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Galaxy Rotations applied to Cosmology

Galaxy Rotations applied to Cosmology. Yuxiang Qin Supervisors: Danail Obreschkow & Chris Power. Contents. Introduction Method & discussion Step 1. Fitting the relation between the specific angular momenta j and the star mass M Step 2. 2 – point correlation

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Galaxy Rotations applied to Cosmology

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  1. Galaxy Rotations applied to Cosmology Yuxiang Qin Supervisors: DanailObreschkow & Chris Power

  2. Contents • Introduction • Method & discussion • Step 1. Fitting the relation between the specific angular momenta j and the star mass M • Step 2. 2 – point correlation • Conclusions & future work

  3. Introduction • Former work: • The HIPASS Catalogue: • Meyer et al. 2004 • Zwaanet al. 2004 • Doyle et al. 2005 • Zwaan et al 2005 • Putman et al. 2002 • Koribalski et al. 2004 • Obreschkow et al 2013 • … … • The HI Parkes All-Sky Survey (HIPASS) • HI blind radio survey • 4315 sources identified by HI content • Declination range: -90° ~ 2° • Velocity range: -1280 ~ 12700 km/s

  4. Method • Step 1_1. • Fitting the relation between the specific angular momenta j and the star mass M

  5. Result Where do these deviations come from ? Observational / Physical

  6. Discussion Do they only result from the observational uncertainty ?

  7. Step 1_ 2. Separate the samples by Hubble Type

  8. Step 2_1. 2– point correlation Definition: Calculation: Landy & Szalay (1993)

  9. Result of the whole HIPASS Datas Assuming the 2 – point correlation function has a power-law form Then we obtain:

  10. Step 2_2. Separate the samples by Hubble Type & Dlog10j 2-point correlation as a function of Hubble type 2-point correlation as a function of Dlog10j

  11. Conclusions & future work • stronger clustering with decreasing specific angular momenta • late-type morphologies cluster less than early-type galaxies • Study with larger samples, in order to obtain more precise result • study the clustering as a function of other physicalproperties like HI mass

  12. Thanks for your listening! • Thanks for the guidance of my supervisors, DanailObreschkowand Chris Power, and the help from Martin Meyer. • Thanks for the program provided by Pauli Pihajokifrom University of Turku

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