Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.eso.org/sci/activities/docs/Call_MUSE_DF.pdf Дата изменения: Tue Nov 17 15:50:18 2015 Дата индексирования: Sun Apr 10 23:24:29 2016 Кодировка: Поисковые слова: http astrokuban.info astrokuban

Call for Ideas: P ublic D e e p F ie ld w it h M U S E
The ESO Director General proposes to dedicate up to 60 nights of Director 's Discretionary Time1 in four forthcoming observing periods to a Public Deep Field using MUSE. To reach the best possible sensitivity with MUSE, this project will be carried out towards the end of 2017 with enhanced seeing capabilities provided by GALACSI ­ the wide-field Ground Layer Adaptive Optics (GLAO) unit of the quad-laser Adaptive Optics Facility (AOF) on UT4 of the Very Large Telescope. Exploiting these genuinely remarkable and unique ESO facilities in this way will yield the deepest unbiased optical spectroscopic observations ever undertaken, with immediate impact and the potential to catalyse further breakthroughs in the era of the James Webb Space Telescope and beyond. The goal of this call is to collect ideas from the astronomical community, ensuring the selection of a target field with the greatest potential to advance our understanding of the Universe. ESO requests that ideas be sent to musepublicsurvey@eso.org no later than: February 29th, 2016 The proposed ideas will be reviewed by a panel appointed by the Director General, chaired by the Director for Science. The selected field will be announced by the end of 2016.

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The conventional Director 's Discretionary Time (DDT) route will be unaffected; typical usage runs to 15 of the 30 nights available in each period for DDT.


C o nt e nt s o f t h e Re s p o n s e t o t h i s C a l l
In response to this Call, proposals for a Public Deep Field with MUSE are expected to contain the following sections: 1. Scientific justification for the selection of suggested field, or small mosaic, including synergies with observations conducted using present and forthcoming ground- and space-based facilities. 2. Fully documented finding chart of the selected field, or small mosaic, demonstrating compliance with the technical requirements given below, including: a. coordinates of the field centre; b. coordinates of the tip-tilt star and of an alternative tip-tilt star; c. coordinates of one or more slow guiding star(s); d. coordinates of a PSF reference star. The proposal should consist of no more than four A4 pages in 12pt font, including the finding chart, with no annexes.

O b s e r va t i o n a l r e q u i r e m e n t s
The following requirements have been set to obtain high spatial resolution and a very deep exposure using MUSE and AOF. Note that in case of a small mosaic of adjacent 1' x 1' MUSE fields, the requirements must be fulfilled for each pointing. MUSE field of view, with AOF/GALACSI: 1' x 1' (see red square in Figure); Due to the dithering process, the field of view with optimal S/N is smaller, typically 58" x 58" MUSE sampling: 0.2" x 0.2"; For a mosaic, overlap between neighboring fields can be limited to 2".

PSF reference star: The point source used to measure the PSF accurately, on individual exposures and on the combined exposure; R(AB) < 20.0; Must be located within the central 50x50" (preferably 40x40") safe area, excluding field edges (see orange square in Figure). AO ti p/tilt star: The star used by AOF/GALACSI; R(AB) < 17.5; Must be located in the AO tip/tilt area (see blue annulus in Figure).


SGS guide star(s): The source(s) used by the slow-guiding system (SGS) to correct for the de-rotator wobble and other low-frequency mismatches between the AO focal plane and the MUSE instrument. The system can use more than one source, if available; the source does not need to be point source ­ compact galaxies can also be used; V(AB) < 20.5; Source must be located in the SGS safe area (see four 8 x 30 arcsec2 green rectangles in Figure, centered at 37" from the field centre). This location ensures that the source can be used throughout the default dithering process. Field location: The limit on the telescope absolute zenith angle, z < 60 deg, gives an absolute declination range between -84.5 and +35.5 deg; To get good AO performance and allow long visibility at low airmass (z < 20 deg), the recommended declination range is between -44.5 and -4.5 deg; Avoiding transits within 5 deg of zenith allows easier scheduling. This translates to declination ranges of -44.5 to -29.5 deg and -19.5 to -4.5 deg; A southern field, i.e. one located between -44.5 and -29.5 deg, would avoid the pointing restriction enforced for northerly winds; The field should have low Galactic extinction; The field must not contain or be located very close to a bright, V(AB) < 12 approx., star or galaxy.

Q u e st i o n s r e l at i n g to t h i s C a l l
Please contact ESO's Director for Science, rob.ivison@eso.org


Figure