Hans-Martin Adorf

The Hubble Deep Field: Observations, data reduction, and galaxy photometry

The Hubble Deep Field (HDF) is a Director’s Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground-based telescopes. The observations were made from 18 to 30 December 1995, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.

Radio-loud Narrow-Line Type 1 Quasars

We present the first systematic study of (non-radio-selected) radio-loud narrow-line Seyfert 1 (NLS1) galaxies. Cross-correlation of the Catalogue of Quasars and Active Nuclei with several radio and optical catalogs led to the identification of ~11 radio-loud NLS1 candidates, including four previously known ones. This study almost triples the number of known radio-loud NLS1 galaxies if all candidates are confirmed. Most of the radio-loud NLS1 galaxies are compact, steep-spectrum sources accreting close to or above the Eddington limit. The radio-loud NLS1 galaxies of our sample are remarkable in that they occupy a previously rarely populated regime in NLS1 multiwavelength parameter space. While their [O III]/Hβ and Fe II/Hβ intensity ratios almost cover the whole range observed in NLS1 galaxies, their radio properties extend the range of radio-loud objects to those with small widths of the broad Balmer lines. Their black hole masses are generally at the upper observed end among NLS1 galaxies but are still unusually small in view of the radio loudness of the sources. Among the radio-detected NLS1 galaxies, the radio index R is distributed quite smoothly up to the critical value of R 10 and covers about 4 orders of magnitude in total. Statistics show that ~7% of the NLS1 galaxies are formally radio-loud, while only 2.5% exceed a radio index R > 100. Implications for NLS1 models are discussed. Several mechanisms are considered as explanations for the radio loudness of the NLS1 galaxies and for the lower frequency of radio-loud galaxies among NLS1 galaxies than among quasars. While properties of most sources (with two to three exceptions) generally do not favor relativistic beaming, the combination of accretion mode and spin may explain the observations.

Grid-Based Data Stream Processing in e-Science

The field of e-science currently faces many challenges. Among the most important ones are the analysis of huge volumes of scientific data and the connection of various sciences and communities, thus enabling scientists to share scientific interests, data, and research results. These issues can be addressed by processing large data volumes on-thefly in the form of data streams and by combining multiple data sources and making the results available in a network. In this paper, we demonstrate how e-science can benefit from research in computer science in the field of data stream management. In particular, we are concerned with processing multiple data streams in grid-based peer-to-peer (P2P) networks. We introduce spatial matching, which is a current issue in astrophysics, as a real-life e-science scenario to show how a data stream management system (DSMS) can help in efficiently performing associated tasks. We describe our new way of solving the spatial matching problem and present some evaluation results. In the course of the evaluation, our DSMS StarGlobe proves to be a valuable computing platform for astrophysical applications.

The radio-loud narrow-line quasar SDSS J172206.03+565451.6

We report identification of the radio-loud narrow-line quasar SDSS J172206.03+565451.6, which we found in the course of a search for radio-loud narrow-line active galactic nuclei (AGNs). SDSS J172206.03+565451.6 is only about the fourth securely identified radio-loud narrow-line quasar and the second-most radio loud, with a radio index R1.4 ≈ 100-700. Its black hole mass, MBH (2-3) × 107 M☉ estimated from Hβ line width and 5100 A luminosity, is unusually small given its radio loudness, and the combination of mass and radio index puts SDSS J172206.03+565451.6 in a scarcely populated region of MBH-R diagrams. SDSS J172206.03+565451.6 is a classical narrow-line Seyfert 1-type object with FWHMHβ 1490 km s-1, an intensity ratio of [O ]/Hβ 0.7, and Fe II emission complexes with Fe λ4570/Hβ 0.7. The ionization parameter of its narrow-line region, estimated from the line ratio [O ]/[O ], is similar to Seyferts, and its high ratio of [Ne ]/[Ne ] indicates a strong EUV-to-soft X-ray excess. We advertise the combined usage of [O ]/[O ] and [Ne ]/[Ne ] diagrams as a useful diagnostic tool to estimate ionization parameters and to constrain the EUV-soft X-ray continuum shape relatively independently from other parameters.

From Newton to Einstein – N-body dynamics in galactic nuclei and SPH using new special hardware and astrogrid-D

The dynamics of galactic nuclei containing multiple supermassive black holes is modelled including relativistic dynamics. It is shown that for certain initial conditions there is no stalling problem for the relativistic coalescence of supermassive black hole binaries. This astrophysical application and another one using a smoothed particle hydrodynamics code are our first use cases on a new computer architecture using GRAPE and new MPRACE accelerator cards based on reconfigurable chips, developed in the GRACE project. We briefly discuss our science applications and first benchmarks obtained with the new hardware. Our present architecture still relies on the GRAPE special purpose hardware (not reconfigurable), but next generations will focus on new architectural approaches including custom network and computing architectures. The new hardware is embedded into national and international grid infrastructures.

AstroGrid-D: Grid technology for astronomical science

Abstract We present status and results of AstroGrid-D, a joint effort of astrophysicists and computer scientists to employ grid technology for scientific applications. AstroGrid-D provides access to a network of distributed machines with a set of commands as well as software interfaces. It allows simple use of computer and storage facilities and to schedule or monitor compute tasks and data management. It is based on the Globus Toolkit middleware (GT4). Chapter 1 describes the context which led to the demand for advanced software solutions in Astrophysics, and we state the goals of the project. We then present characteristic astrophysical applications that have been implemented on AstroGrid-D in chapter 2. We describe simulations of different complexity, compute-intensive calculations running on multiple sites (Section 2.1 ), and advanced applications for specific scientific purposes (Section 2.2 ), such as a connection to robotic telescopes (Section 2.2.3 ). We can show from these examples how grid execution improves e.g. the scientific workflow. Chapter 3 explains the software tools and services that we adapted or newly developed. Section 3.1 is focused on the administrative aspects of the infrastructure, to manage users and monitor activity. Section 3.2 characterises the central components of our architecture: The AstroGrid-D information service to collect and store metadata, a file management system, the data management system, and a job manager for automatic submission of compute tasks. We summarise the successfully established infrastructure in chapter 4, concluding with our future plans to establish AstroGrid-D as a platform of modern e-Astronomy.