Spatially Resolved Millimeter Interferometry of SMM J02399–0136: A Very Massive Galaxy at z = 2.8
By R. Genzel, A. Baker, L. Tacconi, D. Lutz, P. Cox, S. Guilloteau, A. Omont. 2002
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We report high-resolution millimeter mapping with the IRAM Plateau de Bure interferometer of rest-frame 335 μm continuum and CO (3-2) line emission from the z = 2.8 submillimeter galaxy SMM J02399-0136. The continuum emission comes from a ~3'' diameter structure whose elongation is approximately east-west and whose centroid is coincident within the astrometric errors with the brightest X-ray and rest-UV peak (L1). The line data show that this structure is most likely a rapidly rotating disk. Its rotation velocity of ≥420 km s-1 implies a total dynamical mass of ≥3 × 1011 sin−2 i h M☉ within an intrinsic radius of 8 h kpc, most of which is plausibly in the form of stars and gas. SMM J02399-0136 is thus a very massive system, whose formation at z ~ 3 is not easy to understand in current cold dark matter hierarchical merger cosmogonies.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/2c673dab7423e0af4865ace698872212c4241b31
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Citations in the corpus
- Hα Spectroscopy of Galaxies at z > 2: Kinematics and Star Formation (2003, methodology): “…those we present here, withv & 200 km s−1 at a radius of∼ 1′′, although when the lensing correction is applied this radius corresponds to only ∼ 1 kpc. Genzel et al. (2002) have used millimeter interferometry to observe rest-frame 335µm continuum and CO(3–2) line emission from a massive…”
- Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, background): “However, the internal kinematics of one ULIRG at z = 2.8 indicates a mass >∼3 × 1011M⊙ (Genzel et al. 2003) making it a likely precursor to a very massive ETG. Blain et al. (2004) note that submillimeter-selected galaxies at z = 2 − 3 appear to be more strongly clustered than LBGs at the same…”
- A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, background): “Additionally, since the star-formation rates within these forming elliptical galaxies is expected to have been extremely high (e.g. Genzel et al. 2003), this also argues against an IMF that correlates with star-formation rate.”
- The Rest-Frame Optical Spectra of SCUBA Galaxies (2004, methodology): “By measuring the internal dynamics of the galaxies or the velocity offsets between companions, we can also place limits on their masses and so test if these galaxies are truly massive systems (Genzel et al. 2003).”
- Radiation Pressure-supported Starburst Disks and Active Galactic Nucleus Fueling (2005, background): “Most of these stars appear to lie in a thin disk located within 0.1− 0.3 parsecs of the black hole (Levin & Beloborodov 2003; Genzel et al. 2003).”
- Evidence for a Population of High-Redshift Submillimeter Galaxies from Interferometric Imaging (2007, background): “It also agrees with previous interferometric measurements of the angular extent of the millimeter (Downes et al. 1999; Genzel et al. 2003; Downes & Solomon 2003; Kneib et al. 2005; Tacconi et al. 2006) and submillimeter (Iono et al. 2006) emission from SMGs, and marginally with those of the radio…”
- Interferometric Observations of Powerful CO Emission from Three Submillimeter Galaxies at z = 2.39, 2.51, and 3.35 (2003, background): “Finally our observations strengthen the conclusion (e.g. Genzel et al. 2003) that the brightest submillimeter galaxies (S850 ∼ 2–10 mJy, corrected for lensing) have dynamical masses within the central few kpc that are comparable to massive, local early type galaxies (Mgas+Mstars ∼ m∗ ∼ 7× 1010…”