Paola Amico

THE TEAM KECK TREASURY REDSHIFT SURVEY OF THE GOODS-NORTH FIELD

We report the results of an extensive imaging and spectroscopic survey in the Great Observatories Origins Deep Survey (GOODS)-North field completed using DEIMOS on the Keck II telescope. Observations of 2018 targets in a magnitude-limited sample of 2911 objects to RAB = 24.4 yield secure redshifts for a sample of 1440 galaxies and active galactic nuclei (AGNs) plus 96 stars. In addition to redshifts and associated quality assessments, our catalog also includes photometric and astrometric measurements for all targets detected in our R-band imaging survey of the GOODS-North region. We investigate various sources of incompleteness and find the redshift catalog to be 53% complete at its limiting magnitude. The median redshift of z = 0.65 is lower than in similar deep surveys because we did not select against low-redshift targets. Comparison with other redshift surveys in the same field, including a complementary Hawaii-led DEIMOS survey, establishes that our velocity uncertainties are as low as σ ≈ 40 km s-1 for red galaxies and that our redshift confidence assessments are accurate. The distributions of rest-frame magnitudes and colors among the sample agree well with model predictions out to and beyond z = 1. We will release all survey data, including extracted one-dimensional and sky-subtracted two-dimensional spectra, thus providing a sizable and homogeneous database for the GOODS-North field, which will enable studies of large-scale structure, spectral indices, internal galaxy kinematics, and the predictive capabilities of photometric redshifts.

Io: the movie

The Keck II Adaptive Optics system and the NIRC2 camera provide a unique facility for high angular resolution imaging and spectroscopy in the near infrared. In this paper, we present the result of a unique project to map the entire surface of Io in the thermal infrared (Lp band centered at 3.8 μm). This project was undertaken by a team from the W. M. Keck Observatory and UC Berkeley to illustrate the power of this instrumentation. The 75-milliarcsec-resolution images, corresponding to ~200 km of linear spatial resolution on Io, have been combined to build a thermal infrared map of the entire satellite. We have identified 26 hot spots including one that was undetected by the Galileo mission. A movie and a Java applet featuring a volcanically active rotating satellite were created.

ESO’s New CCD Testbench

During the forthcoming years, ESO will implement a large number of CCDs in optical instruments for the Paranal and La Silla observatories. An important step in this process is the CCD characterization and optimization that is done after the device is received from the manufacturer. In order to accommodate the new large CCDs and to interface to the new FIERA controller, ESO is building a new CCD testing facility in Garching. Among the measurements that will be made with this new facility are: quantum efficiency, conversion factor, charge transfer efficiency, dark current, read out noise and cosmetic quality.

Is ESO's adaptive optics facility suited for MCAO?

As of 2013, the ESOs VLT will be equipped with the Adaptive Optics Facility for Ground Layer and Laser Tomography adaptive optics assisted imaging and spectroscopy, using a Deformable Secondary Mirror and four Laser Guide Stars. Following the successful experience of the MAD demonstrator, we initiated a speculative study to evaluate the performance gain obtained by implementing a type of Multi-Conjugate Adaptive Optics correction that benefits from the unique features provided by the AOF. In this paper we present the basic concept and provide a first estimation of the correction performance obtained in the near infrared.

The Detector Systems of the Keck Observatory: UV to 25 Microns

We provide an overview of the Keck Observatory, its instrumentation, detector systems, and plans for new instruments and detector upgrades. Even though the Keck instrumentation is older than that of the new 8 meter telescopes, in several cases the Keck detector systems are leaders in their class. However, in winning the race for the first very large telescope, the Keck Observatory has paid a price in terms of performance, lack of standardization and difficulty in maintenance. We discuss these challenges and our plans and dreams for ensuring that the Keck Observatory has the detector systems needed to stay at the forefront of astronomy.

Highlights of "Scientific Detectors Workshop 2002" The workshop of (in)famous characters in the detector community

This paper provides an overview of the “Scientific Detectors Workshop 2002”, a 5 day meeting held on the Big Island of Hawaii in June 2002. The purpose of this workshop, which is held every 3 years, is to bring together the leading scientists and engineers working in the field of optical and infrared detectors. The 125 participants came from 14 countries on 6 continents and included representation from every major detector designer/manufacturer and 27 astronomical observatories. This paper is a synthesis of the information presented at the workshop. In order to provide context, we begin with an introduction to the use of optical/IR detectors in astronomy and the basic steps in light detection. We then present the major developments in optical and infrared detectors. We conclude with information about the 2002 workshop format and give advance notice of the next workshop, scheduled for 2005.