VST deep imaging surveys - VLT Survey Telescope Nicola R. Napolitano
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VLT Survey Telescope
VST deep imaging surveys
Nicola R. Napolitano
INAF-Observatory of Capodimonte
Follow-up of wide-area X-ray surveys, Ringberg Castle, Bavaria, 25-27 April 2016
The sky of surveys Follow-up of wide-area X-ray surveys, Ringberg Castle, Bavaria, 25-27 April 2016
The sky of surveys
ATLAS-S
ATLAS-N
Follow-up of wide-area X-ray surveys, Ringberg Castle, Bavaria, 25-27 April 2016
The sky of surveys
KIDS -N
ATLAS-S
ATLAS-N
KIDS -S
Follow-up of wide-area X-ray surveys, Ringberg Castle, Bavaria, 25-27 April 2016
The sky of surveys
KIDS -N
ATLAS-S
ATLAS-N
KIDS -S
DES
Follow-up of wide-area X-ray surveys, Ringberg Castle, Bavaria, 25-27 April 2016
The sky of surveys
KIDS -N
ATLAS-S
ATLAS-N
KIDS -S
DES
Follow-up of wide-area X-ray surveys, Ringberg Castle, Bavaria, 25-27 April 2016
VLT Survey Telescope
The VST in a nutshell
• Primary mirror: 2.6m
• Secondary mirror: 0.9m
• F# 5.5
• Field corrector with 3 lenses (2 in the telescope
+ 1 in the camera)
• Field: 1° x 1°
• Shack-Hartmann wavefront sensor
• AcXve M1 shape control (81 acXve axial
support + 3 axial fixed points)
• AcXve M2 posiXoning in 5 dof (hexapod)
• Autoguiding with probe in polar coordinates
• ADC with counter-rotaXng doublet of prisms,
exchangeable with 2 Lens corrector
VLT Survey Telescope
OmegaCAM
268 Mpixel 1°x1°
0.21 arcsec/pixel
32 scienXfic CCDs + 4 outer CCDs
Autoguiding
Image analysis curvature sensor
PI: K. Kuijken
OmegaCAM Consortium: Netherlands, Germany, Italy, ESO
VLT Survey Telescope DIQ=0.45’’
VLT Survey Telescope VST is really opXmized for the Paranal condiXons Primas et al. 2014, Messenger
VLT Survey Telescope
Large field of view vs.
High spaXal resoluXon
NGC1427A NGC1427A
color composite
HST
color composite VST
g’ r’ i’ bands,VST-Tube
0.8” seeing image VEGAS surveyVLT Survey Telescope
KIDS survey
1’’
data quality
ESO DR1 and DR2
PSF FWHM ellipXcity
(De Jong, Kuijken et al., 2015)VST Public Surveys The VST ATLAS PI Tom Shanks (Durham) 4500 square degrees of the Southern Sky in 5 filters to depths comparable to the SDSS + NIR from the VHS VISTA survey. • dark energy equaXon of state by examining the 'baryon wiggles' in the maler power spectrum • high redshim galaxies and quasars.
VST Public Surveys The VST ATLAS PI Tom Shanks (Durham) 4500 square degrees of the Southern Sky in 5 filters to depths comparable to the SDSS + NIR from the VHS VISTA survey. • dark energy equaXon of state by examining the 'baryon wiggles' in the maler power spectrum • high redshim galaxies and quasars.
VST Public Surveys The VST ATLAS PI Tom Shanks (Durham) 4500 square degrees of the Southern Sky in 5 filters to depths comparable to the SDSS + NIR from the VHS VISTA survey. • dark energy equaXon of state by examining the 'baryon wiggles' in the maler power spectrum • high redshim galaxies and quasars. KIDS The Kilo-Degree Survey PI Konrad Kuijken (Leiden) 1500 square degrees in 4 bands (+ NIR VISTA/VIKING survey) ~2 magnitudes deeper than the Sloan Digital Sky Survey (SDSS). • weak gravitaXonal lensing: studying dark maler halos and dark energy with weak lensing, • invesXgaXng galaxy and cluster evoluXon, large-scale angular power spectrum and the equaXon of state of the dark energy • high redshim quasars.
VST Public Surveys The VST ATLAS PI Tom Shanks (Durham) 4500 square degrees of the Southern Sky in 5 filters to depths comparable to the SDSS + NIR from the VHS VISTA survey. • dark energy equaXon of state by examining the 'baryon wiggles' in the maler power spectrum • high redshim galaxies and quasars. KIDS The Kilo-Degree Survey PI Konrad Kuijken (Leiden) 1500 square degrees in 4 bands (+ NIR VISTA/VIKING survey) ~2 magnitudes deeper than the Sloan Digital Sky Survey (SDSS). • weak gravitaXonal lensing: studying dark maler halos and dark energy with weak lensing, • invesXgaXng galaxy and cluster evoluXon, large-scale angular power spectrum and the equaXon of state of the dark energy • high redshim quasars.
VST Public Surveys
Synergy with VISTA telescope u-K wavelength coverage
z
accurate photo-z
Euclid
LSST
CFHTLS Deep
DES
PANSTARRS
CFHTLS Wide
KIDS +VIKING
SDSS+UKIDSS
λ (u → K)VST Public Surveys
ATLAS KIDS
median AB magnitude limits
u-band 22.0(5σ) ! 21.3(10σ) u-band 24.2 (5σ)
g-band 23.1(5σ) ! 22.4(10σ) g-band 25.0 (5σ)
r-band 22.7(5σ) ! 22.0(10σ) r-band 24.9 (5σ)
i-band 22.0(5σ) ! 21.3(10σ) i-band 23.6 (5σ)
z-band 20.9(5σ) ! 22.0(10σ)VST Public Surveys
eROSITA main Science
r-band(5σ)
KIDS
i-band
ATLAS
Clusters
Best characterisaXon, given the scaler of
the esXmator, is reached when m+1 galaxies
are included: r~24, i~23, z~22 (5σ at z ~1).
AGN
luminosity distribuXon of AGN detected
with eROSITAVST future
Call for leWer of Intent for VST GTO large programs on 2016-2021
2500h offered to the whole communityKABS survey
KABS: KiDS VST-ATLAS Bridging Survey
courtesy of T. Dwelly ATLAS web site
(9)
eROSITA custers: r~24, i~23, z~22 (5σ at z ~1)KABS survey
KABS: KiDS VST-ATLAS Bridging Survey
750 h VST Italian GTO in 4.5 years / 1000 deg2 / 3 bands: gri
+ z-band from the VST iz Bright (PI Finoguenov)
+ u-band from DEUCE (PI Shanks)
Finoguenov proposal
Shanks proposal
|b| > 20 deg
E(B-V) < 0.1 mag
N_H < 7e20 cm^-2
-65 < Dec < -30 degKABS survey
KABS: KiDS VST-ATLAS Bridging Survey
750 h VST Italian GTO in 4.5 years / 1000 deg2 / 3 bands: gri
+ z-band from the VST iz Bright (PI Finoguenov)
+ u-band from DEUCE (PI Shanks)
+ WISE (mid-IR)
+ EMU (Radio)
+ VISTA future programs to go deeper than VHS?
KiDS + uKABSz will provide deep photometry suitable for eROSITA and
4MOST science over ~2500 deg2
u-band (5σ) g-band (5σ) r-band (5σ) i-band (5σ) z-band (5σ)
KABS 22.5 24.0 23.8 23.0 22.3
KIDS 24.0 24.0 25.0 24.0 N/AKiDS/KABS survey products
KiDS/KABS photo-z
opgcal bands only
CavuoX et al. 2015
spectroscopy from Gama & SDSS (~22k)
σ=0.03; bias=0.0008; outliers(>15%)=0.4%
90% completeness=22.5(g),21.5(r),20(i) training sample limited
Gaussian aperture/PSF photometry (GAAP)
Photometric calibraXon vs. SDSS
Deep training sample (COSMOS, CDFS)KiDS/KABS survey products
Cavuog, Brescia, Tortora, Longo, et al. in preparagon
2.5
2.0
LTGs
1.5
FΛ !F5500
1.0
ETGs
0.5
0.0
40
T
20
Λ "Å#
4000 6000 8000KiDS/KABS survey products
ASROWISE specialized for KiDS (python+ distributed database ORACLE)
FP5 RTD program funded by the EU "Enhancing Access to Research Infrastructures”
INAF-OACKiDS/KABS survey products
ASROWISE specialized for KiDS (python+ distributed database ORACLE)
FP5 RTD program funded by the EU "Enhancing Access to Research Infrastructures”
INAF-OAC
Astro-Wise is handling data and sourcelists also from other Instruments/projects:
OmegaCAM opgcal
DECAM opgcal/NIR
Subaru opgcal
HST opgcal
VIRCAM NIR
LOFAR Radio
EUCLID opgcal/NIR
is the ideal environment for mulX-band mulX purpose/intrument datasetsKiDS/KABS survey products
ASROWISE specialized for KiDS (python+ distributed database ORACLE)
FP5 RTD program funded by the EU "Enhancing Access to Research Infrastructures”
INAF-OAC
KIDS-CATKiDS/KABS survey products KIDS-CAT – automatic masking
KiDS/KABS survey products
KIDS-CAT – automatic masking
good sources star haloes maskKiDS/KABS survey products
KIDS-CAT – automatic masking
good sources star haloes maskKiDS/KABS survey products
KIDS-CAT – automatic masking
good sources star haloes mask reflec./defectsKiDS/KABS survey products
KIDS-CAT – automatic masking and sourcelists
good sources sure stars flagged sourcesKiDS/KABS Science
KiDS
• gravitaXonal lensing
• dark maler and dark energy (via WL)
• galaxy evoluXon (WEAVE/4MOST)
• galaxy clusters search (eROSITA)
• high redshim quasars (z>7) (eROSITA)
KABS
• detecXon of galaxy clusters (eROSITA/4MOST)
• the census of the AGN populaXon (eROSITA)
• galaxy evoluXon + the dark maler fracXon
and iniXal mass funcXon (4MOST)
• Strong lensing detecXon (4MOST)
• Milky Way satellites search
• the idenXficaXon of colour selected QSOs
(eROSITA)KiDS/KABS Science
A693 cluster as imaged by KiDS
KiDS/KABS: Searching for galaxy clusters
Radovich, Puddu, Bellagamba, Roncarelli, Moscardini et al.
Goal: idenXfy galaxy clusters and measure their mass/
richness at 0 < z < 1 (using KiDS+VIKING but also uKABSz)
Matched filter algorithm by Bellagamba et al. (2011) to
search for galaxy overdensiges in (α, δ, mag, redshim).
~1800 with 95% completeness at zKiDS/KABS Science KiDS/KABS: cosmology Roncarelli, Moscardini, Marulli, Veropalumbo, Moresco et al. Linear growth rate from redshim-space distorXons → galaxy clusters are more strongly biased than galaxies, and less affected by non-linear distorXons at small scales (Marulli et al. 2015) Cosmological constraints from number counts and clustering → exploiXng mass measurements and spaXal properXes of galaxy clusters (Mana et al. 2014) Distance-redshim relaXon from Baryon AcousXc OscillaXons → reconstrucXon not required for clusters due to negligible effects from non-lineariXes (Veropalumbo et al. 2013-2016)
KiDS/KABS Science
KiDS/KABS: Tools for cosmological analyses
Roncarelli, Moscardini, Marulli, Veropalumbo, Moresco et al.
example codes are publicly available
hlp://apps.difa.unibo.it/files/people/
federico.marulli3/CosmoBolognaLib/
2pt correlaXon funcXon of VIPERS halo mass funcXon in massive neutrino
galaxies (Marulli et al. 2013) cosmologies (Marulli et al. 2011)
cosmological constraints from 2pt redshim-space distorXons in
correlaXon funcXon and BAO interacXve dark energy
(Veropalumbo et al. 2016) cosmologies (Marulli et al. 2012)KiDS/KABS Science
KABS: variability and AGN detecgon
Paolillo, De Cicco, Longo, Salvato et al.
VST-GTO observaXons SUDARE/VOICE Survey as test-bed for KABS efficiency
4-yr VST ugri SN Survey completed in P94 (Mar
2015) – COSMOS, and CDFS & ES1 (TBC in 2016)
matched with VIDEO & SERVS
Chandra data (Civano et al. 2012, Cavan et al. 2015)
XMM-Newton (Brusa et al. 2010)KiDS/KABS Science
KABS: variability and AGN detecgon
Paolillo, De Cicco, Longo, Salvato et al.
COSMOS fields showed that:
• there are a number of SNe in the sample
•Purity: 94% are confirmed AGNs (67). Type 1 are
prevalent (89%) compared to Type 2 AGNs
(11%).
•Using the 3.5 years baseline we now confirm
an average completeness of ~ 50% with respect
to X-ray confirmed samples.KiDS/KABS Science
KABS: variability and AGN detecgon
Paolillo, De Cicco, Longo, Salvato et al.
Rescaling the COSMOS single-epoch depth and
S/N raXo to the KABS expected performance we
get, for 1 sq.deg. FOV:
•Detecgons: AGN candidates with mag < 21.5: 115
•Purity: confirmed AGN (by spectroscopy/X-O/opOcal or IR colors): 78/115 = 68%
•Completeness: with respect to X-ray catalogs: 33% (Type 1 AGN 57%, Type 2 AGN 10%)
Assuming 300 X-ray AGNs per sq.deg. down to mg=21.5 we expect to detect ~100/sq.deg.
and thus (considering 22% masked area) 1.6x104 variable AGN over the KABS area with
variability (~200 deg2).KiDS/KABS Science
KiDS/KABS: galaxy structure, morphology, and strong lensing
Napolitano, La Barbera, Tortora, Roy, Radovich, Getman, et al.
KiDS: 70M galaxies expected; 7M with SNR high enough (SNR_r>50) for quanXtaXve
morphology out to z=0.6.
KABS: 23M galaxies expected; 2M with SNR high enough (SNR>50) for quanXtaXve
morphology out to z=0.4-0.5.KiDS/KABS Science
Checking vs. external catalogs: 345 galaxies in KiDS – SDSS overlapping regions
n-index Re luminosity
SPIDER
KIDS
Comparison of structural parameters from KiDS and SPIDER (La Barbera F. et al. 2010). The structural
parameters are derived using 2DPHOT. We show the relaXonship for a) effecXve radius, Re, b) model
magnitude and c) Sérsic index. Data are shown as pink points. The diagonal lines are the one-to-one
relaXons, corresponding to the perfect agreement.KiDS/KABS Science
Checking vs. simulated galaxies
1.5
1
0.5
Log reout
0
-0.5
-0.5 0 0.5 1 1.5
Log reinKiDS/KABS Science
Sample of higher-z galaxies
z=0.3
z=0.4
z=0.5KiDS/KABS Science KiDS/KABS: strong lensing #SL - gal/gal now KiDS ~650 ~1500
KiDS/KABS Science KiDS/KABS: strong lensing
KiDS/KABS Science
KiDS/KABS: strong lensing
KiDS KABS ATLAS
4MOST follow-up?Summary • VST surveys are providing exquisite data for eROSITA/4MOST “pre- imaging”. The deepest among the ongoing/future surveys (KiDS and KABS) will cover about 2500 deg2 of the D-eROSITA. More 3000 deg2 are provided by ATLAS (with the i band supply from VST iz Bright). • KiDS and KABS have the right depth (i>23) for cluster characterizagon of eROSITA cluster up to z=1 and AGN detecgon. Variability would provide high purity of the AGN selecXon and X-ray associaXon • KABS needs complementary data (u-DEUCE, VST iz Bright) to have the sufficient baseline to have photo-z of the order of 0.02 precision.
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