We describe the design and performance of Bolocam, a 144-element, bolometric, millimeter-wave camera. Bolocam is currently in its commissioning stage at the Caltech Submillimeter Observatory. We compare the instrument performance measured at the telescope with a detailed sensitivity model, discuss the factors limiting the current sensitivity, and describe our plans for future improvements intended to increase the mapping speed.

/pdf/current-status-of-bolocam-a-large-format-millimeter-wave-1j5ufn9wnn.pdf

Current status of Bolocam: a large-format millimeter-wave bolometer camera

Over the past three decades interest in the unique spectral measurements offered by terahertz instruments operat-ing outside the Earth's atmosphere has grown enormously. Since the historic flight of Cosmos 669 in 1974, and the first THz telescope with cryo-cooled detectors operated on board Salyut 6 in 1978, satellite instruments have performed both direct detection and heterodyne spectroscopy measurements in the interstellar medium, in external galaxies, in the atmospheres of planets and comets and in the Earth's stratosphere. Seven-teen orbital instruments containing THz sensors or sources have either completed their mission objectives or are currently operational. They originate in Russia, Japan, Europe and the US and cover applications in astrophysics and cosmology; planetary and small solar system body science; and pollution, ozone and climate monitoring on the Earth. At least a dozen serious future mission proposals are under consideration, including new areas of meteorology, terrestrial planet finding and planetary radar spectroscopy. It is truly a golden age for THz space science and applications. This talk will review past, present and future space instruments carrying infrared, millimeter wave and terahertz components and their science objectives.

THz for space: The golden age

The Herschel Mission, Scientific Objectives, and this Meeting

A physical optics (PO) method is presented which in two steps calculates the scattered field of a reflector or a lens in a beam waveguide (BWG). The first step involves a calculation of a set of currents on an auxiliary plane and the second step a field calculation from this current set. The method is named A-PO that refers to the calculation of PO currents on an Auxiliary plane. A-PO is less accurate than PO for sidelobe analysis, but useful for first-pass analysis of the main beam region in a BWG where it is significantly faster than standard PO. Two examples show that the co-polar as well as cross-polar radiation in a submillimeter BWG can be efficiently determined 40 dB below peak.

Physical optics analysis of beam waveguides using auxiliary planes

The exploration of new lands has always been and is still an appealing quest of the Mankind. Today, these new worlds we are talking about are several light years away from us, and are called exoplanets. Recently discovered, it is possible to study their structures, as well as their atmospheric compositions and properties, without the need to resolve their light from their host star. This is indeed possible when a planet regularly pass in front (transit) or behind (occultation) its host star from our point of view. The study of exoplanets and of their atmosphere is of prime importance. It could inform us on present conditions during their formation and evolution, and thus help us to characterise planets in our own Solar system. The characterisation of the orbital and atmospheric properties of transiting exoplanets is among the main goal of this thesis. We use observations in the infrared band, wherein exoplanet spectra present many atmospheric molecular transition features. However several infrared instrument systematics, particularly those on-board the Spitzer telescope (3.6–24 μm), have already led to divergent conclusions on the nature of planetary atmospheres it targeted, depending on the way these systematics were treated. Hence this thesis focuses on the high-precision infrared data reduction and analysis of transiting exoplanets. Our goal is to obtain accurate and non-ambiguous measurements for the characterisation of exoplanets through the recombination of their emission and transmission spectra. Meanwhile, we attempt to better understand the behaviour of infrared detectors in preparation for future missions in this wavelength range, such as the James Webb Space Telescope. This work is organised around the characterisation of the GJ 436 planetary system based on the data reduction and reanalysis of Spitzer observations and of CoRoT-2 with the help of ground-based and Spitzer observations. We use and optimise the partial deconvolution photometry program DECPHOT, fully appropriate to separate the stellar flux contributions from each other and from that of the sky, which is particularly important in the infrared. Besides, we improve aperture photometry. Then we use the Markov chain Monte Carlo algorithm developed by the Liège team to analyse the light curves produced by these two measurement techniques, in addition to radial velocity measurements that

Photométrie de haute précision dans l'infrarouge d'exoplanètes en transit

SPIRE, the Spectral and Photometric Imaging Receiver, will be a bolometer instrument for ESA’s Herschel satellite Its main scientific goals are deep extragalactic and galactic imaging surveys and spectroscopy of star-forming regions in own and nearby galaxies The SPIRE detectors are feedhorn-coupled NTD “spider-web” bolometers The instrument comprises a three-band imaging photometer covering the 250-500 µm range, and an imaging Fourier Transform Spectrometer (FTS) covering 200-670 µm The photometer has a field of view of 4 x 8 arcminutes which is observed simultaneously at 250, 350 and 500 µm, with dichroic beam dividers separating the three spectral bands Its angular resolution is determined by the telescope diffraction limit, with FWHM beam widths of approximately 17, 24 and 35 arcseconds at 250, 350 and 500 µm, respectively An internal beam steering mirror can be used for spatial modulation of the telescope beam, and observations can also be made by scanning the telescope without chopping, providing better sensitivity for source confusion-limited deep surveys The FTS has a field of view of 26 arcminutes and an adjustable spectral resolution of 004 - 2 cm �1 (λ/∆λ = 20 - 1000 at 250 µm) It

/pdf/the-spire-instrument-for-herschel-43mpwhkq4s.pdf

The spire instrument for herschel

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The spire instrument for herschel