FIRST DETECTION OF THE [O III] 88 μm LINE AT HIGH REDSHIFTS: CHARACTERIZING THE STARBURST AND NARROW-LINE REGIONS IN EXTREME LUMINOSITY SYSTEMS

Ferkinhoff, Carl; Hailey-Dunsheath, S.; Nikola, Thomas; Parshley, Stephen C.; Stacey, G. J.; Benford, Dominic J.; Staguhn, Johannes

doi:10.1088/2041-8205/714/1/l147

Cited by 68 publications

(80 citation statements)

References 33 publications

(50 reference statements)

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“…Similar results were found by Ferkinhoff et al 2010 andSturm et al (2010) HaileyDunsheath et al 2010). The interesting conclusion is that, although these systems are intrinsically ULIRG or HyLIRGs, they do not show a deficit in the major PDR cooling lines as seen in nearby ULIRGs.…”

Section: Other Fine Structure Linessupporting

confidence: 87%

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Cool Gas in High-Redshift Galaxies

Carilli

Walter

2013

Annu. Rev. Astron. Astrophys.

1,090

1,251

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Over the last decade, observations of the cool interstellar medium in distant galaxies via molecular and atomic fine structure line emission has gone from a curious look into a few extreme, rare objects, to a mainstream tool to study galaxy formation, out to the highest redshifts. Molecular gas has now been observed in close to 200 galaxies at z > 1, including numerous AGN hostgalaxies out to z ∼ 7, highly starforming sub-millimeter galaxies (median redshift z ∼ 2.5), and increasing samples of 'main-sequence' color-selected star forming galaxies at z∼1.5-2.5. Studies have moved well beyond simple detections, to dynamical imaging at kpc-scale resolution, and multi-line, multi-species studies that determine the physical conditions in the interstellar medium in early galaxies. Observations of the cool gas are the required complement to studies of the stellar density and star formation history of the Universe, as they reveal the phase of the interstellar medium that immediately preceeds star formation in galaxies. Current observations suggest that the order of magnitude increase in the cosmic star formation rate density from z ∼ 0 to 2 is commensurate with a similar increase in the gas to stellar mass ratio in star forming disk galaxies. Progress has been made on determining the CO luminosity to H2 mass conversion factor at high-z, and the dicotomy between high versus low values for main sequence versus starburst galaxies, respectively, appears to persist with increasing redshift, with a likely dependence on metallicity and other local physical conditions. Studies of atomic fine structure line emission are rapidly progressing, with some tens of galaxies detected in the exceptionally bright [C II] 158µm line to date. The [C II] line is proving to be a unique tracer of galaxy dynamics in the early Universe, and, together with other atomic fine structure lines, has the potential to be the most direct means of obtaining spectroscopic redshifts for the first galaxies during cosmic reionization.

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Section: Other Fine Structure Linessupporting

confidence: 87%

“…Conversely, Valtchanov et al (2011) and Ferkinhoff et al (2010; 158µm line is realizing its potential in the study of the cooler atomic gas in distant galaxies. This strong line will be a workhorse-line for redshift determinations in the first galaxies, and in the study of galaxy dynamics at the highest redshifts.…”

Section: Other Fine Structure Linesmentioning

confidence: 99%

Cool Gas in High-Redshift Galaxies

Carilli

Walter

2013

Annu. Rev. Astron. Astrophys.

1,090

1,251

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“…In particular the fine structure line of [CII] at 158 μm is likely the brightest emission line observable at high-z (Maiolino et al 2009). The lines of [OIII] at 52 μm and 88 μm and [OI] at 63 μm have also been reported towards high-redshift lensed systems (Ferkinhoff et al 2010;Sturm et al 2010). …”

Section: Grb Host Galaxies With Almamentioning

confidence: 75%

Pre-ALMA observations of GRBs in the mm/submm range

Postigo

Lundgren

Martín

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) generate an afterglow emission that can be detected from radio to X-rays during days, or even weeks after the initial explosion. The peak of this emission crosses the millimeter and submillimeter range during the first hours to days, making their study in this range crucial for constraining the models. Observations have been limited until now due to the low sensitivity of the observatories in this range. This situation will be greatly improved with the start of scientific operations of the Atacama Large Millimeter/submillimeter Array (ALMA). Aims. In this work we do a statistical analysis of the complete sample of mm/submm observations of GRB afterglows obtained before the beginning of scientific operations at ALMA. Methods. We present observations of 11 GRB afterglows obtained from the Atacama Pathfinder Experiment (APEX) and the SubMillimeter Array (SMA), as well as the first detection of a GRB with ALMA, still in the commissioning phase, and put them into context with a catalogue of all the observations that have been published until now in the spectral range that is covered by ALMA.Results. The catalogue of mm/submm observations collected here is the largest to date and is composed of 102 GRBs, of which 88 have afterglow observations, whereas the rest are host galaxy searches. With our programmes, we contributed with data of 11 GRBs and the discovery of 2 submm counterparts. In total, the full sample, including data from the literature, has 22 afterglow detections with redshifts ranging from 0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peak luminosities spanning 2.5 orders of magnitude, the most luminous reaching 10 33 erg s −1 Hz −1 . We observe a correlation between the X-ray brightness at 0.5 days and the mm/submm peak brightness. Finally we give a rough estimate of the distribution of peak flux densities of GRB afterglows, based on the current mm/submm sample. Conclusions. Observations in the mm/submm bands have been shown to be crucial for our understanding of the physics of GRBs, but have until now been limited by the sensitivity of the observatories. With the start of the operations at ALMA, the sensitivity has improved by more than an order of magnitude, opening a new era in the study of GRB afterglows and their host galaxies. Our estimates predict that, once completed, ALMA will detect up to ∼98% of the afterglows if observed during the passage of the peak synchrotron emission.

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“…The L IR ∼ 3×10 13 L resulted in a first detection of the [NII] 122 µm line from a galaxy at z > 2.5 . In combination with the [OIII] 88 µm line intensity, Ferkinhoff et al (2010) find that the [OIII]/[NII] line ratio of SMM J02399−0136 is consistent with a scenario where the dominant source for the line emission is HII regions ionized by massive O9.5 stars, especially in light of the fact that the detected AGN is no longer considered to be the dominant contributor the IR luminosity of this system (Ivison et al, 2010c). Detected free-free emission from the system implies an AGN contribution to IR luminosity of at most 35% (Thomson et al, 2012).…”

Section: Smm J02399−0136mentioning

confidence: 99%

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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FIRST DETECTION OF THE [O III] 88 μm LINE AT HIGH REDSHIFTS: CHARACTERIZING THE STARBURST AND NARROW-LINE REGIONS IN EXTREME LUMINOSITY SYSTEMS

Cited by 68 publications

References 33 publications

Cool Gas in High-Redshift Galaxies

Cool Gas in High-Redshift Galaxies

Pre-ALMA observations of GRBs in the mm/submm range

Dusty star-forming galaxies at high redshift

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