NUCLEAR STAR CLUSTERS IN 228 SPIRAL GALAXIES WITH HUBBLE

Transcription

1 Inter-Departmental Science Workshop Aranjuez, Spain, 20 October 2013 NUCLEAR STAR CLUSTERS IN 228 SPIRAL GALAXIES WITH HUBBLE Iskren Georgiev International Research Fellow ESTEC, Noordwijk, Netherlands In collaboration with: T.Böker, P.Goudfrooij, Th. Puzia, M.Hilker, S.Mieske, H.Baumgardth

2 Massive/globular star clusters - Mass (~10 5 M, M ) - Size (reff = 3 pc ) - Density (10 3 /pc 3 ) - coeval stellar population Bellini et al. (2010)

3 Massive/globular star clusters - Mass (~10 5 M, M ) - Size (reff = 3 pc ) - Density (10 3 /pc 3 ) - coeval stellar population 2 pc 6.5ly 1.3x10 4 AU Bellini et al. (2010)

4 Massive/globular star clusters - Mass (~10 5 M, M ) - Size (reff = 3 pc ) - Density (10 3 /pc 3 ) - coeval stellar population 2 pc 6.5ly 1.3x10 4 AU Image Credit: NASA/JPL-Caltech Bellini et al. (2010)

5 Image Credit: NASA/JPL-Caltech Massive/globular star clusters - Mass (~10 5 M, M ) - Size (reff = 3 pc ) - Density (10 3 /pc 3 ) - coeval stellar population 2 pc 6.5ly 1.3x10 4 AU Bellini et al. (2010)

6 Massive/globular star clusters - Mass (~10 5 M, M ) - Size (reff = 3 pc ) - Density (10 3 /pc 3 ) - coeval stellar population Ima 2 pc 6.5ly 1.3x10 4 AU

7 Massive/globular star clusters - Mass (~10 5 M, M ) - Size (reff = 3 pc ) - Density (10 3 /pc 3 ) - coeval stellar population Ima 2 pc 6.5ly 1.3x10 4 AU

8 Massive/globular star clusters - Mass (~105M, M ) - Size (reff = 3 pc ) - Density (103 /pc3) - coeval stellar population Ima Omega Centauri 2 pc 6.5ly 1.3x104AU ESO/INAF-VST/OmegaCAM. Acknowledgement: A. Grado/INAF-Capodimonte Observatory

9 Nuclear clusters in the Family of Stellar systems E de dsph UCDs NCs GCs Misgeld & Hilker (2011)

10 Nuclear clusters in the Family of Stellar systems E de dsph UCDs NCs GCs Misgeld & Hilker (2011) * NCs Formation channels - Connection to UCDs (stripped nuclei?) - in situ via gas accretion - in spiraled massive GCs - cluster mergers

11 Nuclear clusters in the Family of Stellar systems E de dsph * Galactic nuclei - cluster to BH dominated nucleus - connections and interplay between NCs and BHs Ferrarese et al. (2006) UCDs NCs GCs Misgeld & Hilker (2011) * NCs Formation channels - Connection to UCDs (stripped nuclei?) - in situ via gas accretion - in spiraled massive GCs - cluster mergers

12 Nuclear Star Clusters in late type Spirals 1x1 kpc NSC half-light radius reff = 4 pc 8 x 8 kpc

13 Nuclear Star Clusters in late type Spirals 1x1 kpc NSC half-light radius reff = 4 pc 8 x 8 kpc The largest database of nuclear star clusters (NSCs) of >200 spiral galaxies with Hubble Space Telescope WFPC2 imaging in the archive

14 Nuclear Star Clusters in late type Spirals 1x1 kpc NSC half-light radius reff = 4 pc 8 x 8 kpc The largest database of nuclear star clusters (NSCs) of >200 spiral galaxies with Hubble Space Telescope WFPC2 imaging in the archive a homogeneous measurement of structural and photometric properties of NSCs

15 Nuclear Star Clusters in late type Spirals 1x1 kpc NSC half-light radius reff = 4 pc 8 x 8 kpc The largest database of nuclear star clusters (NSCs) of >200 spiral galaxies with Hubble Space Telescope WFPC2 imaging in the archive a homogeneous measurement of structural and photometric properties of NSCs Formation, evolution, relation to massive globular clusters and Ultra Compact Dwarf galaxies, and co-existence of NSCs and Massive Black Holes

16 Galaxy sample, NSCs and WFPC2 characteristics Galaxy sample Low-inclination <88 Nearby < 35 Mpc >5000

17 Galaxy sample, NSCs and WFPC2 characteristics Galaxy sample Low-inclination <88 Nearby < 35 Mpc >5000 HST/WFPC2 archive: 340 galaxies 47 programs 9 filters (UV to I) 65 GB raw data

18 Galaxy sample, NSCs and WFPC2 characteristics Galaxy sample Low-inclination <88 Nearby < 35 Mpc >5000 HST/WFPC2 archive: 340 galaxies 47 programs 9 filters (UV to I) 65 GB raw data

19 Galaxy sample, NSCs and WFPC2 characteristics Galaxy sample Low-inclination <88 Nearby < 35 Mpc >5000 HST/WFPC2 archive: 340 galaxies 47 programs 9 filters (UV to I) 65 GB raw data

20 Galaxy sample, NSCs and WFPC2 characteristics Galaxy sample Low-inclination <88 Nearby < 35 Mpc > /pix HST/WFPC2 archive: 340 galaxies 47 programs 9 filters (UV to I) 65 GB raw data 0.1 /pix

21 Galaxy sample, NSCs and WFPC2 characteristics Galaxy sample Low-inclination <88 Nearby < 35 Mpc > /pix HST/WFPC2 archive: 340 galaxies 47 programs 9 filters (UV to I) 65 GB raw data 0.1 /pix structure and photometry for 228 Nuclear Star Clusters

22 Measuring Nuclear Star Cluster properties With the Hubble Space Telescope - Wide Field and Planetary Camera 2 (WFPC2) TinyTIM PSFs - position - filter - breathing etc. Krist et al. (2011) Georgiev & Böker (in prep.)

23 Measuring Nuclear Star Cluster properties With the Hubble Space Telescope - Wide Field and Planetary Camera 2 (WFPC2) TinyTIM PSFs - position - filter - breathing etc. Krist et al. (2011) ishape - TinyTim PSF - Analytic model - Best χ 2 fit model - 10% of PSF FWHM Larsen (1999) Georgiev & Böker (in prep.)

24 Measuring Nuclear Star Cluster properties With the Hubble Space Telescope - Wide Field and Planetary Camera 2 (WFPC2) TinyTIM PSFs - position - filter - breathing etc. Krist et al. (2011) ishape - TinyTim PSF - Analytic model - Best χ 2 fit model - 10% of PSF FWHM Larsen (1999) Georgiev & Böker (in prep.)

25 Measuring Nuclear Star Cluster properties With the Hubble Space Telescope - Wide Field and Planetary Camera 2 (WFPC2) TinyTIM PSFs - position - filter - breathing etc. Krist et al. (2011) ishape - TinyTim PSF - Analytic model - Best χ 2 fit model - 10% of PSF FWHM Larsen (1999) Output - Model magnitude - structural parameters: reff, effective radius ϵ, ellipticity, PA, position angle, Georgiev & Böker (in prep.)

26 Measuring Nuclear Star Cluster properties With the Hubble Space Telescope - Wide Field and Planetary Camera 2 (WFPC2) TinyTIM PSFs - position - filter - breathing etc. Krist et al. (2011) ishape - TinyTim PSF - Analytic model - Best χ 2 fit model - 10% of PSF FWHM Larsen (1999) Output - Model magnitude - structural parameters: reff, effective radius ϵ, ellipticity, PA, position angle, As free of contaminating flux as possible flux and size measurement of 228 NCSs Georgiev & Böker (in prep.)

27 0.2 Distance and S/N dependent resolution limits r eff [pc] 1 0.2pix WF 0.2pix PC PC 30 WF Distance to NSC host galaxy [Mpc] S/N Georgiev & Böker (in prep.)

28 0.2 Distance and S/N dependent resolution limits r eff [pc] 1 Georgiev & Böker (in prep.) 0.2pix WF 0.2pix PC PC 30 WF Distance to NSC host galaxy [Mpc] More than 90% of the NSCs (S/N>30) with robust Reff measurement S/N

29 Stellar populations in Nuclear Star Clusters Myr 10 8 M 500 Myr 1Gyr 2Gyr NCs model colours S/N<30 or unresolved 1Z -16 M F606W [mag] NGC7424 Georgiev & Böker (in prep.) 10 7 M 10 6 M 10 5 M 10 4 M 14Gyr 20 Gyr IC2056 IC0396 NGC3338 NGC2344 NGC4030 NGC4900 NGC1084 NGC6744 NGC4041 NGC2997 NGC5300 NGC3631 NGC3344 NGC3666 NGC7793 UGC08041 NGC3949 NGC4237 NGC1058 NGC3041 NGC1073 NGC3756 UGC09215 NGC5964 NGC1325 NGC4504M074 NGC4595 NGC0959 NGC1559 NGC0428 NGC1809 NGC5530 NGC4559 NGC5334 NGC3274 NGC4525 NGC1042 NGC1249 NGC2835 NGC7741 NGC7713 NGC5556 NGC4635 NGC3913 NGC2283 UGC03574 NGC1003 NGC5112 NGC1258 NGC4534 NGC5068 UGC06983NGC0672 NGC3423 IC0239 MCG NGC7090 NGC3782 NGC4393 NGC F450W - F606W [mag] NSCs span a wide range in metalicity, age and mass

30 Luminosity vs. effective radius of Nuclear Clusters E de dsph UCDs NCs GCs Georgiev & Böker (in prep.) Misgeld & Hilker (2011)

31 Luminosity vs. effective radius of Nuclear Clusters L V [L V, ] N2419 r 10 effv, [pc] wcen M54 1 NSCs NSCs in late-types NSCs in early-types UCDs MW GCs M V [mag] Georgiev & Böker (in prep.)

32 Summary - Largest homogeneous analysis of NSCs in late-type spiral galaxies - NSCs span a wide range in age and mass - NSCs can be the progeny of massive GCs and UCDs Outlook - NSCs in Spiral galaxies - release of a database of structure and photometry of 228 NSCs - Studying the formation and co-evolution of nuclear objects - nuclear clusters and BHs - Stellar pops of NSCs in the NIR: HST/WFC3 (JWST)