WINGS
Photometric (BVJK) and Spectroscopic Wide-Field Survey
of Cluster Galaxies in the local Universe
people involved in the project:
G.Fasano
M.Moles (Madrid.es)
B.M.Poggianti
P.Kjaergaard (Copenhagen.dk)
D.Bettoni
J.Varela (Madrid.es)
C.Marmo
W.Couch (Sydney.au)
E.Pignatelli
A.Dressler (Pasadena.edu)
+ M.D’Onofrio + L.Rizzi + C.Halliday + ... external collaborators...
Scientific targets of WINGS
global properties of galaxy
clusters in the local Universe
• radius
• total luminosity
• stellar mass
• geometry (ε, θ)
PHOTOMETRY
• virial-mass
• scaling laws
of clusters
• sub-clustering
SPECTROSCOPY
Scientific targets of WINGS
global properties of galaxy
clusters in the local Universe
• radius
• total luminosity
• stellar mass
• geometry (ε, θ)
PHOTOMETRY
• virial-mass
• scaling laws
of clusters
• sub-clustering
SPECTROSCOPY
properties of galaxies in nearby clusters as a function of cluster
properties, cluster-centric distance and local density
• morphology
• m T , Re , n
• color map
• E:S0:Sp:Irr
• Lum.Func.
• <µe>–re
• membership
• age-metallicity
• SFH
Scientific targets of WINGS
global properties of galaxy
clusters in the local Universe
• radius
• total luminosity
• stellar mass
• geometry (ε, θ)
PHOTOMETRY
• virial-mass
• scaling laws
of clusters
• sub-clustering
SPECTROSCOPY
properties of galaxies in nearby clusters as a function of cluster
properties, cluster-centric distance and local density
• morphology
• m T , Re , n
• color map
• membership
• E:S0:Sp:Irr
• age-metallicity
• Lum.Func.
link between photometric and
• <µe>–re
spectroscopic properties of galaxies • SFH
provide the astronomical community with a local
bench mark for evolutionary studies (data release)
The photometric survey
Selection: X-Ray flux: FX ≥ 4·10-12 erg cm-2 s-1 (0.1-2.4 keV)
ROSAT All Sky Survey (|b|>20º )
Redshift: 0.04 < z < 0.07 • Field ~1.6Mpc for z=0.04
• Resolution 1”~1.3kpc for z=0.07
(H0=70, q0=0.1)
Sample: 79 clusters (37 North, 42 South)
• broad range of LX and richness
• partial overlap with D80
The photometric survey
Selection: X-Ray flux: FX ≥ 4·10-12 erg cm-2 s-1 (0.1-2.4 keV)
ROSAT All Sky Survey (|b|>20º )
Redshift: 0.04 < z < 0.07 • Field ~1.6Mpc for z=0.04
• Resolution 1”~1.3kpc for z=0.07
(H0=70, q0=0.1)
Sample: 79 clusters (37 North, 42 South)
• broad range of LX and richness
• partial overlap with D80
Observations:
S/N=2/pix at µV~25.5
FWHMmax=1”.3
*completed
WFC CCD mosaics
•
•
*
INT / ESO (BV)
UKIRT (JK)
*in progress
*
*to be done
Abell 2457
The photometric survey
Selection: X-Ray flux: FX ≥ 4·10-12 erg cm-2 s-1 (0.1-2.4 keV)
ROSAT All Sky Survey (|b|>20º )
Redshift: 0.04 < z < 0.07 • Field ~1.6Mpc for z=0.04
• Resolution 1”~1.3kpc for z=0.07
(H0=70, q0=0.1)
Sample: 79 clusters (37 North, 42 South)
• broad range of LX and richness
• partial overlap with D80
Observations:
S/N=2/pix at µV~25.5
FWHMmax=1”.3
*
WFC CCD mosaics
•
•
*
INT / ESO (BV)
UKIRT (JK)
*
Deep catalogs : Sextractor (xc,yc, m, ε, θ, C) ;
completeness: 24.0 (-13.0) / 23.5 (-13.5)
*
Bright catalogs : surface photometry (mT, Re, n)
and morphology (T) of 350-700 galaxies per cluster
Automatic tools for both surface photometry
and morphology are clearly needed !!
*completed
*in progress
*to be done
Abell 2457
Galaxy Automatic Surface PHOtometry Tool
(Pignatelli, E., Fasano, G. and Cassata, P., 2004, submitted to A&A)
GASPHOT
Purpose: to provide reliable estimates of the main photometric and structural parameters
of large galaxy samples by operating in fully automatic (blind) mode
Requirements: • Accuracy - unbiased estimate and small random variance of
the parameters (why not simply Sextractor ?)
?
• Robustness - meaningful results even under critical conditions
(faint / blended objects) and for want of initial guess of the parameters
Galaxy Automatic Surface PHOtometry Tool
(Pignatelli, E., Fasano, G. and Cassata, P., 2004, submitted to A&A)
GASPHOT
Purpose: to provide reliable estimates of the main photometric and structural parameters
of large galaxy samples by operating in fully automatic (blind) mode
Requirements: • Accuracy - unbiased estimate and small random variance of
the parameters (why not simply Sextractor ?)
?
• Robustness - meaningful results even under critical conditions
(faint / blended objects) and for want of initial guess of the parameters
Strategy: • Model - single Sersic law component: robust (small number of parameters) +
flexible enough + easy to be handled by both convolution and best-fitting
• Algorithm - Simultaneous χ2 best-fitting of the major- and minor-axis growth
light curves of each galaxy, by convolving the corresponding model profiles.
Hybrid between 1D (more robust) and 2D (more accurate) approaches
Galaxy Automatic Surface PHOtometry Tool
(Pignatelli, E., Fasano, G. and Cassata, P., 2004, submitted to A&A)
GASPHOT
Purpose: to provide reliable estimates of the main photometric and structural parameters
of large galaxy samples by operating in fully automatic (blind) mode
Requirements: • Accuracy - unbiased estimate and small random variance of
the parameters (why not simply Sextractor ?)
?
• Robustness - meaningful results even under critical conditions
(faint / blended objects) and for want of initial guess of the parameters
Strategy: • Model - single Sersic law component: robust (small number of parameters) +
flexible enough + easy to be handled by both convolution and best-fitting
• Algorithm - Simultaneous χ2 best-fitting of the major- and minor-axis growth
light curves of each galaxy, by convolving the corresponding model profiles.
Hybrid between 1D (more robust) and 2D (more accurate) approaches
galaxy
galaxy
reference
reference
catalog
catalog
star
star
reference
reference
catalog
catalog
SExtractor
SExtractor
Structure:
cycling
cycling
for
for
isophotes
isophotes
of
of
galaxies
galaxies
and
and stars
stars
star
star
profiles
profiles
growth
growth light
light
curves
curves of
of
galaxies
galaxies
(maj/min)
(maj/min)
space
-varying
space-varying
multi
-gaussian
multi-gaussian
PSF
PSF
χχ22 best
-fitting
best-fitting
black
black box
box
model
model
convolution
convolution
(maj/min)
(maj/min)
Performances and Applications
GASPHOT
• Simulations on grid of deVaucouleurs (n = 4) and exponential (n =1) profiles
Performances and Applications
GASPHOT
• Simulations on grid of deVaucouleurs (n = 4) and exponential (n =1) profiles
• Simulations on grid of composite (deVauc.+exp.) profiles
Performances and Applications
GASPHOT
• Simulations on grid of deVaucouleurs (n = 4) and exponential (n =1) profiles
• Simulations on grid of composite (deVauc.+exp.) profiles
• Simulations including blending (cluster-like galaxy distribution)
Performances and Applications
GASPHOT
• Simulations on grid of deVaucouleurs (n = 4) and exponential (n =1) profiles
• Simulations on grid of composite (deVauc.+exp.) profiles
• Simulations including blending (cluster-like galaxy distribution)
• Real Galaxies: comparison with both interactive surface photometry and GALFIT
(single Sersic component)
Performances and Applications
GASPHOT
• Simulations on grid of deVaucouleurs (n = 4) and exponential (n =1) profiles
• Simulations on grid of composite (deVauc.+exp.) profiles
• Simulations including blending (cluster-like galaxy distribution)
• Real Galaxies: comparison with both interactive surface photometry and GALFIT
(single Sersic component)
some applications to the WINGS database:
• Color-Magnitude relations
• <µe> - Re (Kormendy) relations
MORphological PHOtometry Tool
(Fasano, G., Pignatelli, E., Cassata, P. et al., 2004, in preparation)
MORPHOT
can the ““standard”
standard” surface photometry solve the morphology problem ??
from Sanchez-Portal et al. (2004)
from the catalogs of three WINGS clusters
MORphological PHOtometry Tool
MORPHOT
Purpose: to provide automatic morphological type estimations of large galaxy samples.
Strategy: • to search for parameters featuring the statistical behaviour of the pixel set
defining each galaxy and correlating with the visual morphological type.
type
- extending the CAS parameter set (Concentration, Asymmetry, clumpinesS)
- including some global structural parameters from GASPHOT (n, ε).
8 new morphology indicators:
• C1 - average local concavity
• C2 - average local monotonicity
• C3 - average local gradient pointing
• C4 - average local gradient intercept
• C5 - r.m.s. of normalized counts
• C6 - kurtosis of normalized counts
• C7 - median of normalized counts
• C10 - azimuthal structure
MORphological PHOtometry Tool
MORPHOT
Purpose: to provide automatic morphological type estimations of large galaxy samples.
Strategy: • to check dependence of the parameter set on galaxy size.
size
MORphological PHOtometry Tool
MORPHOT
Purpose: to provide automatic morphological type estimations of large galaxy samples.
Strategy: • to get a global morphological estimator by combining such parameters
with ML or NN techniques.
Performances: on 479 visually classified galaxies from 3 WINGS clusters
MORphological PHOtometry Tool
Application:
WINGS clusters:
350-700 galaxies
10’ CPU time
Stars
• Ellipticals
• S0’s
• Early Spirals
• Late Spirals
MORPHOT