JENAM 2004
JENAM 2004
JENAM 2004
JENAM 2004
Started October 2002
JENAM 2004
Core team Granada, at IAA:
S. Leon, (Post-docs)
D. Espada, S. Verley (PhD)
JENAM 2004
J. Sabater (Post-gr)
E. García (Software)
U. Lisenfeld (Postdoc, Univ. Granada)
November: + G. Bergond (Post-doc)
Direct collaborators:
J. Sulentic (University of Tuscaloosa)
W. Huchtmeier
(Max Planck IfR, Bonn)
S. Odewahn (Arizona State University)
M. S. Yun (UMass)
JENAM 2004
Core team Granada, at IAA:
F. Combes (Obs. Paris –LERMA)
M. Rosado (UNAM)
D. Espada, S. Verley (PhD)
A. Bosma, L. Athanassoula (Obs. Marseille)
J. Sabater (Post-gr)
M. Gutiérrez-Valdez (Univ. Guanajuato)
E. García (Software)
I. Puerari
U. Lisenfeld (Postdoc, Univ. Granada)
A. Ballu
JENAM 2004
S. Leon, (Post-docs)
November: + G. Bergond (Post-doc)
(INAOE)
(ENSP Strasbourg)
MOTIVATION
Direct interaction-enhancement connection difficult to
establish
ƒ
E.g groups vs pairs:
HCGs: Evidence for HI depletion, excess SF (Halfa, FIR)
or H2 not observed
(e.g. VM et al ´01, Iglesias-Páramo & Vílchez ´99)
Pairs: SF excess, H2 excess?, no HI deficit
JENAM 2004
(Xu & Sulentic ´91, Zasov & Sulentic ´94)
CONTROL SAMPLES
Selection:
FIELD galaxies (e.g. Kennicut & Kent ´83)
“NORMAL” galaxies (e.g. Boselli et al ´01)
Galaxies with no redshift data are not considered
companions
(Kelm & Focardi ´04: isolated with respect to companions brighter
than 15.5mag)
Number:
JENAM 2004
10 – 100/200 members
(Huchra & Thuan ’77, Vettolani et al ’86, Márquez & Moles ’99, ’00,
Colbert et al ’01, Pisano et al ´02, Varela et al ´04)
CONTROL SAMPLES
Selection:
BUT we usually find, either
FIELD galaxies (e.g. Kennicut & Kent ´83)
“NORMAL” galaxias (e.g. Boselli et al ´01)
Galaxies with
no redshift
are notSAMPLES
considered
monochromatic
observations
of data
LARGE
companions
(Kelm & Focardi ´04: isolated and companion limited at 15.5mag)
Number:
10 – 100/200 members
JENAM 2004
(Huchra & Thuan ’77, Vettolani et al ’86,, Márquez & Moles ’99, ’00,
Colbert et al ’01, Pisano et al ´02, Varela et al ´04)
CONTROL SAMPLES
Selection:
BUT we usually find, either
FIELD galaxies (e.g. Kennicut & Kent ´83)
“NORMAL” galaxias (e.g. Boselli et al ´01)
Galaxies with
no redshift
are notSAMPLES
considered
monochromatic
observations
of data
LARGE
companions
or
(Kelm & Focardi ´04: isolated and companion limited at 15.5mag)
Number:
small samples
10 – 100/200 members
JENAM 2004
(Huchra & Thuan ’77, Vettolani et al ’86,, Márquez & Moles ’99, ’00,
Colbert et al ’01, Pisano et al ´02, Varela et al ´04)
BY THE WAY...
© Karachensetva 1973
CIG: Catalogue of Isolated Galaxies
Selected from CGCG (Zwicky et al 1960-1968) with
mpg < 15.7
δ > -3
Strength:
- Size: 1050 galaxies
- Isolation: no similar sized galaxies (factor 4) within
40*R(companion) -> last interaction several Gyrs ago
JENAM 2004
- Morphology: permits discrimination based on types.
- Depth: large volume to allow sampling of the OLF.
- Completeness: 80-90% up to mZw(corr) = 15.0
OUR SAMPLE: CIG based
Major interactions are excluded
Hierarchical pairs and groups are kept AND quantified:
quantified
•Do truly isolated galaxies exist?
•In what numbers?
•Environmental level where the onset of interaction
induced activity can be first detected?
JENAM 2004
Optical (B) and NIR luminosity.
Atomic gas.
Radiocontinuum & FIR emission.
~ 1000
galaxies
CO & Halfa emission (200 galaxies)
OUR SAMPLE: CIG based
Major interactions are excluded
Hierarchical pairs and groups are kept AND quantified:
quantified
•Do truly isolated galaxies exist?
•In what numbers?
•Environmental level where the onset of interaction
induced activity can be first detected.
JENAM 2004
A large Optical
sample
multiwavelength
(B)for
and a
NIR
luminosity.
Atomic gas. of the low density tail of
characterization
Radiocontinuum & FIR emission.
the 2p correlation function.
CO & Halfa emission.
1. REFINEMENT OF THE SAMPLE
Isolation
Morhologies
Positions
Redshift and distances
JENAM 2004
2. MULTIWAVELENGTH STUDY
3. PUBLIC DATA
ISOLATION
(PhD S. Verley, SEE POSTER)
• Karachentseva was based on visual examination of
plates.
•Our revision
- POSS-I & II to evaluate a minimum physical
distance of 0.5 Mpc, up to B = 17.5 mag
JENAM 2004
- Reduced with AIMTOOL in LMORPHO
Star/galaxy separation
- Catalogs of all potential companions
(Odewahn ´95, ´96)
Isolation parameters:
(PhD S. Verley, SEE POSTER)
Karachentseva re-evaluated
Tidal force parameter (Dahari 1984)
Q: estimation of the gravitational interaction strength.
JENAM 2004
Also calculated for Hickson Compact Groups &
clusters
MORPHOLOGIES
Bibliography: non-uniform data
Contradictory NED vs LEDA
POSSII + CCD based revision (Sulentic et al in prep)
Early types: 16% (Sc dominate)
POSITIONS
(Leon & Verdes-Montenegro A&A 2003)
Revised for full CIG:
JENAM 2004
SExtracted (Bertin & Arnouts 1996) from DSS
and visually revised.
∆Max 44.5” ∆ Mean 1.8”
REDSHIFT AND DISTANCES
Archival + bibliography: 956/1050
478 more than in previous publications.
1/2 from ned & 1/2 from 41 different sources
10+ galaxies from our HI data
JENAM 2004
Distances:
v > 1000 km/s redshift based
v < 1000 km/s bibliographical search
1. REFINEMENT OF THE SAMPLE
2. MULTIWAVELENGTH STUDY
Optical characterization
FIR and radio continuum emission
Atomic gas
JENAM 2004
Molecular gas
Ionized gas
3. PUBLIC DATA
Optical: completeness
Blue magnitudes:
All CIG members have Zw magnitudes
We have corrected mZw from:
• systematic errors in the CGCG Volume I (Kron & Shane ´75)
• galactic dust extinction
• internal extinction
•
(IRAS/DIRBE Schlegel ´98)
(i and morphology following RC3)
K corrections (Pence ´76, Giovanelli ´81)
JENAM 2004
515 have also BT0
mZw(corr)=BT0-0.04 (±0.19)
Optical: completeness
V/Vm
V/Vm test
JENAM 2004
Limiting magnitude
•
CIG complete at 80-95% level up to m = 15 <V/Vm> = 0.42
•
Completeness with respect to CIG subsamples (XS91) significantly
improved (before < 80%).
Optical: OLF
Final sample for OLF calculation:
n= 692 galaxies with known distance, 11 – 15 mag
OLF derivation: global + morphologies
Comparison with different samples and environments
(SSRS2, 2dFGRS, NOG, HCGs)
- E/S0s fainter than in field samples, reflecting CIG
lower density environment.
JENAM 2004
- Sa - Im similar to field and dense environments.
- OLF enhancement in HCGs: ONLY in early types.
FIR & radio emission
J. Sabater DEA
Existing samples are biased toward bright FIR.
CIG will allow to study some open issues:
- Enhancement in weakly interacting pairs?
(Braine &
Combes 1993, Combes et al 1994 vs Perea et al 1997, Verdes-M et
al 1998)
- Difference between barred and non-barred?
1992 vs Perea et al 1997, Verdes-M et al 1998)
JENAM 2004
- FIR, Radio-LB correlation, bivariate LF
- Nuclear activity in isolated galaxies:
FIR-radio correlation
(Young
FIR & radio emission
FIR:
4 IRAS bands coadded from archive data
PSC-IRAS existed for only 303 galaxies
ADDSCAN/SCANPI improves snr by factor 3-5
Radio continuum: archive data re-processing
WENNSS 92cm (Westerbork Northern Sky Survey)
GB6 6 cm (Green Bank)
JENAM 2004
NVSS 20 cm (NRAO VLA Sky Survey)
Atomic gas
PhD D. Espada. SEE POSTER
Reference for M(HI) = f(LB, Ø, t)
HI single dish for nearly 800 CIG members
Origin of asymmetries in isolated galaxies:
Degree of symmetry of the spectra
VLA HI data for 20 asymmetric + isolated
JENAM 2004
ISM in isolated early types: what are they?
20 ISOLATED E’s +S0’s with ISM
Planning XMM observations
Molecular gas study
- Reference sample for molecular gas content missing
Dependence with LB, morphology and bars
Is H2 increased in interactions?
(Braine & Combes 1993,
Perea et al 1997, Verdes-M et al 1998, Leon et al 1998)
- H2 + HI data: total cold gas mass
- H2 + FIR: SFE study
JENAM 2004
CO single dish for 180/200 galaxies
IRAM 30m, FCRAO and Nobeyama.
Ionized gas study
-Local HaLF for well isolated galaxies
- SF as a function of the environment, based on small or
inhomogeneus control samples:
increased in strongly interacting pairs,
inhibited in CGs!
(e.g.
Kennicutt et al.
1987, 1994, Gavazzi et al 1991, 1998, 2002,
JENAM 2004
Young et al 1996, Iglesias-Páramo et al 1999, 2002ab)
Ionized gas study
(PhD S. Verley)
- Dependence of SFR with HI, H2 ¿and/or? HI+H2
(results differ in Kennicutt 1988, 1989,1998).
HII distribution characterization:
-
spiral arms, HII regions sizes & luminosities
JENAM 2004
Halfa images available for 180/205 CIGs
to be finished (weather permitting) early 2005
JENAM 2004
3. PUBLIC DATA (VO standards)
JENAM 2004
SUMMARY
SUMMARY
AMIGAS/OS!!!!
JENAM 2004
Visit AMIGA archive & help yourself
http://www.iaa.csic.es/AMIGA.html