Seyfert’s Sextet(HCG79): Timing the Disruption of Galaxies and the Formation of the Intragroup Medium Omar López-Cruz, Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE) (omarlx@inaoep.mx) Marina Rodríguez-Baras, F. Fabián Rosales-Ortega, Jorge K. Barrera-Ballesteros, Jesús Falcón Barroso, Sebastián F. Sánchez, Héctor J. Ibarra-Medel, Christopher Añorve & The CALIFA Collaboration

Index Why are compact groups important? Dynamics & Sizes Is CALIFA the Right Data Set? Galaxies Stars,Hot Gas, Cold Gas, Dust Environment A new view of SS with CALIFA

All star forming disk galaxies w. M* ≥ 1010 Mo Evolution of gas fraction: epoch of peak cosmic SF rate density (z~2) = epoch of gas-dominated disks (1+z)2 All star forming disk galaxies w. M* ≥ 1010 Mo All points assume α~ 4 => empirical ratio ~ L’CO/R Platen et al. 2011

My God, it’s full of stars… Ibarra-Medel & López-Cruz (2015) in preparation.

Collapsing Overdensities: Simple Theoretical Considerations r2t Radius Velocity r2t Time Spherical infall of cold,collisionless particles: - object at first turnaround today at t0 (radius r1t) will fully collapse by 2t0 object at second turnaround today (radius r2t) was at first turnaround at 0.37 t0 Bertschinger, E. 1985, ApJS, 58, 39 Radius

Can we measure the turn-around radii? Tully (2014)

Hickson (1982, 1993, 1994) adopted a relative magnitude criterion, selecting systems of four or more galaxies whose magnitudes differ by less than 3.0. A distance independent (to first order) compactness criterion was employed: < 26, where is the mean surface brightness of the group calculated by distributing the flux of the member galaxies over the smallest circular area containing their geometric centers

Is CALIFA the right data set to study HGC? It is just right!!! Contains galaxies from almost all environments and conditions. Sánchez et al, 2012, Husemann et al, 2013

b f c e a d

Durbala et al. 2008

STARLIGHT (Cid-Fernandes et al, 2005) SSP from Bruzual & Charlot, STELIB, extinction by Cardielli et al. (1989), IMF by Chabrier (2003), Padova evoltion tracks, We use 25 values of SSP's ages within 0.0001-1.8X1010 yrs, Z = (0.0001, 0.0004, 0.004, 0.008, 0.02, 0.05).

First Surprise: Component H79f is not a tidal tail from component H79b as Nishiura et al (2000ab) had advanced. It is a disrupted galaxy. The action has taken place among the turn-around radii for the Seyfert’s Sextet we have:

Activity in H79b

How does SS compares with SQ? Rodríguez Baras, MSc. Thesis 2012, UAM/UCM Rosales-Ortega et al. 2010

Dust in Galaxies & Intragroup WISE+ IRAC Bitsakis et al. 2010

Where is the rest of the gas? X-rays HI & FIR

Where is the light? 46% (+/- 11 %) Rocha & Mendes de Oliveira (2005)

SS & The LSS

SS & The LSS

Caustics Analysis ss =208.36 Km/s Mdyn =5.5X1012 Msun

Philosophy: Not every hairy hydrofilic mammal ended up as a whale Philosophy: Not every hairy hydrofilic mammal ended up as a whale. Not every high-z dusty galaxy will become an early type galaxy. Evolution is driven by the environment.

Conclusions so far… CALIFA data is proving us with a new view of SS. For the first time we got the HSF in a disrupted galaxy using IFS. Destroyed galaxies can contribute with a large fraction of the intragroup light (Zemcov et al. (2014) says 50%). Unprecedented details on the fate of gas in dense environments. ALMA will coplete the story.

(B-R)=1.3-1.5 mag. (B-R)=1.2-1.3 mag. (B-R)=1.3-1.4 mag. (B-R)=1.3-1.8 mag.

SS & The LSS Ibarra’s Universal Pictures

Counter-rotating core, CALIFA vs. Durbala et al. 2008