#Author Last NameAuthor First NameEmail AddressInstitutionTitleAbstractPresentationDiscussionSplinter SessionSession
1AirdJamesjames.aird@imperial.ac.ukImperial College LondonFaint end of the AGN x-ray luminosity function at z=3We combine Lyman-break galaxy selection with deep Chandra x-ray data to efficiently select AGN at redshift $z\sim 3$. 21 AGN are discovered in 4 fields (Hubble Deep Field-North, Groth-Westphal Strip, Lynx and LALA CETUS). This sample is used to determine the faint end of the x-ray luminosity function at $z\sim 3$, carefully considering corrections for incompleteness in both the x-ray data and Lyman-break selection. We find a significantly steeper slope for the faint end than other work, indicating that the number density of moderate luminosity AGN at high redshift may have previously been underestimated.poster Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments 
2AldcroftTomtaldcroft@cfa.harvard.eduHarvard-Smithsonian Center for AstrophysicsYaxx: Yet Another X-ray XtractorYaxx is a Perl script that facilitates batch spectral processing of X-ray data. It includes automated spectral extraction, fitting, and report generation. The primary emphasis is on having an easily used tool that can be run without requiring an extensive learning curve. However, for those with the motivation, yaxx is highly configurable and can be customized to support complex analysis. Yaxx has been used extensively with Chandra data and a newly developed thread for XMM processing is now available. A modular software design allows for multi-mission support and user customization of the data processing flow.poster Monday: Type I and II AGN, Absorption, XBONGs 
3AshbyMatthewmashby@cfa.harvard.eduHarvard-Smithsonian Center for Astrophysics  posterSpitzer's cryogen will run out in just a few years -- is there any obvious area of overlap between Spitzer and Chandra capabilities that ought to be addressed before that happens?Monday: 'Normal' Galaxies, Tuesday: Groups and Interactions 
4FranckeHaroldhfrancke@das.uchile.clUniversidad de ChileClustering of z=3 AGN in MUSYC-ECDFSThe Multiwavelength Survey by Yale/Chile (MUSYC) covers 1.2 square degrees of sky to U,B,V,R = 26 and K = 22 (AB), and includes the Extended CDF-S field, home of the largest Chandra survey ever conducted at its depth (0.3 square degrees and 228 ks). The X-ray catalogs of this field (Virani et al. 2006, Lehmer et al. 2005) reveal more than 700 Active Galactic Nuclei (AGN). We used the deep optical catalogs to apply the Lyman-Break technique, which yielded a sample of 84 AGN at 2.7 < z < 3.7. We performed a cross-correlation clustering analysis on these AGN and a sample of 1400 Lyman Break Galaxies at z~3. Here we present results on the clustering amplitude, estimates of the dark matter halo masses and number densities of z~3 AGN, and a measurement of the duty cycle for accretion by the SMBH hosted by these AGN.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
5GeorgantopoulosIoannisig@astro.noa.grNational Observatory of AthensSHEEP2: A search for obscured AGN with XMM in the hardest band (7.5-12 keV)We present initial results on our ultra-hard (7.5-12 keV) selected sample from the XMM Serendipitous Source Catalogue (SSC-1XMM). We find 17 sources down to have a flux of 10-13 cgs. The sample has a median redshift of 0.29. We find a number of high X-ray to optical flux ratio objects (log(fx/fo)>1) with four of these not having an optical counterpart down to B=21. The hardness ratio analysis indicates that most of the sources are unobscured.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
6GomezPercypgomez@gemini.eduGemini ObservatoryFirst Results of an optically blind Sunyaev-Zeldovich Cluster SurveyWe will present the first results of an optically blind Sunyaev-Zeldovich Cluster Survey carried out with the ACBAR bolometer array at the South Pole. Cluster candidates detected by the ACBAR array were verified by XMM-Newton and Chandra X-ray observations and by optical imaging and spectra.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: Cluster Formation and Evolution 
7GreenPaulpgreen@cfa.harvard.eduSAOX-ray Spectral Properties of Broad Line AGN in the SDSS/ChaMPAGN unification models spawned in the optical are now confronted with multiwavelength data that break the simplest Type I/II dichotomy. For instance, some broad emission line (optical Type I) AGN (BLAGN) are found to show significant X-ray absorption, and some narow line AGN (NLAGN) show none. Some of the absorbed BLAGN are explained as BALQSOs, but some are not. We cross-correlate the largest intermediate depth Chandra X-ray survey, the ChaMP, with a new SDSS photometric quasar catalog (extending to fainter mags and larger populations than the spectroscopic sample), and study the X-ray spectral properties of luminous broad line quasars. This constrains the absorbed fraction, identifies new BALQSO candidates, and tests claims of decreased absorption with increasing luminosity. We also contrast the X-ray spectral properties of this sample with those of an X-ray-selected BLAGN sample from the ChaMP.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
8HAOHENGhhao@cfa.harvard.eduHarvard UniversityAGN SEDs in COSMOS SurveyThe early result of the AGN (mainly type I) spectral energy distributions (SEDs) in the COSMOS survey is showed in the poster.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
9HornschemeierAnnannh@milkyway.gsfc.nasa.govNASA GSFCDeep X-ray Survey of the Coma Cluster with XMM-NewtonWe present some preliminary results on a 220~ks survey of an off-center region in the Coma cluster. These observations are sensitive to $\approx10^{39}$~erg~s$^{-1}$, allowing us to probe the X-ray emission from normal galaxies fainter than the Milky Way and construct an X-ray luminosity function. This represents a major step forward in characterizing the high energy emission of lower-luminosity galaxies in cluster/group environments. We also report on a major multiwavelength campaign to study the Coma cluster which includes Spitzer, GALEX, and HST data.posterI would like to see an open debate about the merits of an ultra-deep Chandra survey (many Megaseconds). This is our last chance to probe the very distant universe in X-rays (before we lose Chandra's capabilities).Monday: 'Normal' Galaxies, Tuesday: Groups and Interactions 
10HudsonDanieldhudson@astro.uni-bonn.deArgelander Insititute for Astrophysics - Bonn UniversityThe Chandra Follow-Up Of The HIFLUGCS Sample - An Analysis Of The Cores Of All 64 Clusters.The {\it HIFLUGCS} sample is a complete, flux-limited sample of the 64 X-ray brightest clusters outside of the galactic plane. The primary purpose of studying this sample is to provide a local cluster mass function which can be used to constrain cosmological parameters. We present the Chandra follow-up, which includes all 64 clusters, to the original analysis of this sample In this poster we focus on the analysis of the central density peaks of the clusters in the sample. Using high quality Chandra data we determined central temperature, density, entropy, and cooling time. We find that 46 of the clusters have central cooling times shorter than 7.7 Gyr, with a surprising 31 clusters having a central cooling time shorter than 1 Gyr. The high number of clusters with such cooling times implies that the main mechanism for quenching cooling cannot heat cluster cores above a cooling time of ~1 Gyr. Moreover, it implies that clusters with cooling times $\sim$1 - $\s! im$7 Gyr either have not yet cooled to point of needing to be reheated or have been reheated by a different mechanism.poster Monday: X-ray luminosity functions and evolution, Tuesday: Cluster Formation and Evolution 
11KaufmannSarahkaufmann@astro.uni-bonn.deArgelander-Institute for Astronomy at the University of BonnThe X-ray properties of radio-loud core-dominated AGN at different redshiftsWe study a sample of 36 flat-spectrum radio-loud AGN, observed with the X-ray observatories {\it ASCA}, {\it BeppoSax}, {\it Chandra} and {\it XMM-Newton}. The sample covers a broad redshift range up to $z=4.5$ which provides the opportunity to search for evolutionary effects. We found that the basic shape of the X-ray spectra observed in the energy range $2-10 {\rm keV}$ is the same for the full range of different redshifts. About $30\%$ of the objects show a significant amount of excess absorption which is unexpected for highly beamed blazar sources. The excess absorption measured in the quasars seems to increase with redshift.poster   
12KilgardRoyrkilgard@cfa.harvard.eduHarvard-Smithsonian Center for AstrophysicsNormal Galaxies in the Chandra/SWIRE X-ray SurveyWe present results on the normal galaxy population detected in the Chandra/SWIRE X-ray survey, the largest (0.6 sq. deg), deepest (broad bandf lux limit = 7e-16 erg/cm^2/s) contiguous region observed by Chandra to date. We find 49 X-ray sources that are spatially coincident with optically extended galaxies, 6% of the total X-ray sources. We discuss the multiwavelength properties of these galaxies, including classification of the host galaxies based on their spectral energy distribution. We also discuss the contribution of the sources to the total X-ray population of this field and compare our results with those from the ChaMP survey (Kim et al, 2006).posterThis may be contrary to the organizational goals of the meeting, but I would prefer if the splinter sessions did not overlap so closely. I am interested in attending all 3 of the splinter sessions on Monday, but not particularly interested in attending any of them on Tuesday.Monday: 'Normal' Galaxies 
13KimMinsunmkim@cfa.harvard.eduSAOChandra Multiwavelength Project X-ray Point Source Number Counts and the Cosmic X-ray BackgroundWe present the Chandra Multiwavelength Project (ChaMP) X-ray point source number counts and the cosmic X-ray background (CXRB) flux densities in multiple energy bands. To quantitatively characterize the sensitivity and completeness of the ChaMP sample, we perform extensive simulations. We also include the ChaMP+CDFs (Chandra Deep Fields) number counts to cover large flux ranges from $2\times10^{-17}$ to $2.4\times10^{-12}$ (0.5-2 keV) and from $2\times10^{-16}$ to $7.1\times10^{-12}$ (2-8 keV) $erg~cm^{-2}~sec^{-1}$. We detect breaks in the differential number counts and they appear at different fluxes in different energy bands. Assuming a single power law model for a source spectrum, we find that the same population(s) of soft X-ray sources causes the break in the differential number counts for all energy bands. We measure the resolved CXRB flux densities from the ChaMP and the ChaMP+CDFs number counts with and without bright target sources. Adding the known unre! solved CXRB to the ChaMP+CDF resolved CXRB, we also estimate total CXRB flux densities. The fractions of the resolved CXRB without target sources are $78^{+1}_{-1}\%$ and $81^{+2}_{-2}\%$ in the 0.5-2 keV and 2-8 keV bands, respectively. These fractions increase by $\sim1\%$ when target sources are included.poster Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments 
14La FrancaFabiolafranca@fis.uniroma3.itUniversita` Roma treThe Hard X-Ray Luminosity Function of AGNsWe have determined the cosmological evolution of the density of AGNs and of their NH distribution as a function of the unabsorbed 2-10 keV luminosity up to redshift 4. We used the HELLAS2XMM sample combined with other published catalogs, yielding a total of 508 AGNs. Our best fit is obtained with a luminosity-dependent density evolution (LDDE). There is evidence that the fraction of absorbed (NH〉10^22 cm-2) AGNs decreases with the intrinsic X-ray luminosity and increases with the redshift.poster Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments 
15LandtHerminehlandt@cfa.harvard.eduHarvard-Smithsonian Center for AstrophysicsThe Deep X-ray Radio Blazar Survey (DXRBS) - Radio and X-ray Number Counts, Evolution and Luminosity FunctionWe present the faintest blazar sample currently available, based on the Deep X-ray Radio Blazar Survey (DXRBS), which includes 129 flat-spectrum radio quasars and 24 BL Lacs down to radio fluxes and powers more than ~10 times fainter than published blazar samples. Our results constrain blazar evolution, unified schemes, and the so-called "blazar sequence".poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: Cluster Formation and Evolution 
16LehmerBretblehmer@astro.psu.eduPenn State UniversityThe Properties and Redshift Evolution of Intermediate-Luminosity Off-Nuclear X-Ray Sources in the Chandra Deep FieldsWe present a sample of 24 intermediate-redshift ($z \approx 0.05-0.3$) off-nuclear X-ray sources that are coincident with optically bright ($V_{606} < 21$) field galaxies within the {\it Chandra} deep fields. These off-nuclear sources have X-ray properties and optical environments similar to intermediate-luminosity X-ray objects (IXOs) in the local universe. We find that the fraction of intermediate-redshift galaxies hosting an off nuclear source with luminosity $L_{\rm X} > 10^{39}$~erg~s$^{-1}$ is suggestively elevated over the local IXO fraction by a factor of $\approx 1.9^{+1.4}_{-1.3}$. A rise in this fraction may be a consequence of the observed increase in star-formation activity with redshift.poster Monday: 'Normal' Galaxies0
17LewisKarenktlewis@milkyway.gsfc.nasa.govNASA GSFCFollow-up of the XMM Slew Survey: 5070 square degrees and countingThe XMM Slew Survey covers 5070 square degrees and is an order of magnitude more sensitive in the 2-12 keV band than previous all-sky surveys, opening up the possibility of studying large numbers of intermediate redshift AGNs. We have begun a follow-up campaign for ~300 sources with 2-12 keV detections. Although most have optical/IR counterparts, only 1/3 have been robustly classifed (including 65 AGNs). Most are classified simply as "Galaxy". SDSS/6dF spectra of some reveal an AGN, while others appear "dull". Our initial efforts focus on these poorly studied galaxies and includes improved X-ray observations, optical spectroscopy and IR/optical imaging.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
18LonsdaleCarolcjl@ipac.caltech.eduIPAC, Caltech & UCSDThe XMM-LSS / SWIRE SurveyWe are imaging ~10 square degrees with 10ks XMM pointings, reaching 5 x 10^-15 erg/s/cm^2 for point sources. Deep imaging with all 7 Spitzer imaging bands is provided by the SWIRE Legacy survey, and deep 5-band optical imaging from the CFHTLS, as well as extensive radio imaging. The primary objectives of the survey are to detect ~150 clusters to z~1; to study the environmental effects of star formation and AGN activity utlizing the Spitzer data; the physics of the group population; and searches for rare objects. We will present highlights of the results so far. The XMM-LSS / SWIRE catalog will be available for public access in Fall 2006.posterI think it would be useful to frame a discussion on the observational front by asking what areas of parameter space are not yet adequately investigated. I am thinking of a 4-dimensionl space: 1. power/luminosity; 2. redshift; 3. length-scales / environments being sampled; 4. wavelength. We need full coverage across all these parameters in order to fully sample all objects types over all timescales, and their dependence on environment.Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
19MarcoAjellomajello@mpe.mpg.deMax-Planck-Institut für extraterrestrische PhysikThe BAT extragalactic hard X-ray surveyThe BAT instrument, on board the Swift observatory, is surveying the hard X-ray sky to unprecedented sensitivities. After 1 year, BAT has covered the whole sky to <1 mCrab (14-195keV). More than half of the detected sources are extragalactic in origin and the majority of those are Seyfert galaxies with various levels of obscuration. We conducted a campaign for optical identification of BAT sources in a selected field and discovered that most of the sources are new Sy2 galaxies. Moreover, BAT data suggest, unexpectedly, that the fraction of Compton Thick sources is ~10%. We present the results of the extragalactic survey and discuss their implications for the unified AGN model and for the synthesis of the X-ray background.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
20NandraKirpalk.nandra@impeiral.ac.ukImperial College LondonSurvey ChallengesChandra and XMM surveys have now resolved most of the X-ray background below 10 keV. While many of the important matters arising are starting to be addressed, almost all the important issues remain controversial or have large uncertainties. These include, but are not limited to a) how AGN activity evolves, and the accretion history; b) the fraction of absorbed objects and any dependence of absorption on, e.g. luminosity or redshift; c) the triggering mechanism for AGN activity; d) its relationship to star formation and galaxy evolution. Reaching robust conclusions requires careful data reduction and analysis, and proper consideration of biases and completeness. These issues and their implications will be discussed.poster Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments 
21OwenRichardro27@star.le.ac.ukUniversity of LeicesterX-ray Emission from Nearby 'Normal' Spiral GalaxiesWe present preliminary results from a survey of nearby late-type spiral galaxies observed by XMM-Newton. We have developed new procedures to study the point source distribution and unresolved emission present. The X-ray luminosity function of the point sources is used to estimate the proportion of unresolved emission which is truly diffuse, and the origins of this diffuse emission are explored by comparison of its morphology to that in other wavebands. Using a sample of 30-40 galaxies, we aim to extract a consistent set of derived X-ray parameters appropriate to late-type spiral galaxies such as our own.poster Monday: 'Normal' Galaxies, Tuesday: AGN correlation functions, LSS, environments 
22ParkShinaespark@cfa.harvard.eduHarvard-SmithsonianA Spitzer-Chandra Survey of AGN in the Extended Groth StripThe All Wavelength Extended Groth Strip International Survey (AEGIS) is a widespread collaborative effort to study sources in the EGS, a 2 degree by 10 arcmin sky field with low column density and high galactic and ecliptic latitude. Here we take advantage of deep Chandra and Spitzer observations of the field to present the infrared properties of X-ray detected sources, including their color-color identification, SED shape, and source variability. We use these properties in order to better understand multi-wavelength AGN identificationposter Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments 
23PollettaMarimcp@auriga.ucsd.eduUniversity of California, San DiegoSpectral Energy Distributions of Hard X-ray selected AGN in the XMDS SurveyThe spectral energy distributions (SEDs) of AGNs and their dependence on luminosity and absorption are characterized in order to evaluate the selection biases of multi-wavelength surveys, understand the nature of elusive AGNs, investigate the origin of AGN red mid-IR colors, and test model predictions for AGNs at high-z and luminosities. This study is based on a hard (2-10 keV) X-ray selected sample from the XMM-Medium Depth Survey (XMDS). The multi-wavelength data set includes optical data from the VVDS, CFHTL surveys, infrared data from the SWIRE survey, and X-ray data from the XMM-LSS survey.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments0
24RovilosEmmanouelerovilos@astro.noa.grIAA-NOARadio observations of the Chandra Deep Field South Are radio sources more obscured?We have cross-correlated data from the Australia Telescope Compact Array (ATCA) with X-ray observations of the southern \emph{Chandra} Deep Fields, reaching flux depths of 60\,$\mu$Jy and $1.3\times 10^{-16}$\,ergs\,cm$^{-2}$\,s$^{-1}$ respectively. Our aim is to check for the existence of correlation between radio emission and obscuration of AGN. Previous works have shown that radio counterparts are preferentially detected toward obscured AGN, which possibly suggests that both radio emission and X-ray absorption are linked with circumnuclear star formation. Searching for radio counterparts among all X-ray detected sources in the two \emph{Chandra} fields we get detection rates of 14\% and 9\% for the CDF-S and the ECDF-S respectively. After the extraction of ``normal'' galaxies and sources not detected in the hard X-ray band (2$-$8\,keV), we found no strong evidence of correlation between the existence of a radio counterpart and X-ray obscuration. For a sizable fr! action of the sources the radio emission is linked star formation, suggested by the \emph{Spitzer} mid-infrared (24\,$\mu$m) and radio correlation. Limiting our sample to those sources selected by their infrared detection again reveals no correlation between X-ray obscuration and radio detection. However, we detect a correlation if we only consider sources having some degree of obscuration. We interpret this result by linking X-ray obscuration with star-forming activity which is anisotropically distributed round the AGN.poster   
25SabirliKivanckivanc@cmu.eduCarnegie Mellon UniversityThe XMM Cluster SurveyThe XCS is a serendipitous X-ray galaxy cluster survey being conducted using archival data taken by ESA's XMM-Newton satellite. Galaxy clusters trace the large scale structure of the universe, and their number density evolution with redshift provides one way to measure cosmological parameters, independent of cosmic microwave background experiments or supernovae cosmology projects. The current status of the survey and the associated NOAO optical imaging survey will be presented.posterHow can we put together a program to conduct a large area X-ray survey for galaxy clusters which can win approval by NASA or ESA?Tuesday: Cluster Formation and Evolution 
26SaezCristiansaez@astro.psu.eduPennsylvania State University.A Study of AGN evolution in the X-ray band.We present results from a statistical analysis of bright radio-quiet AGNs selected from the Chandra deep field surveys in the redshift range of 0.5poster Monday: X-ray luminosity functions and evolution, Tuesday: Cluster Formation and Evolution 
27SmithRebeccarjs47@star.le.ac.ukUniversity of LeicesterDeveloping a photometric redshift code for use with large X-ray selected AGN samplesThe release of large X-ray catalogues enable large samples of X-ray selected AGN to be investigated. To determine evolutionary properties of such a sample, the redshift of each object must be known. Spectroscopically determined redshifts, although accurate, are time consuming to collect. Photometric redshift estimates are more suitable for large surveys. Using samples of known AGN from several fields we cross-correlate to find optical and infra-red counterparts. Using a photometric redshift code written specifically for use with SDSS colours, we develop a method of obtaining accurate photometric redshifts based on known properties of the sources.poster Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments 
28TrouilleLauratrouille@astro.wisc.eduUniversity of Wisconsin-MadisonOptical Properties of the LHN-2 and CLASXS Chandra X-ray Survey SourcesIn this poster, we present the spectroscopic and photometric observations of the X-ray sources detected in a wide- area, moderately deep Chandra X-ray survey of a second field near the Lockman Hole. We combine our results with the previous Steffen et al. 2004 findings for the CLASXS field. We separate the X-ray sources by optical spectral type and examine the colors, apparent and absolute magnitudes, and redshift distributions for the broad-line and non- broad-line active galactic nuclei. We also compare the group structures in the CDFN with those in this Lockman Hole field as well as the CLASXS field in order to investigate if the environments of the X-ray sources evolve with redshift.poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: Cluster Formation and Evolution 
29WilkesBelindabelinda@cfa.harvard.eduSAO  poster Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments