Crete, August 2004. Started October 2002 Crete, August 2004.

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Crete, August 2004

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Crete, August 2004

Started October 2002Started October 2002

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Crete, August 2004

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Crete, August 2004

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Core team IAA:

S. Leon, U. Lisenfeld, (Post-docs)

D. Espada, S. Verley (PhD)

J. Sabater (Post-gr)

E. García (Software)

Next fall: + 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)

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Core team IAA:

S. Leon, U. Lisenfeld, (Post-docs)

D. Espada, S. Verley (PhD)

J. Sabater (Post-gr)

E. García (Software)

Next fall: + G. Bergond (Post-doc)

F. Combes (Obs. Paris –LERMA)

M. Rosado (UNAM)

A. Bosma, L. Athanassoula (Obs. Marseille)

M. Gutiérrez-Valdez (Univ. Guanajuato)

I. Puerari (INAOE)

A. Ballu (ENSP Strasbourg)

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MOTIVATION Direct interaction-enhancement connection difficult to establish:

Amplitude of the effects and processes not well quantified/understood.

E.g groups vs pairs:

HCGs: Evidence for morphology changes and HI depletion, excess SF not observed

(e.g. VM et al ´01, Iglesias-Páramo & Vílchez ´99)

Pairs: SF excess but no HI deficit

(Xu & Sulentic ´91, Zasov & Sulentic ´94)

E.g. AGN activity frequence

(e.g De Robertis et al ´98, Krongold et al ´03).

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MOTIVATION Direct interaction-enhancement connection difficult to establish:

Amplitude of the effects and processes not well quantified/understood.

E.g groups vs pairs:

HCGs: Evidence for morphology changes and HI depletion, excess SF not observed

(e.g. VM et al 2001, Iglesias-Páramo &Vílchez 1999)

Pairs: SF excess but no HI deficit

(Xu & Sulentic 1991, Zasov & Sulentic 1994)

E.g. AGN activity frequence (e.g De Robertis et al 1998, Krongold et al 2003).

Reflect the lack of a

suitable control samplesuitable control sample

against which properties of

interacting samples can be compared

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SAMPLES OF ISOLATED GALAXIES

Selection:

FIELD galaxies (e.g. Kennicut & Kent ´83)

“NORMAL” galaxias (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:

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)

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Selection:



Galaxies with no redshift data are not considered companions (Kelm & Focardi ´04: isolated and companion limited at

15.5mag)

Number:

10 – 100/200 members


BUT we usually find, either

monochromatic observations of LARGE SAMPLES

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Selection:



Galaxies with no redshift data are not considered companions (Kelm & Focardi ´04: isolated and companion limited at

15.5mag)

Number:

10 – 100/200 members


BUT we usually find, either

monochromatic observations of LARGE SAMPLES

or small samples

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BY THE WAY...BY THE WAY...© Karachensetva 1973© Karachensetva 1973

CIGCIG:: CCatalogueatalogue ofof IIsolated solated GGalaxiesalaxiesSelected from CGCG (Zwicky et al 1960-1968) with

mpg < 15.7 > -30

Strength:

- Size: 1050 galaxies

- Isolation: no similar sized galaxies (factor 4)

within 40*R(companion) -> last interaction

several Gyrs ago

- Morphology: permits discrimination based on

types.

- Depth: large volume to allow sampling of the

OLF.

- Completeness: 80-90% up to mZw(corr) = 15.0

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BY THE WAY...BY THE WAY...© Karachensetva 1973© Karachensetva 1973

CIGCIG:: CCatalogueatalogue ofof IIsolated solated GGalaxiesalaxies

CIG: 1050 galaxies

XS91: 476 CIGs from Xu & Sulentic ´91

LB, LFIR

AIG: 280 CIGs from Arecibo sample,

Haynes & Giovanelli ´84

LB, HI

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OUR SAMPLE: CIG basedOUR SAMPLE: CIG basedMajor interactions are excluded

Hierarchical pairs and groups are kept AND quantifiedquantified:

•Do truly isolated galaxies exist?

•In what numbers?

•Environmental level where the onset of

interaction induced activity can be first

detected. Optical (B) and NIR luminosity.

Atomic gas.

Radiocontinuum & FIR emission.

CO & Halfa emission.

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OUR SAMPLE: CIG basedOUR SAMPLE: CIG basedMajor interactions are excluded

Hierarchical pairs and groups are kept AND quantifiedquantified:

•Do truly isolated galaxies exist?

•In what numbers?

•Environmental level where the onset of

interaction induced activity can be first

detected. Optical (B) and NIR luminosity.

Atomic gas.

Radiocontinuum & FIR emission.

CO & Halfa emission.

A large sample for a multiwavelength

characterization of the low density tail of

the 2p correlation function.

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PUBLIC DATAPUBLIC DATA

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COMING SOON:COMING SOON: INTEGRATION IN VO StandardsINTEGRATION IN VO Standards

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1. REFINEMENT OF THE SAMPLE1. REFINEMENT OF THE SAMPLE

Isolation

Morhologies

Redshift and distances

Positions

2. MULTIWAVELENGTH STUDY2. MULTIWAVELENGTH STUDY

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ISOLATION ISOLATION (PhD S. Verley, SEE POSTER)

• Our revision (n = 100 with v < 1500 km/s excluded):

POSS-I & II to evaluate a minimum physicaldistance of 0.5 Mpc, up to B = 17.5 mag

Reduced with AIMTOOL in LMORPHO (Odewahn ´95, ´96) Star/galaxy separation

Catalog of all potential companions

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Isolation parameters:

Karachentseva re-evaluated

Tidal force parameter (Dahari 1984)

Q: estimation of the gravitational interaction strength.

Also calculated for Hickson Compact Groups

Final steps: - background galaxies rejection (several

methods being tested).- bias minimization (distance, size).

(PhD S. Verley, SEE POSTER)

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Ver de donde saleIsolation parameters:



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MORPHOLOGIES: MORPHOLOGIES: Bibliography non-uniform Bibliography non-uniform data data Contradictory NED vs LEDA

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E S0 Sa Sb Sc Sd Im

E

S

0

Sa

S

b

Sc

Sd

ImMORPHOLOGIES: MORPHOLOGIES: Bibliography non-uniform Bibliography non-uniform data data Contradictory NED vs LEDA

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E S0 Sa Sb Sc Sd Im

E

S0

Sa

Sb

Sc

Sd

Im

LEDA

Ours

MORPHOLOGIESMORPHOLOGIES

POSSII + CCD based revision POSSII + CCD based revision (Sulentic et al in (Sulentic et al in

prep)prep)

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E S0 Sa Sb Sc Sd Im

E

S0

Sa

Sb

Sc

Sd

Im

LEDA

Ours

MORPHOLOGIESMORPHOLOGIES

POSSII + CCD based revision POSSII + CCD based revision (Sulentic et al in (Sulentic et al in

prep)prep)

Early types:

CIG: 16% (Sc dominate)

HCGs: 55%

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REDSHIFT AND DISTANCESREDSHIFT AND DISTANCES

Archival + bibliography: 956/1050 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.

Distances:Distances:v > 1000 km/s redshift basedv > 1000 km/s redshift basedv < 1000 km/s bibliographical searchv < 1000 km/s bibliographical search

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POSITIONSPOSITIONS (Leon & Verdes-Montenegro A&A 2003)

Revised for full CIG:

SExtracted (Bertin & Arnouts 1996) from DSS

and visually revised.

Max 44.5”

Mean 1.8”

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1. REFINEMENT OF THE SAMPLE1. REFINEMENT OF THE SAMPLE

2. MULTIWAVELENGTH STUDY2. MULTIWAVELENGTH STUDY

Optical characterization:

Completeness

OLF: CIG & HCGs

Work in parallel

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Optical: completenessOptical: completenessBlue magnitudes:

All CIG members have mZw magnitudes

515 have also BT0

We have corrected mZw from:• systematic errors in the CGCG Volume I (Kron & Shane

´75)

• galactic dust extinction (IRAS/DIRBE Schlegel ´98)

• internal extinction (i and morphology following RC3)

• K corrections (Pence ´76, Giovanelli ´81)

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Optical: completenessOptical: completenessBlue magnitudes:mZw(corr)=BT0-0.04 (±0.19)

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Optical: completenessOptical: completenessV/Vm test

CIG complete at 80-95% level up to m = 15 <V/Vm>

= 0.42

Completeness correction 1.9

V/V

m

Limiting magnitude

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Optical: completenessOptical: completenessV/Vm test

V/V

m

Limiting magnitude

Completeness with respect to CIG subsamples

(XS91) significantly improved (before below 80%).

OUR FINAL SAMPLE FOR OLF CALCULATION:

n= 692 galaxies with

known distance

11 – 15 mag

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Optical: OLFOptical: OLF

CIG sample α = -1.27 ± 0.06 M* = -20.31 ± 0.07

Local dwarfs excl. α = -1.04 ± 0.09 M* = -20.15 ± 0.07

ALL 1051 CIG

v < 1500 km/s CIG

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log φ

CIG sample

Local dwarfs excl.

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Sample Ф α M*

CIG n = 692 6.3e-4 ± 0.7e-4 -1.27 ± 0.06

-20.31 ± 0.07

CIG Local dw excl. 7.9e-4 ± 0.7e-4 -0.84± 0.09 -20.07 ± 0.07

AIG (XS91) n = 280 4.7e-4 -1.4 -19.5

CIG (XS91) n = 476 10.3e-4 -1.4 -19.6

BTo

mZ

w-

unco

rr

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Sample Ф α M*

CIG n = 692 6.3e-4 ± 0.7e-4 -1.27 ± 0.06

-20.31 ± 0.07

CIG Local dw excl. 7.9e-4 ± 0.7e-4 -0.84± 0.09 -20.07 ± 0.07

AIG (XS91) n = 280 4.7e-4 -1.4 -19.5

CIG (XS91) n = 476 10.3e-4 -1.4 -19.6

Reproduced when mZw uncorrected are used

mZ

w-

unco

rrB

To

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Sample Ф α M*

CIG n = 692 6.3e-4 ± 0.7e-4

-1.27 ± 0.06

-20.31 ± 0.07

CIG Local dw excl. 7.9e-4 ± 0.7e-4

-0.84± 0.09 -20.07 ± 0.07

AIG (XS91) n = 280 4.7e-4 -1.4 -19.5

CIG (XS91) n = 476 10.3e-4 -1.4 -19.6

Field galaxies, Binggeli et al

-0.9 to -1.25

-19.86

Felten: BTo = BT -0.25

-19.86 -20.11

mZ

w-

unco

rrB

TB

To

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OLF: CIG & HCGsOLF: CIG & HCGs

Mabs

CIG

CIG, v < 1500 excl.

HCGs shifted upwards

Slight enhancementlo

g φ

(M

pc-

3 M

ag

-

1

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OLF: CIG & HCGs: Early typesOLF: CIG & HCGs: Early types

Mabs

E’s CIG

E+S0’s HCGs

E+S0’s CIG

log φ

Clear enhancement

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OLF: CIG & HCGs: SpiralsOLF: CIG & HCGs: Spirals

Mabs

log φ

CIG spirals

CIG spirals, v < 1500 excl.

HCGs spirals shifted upwards

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OLF: CIGs & HCGs, OLF: CIGs & HCGs, morphologiesmorphologiesSample φ α M*

CIG E’s + S0’s 1.4e-4 ± 0.6e-4

-1.17 ± 0.24

-19.83 ± 0.31

HCGs 3.0e-6 ± 1.3e-6

-1.85± 0.16 -20.94 ± 0.22

CIG, spirals (Sa –Sd) 5.8e-4 ± 0.6e-4

-1.02 ± 0.08

-20.22 ± 0.08

HCGs 6.7e-6 ± 2.4e-6

-1.33± 0.25 -20.32 ± 0.22

CIG, Sa - Im 5.1e-4 ± 0.6e-4

-1.28 ± 0.07

-20.34 ± 0.08

HCGs 7.3e-6 ± 2.7e-6

-1.44± 0.23 -20.33 ± 0.21

CIG, Sm - Im 1.2e-5 ± 1.0e-5

-2.23 ± 0.15

-20.82 ± 0.38

Equivalent mag systems

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Work in parallelWork in parallel

FIR: 4 IRAS bands coadded from archive data

Only PSC-IRAS existed for 303 galaxies

Improves snr by factor 3-5.

Radio continuum: archive data re-processingWENNSS 92cm (Westerbork Northern Sky Survey)GB6 6 cm (Green Bank) NVSS 20 cm (NRAO VLA Sky Survey)

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Atomic gas study:

HI single dish for nearly 800 CIG members.

VLA HI data for 20 asymmetric + isolated

Molecular gas study:

CO single dish for 200 galaxies

Ionized gas study:

Halfa images for 200 galaxies

Local HaLF + HII distribution characterization

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Atomic gas study:





Ionized gas study:



PhD D. Espada. SEE POSTER

with some ISOLATED E’s with ISM +S0’s

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Atomic gas study:





Ionized gas study:



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SUMMARY:

AMIGOS!!!!

Visit AMIGA archive & help yourself

http://www.iaa.csic.es/AMIGA.html

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Wait some months and data will become better…

like good wine…

HICO

http://www.iaa.csic.es/AMIGA.html

Crete, August 2004. Started October 2002 Crete, August 2004.

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