Lyman Break Galaxies
M. Pettini
Abstract: I shall present the results of the latest work by our group on Lyman break galaxies with particular emphasis on:
1. The determination of their Lyman continuum emission;
2. Their emission line spectra at near-infrared wavelengths, obtained with both ISAAC and NIRSPEC; and
3. Their stellar populations and interstellar abundances, now accessible for study with the new Echellette Spectrograph and Imager.

ESO observations of the HDF-S
M. Dennefeld
Abstract: No abstract submitted.

Results from the Caltech Faint Galaxy Redshift Survey
J. Cohen
Abstract: Recent results from the Caltech Faint Galaxy Redshift Survey on galaxy clustering, close pairs and merger rates, the evolution of galaxy morphology with time, galaxy spectral energy distributions, the galaxy luminosity function, and galaxy evolution with redshift in general will be discussed.

Far-UV studies of the HDFs
H. Ferguson
Abstract: Results from a recent HST survey of field galaxies at wavelengths 1600 A and 2300 A will be presented. The observations provide statistics of Lyman-break galaxies at redshifts z < 2.5, offering robust photometric redshifts for moderate-redshift star-forming galaxies fainter than groundbased spectroscopic limits. For galaxies with measured spectroscopic redshifts, the data also provide a measurement of the fraction of Lyman continuum radiation that escapes from the ISM. UV rest-frame morphologies for moderate and low-redshift galaxies allow a straightforward comparison with HDF optical observations of galaxies at redshifts z > 2.5. Finally, the 1600 A observations are used to set a constraint on the diffuse UV background not accounted for by individually detected sources.

Deep multicolor galaxy surveys: constraining models of galaxy formation
A. Fontana
Abstract: Multicolor imaging surveys of extragalactic fields are a powerful tool to study galaxy evolution and formation. I will review our recent results on the analysis of public surveys from HST (HDFN+HDFS) and ESO telescopes (NDF, EIS) as well as the first results of a deep multicolor imaging survey carried on at the Rome Obseravtory with the NTT and the VLT over several extragalactic fields.
Based on a photometric redshifts derived for the whole data sample, we are able to place constraints on several observables that describe the evolution of galaxies at high redshift, such as the UV luminosity density, the luminosity function and the number evolution of massive galaxies. These observables are compared with the prediction of semi-analytic Cold Dark Matter models for galaxy formation and evolution, of which we have developed a new rendition.

IR Surveys
M. Dickinson
Abstract: Since the development of infrared array detectors, deep near-infrared imaging surveys have played an important role for studying galaxy evolution and (optimistically) cosmology. Deep near-IR data offer the only means of tracking familiar rest-frame optical light from galaxies out to redshifts > 1, reducing the impact of both stellar M/L evolution and extinction on source counts and color distributions. I will briefly review some history of deep near-infrared field galaxy surveys, highlighting the ways in which they have influenced our present thinking about galaxy evolution. I will use ground-based and HST/NICMOS near-infrared observations of the Hubble Deep Field North to illustrate some results from current, state-of-the-art near-IR surveys, and look at expectations for the near future that are made possible thanks to larger-format detectors, adaptive optics, multiplexing IR spectrographs, and new space-based facilities such as SIRTF.

Deep ISAAC / VLT imaging of HDF-South
M. Franx
Abstract: No abstract submitted.

First results from the Infrared-Selected SPICES Survey
D. Stern, P. Eisenhardt, S.A. Stanford, B. Holden, P. Rosati, P. Tozzi, R. Elston, K. Wu, H. Spinrad, A. Connolly
Abstract: We present the first results from SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey. Our survey is designed to study galaxy formation and evolution out to z = 2. We have deep ground-based BRIzJK imaging covering 100 square arcminutes split into four fields across the sky. Optical images reach depths of = 25 mag (AB; 3s). The infrared images reach = 23 mag (AB; 3s). We are pursuing spectroscopy of the K < 20 (Vega) sample: we currently have = 500 redshifts from the Keck telescopes. The spectroscopic sample is being used to train photometric redshifts for the complete sample. We discuss preliminary results from this survey, including the surface density and nature of extremely red objects. We detail optical/near-infrared identifications of X-ray sources identified from a deep, 190 ks observation of one field with the Advanced CCD Imaging Spectrometer on the Chandra X-Ray Observatory. We discuss identification fraction, properties, Hubble Space Telescope morphologies, and spectroscopic follow-up of these X-ray sources.
Portions of this work was carried out at the Jet Propulstion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration.

The question of EROs and their link with high-z galaxies
A. Cimatti
Abstract: Extremely red objects (EROs) provide the possibility to constrain the evolution of elliptical galaxies and to study the population of dust reddened high-z objects. I will review the recent results obtained with wide field imaging, HST imaging, deep spectroscopy and submm-mm-radio observations. I will discuss the general implications of such results in the framework of massive galaxy formation and evolution.

ISAAC spectroscopy of z=2.2 H-alpha emitting galaxies in the HDFS
A. Moorwood, P.P van der Werf, J.G. Cuby, E. Oliva
Abstract: A sample of 6 Ha emitting galaxies at z~2.2 discovered in a 2.1 µm narrow band filter survey conducted with SOFI at the NTT has been spectroscopically confirmed using ISAAC at the VLT. Although small, this is the largest sample of such objects established to date. The survey covered ~100 sq. arcmin, including the Hubble Deep Field South, and reached a 3s line flux limit ~ 5x10^-17 erg cm-2 s-1. Curiously, none of these objects fall in the WFPC2 and STIS fields but some lie in the HST flanking fields and in the ESO EIS deep survey. Only one appears to be an interacting system (with two main components within ~10kpc) and several exhibit U band absorption in the Lyman a forest. Based on their Ha fluxes, the typical star formation rates of individual galaxies are around 25 Mo/yr without any correction for extinction. This is up to a factor of 4 higher than SFRs estimated from the rest frame UV continuum fluxes of those observed by HST - consistent with lower extinction at Ha. The observed dispersion velocities are ~100 km s-1 implying that these are relatively well developed systems providing the gas motions are related to mass. Evidence that this is the case is provided by the rotation curve of one galaxy observed under good seeing conditions which implies a terminal velocity of >= 140 km s-1 at r >= 3 kpc - typical of nearby spirals. The luminosity, MB, of this galaxy derived from its infrared H band magnitude lies ~3 mags. above the local Tully - Fisher relationship. Within considerable uncertainties, due to the small size of our sample, the Ha luminosity function at z = 2.2 is the same as measured at z ~1.3 by Yan et al. (1999) using NICMOS on the HST. The corresponding star formation rate density of 0.12 Mo/Mpc3/yr is also consistent with that at z~3-4.5 derived from extinction corrected UV continuum measurements by Steidel et al. (1999).

Lyman-alpha based searches for galaxies with z > 6
R. McMahon
Abstract: I will present recent results on searches for high redshift galaxies based on the detection of the Lyman-alpha emission line with an emphasis on what the future holds for such searches. My talk will include the description of a new instrument that is designed to detect Lyman-alpha galaxies up to redshifts of 10.

The Hubble Deep Fields: untangling evolution from selection biases
S. Driver
Abstract: Differences between the high-z population and low-z population can readily be ascribed to one of two possibilities. Evolution or a selection bias. Distinguishing between these two is difficult but vital if we are to be able to understand and decipher galaxy evolution. Here we introduce the bivariate brightness distribution, this is a method by which we can track selection bias and thereby be assured that the changes we see are real and not due to a change in our selection window.
We illustrate the method and its effectiveness through data from the Hubble Deep Fields and present our conclusions as to the evolution of ellipticals, spirals and irregulars from z=1 to 0.

The Evolution of Galaxy Morphology from high to low redshifts
C. Conselice
Abstract: Galaxy morphologies are one of the few features of galaxies that can be studied in large numbers with deep high resolution imaging. Much of our information about galaxy properties at high redshift must necessarily be derived from these appearances. Current deep fields allow us to reliably study galaxy morphologies, and thus the evolution of galaxy populations out to redshifts beyond z ~ 3. Using a physical morphology system that relates physical features of galaxies to their appearances, we can determine the physical state of a galaxy based only on its gross properties. When these parameters are properly calibrated and tested on simulated data, they are powerful tools for deciphering in a quantitative way how galaxies have evolved. By using a system that contains parameters such as asymmetry, color, and concentration indexes, we can trace changes in the galaxy population due to galaxy interactions, mergers, and star formation from high to low redshifts.

The FORS Deep Field and High-z Galaxies
R. Bender
Abstract:No abstract submitted.

The CADIS search for galaxies at z > 4.7
K. Meisenheimer
Abstract: A central part of the Calar Alto Deep Imaging Survey (CADIS) is a deep emission line survey (Flim ~= 3x10^-20 Wm-2) for primeval Lyman-alpha galaxies at z > 4.7. The survey observations will cover 1/6 square degree in three redshift intervals around z = 4.77, 5.75, 6.57 and are completed to 75%. Survey limits and area are ideally suited to complement existing Lyman-a searches at the bright end and thus constrain the luminosity function. A refined analysis which minimizes known sources of contamination is now available for 1/3 of the survey. Although spectroscopic verification of the Lyman-a candidates is still pending due to our limited access to very large telescopes, the low detected abundance of Lyman-a candidates already implies that the peak of star formation in massive galaxies happened at redshifts z ~= 6 or later.

Kinematics and evolution of intermediate redshift (0.2 < z < 1.3) galaxies
N.P. Vogt
Abstract: We review the status of current observations of the fundamental parameters of intermediate redshift (0.2 < z < 1.3) galaxies. Recent advances in instrumentation of 8-10m class telescopes have made possible detailed measurements of galaxy kinematics and mass, in both the optical and the infrared passbands. By studying such well known star formation indicators as [OII]3727A (in the optical) and H-a (redshifted to the infrared), the internal velocity structure of galaxies can be traced through this entire redshift regime. The combination of throughput and optimum seeing conditions yields spectra which can be combined with high resolution multiband imaging to explore the evolution of galaxies of various morphologies, and to place constraints on current models of galaxy formation.

DEEP: Pre-DEIMOS Results to I ~ 24 on Galaxy Evolution and Kinematics
D.C. Koo
Abstract: For over 6 years, we have used Keck spectra and HST images to undertake deep field surveys of about 1000 distant galaxies to limits I ~ 24. These pilot programs have proven critical in designing and preparing for our intended DEEP survey of 50,000 galaxies to redshifts z ~ 1. Although detection and recognition of such galaxies are not difficult, gathering the wealth of information needed to decipher the physical mechanisms and their role in evolution of diverse galaxy types and environments will require much larger samples and wide wavelength coverage. For this talk, I present some pre-DEIMOS highlights from the DEEP program. These include studies of E/S0's and bulges, disk sizes and their evolution in surface brightness, compact galaxies and their role in galaxy evolution, and high redshift z ~ 3 galaxies. A novel aspect of our surveys is the use of kinematics via line widths or rotation curves to measure the masses of very distant galaxies.

LSS with 2dFGRS
J.A. Peacock
Abstract: No abstract submitted.

Investigating the evolution of galaxy clustering with the Canada-France Deep Fields Survey
H.J. McCracken, O. LeFevre, M. Brodwin , S. Lilly , D. Crampton
Abstract: The Canada-France Deep Fields survey is a large, multi-waveband imaging survey which has been carried out using the University of Hawaii's 8K Camera at CFHT, with additional U-band data being provided by CTIO and KPNO. The survey covers four original fields of the Canada France Redshift Survey, and in total spans one square degree of sky and contains 100,000 galaxies to UBVI(AB)~26. It is one of the largest and deepest surveys completed to date at this depth. In my talk I will present results for the evolution of the colour-selected and mangnitude-selected galaxy clustering derived from this sample. Our large sample of galaxies in combination with four deep fields widely separated on the sky provides the most reliable and accurate measurement of the angular correlation function yet carried out at these depths. Furthermore, the large database of spectroscopic redshifts (>1000) in these fields will permit an accurate calibration of our photometric redshifts and allows to trace the evolution of the field galaxy luminosity function out to z~1 with a large sample of galaxies.

The VIRMOS-VLT Deep Survey
O. Le Fevre
Abstract: The VIRMOS-VLT deep survey is a coordinated approach to study the evolution of galaxies, large-scale structures, AGNs, clusters of galaxies, over the redshift range 0<5+. I will present the survey strategy based on (1) deep imaging over 16deg2 in 4 areas, and (2) on more than 150000 redshifts which will be acquired with the VIMOS and NIRMOS instruments being developed by our team.

The DEIMOS/DEEP survey with the Keck Telescope
M. Davis
Abstract: Beginning mid-2001, the new DEIMOS spectrograph will be used for a redshift survey of ~60,000 galaxies selected to have photo-Z in the range 0.7 < z < 1.4. The survey will have two components, the 1HS will occupy 90 nights of Keck time with 1-hour integrations per field, and the 3HS will occupy 30 nights of Keck time with 3-hour integrations per field. The plan is to observe all galaxies with resolution R~5000, and we expect to observe an average of 130 galaxies per mask. This talk will outline our plans and science goals.

Clustering at High-z
M. Giavalisco
Abstract: No abstract submitted.

Strong clustering of very red galaxies in the Las Campanas IR survey
P.J. McCarthy, R. Carlberg, R. Marzke, A. Firth, H. Chen, R. McMahon, J. Wilson, R. Ellis, S. Persson, A. Oemler, C. Sabbey, J. Lewis
Abstract: We report results from the Las Campanas Infrared Survey – a wide area deep survey aimed at understanding the clustering and evolution of early type galaxies at redshifts near 1. We have completed a survey of 2000 square arc-minutes to a 5 sigma limit of H = 20.5. We have isolated a sample of potential z = 1 early-type systems and EROs by a color cut of I – H > 4. At our limiting depth we measure an average surface density for such objects of 0.3 per square arc-minute. We measure an angular clustering signal that is 8-10 times larger than that of the complete H selected sample. We have used three approaches to characterizing the redshift distribution of the I – H > 4 sample. We will discuss the implications for the 3-dimensional clustering length and the relationship between present-day early type galaxies and red color-selected objects at faint infrared magnitudes.

Weak lensing by large-scale structures
Y. Mellier
Abstract: In the beginning of 2000 4 groups have annouced the detection of cosmic shear signal in their deep images. The cosmic shear produced by weak gravitational lensing of large-scale structures of the universe has an important potential for cosmology, so these detection produced a strong exictement in our community. I will describe the scientific interest of these surveys and our results obtained on 50 fields with the VLT. By using jointly our CFHT and VLT measurements, I will show which kind of constraints we already have on cosmological models and our future prospects.

Lensing Masses of Local Edge-on Galaxies from DEEP VLT imaging
T. Broadhurst
Abstract:Deep high resolution images of local edge-on galaxies have been obtained for comparing the lensing mass derived from distortions of faint background galaxies with the dynamical mass inferred from the disk rotation. First results will be presented showing obvious detections of the disk and halo lensing signal of individual massive galaxies.

The present: the Capodimonte Deep Field. The Future: science with the VST
M. Capaccioli
Abstract: The Astronomical Observatory of Capodimonte (OAC) is carrying out a project, named Capodimonte Deep Field (CDF), of deep multi-color photometry in B,V,R, and intermediate band filters, on a 1°x1° field centered at R.A. = 12h 25m and Dec = -12° 48'. The CDF, which rests on the use of the OAC guaranteed time at the ESO 2.2m WFI, is aimed at providing targets for a variety of galactic and extragalactic programs, such as the detection of distant and/or poor clusters, high redshift QSOs, and intermediate redshift galaxies, with the goal of studying their luminosity functions, colors, clustering, and dynamical properties. This project is also understood by us as a unique opportunity to heavily test the scientific and technical tools for the exploitation of a wide field imager in view of the coming into operation of the VLT Survey Telescope (VST). In other words, the CDF is also a pilot experiment for future surveys to be carried out at the VST. The goals of the OAC community, so far expressed for the use of the OAC time of VST, contemplate the study of the Milky Way structure, i.e. halo population of white dwarfs and detection of MACHOs via lensing, plus stellar and surface photometry of nearby galaxies with an unprecedented field of view and accuracy in the sky removal in the faint outer regions of galaxian haloes. Through narrow-band imaging surveys of extragalactic emission line objects, we plan to investigate objects such as extragalactic PNe or Ly-a emitters, with high accuracy and on a short time scale. Furthermore, being the VST particularly suited for the observational cosmology, studies of deep number counts, of the luminosity functions vs. morphological types, of galaxy correlation functions, and of large scale structure on areas of hundred square degrees are seen within reach of the VST in a time scale of one-two year of observing with this dedicated instrument.

Science with VISTA
W. Sutherland
Abstract: We discuss the science programme and design drivers for VISTA, (Visible Infrared Survey Telescope for Astronomy), which is a 4-metre telescope to be located near Paranal, operational by 2004, with 2 degree visible and 1 degree IR fields.

Clustering of galaxy clusters in CDM Universes
S. White
Abstract: Recent progress in simulating the evolution of structure in Cold Dark Matter cosmologies makes it possible to produce ensembles of artificial Ômock surveysÕ which are large and detailed enough for direct confrontation with ongoing and planned large-scale surveys. I will review some of this work concentrating on evolutionary predictions for the abundance, spatial distribution, structure and galaxy content of galaxy clusters.

Galaxy Clusters as Cosmological Probes
S. Borgani
Abstract: Clusters of galaxies have a long tradition as powerful diagnostics for cosmological models. In particular, their evolution is a sensitive probe for the average density of the Universe and for the nature of cosmic density perturbation. In the first part of my talk I will review recent results that we obtained from the analysis of the ROSAT Deep Cluster Survey (RDCS), which probes the cluster evolution out to z~1.3. In the second part I will discuss the limitations in these cosmological constraints arising from the still partial knowledge of the physics of the intra-cluster medium (ICM). In this context, I will highlight the role that high-resolution hydrodynamical simulations can play for a better understanding of the ICM evolution and its connection with galaxy formation processes.

Optical-Infrared Observations of X-ray Clusters
P. Rosati
Abstract: No abstract submitted.

Optical-Infrared Cluster Surveys
L. Da Costa
Abstract: No abstract submitted.

Physical Properties of High-z Clusters
P. van Dokkum
Abstract: I review recent results on the properties of distant clusters and the galaxies within them, with emphasis on results obtained from deep, large field HST observations. The available evidence suggests that a large fraction of present-day cluster galaxies were assembled or transformed from other morphological types at z<1, although most of their stars were formed at much higher redshift. Direct evidence for recent formation of massive elliptical galaxies is provided by the large number of red mergers in one the most distant clusters studied to date, MS 1054–03 at z=0.83. With NICMOS on HST, high resolution studies of clusters can be pushed beyond z=1. First results will be presented of a morphological study of the galaxy population in a cluster at z=1.27. The Advanced Camera for Surveys (ACS) on HST may revolutionize this field, because it is a factor ~10 more efficient for deep, large field studies than WFPC2.

The HST Advanced Camera and the high-z cluster program
G. Illingworth
Abstract: Over the last five years we have seen a dramatic increase in our understanding of galaxies in distant clusters. While this is due, primarily, to the high resolution imaging capability of HST, the multiobject spectroscopic capability of the Keck telescopes has played a key role. In particular, wide-field, multi-color WFPC2 mosaics with HST of intermediate redshift clusters to z~1, and spectroscopic membership and high S/N spectroscopy with LRIS on Keck, has provided new insights into the nature of elliptical and S0 galaxies in the cluster environment over a wide range of densities. Most ellipticals, and a significant fraction of the S0 population, have large luminosity-weighted ages, suggesting that their stellar populations were formed at redshifts beyond z~2, though the existence of substantial numbers of major mergers in MS 1054-03 at z=0.83 suggests that final assembly of such galaxies may not have occurred until much later for a significant fraction of early-type galaxies. The launch of the HST Advanced Camera, the ACS, in late 2001, combined with a substantial increase in the number of multi-object spectrographs on large telescopes (like NIRMOS and VIRMOS on the VLT, and DEIMOS on Keck), will result in a further dramatic improvement in our ability to utilize galaxies in distant clusters as probes of galaxy formation and evolution in dense environments. This talk will concentrate on the capabilities of the ACS and the goals of the ACS Science Team’s distant cluster program.

Planned SIRTF observations of the AXAF-South and other deep fields
M. Rieke
Abstract: The Guaranteed Time Observering program for the Space Infrared Telescope Facility (SIRTF) includes a survey of 9 square degrees to moderately deep depths and another 2 square degrees very deeply. Smaller areas will be surveyed to the confusion limit at most wavelengths observable with SIRTF. The two square degree area is split between five fields each of which includes a region either surveyed already by Chandra or XMM or on the schedule to be observed. The AXAF Southern Deep Field is included in the program. These surveys will be conducted at the full range of wavelengths available to the SIRTF imagers, IRAC and MIPS. The potential for SIRTF to make contributions to both understanding the far-infrared background discovered by COBE and to understanding galaxly evolution will be discussed.

SCUBA deep fields
A.W. Blain
Abstract: For the first time instruments in the millimetre (mm) and submm wavebands have achieved the sensitivities and mapping speeds required to detect previously unknown high-redshift galaxies in blank-field surveys. These mm and submm surveys have very different selection functions as compared with optical and radio surveys, and so identifying the multi-waveband counterparts to the detected sources is very challenging in general. I will mainly describe the results of surveys made using the SCUBA 850-micron camera at the JCMT, but also include the results of observations made using the MAMBO 1.25-mm camera at the IRAM 30-m telescope and the various mm-wave interferometers. The consequences for our understanding of the evolution of galaxies will be outlined and the prospects of exploiting the fast-evolving developments in submm-wave instrumentation technology will be described. Throughout the presentation the importance of multi-wavelength observations and the complentarity of different deep datasets will be highlighted.

Radio observations of the Hubble Deep Field South – a new class of radio-luminous galaxies?
R. Norris
Abstract: We have made a deep radio survey of the Hubble Deep Field South and its flanking fields at four wavelengths (20, 13, 6, and 3 cm) with the Australia Telescope Compact Array. About 400 hours of telescope time have so far been dedicated to this observation, and we have now reached an rms of about 10 microJy at each wavelength. As in the HDF-N, most of the stronger radio sources do not correspond to bright optical galaxies, and vice versa. Instead, the radio observations tend to sample a different population of galaxies from those that dominate at optical wavelengths. For example, the strongest (~ 1 mJy) radio source in the HDF-S corresponds to a faint (R=27) very reddened galaxy, which has an optical/radio luminosity ratio quite unlike anything seen in the local Universe. The radio and optical luminosities of this and similar galaxies are inconsistent with conventional starburst galaxies, ULIRGs, or radio-loud galaxies. Instead, we speculate that they may consist of a radio-loud active nucleus embedded in a very dusty starburst galaxy - a configuration which is not found at later epochs.

VLA observations of the Chandra Deep Field South X-ray Field
K. Kellermann
Abstract: The VLA has been used for deep surveys of a number of fields between 1.4 and 8 GHz, reaching radio sources as weak as 7 mJy. Most microJy sources are identified with AGN or with distant galaxies having active starforming regions. Some sources, however, remain unidentified even at the limit of the most sensitive optical observations in the Hubble Deep Field. One of the fields surveyed with the VLA is coincident with the Chandra Deep Field South (Giacconi et al. 2000, astro-ph 0007240). The VLA observations of the CDFS reached a limiting flux density (5-s) of 135 and 200 mJy at 4.9 and 1.5 GHz, respectively, with 12 hours of integration at each frequency. We detected about 30 radio sources, of which seven have clear x-ray counterparts including one system of apparently peculiar interacting galaxies at a red shift of 0.07. Significantly more VLA observations will be proposed in order to reach weaker radio sources to complement the planned deep Chandra observations and the existing extensive optical material.

An ultra-deep radio survey: dust-free estimate of the star-formation rate
B. Mobasher
Abstract: A deep radio survey is carried out in the southern hemisphere, using the Australia Telescope Compact Array (ATCA). The survey covers an area of 3 sq. deg. and is complete to 0.1 mJy at 1.4 GHz. A sub-area of 50 arcmin2 of this, is further surveyed to S (1.4 GHz) = 40 micro-Jy. About 50% of the sub-mJy / micro-Jy radio sources are identified with an optical counterpart to R=22.5 mag. For the optically identified sources, redshifts and spectral features (Halpha and [OII]3727), sensitive to star formation, were measured using the 2-degree Field (2dF) spectroscopic facility at the Anglo-Australian Telescope. Using their 2dF spectra, these sources were then classified into absorption line, star-forming and Seyfert galaxies. Surveys selected at radio wavelengths are not biased by dust extinction contrary to optical or Halpha selected surveys. Moreover, at faint flux levels (sub-mJy / micro-Jy regime), the radio surveys are dominated by star-forming galaxies. These data are used to establish the 1.4 GHz and Halpha luminosity function of the star-forming galaxies. The 1.4 GHz and Halpha luminosity densities are then used to estimate the dust-free star-formation rate (SFR) density at z < 1. Comparison between the estimated SFR densities is then used to constrain dust extinction in these objects. Combining these data with the follow-up mid and far-infrared observations by the Infrared Space Observatory (ISO), the nature of the micro-Jy radio population is studied.

ESO Survey for Trans-Neptunian Objects (with O. Hainaut)
O.Hainaut, H.Boehnhardt, A.Delsanti
Abstract: About 250 objects have been discovered in the outer region of the Solar System, the Trans-Neptunian Objects (TNOs). They are believed to be the largest members of the Kuiper Belt, a reservoir for Short Period Comets. Dynamical studies of this population will reveal information on the formation and evolution of the early Solar System. Physical studies of these objects will also give information on the composition of the proto-solar nebula. Because of the way they were tailored, early TNO surveys were sensitive only to fairly nearby objects (i.e. heliocentric distances closer than 50AU). As a consequence, very few objects (about 5) were found at larger distances. Nevertheless, the heliocentric distribution of these objects over a 30–150AU range contains a lot of information that is not accessible while studying only the nearby objects. We embarked into a survey program aimed at discovering many new objects; the observing strategy is finely tuned in order not to introduce a distance selection bias. This project was awarded observation on the ESO/MPI 2.2m with the WFI camera, first as a pilot project, and now as a "Large Program". In order to process the large quantity of data produced by this program, we developed a simple reduction pipeline, and a quite advanced automatic TNO detection program. This program has been extensively tested on artificial and natural data, showing that its efficiency is at least equivalent to that of a trained human, with a gigantic advantage of speed and endurance with respect to any human. We will present these tools, and the first results of the survey, in the perspective of a very large program for which we would request all dark nights on the 2.2m for 3-4 yrs after its de-commissioning.

Deep in a star-forming region with the VLT: looking for sub-Jupiter mass objects
F. Comeron
Abstract: One of the most remarkable results of spectral evolution models for isolated objects with brown dwarf and giant planet masses is the prediction of a large increase in the flux at near-infrared wavelengths over the black body curve for objects of the same temperature and luminosity. These same models also predict rather exotic near-infrared colors for such objects, which have been confirmed by methane brown dwarfs discovered in a variety of surveys. Observationally, this means that very low mass substellar objects are not only detectable, but also relatively easy to identify. While the methane brown dwarfs identified so far are relatively evolved objects with low luminosities and masses in the range of ~10 Jupiter masses, objects with similar temperatures in star forming regions should have masses in the Jupiter-Saturn range. Model predictions indicate that they could be detectable in deep images of star forming complexes within a few hundred parsecs from the Sun. Their identification would be essential not only to demonstrate their existence, but also to provide critical tests on different assumptions on the input physics that have dramatic consequences on the predicted emitted spectrum. Here I report on a deep JHK survey carried out with ISAAC at the VLT of a selected area in the Chamaeleon I complex, one of the most nearby star forming regions where very young brown dwarfs have been recently found. The vast majority of the objects detected have the colors expected from background high-redshift galaxies. However, one object stands out because of its very blue H-K color, while being undetected at J. The unique colors of this object suggest a temperature of order of 1,000 K or less. The blue H-K color may be due to the K-band flux being greatly reduced by methane and molecular hydrogen absorption, while the non-detection at J may indicate an abundant presence of dust in the photosphere. I briefly discuss the main sources of uncertainty involved in the comparison to models, the ways in which the present observations favour different assumptions in the treatment of the model atmospheres, and the constraints that this single detection in the entire observed field sets on the abundance of these objects.

Search for nearby faint high proper motion stars
R.-D. Scholz
Abstract: A new high proper motion survey of the southern sky has been started using a re-reduction of APM measurements of UKST plates (Scholz et al. 2000). The main aim of the survey is to extend the existing proper motion catalogues to fainter magnitudes and to detect new nearby low-luminosity objects. The lower proper motion limit of our survey is defined by the initial 5 arcsec matching radius used for the identification of the objects measured on the R- and BJ-plates and by the epoch difference between the plates in a given field. With typical epoch differences of about 15 years the stars with proper motions larger than 0.3 arcsec/yr can be found. North of d = -20° we are able to detect only very large proper motion stars (with m >1 arcsec/yr) due to the smaller epoch difference of typically 5 years between the UKST R and BJ plates in this region. The ongoing survey covers now already more than 3000 square degrees, and the list of detected high proper motion objects with 10 < R < 20 exceeds 800 with about 50% of them being new discoveries. Spectroscopic follow-up observations of the faintest high proper motion discoveries have confirmed two groups of objects: extremely cool white dwarfs and very late-type red dwarfs/subdwarfs. For accurate estimates of their absolute magnitudes, trigonometric parallax measurements are needed. Among the new high proper motion objects, the coolest subdwarf was discovered in follow-up observations with Keck (Schweitzer et al. 1999). The APM discoveries have also lead to the finding of a new new population of ancient Halo white dwarfs that make up 10% of the Galactic Halo dark matter (Ibata et al. 2000).

Working on other people's "waste": stars in extragalactic surveys
N. Christlieb
Abstract: The primary aims of many deep-field, but also a lot of wide-field surveys, belong to the field of extragalactic astronomy. However, in many surveys also interesting stars can be found. One example is the Hamburg / ESO objective-prism survey (HES), which covers the total southern extragalactic sky down to B ~ 17.5. The HES is primarily targetting bright quasars. Because of its spectral resolution of ~15 Å at Hg, e.g. metal-poor stars, white dwarfs, or carbon stars can be selected efficiently in that survey. In my talk I will give examples of interesting types of stars that could be found in deep fields, and I will give an overview of methods that can be used to select them.

Stellar Surveys and the Omegacam
K. Kuijken
Abstract: No abstract submitted.

The Energetics of the Universe
P. Madau
Abstract: No abstract submitted.

Closing in on the Hydrogen reionization edge signal at z<7.2 with deep STIS/CCD Parallels
R.A. Windhorst, R. Bernstein, N. Collins, P. Plait, B. Woodgate, J. Mather, P. Shaver
Abstract: We present the first results of a project with the Hubble Space Telescope to take STIS parallel spectra to constrain the onset of reionization. This epoch would have left a faint but sharp spectral feature on top of the global background that marks the transition from a neutral to a fully ionized IGM at a predicted redshift zion=5– 10. This "Hydrogen edge" is due to a rapid change in recombination from the Hydrogen Lyman series at z~ zion (Gnedin & Ostriker 1997), and leaves a sharp signal in the recombination spectrum *3 dex below the Zodiacal background (Baltz et al. 1998). HST is unique in that it can constrain this signal with the STIS CCD spectrograph plus its long-slit and G750L grating, covering the range l ~ 5240– 10,270Å or z~3.3– 7.5. The parallel data were scheduled in a fully automated way, and the first data were obtained this summer. The parallels were designed to use only orbital dark-time by padding the start and end of each orbit with direct finder exposures and with STIS calibrations. The contemporaneous STIS calibrations are essential to reduce systematics. We found a faint but significant spectral emission band at 8457Å on top of the Zodiacal foreground, which we identify with a weak atmospheric O-I line that entered some of the parallels (despite the use of mostly orbital dark time), rather than coming from the reionization feature. Knowing the wavelength and significance of detection of this atmospheric O-I line, we set tentative limits the real Hydrogen edge signal of <=2x 10^21 erg/cm2/s/Hz/sr at z_ion>=5. The result from this first pass in the parallel data reduction is set by the limited S/N obtained so far, and we estimate that it will be ultimately limited by CTE effects plus on-orbit radiation damage in the STIS CCDs, by faint on-orbit O-I lines, and by our knowledge of the Zodiacal foreground spectrum. We outline how these constraints to the Hydrogen reionization edge can be further improved.

The CMB
K. Gorski
Abstract: No abstract submitted.

Images of the Early Universe from the BOOMERanG experiment
P. De Bernardis and the BOOMERanG team
Abstract: The Cosmic Microwave Background anisotropy experiment BOOMERanG has recently produced wide, uncontaminated images of the last scattering surface at redshift 1000. Here we describe the technical advances which made this possible, present the images and discuss the associated uncertainties, including the effect of dust in our galaxy. We shortly review the impact of these data in the current theory of inflation and formation of structures in the Universe.

ISO Deep Surveys
D. Elbaz
Abstract: No abstract submitted.

The FIR Background
J.-L. Puget
Abstract: The Cosmic Infrared Background is now measured or well constrained in the whole infrared range. The implications of the ratio of the relative energy content in the infrared and the optical -UV cosmic background will be discussed. The spectrum of the background in the submillimeter range can be used to compute the infrared production rate as a function of redshift. This will be compared with our present understanding of the nature of the sources which makes this background.

Recent results on the X-ray Survey of the Chandra Deep Field South
R. Giacconi, P. Rosati, P. Tozzi, M. Nonino, G. Hasinger, C. Norman, J. Bergeron, S. Borgani, R. Gilli, R. Gilmozzi, W. Zheng
Abstract: We present results from 300 ks of X-ray observations obtained with the Advanced CCD Imaging Spectrometer on the Chandra X-ray Observatory. We reach a flux of 10-16 erg s-1 cm-2 in the 0.5-2 keV soft band and 10-15 erg s-1 cm-2 in the 2-10 keV hard band. Our combined sample now reaches a total of over 200 sources in ~ 0.1 square degrees with S/N ~ 2. We use the FORS-1 imaging spectrometer for identifications, supplemented by the information obtained with the ESO Imaging Survey (EIS) and the ESO Wide Field Imager Survey (WFI). Positional accuracy is ~ 1" in the central 6' . Optical spectra have been obtained for a small fraction of the sample. Cumulative X-ray spectra for sources into broad flux bins show the hardening of the X-ray spectra at fainter fluxes. Hardness ratios for individual sources confirm this result and provide elements for classification. We discuss the LogN-LogS relationship and the discrete source contribution to the integrated X-ray sky flux. We compare Fx/Fopt of the sources observed in this survey to that of ROSAT and note a number of sources which appear to be galaxies that cluster at low Fx/Fopt. The R - K vs R color diagrams show a reddening of the Chandra sources with increasing magnitudes. A few objects have R – K > 6. We compare our findings with previous results and with the predictions of models of the X-ray background.

FIRST and other radio surveys
D.J. Helfand
Abstract: The first radio sky surveys, conducted fifty years ago, opened a new window on the Universe, discovered the first AGN, and provided some of the earliest evidence that the Universe was evolving. The last five years has seen a twenty-fold increase in the number of catalogued radio sources to a total in excess of 2 million. More importantly, a fifty-fold increase in angular resolution over previous surveys allows optical identifications to be obtained for very large source samples. At flux densities above ~1 mJy, the centimetric sky is dominated by AGN; indeed, at high Galactic latitudes, the source population is 99.97% extragalactic. Thus, we are entering a new age in which radio astronomy can contribute in fundamental ways to the study of AGN populations, as well as address questions concerning large-scale structure and the evolution of the Universe. We began collecting Faint Images of the Radio Sky at Twenty-cm with the VLA in April of 1993. The goal is to construct the centimetric equivalent of the Palomar Sky Survey over the same 10,000 deg2 of the northern sky that will be covered by the Sloan Digital Sky Survey. The 20,000 two-million pixel images we have produced to date cover ~8000 deg2 and contain 725,000 radio sources with subarcsecond positions down to the survey threshold of 1.0 mJy. At the same time, the NRAO VLA Sky Survey has completed its coverage of 3 pi steradian at a lower angular resolution and sensitivity, compiling a catalog of over 1.6 million sources, and the Sydney University Molonglo Sky Survey is completing the sky at the most southerly declinations. In this presentation, I will review the success of our source identification programs, present results of the FIRST Bright Quasar Survey which has discovered more than 1000 new bright quasars to date, discuss the implications of these results for such problems as the radio-loud/radio-quiet dichotomy in AGN, and explore some of the broader cosmological questions these new surveys allow us to address such as the detection weak-lensing shear on large scales and the discovery of high redshift clusters.

The evolution of AGNs at 15 micron from the ELAIS from high to low redshift
F. La Franca
Abstract: We present the analysis of the evolution of type 1 and 2 AGNs in the infrared (15 mm) and obtained using data coming from ISO. The analysis is carried out using the new sample of about 30 AGNs down to 1 mJy selected by the European Large Area Survey (ELAIS) with ISO in the S1 region and spectroscopically identified with the 2dF/AAT and with EMMI-EFOSC2 / NTT-3.6 / ESO.

The 2dF QSO redshift survey
B. Boyle
Abstract: I present and discuss some of the results to date from the 2dF QSO redshift survey. Now 50% complete, the current survey comprises over 13000 QSOs with z < 2.9.

QSOs in SDSS
Xiaohui Fan
Abstract: The Sloan Digital Sky will obtain CCD images in five optical bands down to r=23 over 10,000 square degrees of high galactic latitude sky, and take spectra of one million galaxies and 100,000 quasars, including about 500 at z>4 in the next five years. The survey has started formal operation. A high-redshift quasar survey has been carried out using the SDSS commissioning data. We have discovered more than 150 quasars at 3.5 < z < 5.8, including five at z>5. This sample is used to study evolution and the large scale distribution of high-redshift quasars. A very luminous z=5.8 quasar was recently discovered from the SDSS data. I will discuss the implication of this object on the theoretical models of re-ionization and quasar evolution.

Large area hard X-ray surveys and multiwavelength follow-ups
F. Fiore and the HELLAS collaboration
Abstract: We present optical, infrared and radio follow-up of X-ray high energy (2–10 keV, 5–10 keV), large area BeppoSAX and Chandra surveys. The multiwavelength data indicate that the at least half of the X-ray sources are "intermediate" AGN, i.e. type 1.8-1.9 AGN, 'red' quasars, and even a few broad line, blue continuum quasars, all obscured in X-rays by columns of the order of 10^22-23.5 cm-2 but showing a wide dispersion in optical extinction. Intriguingly we also find a few X-ray bright optically dull galaxies. We discuss how our findings can help in discriminating between competing scenarios for the hard X-ray cosmic background.

The Lockman hole and other X-ray deep fields
G. Hasinger
Abstract: I will review the deep X-ray surveys and accompanying multiwavelength coverage in the Lockman Hole, which by now is one of the best-studied areas in the sky. Being the location of the deepest ROSAT survey ever (1.2 Msec exposure), this field has now also been covered by XMM-Newton and the Chandra HRC. Deep and wide optical and NIR coverage, radio and infrared surveys exist to make this a very powerful diagnostic for the cosmic history of active galactic nuclei and their relation to the star forming history as a function of cosmic time.

New results on QSO Absorption lines at the VLT
S. D'dorico
Abstract: The UVES echelle spectrograph installed in October 1999 at the VLT Kueyen telescope is particularly suited for high resolution spectroscopy of relatively faint targets (m=17-19) in the UV and red region of the spectrum. A suite of scientific results extracted from observations of absorption spectra of QSOs obtained during the Commissioning of the instrument is presented. It includes abundances determinations in high redshift DLA systems, the characteristics of the Lyman alpha forest at z ~ 2 and the spatial properties of absorption systems from the spectra of two close line-of-sights.

Optical identification of absorbers
J. Bergeron
Abstract: No abstract submitted.

The metal and baryon content of the IGM at high redshift
M. Haehnelt
Abstract: No abstract submitted.

Damped Lyman-alpha probes of galaxy formation
A.M. Wolfe
Abstract: Evidence is presented that the damped Lya absorption systems are the high-redshift (z > 3) progenitors of galaxy disks. I discuss kinematic evidence that the damped Lya systems are rotating disks. I also discuss implications of the lack of metal-poor damped Lya systems with line width Dv > 100 km s-1. I then present new evidence stemming from correlations between element-abundance ratios and [Fe/H], which connects damped systems to the thick stellar disk of the Galaxy. I discuss the connections between damped Lya systems and Lyman break galaxies, and how [CII] 158 mm emission from damped Lya systems discriminates among competing theories of galaxy formation.

Constraints on the nature of high-redshift damped Lyman-alpha systems
J.P. Gardner
Abstract: We use hydrodynamic cosmological simulations to study damped Lya (DLA) and Lyman Limit (LL) absorption at redshifts z=2-4 in five variants of the cold dark matter scenario: COBE-normalized (CCDM), cluster-normalized (SCDM), and tilted (TCDM) W=1 models, and open (OCDM) and flat (LCDM) W0=0.4 models. The simulations resolve the formation of dense concentrations of neutral gas in halos with circular velocity vc>= vc,res = 125 kms for W=1 and 80 kms for W0=0.4, at z=2. We find a clear relation between HI column density and projected distance to the center of the nearest galaxy, with DLA absorption usually confined to galactocentric radii less than 10-15 kpc and LL absorption arising out to projected separations of 30 kpc or more. We find no evidence of LL absorption occurring outside galactic halos. Considering only absorption in the resolved halos, all five models fall short of reproducing the observed amount of DLA and LL absorption at these redshifts, sometimes by large factors (especially for LL absorption and for TCDM). If any of these cosmological models is correct, then a substantial fraction of DLA and LL absorption must arise in halos with vc<=100 kms; this conclusion seems qualitatively consistent with imaging studies of DLA systems but requires that the large velocity spreads in associated metal-line absorption be boosted by non-equilibrium dynamics. We also find evidence for non-equilibrium effects on the geometric cross section for high column density absorption. Individual absorbers are smaller in more massive halos because gas sinks deeper into the potential wells, but more massive halos tend to have multiple gas concentrations and therefore have larger absorption cross sections on average.

Near-infrared spectroscopy of high-redshift damped Lyman-alpha systems
A.J. Bunker, F.J. Clarke, A.M.N. Ferguson,R.A. Johnson, R.G. McMahon, I.R. Parry, M. Pettini, R.S. Somerville, S.J. Warren
Abstract: We assess the feasibility of detecting star formation in damped Lyman-alpha systems (DLAs) at z>1 through near-infrared spectroscopy using the Cambridge Infrared Panoramic Survey Spectrograph (CIRPASS) integral field unit on the 8-m Gemini telescopes. Although their relation to galaxies is not well established, high-z DLAs contain most of the neutral gas in the Universe, and this reservoir is depleted with time – presumably through star formation. Line emission should be an indicator of star formation activity, but searches based on Lyman-alpha are unreliable because of the selective extinction of this resonant UV line. Using the more robust lines H-alpha/H-beta/[O III] forces a move to the near-infrared at z>1. For line emission searches, spectroscopy is more sensitive than imaging, but previous long-slit spectroscopic searches have been hampered by the likelihood that any star forming region in the DLA galaxy disk would fall outside the narrow slit (see Bunker et al. 1999 MNRAS 309, 875). The integral field unit of CIRPASS will cover sufficient solid angle (13"x4") to intercept these, even in the extreme case of large galactic disks at high redshift. On an 8-m class telescope, star formation rates of 1 solar mass/yr will be reached at z=1.4 with H-alpha in H-band (10sigma, 3hours for for compact regions of star formation and H0=70km/s/Mpc, OmegaM=1). Such star formation rates are below L* for the high-z Lyman-break population, and are comparable locally to the luminous giant HII complexes in M101. It appears that CIRPASS on Gemini will have both the sensitivity and the survey area to measure star formation rates in z>1 damped Lyman-alpha systems. Hence, CIRPASS observations will potentially probe the nature of damped Lyman-alpha systems and address their relation to galaxies.

Molecular hydrogen abundance in the z=3.4 damped Ly-alpha galaxy
S.A. Levshakov, P. Molaro, M. Centurion, S. D'Odorico, P. Bonifacio, and G. Vladilo
Abstract: We have discovered molecular hydrogen H2 in a fourth damped Ly-alpha galaxy with high neutral hydrogen column density, log N(HI) = 21.41 (cm-2) at redshift z = 3.3901 toward the quasar Q0000– 2620. The VLT/UVES observations have allowed for the first time the detection of H2 in gas with very low metallicity, [Fe/H] = – 2, and extremely low dust-to-gas ratio, less than 0.2% of that in the Milky Way. The measured H2 fractional abundance of log f(H2) = – 7.4 is lower than a typical value for Galactic interstellar clouds of high N(HI) column density by a factor of (2-3). Thus this is the lowest H2 fractional abundance ever measured. The derived H2 abundance excellently fits in the linear relation between log f(H2) and [Cr/Zn] measured for other three damped Ly-alpha galaxies showing H2 absorption. This means that the measure of the heavy element depletion, [Cr/Zn], and the molecular hydrogen abundance are strongly correlated at high redshift.

Millimeter Observations of the Early Universe: the MAMBO surveys
F. Bertoldi et al.
Abstract: We summarize results from deep imaging and pointed observations using the Max-Planck Millimeter Bolometer "MAMBO" at the IRAM 30 m telescope. Our observations include sensitive imaging over wide fields (> 100 deg2), plus pointed observations of selected samples of high redshift objects. Our wide field imaging resulted in the detection of over 100 background sources, providing stringent constraints on the mm source counts at sensitivities comparable to typical SCUBA surveys with the advantage of having wide fields to obtain significant counts of bright (>5 mJy) sources, and to study source clustering properties on Mpc scales. Our primary pointed observations have targeted large samples of QSOs at high redshift, including the PSS and SDSS samples. With over 30 detections, these observations have more than quadrupled the number of high redshift QSOs showing thermal dust emission, including the detection of the most distant (z=5.5) dust emitting source yet known.