STAR FORMATION RATES FROM [C II] 158 μm AND MID-INFRARED EMISSION LINES FOR STARBURSTS AND ACTIVE GALACTIC NUCLEI

We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the [C II] fine-structure line and the underlying far-infrared (FIR) dust continuum emission in J1120+0641, the most distant quasar currently known (z 7.1 = ). We also present observations targeting the CO(2-1), CO(7-6), and emission in the field covered by ALMA (∼ 25″). At the resolution of our ALMA observations (0 23, or 1.2 kpc, a factor of ∼70 smaller beam area compared to previous measurements), we find that the majority of the emission is very compact: a high fraction (∼80%) of the total line and continuum flux is associated with a region 1-1.5 kpc in diameter. The remaining ∼20% of the emission is distributed over a larger area with radius 4 kpc. The [C II] emission does not exhibit ordered motion on kiloparsec scales: applying the virial theorem yields an upper limit on the dynamical mass of the host galaxy of 4.3 0.9 10 10 ( ) M  , only ∼20×higher than the central black hole (BH). The other targeted lines (CO(2-1), CO(7-6), and [C I]) are not detected, but the limits of the line ratios with respect to the [C II] emission imply that the heating in the quasar host is dominated by star formation, and not by the accreting BH. The star formation rate (SFR) implied by the FIR continuum is 105-340 M yr 1 - , with a resulting SFR surface density of ∼100-350 M yr 1 - kpc −2 , well below the value for Eddington-accretion-limited star formation.

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“…This is only ∼30% lower than that of local starburst galaxies (e.g., Díaz-Santos et al 2013;Sargsyan et al 2014).…”

Section: [C Ii] Emission Linementioning

confidence: 73%

The Compact, ∼1 kpc Host Galaxy of a Quasar at a Redshift of 7.1

Venemans

Walter

Decarli

et al. 2017

ApJ

119

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“…The far-IR fine-structure transitions [Cii] 2 P 3/2 − 2 P 1/2 at 157.7 µm, [Oi] 3 P 2 − 3 P 1 at 63.2 µm, and [Oiii] 3 P 1 − 3 P 0 at 88.4 µm (hereafter referred to as [C II], [O I], and [O III]) have been used as diagnostic tracers of the interstellar medium (ISM) and star formation activity for over two decades (e.g., Malhotra et al 1997;Luhman et al 1998;Fischer et al 1999;Luhman et al 2003;Sturm et al 2010;Stacey et al 2010;Ferkinhoff et al 2010;Wang et al 2013b;De Looze et al 2014;Pineda et al 2014;Sargsyan et al 2014;Rigopoulou et al 2014;Capak et al 2015;Gullberg et al 2015;Willott et al 2015;Díaz-Santos et al 2013;Diaz-Santos et al 2017). [C II] is often observed to be one of the strongest emission lines in the spectra of galaxies, and can comprise up to ∼ 0.1 − 1% of the infrared (IR) luminosity (Stacey et al 1991;Helou et al 2001).…”

Section: Introductionmentioning

confidence: 99%

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Olsen

Greve

Narayanan

et al. 2017

ApJ

103

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Of the almost 40 star forming galaxies at z > ∼ 5 (not counting QSOs) observed in [C II] to date, nearly half are either very faint in [C II], or not detected at all, and fall well below expectations based on locally derived relations between star formation rate and [C II] luminosity. This has raised questions as to how reliable [C II] is as a tracer of star formation activity at these epochs and how factors such as metallicity might affect the [C II] emission. Combining cosmological zoom simulations of galaxies with SÍGAME (SImulator of GAlaxy Millimeter/submillimeter Emission) we have modeled the multi-phased interstellar medium ( We find that the [C II] emission is dominated by the diffuse ionized gas phase and molecular clouds, which on average contribute ∼ 66% and ∼ 27%, respectively. The molecular gas, which constitutes only ∼ 10% of the total gas mass is thus a more efficient emitter of [C II] than the ionized gas, which makes up ∼ 85% of the total gas mass. A principal component analysis shows that the [C II] luminosity correlates with the star formation activity of a galaxy as well as its average metallicity. The low metallicities of our simulations together with their low molecular gas mass fractions can account for their [C II]-faintness, and we suggest these factors may also be responsible for the [C II]-faint normal galaxies observed at these early epochs.

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“…8) found by the South Pole Telescope (SPT; Gullberg et al 2015) and Herschel (Cox et al 2011;Valtchanov et al 2011;Riechers et al 2013;Magdis et al 2014;Rawle et al 2014), and many should fall along the local LIRG/ULIRG relation when corrected for magnification, as shown by a detailed study of a z = 2.013 lensed [C II] source by Schaerer et al (2015). Determining whether the larger scatter associated with the remaining Magdis et al (2013) and a study of 130 mid-and far-IR selected galaxies by Sargsyan et al (2014) also drew a similar conclusion.…”

Section: [C Ii]/fir Ratio and High Radiation Fieldmentioning

confidence: 96%

Early Science with the Large Millimeter Telescope: CO and [C ii] Emission in thez = 4.3 AzTEC J095942.9+022938 (COSMOS AzTEC-1)

Yun¹,

Aretxaga²,

Gurwell³

et al. 2015

Mon. Not. R. Astron. Soc.

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Measuring redshifted CO line emission is an unambiguous method for obtaining an accurate redshift and total cold gas content of optically faint, dusty starburst systems. Here, we report the first successful spectroscopic redshift determination of AzTEC J095942.9+022938 ("COSMOS AzTEC-1"), the brightest 1.1mm continuum source found in the AzTEC/JCMT survey (Scott et al. 2008), through a clear detection of the redshifted CO (4-3) and CO (5-4) lines using the Redshift Search Receiver on the Large Millimeter Telescope. The CO redshift of z = 4.3420 ± 0.0004 is confirmed by the detection of the redshifted 158 µm [C II] line using the Submillimeter Array. The new redshift and Herschel photometry yield L F IR = (1.1 ± 0.1) × 10 13 L and SF R ≈ 1300 M yr −1 . Its molecular gas mass derived using the ULIRG conversion factor is 1.4 ± 0.2 × 10 11 M while the total ISM mass derived from the 1.1mm dust continuum is 3.7 ± 0.7 × 10 11 M assuming T d = 35 K. Our dynamical mass analysis suggests that the compact gas disk (r ≈ 1.1 kpc, inferred from dust continuum and SED analysis) has to be nearly face-on, providing a natural explanation for the uncommonly bright, compact stellar light seen by the HST.9 L is remarkably high, but it is only 0.04 per cent of the total IR luminosity. AzTEC COSMOS-1 and other high redshift sources with a spatially resolved size extend the tight trend seen between [C II]/FIR ratio and Σ F IR among IR-bright galaxies reported by Díaz-Santos et al. (2013) by more than an order of magnitude, supporting the explanation that the higher intensity of the IR radiation field is responsible for the "[C II] deficiency" seen among luminous starburst galaxies.

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STAR FORMATION RATES FROM [C II] 158 μm AND MID-INFRARED EMISSION LINES FOR STARBURSTS AND ACTIVE GALACTIC NUCLEI

Cited by 75 publications

References 49 publications

The Compact, ∼1 kpc Host Galaxy of a Quasar at a Redshift of 7.1

The Compact, ∼1 kpc Host Galaxy of a Quasar at a Redshift of 7.1

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Early Science with the Large Millimeter Telescope: CO and [C ii] Emission in thez = 4.3 AzTEC J095942.9+022938 (COSMOS AzTEC-1)

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