Text of Crete, August 2004. Started October 2002 Crete, August 2004
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)