We have entered the phase of extrasolar planets characterization, probing theiratmospheres for molecules, constraining their horizontal and vertical temperature profiles and estimating the contribution of clouds and hazes. We report here a short review of the current situation using ground based andspace based observations. What are the future challenges and how can we better address them? Is there a nichefor DOME C observations?

Dome C is likely to be the best site in the world for mm and sub-mm observations.In this paper we focus on what can be done from Dome C toinvestigate the detailed properties of the Cosmic MicrowaveBackground (CMB). Two experiment typologies are particularly promising:precision measurements of the polarization of the CMB, to confirmthe presence of an inflation phase in the very early universe, andhigh resolution measurements of the Sunyaev-Zeldovich effect (SZE) in clustersof galaxies, which can be used to investigate dark energy anddark matter in the Universe. Several important teams are currently carrying outexperiments of the first kind; Dome C is the location of the BRAIN experiment,which uses bolometric interferometry as the tool to producesensitive measurements with low systematic effects, and certainly orthogonalto the systematic effects of all other instruments currently developed to this purpose.Dome C will be an ideal location for a large dish telescope for mmand sub-mm measurements. In addition to cutting-edge sub-mm science,a telescope complementing SPT (in size and/or in frequency)will be ideal for special CMB observation, like the detection of non-Gaussian features,the measurement of relativistic effects in SZE, the measurement of the SZE resultingfrom the decay products of super-symmetric dark matter in selectedclusters.

The science case for FIR/Submm surveys of the extragalactic sky to be carried out from Dome C is reviewed. The main questions concerning the formation and evolution of galaxies making up the CIRB are outlined and opportunities to exploit Dome C unique observing conditions through single-dish observations are discussed.

The importance of a Dome C facility for studies of massive star formation is highlighted. Using an example of a statistical study of 380 candidate massive protostars based on the GLIMPSE legacy program data from the Spitzer Space Telescope, the relevance of a Dome C facility for further science progress is argued. The GLIMPSE point source photometry was used to a conduct colour-magnitude analysis, and radiative transfer modelling of the spectral energy distributions of the massive protostars. The results support an accretion scenario for the process of massive star formation up to masses of 50 M๏. The available spectral energy distrubutions of the massive protostellar candidates are largely inadequate in the crucial bands from 10–500 μm. This wavelength range can be effectively filled in with a nominal Dome C observing facility which can be highly cost effective compared to a space facility. Narrow-band emission line imaging of massive star forming regions in the 10–20 micron bands using high temperature emission lines can yield invaluable information on the nature of OB stars in the Milky Way and nearby galaxies. Such observations are crucial for our understanding of the influence of OB stars in controlling the galactic turbulence, feedback effects, influence on other low mass stars in the vicinity, and controlling the star formation rate.

We present the science case for ICE-T, the International Concordia Explorer Telescope, a double telescope optimized for ultra-high and ultra wide field optical time-series photometry fromDome C. ICE-T consists of two 60 cm 8°×8°-FOV Schmidt telescopes for Sloan g and i photometry and one independent 25 cm, solar, full-disk, Ca ii-K imagingtelescope on a single mount. ICE-T is therefore operable during night and day. A 28 cm narrow-field Maksutov spectrophotometric telescope for night-time aerosol measurements (TAVERN-SP) will beprovided by AWI early on and operated in parallel with IRAIT and later with ICE-T. The low scintillation noise and the long continuous darkness are among the unique properties for highprecision optical time-series photometry.

In this paper we review the progress towards the deployment of alarge "PILOT-like" telescope at Concordia Station, Dome C. PILOT isa proposed 2.4 m optical/IR telescope that will cost in excess of EUR10 m, and is thus representative of the scale of facility that willtransform Concordia into a significant international observatory. Adesign study of PILOT, funded by the Australian government, iscurrently underway. We describe the current status of this designstudy, and discuss the implications that major internationalprojects such as PILOT hold for the future of Antarctic astronomy atConcordia.

A description of the early days of infrared site testing at the SouthPole is given, with special attention paid to the data whichquantified the conditions during summer and the long twilight period.Such times are also provide relatively benign conditions for humans inAntarctica as well. We show that they are favourable for manyobserving programs that require the thermal infrared, and then discussa number of specific projects that could be undertaken. Such projectsmight mark the first to be conducted with any new telescope inAntarctica, as they would enable science to be carried out during thecommissioning period.

At Dome C most of the seeing is located in the lower atmosphere, below 50 meters height.In this introduction we describe ways in which one might mitigate those ground layer seeingeffects and thus be limited solely by the ~0.25 arcsec seeing of the so-called“free atmosphere”.

Many problems in time domain astronomy are bestapproached with continuous,high frequency (<1 minute) observations over a large area of the sky, because event rates are generally less than 0.01 detections per sq. degree in a year. For GRBs and theearliest stages of SNe, follow-up spectroscopy, multiband photometry andpolarization measurements need to be triggered in seconds or minutes.Plateau sites in Antarctica are optimal for a new survey, Xian(eXtreme Imaging Antarctic Network), for which the scientific motivation is presented.

The operation of any base or expedition to Antarctica is regulatedby the mutual agreement among nations in the “Antarctic Treaty”.This treaty deals with the major aspects of life in Antarctica andits main principles and provisions are described in what follows.

Core collapse and thermonuclear supernovae are among the brightest objects in the Universe. However, although we have an ample knowledge of their optical properties, comparatively little is still known in the infrared. Dome C seems to be the best place on Earth for astronomical observations at infrared and submillimeter wavelengths. The telescope IRAIT (International Robotic Antarctic Infrared Telescope) will be the first European astronomical facility at Dome C, and it is planned to be fully operational by the end of 2008. IRAIT will be equipped with the AMICA camera for near- andmid- infrared imaging and photometry. As a key scientific project with IRAIT, we propose a long term study of near- (K) and mid- (LMNQ) infrared light curves of bright supernovae.

The International Robotic Antarctic Infrared Telescope(IRAIT)will be the first European infrared telescope to operate onthe Antarctic Plateau: IRAIT is scheduled to arrive at Dome Cduring the 2007–2008 Antarctic campaign. The main IRAIT FocalPlane Instrument is AMICA (Antarctic Multiband Infrared CAmera)an instrument designed to observe in the Near- and Mid-infrared(2–28 μm). Here we give a brief description of thetelescope and discuss which kind of science could be performedfrom Dome C.

Antarctica offers unique conditions for ground-based observations, such as low sky background in the infrared, improved seeing, and low turbulence and scintillation noise. These properties are particularly beneficial to imaging, precision photometry, and infrared observations. It may be less clear if Antarctica offers equally compelling advantages for spectroscopy, in particular in the optical domain. However, scientific programmes that make use of imaging (or 3D) spectroscopy for selected follow-up studies of IR surveys, long-termmonitoring of extended targets and resolved stellar population studies in crowded fields, also benefit from the site conditions at Dome C.

Near-infrared spectro-photometry, at a spectral resolution of ~100, allows to characterize a great variety of stellar sources, from late-typegiants to emission line stars. Various components of the inter-stellar medium can also be traced. This technique can therefore be very fruitful, in addition, for studies of star forming regions, the Milky Way and external galaxies.The outstanding environmental conditions that are expected at Dome C should be favorable to carry out spectro-photometric surveys in the 1 to 2.5 μm region, that would usefully complement space-borne projects.

We have developed a Wide Field Cryogenic Telescope II (WFCT-II), which containsa whole telescope-optics in a cryostat to suppress thermal emission from the whole telescope.The cryostat is of a cylindrical shape of 800 mm length and 300 mm diameter.The telescope inside is a Ritchey-Chretien system with the primary mirror of 231 mm in diameterand a focal length of 1500 mm.
The InSb 1k × 1k infrared array detector (Aladdin II) has a FoV of 1 square degreeand a resolution of 3'' × 3''/pixel.
We can install 5 filters whose wavelengths range from 1 μm to 5 μm.

Cosmic shear offers a remarkably clean way to measure the equation of state of the Universe and its evolution. Resolution over a wide field is paramount, and Antarctica offers unique possibilities in this respect. There is an order of magnitude gain in speed over temperate sites, or a factor three in surface density. This means that PILOT outperforms much larger telescopes elsewhere, and can compete with the proposed DUNE space mission.

First time-series observations with the 25-cm sIRAIT Antarcticpilot telescope from May 2007 are presented and show that the siteis well suited for time-series high-precision photometry. Ourtarget stars were one spotted 5.998-day rotating variable and oneshort-period δ-Scuti star. A total of 13 000 BVR CCDframes covered a time series of 243 consecutive hours.

Dome Fuji is potentially one of the best astronomical sites in Antarctic plateau. We have a plan to build a 2-m class infrared telescope at Dome Fuji, and have been evaluating the site since the 2006/2007 Antarctic summer. We present the outline of a 2-m class telescope project and some results of our SODAR measurements.

The unexpected diversity of exoplanets includes a growing number of super Earth-planets, i.e. exoplanets with masses smaller than 10 Earth masses and a similar chemical and mineralogicalcomposition like Earth. We present a thermal evolution model for a super-Earth to calculate the sourcesand sinks of atmospheric carbon dioxide. The photosynthesis-sustaining habitable zone (pHZ) isdetermined by the limits of biological productivity on the planetary surface. We apply the model tocalculate the habitability of super-Earths in Gliese 581. The super-Earth Gl 581c is clearly outside thepHZ while Gl 581d at the outer edge of the pHZ could at least harbor some primitive life forms.

IRAIT (International Robotic Antarctic Infrared Telescope) is a telescope with an 80 cm aperture, ready for installation at Dome C. Equipped with AMICA (Antarctic Multiband Infrared CAmera), the main focal plane instrument, it will observe in near (1–5 μ) and mid infrared regions (5–28 μ), benefiting from the exceptional site characteristics. The installation will start in December 2007. An overview of interfacing devices and the integration of various IRAIT subsystems are here presented.