{
  "id": "1804.03669",
  "version": "v1",
  "published": "2018-04-10T18:01:39.000Z",
  "updated": "2018-04-10T18:01:39.000Z",
  "title": "ZFIRE: 3D Modeling of Rotation, Dispersion, and Angular Momentum of Star-Forming Galaxies at z~2",
  "authors": [
    "Leo Y. Alcorn",
    "Kim-Vy Tran",
    "Karl Glazebrook",
    "Caroline M. Straatman",
    "Michael Cowley",
    "Ben Forrest",
    "Glenn G. Kacprzak",
    "Lisa J. Kewley",
    "Ivo Labbé",
    "Themiya Nanayakkara",
    "Lee R. Spitler",
    "Adam Tomczak",
    "Tiantian Yuan"
  ],
  "comment": "Accepted to ApJ",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We perform a kinematic and morphological analysis of 44 star-forming galaxies at $z\\sim2$ in the COSMOS legacy field using near-infrared spectroscopy from Keck/MOSFIRE and F160W imaging from CANDELS/3D-HST as part of the ZFIRE survey. Our sample consists of cluster and field galaxies from $2.0 < z < 2.5$ with K band multi-object slit spectroscopic measurements of their H$\\alpha$ emission lines. H$\\alpha$ rotational velocities and gas velocity dispersions are measured using the Heidelberg Emission Line Algorithm (HELA), which compares directly to simulated 3D data-cubes. Using a suite of simulated emission lines, we determine that HELA reliably recovers input S$_{0.5}$ and angular momentum at small offsets, but $V_{2.2}/\\sigma_g$ values are offset and highly scattered. We examine the role of regular and irregular morphology in the stellar mass kinematic scaling relations, deriving the kinematic measurement S$_{0.5}$, and finding $\\log(S_{0.5}) = (0.38\\pm0.07)\\log(M/M_{\\odot}-10) + (2.04\\pm0.03)$ with no significant offset between morphological populations and similar levels of scatter ($\\sim0.16$ dex). Additionally, we identify a correlation between M$_{\\star}$ and $V_{2.2}/\\sigma_g$ for the total sample, showing an increasing level of rotation dominance with increasing M$_{\\star}$, and a high level of scatter for both regular and irregular galaxies. We estimate the specific angular momenta ($j_{disk}$) of these galaxies and find a slope of $0.36\\pm0.12$, shallower than predicted without mass-dependent disk growth, but this result is possibly due to measurement uncertainty at M$_{\\star}$ $<$ 9.5. However, through a K-S test we find irregular galaxies to have marginally higher $j_{disk}$ values than regular galaxies, and high scatter at low masses in both populations.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2018-04-10T18:01:39.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "angular momentum",
      "star-forming galaxies",
      "mass kinematic scaling relations",
      "3d modeling",
      "dispersion"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}