vvvsurvey.org
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vvvsurvey.org
VVV Survey A Progress Report 28 Jan 2010 Phil Lucas, Dante Minniti, for the VVV Science Team VVV SV Observations vvvsurvey.org No dry runs acquired for VVV yet (wrong time of the year). Only 2 hours during VISTA SV granted by the ESO DG. Requested observations of a single bulge field in order to: - test and optimize OBs and strategy - check photometry in a crowded field - test limiting magnitudes and errors - check astrometric accuracy vvvsurvey.org B L VVV OBs vvvsurvey.org Preparation of >2500 OBs for: - VVV dry runs to be observed in Feb 2010 - 16 disk tiles in ZYJHKs - all 196 disk tiles to be observed in semester 2010A: - multicolor ZYJHKs - Ks 5 epochs - all 352 bulge tiles to be observed in semester 2010A: - multicolos ZYJHKs - Ks 5 epochs This major activity was carried out recently by M. Hempel and R. Saito with help from M. Rejkuba, P. Lucas, V. Ivanov. Many details needed to be solved, many problems encountered (skies, concatenations, labeling, etc), this was indeed a huge work. vvvsurvey.org VISTA Tile b333 contains the Galactic Center e.g. problem with tiling on the GC, needed shift of position for all OBs VVV SV Observations vvvsurvey.org The 2 hs of observations during SV were successful: Observations of one bulge field at (l, b) = 2.6, -3.1 Acquired with variable seeing at high airmass. Single ZYJHKs observations acquired on 23 Nov 09. Other 12 different epochs of Ks spread between 19-29 Nov 09. Data reduced at CASU and made available to the VVV Team. What follows is a first look at these data. vvvsurvey.org B L Dry runs fields to be observed in Feb 2010 SV field observed in Nov 09: RA = 18:02:58.872 DEC = -28:36:59.04 vvvsurvey.org B L Dry runs fields to be observed in Feb 2010 SV field observed in Nov 09: RA = 18:02:58.872 DEC = -28:36:59.04 VVV SV Observations vvvsurvey.org NOVEMBER 2009 19th - seeing = 0.7” 20th - seeing = 0.8” 21st - seeing = 0.9” ll a filters =aKs tv er filters = Ks - Ks y 22nd - seeing = 1.3” 23rd - seeing = 1.0” hig h filters = Ks - Ks air ma ss filters = Ks es filters = Z - Y - J - H - Ks - Ks 24th - seeing = 1.0” filters = Ks 25th - seeing = 0.8” 26th - seeing = 1.1” 27th - seeing = 1.0” filters = Ks 13 different epochs in filters = Ks Ks - useful for RR Lyr filters = Ks search 28th - vvvsurvey.org VISTA 2MASS J-band 80”x110” Higher resolution Deeper magnitudes R. Barba Ks band vvvsurvey.org VISTA H-band Z band P. Lucas Problem with sky: residual stars seen. Will solve by concatenating multiple tiles. Ks band vvvsurvey.org VISTA H-band Z band P. Lucas Problem with sky: residual stars seen. Will solve by concatenating multiple tiles. vvvsurvey.org VISTA Ks-band Problems with sky substraction - e.g. chip 16 vvvsurvey.org VISTA 1 5 9 13 2 6 10 14 3 7 11 15 16 detectors 4 8 12 16 Ks-band pawprint with vvvsurvey.org VISTA Ks-band defects of detector 1 vvvsurvey.org VISTA Ks-band these defects of det. 6 were solved by Dec, but new defects appeared on det. 16 vvvsurvey.org VISTA Ks-band these defects of det. 6 were solved by Dec, but new defects appeared on det. 16 vvvsurvey.org VISTA Photometry of VVV test bulge test field: sample CMD containing 300.000 stars CASU pawprints catalogs contain 0.6 million stars/sqdeg, but PSF photometry yields ~1 million stars/ sqdeg. We are investigating the sources of this difference. VVV would produce multicolor and multiepoch photometry for about 5x108 sources in total O. Gonzalez background galaxies ? vvvsurvey.org VISTA Ks-band Photometry: comparisons with 2MASS (blue), and with different apertures from the pipeline (other colors). Astrometry OK Photometry OK small apertures (green) better large apertures for faint sources (red) better for bright sources O. Gonzalez vvvsurvey.org green = 2MASS black = VISTA O. Gonzalez vvvsurvey.org green = 2MASS RR Lyr zone black = VISTA O. Gonzalez vvvsurvey.org VISTA Ks-band 45”x45” Two known bulge RR Lyrae stars vvvsurvey.org VISTA Ks-band 6 epochs shown out of a total of 13 epochs observed vvvsurvey.org VISTA Ks-band 6 epochs shown out of a total of 13 epochs observed vvvsurvey.org Geryon cluster at PUC • 128 CPUs Xeon Intel • 2.0 GHz 512 cores 576 GB RAM 20 TB disk VVV Database: Thank funding Universities and Agencies in Chile: vvvsurvey.org Thank funding Universities and Agencies in Chile: vvvsurvey.org and STFC, UH, U Manchester, QMLondon, RAL,ROE, CASU and WFAU! VVV Scientific Goals vvvsurvey.org What is the 3-D structure of the bulge? How did the Milky Way form? To find bulge RR Lyrae To find eclipsing binaries and planetary transits To search for new star clusters To map star forming regions along the plane To search for microlensing events To monitor the variability around the Galactic Center (Also high proper motion objects, KBOs, SN light echoes, background QSOs...) vvvsurvey.org Conclusions The high quality of the data suggests that the VVV Survey would be able to accomplish these goals: images: OK photometric accuracy: OK astrometric accuracy: OK sensitivities: OK variability detection: TBD vvvsurvey.org The VVV Science Team: working with ESO and VISTA to obtain a 3-D view of our Galaxy.