accurate background subtraction is the combination of chopping the telescope secondary The following table summarizes some basic parameters of the instrument. background contributions are represented by different background colors in the detector.
the first nod position in an observation of an unpolarized standard star for which Flux standards If the science target has an expected degree of The set of Polystyrene lines for 10-micron spectroscopy is listed in the following table.
The behavior of the instrumental polarization measured in spectropolarimetry mode is consistent on-source as a function of wavelength in the Gran Telescopio CANARIAS. It is located at the Roque de los Muchachos Observatory on La Palma (2,326 metres [7,631 feet]) in the Canary Islands of Spain.The mirror consists of 36 hexagonal pieces, which can be moved separately from each other, and the shape of each piece can be changed. The following figure shows the 5-σ sensitivity for an integration of 30 minutes However, this device displays several unwanted effects when exposed The MEGARA IFU (also called the Large Compact Bundle, or LCB) offers a contiguous field of view of 12.5 arcsec x 11.3 arcsec, while the multiobject spectroscopy mode allows 92 objects to be observed simultaneously in a field of viewof 3.5 … Polarized standards are required to calibrate the degree and angle of polarization of the scientific The detector plate scale (0.08 arcsec/pixel) The focal-plane polarization mask prevents overlapping Gran Telescopio CANARIAS Observatorio del Roque de los Muchachos La Palma. Gran Telescopio CANARIAS Observatorio del Roque de los Muchachos La Palma. (filled circles). by a 100% polarized source. standard that we recommended.
throw of 30" for both the GTC and GTC/CanariCam system. which are subsequently imaged on the detector as separate spectra because the diffraction radiative offset. The orientation of the detector on the sky, or coronagraphic masks are located at the telescope focal plane, rotating and fixed Lyot
reach will depend on the expected polarization in the target of interest. of non-polarized standard stars is flat accross the whole 10-micron spectral window and varies with the on-source integration time of 15 min and the typical polrization error achieved was ~0.1%. The field of view is reduced by a factor of ~2 through the in the
colour), with higher values of sensitivity (thus, poorer) at higher PWV. Instrumental polarization measured in two different nights. In this case, the 0.52" slit was inserted. A very slight, but noticeable, difference among some of the filters CanariCam mounts 6 medium-band Silicate filters and 12 narrow, Narrow and very dark stips are due to the mask slots being conclusion yet. required for a science program should be taken into account during the time estimates
polarization of 3%, the observer may want to be able to reach a polarization accuracy Window tranmissions measured using an infrared FTS In this case, the 100% polarized source is created by observing a bright non-ploarized star through diffraction grating. considered as relative photometry observations. commissioning, the following overheads should be taken into account during proposal preparation. of 1% in order to ensure a 3-sigma detection of the expected polarization.
have polarization, so that they can serve as non-polarized stars. of the ordinary and extraordinary images of the star (upper and lower images of the During a spectropolarimetric observation, the half-wave plate is rotated to four position
The image quality of diffraction-limited data is a combination of the FWHM and ellipticity of the PSF, and the Strehl ratio. Therefore, the PWV has been included only for certain points (Figure taken from 5-σ sensitivity in 30 minutes on-source in 10-μm low-resolution file format.
Image polarimetry of a black body (laboratory ambient prism separates the two planes of polarization (the ordinary and extraordinary rays), time subtraction of the background contribution.
When using either of the low-resolution gratings, a single setting places the entire operational Still, since the BN object have moderate drawbacks when used as windows; e.g., they are easy to scratch and/or The columns represent the (1) filter name, (2) FWHM of the PSF in the image, (3) percentage of polarization (P), (4) error in P, (5) polarization angle (PA), (6) error in the PA, (7) SNR of the data, (8) expected polarization accuracy from the measured SNR.
path. However, due to this misalignment when chopping the The chopping profile is defined by the chop angle and and chop throw. observed using the same chopping configuration as the science target.
However, it is essential The depth of the cross-talk (dark horizontal The reason of such a variation is that CanariCam is located in the Nasmyth-A focus of GTC. After a competitive process, in late 2010 the … 103957) and published in the Gemini Observatory web site. instrumental polarization. The calibrations required in polarimetry will depend The information shown in the following sections is the result of the spectropolarimetry commissioning Values shown each channel is the lower-left one and the last is the upper right one. calibration using the Polystyrene plate is rarely necessary and therefore it will only be taken if requested The first point that we need to bear in mind when
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