The European HST science data archive

The design of the Data Management Facility (DMF), the system to handle the data from HST, has been based on the concepts of modularity and flexibility, so that changes inevitably due to occur during the long lifetime of the project could be gracefully accomodated. At the Space Telescope European Coordinating Facility (ST-ECF), new constraints have led the archive group to evolve the system, so to allow a more efficient ingesting of the data imported from the Space Telescope Science Institute (STScI), an easier browsing of the HST catalogue of observations, and a more efficient servicing of archive researchers' retrieval requests. In this paper, the European Science Data Archive of HST data is described, with particular reference to dataflow, hardware and software system structure, operations, differences with DMF, and foreseen developments.Affiliated with the Astrophysics Division, Space Science Dept., ESAThe observations of the NASA/ESA Hubble Space Telescope are obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.     

Utilization of the European Hubble Space Telescope Science Data archive

The Hubble Space Telescope (HST) is a very complex astronomical observing facility, producing data with unique calibration and analysis requirements. The data are collected in Science Data Archives which are available through computer networks world wide. This paper describes the approaches and technologies which are being used at the Space Telescope European Coordinating Facility (ST-ECF) to enable users in different institutions to efficiently work with HST data.     

Astrovirtel—From Archival Research to the Astrophysical Virtual Observatory

Given the high cost of modern astronomical observing facilities it is evident that efforts must be made to optimally exploit the data in order to maximize the return on investment. This concept was first implemented on a large scale for the Hubble Space Telescope, and has since been taken over for other space borne and large ground-based facilities. The European HST Science Data Archive is located at the European Southern Observatory (ESO). It has been extended to include data from ESO telescopes and instruments, especially the Very Large Telescope (VLT) and Wide Field Imager (WFI). It was thus natural to design the archive such that queries could be extended across its full content, regardless of the origin of the data. This constituted a first step toward a virtual observatory. The Astrovirtel program, first established in 1999–2000 with funding provided by the European Commission, makes it possible for scientists to use this facility for their investigations. At the same time it allowed us to establish science requirements for archive cross queries, and to define capabilities required for VO's. Recently the European Commission decided to provide the funding for the implementation of the Astrophysical Virtual Observatory (AVO). This will include several European observatories and scientific organizations. It is being developed in close coordination with the US National Virtual Observatory.     

Understanding physical processes in the diffuse ISM using high-resolution UV spectroscopy

Our understanding of the important physical processes operating in the diffuse interstellar medium (ISM) has advanced in recent years from the analysis of high-resolution ultraviolet (UV) spectra obtained with the Hubble Space Telescope (HST) and the Far-Ultraviolet Spectrograph Explorer (FUSE) and from high-fidelity simulations of the kinematics and energetics of the ISM. Nevertheless, much remains to be learned from observations with the Space Telescope Imaging Spectrograph (STIS) instrument on HST and spectrographs on the World Space Observatory (WSO). I will describe several major unanswered questions and suggest how future UV observations can answer these questions. I will also summarize the instrument requirements needed for a future UV spectroscopic mission and recommend how to achieve a successful mission.     

STAGES: the Space Telescope A901/2 Galaxy Evolution Survey

We present an overview of the Space Telescope A901/2 Galaxy Evolution Survey (STAGES). STAGES is a multiwavelength project designed to probe physical drivers of galaxy evolution across a wide range of environments and luminosity. A complex multicluster system at   z ∼ 0.165  has been the subject of an 80-orbit F606W Hubble Space Telescope (HST) /Advanced Camera for Surveys (ACS) mosaic covering the full     span of the supercluster. Extensive multiwavelength observations with XMM–Newton , GALEX, Spitzer , 2dF, Giant Metrewave Radio Telescope and the 17-band COMBO-17 photometric redshift survey complement the HST imaging. Our survey goals include simultaneously linking galaxy morphology with other observables such as age, star formation rate, nuclear activity and stellar mass. In addition, with the multiwavelength data set and new high-resolution mass maps from gravitational lensing, we are able to disentangle the large-scale structure of the system. By examining all aspects of an environment we will be able to evaluate the relative importance of the dark matter haloes, the local galaxy density and the hot X-ray gas in driving galaxy transformation. This paper describes the HST imaging, data reduction and creation of a master catalogue. We perform the Sérsic fitting on the HST images and conduct associated simulations to quantify completeness. In addition, we present the COMBO-17 photometric redshift catalogue and estimates of stellar masses and star formation rates for this field. We define galaxy and cluster sample selection criteria, which will be the basis for forthcoming science analyses, and present a compilation of notable objects in the field. Finally, we describe the further multiwavelength observations and announce public access to the data and catalogues.     

Prospects for astrometry with the Hubble Space Telescope

The Hubble Space Telescope (HST), a large optical telescope having an aperture of 2.4 meters and a length of 8.8 meters, is being developed by the National Aeronautics and Space Administration. This telescope will be placed into earth orbit by the space shuttle. Astrometric observations with the HST are made using a Fine Guidance Sensor which is capable of measuring the position of one object relative to another with an accuracy of ±0.002 arcseconds. The astrometric user of HST will be provided with an Astrometric Data Reduction Software package (ADRS). The variety of astrometric problems to be investigated with HST is discussed.     

超轻量镜面系统的研制

空间望远镜的研制一直要求系统的轻量化,美国宇航局（NASA）最近研制的韦伯太空望远镜,其主镜系统面密度相对于哈勃空间望远镜已大幅减轻。在韦伯望远镜主镜系统的研制过程中,NASA开展了一系列关于超轻量镜面系统的验证计划,多家机构拿出多个方案参与竞标。本文选取几个比较典型的方案,介绍这些镜面系统的设计思想、结构、材料、加工以及相关测试结果,期望能对国内相关方面的工作提供参考。     

The VOISE algorithm: a versatile tool for automatic segmentation of astronomical images

The auroras on Jupiter and Saturn can be studied with a high sensitivity and resolution by the Hubble Space Telescope ( HST ) ultraviolet (UV) and far-ultraviolet Space Telescope Imaging Spectrograph (STIS) and Advanced Camera for Surveys (ACS) instruments. We present results of automatic detection and segmentation of Jupiter's auroral emissions as observed by the HST ACS instrument with the VOronoi Image SEgmentation (VOISE). VOISE is a dynamic algorithm for partitioning the underlying pixel grid of an image into regions according to a prescribed homogeneity criterion. The algorithm consists of an iterative procedure that dynamically constructs a tessellation of the image plane based on a Voronoi diagram, until the intensity of the underlying image within each region is classified as homogeneous. The computed tessellations allow the extraction of quantitative information about the auroral features, such as mean intensity, latitudinal and longitudinal extents and length-scales. These outputs thus represent a more automated and objective method of characterizing auroral emissions than manual inspection.     

High resolution imaging of Pluto and Charon with the Faint Object Camera of the Hubble Space Telescope

Images of the Pluto-Charon system were obtained with the Faint Object Camera (FOC) of the Hubble Space Telescope (HST) with the aim of determination of radii, fluxes, and albedos. The resolution of the already diffraction limited images was further improved by image restoration, yielding indications of surface albedo distributions which are qualitatively consistent with models derived from observations of Pluto-Charon mutual eclipses.Based on Observations with the NASA-ESA Hubble Space Telescope, which is operated by AURA, Inc., under NASA contract NAS 5-26555.     

Hubble Space Telescope observations of SV Cam – I. The importance of unresolved star-spot distributions in light-curve fitting

We have used maximum entropy eclipse-mapping to recover images of the visual surface brightness distribution of the primary component of the RS CVn eclipsing binary SV Cam, using high-precision photometry data obtained during three primary eclipses with Space Telescope Imaging Spectrograph aboard the Hubble Space Telescope ( HST ). These were augmented by contemporaneous ground-based photometry secured around the rest of the orbit. The goal of these observations was to determine the filling factor and size distribution of star-spots too small to be resolved by Doppler imaging. The information content of the final image and the fit to the data were optimized with respect to various system parameters using the χ² landscape method, using an eclipse-mapping code that solves for large-scale spot coverage. It is only with the unprecedented photometric precision of the HST data (0.000 15 mag) that it is possible to see strong discontinuities at the four contact points in the residuals of the fit to the light curve. These features can only be removed from the residual light curve by the reduction of the photospheric temperature, to synthesize high unresolvable spot coverage, and the inclusion of a polar spot. We show that this spottedness of the stellar surface can have a significant impact on the determination of the stellar binary parameters and the fit to the light curve by reducing the secondary radius from  0.794 ± 0.009  to  0.727 ± 0.009 R_⊙  . This new technique can also be applied to other binary systems with high-precision spectrophotometric observations.     

The GALEX public archive at MAST

The Galaxy Evolution Explorer (GALEX) was successfully launched on April 28, 2003. Over the last 7 years, the GALEX mission has expanded our understanding of the process of star formation and galaxy evolution. GALEX data, consisting of far-UV (1344-1786A) and near-UV (1771-2831A) imaging over most of the sky, and grism spectroscopy, are available to the entire astronomical community and to the general public via the Multi-mission Archive at Space Telescope (MAST). The main characteristics and access tools to the large data archive (16TB) are presented. Groups within the GALEX Science Team, and the MAST archive teams, have undertaken complementary projects to conduct all-sky searches for time-variable and transient sources within GALEX data (e.g. Welsh et al. in Astron. J. 130:823, 2005; Wheatley et al. in Astron. J. 136:259, 2008). Results and tools for variability searches developed by MAST during this process, will be made available to the general community.     

The James Webb Space Telescope and its Infrared Detectors

The James Webb Space Telescope (JWST) was conceived as the scientific successor to the Hubble Space Telescope (HST) and Spitzer Space Telescope. The instrument suite provides broad wavelength coverage and capabilities aimed at four key science themes: 1) The end of the dark ages: first light and reionization, 2) The assembly of galaxies, 3) The birth of stars and protoplanetary systems, and 4) Planetary systems and the origins of life. To accomplish these ambitious goals, JWST's detectors provide state-of-the-art performance spanning the λ = 0.6–28 μm wavelength range. In this paper, we describe JWST with an emphasis on its infrared detectors.     

The Next Generation Space Telescope

The design life time of the Hubble Space Telescope will nominally end in 2005. Even though it might be possible to extend the operational life beyond that date it is evident that a successor to Hubble must be planned for now. Based on the report ‘HST and Beyond’ (Dressler 1996)) and aligned with the NASA ‘Origins’ program a study has been initiated to explore options for a telescope with an aperture of larger than 4 meters and possibly as large as 8 meters, optimized for the near infrared (≈ 1-5 micron) to be placed in an orbit far from Earth. The study started in December 1995 and has been proceeding with considerable momentum. At the current time three studies have been completed (NASA in-house, TRW, and Lockheed), which are being used to explore technological and programmatic challenges. The studies are to be merged. It is impressive to see what can be done with existing technology and within the capabilities of existing organizational arrangements. The goal is to complete the study within one year with the goal of entering into phase A as soon as possible. Formal agreements between ESA and NASA will have to be negotiated if Europe is to play a meaningful role in this exercise. Without such agreements, it is clear that European astronomers will not have access to the NGST in the way that they currently enjoy the opportunities provided by the HST. This revised version was published online in July 2006 with corrections to the Cover Date.     

Detailed study of B037 based on HST images

B037 is of interest because it is both the most luminous and the most highly reddened cluster known in M31.Deep observations and high spatial resolution images with the Advanced Camera for Surveys on the Hubble Space Telescope(HST) first showed that this cluster is crossed by a dust lane.Photometric data in the F606W and F814W filters obtained in this paper indicate that colors of(F606W-F814W) in the dust lane are redder-0.4 mag than ones in the other regions of B037.The HST images show that this dust lane ...     

Major prospects of exoplanet astronomy with the World Space Observatory–UltraViolet mission

The success of the International Ultraviolet Explorer (IUE) first and then of the STIS and COS spectrographs on-board the Hubble Space Telescope (HST) demonstrate the impact that observations at UV wavelengths had and are having on modern astronomy. Several discoveries in the exoplanet field have been done at UV wavelengths. Nevertheless, the amount of data collected in this band is still limited both in terms of observed targets and time spent on each of them. For the next decade, the post-HST era, the only large (2-m class) space telescope capable of UV observations will be the World Space Observatory–UltraViolet (WSO–UV). In its characteristics, the WSO–UV mission is similar to that of HST, but all observing time will be dedicated to UV astronomy. In this work, we briefly outline the major prospects of the WSO–UV mission in terms of exoplanet studies. To the limits of the data and tools currently available, here we also compare the quality of key exoplanet data obtained in the far-UV and near-UV with HST (STIS and COS) to that expected to obtain with WSO–UV.     

Unusual comets (?) as observed from the Hubble Space Telescope

In separate projects, the Hubble Space Telescope has been used to assess the nature of 3 unusual objects: Chiron, Pholus and P/Shoemaker-Levy 9. This paper will compare these objects and discuss how the unique capabilities of the HST may be used to address the issue of cometary activity in each. Chiron, which has exhibited obvious cometary characteristics for several years, might have a bound dust coma that is unresolvable from the ground. In an attempt to directly observe this bound coma, we have obtained a series of images of Chiron with the HST Planetary Camera. Inner coma structure out to 0.″2 has been detected. From these observations we infer a low bulk nucleus density for Chiron. Both HST and ground-based images of 5145 Pholus have been obtained to search for evidence of activity. The ground-based data give the most sensitive limits; however, it is shown that the WFPC-2 on HST can give limits 2–3 orders of magnitude more sensitive than conventional ground-based limits. Finally, as part of a collaborative effort, we have been obtaining HST observations of SL9 in order to determine the fragment sizes and to assess their nature (i.e., cometary vs. asteroid). Both ground-based observations from the UH 2.2m telescope on Mauna Kea and HST observations show that the near-nucleus dust is redder than the sun. While FOS spectra did not detect OH emission, the WFPC-2 HST data show that the inner coma remained very circular from July 1993 up until 2 weeks prior to impact, implying continued production of dust.     

The cosmic origins spectrograph: capabilities and prelaunch performance

The Cosmic Origins Spectrograph (COS) is an ultraviolet spectrograph scheduled for installation in the Hubble Space Telescope (HST) during HST Servicing Mission 4, currently planned to occur in August 2008. COS was designed to maximize sensitivity to faint point sources, and will provide limiting sensitivities at moderate spectral resolutions (R～20,000) that are a factor of 2 to >10 times better than those provided by previous ultraviolet spectrographs on HST. Here, we present an overview of the some of the science areas that will be addressed by COS observations and provide a summary of the capabilities of COS and the expected on-orbit performance.     

The space density of low-redshift active galactic nuclei

We present a new determination of the optical luminosity function (OLF) of active galactic nuclei (AGN) at low redshifts ( z <0.15) based on Hubble Space Telescope ( HST ) observations of X-ray-selected AGN. The HST observations have allowed us to derive a true nuclear luminosity function for these AGN. The resulting OLF illustrates a two power-law form similar to that derived for quasi‐stellar objects (QSOs) at higher redshifts. At bright magnitudes, M _B <−20, the OLF derived here exhibits good agreement with that derived from the Hamburg/European Southern Observatory (ESO) QSO survey. However, the single power-law form for the OLF derived from the Hamburg/ESO survey is strongly ruled out by our data at M _B >−20. Although the estimate of the OLF is best fitted by a power-law slope at M _B <−20.5 that is flatter than the slope of the OLF derived at z >0.35, the binned estimate of the low-redshift OLF is still consistent with an extrapolation of the z >0.35 OLF based on pure luminosity evolution.     

Pixel-based correction for Charge Transfer Inefficiency in the Hubble Space Telescope Advanced Camera for Surveys

Charge Transfer Inefficiency (CTI) due to radiation damage above the Earth's atmosphere creates spurious trailing in Hubble Space Telescope ( HST ) images. Radiation damage also creates unrelated warm pixels – but these happen to be perfect for measuring CTI. We model CTI in the Advanced Camera for Surveys (ACS)/Wide Field Channel and construct a physically motivated correction scheme. This operates on raw data, rather than secondary science products, by returning individual electrons to pixels from which they were unintentionally dragged during readout. We apply our correction to images from the HST Cosmic Evolution Survey (COSMOS), successfully reducing the CTI trails by a factor of ∼30 everywhere in the CCD and at all flux levels. We quantify changes in galaxy photometry, astrometry and shape. The remarkable 97 per cent level of correction is more than sufficient to enable a (forthcoming) reanalysis of downstream science products and the collection of larger surveys.