the chemical enrichment of centauri john e. norris research schoool of astronomy & astrophysics...
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THE CHEMICAL ENRICHMENT OF CENTAURI
JOHN E. NORRIS
RESEARCH SCHOOOL OF ASTRONOMY & ASTROPHYSICS
MOUNT STROMLO & SIDING SPRING OBSERVATORIES
AUSTRALIAN NATIONAL UNIVERSITY
PLAN OF ATTACK• Historical review (pre ~1995)• Chemical abundances on the Red Giant Branch
– Metallicity Distribution Function & relative abundances– constraints on enriching stars and age spread
• Kinematics vs. abundance– Constraints on formation mechanisms
• Three populations• Main sequence studies
– Constraints on the population parameters
Collaborators: M.S.Bessell, K.Bekki, R.D.Cannon, G.S.Da Costa, K.C.Freeman, M.Mayor, K.Mighell, G.Paltoglou, P.Seitzer, L.Stanford
Abundance inhomogeneity of Cen (1960-1995)
• Discovery of CH star– Harding (1962)
• Wide giant branch
– Woolley et al (1966, photographic), Cannon & Stobie (1972, photoelectric)
Cen 47 Tuc
Cannon & Stobie 1972, MNRAS, 162, 207 Lee 1977, A&AS, 27, 381
Abundance inhomogeneity of Cen (1960-1995)
• Discovery of CH star– Harding (1962)
• Wide giant branch – Woolley et al (1966, photographic), Cannon & Stobie (1972, photoelectric)
• [Ca/H] spread among RR Lyrae stars– Freeman & Rodgers (1975, low res)
• Large CN variations among red giants– Norris & Bessell (1975, low res), Dickens & Bell (1976, low res)
• Large CO spread among red giants– Persson et al (1980, IR photometry)
[Ca/H] = log(N(Ca)/N(H))* -log(N(Ca)/N(H))o
Persson et al 1980, ApJ, 235, 452
C and/or O enhance-ment unique to Cen
Abundance inhomogeneity of Cen (1960-1995)
• Discovery of CH star– Harding (1962)
• Wide giant branch – Woolley et al (1966, photographic), Cannon & Stobie (1972, photoelectric)
• [Ca/H] spread among RR Lyrae stars– Freeman & Rodgers (1975, low res)
• Large CN variations among red giants– Norris & Bessell (1975, low res), Dickens & Bell (1976, low res)
• Large CO spread among red giants– Persson et al (1980, IR photometry)
• Heavy element abundance spreads – High resolution spectroscopy– Cohen (1981; 5 stars), Gratton (1982; 8), Francois et al (1988; 6),
Paltoglou & Norrris (1989; 15), Brown & Wallerstein (1993; 6), Norris & Da Costa (1995; 35), Smith et al (1995; 7)
Norris, Freeman & Mighell 1996, ApJ, 462, 241
Ca II H&K
Ca II infrared triplet
ROA 253
Low resolution (R~4000) [Ca/H] from Ca II H&K and Ca II infrared triplet
ROA 253
Norris, Freeman & Mighell 1996, ApJ, 462, 241
Ca II H&K AAT
Ca II triplet74-inch
Ca II triplet74-inch
[Ca/H] abundance histograms
METALLICITY DISTRIBUTION FUNCTION
[Ca/H] = log(N(Ca)/N(H))*
-log(N(Ca)/N(H))o
Norris, Freeman & Mighell 1996, ApJ, 462, 241
Two populations
First population: [Ca/H]0 = -1.59 <[Ca/H]> = -1.29
Second population: [Ca/H]0 = -1.09 <[Ca/H]> = -0.83
Simple model,closed box approximation:
metal-rich/metal-poor ~ 0.20
High resolution spectrum obtained withAAT UCL Echelle Spectrograph (UCLES)
High resolution spectra of 35 red giants(AAT UCLES, R~35,000;
Norris & Da Costa 1995, ApJ, 447, 680
[alpha/Fe] vs. [Fe/H](NB: heavily biased sample)
Enrichment by SNe II
Cen Other clusters
Norris & Da Costa 1995, ApJ, 447, 680
[neutron capture/Fe] vs. [Fe/H]
Enrichment by (intermediate-mass) AGB stars
Cen Other clusters
Norris, Freeman & Mighell, 1996 ApJ, 462, 241
Heavily biased sample(AAT UCLES high-res)
Unbiased sample(AAT, 74-inch low-res)
Normal globular clustersNo counterpartelsewhere in Galaxy. Suggestscausal link between populations
[Fe/H]-1.5-2.0 -1.0
0.0
0.0
0.0
1.0
1.0
1.0
Smith et al 2000, AJ, 119, 1239
5Mo
3Mo1.5Mo
5Mo3Mo1.5Mo
5Mo
3Mo1.5Mo
[Rb/Zr]
[Rb/Zr]
[Rb/Zr]
Star formation occurred over 2-3 Gyr
Norris, Freeman & Mighell 1996, ApJ, 462, 241
[Ca/Fe] vs. radius
Abundance decreases with radial distance
Norris, Freeman, Mayor & Seitzer 1997, ApJ, 487, L187
Rotation vs. abundance
Metal-poor sample:V = 10.7 +/- 1.8 km/s
Metal-rich sample:V = 3.0 +/- 2.4 km/s
Metal-poor population rotating more rapidly
Metal-poor sample kinematically hotter and rotating more rapidly.
Kinematics vs. abundance
Norris, Freeman, Mayor & Seitzer 1997, ApJ, 487, L187
O Not ELS collapseO Kinematically consistent with binary cluster evolution (e.g. Makino et al 1991 Ap&SS, 185, 63); but not clear this works chemically
Cen
Lee et al 1999,Nature, 402, 55
Ferraro et al 2004, ApJ, 603, L81Pancino et al 2000, ApJ, 584, L83
‘Third’ population
Pancino et al 2002, ApJ, 568, L101
Enrichment by SNe Ia
[Ca/Fe]
[Fe/H]
Sollima et al. 2005, MNRAS, 357, 265
To Cen’s main sequence withAAT Two Degree Field
Spectrographs
… working with Laura Stanford, Gary Da Costa & Russell Cannon(Stanford et al 2006, ApJ, 647,1075)
1998/992002
Stars observed in 2002 box Cen radial-velocity
members in 2002 box
Stanford thesis
Stanford thesis
Metallicity Distribution Function
Stanford et al (2006, ApJ, 647, 1075)
Stanford et al. (2006, ApJ, 647, 1075)
Stanford et al. (2006, ApJ, 647, 1075)
From -
• Ages of individual star in the CMD determined from YY isochrones, taking into account correlated age-metallicity errors
• Comparisons of Monte-Carlo CMD simulations with that of the cluster
There exists an age-metallicity relation, with the more metal-rich populations being younger by 2-4 Gyr than the metal poor one
Stanford et al. 2006, ApJ, 647, 1075Age ranges from the literature
Stanford et al. (2006, in prep)
[Sr/Fe] = +1.6[Ba/Fe] < +0.8:
Bedin et al. 2004, ApJ, 605, L125 (astro-ph/0403112) (also Anderson 1997, 2000, 2003 Thesis U
Berkeley & ASP Proceedings)
Anderson’s double main sequence
HST data
Bedin et al. suggest:
• Observations and/or modelling wrong
• Bluer main sequence has [Fe/H] < -2.0
• Bluer main sequence has higher helium (Y > 0.3)
• Two clusters superimposed, separated by 1-2 kpc along
line of sight
Majority, metal-poor population should be bluest!
Note: X = hydrogen mass fraction Y = helium mass fraction Z = heavy element mass fraction
Pop 1st 2nd 3rd[Fe/H] -1.7 -1.2 -0.6Y 0.23 0.23 0.23Age(Gyr) 16 16 16Fraction 0.80 0.15 0.05
Revised Yale Isochrones Norris 2004, ApJ 612, L25
Pop 1st 2nd 3rd[Fe/H] -1.7 -1.2 -0.6Y 0.23 0.23 0.23Age(Gyr) 16 14 12Fraction 0.80 0.15 0.05
Revised Yale Isochrones Norris 2004, ApJ, 612, L25
Pop 1st 2nd 3rd[Fe/H] -1.7 -1.2 -0.6Y 0.23 0.35 0.38Age(Gyr) 16 15 14Fraction 0.80 0.15 0.05
Revised Yale Isochrones Norris 2004 ApJ, 612, L25
Bedin et al. 2004, ApJ, 605, L125 (astro-ph/0403112) (also Anderson 1997, 2000, 2003 Thesis U
Berkeley & ASP Proceedings)
Anderson’s double main sequence
HST data
Piotto et al. 2005, ApJ, 621, 777
The blue main sequence is more metal-rich by 0.3 dex!
VLT Giraffe
BUT …
• Canonically, Y/Z ~3-4, and with an increase from [Fe/H] = -1.7 to -1.2 one expects only Y = 0.003!
• Suggests non-canonical evolution.
OBSERVATIONALLY …
• Determine Y from hot blue horizontal-branch stars?• Use sensitivity of HB luminosity and Teff to helium?• Zero-Age HB RR Lyraes of 2nd pop should be brighter by 0.2-
0.3mag. In contrast, the observed metal-richer RR Lyraes are fainter by 0.2-0.3mag! (see also Sollima et al. 2006, ApJ, 640, L43)
But … are the variables representative of the populations?
Ferraro et al 2004 ApJ, 603, L81
Pop 1st 2nd Alt.2nd[Fe/H] -1.7 -1.2 -1.2Y 0.23 0.35 0.23Age(Gyr) 14 12 12Fraction 0.80 0.15 0.15Turnoff mass (Msun) 0.82 0.71 0.85
Rey et al 2004
D’Cruz et al 2000 ApJ, 530, 352 - HST UV observations
“… over 30% of the HB objects are “extreme” HB or post-HB stars”
see also:Lee et al., 2005, ApJ, 621, L57
CANDIDATES FOR PRODUCERS OF HELIUM
• Massive stars (~60 Mo) with rotationally driven mass loss (Maeder & Meynet astro-ph/0601425) - also produce copius C, N, and O
• 10-14 Mo SNe (Piotto et al 2005, ApJ, 621, 777)
• More massive (~6-7 Mo) AGB stars• Problems with self enrichment by above candidates within a closed
system producing so much helium. (Pre-Maeder & Meynet) Bekki & Norris (2006, ApJ, 637, L109) suggested second population formed from gas “ejected from field stellar populations that surrounded Cen when it was the nucleus of an ancient dwarf galaxy”
• Helium diffusion in protocluster phase (Chuzhoy astro-ph/0602593): “Element diffusion can produce large fluctuations in the initial helium abundance of the star-forming clouds. Diffusion time-scale … can fall below108 years in the neutral gas clouds dominated by collisionless dark matter or with dynamically important radiation or magnetic pressure. ”
SUMMARY• Cen possesses at least three distinct populations, described
to first approximation by: Population First Second Third Fraction 0.80 0.15 0.05 [Fe/H] -1.7 -1.2 -0.6 Y 0.23 0.35 0.38: YY Age (Gyr) 14 12 12: (Vr) (km/s) 13 8 13
Rotation (km/s) 11 3 unknown
• The origin of the helium in the second population is currently not understood.
• System not formed in an ELS scenario, but more likely as a dwarf galaxy having multiple star-formation episodes well away from the forming Galaxy, and later being captured by it.
98/9998/99
2002
Stanford thesis (2006, ApJ, 647, 1075)
Age-Metallicity Relation
Stanford et al (2006, ApJ, 647, 1075)
Sollima et al. 2005, ApJ, 634, 332
Smith, Cunha & Lambert 1995 AJ, 110, 2827
Mixing line
[Fe/H]
[Ba/Fe]
Metallicity RangeStanford thesis work
Age-Metallicity Relation
Stanford et al (2006, ApJ, 647, 1075)
Norris & Da Costa 1995 ApJ, 447, 680
[iron peak/Fe] vs. [Fe/H]
Cen Other clusters
Stanford thesis work
Observations
Simulations of populations: [Fe/H] FractionFirst -1.7 0.80Second -1.2 0.15Third -0.6 0.05
0 Gyr
6 Gyr
4 Gyr
2 Gyr
Age spread
Stanford thesis work
[Fe/H]
Age(Gyr)
15
10
5
-2 -1
Turnoff stars
THE CHEMICAL ENRICHMENT OF CENTAURI
JOHN E. NORRIS
RESEARCH SCHOOOL OF ASTRONOMY & ASTROPHYSICS
MOUNT STROMLO & SIDING SPRING OBSERVATORIES
AUSTRALIAN NATIONAL UNIVERSITY
AAT Two Degree Field - Plate with fibres
D’Cruz et al 2000 ApJ, 530, 352 - HST UV observations
‘Normal’ Horizontal Branch
EHB
“… over 30% of the HB objects are “extreme” HB or post-HB stars”
V ~ 16