Prof. Niranjan Thatte

Abstract:

integral field spectroscopy in the K-band (1.9-2.4 mu m) was performed on four IR-bright star clusters in NGC4038/39 ("The Antennae"). Two of them (hereafter F1 and F2) are located in the overlap region of the two galaxies, and together comprise approximate to 25% of the total 15 mu m and approximate to 10% of the total non-thermal 4.8 GHz emission from this pair of merging galaxies. The other two clusters, each of them spatially resolved into two components, are located in the northern galaxy, one on the eastern (F3) and one on the western (F4) "loop" of blue clusters. Comparing our analysis of Br gamma, CO-bandheads, H alpha (from archival HST data), and V-K colours with stellar population synthesis models indicates that the clusters are extincted (A(v) approximate to 0.7 - 4.3 mags) and young, displaying a significant age spread (4 - 10x10(6) yrs). Using our derived age estimates and assuming the parameters of the IMF, we find that these clusters have masses that range from a few x10(5) to a few x10(6) M-circle dot.

Abstract:

SPIFFI (SPectrometer for Infrared Faint Field Imaging) is the integral field spectrograph of the VLT-instrument SINFONI (SINgle Far Object Near-infrared Investigation). SINFONI is the combination of SPIFFI with the ESO adaptive optics system MACAO (Multiple Application Concept for Adaptive Optics) offering for the first time adaptive optics assisted near infrared integral field spectroscopy at an 8m-telescope. SPIFFI works in the wavelength ranger from 1.1 to 2.5 mu m with a spectral resolving power ranging from R = 2000 to 4500. Pixel scale ranges from 0.25 to 0.025 seconds of are. The SPIFFI field-of-view consists of 32 x 32 pixels which are rearranged with an image slicer to a form a long slit.Based on the 3D slicer concept with plane mirrors, an enhanced image slicer was developed. The SPIFFI image slicer consists of two sets of mirrors, called the small and the large slicer. The small slicer cuts a square field of view into 32 slitlets, each of which is 32 pixels long. The large slicer rearranges the 32 slitlets into a 1024 pixels long slit. The modifications to the 3D slicer concept affect the angles of the plane mirrors of small and large slicer and lead to an improved slit geometry with very little light losses. At a mirror width of 0.3mm the light loss is < 10%. All reflective surfaces are flat and can be manufactured with a high surface quality. This is especially important for the adaptive optics mode of SINFONI. We explain the concept of the SPIFFI mirror slicer and describe details of the manufacturing process.

Abstract:

The technique of integral field spectroscopy,: which provides simultaneous spectra for each pixel of a contiguous two-dimensional field of view, holds tremendous promise for improving our ability to study circumstellar environments. The technique becomes especially important at near infrared wavelengths, where rapid changes in the night sky background level limit the use of standard scanning techniques. In addition, combining the capabilities of adaptive optics systems with near infrared integral field spectrographs provides an unique way to enhance-spatial resolution for ground based observations. We present the technique of integral field spectroscopy, with special emphasis on the near infrared, and illustrate future developments by describing SINFONI, an adaptive optics assisted near infrared integral field spectrometer for the ESO VLT.

Abstract:

We propose to build a NIR imager/spectrograph for the LET which will support (1) seeing and diffraction limited direct imaging, (2) seeing and diffraction limited long-slit spectroscopy, (3) integral field spectroscopy and (4) tin small fields) OH-suppressed imaging of very faint objects. The instrument will cover the zJHK spectral bands with optimization for the K band. Therefore the optics will be cold (77 K). Whether the wavelength coverage can be extended to 5 mu without seriously compromising the K-band performance will be investigated during the design phase. At present a 2048 x 2048 HgCdTe array is foreseen as detector. Space will be reserved for the possibility of adding a (cold) multiple object spectroscopy unit. The feasibility of such a device will be investigated in parallel to the development of the main instrument. Six German institutes will cooperate to develop this LBT instrument.

Abstract:

Near infrared instrumentation at 4 and 8 meter class telescopes has grown rapidly in the past few years with the advent of 1024(2) and 2048(2) detector arrays. We present a brief review of high resolution spectroscopic capabilities available worldwide, with an eye on new developments, e.g. spatially resolved spectroscopy offered by integral field instruments.Observing at near-infrared wavelengths has its own quirks. We discuss observing strategies to get past the limits of high background (including both thermal background and background due to OH sky emission lines), Variations in atmospheric transmission, and detector constraints. Special attention is given to the subject of OH suppression/avoidance, which can significantly increase the sensitivity in the J, EI and short K windows. This is especially important for (fainter) high redshift targets, where the rest frame visible diagnostic lines are shifted into the near infrared.