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The study of the physical properties of high-redshift galaxies has become one of the major goals of extragalactic astronomy. In particular the massassembly histories of galaxies have been the focus of many studies at redshifts 1 to 3. In the purpose of probing the dynamics of intermediate and high-redshift galaxies, we have designed a research program to carry out a near-infrared spectroscopic follow up of spatially resolved distant galaxies. Here, we present the results for A370-A5 (z=1.341), an arc behind the lens cluster Abell 370 (z=0.374), observed in the case of science verification programme of SINFONI/VLT. The natural magni fication due to massive galaxy clusters allows to spatially resolve and constrain the dynamics of young star forming galaxies 1 to 3 magnitudes fainter than those selected in blank fields. Thus, the study of lensed galaxies allows to probe a low mass regime of galaxies not accessible in standard observation. In this particular case, we found that the gas distribution and kinematics are consistent with a bipolar outflow with a range of velocities of v ~ 100km/s. [ABSTRACT FROM AUTHOR]

We present results from a new method of exploring the distant Universe. We use 3-D spectroscopy to sample a large cosmological volume at a time when the Universe was less than 3 billion years old to investigate the evolution of star-formation activity. Within this study we also discovered a high redshift type- II quasar which would not have been identified with imaging studies alone. This highlights the crucial role that integral-field spectroscopy may play in surveying the distant Universe in the future. [ABSTRACT FROM AUTHOR]

We summarise recent results from two programmes of integral field spectroscopy (IFS) on galaxy emission line haloes. Firstly, we present SAURON IFS of the 100 kpc-scale diffuse Lyα-emitting blobs in the SSA22 protocluster at z=3.09 and show how IFS helped uncover evidence for a galaxy-wide superwind outflow. Secondly, we present VIMOS observations of Hα emission in the cores of z ∼ 0.1 cooling flow clusters and illustrate how IFS is an essential tool for understanding these complex regions. [ABSTRACT FROM AUTHOR]

SN 1987A is located in the Large Magellanic Cloud and thus close enough to study the very late time evolution of a supernova and its transition to a supernova remnant. After almost two decades the supernova ejecta have now reached the pre-explosion circumstellar ring and started to interact with it. The system presents a complex structure involving forward and reflected shocks with highly diferent physical conditions in close spatial proximity. The supernova ring system is currently observed in X-rays (Park et al. 2004,2005), optical (Graves et al. 1996, Michael et al. 2003), mid-infrared (Bouchet et al. 2004) and radio (Manchester et al. 2005). The near-infrared data presented here complement all this. Based on science verification observations with SINFONI we present the supernovaring interaction as it appears in the near-infrared. SINFONI's adaptive optics supported integral field spectrograph spatially resolves the ring and the data thus provide new information and details for this unique object. [ABSTRACT FROM AUTHOR]

We present a study of a peculiar Supernova Remnant MF16, associated with the Ultraluminous X-ray Source (ULX) NGC6946 ULX-1. Observations were taken with the Multi-Pupil Fiber Spectrograph (MPFS) on 6-m telescope in January 2005. The nebula is found to be highly asymmetric, one of the parts being much denser and colder. Two-component structure of the emission lines and radial velocity gradient in some of them argue for a non-spherical shell, expanding with a velocity of about 100 km s-1. Neither shock models nor X-ray emission can adequately explain the actual emission line spectrum of MF16, so we suggest an additional ultraviolet source with a luminosity of about 1040erg s-1. We confirm coincidence of the ULX with the central star and identify radio emission observed by VLA with the densest part of the nebula. [ABSTRACT FROM AUTHOR]

It is now possible to measure detailed spectral indices for stellar populations in spiral disks. We propose to interpret these data using evolutionary synthesis models computed from the Star Formation Histories obtained from chemical evolutionary models. We find that this technique is a powerful tool to discriminate between old and young stellar populations. We show an example of the power of Integral Field spectroscopy in unveiling the spatial distribution of populations in a barred galaxy. [ABSTRACT FROM AUTHOR]

We present first results of a program with the integral field spectrometer SINFONI on the ESO-VLT (Very Large Telescope) Yepun to observe obscured stellar clusters in Hii regions in the infrared H and K bands with the goals of obtaining a more complete and less biased picture of the Milky Way's spiral structure,and of improving our understanding of the spatial distribution of Galactic Hii regions. The classification in spectral subclasses of early type stars together with the extinction determination and the stellar apparent magnitudes enable us to obtain spectrophotometric distances, which are independent and complementary to kinematic distances and free from the ambiguity inherent to the latters' determination. Most importantly, our method is much less limited by interstellar extinction than previous optical programmes, allowing studies along lines of sight where optical measurements are impossible. [ABSTRACT FROM AUTHOR]

Spatially resolved spectroscopy on a sample of planetary nebulae (PNe) has been carried out using INTEGRAL (WHT) and PMAS (Calar Alto). We present here our preliminary results for Abell 30, a nebula with a system of outflowing, H-deficient knots surrounding the central star. We have investigated the spectra of these knots, and find distinct difierences to the surface brightness distribution in difierent emission lines (difierent ions), particularly interestingly so for the C and O recombination lines. [ABSTRACT FROM AUTHOR]

The ultraluminous X-ray sources (ULXs) were isolated in external galaxies for the last 5 years. Their X-ray luminosities exceed 100-10000 times those of brightest Milky Way black hole binaries and they are extremely variable. There are two models for the ULXs, the best black hole candidates. 1. They are supercritical accretion disks around a stellar mass black hole like that in SS433, observed close to the disk axes. 2. They are Intermediate Mass Black Holes (of 100-10000 solar masses). Critical observations which may throw light upon the ULXs nature come from observations of nebulae around the ULXs. We present results of 3D-spectroscopy of nebulae around several ULXs located in galaxies at 3-6 Mpc distances. We found that the nebulae to be powered by their central black holes. The nebulae are shocked and dynamically perturbed probably by jets. The nebulae are compared with the SS433 nebula (W50). [ABSTRACT FROM AUTHOR]

We present GMOS-IFU spectroscopic observations of the proplyd 167-317 (LV2) near the Trapezium cluster in the Orion nebula, obtained at the Gemini South Observatory. The proplyd was observed in optical wavelengths ranging from ≃ 5515 Åto ≃ 7630Å. The ionized photo-evaporated flow was detected together with a microjet and possibly the blue-shifted jet that appear in most of the detected emission lines as multiple peaks at different velocities. Typically, there is a low velocity peak at ∼ 30 km s-1, a high velocity red-shifted peak at ∼ 100 km s-1 and a very faint blue-shifted peak at ∼ -60 km s-1. The observations also allowed us to determine spatially the emitting regions. The red-shifted jet is located to the SE of the central emission. We find evidences that the red-shifted jet has a variable velocity, which slowly drops with increasing distance from the proplyd [ABSTRACT FROM AUTHOR]

Emission nebulae like H II regions, Planetary Nebulae, Novae, Herbig Haro objects etc. are found as extended objects in the Milky Way, but also as point sources in other galaxies, where they are sometimes observable out to very large distances due to the high contrast provided by some prominent emission lines. It is shown how 3D spectroscopy can be used as a powerful tool for observations of both large resolved emission nebulae and distant extragalactic objects, with special emphasis on faint detection limits. [ABSTRACT FROM AUTHOR]

The discovery of luminous hard X-ray sources hosted by "normal" galaxies with optical spectra typical of early-type systems (XBONG; Comastri et al. 2002, (3)) represents one of the most surprising results of Chandra and XMM-Newton surveys. Why the relatively bright X-ray emission, typical of moderately luminous (1042-43erg s-1) Active Galactic Nuclei (AGN), does not leave any optical signature of the presence of a nuclear source is still subject of debate. Although several possibilities have been discussed in the recent years, the main concern about the nature of these sources is that the AGN emission lines may be "hidden" by the host galaxy starlight. The already granted VIMOS-IFU observations will provide us with a unique opportunity to understand these enigmatic sources. High spatial resolution, integral field spectroscopy in the optical, isolating the nuclei of the XBONGs, would help to settle the AGN line absence vs. starlight dilution controversy. The 3D-spectroscopy will also provide a clear insight into the optical properties of these X-ray emitting galaxies and, therefore, into the nature of the obscured super-massive black holes (SMBH) they host. [ABSTRACT FROM AUTHOR]

We present some preliminary (half-way) results on our adaptive optics spectroscopic survey of AGN at spatial scales down to 0.085". Most of the data were obtained with SINFONI which provides integral field capability at a spectral resolution of R ∼ 4000. The themes on which we focus in this contribution are: star formation around the AGN, the properties of the molecular gas and its relation to the torus, and the mass of the black hole. [ABSTRACT FROM AUTHOR]

We present results from a series of follow-up observations of a subsample of the representative SAURON survey elliptical (E) and lenticular (S0) galaxies using the OASIS integral-field spectrograph. These observations focus on the central 10 " x 10 ", with roughly double the spatial resolution of the SAURON observations. This increased spatial resolution reveals a number of interesting and previously unresolved features in the measured stellar kinematics and absorption-line strengths. We find that galaxies exhibiting the youngest global stellar populations (as measured with SAURON) often contain a distinctly young central region (on scales of a few hundred parsec or less) compared to the rest of the galaxy. Moreover, these compact, young components are found to be mostly counter-rotating with respect to the rest of the galaxy. Given that there is no well-established reason for such young components to 'prefer' counter- over co-rotation, this finding raises the following questions: How common are these small KDCs as a function of age? Why are there more young than old compact KDCs? Where are the equivalent co-rotating components? We explore these questions using simple simulated velocity fields and stellar population models, and find that the fading of the young component as it evolves, coupled with the fact that counter-rotating components are more easily detected in the velocity field, may help explain the observed trends. [ABSTRACT FROM AUTHOR]

I review observable manifestations of various AGN shocks, discuss some key past 3D results, and outline some recent improvements in the computational framework within which spectra are interpreted. New models of dusty clouds broaden the scope of photoionization by providing a self-consistent basis for the successful matter-bounded/ionization-bounded model sequences, and can undermine the case for shocks in some AGN. However, we are only beginning to explore computationally the time evolution of shocks in 3D. The cyclical nature of high-velocity shock compression may provide a natural time scale for some AGN phenomena. It would be premature to dismiss a r ôle for shocks in datasets that encompass only a few strong emission-lines. We need comprehensive IFU spectra. [ABSTRACT FROM AUTHOR]

We present results of the analysis of the population of massive stars recently discovered in the central cluster of the Galaxy. A spectral classification of all stars is made based on their K band spectra. Population synthesis models and the HR diagram are used to show that the population was born in a burst of star formation ∼ 6 Myrs ago. Finally, special emphasis is given to two stars with special properties: GCIRS34W and GCIRS16SW. [ABSTRACT FROM AUTHOR]

The main results on the stellar population properties of nearby disk galaxies obtained with the Multi-Pupil Fiber/Field Spectrograph (MPFS) of the 6m telescope during the last ten years are reviewed. [ABSTRACT FROM AUTHOR]

In this contribution we present the analysis of the ionization structure of a sample of six low-z Ultraluminous Infrared Galaxies using Integral Field Spectroscopy. We discuss the possible ionizing mechanisms responsible, focussing especially on the external regions (d ∼ 2 - 10 kpc). The observed line ratios are better explained by the presence of shocks with velocities of 150 to 500 km s-1. This is supported by the existence of a positive correlation between the ionization state and the velocity dispersion, especially when using the [O i]λ6300/Ha ratio. We discuss the origin of these shocks. We find no evidence for signatures of superwinds in the extranuclear regions. We propose as an alternative explanation the existence of tidally induced large-scale gas flows caused by the merging process itself as the mechanism causing these shocks. Finally, there is one galaxy where the line ratios in the external regions cannot be explained by shocks. [ABSTRACT FROM AUTHOR]

We are using integral field spectroscopy (IFS) data together with archival Hubble Space Telescope (HST) images, for carrying out a program aimed at studying a representative sample of local luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs; 11 ≤ log(LIR/L⊙)≤13). Our goals are to characterize the stellar and ionized gas structure, the two dimensional extinction and star formation, the kinematical properties and the dynamical mass tracers. Here we will review some of the most interesting results obtained from our sample, including detailed studies for some individual galaxies. The implications for deriving the star formation rate (SFR) and mass when studying high-redshift galaxies will be briefly discussed too. [ABSTRACT FROM AUTHOR]

The galaxy pair AM 1353-272 nicknamed "The Dentist's Chair" shows two ∼30 kpc long tidal tails. Previous observations using multi-slit masks showed that they host up to seven tidal dwarf galaxies. The kinematics of these tidal dwarfs appeared to be decoupled from the surrounding tidal material. New observations of the tip of the southern tidal tail with the VIMOS integral field unit confirm the results for two of these genuine tidal dwarfs but raise doubts whether the velocity gradient attributed to the outermost tidal dwarf candidate is real. We also discuss possible effects to explain the observational difference concerning the strongest velocity gradient seen in the slit data, which is undetected in the new integral field data, but arrive at no firm conclusion. Additionally, low-resolution data covering most of the two interacting partners show that the strongest line emitting regions of this system are the central parts. [ABSTRACT FROM AUTHOR]

Using 15 deployable integral field units of FLAMES/GIRAFFE at VLT, we have recovered the velocity fields of 35 galaxies at intermediate redshift (0.4 ≤ z ≤ 0.75). This facility is able to recover the velocity fields of almost all the emission line galaxies with I(AB)≤ 22.5. We find that less than 40% of intermediate redshift galaxies are indeed rotating disks, producing a Tully-Fischer relationship (stellar mass or M(K band) versus Vmax) which has apparently not evolved in slope, zero point and scatter, since z=0.6. The very large scatters found in previously reported Tully-Fischer relationships at moderate redshifts are apparently due to the difficulty to identify the nature of velocity fields with slits. Indeed a majority of intermediate redshift starbursts are not rotating disks: 60% of galaxy velocity fields evidence the fact that they have not reached their dynamical equilibrium. Those galaxies include mergers, compact galaxies and/or inflow/outflows and their presence suggests a strong evolution in the dynamical properties of galaxies during the last 7 Gyrs. We also used the moderately high spectral resolution of FLAMES/GIRAFFE (R=10000) to derive 2D maps of electronic densities from the [OII] 3726,3729 line ratios. This allows us to identify an outflow and few giant HII regions with densities similar to Orion, but at z=0.6. It leads to a new technique for mapping extinctions, star formation rate densities, gas metal abundances in distant galaxies, which, combined with velocity fields, allows to investigate the details of galaxy physics at large lookback times. Integral field spectroscopy is a mature technique which will be applied to Extremely Large Telescopes. We summarize some of the extragalactic science cases, and discuss their resulting requirements (image quality, field, multiplex & spectral resolution), which can be compared to adaptive optics techniques such as GLAO (Ground Layer Adaptive Optics) , FALCON (or Distributed Adaptive Optics) and Laser Guide Stars.Integral field spectroscopy is a mature technique which will be applied to Extremely Large Telescopes. We summarize some of the extragalactic science cases, and discuss their resulting requirements (image quality, field, multiplex & spectral resolution), which can be compared to adaptive optics techniques such as GLAO (Ground Layer Adaptive Optics) , FALCON (or Distributed Adaptive Optics) and Laser Guide Stars. [ABSTRACT FROM AUTHOR]

We report on integral field spectroscopy observations, performed with the PPAK module of the PMAS spectrograph, covering a field-of-view of ∼74"×64" centered on the core of the galaxy cluster Abell 2218. A total of 43 objects were detected, 27 of them galaxies at the redshift of the cluster. We deblended and extracted the integrated spectra of each of the objects in the field using an adapted version of tt galfit for 3D spectroscopy (tt galfit3d). We use these spectra, in combination with morphological parameters derived from deep HST/ACS images, to study the stellar population and evolution of galaxies in the core of this cluster. [ABSTRACT FROM AUTHOR]

We present the on-going observational program of a VIMOS Integral Field Unit survey of the central regions of massive, gravitational lensing galaxy clusters at redshift z ≃ 0.2. We have observed six clusters using the low-resolution blue grism (R ≃ 200), and the spectroscopic survey is complemented by a wealth of photometric data, including Hubble Space Telescope optical data and near infrared VLT data. The principal scientific aims of this project are: the study of the high-z lensed galaxies, the transformation and evolution of galaxies in cluster cores and the use of multiple images to constrain cosmography. We briefly report here on the first results from this project on the clusters Abell 2667 and Abell 68. [ABSTRACT FROM AUTHOR]

We present an integral field spectroscopy survey of rich clusters of galaxies aimed at studying their lensing properties. Thanks to knowledge of the spectroscopic characteristics of more than three families of multiple images in a single lens, one is able in principle to derive constraints on the geometric cosmological parameters. We show that this ambitious program is feasible and present some new results, in particular the redshift measurement of the giant arc in A2667 and the redshift confirmation of the counter-image of the radial arc in MS2137-23. Prospects for the future of such a program are presented. [ABSTRACT FROM AUTHOR]

Selective amplification of the line and continuum source by microlensing in a lensed quasar can lead to changes of continuum spectral slopes and line shapes in the spectra of the quasar components. Comparing the spectra of different components of the lensed quasar and the spectra of an image observed in different epochs one can infer the presence of millilensing, microlensing and intrinsic variability. Especially, microlensing can be used for investigation of the unresolved broad line (BLR) and continuum emitting region structure in active galactic nuclei (AGN). Therefore the spectroscopic monitoring of selected lensed quasars with 3D spectroscopy open new possibility for investigation of the BLR structure in AGN. Here we discuss observational effects that may be present during the BLR microlensing in the spectra of lensed QSOs [ABSTRACT FROM AUTHOR]

I briefly recall some basic features of gravitational lensing, chiefly in the context of multiple image formation which is the most widely observed phenomenon of ‘galaxy lensing'. In such cases, the angular scales involved are suitably matched to the sizes of existing integral field units, and therefore the impact of 3D spectroscopy has been largest. I review some recent advances of studying galaxy-scale gravitational lensing with integral field units, highlighting the investigation of small-scale structure in both lenses and sources. [ABSTRACT FROM AUTHOR]

We present Gemini North GMOS/IFU observations of the roots of the NGC 1569 super-galactic wind. This forms part of a larger and on-going study of the formation and collimation mechanisms of galactic winds. Four IFU pointings cover the base of the outflows originating from the central super-star clusters; we present a preliminary analysis for two positions. The choice of single-slit mode and the R831 grating (dispersion = 0.34 Å pix−) allowed us to cover the spectral range 4740-6860Å through 500 object fibres. We observe the nebular diagnostic lines of Hα, Hβ, [OIII]λλ4959,5007, [NII]λλ6548,6583, [SII]λλ6716, 6731. The data were reduced using the standard Gemini pipeline included with IRAF, and corrected for differential atmospheric refraction. We find emission lines clearly composed of multiple components—in most cases a bright narrow feature (intrinsic FWHM = 50 kms−1) superimposed on a fainter broad component (FWHM ≤ 300 kms−1). We discuss the origin of these components, in the context of the wind/interstellar medium interaction. [ABSTRACT FROM AUTHOR]

3D spectroscopic techniques allow the assessment of different types of motions in extended objects. In the case of spiral galaxies, thes type of techniques allow us to trace not only the (almost) circular motion of the ionized gas, but also the motions arising from the presence of structure such as bars, spiral arms and tidal features. We present an analysis of non-circular motions in spiral galaxies in interacting pairs using scanning Fabry-Perot interferometry of emission lines. We show how this analysis can be helpful to differentiate circular from non-circular motions in the kinematical analysis of this type of galaxies. [ABSTRACT FROM AUTHOR]

We present VLT-VIMOS-IFU spectroscopy of the overlap region in the merging Antennae galaxies (NGC∼4038/39). This regions contains six complexes of young massive clusters, three of which display strong Wolf-Rayet features, indicating extremely young ages (∼3-7∼Myr). The high area normalised star formation rates within these young complexes places them in the regime of starburst galaxies, thereby justifying the designation of localised starbursts. The ionised gas surrounding the complexes is expanding at speeds of 20-40∼km/s. This slow expansion can be understood as a bubble, caused by the stellar winds and supernovae within the complexes, expanding into the remnant of the progenitor giant molecular cloud. We also find that the complexes are likely to lose a large fraction of their extended material to the surrounding regions, however the central regions may merge into a single massive star cluster. [ABSTRACT FROM AUTHOR]

We present selected results from integral-field spectroscopy of 48 earlytype galaxies observed as part of the SAURON survey. Maps of the Hβ Fe5015, Mgb and Fe5270 indices in the Lick/IDS system were derived for each of the survey galaxies. The metal line strength maps show generally negative gradients with increasing radius roughly consistent with the morphology of the light profiles. Remarkable deviations from this general trend exist, particularly the Mg b isoindex contours appear to be flatter than the isophotes of the surface brightness for about 40% of our galaxies without significant dust features. Generally these galaxies exhibit significant rotation. We infer from this that the fast-rotating component features a higher metallicity and/or an increased Mg/Fe ratio, as compared to the galaxy as a whole. We also use the line strength maps to compute average values integrated over circular apertures of one effective radius, and derive luminosity weighted ages and metallicities. The lenticular galaxies show a wide range in age and metallicity estimates, while elliptical galaxies tend to occupy regions of older stellar populations. [ABSTRACT FROM AUTHOR]

We present results from our ongoing effort to understand the nature and evolution of nearby galaxies using the SAURON integral-field spectrograph. In this proceeding we focus on the study of the particular case formed by the interacting galaxies NGC5953 and NGC5954. We present stellar and gas kinematics of the central regions of NGC5953. We use a simple procedure to determine the age of the stellar populations in the central regions and argue that we may be witnessing the formation of a kinematically decoupled component (hereafter KDC) from cold gas being acquired during the ongoing interaction with NGC5954. [ABSTRACT FROM AUTHOR]

We consider some results on the gas and stellar kinematics of nearby galaxies recently obtained on the 6m telescope of SAO RAS using panoramic spectroscopy methods. The circumnuclear regions of the galaxies were observed with integral-field spectrograph MPFS. The large-scale ionized gas kinematics was studied with the scanning Fabry-Perot interferometer (FPI) in the multi-mode focal reducer SCORPIO. The main attention is devoted to kinematically decoupled regions in the galaxies: bars, spirals, polar disks and rings. [ABSTRACT FROM AUTHOR]

Early-type galaxies exhibit a wealth of photometric and dynamical structures. These signatures are fossil records of their formation and evolution processes. In order to examine these structures in detail, we build models aimed at reproducing the observed photometry and kinematics. The developed method is a generalization of the one introduced by (12), consisting in an N-body representation, in which the weights of the particles are changing with time. Our code is adapted for integral-field spectroscopic data, and is able to reproduce the photometric as well as stellar kinematic data of observed galaxies. We apply this technique on SAURON data of early-type galaxies, and present preliminary results on NGC 3377 [ABSTRACT FROM AUTHOR]

The integral field spectrograph mode of the Kyoto tridimensional spectrograph II is optimized for a high spatial resolution with the ~ 0″.1 sampling when mounted on the Subaru Telescope, while a wider field of view is emphasized on the University of Hawaii 88-inch Telescope (UH88). One of our main targets is to resolve activities in nearby galaxies. Examples are shown: one is the low ionization emission line region in the galaxy NGC 1052 observed with the Subaru. The spatial resolution of ~ 0".4 has revealed the structures, both in space and velocity, of the AGN outflow. An example observed with the UH88 is an interacting galaxy system NGC 6090. Through analyses of the spatial variations of emission line ratios, we have found rapid large-scale metal/abundance enhancement in starbursts. [ABSTRACT FROM AUTHOR]

We briefly review here the progress made using integral-field spectroscopy in the field of nearby galaxies, via the illustration of a few recent results. [ABSTRACT FROM AUTHOR]

Among the solutions for 3D spectroscopy, an Imaging Fourrier Transform Spectrometer (IFTS) has the unique capability of making possible flexible high spectral resolution on a wide field. After a brief review of scientific programmes which need this combination, illustrated with results from BEAR, a prototype IFTS, the perspectives for IFTS at Dome C and on an ELT are presented. [ABSTRACT FROM AUTHOR]

3-D spectroscopy assisted by adaptive optics (AO), provides an extremely eficient way to study the surface or atmospheric composition of planetary bodies. AO supported near-infrared instruments such as NACO and SINFONI - which provide both the high-angular resolution required for spatially resolving the disks of small solar system bodies and the spectral resolution adequate for compositional studies - open new windows of investigation to planetary scientists. Since their installation in UT4 (Yepun) at ESO/VLT, these instruments have been used to map the surface and atmospheric composition of small angular-size bodies such as Vesta and Titan, to study the spatial compositional variation of Pluto's moon Charon and to obtain spectra of faint bodies such as the trans-neptunian objects. Focusing on these targets, we demonstrate and compare the capabilities of the NACO Fabry-Perot (FP) imager (12) and the new integral-field spectrograph SINFONI (6; 10). The prospects for 3-D spectroscopy applied to the understanding of our solar system are discussed. [ABSTRACT FROM AUTHOR]

We explore the use of Integral Field Spectroscopy (IFS) for observing extrasolar planet transits. We show that IFS can improve the photometric accuracy in high S/N time series observations with respect to standard slit spectrophotometry. Ground based observations of HD209458b obtained with WHT + INTEGRAL during a transit have led to an accuracy in relative spectrophotometry (i.e line / continuum) not far from that expected by photon noise. This result indicates that these types of ground based observations can constrain the characterization of the transmission spectrum of extrasolar planets [ABSTRACT FROM AUTHOR]

We present the first realistic simulations of how high-redshift star forming galaxies will be observed by MIRI (Mid IR Instrument). The simulations presented have been developed using the new tool Specsim, and are part of an ongoing project aimed at studying a representative sample of Ultraluminous Infrared Galaxies (ULIRGs) with integral field spectroscopy (IFS) data. [ABSTRACT FROM AUTHOR]

The Near Infrared Spectrograph (NIRSpec) on board of the James Webb Space Telescope (JWST) will be equipped with an Integral Field Unit (IFU) which will allow the two-dimensional spectral characterization of astronomical objects with unprecedented depths, especially in the 2-5 micron wavelength range. In particular, NIRSpec-IFU observations of high-z galaxy populations will permit the capture of their often complex two-dimensional physical and kinematical structure, a pre-requisite for carrying out a number of studies. These types of observations will also help to understand possible observational biases of large 1D (i.e. slit) surveys to be carried out in multi-object mode. Here we describe the main characteristics of the NIRSpec-IFU, as well as its expected sensitivity and performance for observations of high-z galaxy populations. [ABSTRACT FROM AUTHOR]

The 3D-NTT will be a visitor instrument for the NTT, built by GEPI (Paris) and LAM (Marseille) with the collaboration of LAE (Montréal, Canada) and AAO (Australia). It is a spectro-imager offering two modes: a low resolution mode (100-5000) with a Tunable Filter, and a high resolution mode (5000 - 40 000) with a standard scanning Fabry-Perot. A large variety of programmes may be led with such an instrument as has been shown recently (1997-2003) with the Taurus Tunable Filter on the AAT and WHT. In the frame of a large scientific coollaboration, gathering European teams as well as collaborators from other countries, we propose a Large Programme (IOGA) dedicated to the study of ionized gas in galaxies, at low and high z, to be undertaken with the 3D-NTT. Nearby IR galaxies (IRGs) are the key to understanding the formation and evolution of galaxies, as they are believed to be the local counter-part of the numerous luminous starburst galaxies at high z. To understand the nature, origin and evolution of IRGs, we propose to map the star formation and kinematics in 500 galaxies and obtain dust extinction, metal abundances and electron density maps in 50 of them for obtaining a reference sample with high spectral and spatial resolution (sub-kpc) to be compared with distant objects being observed on the VLT (GIRAFFE, SINFONI). We will take advantage of both modes proposed by the instrument: high resolution mode with scanning Fabry Perot (FOV 5.5' or 11'), and low resolution mode with Tunable Filter and larger field (FOV 20'). This mode will be used at high z to look for star forming galaxies around quasars with a range of intrinsic UV luminosity. Star forming galaxies exist in significant numbers around low power quasars and we want to check if this remains true around more distant and luminous quasars. This may be the first evidence that powerful UV fields can suppress or delay widespread star formation in galaxies and, as such, may provide important constraints on cosmological models. [ABSTRACT FROM AUTHOR]