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
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B
L
VVV OBs
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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.
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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
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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.
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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 -
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VISTA
2MASS
J-band
80”x110”
Higher resolution
Deeper magnitudes
R. Barba
Ks band
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VISTA
H-band
Z band
P. Lucas
Problem with sky:
residual stars seen. Will solve by concatenating multiple tiles.
Ks band
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VISTA
H-band
Z band
P. Lucas
Problem with sky:
residual stars seen. Will solve by concatenating multiple tiles.
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VISTA
Ks-band
Problems with sky substraction - e.g. chip 16
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VISTA
1
5
9
13
2
6
10
14
3
7
11
15
16 detectors 4
8
12
16
Ks-band
pawprint with
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VISTA
Ks-band
defects of
detector 1
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VISTA
Ks-band
these defects of det.
6 were solved by Dec,
but new defects
appeared on det. 16
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VISTA
Ks-band
these defects of det.
6 were solved by Dec,
but new defects
appeared on det. 16
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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
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green = 2MASS
black = VISTA
O. Gonzalez
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green = 2MASS
RR Lyr
zone
black = VISTA
O. Gonzalez
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VISTA
Ks-band
45”x45”
Two known bulge RR Lyrae stars
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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
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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.