Highly-excited CO emission in APM 08279+5255 at<i>z</i> = 3.9

Weiß, A.; Downes, D.; Neri, R.; Walter, Fabian; Henkel, C.; Wilner, David J.; Wagg, Jeff; Wiklind, T.

doi:10.1051/0004-6361:20066117

Cited by 264 publications

(467 citation statements)

References 73 publications

(141 reference statements)

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“…the center of M82 (Weiß et al 2007) or with what is typically observed in high-z sub-mm galaxies (SMGs; e.g., Bothwell et al 2013;Spilker et al 2014). ID.1 shows a CO(7-6)/CO(3-2) ratio r 73 =0.2, consistent with a high-density photon-dominated region (Meijerink et al 2007).…”

Section: Co Excitationmentioning

confidence: 89%

“…To date, only some several hundred sources at > z 1 have been detected in a molecular gas tracer (typically the rotational transitions of the carbon monoxide 12 CO molecule; e.g., Carilli & Walter 2013). This sample is dominated by "extreme" sources, such as QSO host galaxies (e.g., Bertoldi et al 2003;Walter et al 2003;Weiß et al 2007;Wang et al 2013) or submillimeter galaxies (e.g., Frayer et al 1998;Neri et al 2003;Greve et al 2005;Bothwell et al 2013;Riechers et al 2013;Aravena et al 2016), with IR luminosities  L 10 IR 12  L and star formation rates (SFRs) 100  M yr −1 . These extreme sources might contribute significantly to the star formation budget in the universe at > z 4, but their role declines with cosmic time (Casey et al 2014).…”

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confidence: 99%

“…Atz 0, the conversion factor that is typically used is ∼4  M (Kkm s −1 pc 2 ) −1 for "normal" * > M 10 9  M starforming galaxies with metallicities close to solar (see Bolatto et al 2013, for a recent review). If other CO transitions are observed instead of the J=1  0 ground state transition, a further factor is required to account for the CO excitation (see, e.g., Weiß et al 2007;Daddi et al 2015). Tacconi et al (2010) and Daddi et al (2010a) investigated the molecular gas content of highly star-forming galaxies atz 1.2 andz 2.3 via the CO(3-2) transition.…”

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confidence: 99%

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The Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Molecular Gas Reservoirs in High-Redshift Galaxies

Decarli

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Aravena

et al. 2016

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We study the molecular gas properties of high-z galaxies observed in the ALMA Spectroscopic Survey (ASPECS) that targets a ∼ 1 arcmin 2 region in the Hubble Ultra Deep Field (UDF), a blind survey of CO emission (tracing molecular gas) in the 3 mm and 1 mm bands. Of a total of 1302 galaxies in the field, 56 have spectroscopic redshifts and correspondingly well-defined physical properties. Among these, 11 have infrared luminosities L IR > 10 11 L , i.e. a detection in CO emission was expected. Out these, 7 are detected at various significance in CO, and 4 are undetected in CO emission. In the CO-detected sources, we find CO excitation conditions that are lower than typically found in starburst/SMG/QSO environments. We use the CO luminosities (including limits for non-detections)

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Section: Co Excitationmentioning

confidence: 89%

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confidence: 99%

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confidence: 99%

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The Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Molecular Gas Reservoirs in High-Redshift Galaxies

Decarli

Walter

Aravena

et al. 2016

ApJ

104

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“…This is in contrast with high-z quasar host galaxies, which can typically be modeled as dominated by a single high-excitation gas component (e.g. Riechers et al, 2011a;Weiß et al, 2007).…”

Section: Co Excitation and Spectral Line Energy Distributionsmentioning

confidence: 94%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…At lowz, molecular outflows have been observed in luminous AGNs (e.g., Feruglio et al 2010;Cicone et al 2014), and very high excitation CO lines have been observed in some AGNs (e.g., Weiß et al 2007;Hailey-Dunsheath et al 2012;Spinoglio et al 2012), but these components represent a small fraction in mass of the total molecular gas reservoirs in star-forming galaxies.…”

Section: Introductionmentioning

confidence: 99%

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Sharon

Riechers

Hodge

et al. 2016

ApJ

133

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We present CO(1-0) observations obtained at the Karl G. Jansky Very Large Array for 14z 2 galaxies with existing CO(3-2) measurements, including 11 galaxies thatcontain active galactic nuclei (AGNs) and three submillimeter galaxies (SMGs). We combine this sample with an additional 15z 2 galaxies from the literature that have both CO(1-0) and CO(3-2) measurements in order to evaluate differences in CO excitation between SMGs and AGN host galaxies, tomeasure the effects of CO excitation on the derived molecular gas properties of these populations, and to look for correlations between the molecular gas excitation and other physical parameters. With our expanded sample of CO(3-2)/CO(1-0) line ratio measurements, we do not find a statistically significant difference in the mean line ratio between SMGs and AGN host galaxies as can be found in the literature; we instead find =  r 1.03 0. for both populations combined). We also do not measure a statistically significant difference between the distributions of the line ratios for these populations at the p=0.05 level, although this result is less robust. We find no excitation dependence on the index or offset of the integrated Schmidt-Kennicutt relation for the two CO lines, and weobtain indices consistent with N=1 for the various subpopulations. However, including low-z "normal" galaxies increases our best-fit Schmidt-Kennicutt index toÑ 1.2. While we do not reproduce correlations between the CO line width and luminosity, we do reproduce correlations between CO excitation and star-formation efficiency.

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Highly-excited CO emission in APM 08279+5255 atz = 3.9

Cited by 264 publications

References 73 publications

The Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Molecular Gas Reservoirs in High-Redshift Galaxies

The Alma Spectroscopic Survey in the Hubble Ultra Deep Field: Molecular Gas Reservoirs in High-Redshift Galaxies

Dusty star-forming galaxies at high redshift

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

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