Globular Cluster Systems in Giant Ellipticals
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1 Globular Cluster Systems in Giant Ellipticals Karla Adriana Alamo Martínez CRyA - UNAM (México) ESO Chile Rosa Amelia González - CRyA-UNAM Michael West - ESO Chile John Blakeslee - Herzberg Institute for Astrophysics
2 Outline Introduction Giant Ellipticals / Fossil Groups / Abell 1689 Globular Clusters Goals Methodology Analysis Preliminary Results Future work
3 Introduction: Giant Ellipticals Hierarchical scenario Spheroidal shape mergers Morphology - Galactic density relation (Dressler 1980) Credit: NASA, ESA, and The Hubble Heritage Team (STScI/AURA)/
4 Giant Ellipticals : Link between galaxy clusters and regular galaxies Credit: X-ray: NASA/CXC/UCI/A.Lewis et al. Optical: Pal.Obs. DSS But... problems with time scale How to reconstruct their assembly history?
5 Globular Clusters very dense stellar objects galactic merger survivors Spectroscopic studies have revealed old ages. (Burstein et al. 1984) Ideal tool to reconstruct the history of giant ellipticals. M80 Credit: The Hubble Heritage Team (AURA/ STScI/ NASA)
6 Systems of Globular Clusters color metallicity N V - I Larsen et al. (2001) M V -7.4 Merger of gas-rich galaxies Ashman & Zepf (1992) Accretion of metal-poor population (using the GC mean metallicity and mass of the galaxy relation) Côte, Marzke & West (1998) Artifact of nonlinear color-metallicity relations Yoon et al. (2006)
7 Specific Frequency of GC, S N Efficiency of GC formation by mass unity, η - Globular cluster population - Velocity dispersion - X-ray emission Blakeslee et al This could be explained if the GC population of the BCG scales with the total mass of the galaxy cluster η 0.5/10 9 M Blakeslee 1999
8 Fossil Groups System dominated by a giant elliptical ( m>2) luminous as cd galaxies Extended X-ray emission NGC 1132 Credit: NASA, ESA, and the Hubble Heritage (STScI/AURA)- ESA/Hubble Collaboration Credit: X-ray: NASA/CXC/Penn State/G. Garmire
9 Fossil Groups Explanations for their nature: end product of galaxy mergers within a normal group but... high M/L Anomalous luminosity function Seyfert's Sextet Image Credit: NASA, J. English (U. Manitoba), S. Hunsberger, S. Zonak, J. Charlton, S. Gallagher (PSU), and L. Frattare (STScI)
10 Abell 1689 very massive and far system Abell 1689 X-ray: NASA/CXC/MIT/E.-H Peng et al; Optical: NASA/STScI 2 x10 15 M, M/L 400, z=0.18 Broadhurst et al. 2004
11 Goals Detect and analyze the CG system in FG Prototype, NGC 1132 Nearest one, NGC 6482 Most massive known to date, ESO Compare with cd and giant ellipticals in clusters Infer reliable assembling histories Detect and analyze the CG system in Abell 1689 Test if the formation of GC per mass is universal Establish a galaxy formation scenario
12 Methodology F850 SDSS z F475 SDSS g 3.5 NGC 6482 z=0.013;54 Mpc 0.26kpc/arcsec 54.6kpc NGC 1132 z=0.023;95 Mpc 0.46kpc/arcsec 96.6 kpc ESO 306-G017 z=0.039;146 Mpc 0.7kpc/arcsec 147kpc
13
14 Methodology Detected in g and z m 0-5 < m < mcut ; m< < g-z < 2.0 CLASS_STAR>0.7 ε<0.3 z [mag] z [mag] NGC 6482 NGC 1132 z [mag] ESO g z
15 N Analysis: Color Distribution NGC NGC ESO N 45 N g z g z g z μ blue # blue μ red # red σ p-value NGC NGC ESO
16 recovered/added Analysis: GCLF 60 m 0! 26.3 m 0! ! 1.4! NGC N g [mag] g [mag] NGC m 0! m 0! ! 1.4! N g g [mag] g [mag]
17 Analysis: GCLF m 0! m 0! ! 1.4! ESO N m " 26.5 g [mag] m " 26.5 g [mag] V=g (g-z) m 0 N GC M g M z S V N L X (10 42 erg/s) NGC NGC ESO Mendes de Oliveira et al. (2006)
18 Analysis: Spatial Distribution ESO NGC log N arcsec N 0 = 0.05 R CG e = n CG = = 2.19 log N arcsec N 0 = 0.02 R e CG = n CG = = log(r) [arcsec] NGC log(r) [arcsec] log N arcsec N 0 = 0.03 R e CG = 65.9 n CG = = log(r) [arcsec]
19 Analysis: B 4 isophotal parameter fast rotators disky z 0.05 B slow rotators boxy g NGC 6482 NGC 1132 ESO B log(r) [arcsec]
20 Analysis: Surface Brightness NGC 6482 mag(z) arcsec 2! ! mag(g) arcsec ! e = r e = 16.9 n = ! e = r e = n = 3.48 log(r) [arcsec] NGC log(r) [arcsec]
21 mag(z) arcsec 2 Analysis: Surface Brightness NGC mag(g) arcsec ! e = ; r e = ; 106 n = 6.93 ; ! log(r) [arcsec] NGC ! e = r e = 94.6 n = 6.54 ; ; ; ! log(r) [arcsec]
![0 0.5 1.0 1.5 2.0 log(r) [arcsec] ESO 306017 16 18 20! e = 16.75 ; 28.44 r e = 3267.](/docs-images/94/121056939/images/22-4.jpg "39; 1252 22 n = 12.59 ; 10.2 24! 0.2 0.1 0.0 0.1 0.2 1.0 0.5 0.0 0.5 1.0 1.5 2.")
22 mag(z) arcsec 2 Analysis: Surface Brightness ESO mag(g) arcsec ! e = ; r e = ; 564 n = 7.07 ; ! log(r) [arcsec] ESO ! e = ; r e = ; n = ; ! log(r) [arcsec]
23 Analysis: Spatial Distribution NGC NGC log N arcsec N 0 = 0.02 R e CG = n CG = = 1.29 mag(z) arcsec ! e = r e = n = log(r) [arcsec]! log(r) [arcsec] R SB e R GC e NGC NGC ESO
24 Preliminary Results GC color distribution is bimodal. If X-ray luminosity is an indication of the total mass, the GC population is bluer for more massive systems. Spatial distribution of GC is more extended than the galaxy light for NGC6482. However, is the opposite for NGC1132 and ESO The SN for ESO is anomalous. Isophotes disky. Product of mergers with mass ratio 4:1 Deviations from Sérsic profiles signatures of recent interaction.
25 Future Work Fossil Groups Spatial distribution of blue and red populations Subtract core-sérsic Estimate η Errors
26 Future Work Abell 1689 F814 Detect the GC system Bright (as explained before) Faint (Surface Brightness Fluctuations) N± N Sources of fluctuations: stars, GCs, galaxies and instrumental noise
27 power spectrum (z=0.05) P(k)=P 0 x E(k) + P 1 P 0 N CG S N assuming a range for σ LF Blakeslee, J. 1997
28 Estimation of bias and completeness inverse K-correction to each component using Bruzual & Charlot (2003) SSP models re-size the image cosmological angular size cosmological effects dimming of surface brightness as (1+z) -4 different signal-to-noise ratios considering different exposure times M87 z=0.0039
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30 end
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