1 / 19

Oct 16, 2009 Kaifeng

NAOC and Steward Observatory The South Galactic Cap U-band Sky Survey with the Bok 2.3m Telescope. Fan Zhou NAOC. Oct 16, 2009 Kaifeng. Why do we need the survey?. To supply the input source catalogue for LAMOST;

Download Presentation

Oct 16, 2009 Kaifeng

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. NAOC and Steward Observatory The South Galactic Cap U-band Sky Survey with the Bok 2.3m Telescope Fan Zhou NAOC Oct 16, 2009 Kaifeng

  2. Why do we need the survey? • To supply the input source catalogue for LAMOST; • To classify of the stars, galaxies, AGN and quasars in the south Galactic cap region with the color-color diagram; • To detect the red shift z<3 quasar candidates combining the photometry in other bands; • To estimate the red shift of the galaxies with PhotoZ combining the photometry in other bands; • To find out some starburst galaxies candidates; • It can help us estimate the metallicity of the stellar populations in the galaxies; • To identify the type of the stars in the color-color diagram combining the photometry in other bands, which can help us the control the completeness of the star type for the LAMOST observations; • It can be helpful for the flux calibration of the LAMOST spectra.

  3. Why do we need the survey? 图1:SDSS测光中的恒星(×),星系(△)和类星体(其中红移z< 3.5的源用□表示,红移z≥ 3.5的源用■表示)的双色图。 图2:1个太阳质量,年龄是1 Gyr的谱能量分布随金属丰度的变化。

  4. Project Directors • PI: Prof. Xu Zhou • PI: Prof. Michael Lesser

  5. The Bok • Organization: Steward Observatory. • Location: Kitt Peak, Arizona, USA • Wavelength: optical, infrared • Diameter: 2.3m (90 inches)

  6. Location―Kitt Peak • Altitude: 6,900 ft (2071 m) • Latitude: +31° 57' 46.5“ • Longitude: 111°36' 01.6"W • Time Zone: +7 hours

  7. The Telescope The Bok 90 inch (2.3 meter) Reflector Telescope

  8. CCDs • Focal Plane Array • CCDs: Four Lockheed Martin CCD4185 (unpackaged = CCD485 packaged) • Single CCD Format: 4096 x 4097 pixels • Single CCD Active Area: 61.20 mm x 61.21 mm • Inter-CCD Gap: 15.76 mm (~1050 pixels) • Total Focal Plan Array Area: 138.16 mm x 138.18 mm • Total Active Area: 122.40 mm x 122.42 mm • Total Pixel Count: 4 x 4096 x 4097 = 67125248 • Pixel Size: 15 µm • Plate Scale: 30.20"/mm • Pixel Scale: 0.453"/pixel • Edge-to-Edge Field-of-View: 1.159° x 1.159° • Active Field-of-View: 1.027° x 1.027°

  9. CCD configuration

  10. The CCD Overlapping

  11. The CCD Mosaic

  12. CCD QE

  13. SDSS DR7

  14. The U-band Sky MAP

  15. The U-band Sky Survey

  16. Flux Calibration

  17. Total Observation Time • If we got 55 nights: 55 nights ×10 hours / nights =550 hours • Calibration: 387×3min=21 hours • Each field: (550-21)hours×3/4 clear night/3700=6.43 min • If we got 80 nights: 80 nights ×10 hours / nights =800 hours • Each field: (800-21)hours×3/4 clear night/3700=9.47 min

  18. Thank you!

More Related