Brightest Cluster Galaxies as seen by Integral-Field Spectroscopy

Summary of 2015 papers, stellar populations and stellar kinematics of BCGs

Transcript

1. BRIGHTEST CLUSTER GALAXIES AS SEEN BY INTEGRAL-FIELD SPECTROSCOPY Paola Oliva-Altamirano, Swinburne University
2. BRIGHTEST CLUSTER GALAXIES AS SEEN BY INTEGRAL-FIELD SPECTROSCOPY Disclaim er Paola Oliva-Altamirano, Swinburne University
3. BRIGHTEST CLUSTER GALAXIES AS SEEN BY INTEGRAL-FIELD SPECTROSCOPY This is NOT my current work Disclaim er Paola Oliva-Altamirano, Swinburne University
4. • Sarah Brough, AAO • Warrick Couch, AAO • Kim-Vy Tran, Texas A&M • Jimmy, Texas A&M IN COLLABORATION WITH • Chris Lidman, AAO • Richard McDermid, AAO • Chris Miller, University of Michigan • Rob Sharp, ANU
5. OUTLINE C4 2055
6. OUTLINE • Brief description of Brightest Cluster Galaxies (BCG) Evolution C4 2055
7. OUTLINE • Brief description of Brightest Cluster Galaxies (BCG) Evolution • Why is integral-field spectroscopy important to study these galaxies? C4 2055
8. OUTLINE • Brief description of Brightest Cluster Galaxies (BCG) Evolution • Why is integral-field spectroscopy important to study these galaxies? • Stellar Kinematics and Stellar populations of BCGs C4 2055
9. BRIGHTEST CLUSTER GALAXY (BCG) Refers to the central dominant galaxy in a cluster C4 2055
10. BCG FORMATION HYPOTHESIS From Cool Cores Cowie & Binney 1977 ∆CDM mergers Tonry 1985, Yamada +2002, Jordan +2004 Two phases scenario Oser +2010
11. BCG EVOLUTION • BCGs are expected to be at the end of the hierarchical evolution Lacey & Cole 1993
12. BCG EVOLUTION • BCGs are expected to be at the end of the hierarchical evolution Lacey & Cole 1993
13. MERGERS ARE IMPORTANT IN BCG EVOLUTION Summary of the Current Picture: At high redshifts (z>0.8) BCGs grow by Major Mergers Rapidly Burke & Collins 2013, Lidman +2013 At low redshifts (z>0.3) BCGs grow by Minor Mergers Slowly Edwards & Patton 2012, Oliva-Altamirano +2014 Observations of Lin +2013 Semi-Analytical model Guo +2011
14. MERGERS ARE IMPORTANT IN BCG EVOLUTION Summary of the Current Picture: At high redshifts (z>0.8) BCGs grow by Major Mergers Rapidly Burke & Collins 2013, Lidman +2013 At low redshifts (z>0.3) BCGs grow by Minor Mergers Slowly Edwards & Patton 2012, Oliva-Altamirano +2014 Observations of Lin +2013 Semi-Analytical model Guo +2011
15. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
16. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
17. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
18. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
19. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
20. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
21. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
22. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION
23. INTEGRAL-FIELD SPECTROSCOPY (IFS) IS AN OPEN WINDOW TO BCG’S EVOLUTION And the Massive survey
24. The accretion histories of BCGs can be traced by…
25. Stellar Kinematics The accretion histories of BCGs can be traced by…
26. Stellar Kinematics The accretion histories of BCGs can be traced by… Stellar Populations
27. Stellar Kinematics The accretion histories of BCGs can be traced by…
28. Stellar Kinematics The accretion histories of BCGs can be traced by…
29. KINEMATICS IN A NUTSHELL… Fit our spectra to stellar libraries.
30. KINEMATICS IN A NUTSHELL… Fit our spectra to stellar libraries. V, σ
31. KINEMATICS IN A NUTSHELL… Fit our spectra to stellar libraries. V, σ
32. KINEMATICS IN A NUTSHELL… Fit our spectra to stellar libraries. V, σ
33. KINEMATICS IN A NUTSHELL…
34. KINEMATICS IN A NUTSHELL…
35. KINEMATICS IN A NUTSHELL…
36. KINEMATICS IN A NUTSHELL…
37. KINEMATICS IN A NUTSHELL… Rotating Galaxies
38. KINEMATICS IN A NUTSHELL… Rotating Galaxies 2.0 1.0 0.0 v z Dispersion Dominated Galaxies
39. KINEMATICS IN A NUTSHELL… Rotating Galaxies 2.0 1.0 0.0 v z Dispersion Dominated Galaxies
40. KINEMATICS IN A NUTSHELL… Rotating Galaxies 2.0 1.0 0.0 v z Dispersion Dominated Galaxies Proxy for Angular momentum
41. KINEMATICS IN A NUTSHELL… Rotating Galaxies 2.0 1.0 0.0 v z Dispersion Dominated Galaxies Ellipticity Proxy for Angular momentum
42. KINEMATICS IN A NUTSHELL… Rotating Galaxies 2.0 1.0 0.0 v z Dispersion Dominated Galaxies Ellipticity Fast Rotators Proxy for Angular momentum
43. KINEMATICS IN A NUTSHELL… Rotating Galaxies 2.0 1.0 0.0 v z Dispersion Dominated Galaxies Ellipticity Fast Rotators Slow Rotator Proxy for Angular momentum
44. USING KINEMATICS TO TRACE MERGERS HYDRODYNAMICAL MODELS Gas Rich Major Mergers Create disks and show rotation Dry Major Merger Create dispersion supported galaxies Bournaud +2005 Boylan-Kolchin +2006, Naab & Burkert 2003, Bois +2011
45. Naab +2014 2.0 1.0 0.0 v σ z FR with gas rich minor mergers SR with gas rich major mergers SR with gas poor minor mergers Major merger
46. Naab +2014 2.0 1.0 0.0 v σ z FR with gas rich minor mergers SR with gas rich major mergers SR with gas poor minor mergers Major merger
47. Cappellari’s talk 2015
48. BCGS ARE PREDICTED TO BE SLOW ROTATORS This cannot be proven by SAURON, ATLAS3D, or CALIFA because their samples cover small volumes. These surveys have only include one BCG, M87
49. BCGS ARE PREDICTED TO BE SLOW ROTATORS This cannot be proven by SAURON, ATLAS3D, or CALIFA because their samples cover small volumes. These surveys have only include one BCG, M87
50. OTHER INDIVIDUAL STUDIES SUGGEST NO TREND IN THE STELLAR KINEMATICS… BCGs in the Coma Cluster Houghton +2013
51. OTHER INDIVIDUAL STUDIES SUGGEST NO TREND IN THE STELLAR KINEMATICS… BCGs in the Coma Cluster Houghton +2013
52. OTHER INDIVIDUAL STUDIES SUGGEST NO TREND IN THE STELLAR KINEMATICS… BCGs in the Coma Cluster Houghton +2013 M87 slow rotator with a kinematically decoupled core Emsellem +2014
53. DEDICATED IFS OBSERVATIONS OF BCGS BROUGH +2011, JIMMY +2013, OLIVA-ALTAMIRANO +2014, OLIVA-ALTAMIRANO +SUBMITTED 10 BCGs, 7 of them with close massive companions. Selected from the SDSS C4 catalogue (von der Linden +2007). Observed with VIMOS on the VLT
54. JIMMY +2013 found slow and fast rotators within the 10 BCGs… Brough +2011, Jimmy +2013
55. JIMMY +2013 found slow and fast rotators within the 10 BCGs… Brough +2011, Jimmy +2013
56. Are mergers the cause of the fast rotation in BCGs ?
57. Mixed Merger History Fast Rotator Slow Rotator Merging Not Merging
58. Mixed Merger History Fast Rotator Slow Rotator Merging Not Merging However the Merging BCGs in this sample are going through MINOR mergers. Next question: Is the fast rotation an indication of future MAJOR mergers?
59. What about the Environment?
60. NEW OBSERVATIONS 12 BCGS SELECTED FROM GAMA AND THE SDSS C4 CATALOGUE OBSERVED WITH SPIRAL ON THE AAT OLIVA-ALTAMIRANO +SUBMITTED
61. NEW OBSERVATIONS 12 BCGS SELECTED FROM GAMA AND THE SDSS C4 CATALOGUE OBSERVED WITH SPIRAL ON THE AAT These galaxies + other observations in the literature cover a wider range in stellar masses: 10<log(M/Mo)<11.8 and host halo cluster masses: 12<log(M/Mo)<15.5 OLIVA-ALTAMIRANO +SUBMITTED
62. 29 BCGS, ~40% OF THE GALAXIES ARE FAST ROTATORS New observations Jimmy +2013 Other galaxies in the literature: Coma, Virgo, Fornax, Abell 1689, 85, 168 and 2399 Cappellari 2013b, Emsellem et al. 2014, Scott et al. 2014, Houghton et al. 2013, D'Eugenio et al. 2012 and Fogarty et al. 2014 Oliva-Altamirano +submitted Proxy for Angular momentum 0.6
63. BCG rotation vrs Stellar Mass Angular Momentum Stellar Mass
64. BCG rotation vrs Stellar Mass Angular Momentum Stellar Mass
65. BCG rotation vrs Stellar Mass Angular Momentum Stellar Mass
66. BCG rotation vrs Stellar Mass Angular Momentum Stellar Mass
67. BCG rotation vrs Stellar Mass Stellar Mass log(M/Mo): FR: 11.03 +/- 0.08 SR: 11.32 +/-0.07 No FR after 11.5 Angular Momentum Stellar Mass
68. BCG rotation vrs Halo Mass Angular Momentum Cluster Malo Mass
69. BCG rotation vrs Halo Mass Angular Momentum Cluster Malo Mass
70. BCG rotation vrs Halo Mass Angular Momentum Cluster Malo Mass Cluster halo Mass log(M/Mo): FR: 14.2 +/- 0.14 SR: 14.63 +/- 0.18 No FR after 15
71. STELLAR MASS - CLUSTER HALO MASS RELATIONSHIP Stellar Mass Cluster Malo Mass Bigger Galaxies live in Bigger Clusters
72. BGCs evolve from fast-rotating group galaxies to slow-rotating cluster galaxies STELLAR MASS - CLUSTER HALO MASS - ANGULAR MOMENTUM RELATIONSHIP?
73. CLUSTER DOMINANCE Tremaine & Richstone 1977; Loh & Strauss 2006; Smith et al. 2010; Dariush et al. 2010; Coenda et al. 2012; Martel et al. 2014
74. CLUSTER DOMINANCE Dominance = Mag 1 - Mag 2 Tremaine & Richstone 1977; Loh & Strauss 2006; Smith et al. 2010; Dariush et al. 2010; Coenda et al. 2012; Martel et al. 2014
75. CLUSTER DOMINANCE Dominance = Mag 1 - Mag 2 Dominance < 1: Could indicate that the host halo has recently gone through a cluster-cluster merger Tremaine & Richstone 1977; Loh & Strauss 2006; Smith et al. 2010; Dariush et al. 2010; Coenda et al. 2012; Martel et al. 2014
76. CLUSTER DOMINANCE Dominance = Mag 1 - Mag 2 Dominance < 1: Could indicate that the host halo has recently gone through a cluster-cluster merger Dominance > 3: Could indicate that the host cluster has not gone through recent mergers Tremaine & Richstone 1977; Loh & Strauss 2006; Smith et al. 2010; Dariush et al. 2010; Coenda et al. 2012; Martel et al. 2014
77. BCG rotation vrs Cluster Dominance % of cluster mass residing in cluster substructure Smith +2010 Angular Momentum Cluster Dominance Dominance: FR: 0.81+/-0.14 SR: 1.54 +/-0.13 No FR after 1.5
78. BCG rotation vrs Cluster Dominance % of cluster mass residing in cluster substructure Smith +2010 Angular Momentum Cluster Dominance Dominance: FR: 0.81+/-0.14 SR: 1.54 +/-0.13 No FR after 1.5
79. BCG rotation vrs Cluster Dominance % of cluster mass residing in cluster substructure Smith +2010 Angular Momentum Cluster Dominance Dominance: FR: 0.81+/-0.14 SR: 1.54 +/-0.13 No FR after 1.5
80. BCG rotation vrs Cluster Dominance % of cluster mass residing in cluster substructure Smith +2010 Angular Momentum Cluster Dominance Dominance: FR: 0.81+/-0.14 SR: 1.54 +/-0.13 No FR after 1.5
81. Stellar Mass - Cluster Malo Mass relationship Dominance
82. Stellar Mass - Cluster Malo Mass relationship Dominance
83. Stellar Mass - Cluster Malo Mass relationship Dominance
84. Stellar Mass - Cluster Malo Mass relationship Dominance
85. Stellar Mass - Cluster Malo Mass relationship Dominance
86. Stellar Mass - Cluster Malo Mass relationship Dominance
87. XMM-Newton X-ray data Fogarty +2014 The two BCGs in Abell 2399 are fast-rotating
88. XMM-Newton X-ray data Fogarty +2014 The two BCGs in Abell 2399 are fast-rotating
89. • RECENT MINOR mergers do not change the angular momentum of BCGs (Jimmy +2013) • There is a connection between the stellar mass - cluster halo mass relationship and the BCG rotation (Oliva-Altamirano +submitted) • Cluster - cluster mergers can affect the BCG rotation (Oliva-Altamirano +submitted) SUMMARY:
90. • RECENT MINOR mergers do not change the angular momentum of BCGs (Jimmy +2013) • There is a connection between the stellar mass - cluster halo mass relationship and the BCG rotation (Oliva-Altamirano +submitted) • Cluster - cluster mergers can affect the BCG rotation (Oliva-Altamirano +submitted) SUMMARY:
91. • RECENT MINOR mergers do not change the angular momentum of BCGs (Jimmy +2013) • There is a connection between the stellar mass - cluster halo mass relationship and the BCG rotation (Oliva-Altamirano +submitted) • Cluster - cluster mergers can affect the BCG rotation (Oliva-Altamirano +submitted) stellar mass halo mass Angular momentum SUMMARY:
92. • RECENT MINOR mergers do not change the angular momentum of BCGs (Jimmy +2013) • There is a connection between the stellar mass - cluster halo mass relationship and the BCG rotation (Oliva-Altamirano +submitted) • Cluster - cluster mergers can affect the BCG rotation (Oliva-Altamirano +submitted) stellar mass halo mass Angular momentum SUMMARY: Dominance = Mag 1 - Mag
93. Stellar Kinematics The accretion histories of BCGs can be traced by… Stellar Populations
94. Stellar Kinematics The accretion histories of BCGs can be traced by… Stellar Populations
95. 5" The"galaxy"is" divided"into"annuli" that"follow"flux"" The"result:"one" spectrum"per" annulus"" Method'' Age"and"metallicity"per" spectrum"as"a"func<on"of" radius" " Full"spectrum"fi?ng"STECKMAP" Models:"Vazdekis"et."al."2010" Library:"MILES"SánchezQBlázquez"et."al."2006"
96. ACCRETION HISTORIES FROM STELLAR POPULATION GRADIENTS R Met Met R Cosmological simulations of Kobayashi +2004, Hirshmann +2014
97. ACCRETION HISTORIES FROM STELLAR POPULATION GRADIENTS R Met Met R Steep Met gradients >0.4: Could be due to core collapsed formation or major mergers involving high fractions of gas. Cosmological simulations of Kobayashi +2004, Hirshmann +2014
98. ACCRETION HISTORIES FROM STELLAR POPULATION GRADIENTS R Met Met R Steep Met gradients >0.4: Could be due to core collapsed formation or major mergers involving high fractions of gas. Shallow Met gradients >0.3: Are the result of major dissipationless mergers. Cosmological simulations of Kobayashi +2004, Hirshmann +2014
99. BCG STELLAR POPULATION GRADIENTS (SAME GALAXIES FROM JIMMY +2013) BCGs, ΔFe/H = -0.11+/-0.1 E-T, ΔZ/H = -0.19+/-0.1 Oliva-Altamirano +2015 Metallicity Dynamical Mass
100. BCG STELLAR POPULATION GRADIENTS (SAME GALAXIES FROM JIMMY +2013) Gradient = 0.3 BCGs, ΔFe/H = -0.11+/-0.1 E-T, ΔZ/H = -0.19+/-0.1 Oliva-Altamirano +2015 Metallicity Dynamical Mass
101. BCG STELLAR POPULATION GRADIENTS (SAME GALAXIES FROM JIMMY +2013) Gradient = 0.3 BCGs, ΔFe/H = -0.11+/-0.1 E-T, ΔZ/H = -0.19+/-0.1 Oliva-Altamirano +2015 Metallicity Dynamical Mass
102. BCG STELLAR POPULATION GRADIENTS (SAME GALAXIES FROM JIMMY +2013) Gradient = 0.3 BCGs, ΔFe/H = -0.11+/-0.1 E-T, ΔZ/H = -0.19+/-0.1 The BCG stellar population gradients are shallow and similar to those of early-type galaxies Oliva-Altamirano +2015 Metallicity Dynamical Mass
103. PREVIOUS RESULTS Loubser +2012, ∆Z/H = -0.28±0.06 Brough +2007, ∆Z/H = -0.31±0.05 Long-slit spectroscopy Loubser +2012 Metallicity
104. NEW RESULTS The BCG stellar population gradients are still shallow out to ~3 Re Green +2015 IFS spectroscopy from the MASSIVE survey Ma +2014
105. NEW RESULTS The BCG stellar population gradients are still shallow out to ~3 Re Green +2015 IFS spectroscopy from the MASSIVE survey Ma +2014 us
106. NEW RESULTS The BCG stellar population gradients are still shallow out to ~3 Re Green +2015 IFS spectroscopy from the MASSIVE survey Ma +2014 us
107. BCG CENTRAL STELLAR POPULATIONS (SAME GALAXIES FROM JIMMY +2013) Oliva-Altamirano +2015 BCGs, age = 8.9+/-3.1 E-T, age = 12.0 +/-3.8 Metallicity Dynamical Mass
108. BCG CENTRAL STELLAR POPULATIONS (SAME GALAXIES FROM JIMMY +2013) Oliva-Altamirano +2015 BCGs, age = 8.9+/-3.1 E-T, age = 12.0 +/-3.8 Metallicity Dynamical Mass
109. BCG CENTRAL STELLAR POPULATIONS (SAME GALAXIES FROM JIMMY +2013) The BCG central stellar populations are similar to those of early-type galaxies, with a wider range in ages Oliva-Altamirano +2015 BCGs, age = 8.9+/-3.1 E-T, age = 12.0 +/-3.8 Metallicity Dynamical Mass
110. PREVIOUS RESULTS 1.9 Log σ 2.5 1.1 Log Age 0.5 1.9 Log σ 2.5 0.02 [Fe/H] -0.14 Fitzpatrick +2012, Stacked SDSS galaxies BCGs show: slightly younger ages, slightly higher metallicities
111. PREVIOUS RESULTS Loubser +2009, Long-slit spectroscopy BCGs have: wide range of ages, slightly higher metallicities Log Age young old [Z/H]
112. BCGS HAVE DIVERSE EVOLUTIONARY PATHS Wen +2014 Continuous star-formation Passive evolution
113. BCGS HAVE DIVERSE EVOLUTIONARY PATHS SAM: Tonini +2012 Continious star formation up to z = 0.8
114. • BCGs have similar high metallicities: similar to early-type galaxies • BCGs have a wide range of ages: some similar to early-types other younger • BCGs have shallow stellar population gradients, even at large radii (Green +2015) SUMMARY: Oliva-Altamirano +2015
115. FUTURE PROJECTS Combined observations from the and KOALA (IFS on the AAT)
116. FUTURE PROJECTS Combined observations from the and KOALA (IFS on the AAT)
117. FUTURE PROJECTS Combined observations from the and KOALA (IFS on the AAT) Same projects larger samples (Sarah Brough with SAMI)
118. FUTURE PROJECTS Combined observations from the and KOALA (IFS on the AAT) Same projects larger samples (Sarah Brough with SAMI) Does the angular momentum of the BCG correlate with the Angular momentum of its host cluster? (P. Oliva-Altamirano)
119. FUTURE PROJECTS Combined observations from the and KOALA (IFS on the AAT) Same projects larger samples (Sarah Brough with SAMI) Does the angular momentum of the BCG correlate with the Angular momentum of its host cluster? (P. Oliva-Altamirano) What is the star formation history of these galaxies? When do they quench?(P. Oliva-Altamirano)