Astronomical instrumentation

Abstract:

Some of the most 'active' galaxies in the Universe are obscured by large quantities of dust and emit a substantial fraction of their bolometric luminosity in the infrared. Observations of these infrared luminous galaxies with the Infrared Space Observatory (ISO) have provided a relatively unabsorbed view to the sources fuelling this active emission. The improved sensitivity, spatial resolution and spectroscopic capability of ISO over its predecessor Infrared Astronomical Satellite (IRAS) of enabled significant advances in the understanding of the infrared properties of active galaxies. ISO surveyed a wide range of active galaxies which, in the context of this review, includes those powered by intense bursts of star formation as well as those containing a dominant active galactic nucleus (AGN). Mid-infrared imaging resolved for the first time the dust enshrouded nuclei in many nearby galaxies, while a new era in infrared spectroscopy was opened by probing a wealth of atomic, ionic and molecular lines as well as broad band features in the mid-and farinfrared. This was particularly useful, since it resulted in the understanding of the power production, excitation and fuelling mechanisms in the nuclei of active galaxies including the intriguing but so far elusive ultraluminous infrared galaxies. Detailed studies of various classes of AGN and quasars greatly improved our understanding of the unification scenario. Far-infrared imaging and photometry revealed the presence of a new very cold dust component in galaxies and furthered our knowledge of the far-infrared properties of faint starbursts, ULIGs and quasars. We summarise almost nine years of key results based on ISO data spanning the full range of luminosity and type of active galaxies. © 2005 Springer.

Abstract:

We are using adaptive optics on Keck and the VLT to probe the dynamics and star formation in Seyfert and QSO nuclei, obtaining spatial resolutions better than 0.1" in the H- and K-bands. The dynamics are traced via the 2.12um H_2 1-0S(1) line, while the stellar cluster is traced through the CO 2-0 and 6-3 absorption bandheads at 2.29um and 1.62um respectively. Matching disk models to the H_2 rotation curves allows us to study nuclear rings, bars, and warps; and to constrain the mass of the central black hole. The spatial extent and equivalent width of the stellar absorption permits us to estimate the mass of stars in the nucleus and their contribution to the emission. Here we report on new data for I Zwicky 1, Markarian 231, and NGC 7469.

Abstract:

The ROSAT-European Southern Observatory (ESO) flux-limited X-ray (REFLEX) galaxy cluster survey and the Two-degree Field Galaxy Redshift Survey (2dFGRS), respectively, comprise the largest, homogeneous X-ray selected cluster catalogue and completed galaxy redshift survey. In this work, we combine these two outstanding data sets in order to study the effect of the large-scale cluster environment, as traced by X-ray luminosity, on the properties of the cluster member galaxies. We measure the LX - σr relation from the correlated data set and find it to be consistent with recent results found in the literature. Using a sample of 19 clusters with LX ≥ 0.36 × 10⁴⁴ erg s^-1 in the 0.1-2.4 keV band, and 49 clusters with lower X-ray luminosity, we find that the fraction of early spectral type (η ≤ -1.4), passively evolving galaxies is significantly higher in the high-LX sample within A 200- We extend the investigation to include composite bj cluster luminosity functions, and find that the characteristic magnitude of the Schechter-function fit to the early-type luminosity function is fainter for the high-Lx sample compared to the low-Lx sample (ΔM* = 0.58 ± 0.14). This seems to be driven by a deficit of such galaxies with MbJ, ∼ -21. In contrast, we find no significant differences between the luminosity functions of star-forming, late-type galaxies. We believe these results are consistent with a scenario in which the high-LX clusters are more dynamically evolved systems than the low-LX clusters. © 2005 RAS.

Abstract:

Infrared bright galaxies (LIRGs and ULIRGs) represent the bulk of the cosmic infrared background and play a major role in the cosmic star formation and accretion histories. For this reason they have been subject of intensive studies at all wavelengths. However, being very dusty galaxies, one of the key wavelength range to understand their evolutionary stages and the physic involved, is the Mid-Far-Infrared and sub-millimeter window. Previous (IRAS and ISO) and current (SPITZER) infrared missions, already shed light on the nature and the evolution of these galaxies, but still many phenomena lack of a complete understanding. For example, the processes triggering the starburst and AGN activities as well as trends with the interaction stage, are not well established yet, partially because at FIR wavelengths it has not been possible so far to spatially resolve these different components even in nearby objects. With its passively cooled 3.5 meter telescope, HERSCHEL will offer this opportunity for the first time. In particular, the PACS instrument, is unique for tackling some important open issues thanks to its spectro imaging capability at FIR wavelengths. We will illustrate some of these exciting new opportunities using examples from the Guaranteed Time program on infrared bright galaxies, that is currently being developed. ISO has undoubtedly shown that the use of Mid-Far-infrared spectroscopy is a powerful tool for establishing the physical conditions of the ISM and separating the starburst and AGN activity contributions which often coexist in (U)LIRGs. However, such a coexistence makes the central regions of (U)LIRG very peculiar such that we expect the ISM in their central regions to be very different than in normal star-forming galaxies. One known example is the fact that ultra luminous infrared galaxies have less [CII] emission w.r.t. the total FIR emission ([CII] deficiency) than what is found in normal galaxies. This result, found in several studies based on ISO spectroscopy, points towards a different heating/cooling balance of the ISM in infrared bright galaxies, but the causes and the related physic remain unknown. With PACS it will be possible to take full resolution complete PACS scans of representative nearby sources such that we can probe the ISM physics in central starbursts, the circum-nuclear molecular rings, disks and winds, separately. Moreover, a survey of the most important FIR structure lines will become feasable for large samples spanning from starburst, AGNs and obscured objects, at local and intermediate redshift. Observations with the PACS photometric camera in its three bands (70,110 and 170 μm) will complement the science possible with the integral field spectroscopy, because HERSCHEL will be able to resolve for the first time individual dust enshrouded activity knots, i.e. the place where star formation is triggered, to locate the starburst regions and their relative contributions in interacting systems. Due to the unprecedent spatial resolution HERSCHEL provides at FIR and sub-millimeter wavelengths and the improved sensitivities of its instruments, we expect that a significant part of HERSCHEL observing time will be spent on the study of high redshift galaxies. Detailed studies of nearby templates, as illustrated here, will significantly contribute in understanding in detail the physics governing the diagnostic diagrams and the change in spectral characteristics which are the basic tools for studying unresolved galaxies at high redshift. © 2005 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.