Il Sistema degli Ammassi Globulari nella galassia di Andromeda
Transcript of Il Sistema degli Ammassi Globulari nella galassia di Andromeda
Il Sistema degli Ammassi Globulari nella galassia di Andromeda
Flavio Fusi PecciINAF Osservatorio Astronomico
Bologna
La galassia nana del Sagittario
La galassia ellittica nana del Sagittario orbita attorno alla Via lattea ogni milione di anni. In un lontano futuro verrà “mangiata” dalla nostra galassia unendosi ad essa:
Alcune caratteristiche principali:Costellazione: SagittarioDistanza: 88 000 a.l.Magnitudine visuale: 4,5Diametro: 10 000 a.lTipo: dE
Figure 1 from PAndAS' Progeny:
Richardson et al. 2011 ApJ 732 76
Figure 3 Evidence for an Accretion Origin for the Outer Halo Globular Cluster System of M31
A. D. Mackey et al. 2010 ApJ 717 L11
M31 and the Milky Way are running towards each other at ~100km/sand they will finally collide in ~4 billion years
(It is likely the sun will be flung into a new region of our galaxy, but our Earth and solar system are in no danger of being destroyed!!!)
GALAXY FORMATION MECHANISM
• SINGLE, LARGE SCALE COLLAPSE
! < 109 yrs ~ 2 – 5 x 108 yrs
Eggen, Lynden Bell, Sandage 1962
• RANDOM MERGERS OF FRAGMENTED GAS CLOUDS
! ~ 2 – 4 x 109 yrs (… 1010 yrs?)
Searle, Zinn 1978
• MULTI-PHASE IN SITU FORMATION
Forbes, Bropie, Grillmair 1997• “CONTINUOUS” MERGERS
Zepf, Ashman 1993• TIDAL STRIPPING + CAPTURE
Cotè, Marzre, West 1992
GCs useful tools to study f.i.:
• Stellar evolution • Stellar dynamics• Distance indicators• Peculiar objects (variables, binaries, blue
stragglers, millesecond pulsars, etc.)• Templates of stellar populations• Parent galaxy formation, evolution, masses, etc. • Constraints on cosmic age, helium abundance, etc.
• etc. etc.
Come “appaiono” i GC’sman mano che si allontanano ?
• Diametro apparente e risoluzione in stelle sempre minore…
• Magnitudine integrata apparente sempre più debole….• Colori integrati diversi …. Metallicità ed età diverse..• Velocità radiale … compatibile con galassia parente..
• Galassia: (m-M) = 10-18 mag diam =50’-10’• Nubi di Mag: (m-M) = 18-20 mag diam =10’-2’• Andromeda: (m-M) = 24-25mag diam =20’’ - 2’’• Bordi Gruppo Locale: (m-M) = 27 mag diam=2’’-0.5’’• A (m-M) > 28…. 30… sono “uguali” alle stelle, hanno la
stessa “identica” Point Spread Function… e “… allora sono guai !” … come dice Edoardo Bennato
Telescopio Cassini 152 cm Loiano
• Circa 150 lastre
• 1- 2 ore di posa
• Seeing < 1",5 spesso ! 1"
• V > 20
25 x 25 cm
72'
scala 17"/mm
in totale un centinaio di lastre a grande campo BUONE (e centinaia di frames CCD post-1983)
oltre 350 GC selezionati da un campione di oltre 1000 candidati,
in un campo di 3° x 3° (~30 kpc)
oltre 30 kpc i GC previsti sono poche unità, ma si devono ispezionare molte migliaia di immagini (~1500/sqdeg)!
astrometria (<rms> ⇒ " ± 0,5" # ± 0,3")
1. Ricerca e selezione
2. Fotometria multicolore (FUV + UBVRIJHK)3. Morfologia
4. Spettroscopia
5. Identificazioni sorgenti X
6. Osservazioni HST
• 152 cm Loiano
• 2m Schmidt Tautenburg
• Palomar Schmidt
• 4m Kitt Peak
• Schmidt Campo Imperatore
• TNG
• LBT
• EINSTEIN
Fotometria di stelle singole nel GC’s
•…. dal 1993 in avanti HST
•… UV con GALEX
The most widely used catalogue of M31 GCs has been assembled
and is manteined at the Bologna observatory:
RBC
Lists more than two-thousands clusters, candidate clusters, previously believed candidates that now have a different
classifications
Includes positions, optical, NIR and UV colors, velocities, spectral indices,
metallicities…
~600 web contacts per year from all over the world
Studying an extragalactic GC system:methods and problems
Identify candidates: by shape (nearly stellar but extended; round; etc.), by color …
Verify the nature against possible contaminants: spectra (radial velocity, spectral type …) and, ultimately, resolve into stars (feasible only within the LG, with current instrumentation).
Colors and spectral indices to infer ages and metallicities
Spectroscopic Surveys of Candidate M31 GCs
How to discriminate a genuine cluster from a contaminant?
Cosmologic recession velocity ==> background galaxy
Vr around 0 km/s foreground Galactic star
Right Vr, emission lines ==> HII region
If Vr <-150 km/s ==> cluster
If -150<Vr<200 km/s and extended ==> cluster
Resolved into stars ==> cluster
Are they similar to their MW counterparts? CMDs with HST
Only an external corona is currently resolved into stars with HST: the typical CMD reaches just below the HBRich et al. 2005
M31 GCs show the same variety of HB morphologies as their MW counterparts.
The only case in which the TO level has been reached: 100 HST orbitsBrown et al. 2004
RR Lyr light curves in B514 from HST
Contreras et al. 2008
Endemic Clusters Species
Bright clusters at very large distances from theGalactic center:Only one counterpart in the MW (NGC2419)!
ECs
GCs
Extended Clusters: old & metal poor with 5"rh
Endemic Clusters Species
Massive YoungClusters
They lie in thedisc and have disc kinematics
Age < 1 Gyr
Mass > 104 M⊙
No counterpartin the MW
but…
A handful (12) of clusters with Red Super Giants are being discovered in the IR in the MW disc (Messineo et al. 2009). All of them have age< 20 Myr, while all MYC in our M31 sample have age > 25 Myr and mostof them have age > 50 Myr
How many? Luminosity Function
• A factor ≃ 3 more clusters, at least
• Note: the peaks of the distributions coincide, this is the basis for the use of GC LFs as distance indicators
• The M31 sample may be seriously incomplete for MV>-5
Old clusters have the same color Distribution. Young massive clusters seems relatively frequent in M31 and are missing in the MW but this may be (partly) due to selection effects as weare immersed in the MW Disc, while we see the Disc of M31 from “above”
Fusi Pecci et al. 2005
Spectra & Spectral indices
1, 4, 13 Gyr @ Z⊙ [Fe/H]= -1.7, -0.4, +0.4 @ 10 Gyr
FIXED
METALLICITY
FIXED
AGE
The sensitivity to age and metallicity is not better than that of integrated colors
BUT 1.They are reddening free2.One can take advantage of the different sensitivity of different indices to disentangle age and metallicity
Spectra & Spectral indices
H!
H!
"
"
An example:At fixed amplitude of the Balmer jump #Differences in H$ traces differences in
ages, for ages > 1Gyr
Large values of H$ (> 3.5 Å) always indicate young ages
Fusi Pecci et al. 2005
15
8 2
Spectra & Spectral indices
Another example:A metallicity scale for old GCs based on
Lick indices
Galleti et al. 2009
Brodie & Huchra 1990
Spectra & Spectral indices
Compare metallicity from Lick indices vs. from CMDs:
we can do this only in M31Galleti et al. 2009
Rotation as a function of metal content
MW GC’sZinn 1985
Only clusters with [Fe/H]>-0.8Rotate
The net rotation of the metal-poor clusters is consistent with Zero
M31 GC’s: the ratio of dispersion to rotational velocity increases with decreasing metallicityBut the rotation pattern is present at any metallicity.
Galleti et al. 2009
The horizontal branch luminosity vs. metallicity of M 31 globular clusters
A&A 544, A155 (2012) L. Federici - C. Cacciari - M. Bellazzini - F. Fusi
Pecci – S. Galleti - S. Perina
The horizontal branch morphology of M 31 globular clusters.
Extreme second parameter effect in outer halo clusters
A&A 546, A31 (2012)
S. Perina - M. Bellazzini – A. Buzzoni - C. Cacciari
45
Not all GCs were created simple…from the “classical” ω Cen …
Norris et al. 1996
Bedin et al. 2004Ferraro et al. 2004
Lee et al. 1999
B-V
V
46
Not all GCs were created simple…to M54, NGC 2808, M22, etc …
NGC2808: Piotto et al. 2005
M54: Siegel et al. 2007M22: courtesy A.Milone
Conclusion• As shown for NGC 6441 & 6388, there is a quite
wide group of metal-rich GCs in M31 which share the UV-excess + BHB anomaly
• Most of these objects are among the brightest metal-rich GCs in M31, brighter (i.e. more massive) than ω Cen in the MW
• Very Bright (i.e. very massive) metal-rich GC’s in M31 (probably) contain multi-populations (possibly) He-enriched at various levels (even quite high) as found in ω Cen in the MW
Helium-rich Globular clusters?Helium-rich Globular clusters?
Rey et al (2007) (adapted)
X
M87
M31
MW
Wilkinson & Evans (1999) used motions of 27 globularclusters and satellites : made a dynamical model of thehalo and estimated the total mass to be
Mtotal = 1.9 +3.6 - 1.7 x 1012 M
La massa della Via Lattea ....
Evans & Wilkinson (2000) used satellites and GCs in M31 to derive a lower limit on the mass of
1.2+3.6 -1.7 x 1012 M
for M31 - similar to the Galaxy, within the uncertainties
La massa di M31
For comparison, from least action arguments, the likely mass of the local group is 4-8 x 1012 M
( Peebles 1996, Schmoldt & Saha 1998)
Within the uncertainties, most of the mass in the Local Groupcould be in the two large spirals
La massa totale di MW + M31 ~ 3 x 1012 M