LAMOST Sky Survey --Site limitations and survey planning

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1 LAMOST Sky Survey --Site limitations and survey planning Chao Liu, Licai Deng National Astronomical Observatories, CAS Heidi Newberg Rensselaer Polytechnic Institute

2 Overview Site limitations that strictly constrain the survey and subsequently scientific goals of LAMOST weather and sky brightness Proposal of Milky Way stellar survey with LAMOST (LEGUE) c.f. a previous talk of Heidi Newberg

3 LAMOST optics

4 LAMOST Facts Aperture: ~4m Type: Schmidt, Alt-Az, Meridian Focal length: 20m Field of view: 5 degree diameter Size of focus plane: 1.75m Sky coverage: Dec>-10degrees, 1.5hours around meridian Wavelength: 370~900nm, R=1000/2000 Number of fibers: 4000, 16 spectrographs with 250 fibers each

5 Location Location: E N40 23 Elevation: ~900m

6 Weather Climate: Continental Monsoon Summer: rainy, cloudy, humid Winter: cold, dry, clear Spring: windy BATC weather logs from to The redder dots represents the better weather nights

7 Footprint of the planning LAMOST Survey of Milky Way stars sqdegs in total (blue area are double counted)

8 Extinction Coefficient BATC historical data from k=0.3 Y. Liu et al. 2003

9 Seeing BATC is a Schmidt telescope with CCD image resolution of 1.7arcsec/pixel A small telescope is being used to monitor the seeing for LAMOST Y. Liu et al. 2003

10 Sky Brightness Moon Light pollution from nearby cities turning worse due to economy development Climate factors Air pollutions Scattering surrounding ground of MA

11 Moon contribution in sky brightness BATC monitor data pointing to the North pole from In order to estimate the sky brightness for any position of the sky at any time, we need a model to describe the sky brightness as a function of moon phase and angular separation between moon and sky position etc. Y. Liu et al. 2003

12 Modeling the sky brightness Krisciunas & Schaefer 1991 based on observation at Mauna Kea where αis the phase angle of the moon, ρ is the angular separation between the observation sky position and the moon, f(ρ) is the atmospheric scattering function, which is the sum of Rayleigh and Mie scattering, Z is the zenith distance of the sky position. k is the extinction coeffecient, and Bmoon is the model surface brightness contributed of the moon

13 Testing the model with sky brightness data at the north pole in Xinglong observed by BATC from The data includes bad weather which is not suitable for observation as well. The model sky brightness is ~0.3mag deeper than the data. Difficulties for the model applying on Xinglong: -different atmospheric scattering -extinction coefficient -weather conditions

14 The dark night sky brightness Limited mag with 90min exposure at 550nm (Xue Y. 2008) -BATC sky brightness data is turning worse in the future years. -Fiber mag of sky brightness at 20.5mag would be 17.6~18.4mag -This will constrain the scientific goal of LAMOST ObjType skybr=20.5 skybr=19.5 skybr=19 S/N=3 S/N=10 S/N=3 S/N=10 S/N=3 S/N=10 Pointed src Elliptical Spiral

15 Sky Coverage DEC=-10~70degs (vignetting is significant when DEC>70deg ) 902 plates, each of which is ~20 sqdegs: 605 in higher Galactic latitude ( b >20) and 297 in lower Galactic latitude ( b <20) The strategy of the survey is to assign the dark and grey nights to fainter objects at high latitude and assign the bright nights to brighter objects at low latitude

16 Observe high latitude at grey/dark nights Sky brightness Dec Repeat times 580 of 605 plates will be observed from ; totally 2609 observed plates Average repeat times:~4.5

17 Observe low latitude at bright nights Sky brightness 204 of 297 plates will be observed from ; totally 609 observed plates Averag repeat times~3 Dec Repeat times

18 LAMOST is a meridian telescope and cannot point to any position, thus the sky footprint of one-year survey is discontinuous. The following plots are survey footprints in 2010

19 Maximum number of spectra (5-year plan) Total observed plates: ~3218 High latitude( b >20, g<20): ~2609 Low latitude( b <20, B<16):~609 Total number of spectra/year High latitude: 2609/5*3500~1.8 x 10 6 Low Latitude: 609/5*3500*2.5~1.1 x 10 6 Totally ~1.9 x 10 6 A 5-year plan: ~1.45 x 10 7 spectra 9 x 10 6 in high latitude (stars, QSOs and Galaxies) 5.5 x 10 6 in low latitude (stars, HI, HII, CO,...)

20 The LAMOST Survey of Milky Way Stars(LEGUE) Basics 2.5 million stellar spectra in 5 years 17<g<20 at high latitude B<16 at low latitude use dark/grey nights at high latitude with a quarter of the fibers pointing to stellar objects bright nights at low latitude with most fibers pointing to stellar objects R=5000 grating used at low latitude

21 The LAMOST Survey of Milky Way Stars(LEGUE) Scientific goals Substructure, formation and evolution of the Galactic stellar halo kinematics, formation history, chemical and dynamical evolution of the disk population

22 Substructure of the Milky Way

23

24 Ivezic et al. 2008

25

26

27 Outstanding problems The observation data is more complicated than models, how do we compare them? What the dark matter potential of the Milky Way looks like? How many stellar components are there in the Milky Way, and how to describe them? What is the detail structure of the Milky Way s disks? How is it related to Monoceros/Canis Major? How many dwarf galaxies are merged to create the Milky Way, and when? Study the frequency of metallicity as a function of position in the Milky Way, favoring detection of rare, low metallicity stars. Disentangle the components of the Galactic disks and possible tidal debris therein Describe the chemical evolution of the Galactic disks. How do we utilize all of the partial chemical, kinematical, and spatial information at the same time?

28 Suggestions for target selection Understand the limitation of the telescope: instrument, site and time allocation Identify the grand challenge science goals that can be accomplished, and design a grand survey that can be analyzed statistically. How to consistently select target objects from both SDSS footprint and non-sdss

29 Thanks!

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