Updates: 10.05.2012 (Tolga)
5.2 Current and Future Survey Projects
Updates: 11.05.2012 (Aliş)
CFHQSIR (CFHTLS Y-band WIRCam Large Program)
The CFHQSIR* survey consists in WIRCam Y-band imaging of the 171 CFHTLS Wide fields distributed over four patches across the sky. The main scientific objective of CFHQSIR is to search for quasars at redshifts ~7 (the principal investigators are J.-G. Cuby for France & C. Willott for Canada). CFHQSIR will also detect brown dwarfs and complement the CFBDSIR program. As a near IR counterpart of the CFHTLS, CFHQSIR will be of general interest to a large community of CFHTLS users.
Each WIRCam pointing (20'x20' field of view, 9 WIRCam pointings are needed to cover one single one square degree MegaCam tile) consists of 4-dithered 75 second Y-band exposures split in two 2-exposure visits separated by at least 20 days. At the end of the survey, all four CFHTLS Wide patches made from a total of 171 MegaCam pointings will lead to a sky coverage of 150 sq.deg. once the overlaps between pointings and gaps have all been accounted for. The depth of the total 5mn integration will be defined by the ~0.6" median image quality and low to medium sky background.
Updates: 11.05.2012 (Aliş)
WIRDS is a program devoted to detect galaxy clusters using CFHTLS optical data added with NIR observations are being taken with WIRCAM attached to the CFHT. So far program focused on the Deep fields of the CFHTLS due to limited time allocation. Inclusion of NIR data to the optical CFHTLS data it will become possible to detect galaxy clusters further than z>1.1.
Updates: 12.05.2012 (Aybüke)
UKIRT Infrared Deep Sky Survey - UKIDSS
UKIDSS is the next generation near-infrared sky survey, the successor to 2MASS. UKIDSS began in May 2005 and surveyed 7500 square degrees of the Northern sky, extending over both high and low Galactic latitudes, in JHK to K=18.3. This depth is three magnitudes deeper than 2MASS.
UKIDSS consists of 5 different surveys: Large Area Survey (LAS), 4000 sq. degs, K=18.4; Galactic Plane Survey (GPS), 1800 sq. degs, K=19.0; Galactic Clusters Survey (GCS), 1400 sq. degs, K=18.7; Deep Extragalactic Survey (DXS), 35 sq. degs, K=21.0; Ultra Deep Survey (UDS), 0.77 sq. degs, K=23.0.
Four of the principal quarry of UKIDSS are: the coolest and nearest brown dwarfs, high-redshift dusty starburst galaxies, elliptical galaxies and galaxy clusters at redshifts 1‹z‹2, and the highest-redshift quasars, at z=7.
UKIRT Hemisphere Survey - UHS
The aim of UHS is to survey Dec < 60 deg in K <~18.2 and J (and H later on) especially the areas that were not covered by UKIDSS and thus to be the Northern sky equivalent of the VISTA VHS survey.
Updates: 14.05.2012 (Korhan)
The Synoptic All-Sky Infrared Survey - SASIR
SASIR is a dedicated wide-field (1degree diameter) large aperture telescope (6.5m in diameter) project aiming deep and synoptic imaging of the whole Northern sky simultaneously in NIR bands (Y, J, H and K) with four independent focal planes.
Fig-5.2-1. SASIR-UKIDSS-VISTA numbers in z
It is submitted to the "Optical and IR astronomy from the ground" program prioritization panel of the Astro2010 Decadel Survey.
In the mountains of Baja California, at the San Pedro Mártir (SPM) Observatory, a 6.5 meter telescope will be constructed over the next several years. The JHKs survey, based upon a camera with ~124 2k x 2k IR arrays and a field of view of 0.7 degrees, is expected to begin in 2017 and last for 4 years. The aim is to repeatedly image the sky to a level 100 - 500 times deeper than the 2MASS survey, uncovering the most distant objects and revealing the transient universe.
Updates: 14.05.2012 (Korhan)
The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)
The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) is a National Major Scientific Project undertaken by the Chinese Academy of Science. The site is about 100 miles northeast of Beijing, China. The large, 4-meter mirror of LAMOST enables it to obtain spectra of faint objects. LAMOST is designed with 4000 optical fibers in the optical path, covering a large region of the sky simultaneously. This unique system will be used to conduct a survey of 10 million stars in our Galaxy, as well as millions of distant galaxies, over a 5-year period. LAMOST can thus obtain spectra of more than 10000 stars per night, and more than 2 million stars per year.
The LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) is a survey that will obtain spectra of roughly 8 million stars selected for the detailed study of our Milky Way Galaxy.
Resolution(s): R=1800, 5000, Wavelength range: 3700-9000 Angstroms (R=1800 mode) and field of view is 5 degree.
LAMOST will survey at least 2.5 million Galactic halo stars selected from SDSS imaging (where available - otherwise, targets will be chosen from the XuYi survey, PanSTARRS, or SuperCOSMOS photometry) with |b| > 20°. The spheroid survey will cover at least 5000 square degrees in two contiguous sky areas in the north and south Galactic caps, at a density of at least 320 stars per square degree.Fibers will be assigned to targets based on a simple, uniform set of selection criteria using g, (g-r), (u-g), proper motion, and weighted random sampling to ensure a statistical sample is obtained that can be used to infer the characteristics of the stellar populations probed. It started to observe in October 24, 2011 and will continue over 5 years.
What can be done with DAG
- Perform complementing observations especially in the near-IR.
- The LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) survey is an on-going project and it will have low resolution data (spectroscopic resolution 1500-5000) in next 5 years. It will provide lots of new objects and by using its MOS-fiber instrument it will have a big amount of object numbers. It's necessary to compete with this size of survey DAG may need a kind of MOS and high resolution instrument at all.
- DAG and SASIR projects will cover the northern sky and especially in same infrared range(JHK) in approximately the same years. In near future, DAG should have abilities to make deep or ultra-deep surveys or well-design instruments for deep objects.