Crete, August 2004

Started October 2002

Crete, August 2004

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)

Crete, August 2004 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)

Crete, August 2004 IAA: S. Leon, U. Lisenfeld (Post-docs) D. Espada, S. Verley (PhD) J. Sabater (Post-gr) E. García (Software) 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) Crete, August 2004 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 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).

Crete, August 2004 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 sample against which properties of interacting samples can be compared

Crete, August 2004 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)

Crete, August 2004 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 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 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 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 small samples

Crete, August 2004 BY THE WAY... © Karachensetva 1973 CIG: Catalogue of Isolated Galaxies Selected from CGCG (Zwicky et al ) with mpg -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

Crete, August 2004 BY THE WAY... © Karachensetva 1973 CIG: Catalogue of Isolated Galaxies CIG: 1050 galaxies XS91: 476 CIGs from Xu & Sulentic ´91 LB, LFIR AIG: 280 CIGs from Arecibo sample, Haynes & Giovanelli ´84 LB, HI

Crete, August 2004 OUR SAMPLE: CIG based Major interactions are excluded quantified Hierarchical pairs and groups are kept AND quantified: 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.

Crete, August 2004 OUR SAMPLE: CIG based Major interactions are excluded quantified Hierarchical pairs and groups are kept AND quantified: 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 PUBLIC DATA

Crete, August 2004 COMING SOON: INTEGRATION IN VO Standards

Crete, August REFINEMENT OF THE SAMPLE Isolation Morhologies Redshift and distances Positions 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 ISOLATION ISOLATION (PhD S. Verley, SEE POSTER) Karachentseva (1986) revised using codes from Adams 0 isolated (n = 903) 1 marginally isolated (n=84) 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 ISOLATION ISOLATION (PhD S. Verley, SEE POSTER) 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 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)

Crete, August 2004 Ver de donde sale Isolation parameters: Karachentseva re-evaluated Tidal force parameter (Dahari 1984)

Crete, August 2004 Ver de donde sale Isolation parameters: Karachentseva re-evaluated Tidal force parameter (Dahari 1984)

Crete, August 2004 Ver de donde sale Isolation parameters: Karachentseva re-evaluated Tidal force parameter (Dahari 1984)

Crete, August 2004 Ver de donde sale Isolation parameters: Karachentseva re-evaluated Tidal force parameter (Dahari 1984)

Crete, August 2004 Ver de donde sale Isolation parameters: Karachentseva re-evaluated Tidal force parameter (Dahari 1984)

Crete, August 2004 Ver de donde sale Isolation parameters: Karachentseva re-evaluated Tidal force parameter (Dahari 1984)

Crete, August 2004 MORPHOLOGIES: Bibliography non-uniform data Contradictory NED vs LEDA

Crete, August 2004 E S0 Sa Sb Sc Sd Im MORPHOLOGIES: Bibliography non-uniform data Contradictory NED vs LEDA

Crete, August 2004 LEDA:Scd NED: Sa E S0 Sa Sb Sc Sd Im

Crete, August 2004 MORPHOLOGIES POSSII + CCD based revision (Sulentic et al in prep) 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 E S0 Sa Sb Sc Sd Im LEDA Ours MORPHOLOGIES POSSII + CCD based revision (Sulentic et al in prep)

Crete, August 2004 E S0 Sa Sb Sc Sd Im LEDA Ours MORPHOLOGIES POSSII + CCD based revision (Sulentic et al in prep) Early types: CIG: 16% (Sc dominate) HCGs: 55%

Crete, August 2004 LEDA:Scd NED: Sa Ours: Sc E S0 Sa Sb Sc Sd Im LEDA Ours

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) aqui va histograma de tipos y los de HCGs Our types LEDA types

Crete, August 2004 REDSHIFT AND DISTANCES Archival + bibliography: 956/ more than in previous publications. 1/2 from ned 1/2 from 41 different sources + 10 galaxies from our HI.Distances: v > 1000 km/s redshift based v < 1000 km/s bibliographical search

Crete, August 2004 REDSHIFT AND DISTANCES Archival + bibliography: 956/ more than in previous publications. 1/2 from ned 1/2 from 41 different sources + 10 galaxies from our HI.Distances: v > 1000 km/s redshift based v < 1000 km/s bibliographical search New CIG with z added to v > 5000 km/s Our CIG with z CIG XS91 with z AIG with z

Crete, August 2004 REDSHIFT AND DISTANCES Archival + bibliography: 956/ more than in previous publications. 1/2 from ned 1/2 from 41 different sources + 10 galaxies from our HI.Distances: v > 1000 km/s redshift based v < 1000 km/s bibliographical search New CIG with z added to v > 5000 km/s CIG: all 1051 galaxies XS91: 476 CIGs from Xu & Sulentic ´91 AIG: 280 CIGs from Arecibo sample, Haynes & Giovanelli ´84

Crete, August 2004 REDSHIFT AND DISTANCES Archival + bibliography: 956/ more than in previous publications. 1/2 from ned 1/2 from 41 different sources + 10 galaxies from our HI.Distances: v > 1000 km/s redshift based v < 1000 km/s bibliographical search New CIG with z added to v > 5000 km/s Our CIG with z CIG XS91 with z AIG with z

Crete, August 2004 POSITIONS POSITIONS (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”

Crete, August REFINEMENT OF THE SAMPLE 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 Optical characterization: Completeness OLF: CIG & HCGs Work in parallel

Crete, August 2004 Optical: spatial homogeneity Distribution on the sky 0 – 3000 km/s 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 Distribution on the sky 3000 – 6000 km/s 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 Distribution on the sky 6000 – 9000 km/s 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 Distribution on the sky 9000 – km/s 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 Optical: completeness Blue magnitudes: All CIG members have mZw magnitudes 515 have also BT 0 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)

Crete, August 2004 Optical: completeness Blue magnitudes: mZw(corr)=BT (±0.19)

Crete, August 2004 Optical: completeness Blue magnitudes: mZw(corr)=BT (±0.19) Residuals

Crete, August 2004 Optical: completeness Apparent magnitude distribution 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 AIG with z

Crete, August 2004 Optical: completeness V/Vm test CIG complete at 80-95% level up to m = 15 = 0.42 Completeness correction 1.9 V/Vm Limiting magnitude

Crete, August 2004 Optical: completeness V/Vm test V/Vm 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

Crete, August 2004 Optical: completeness V/Vm test Completeness with respect to Xu & Sulentic 1991 significantly improved. Our CIG CIG XS91 V/Vm Limiting magnitude

Crete, August 2004 Optical: absolute magnitudes Our CIG with z CIG XS91 with z AIG with z

Crete, August 2004 Optical: OLF CIG sample α = ± 0.06 M* = ± 0.07 Local dwarfs excl. α = ± 0.09 M* = ± 0.07 ALL 1051 CIG v < 1500 km/s CIG

Crete, August 2004 Optical: OLF CIG sample α = ± 0.06 M* = ± 0.07 Local dwarfs excl. α = ± 0.09 M* = ± 0.07 log φ CIG sample Local dwarfs excl.

Crete, August 2004 Optical: OLF Sample Фα M* CIG n = e-4 ± 0.7e ± ± 0.07 CIG Local dw excl. 7.9e-4 ± 0.7e ± ± 0.07 AIG (XS91) n = e CIG (XS91) n = e BTo mZw-uncorr

Crete, August 2004 Optical: OLF Sample Фα M* CIG n = e-4 ± 0.7e ± ± 0.07 CIG Local dw excl. 7.9e-4 ± 0.7e ± ± 0.07 AIG (XS91) n = e CIG (XS91) n = e Reproduced when mZw uncorrected are used mZw-uncorr BTo

Crete, August 2004

Optical: OLF Sample Фα M* CIG n = e-4 ± 0.7e ± ± 0.07 CIG Local dw excl. 7.9e-4 ± 0.7e ± ± 0.07 AIG (XS91) n = e CIG (XS91) n = e Field galaxies, Binggeli et al -0.9 to mZw-uncorr BTBT BTo

Crete, August 2004 Optical: OLF Sample Фα M* CIG n = e-4 ± 0.7e ± ± 0.07 CIG Local dw excl. 7.9e-4 ± 0.7e ± ± 0.07 AIG (XS91) n = e CIG (XS91) n = e Field galaxies, Binggeli et al -0.9 to Felten: B T o = B T  mZw-uncorr BTBT BTo

Crete, August 2004 OLF: CIGs & HCGs CIGs HCGs Mabs

Crete, August 2004 OLF: CIG & HCGs Mabs CIG CIG, v < 1500 excl. HCGs log φ (Mpc -3 Mag -1

Crete, August 2004 OLF: CIG & HCGs Mabs CIG CIG, v < 1500 excl. HCGs shifted upwards Slight enhancement log φ (Mpc -3 Mag -1

Crete, August 2004 OLF: CIG & HCGs: Early types Mabs E’s CIG E+S0’s HCGs E+S0’s CIG log φ Clear enhancement

Crete, August 2004 OLF: CIG & HCGs: Spirals Mabs log φ CIG spirals CIG spirals, v < 1500 excl. HCGs spirals

Crete, August 2004 OLF: CIG & HCGs: Spirals Mabs log φ CIG spirals CIG spirals, v < 1500 excl. HCGs spirals shifted upwards

Crete, August 2004 OLF: CIG & HCGs: Spirals Mabs log φ CIG spirals CIG spirals, v < 1500 excl. HCGs spirals shifted upwards

Crete, August 2004 OLF: CIGs late types CIG Mabs log φ CIG Sdm - Im

Crete, August 2004 OLF: CIGs & HCGs Sample Фα M* CIG n = e-4 ± 0.7e ± ± 0.07 CIG Local dw excl. 7.9e-4 ± 0.7e ± ± 0.07 HCGs (SR94) M< e-6 ± 2.7e ± ± 0.15 HCGs (SR94) All 1.8e-5 ± 0.3e ± ± 0.11 mZw-corr BTo

Crete, August 2004 OLF: CIGs & HCGs, morphologies Sample Фα M* CIG E’s 3.4e-5 ± 6.3e ± ± 1.43 HCGs 1.8e-6 ± 0.8e ± ± 0.25 CIG E’s + S0’s 1.4e-4 ± 0.6e ± ± 0.31 HCGs 3.0e-6 ± 1.3e ± ± 0.22 CIG, spirals (Sa –Sd) 5.8e-4 ± 0.6e ± ± 0.08 HCGs 6.7e-6 ± 2.4e ± ± 0.22 CIG, Sa - Im 5.1e-4 ± 0.6e ± ± 0.08 HCGs 7.3e-6 ± 2.7e ± ± 0.21 CIG, Sm - Im 1.2e-5 ± 1.0e ± ± 0.38 Equivalent mag systems

Crete, August 2004 OLF: CIGs & HCGs, morphologies Sample φα M* CIG E’s + S0’s 1.4e-4 ± 0.6e ± ± 0.31 HCGs 3.0e-6 ± 1.3e ± ± 0.22 CIG, spirals (Sa –Sd) 5.8e-4 ± 0.6e ± ± 0.08 HCGs 6.7e-6 ± 2.4e ± ± 0.22 CIG, Sa - Im 5.1e-4 ± 0.6e ± ± 0.08 HCGs 7.3e-6 ± 2.7e ± ± 0.21 CIG, Sm - Im 1.2e-5 ± 1.0e ± ± 0.38 Equivalent mag systems

Crete, August 2004

Work 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-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: 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

Crete, August 2004 Work in parallel 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 PhD D. Espada. SEE POSTER with some ISOLATED E’s with ISM +S0’s

Crete, August 2004 Work in parallel 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

Crete, August 2004 SUMMARY: AMIGOS!!!! Visit AMIGA archive & help yourself

Crete, August 2004 Wait some months and data will become better… like good wine… HI CO

Crete, August 2004

Atomic gas (HI) Atomic gas (HI) (PhD D. Espada. SEE POSTER) Goal 1: Referencia for M(HI) = f(LB, Ø, t) Trabajo previo: Survey de Haynes & Giovanelli (1984) para n=324 gal. Mejora: cantidad: duplicar la muestra (menor dispersión submuestras) calidad: compilación bibliográfica exhaustiva selección de los mejores espectros (tamaño/haz) repetición de observaciones mejorables (Espada et al. in prep)

Crete, August 2004 M(HI) obs - M(HI) pred. grupos Def(HI) = falta 45% HI Revisión de contenido de HI en entornos densos Análisis single dish 72 GCs VLA para 16 GCs Verdes-M. et al A&A (2001)

Crete, August 2004 = falta 31% de HI Def(HI) = 0.97 falta 89% HI Revisión de contenido de HI en entornos densos Grupos VLA M(HI) obs - M(HI) pred. grupos VLA

Crete, August 2004 GALAXIAS INDIVIDUALES Def(HI) = falta 76% HI Extracción (stripping) eficiente del gas (mapas VLA) HCG 92b Def(HI) > 2.15 falta 99% HI

Crete, August 2004 ¿? Perturbación mínimaGas en colas Galaxias sin gas Gas en una nube Deficiencia extrema

Crete, August 2004 Comparación con otros entornos Huchtmeier & Richter 1989 Garcia-Barreto et al 1994 Bravo-Alfaro et al 2000

Crete, August 2004 Optical: OLF CIG sample α = ± 0.06 M* = ± 0.07

Crete, August 2004 Gas atómico (HI) Goal 2: Symmetry of the spectra Trabajo previo: aisladas: n=104 (Haynes et al 1998) n=30 (Matthews et al 1998) 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 2b: Mapas de galaxias aisladas Estudio VLA (propuesta para próximo deadline): Muestra: asimétricas óptico Y espectro HI Objetivo: origen de asimetrías en galaxias aisladas intrínsecas/inducidas por compañeras pequeñas nivel cero para definición de perturbación F1F1 F2F2 vmvm V F F1F1 F2F2 a =

Crete, August 2004 Gas atómico (HI) Goal 3: Gas in isolated early types Resultado provisional: tasa de detección del 40%, en muchos casos también FIR (SF) Origen standard: acreción de compañeras (cf. Huchtmeier, 1994) minor/major merger (Morganti et al. 1997; Balcells etal. 2001) De nuevo sorprendente: ¿son tipos tempranos?, y si lo son ¿representan Es primordiales?

Crete, August 2004 Status gas atómico (HI) Bibliografía revisión y selección completa: 407 CIGs Observaciones propias: hasta el 90% restante Green Bank (72) Arecibo (34) Nancay (80+X) Effelsberg (157)

Crete, August 2004 FIR y radiocontinuo Procesado de datos de archivo PSC-IRAS existentes para 303 galaxias 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 FIR Radio (Leon et al. in prep) (A. Ballu & J. Sabater)