1. 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)
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

2. 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

3. 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* ≥ Mo
All points assume α~ 4 => empirical ratio ~ L’CO/R
Platen et al. 2011

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

5. 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

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

7. 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

8. 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,

9. b f c e a d

12. Durbala et al. 2008

14. 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 X1010 yrs, Z = (0.0001, , 0.004, 0.008, 0.02, 0.05).

15. 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:

16. Activity in H79b

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

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

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

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

21. SS & The LSS

22. SS & The LSS

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

24. 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.

25. 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.

27. (B-R)= mag.
(B-R)= mag.
(B-R)= mag.
(B-R)= mag.

32. SS & The LSS
Ibarra’s Universal Pictures

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