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Diapositiva 1J. Sabater (Post-gr)
E. García (Software)
Direct collaborators:
W. Huchtmeier (Max Planck IfR, Bonn)
S. Odewahn (Arizona State University)
M. S. Yun (UMass)
J. Sabater (Post-gr)
E. García (Software)
M. Rosado (UNAM)
M. Gutiérrez-Valdez (Univ. Guanajuato)
J. Sabater (Post-gr)
E. García (Software)
M. Rosado (UNAM)
M. Gutiérrez-Valdez (Univ. Guanajuato)
See Posters:
AMIGA:Quantifying the environment of the most isolated galaxies. Verley et al.
AMIGA: Properties of the HI in Galaxies as a function of isolation. Espada et al.
Crete, August 2004
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).
Crete, August 2004
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 sample
Crete, August 2004
“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)
Crete, August 2004
“NORMAL” galaxias (e.g. Boselli et al ´01)
Galaxies with no redshift data are not considered companions
(Kelm & Focardi ´04: isolated and companion limited at 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)
BUT we usually find, either
monochromatic observations of LARGE SAMPLES
Crete, August 2004
“NORMAL” galaxias (e.g. Boselli et al ´01)
Galaxies with no redshift data are not considered companions
(Kelm & Focardi ´04: isolated and companion limited at 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)
BUT we usually find, either
monochromatic observations of LARGE SAMPLES
or
Selected from CGCG (Zwicky et al 1960-1968) with
mpg < 15.7 > -30
- 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
Crete, August 2004
BY THE WAY...
CIG: 1050 galaxies
LB, LFIR
Haynes & Giovanelli ´84
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.
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.
Crete, August 2004
Isolation
Morhologies
Reference sample, among others, for radiocont., HI, CO and FIR
(Adams et al 1980, Haynes & Giovanelli 1980 and ss, Young et al 1986, Xu and Sulentic 1991, Hernández-Toledo et al 1999)
2. MULTIWAVELENGTH STUDY
Crete, August 2004
Karachentseva (1986) revised using codes from Adams
0 isolated (n = 903)
2 definitely not isolated (n=64)
Our revision (n= 100 with v < 1500 km/s excluded):
POSS-I & II to evaluate a minimum physical
distance of 0.5 Mpc, up to B = 17.5 mag (CGCG 15.7)
Reduced with AIMTOOL in LMORPHO (Odewahn ´95, ´96) Star/galaxy separation
Catalog of all potential companions
Reference sample, among others, for radiocont., HI, CO and FIR
(Adams et al 1980, Haynes & Giovanelli 1980 and ss, Young et al 1986, Xu and Sulentic 1991, Hernández-Toledo et al 1999)
Crete, August 2004
Our revision (n = 100 with v < 1500 km/s excluded):
POSS-I & II to evaluate a minimum physical
distance 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
Reference sample, among others, for radiocont., HI, CO and FIR
(Adams et al 1980, Haynes & Giovanelli 1980 and ss, Young et al 1986, Xu and Sulentic 1991, Hernández-Toledo et al 1999)
Crete, August 2004
Q: estimation of the gravitational interaction strength.
Also calculated for Hickson Compact Groups
Final steps:
- bias minimization (distance, size).
Crete, August 2004
Crete, August 2004
Crete, August 2004
Crete, August 2004
Crete, August 2004
Crete, August 2004
Crete, August 2004
MORPHOLOGIES: Bibliography non-uniform data
Contradictory NED vs LEDA
Crete, August 2004
Reference sample, among others, for radiocont., HI, CO and FIR
(Adams et al 1980, Haynes & Giovanelli 1980 and ss, Young et al 1986, Xu and Sulentic 1991, Hernández-Toledo et al 1999)
Crete, August 2004
LEDA
Ours
MORPHOLOGIES
Crete, August 2004
LEDA
Ours
MORPHOLOGIES
Early types:
LEDA
Ours
Reference sample, among others, for radiocont., HI, CO and FIR
(Adams et al 1980, Haynes & Giovanelli 1980 and ss, Young et al 1986, Xu and Sulentic 1991, Hernández-Toledo et al 1999)
aqui va histograma de tipos y los de HCGs
Our types
LEDA types
1/2 from ned
1/2 from 41 different sources + 10 galaxies from our HI.
Distances:
Crete, August 2004
REDSHIFT AND DISTANCES
Archival + bibliography: 956/1050
1/2 from ned
1/2 from 41 different sources + 10 galaxies from our HI.
Distances:
New CIG with z added to v > 5000 km/s
Our CIG with z
CIG XS91 with z
1/2 from ned
1/2 from 41 different sources + 10 galaxies from our HI.
Distances:
New CIG with z added to v > 5000 km/s
CIG: all 1051 galaxies
AIG: 280 CIGs from Arecibo sample,
Haynes & Giovanelli ´84
Crete, August 2004
REDSHIFT AND DISTANCES
Archival + bibliography: 956/1050
1/2 from ned
1/2 from 41 different sources + 10 galaxies from our HI.
Distances:
New CIG with z added to v > 5000 km/s
Our CIG with z
CIG XS91 with z
Revised for full CIG:
and visually revised.
Reference sample, among others, for radiocont., HI, CO and FIR
(Adams et al 1980, Haynes & Giovanelli 1980 and ss, Young et al 1986, Xu and Sulentic 1991, Hernández-Toledo et al 1999)
2. MULTIWAVELENGTH STUDY
Little correspondence with nearby cluster cores
Some correspondence with LS struct. (Haynes & G 83)
Autocorrelation function: weak clustering (Vettolani et al 1986)
Crete, August 2004
Optical: spatial homogeneity
Little correspondence with nearby cluster cores
Some correspondence with LS struct. (Haynes & G 83)
Autocorrelation function: weak clustering (Vettolani et al 1986)
Crete, August 2004
Optical: spatial homogeneity
Little correspondence with nearby cluster cores
Some correspondence with LS struct. (Haynes & G 83)
Autocorrelation function: weak clustering (Vettolani et al 1986)
Crete, August 2004
Optical: spatial homogeneity
Little correspondence with nearby cluster cores
Some correspondence with LS struct. (Haynes & G 83)
Autocorrelation function: weak clustering (Vettolani et al 1986)
Crete, August 2004
Optical: velocity homogeneity
Comparison with homogeneus distribution with same size and redshift distribution and Schecter OLF.
Crete, August 2004
Optical: velocity homogeneity
Scaled homogeneus distribution: fits 2/3 of CIG, rest follows Local and Pisces-Perseus
Crete, August 2004
Optical: homogeneity
The CIG is likely as close as we can hope to come to a local homogeneus component of the galaxy distribution
HCGs and CIGs share a similar avoidance of the most clustered regions.
Crete, August 2004
515 have also BT0
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)
Crete, August 2004
Residuals
n =19 brighter than mapp = 11 mag:
few large and bright galaxies in the nearby Universe that escaped deletion by K73
Our CIG with z
CIG XS91 with z
Optical: completeness
V/Vm test
CIG complete at 80-95% level up to m = 15 <V/Vm> = 0.42
Completeness correction 1.9
n= 692 galaxies with
Our CIG
CIG XS91
Local dwarfs excl. α = -1.04 ± 0.09 M* = -20.15 ± 0.07
ALL 1051 CIG
Local dwarfs excl. α = -0.84 ± 0.09 M* = -20.07 ± 0.07
log φ
CIG sample
mZw-uncorr
BTo
Sample

α
M*
-0.9 to -1.25
-0.9 to -1.25
Mabs
HCGs spirals
HCGs spirals shifted upwards
HCGs spirals shifted upwards
1.4e-4 ± 0.6e-4
-1.17 ± 0.24
-19.83 ± 0.31
1.4e-4 ± 0.6e-4
-1.17 ± 0.24
-19.83 ± 0.31
Only PSC-IRAS existed for 303 galaxies
Improves snr by factor 3-5.
Radio continuum: archive data re-processing
WENNSS 92cm (Westerbork Northern Sky Survey)
GB6 6 cm (Green Bank)
NVSS 20 cm (NRAO VLA Sky Survey)
Crete, August 2004
Work in parallel
Atomic gas study:
VLA HI data for 20 asymmetric + isolated
Molecular gas study:
Ionized gas study:
Crete, August 2004
Work in parallel
Atomic gas study:
VLA HI data for 20 asymmetric + isolated
Molecular gas study:
Ionized gas study:
with some ISOLATED E’s with ISM +S0’s
Crete, August 2004
Work in parallel
Atomic gas study:
VLA HI data for 20 asymmetric + isolated
Molecular gas study:
Ionized gas study:
Crete, August 2004
http://www.iaa.csic.es/AMIGA.html
like good wine…
Trabajo previo:
Mejora:
cantidad:
calidad:
repetición de observaciones mejorables
Crete, August 2004
Def(HI) = 0.26 + 0.05
falta 45% HI
Análisis
Crete, August 2004
<Def(HI)> = 0.16 + 0.10
Grupos VLA
Def(HI) = 0.97
HCG 92b Def(HI) > 2.15
Crete, August 2004
Gas atómico (HI)
Trabajo previo:
50-75% de perfiles asimétricos
entornos más densos: % similares
Swaters et al (2002), Richter & Sancisi (1994), Sulentic & Arp (1983)
Resultado sorprendente, ¿aislamiento?
Crete, August 2004
Gas atómico (HI)
Objetivo: origen de asimetrías en galaxias aisladas
intrínsecas/inducidas por compañeras pequeñas
F1
F2
vm
V
F
F1
F2
a =
Resultado provisional:
en muchos casos también FIR (SF)
Origen standard:
minor/major merger (Morganti et al. 1997; Balcells etal. 2001)
De nuevo sorprendente:
¿representan Es primordiales?
Crete, August 2004
Green Bank (72) Arecibo (34)
Nancay (80+X)
Coadición de scans IRAS para la muestra completa
FRESCO: procesado IRAS para fuentes extensas.
(Verdes-M. et al. in prep)
NVSS 20 cm (NRAO VLA Sky Survey), res 50”
mejorando la snr de los archivos:
322 detecciones
(A. Ballu & J. Sabater)