Interferometric Observations of Powerful CO Emission from Three Submillimeter Galaxies at z = 2.39, 2.51, and 3.35

By R. Neri, R. Genzel, R. Ivison, F. Bertoldi, A. Blain, S. Chapman, P. Cox, T. Greve, A. Omont, D. Frayer. 2003

181 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1594e243f26a03a6964d90152c3f54134a45f624

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. D. Narayanan
4. D. M. Alexander
5. R. Somerville
6. R. Dav'e
7. A. Dekel
8. Thomas J. Cox

In Nuclear and High Energy Physics

1. D. M. Alexander
2. P. Hopkins
3. L. Hernquist
4. R. Ivison
5. I. Smail
6. C. Carilli
7. S. Chapman
8. A. Blain

Citations in the corpus

• A survey of molecular gas in luminous sub-millimetre galaxies (2012, methodology): “08+470016.2 150 0.17 0.7 – – Neri et al. (2003) SMM J105141.”
• COLD GASS, an IRAM legacy survey of molecular gas in massive galaxies - II. The non-universality of the molecular gas depletion time-scale (2011, unknown): “…used to characterize the molecular gas content of submillimetre galaxies (SMGs; e.g. Frayer et al. 1998; Downes & Solomon 2003; Genzel et al. 2003; Neri et al. 2003; Kneib et al. 2005; Tacconi et al. 2008; Bothwell et al. 2010; Engel et al. 2010) and normal star-forming galaxies at z > 1 (e.g.…”
• Tracing the molecular gas in distant submillimetre galaxies via CO(1-0) imaging with the EVLA (2010, methodology): “…/m nras/article-abstract/412/3/1913/1055927 by guest on 11 D ecem ber 2018 2002; Chapman et al. 2005), with redshifts determined via Keck spectroscopy (Chapman et al. 2003, 2005) and confirmed via detections of 12CO J = 3–2 at PdBI (Neri et al. 2003; Greve et al. 2005; Tacconi et al. 2006, 2008).”
• Evidence for Extended, Obscured Starbursts in Submillimeter Galaxies (2004, background): “While evidence for massive amounts of molecular gas in SMGs has now been established (Frayer et al. 1998; Neri et al. 2003; T. Greve et al. 2004, in preparation), and X-ray luminosities are consistent with a dominant role for star formation in the energetics of SMGs (D. Alexander et al. 2004, in…”
• The Star Formation Rate and Dense Molecular Gas in Galaxies (2003, background): “The highest LCO detected among submillimeter galaxies is ∼ 0.7 × 10 11Kkms−1pc2 (Neri et al. 2003; Greve, Ivison, & Papadopoulos 2003).”
• Submillimeter Galaxies at z ~ 2: Evidence for Major Mergers and Constraints on Lifetimes, IMF, and CO-H2 Conversion Factor (2008, methodology): “For all four SMGs we applied an average of the isotropic estimator above and the ‘‘global rotating disk estimator’’ introduced by Neri et al. (2003), corrected for sin (i)h i ¼ /4 ¼ 1/1:27318 in velocity and sin2(i) ¼ 2/3 in mass, resulting in Mdyn;disk R R1=2 6 ; 104 v 2FWHM km s 1 R1=2 kpc M ð…”
• Cool Gas in High-Redshift Galaxies (2013, methodology): “4.3.3 Other fine structure lines There have been only a few detections of fine structure lines other than [C II] at high redshift to date, mostly in strongly lensed systems using principally the PdBI and Herschel.”
• Can the faint submillimetre galaxies be explained in the Λ cold dark matter model (2005, background): “This type of picture is hinted at observationally by the very large gas fractions implied by CO measurements of SMGs (e.g. Neri et al. 2003).”
• THE STELLAR MASS CONTENT OF SUBMILLIMETER-SELECTED GALAXIES (2010, methodology): “We consider as possible scenarios that SMGs are starbursts of constant SFR of duration 50, 100, 200, and 400 Myr, covering the range of estimates of the duration of the starburst in the SMG phase from CO observations (e.g., Neri et al. 2003; Greve et al. 2005; Tacconi et al. 2006).”
• SUBMILLIMETER GALAXIES AS PROGENITORS OF COMPACT QUIESCENT GALAXIES (2014, background): “A large fraction of SMGs with measured CO profiles, show double peaked profiles, evident of ongoing major mergers or rotation (Frayer et al. 1999; Neri et al. 2003; Sheth et al. 2004; Kneib et al. 2005; Greve et al. 2005; Tacconi et al. 2006; Riechers et al. 2011b; Ivison et al. 2013; Fu et al.…”
• DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, background): “So far, only a handful of cases have gone through this whole chain of observations (e.g., Genzel et al. 2003; Greve et al. 2005; Neri et al. 2003), but a high success rate gives confidence in the first step of the identification process.”
• An interferometric CO survey of luminous submillimetre galaxies (2005, methodology): “Thus, dynamical masses were calculated using the ’merger’ formula given in Neri et al. 2003 (see also Genzel et al. 2003), and reported in Table 3.”
• MOST SUBMILLIMETER GALAXIES ARE MAJOR MERGERS (2010, methodology): “The full available correlator capacity was configured to cover 1 GHz in each polarisation, which adequately covers the broad CO lines seen in SMGs (Genzel et al. 2003; Neri et al. 2003; Greve et al. 2005).”
• Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, background): “There is significant observational support for this picture (e.g. Ivison et al. 2002, 2007, 2010; Chapman et al. 2003; Neri et al. 2003; Smail et al. 2004; Swinbank et al. 2004; Greve et al. 2005; Tacconi et al. 2006, 2008; Bouché et al. 2007; Biggs & Ivison 2008; Capak et al. 2008; Younger et al.…”
• Characterization of Scuba-2 450 μm and 850 μm selected galaxies in the COSMOS field (2013, background): “Follow-up studies of their molecular and ionised gas properties (Swinbank et al. 2004; Neri et al. 2003; Greve et al. 2005; Tacconi et al. 2006, 2008; Bothwell et al. 2010; Engel et al. 2010; Banerji et al. 2011; Alaghband-Zadeh et al. c© 0000 RAS ar X iv :1 30 2.”
• Molecular Gas at High Redshift (2005, background): “Neri et al. (2003).”
• MOLECULAR GAS IN z ∼ 6 QUASAR HOST GALAXIES (2010, background): “The dynamical masses (Mdyn) of the eight z∼6 quasars can be expressed as Mdyn ≈ 2.3 × 105vcir 2R (e.g., Neri et al. 2003; Walter et al. 2004; SV05; Narayanan et al. 2008), where R is the disk radius in kpc and vcir is the maximum circular velocity of the gas disk in km s−1.”
• The Spectral Energy Distribution of CO lines in M82 (2005, result): “However, there are a few examples where the flux density from the CO J = 3→2 transition is similar or higher than that of the J = 7→6 line (see e.g. SMM 14011+0252 (z = 2.5, Downes & Solomon 2003), SMM 16368+4057 (z = 2.4, Neri et al. 2003).”
• The Rest-Frame Optical Spectra of SCUBA Galaxies (2004, methodology): “…goal of these observations was to provide precise systemic redshifts of the SMGs/OFRGs to compare to those measured in the UV and also to provide a precise redshift for our ongoing CO mapping program on the Plateau de Bure interferometer (Neri et al. 2003; T. R. Greve et al. 2004, in preparation).”