ratios suggest that the [OII] and [SII] emitting zones are overlaping in normal Sy1s but separated in NLS1s. Our data also indicate that a large range of densities, covering at least 4 orders of magnitude (10^2 -- 10^6 cm^-3), must exist in the NLR of narrow-line Seyfert 1 galaxies. Photoionization models that consider the NLR as composed of a combination of matter-bounded and ionization-bounded clouds succesfully reproduced the observed emission line ratios. This scenario naturally explains the low [OIII] 5007/Hbeta ratios observed in NLS1s as well as the large range of densities found. We explore the effects of low-ionization warm absorbers, located between the BLR and NLR, on the line ratios emitted by the NLR of NLS1s. 7. TITLE : Prof VNAME : Martin NNAME : Gaskell TITLE OF PAPER : WHAT IS KNOWN ABOUT BROAD LINE REGIONS -- AN OVERVIEW Abstract : Since narrow-line Seyfert 1's (NLS1s) represent one extreme of a continuum of broad-line region (BLR) properties, any explanation of NLS1s has to be consistent with what is known about BLRs in general. In this talk I will review the main properties of BLRs. Our knowledge of BLRs has come from three main lines of attack: the modelling of emission line intensities using photoionization codes, the study and comparison of emission line profiles, and ``reverberation mapping''. We cannot claim to have an understanding of BLRs until the results of all three approaches are reconcilled. Additional insights into the nature of BLRs, come from a comparison of BLR properties with other quasar properties. There is reasonable agreement among workers on average (integrated) properties of the BLR gas, such as composition, density, and distance from the central energy source. There is also a general concensus that the BLR is ``stratified'' with the higher-ionization regions being closer in. However, there is disagreement over whether BLR properties change continuously with radius or whether there are two fundamentally different types of BLR gas. I will argue for the latter: a high-ionization, rapidly-moving, traditional, ``BLR I'', and a lower-ionization, spatially- and kinematically-distinct, ``BLR II''. The area where there is most disagreement among researchers is in the kinematics of the BLR. The blueshifting of high-ionization lines and the presence of blueshifted intrinsic absorption lines in some objects argue for radial outflow, but reverberation mapping has completely failed to reveal such an outflow. There is good evidence for a disc component of the BLR, probably in all objects. The current (very tentative) standard BLR model consists of a disk (BLR II) with a corona above it (BLR I). 8. TITLE : VNAME : Joanna NNAME : Kuraszkiewicz TITLE OF PAPER : The UV spectra of NLS1s - implications for their broad line region. Abstract : We study the UV spectra of NLS1 galaxies and compare them with "normal", broad-line AGN. The NLS1 spectra show narrower UV lines, weaker CIV$\lambda$1549 and CIII]$\lambda$1909 emission, and stronger AlIII$\lambda$1857 emission. These UV line properties add to the optical and X-ray properties known to be part of the Boroson \& Green eigenvector 1. We show that the observed line properties are due to a smaller ionization parameter, somewhat higher BLR cloud densities, and larger BLR radii. These modified conditions are the result of the steep soft-X-rays (which characterize the NLSy1s SEDs), which change the equilibrium of the two phase cloud-intercloud medium. Using a model of an accretion disk with corona, we also show that the steep soft and the hard-X-ray continua can be explained if the $L/L_{Edd}$ ratios are larger than in "normal" Seyfert1/QSO strengthening earlier suggestions that the $L/L_{Edd}$ is the physical parameter driving eigenvector 1. 9. TITLE : Dr VNAME : Paul NNAME : O'Brien TITLE OF PAPER : Coronal line emission from NLS1s Abstract : Optical and near-IR emission-line spexctra have been obtained for a number of NLS1s with X-ray spectra. The preliminary results of this study will be presented. 10. TITLE : Dr VNAME : Fabrizio NNAME : Nicastro TITLE OF PAPER : Broad Emission Line Regions in AGN: the Link with the Accretion Power Abstract : F. Nicastro \& M. Elvis We present a model which relates the Broad Emission Line Regions of AGN to the accretion mechanism. Based on the Kepleraian assumption for the high velocity clouds of the gas responsible for the production of the Broad Emission Lines, we propose a link between that gas and a critical region of a Shakura-Sunyaev accretion disk. This region is where the radiation pressure starts to dominate over the gas pressure, and the disk becomes unstable. We show that in the framework of this picture the observed range of H$\beta$ FWHM from Broad Line to Narrow Line type 1 AGN is quite well reproduced as a function of the accretion rate. This interval of velocities is the only permitted range and goes from $\sim 25,000$ km s$^{-1}$ for sub-Eddington accretion rates, to $\sim 500$ km s${-1}$ for super-Eddington accretion rates. At accretion rates lower than a critical value this region of the disk falls inside the last stable orbit, and so does not longer exist. Low luminosity AGN emitting at this low rate would not have a Broad Emission Line Region. We also show that the relationship between the predicted FHMH and the accretion rate is quite insensitive to the mass of the central black hole. As a result Narrow Line type 1 AGN can also host a large mass black hole (as recently observed). Finally we show that, due to the presence of the Lightman Eardley instabilities in the radiation pressure dominated region of the accretion disk, type 1 AGN accreting close to the critical accretion rate, and hosting black holes of $\sim 10^7$ M$_{\odot}$, would switch between the two typical Seyfert 1 and Narrow Line Seyfert 1 states, on timescales of months-to-year. 11. TITLE : Mr VNAME : Simon NNAME : Vaughan TITLE OF PAPER : X-ray spectral complexity in NLS1s Abstract : We present a systematic analysis of the ASCA spectra of 22 "narrow-line" Seyfert 1 galaxies. Eighteen require a soft excess component, which can contain the bulk of the luminosity, even in the relatively hard ASCA band. Nine of these objects show evidence for an absorption feature either in the energy range 1.1-1.4 keV or 0.7-0.9 keV, possibly both types are due to absorption in highly ionized material - the "warm absorber" - with the 1.1-1.4 keV absorption produced in more strongly ionised gas. We also consider the case of the NLS1 Ark 564 in detail using simultaneous ASCA and RXTE observations and discuss the possibility of reflection from a strongly irradiated accretion disc. 12. TITLE : Dr VNAME : Rick NNAME : Edelson TITLE OF PAPER : X-ray Variability of Ark 564 Abstract : Ark 564, the brightest NLS1 in the hard X-ray sky, has been monitored with XTE once every 4 days since Jan 1999 and simultaneously with ASCA for continuous 2 day period. This talk will summarize both of these campaigns, focusing on a comparison of long-term variability with "normal" Seyfert 1s in the former data set and studies of the spectral variability and interband lags in the latter. These high quality RXTE light curves suggest similarities with variability in X-ray binaries. If the variability in AGN and X-ray binaries has the same origin, this poses a theoretical question: what physical mechanism produces these rapid, aperiodic variations in objects that differ in mass and luminosity by a factor of >10^6? 13. TITLE : Dr VAAME : Stefanie NNAME : Komossa TITLE OF PAPER : Warm Absorbers in NLSy1 Galaxies Abstract : Warm absorbers are an important new probe of the conditions within the central regions of active galaxies. They have been observed in $\sim$50\% of the well-studied Seyfert galaxies and have also been detected in quite a number of Narrow-line Seyfert\,1 galaxies (NLSy1). Here, we present a study of the X-ray properties of several NLSy1s with focus on their warm absorbers. In a first part, we discuss properties of some safely identified (dusty and dust-free) warm absorbers in NLSy1 galaxies, and study multi-wavelength consequences of the presence of the ionized material (e.g., its potential contribution to high-ionization optical iron lines). In a second part, we investigate if the presence of a warm absorber in individual NLSy1s could account for the peculiar spectral properties of these galaxies: (i) Several scenarios are explored to account for the recently observed peculiar absorption features around $\sim$1.1 keV on the basis of detailed photoionization models. (ii) The strong spectral variability of RX J0134.3-4258 (from $\Gamma \simeq -4.4$ in the ROSAT all-sky survey observation, to $\simeq -2.2$ in our subsequent pointing) is discussed and examined in terms of warm absorption. The photoionization calculations were carried out with Ferland's code {\em Cloudy}. 14. TITLE : Dr VNAME : Shin NNAME : Mineshige TITLE OF PAPER : Origin of soft X-ray excess and variability Abstract : What is expected in an accretion disk shining at the Eddington luminosity? Possible origins of soft X-ray excess and large variability are discussed based on the steady and time-dependent accretion disk models and 3D MHD disk simulations. Especially, we stress the importance of advective energy transport in the optically thick disks and the role of magnetic fields. 15. TITLE : Dr VNAME : Andreas NNAME : Eckart TITLE OF PAPER : Molecular Gas and Star Formation in the Host Galaxy of I~Zw~1 Abstract : Recent analysis of our high angular resolution NIR imaging spectroscopic data in conjunction with sub-arcsecond Plateau de Bure interferometric mm-line observations indicate the presence of a circum-nuclear starburst ring in I~Zw~1. The molecular gas of the host galaxy could be traced through out the visible extend of the host. We have detected a circumnuclear gas ring of diameter $\sim$ 1.5'' ( 1.5 kpc) in its millimetric CO line emission and have mapped the disk and the spiral arms of the host galaxy in the $^{12}$CO(1-0) line at 115 GHz as well as in the H (1.65 $\mu$m) and K (2.2 $\mu$m) band. We have obtained new (sub-)arcsecond resolution data of the $^{12}$CO (2-1) line emission as well as the $^{13}$CO (1-0) line emission. This new data allows a more detailed analysis of the nuclear gas dynamics as well as an investigation of the molecular gas excitation. New high angular resolution NIR imaging, using the MPE SHARP camera at the ESO NTT, as well as HST V-band data provide an improved estimate of the size of the central stellar cluster as well as the distribution of the underlying extended emission. A comparison to broad band spectra of other galaxies suggests bluer disk colors for I~Zw~1, and that star formation in the host galaxy and the western companion of I~Zw~1 is enhanced. This is also supported by a starburst analysis using all available data on the northwestern spiral arm. The presence of molecular material within the disk and right on the arm indicates that at least in this region 10~kpc from the nucleus star formation, and not scattered light from the AGN nucleus, is responsible for the blue disk colors. 16. TITLE : Dr VNAME : Joern NNAME : Wilms TITLE OF PAPER : The Soft State of Galactic X-ray Binaries Abstract : I present the results of our three year monitoring campaign of the galactic black hole binaries LMC X-3 and LMC X-1 with RXTE. These observations allow the study of the soft state in these objects over a long period of time. I will discuss the long term spectral variability of these sources in the context of accretion disk corona models. 17. TITLE : Prof VNAME : Bozena NNAME : Czerny TITLE OF PAPER : Disk/corona model of accretion flow Abstract : We propose the model of accretion flow onto black hole consisting of the accretion disk with a corona which is based on physical assumptions and does not contain any arbitrary parameters describing the division of the flow into cold (disk) and hot (corona) part apart from the viscosity parameter alpha. The complete model is determined by the mass, accretion rate and the viscosity parameter. We present the radial dependencies of parameters of such a two-phase flow with and without advection in the corona for the model based on assumptions used by Witt et al. 1997. Within the frame of this model, the fraction of the luminosity emitted in hard X-rays strongly decreases with an increase of the luminosity to the Eddington luminosity ratio. This trend clearly identifies NLS1 galaxies with objects relatively close to the Eddington luminosity. We show that the more appropriate criterion for the disk/corona transition is given by condition of no evaporation due to the thermal conduction (Rozanska & Czerny 1999, astro-ph 9906101), if a static solution in the vertical direction can be found, or the condition of satisfying the continuity equation by the corona if condensation/evaporation preceeds. We discuss the changes introduced to the model by the new approach to the disk/corona dicvision. 18. TITLE : Dr VNAME : Astrid NNAME : Orr TITLE OF PAPER : NLSy1 and Sy1: a comparison of ionized X-ray absorber properties. Abstract : NLSY1 distinguish themselves from the average Sy1 AGN by their extreme observational properties: the strongest and hottest soft excesses and in some cases huge amplitude and rapid variability. Furthermore there are over a dozen of NLSy1 with observed soft X-ray spectral complexity which may be caused by warm absorbers. I will give a general review of warm absorber observations and models in AGN and NLSy1 in particular. I will also present first results from a systematic study of warm absorbers in AGN using BeppoSAX public archive data for spectral fitting with photoionization models. Because of its good low-energy resolution and effective area down to 0.1 keV BeppoSAX is very efficient for the study of the complex spectral features in the soft X-ray. The broad band sensitivity of BeppoSAX also allows a much more accurate measure of the underlying continuum than other X-ray observatories. The NLSy1 warm absorber properties with respect to Sy1 in general will be discussed for this study. 19. TITLE : Dr VNAME : Amri NNAME : Wandel TITLE OF PAPER : Black Hole and Host Masses of NLS1 Abstract : Recently reliable mass estimates of the central black holes in AGN became feasible due to emission-line reverberation technique. Using this method as a calibrator, it is possible to determine masses of a wider range of AGN, in particular NLS1. Do NLS1 have smaller black holes than ordinary Sy1s? How do the relate to their host galaxies? I review the methods of mass determination, and use NGC 4051 as a Rosetta Stone to takle this and related questions. 20. TITLE : Mr. VNAME : Toshihiro NNAME : Kawaguchi TITLE OF PAPER : Soft X-ray Excess in Active Galactic Nuclei Abstract : We study emission spectrum emerging from the vertical disk-corona structure composed of two-temperature plasma by solving hydrostatic equilibrium and radiative transfer self-consistently. The key question is what physical condition exhibits soft X-ray excess with a spectral index $\alpha$ ($F_{\nu} \propto {\nu}^{- \alpha}$) of 1.0 -- 3.5 and hard X-ray tail at the same time. Advective cooling is also included in the top of the disk, corona, in the present study. Our model can nicely reproduce soft X-ray excess with $\alpha$ of about 1.5 and hard tail to $\sim$ 50 keV with a different slope. The broken power laws ($\alpha \sim$ 1.5 below 2keV and $\sim$ 0.5 above) are the results of unsaturated Comptonization in soft X-rays and bremsstrahlung emission in hard X rays. Temperature of the corona and spectral shape are insensitive to the blackhole mass, while that of the disk is sensitive to the mass. 21. TITLE : Dipl.Phys. VNAME : Marion NNAME : Pfeiffer TITLE OF PAPER : Coronal Lines and the warm x-ray absorber in Seyfert 1-Galaxies Abstract : The conditions of the FHIL gas (e.g. Osterbrock 1981, Appenzeller et al 1988, Giannuzzo et al, 1995) in AGN are very similiar to the conditions of the warm absorber gas (e.g. Fabian et al 1994, Reynolds et al 1995, Nandra et al 1996), causing absorption features found in X-ray spectra below 1 keV in approximately half of all luminous Seyfert 1-galaxies (Reynolds, 1997). The FHIL region temperatures are in the order of 10^5 K and densities are around 10^6 cm^-3 (Erkens et al, 1997). In addition to the indication that these two plasmas have similiar conditions, Erkens, Appenzeller and Wagner, 1997 found a correlation between the strength of the FHILs and the ROSAT spectral index. This result is interpreted as a correlation of the FHIL strength and width with the column density of the warm X-ray absorber. With high-quality ASCA spectra it is possible to measure the ratio of the strength of the edges. We selected a sample of 21 Seyfert 1-galaxies and 3 Seyfert 2-galaxies which have been observed by ASCA and where the presence of O VII and O VIII absorption edges was suggested. This sample was observed in the optical range and the line widths of the coronal lines were measured. We compare the line widths of the FHILs to the X-ray properties of the sources. 22. TITLE : Dr VNAME : Ludmila NNAME : Nazarova TITLE OF PAPER : The effect of an attenuated continuum on the coronal line spectrum of NGC1068 and the Circinus galaxy. Abstract : The line fluxes have been calculated using (a) a non-thermal (nuclear) continuum source and (b) the non-thermal continuum plus a UV bump due to a stellar cluster. We take into account the effect of attenuation of these continua by gas with column density 10$^{22}$ cm $^{-2}$ located between the nucleus and the coronal line region. The calculated coronal line ratios are in a good agreement with those observed in NGC1068 for model in which about 40% of the line emission comes from gas illuminated by unattenuated, non-thermal continuum, and about 60% from gas illuminated by attenuated, non-thermal continuum. In the Circinus galaxy the coronal line emission comes from the gas illuminated entirely by attenuated, non-thermal continuum. 23. TITLE : PROFESSOR VNAME : H. RICHARD NNAME : MILLER INSTITUTE : GEORGIA STATE UNIVERSITY COUNTRY : USA CONTRIBUTION : Talk TITLE OF PAPER : A SEARCH FOR RAPID OPTICAL VARIABILITY IN 5 NLS1 GALAXIES Abstract : One of the identifying characteristics of NLS1 galaxies is the existence of persistent giant-amplitude variability observed at soft X-ray energies. It would be of great in- terest to determine if a similar phenomenon is present at optical wavelengths, and if so, what is the relationship be- tween the variability observed in these defferent regimes. During the past two years, we have embarked upon a program of investigation which has as its primary goal the detection of rapid optical variations, if they exist, for a sample of five NLS1 galaxies. The results are clearly positive for IRAS 13224-3809. However, the results are less conclusive for the other four galaxies in our sample(AKN 564, MRK 766, PG 1404+226 and PG 1244+026). A summary of the results of our program will be presented. 24. TITLE : VNAME : Maria del Carmen NNAME : Polletta COUNTRY : Switzerland CONTRIBUTION : Talk TITLE OF PAPER : ISOPHOT Observations of Narrow Line Seyfert 1 Galaxies Abstract : Broad infrared spectra (7-200 microm) of four NLSy1 galaxies, obtained with the imaging photo-polarimeter (ISOPHOT) on-board ISO, are presented. The distribution of infrared luminosities, temperatures, opacities and sizes of the emitting dust component are derived from the analysis of the observed infrared spectra of the four selected objects. A comparison between the observed infrared spectra and the optical emission line properties suggests that these objects suffer different degrees of dust absorption according to the inclination of the line of sight. 25. TITLE : Dr VNAME : Takashi NNAME : Murayama COUNTRY : Japan CONTRIBUTION : Talk TITLE OF PAPER : How do we see the nuclear region (r < 0.1 pc) of NLS1s? Abstract : We propose two statistical tests to investigate how we see the nuclear region (r < 0.1 pc) of NLS1s. [I] The HINER (high-ionization nuclear emission-line region) tests: S1s have systematically higher flux ratios of [Fe VII]6087 to [O III]5007 than S2s. This is interpreted as that a significant part of the [Fe VII]6087 emission arises from the the inner wall of dusty tori which cannot be seen in the S2s (Murayama & Taniguchi 1998, ApJ, 497, L9). [II] The MIR (mid-infrared) test: S1s have systematically higher flux ratios of L band (3.5 micron) to IRAS 25 micron band than S2. This is also interpreted as that a significant part of the L band emission arises from the inner wall of dusty tori because the tori are optically thick enough to absorb the L band emission if the tori are viewed from a nearly edge on (Murayama et al. 1999, ApJ, in press). Applying these tests for a sample of NLS1s, we have found that the NLS1s have nearly the same properties of S1s. It is thus concluded that we see the dusty tori of NLS1s from a nearly face-on view. We discuss which model is feasible to explain the observed properties of NLS1s. 26. TITLE : Dr VNAME : Kiyoshi NNAME : Hayashida CITY : Toyonaka COUNTRY : Japan CONTRIBUTION : Talk TITLE OF PAPER : Estimation of Central Black Hole Masses in NLS1s from X-ray Variability and X-ray Spectrum Abstract : ASCA observations of narrow line Seyfert 1 galaxies (NLS1) are presented. We focus on the black hole size of the NLS1 sources by employing two independent methods for the mass estimation; one is using X-ray variability, the other is using blackbody fit to the soft component. Although the coincidence is not good for some sources, the mass estimated in these ways ranges from $10^4$ to $10^7$ $M_\odot$, systematically smaller than those for typical (broad line) Seyfert 1. We consider the small mass black hole is the principal cause of the several extreme characteristics of the NLS1s. 27. TITLE : Dr VNAME : Jason NNAME : Taylor INSTITUTE : United States Naval Academy COUNTRY : USA CONTRIBUTION : Talk TITLE OF PAPER : Are Narrow-Line Seyfert 1s really strange? Abstract : Narrow-line Seyfert 1s (NLS1s) are generally considered to be ``strange'' AGNs. They are characterized by low (~500-2000 km/s) Hbeta FWHMs, high (~2.5-4.5) 0.1-2.4 keV photon indexes, lack of lobed radio emission, and low redward Hbeta emission. Boroson and Green (1992) hypothesized that, provided the motion of the emission clouds is controlled by gravity, NLS1s may simply accrete closer to their Eddington limits than other AGNs. However, only some AGN line emission models actually fall into this category. One such model is the stellar wind line emission model. Because the BLR region of this model scales with the tidal radius, these models predict FWHMs proportional to the -1/3 power of L/L_Edd for AGNs selected from flux-limited surveys. Thus, the NLS1 black holes are approximately 3^3=27 times less massive than those in other Seyfert 1s if the stellar line emission model is correct. The stellar wind model also predicts that NLS1s should have higher wind edge densities. NLS1 spectra appear to support this result as well. Moreover, the redward wing of the Hbeta profile is enhanced in stellar wind models that have an occulting accretion disk and an inter-cloud medium, but only if the cloud density is relatively low (as it would be in low L/L_Edd AGNs). This is because Hbeta emission from low L/L_Edd AGNs requires relatively high densities and inbound stellar winds in these models have higher densities in their line-emitting regions than do outbound winds. Even the radio and continuum properties of NLS1s can be explained provided we assume that particle acceleration and hard X-ray emission are strong functions of black hole mass rather than only luminosity. For better or worse, if the stellar wind line emission is correct, NLS1s are not much stranger than the other AGNs. 28. TITLE: : Dr. VNAME: : Herman L. NNAME: : Marshall INSTITUTE: : M.I.T. CONTRIBUTION : Talk TITLE OF PAPER : First results from Chandra I'd like to give a talk about the first AGN observations with the AXAF HETGS (high resolution spectrometer) and possibly a poster on my compendium of 7 AGN spectra (including both NLS1 and normal S1) from EUVE. One of the first AGN to be observed with the HETGS will be NGC 1275 (in the Perseus cluster) and there should be plenty of time to have a good result by the time of the meeting (since the observation is tentatively scheduled for mid-September). 29. TITLE: : Dr. VNAME: : Martin NNAME: : Elvis INSTITUTE: : Harvard-Smithsonian CONTRIBUTION : Talk TITLE OF PAPER : A Structur for Quasar Nuclei Abstract: We propose a simple unifying structure for the inner regions of quasars and AGN. This empirically derived model links together the BALs, the narrow UV/X-ray ionized absorbers, the BELR, and the 5 Compton scattering/fluorescing regions into a single structure. The model also suggests an alternative origin for the large-scale bi-conical outflows. Some other potential implications of this structure are discussed. --------------------------------------------------------------------- ABSTRACTS OF POSTER CONTRIBUTIONS 1. TITLE : VNAME : Mara NNAME : Salvato INSTITUTE : AIP Potsdam DEPARTMENT : STREET : An der Sternwarte 16 CITY : Potsdam STATE : PCODE : D-14482 COUNTRY : Germany CONTRIBUTION : Poster TITLE OF PAPER : Galaxy interactions in a X-ray selected Seyfert sample Abstract : M. Salvato, P. Bo/"hm, G. Hasinger, I. Lehmann (AIP), P. Rafanelli (Univ. Padova, Italy). From the ROSAT Bright Survey (RBS) we have extracted an unbiased statistical complete flux-limited (ROSAT PSPC 0.5-2 Kev countrate $>0.3 cts/se$) sample of 101 nearby Seyferts ((z$<$0.1). The aim is to study their morphological properties and the environment in the context of the relation between galaxy interaction and AGN activity. We are analysing B and R images using the Adaptive Filters to recognize faint signs of interaction. We present the first results from the analysis of the sample. 2. TITLE : VNAME : Ingo NNAME : Lehmann INSTITUTE : AIP Potsdam DEPARTMENT : STREET : An der Sternwarte 16 CITY : Potsdam STATE : PCODE : D-14482 COUNTRY : Germany CONTRIBUTION : Poster TITLE OF PAPER : Spectroscopic discrimination between Seyfert and field galaxies in the ROSAT Deep Surveys I. Lehmann (AIP), G. Hasinger (AIP), M. Schmidt (Caltech) Abstract : The ROSAT Deep Survey (RDS) in the Lockman Hole contains a complete sample of 50 X-ray sources with fluxes in the 0.5-2 keV band larger than 5.5 $\cdot$ 10$^{-15}$ erg cm$^{-2}$ s$^{-1}$. We have reached a complete optical/infrared identification, where over ~85 \% of the sources are quasars and Seyfert galaxies (Lehmann et al. 1999). During the course of our optical identification work, we have obtained optical spectra of 67 narrow-emission line galaxies (NELG), which are physically not associated with the X--ray sources. We present the optical emission line properties (EW and FWHM) of the RDS quasars and Seyfert galaxies in comparison with other AGN samples. Furthermore, we discuss the spectroscopic discrimination between Seyfert and field galaxies (NELG). The analysis of the emssion lines has revealed that only one of the 43 RDS AGN fits the criteria of Narrow-Line Seyfert 1 galaxies. 3. TITLE : Prof VNAME : K.P. NNAME : Singh INSTITUTE : Tata Institute of Fundamental Research DEPARTMENT : Astronomy and Astrophysics STREET : Homi Bhabha Road CITY : MuMBAI STATE : MAHARASHTRA PCODE : 400 005 COUNTRY : INDIA CONTRIBUTION : Poster TITLE OF PAPER : Discovery of a Narrow Line Seyfert 1 Galaxy Abstract : We have identified an ultrasoft X-ray source detected with ROSAT with a new narrow line Seyfert 1 galaxy. We will present its X-ray and optical spectral characteristics. It optical spectrum shows fairly strong Fe II emission lines, and its X-ray spectrum has an extremely steep power-law index, making it an extrmely interesting example of this class of AGNs. 4. TITLE : Associate Professor VNAME : Laura NNAME : Kay INSTITUTE : Barnard College, Columbia University DEPARTMENT : Physics STREET : 3009 Broadway CITY : New York STATE : New York PCODE : 10027 COUNTRY : USA CONTRIBUTION : Poster TITLE OF PAPER : Spectropolarimetry of Xray Selected NLS1 Galaxies Abstract : Authors: L. Kay, K. Leighly, J. Halpern (Columbia University), E. Moran (U. C. Berkeley), and A. M. Magalhaes (IAG-USP, Brazil) We present optical spectropolarimetry of a group of Xray selected NLS1 galaxies, obtained at the Lick 3m and CTIO 4m telescopes in 1998 and 1999. The results will allow us to investigate the relationships between NLS1s and BALQSOs, and the properties of dusty warm absorbers in NLS1s. 5. TITLE : Dr VNAME : James NNAME : Reeves INSTITUTE : University of Leicester DEPARTMENT : Physics and Astronomy STREET : University Road CITY : Leicester STATE : PCODE : LE1 7RH COUNTRY : UK CONTRIBUTION : Poster TITLE OF PAPER : PDS 456: an Extreme Accretion Rate Quasar? Abstract : We present simultaneous ASCA and RXTE observations of the most luminous known AGN in the local (z<0.3) Universe, the recently discovered quasar PDS 456. Multi-wavelength observations conducted show that PDS 456 has a bolometric luminosity of 10^{47} erg/s, peaking in the UV band. The broad-band X-ray spectrum (obtained by ASCA and RXTE) contains considerable complexity. The most striking feature present is a deep, highly ionized iron K edge, observed at 8.7 keV in the quasar rest frame. This feature originates from highly ionized matter, possibly the inner accretion disk. PDS 456 shows unusually fast variability for a quasar, varying by a factor of 2.1 in 17 ksec. Taken with the bolometric luminosity, this implies that the bulk of the X-rays in PDS 456 are emitted within a few Schwarzschild radii of the central super-massive black hole. Finally we note that the unusual properties of PDS456; fast variability, high ionisation features and a steep X-ray spectrum are common with the NLS1s. Thus we conclude that PDS 456 is a quasar with an unusually high accretion rate. 6. TITLE : VNAME : Agnieszka NNAME : Janiuk INSTITUTE : N. Copernicus Astronomical Center DEPARTMENT : Polish Academy of Sciences STREET : Bartycka 18 CITY : Warsaw STATE : PCODE : 00-716 COUNTRY : Poland CONTRIBUTION : Poster TITLE OF PAPER : X-ray reprocessing in Narrow-line Seyfert Galaxy Ton S180 Abstract : We present the results of spectral analysis of the ASCA data for the Seyfert galaxy Ton S180. We model both the primary and reflected continuum as well as iron K-alpha line. The reprocessed component is calculated self-consistently and the line energy depends on the ionization state of the reprocessor. We show that the reprocessing matter is highly ionized and the reflected spectrum is broadened due to kinematic and relativistic effects. We find the soft to hard luminosity ratio to be of the order of 2.5 and the accretion rate approximately corresponding to the Eddington limit value. 7. TITLE : Ph.D. student VNAME : OHAD NNAME : SHEMMER INSTITUTE : Tel-Aviv University DEPARTMENT : Astrophysics STREET : CITY : Tel-Aviv STAT PCODE : 69978 COUNTRY : Israel CONTRIBUTION : Poster TITLE OF PAPER : Optical variability of NLS1 observed at the Wise Observatory Abstract : Authors: Ohad Shemmer and Hagai Netzer We report the preliminary results of a spectrophotometric monitoring program of narrow line Seyfert 1 galaxies conducted at the Wise Observatory. We present Balmer lines and optical continuum light curves for several objects that have never been monitored in this way. The data will be used to evaluate the line-to-continuum time lag in an attempt to test the idea that the accretion rate in NLS1s is larger than in other Seyfert 1 galaxies. 8. TITLE : Mr VNAME : James NNAME : Smith INSTITUTE : University of Hertfordshire DEPARTMENT : Physics & Astronomy STREET : College Lane CITY : Hatfield STATE : Herts PCODE : Al10 9AB COUNTRY : England CONTRIBUTION : Poster TITLE OF PAPER : Optical Spectropolarimetry of NLS1's Abstract : I present spectropolarimetric observations of the broad H- alpha line in several narrow-line Seyfert 1 galaxies (NLS1). Whilst, in general, Seyfert 1 galaxies exhibit a relatively wide range of polarisation properties, the polarisation properties of our sample of NLS1s are consistant. I discuss possible reasons for this and indicate how these obser- vations can help reveal why NLS1s have relatively narrow broad-line widths in the context of the unified scheme. 9. TITLE : VNAME : Delphine NNAME : Porquet INSTITUTE : Observatoire de Paris-Meudon DEPARTMENT : DAEC STREET : 5, place Jules Jansen CITY : Meudon STATE : PCODE : 92195 Meudon Cedex COUNTRY : France CONTRIBUTION : Poster TITLE OF PAPER : Theoretical study of the observed broad absorption features in the soft X-ray range in NLS1. Abstract We will model the broad absorption features detected near 1-1.4 keV in several Narrow Line Seyfert 1 Galaxies, investigating the physical parameters of the absorbing medium. Taking into account the peculiar soft X-ray excess which is well fitted by a blackbody, the observed properties of the absorption features can be correctly reproduced. We stress that the emission coming from the absorbing medium (related to the covering factor) has a strong influence on the resulting X-ray spectrum, in particular on the apparent position and depth of the absorption features. A non-solar iron abundance may be required to explain the observed deep absorption. We will also investigate the influence of an additional ionization process (collision, shock) on the predicted absorption features. 10. TITLE : Grupe VNAME : Dirk CONTRIBUTION : POSTER TITLE OF PAPER: : The enigmatic soft-X-ray NLSY1 RX J0134.2-4258 D. Grupe, K.M., Leighly, and H.-C. Thomas Abstract: We report the discovery and the follow-up observations of the enigmatic soft X-ray AGN RX J0134.2--4258. While its spectrum was one of the softest observed from an AGN during the ROSAT All-Sky Survey, its spectrum was found to be dramatically harder during a pointed observation although the count rate remained constant. In a pointed observation the spectrum appears softer when it is fainter, and spectral fits show that it is primarily the hard energy component that varies. An ASCA observation confirms the presence of a hard X-ray power law, the slope of which is rather flat compared with other NLS1s. Survey and followup radio observations reveal that RX J0134.2--4258 is also unusual in that is is a member of the rare class of radio-loud NLS1s, and, with R=71, it holds the current record for large radio-to-optical ratio. We present the results from analysis of the ROSAT pointed observation, an ASCA observation, optical and radio observations of this peculiar source, and discuss possible scenarios to explain its strange behaviour. 11. TITLE : Dr VNAME : Mitsuru NNAME : Takeuchi INSTITUTE : Osaka-Kyoiku University DEPARTMENT : Astronomical Institute STREET : Asahigaoka CITY : Kashiwara STATE : Osaka PCODE : 582-8582 COUNTRY : Japan CONTRIBUTION : Poster TITLE OF PAPER : X-Ray Fluctuations from the Slim Disks Abstract : The recent X-ray observations report that not only stellar black hole candidates (SBHCs) in its low state (not bright sources) but also super-luminal jet sources (bright sources) exhibit X-ray fluctuations. If we consider that X-ray fluctuations of bright sources originate from its accretion disks, the fluctuations are made in the optically thick, advection-dominated disk, what we call the slim disk (bright disk). However, the time evolution of the slim disk have not been investigated so far. The numerical calculations by Manmoto et al. (1996) is well known as the time evolution of the optically thin, advection-dominated disk (not bright disk). The disturbance added into the optically thin, advection-dominated disk falls into the central star. The disk luminosity increases when the disturbance falls, and the light curve in this process is in good agreement with the X-ray shot configuration of SBHC, Cyg X-1 in its low state. I investigate how the luminosity of the slim disk with a disturbance varies. I add the same disturbance as Manmoto et al. (1996) into the slim disk, and as this result, the similar light curve as that of the optically thin, advection-dominated disk is obtained. In addition to SBHCs and jet sources, it has recently reported that some Seyfert galaxies also exhibit X-ray fluctuations. My calculation shows that the slim disk (the bright disk) can also make X-ray fluctuations, and is important one to explain X-ray fluctuations of jet sources and some Seyfert galaxies. 12. TITLE : Dr VNAME : Stefanie NNAME : Komossa INSTITUTE : MPE CONTRIBUTION : Poster TITLE OF PAPER : An optical and X-ray study of the Narrow-line QSO 0117.2-2837 Stefanie Komossa, Dirk Grupe, M. Janek Abstract: We discuss the multi-wavelength properties of 1E 0117.2-2837 which shows one of the steepest X-ray spectra in the {\sl ROSAT} band. We present a study of the X-ray spectral and variability properties of this source, and discuss possible emission/absorption mechanisms to account for the steep X-ray spectrum. Our optical spectra classify 1E 0117.2-2837 as belonging to the group of Narrow-line AGN with strong FeII emission and a small FWHM of the H$\beta$ emission line. 13. TITLE : Dr VNAME : Wolfgang NNAME : Pietsch INSTITUTE : MPE CONTRIBUTION : Poster TITLE OF PAPER : New NLS1 galaxies detected in RASS galaxies W. Pietsch, K. Bischoff, Th. Boller Abstract: Cross correlations of the ROSAT All Sky Survey (RASS) source catalogue with the Catalogue of Principal Galaxies yielded 903 X-ray sources with galaxy counterparts. In several of them the X-ray emission can be attributed to known Active Galactic Nuclei (AGN) or emission from hot gas in clusters of galaxies, while in other galaxies the detected X-ray luminosity is in the range expected for normal spirals and ellipticals following the results of the Einstein observatory. Of special interest were X-ray bright galaxies for which no reason for their X-ray brightness was known. They were followed up by X-ray imaging with the ROSAT HRI and/or optical spectroscopy using the 2.2 m telescopes at Calar Alto and La Silla. In this program we detected more than 100 previously unknown relatively nearby AGN of different type. Here we present details on six newly discovered narrow line Seyfert 1 galaxies.