Detecting the most distant (z&gt;7) objects with ALMA

Walter, Fabian; Carilli, C. L.

doi:10.1007/s10509-007-9634-1

Cited by 14 publications

(10 citation statements)

References 19 publications

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“…In the near future, high‐frequency ALMA surveys will start to detect [C ii ] emission in sources from z ≳ 1 out to high redshifts (Walter & Carilli 2008). These surveys will have sufficient sensitivity to detect Lyman‐break galaxies with star formation rates of ≲10 M ⊙ yr −1 and metallicities below 0.1 Z ⊙ (Mannucci et al 2009).…”

Section: Discussionmentioning

confidence: 99%

The potential influence of far-infrared emission lines on the selection of high-redshift galaxies

Smail

Swinbank

Ivison

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

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We investigate whether strong molecular and atomic emission lines at far‐infrared wavelengths can influence the identification and derived properties of galaxies selected from broad‐band, far‐infrared or submillimetre observations. Several of these lines, for example, [C ii] 158 μm, have been found to be very bright in some galaxies, with fluxes of ≳0.1–1 per cent of the total far‐infrared luminosity, and may be even brighter in certain populations at high redshifts. At redshifts where these lines fall in instrument passbands, they can significantly increase the broad‐band flux measurements. We estimate that the contributions from line emission could boost the apparent broad‐band flux by ≳20–40 per cent in the Herschel and SCUBA‐2 bands. Combined with the steep source counts in the submillimetre and far‐infrared bands, line contamination has potentially significant consequences for the properties of sources detected in flux‐limited continuum surveys, biasing the derived redshift distributions and bolometric luminosities. Indeed, it is possible that some z > 4 sources found in 850‐μm surveys are being identified in part due to the line contamination from strong [C ii] emission. These biases may be even stronger for less‐luminous and lower metallicity populations at high redshifts, which are observable with the ALMA and which may have even stronger line‐to‐continuum ratios.

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Section: Discussionmentioning

confidence: 99%

The potential influence of far-infrared emission lines on the selection of high-redshift galaxies

Smail

Swinbank

Ivison

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

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“…The observations presented here are currently the best means by which to quantify star formation rates and their surface densities in quasars at the earliest cosmic epochs. They thus demonstrate that [CII] observations will play a key role in studies of resolved star formation regions in the first Gyr of the Universe using the upcoming Atacama Large Millimeter/submillimeter Array (ALMA) 25 . There is good agreement between the optical quasar and the peak of the continuum emission, as well as the peak of the molecular gas emission traced by CO, demonstrating that our astrometry is accurate on scales of < 0.1 ′′ .…”

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confidence: 91%

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confidence: 91%

A kiloparsec-scale hyper-starburst in a quasar host less than 1 gigayear after the Big Bang

Walter

Riechers

Cox

et al. 2009

Nature

Self Cite

237

286

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The host galaxy of the quasar SDSS J114816.64+525150.3 (at redshift z=6.42, when the Universe was <1 billion years old) has an infrared luminosity of 2.2×10 13 L 1,2 ⊙ , presumably significantly powered by a massive burst of star formation 3,4,5,6 . In local examples of extremely luminous galaxies such as Arp 220, the burst of star formation is concentrated in the relatively small central region of < 100 pc radius 7,8 . It is unknown on which scales stars are forming in active galaxies in the early Universe, which are likely undergoing their initial burst of star formation. We do know that at some early point structures comparable to the spheroidal bulge of the Milky Way must have formed. Here we report a spatially resolved image of [CII] emission of the host galaxy of J114816.64+525150.3 that demonstrates that its star forming gas is distributed over a radius of ∼ 750 pc around the centre. The surface density of the star formation rate averaged over this region is ∼1000 M ⊙ year −1 kpc −2 . This surface density is comparable to the peak in Arp 220, though ∼2 orders of magnitudes larger in area. This vigorous star forming event will likely give rise to a massive spheroidal component in this system.The forbidden 2 P 3/2 → 2 P 1/2 fine-structure line of ionized Carbon ([CII]) at 158 microns provides effective cooling in regions where atomic transitions cannot be excited, and therefore helps gas clouds to contract and form stars. [CII] emission is thus known to be a fundamental diagnostic tool of the starforming interstellar medium 9,10 . Given the very bright continuum emission of the central accreting black hole of quasars in optical and near-infrared wavebands, standard star formation tracers (such as hydrogen recombination lines) cannot be used to study star formation in these systems. The [CII]

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“…Atomic lines such as the fine-structure line of singly-ionized carbon, [C ii], probe the interstellar medium and the outer parts of star-forming regions. It has been recognized that the Electronic address: chris.willott@nrc.ca [C ii] line will likely become the most useful line for studying very high redshift galaxies with the Atacama Large Millimeter Array (ALMA; Walter & Carilli 2008). Indeed early ALMA observations already show detections of [C ii] in normal star-forming galaxies at z > 4 (Wagg et al 2012;.…”

Section: Introductionmentioning

confidence: 99%

REDSHIFT 6.4 HOST GALAXIES OF 10⁸SOLAR MASS BLACK HOLES: LOW STAR FORMATION RATE AND DYNAMICAL MASS

Willott¹,

Omont²,

Bergeron³

2013

ApJ

149

230

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We present ALMA observations of rest-frame far-infrared continuum and [C ii] line emission in two z = 6.4 quasars with black hole masses of ≈ 10 8 M . CFHQS J0210-0456 is detected in the continuum with a 1.2 mm flux of 120 ± 35 µJy, whereas CFHQS J2329-0301 is undetected at a similar noise level. J2329-0301 has a star formation rate limit of < 40 M yr −1 , considerably below the typical value at all redshifts for this bolometric luminosity. By comparison with hydro simulations, we speculate that this quasar is observed at a relatively rare phase where quasar feedback has effectively shut down star formation in the host galaxy. [C ii] emission is also detected only in J0210-0456. The ratio of [C ii] to far-infrared luminosity is similar to that of low redshift galaxies of comparable luminosity, suggesting the previous finding of an offset in the relationships between this ratio and far-infrared luminosity at low-and high-redshift may be partially due to a selection effect due to the limited sensitivity of previous continuum data. The [C ii] line of J0210-0456 is relatively narrow (FWHM = 189±18 km s −1 ), indicating a dynamical mass substantially lower than expected from the local black hole -velocity dispersion correlation. The [C ii] line is marginally resolved at 0. 7 resolution with the blue and red wings spatially offset by 0. 5 (3 kpc) and a smooth velocity gradient of 100 km s −1 across a scale of 6 kpc, possibly due to rotation of a galaxy-wide disk. These observations are consistent with the idea that stellar mass growth lags black hole accretion for quasars at this epoch with respect to more recent times.

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Detecting the most distant (z>7) objects with ALMA

Cited by 14 publications

References 19 publications

The potential influence of far-infrared emission lines on the selection of high-redshift galaxies

The potential influence of far-infrared emission lines on the selection of high-redshift galaxies

A kiloparsec-scale hyper-starburst in a quasar host less than 1 gigayear after the Big Bang

REDSHIFT 6.4 HOST GALAXIES OF 10⁸SOLAR MASS BLACK HOLES: LOW STAR FORMATION RATE AND DYNAMICAL MASS

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Detecting the most distant (z>7) objects with ALMA

Cited by 14 publications

References 19 publications

The potential influence of far-infrared emission lines on the selection of high-redshift galaxies

The potential influence of far-infrared emission lines on the selection of high-redshift galaxies

A kiloparsec-scale hyper-starburst in a quasar host less than 1 gigayear after the Big Bang

REDSHIFT 6.4 HOST GALAXIES OF 108SOLAR MASS BLACK HOLES: LOW STAR FORMATION RATE AND DYNAMICAL MASS

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REDSHIFT 6.4 HOST GALAXIES OF 10⁸SOLAR MASS BLACK HOLES: LOW STAR FORMATION RATE AND DYNAMICAL MASS