The FMOS-COSMOS Survey of Star-forming Galaxies at Z ∼ 1.6. V: Properties of Dark Matter Halos Containing Hα Emitting Galaxies
- Institute for Astronomy, Department of Physics, ETH Zürich, Wolfgang-Pauli-Strasse 27, CH-8093 Zürich (Switzerland)
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo, Kashiwanoha, Kashiwa, Chiba 277-8583 (Japan)
- Laboratoire AIM-Paris-Saclay, CEA/DSM-CNRS-Université Paris Diderot, Irfu/Service d’Astrophysique, CEA-Saclay, Orme des Merisiers, F-91191 Gif-sur-Yvette (France)
- INAF Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova (Italy)
- Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)
- Dipartimento di Fisica e Astronomia, Università di Padova, vicolo dell’Osservatorio, 2, I-35122 Padova (Italy)
- Research Center for Space and Cosmic Evolution, Ehime University, Bunkyo-cho 2-5, Matsuyama, Ehime 790-8577 (Japan)
- School of Physics and Astronomy, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623 (United States)
- Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, F-13388 Marseille (France)
- Astronomy Program, Department of Physics and Astronomy, Seoul National University 599 Gwanak-ro, Gwanak-gu, Seoul, 151-742 (Korea, Republic of)
We study the properties of dark matter halos that contain star-forming galaxies at 1.43 ≤ z ≤ 1.74, using the FMOS-COSMOS survey. The sample consists of 516 objects with a detection of the Hα emission line, which represent the star forming population at this epoch, having a stellar mass range of 10{sup 9.57} ≤ M {sub *}/M {sub ⊙} ≲ 10{sup 11.4} and a star-formation rate range of 15 ≲ SFR/(M {sub ⊙} yr{sup −1}) ≲ 600. We measure the projected two-point correlation function while carefully taking into account observational biases, and find a significant clustering amplitude at scales of 0.04–10 h {sup −1} cMpc, with a correlation length r{sub 0}=5.26{sub −0.62}{sup +0.75} h{sup −1} cMpc and a bias b=2.44{sub −0.32}{sup +0.38}. We interpret our clustering measurement using a halo occupation distribution model. The sample galaxies appear to reside in halos with mass M{sub h}=4.71{sub −1.62}{sup +1.19}×10{sup 12} h{sup −1} M{sub ⊙} on average, which will likely become present-day halos of mass M {sub h} (z = 0) ∼ 2 × 10{sup 13} h {sup −1} M {sub ⊙}, equivalent to the typical halo mass scale of galaxy groups. We then confirm the decline of the stellar-to-halo mass ratio at M {sub h} < 10{sup 12} M {sub ⊙}, finding M {sub *}/M {sub h} ≈ 5 × 10{sup −3} at M {sub h} = 7. 5 × 10{sup 11} M {sub ⊙}, which is lower by a factor of 2–4 than those measured at higher masses (M {sub h} ∼ 10{sup 12–13} M {sub ⊙}). Finally, we use our results to illustrate the future capabilities of Subaru’s Prime-Focus Spectrograph, a next-generation instrument that will provide strong constraints on the galaxy-formation scenario by obtaining precise measurements of galaxy clustering at z > 1.
- OSTI ID:
- 22876032
- Journal Information:
- Astrophysical Journal, Vol. 843, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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