FIRST DETECTIONS OF THE [N II] 122 μm LINE AT HIGH REDSHIFT: DEMONSTRATING THE UTILITY OF THE LINE FOR STUDYING GALAXIES IN THE EARLY UNIVERSE

Ferkinhoff, Carl; Brisbin, D.; Nikola, Thomas; Parshley, Stephen C.; Stacey, G. J.; Phillips, T. G.; Falgarone, É.; Benford, Dominic J.; Staguhn, Johannes; Tucker, C.

doi:10.1088/2041-8205/740/1/l29

Cited by 64 publications

(80 citation statements)

References 45 publications

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“…Hailey-Dunsheath et al, 2010;Wagg et al, 2010;De Breuck et al, 2011;Ferkinhoff et al, 2011;Swinbank et al, 2012;Coppin et al, 2012). These studies have found that at typical ULIRG luminosities, where local galaxies exhibit a clear [CII]/FIR deficit, some high-z SMGs appear to show a [CII] excess.…”

Section: The [Cii]-fir Deficit In Galaxiesmentioning

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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Section: The [Cii]-fir Deficit In Galaxiesmentioning

confidence: 94%

Dusty star-forming galaxies at high redshift

2014

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“…Oberst et al (2006Oberst et al ( , 2011 used the observed [CII]/[NII] 205 µm ratio in the Carina nebula to constrain the contribution from HII regions to 30%. This technique has since also been applied to high redshift objects (Ferkinhoff et al 2011;Decarli et al 2014). …”

Section: Other Contributions To the [Cii] Emissionmentioning

confidence: 99%

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Gullberg

Breuck

Vieira

et al. 2015

Monthly Notices of the Royal Astronomical Society

147

224

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We present [CII] observations of 20 strongly lensed dusty star forming galaxies at 2.1 < z < 5.7 using APEX and Herschel. The sources were selected on their 1.4 mm flux (S 1.4 mm > 20 mJy) from the South Pole Telescope survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. Eleven out of 20 sources observed in [CII] also have low-J CO detections from ATCA. A comparison with midand high-J CO lines from ALMA reveals consistent [CII] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [CII], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [CII] to CO(1-0) luminosity ratios in the SPT sample of 5200 ± 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [CII] and CO emitting gas with a higher [CII] than CO excitation temperature, high CO optical depth τ CO (1-0) 1, and low to moderate [CII] optical depth τ [CII] 1. The geometric structure of photodissociation regions allows for such conditions.

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“…3 in Kamphuis et al 2007 −3 , the ratio of these two lines is relatively insensitive to the gas density. If the emission arises from H regions 4 , then the ratio gives an indication of the effective stellar temperature of the ionizing source (Ferkinhoff et al 2011) and thus can be used to constrain the stellar classification of the youngest stars in a H region. We find that for the majority of the mapped region of NGC 891 (see (2014), we compare our observed ratios to the model predictions.…”

Section: Ionised Gas Characteristicsmentioning

confidence: 99%

Insights into gas heating and cooling in the disc of NGC 891 fromHerschelfar-infrared spectroscopy

Hughes

Foyle

Schirm

et al. 2015

A&A

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We present Herschel PACS and SPIRE spectroscopy of the most important far-infrared cooling lines in the nearby, edge-on spiral galaxy, NGC 891: [C] with increasing FIR colour suggests that polycyclic aromatic hydrocarbons (PAHs) may become important for gas heating in the central regions. We compare the observed flux of the FIR cooling lines and total IR emission with the predicted flux from a PDR model to determine the gas density, surface temperature and the strength of the incident far-ultraviolet (FUV) radiation field, G 0 . Resolving details on physical scales of ∼0.6 kpc, a pixel-by-pixel analysis reveals that the majority of the PDRs in NGC 891's disc have hydrogen densities of 1 < log(n/cm −3 ) < 3.5 experiencing an incident FUV radiation field with strengths of 1.7 < log G 0 < 3. Although these values we derive for most of the disc are consistent with the gas properties found in PDRs in the spiral arms and inter-arm regions of M 51, observed radial trends in n and G 0 are shown to be sensitive to varying optical thickness in the lines, demonstrating the importance of accurately accounting for optical depth effects when interpreting observations of high inclination systems. Increasing the coverage of our analysis by using an empirical relationship between the MIPS 24 µm and [N] 205 µm emission, we estimate an enhancement of the FUV radiation field strength in the far north-eastern side of the disc relative to the rest of the disc that coincides with the above-average star formation rate surface densities and gas-to-dust ratios. However, an accurate interpretation remains difficult due to optical depth effects, confusion along the line-of-sight and observational uncertainties.

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FIRST DETECTIONS OF THE [N II] 122 μm LINE AT HIGH REDSHIFT: DEMONSTRATING THE UTILITY OF THE LINE FOR STUDYING GALAXIES IN THE EARLY UNIVERSE

Cited by 64 publications

References 45 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Insights into gas heating and cooling in the disc of NGC 891 fromHerschelfar-infrared spectroscopy

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