SIMULATOR OF GALAXY MILLIMETER/SUBMILLIMETER EMISSION (SÍGAME): THE [C ii]–SFR RELATIONSHIP OF MASSIVE<i>z</i>= 2 MAIN SEQUENCE GALAXIES

Olsen, Karen P.; Greve, T. R.; Narayanan, Desika; Thompson, Raymond H.; Toft, Sune; Brinch, Christian

doi:10.1088/0004-637x/814/1/76

Cited by 62 publications

(83 citation statements)

References 112 publications

(228 reference statements)

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“…The GMC sizes (R GMC ) are derived from a pressure-normalized mass-size relation (Olsen et al 2015), which results in cloud radii in the range 5.8 to 43.6 pc (Fig. 3).…”

Section: Cosmological Galaxy Formation Simulationsmentioning

confidence: 99%

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

Olsen

Greve

Narayanan

et al. 2017

ApJ

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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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“…The GMC sizes (R GMC ) are derived from a pressure-normalized mass-size relation (Olsen et al 2015), which results in cloud radii in the range 5.8 to 43.6 pc (Fig. 3).…”

Section: Cosmological Galaxy Formation Simulationsmentioning

confidence: 99%

“…For the diffuse clouds we exclude turbulence by setting it to 0 km s −1 , after a test showed that setting the turbulence to 10 km s −1 only decreases the [C II] luminosities by on average 0.07 dex. For the GMCs we use the velocity dispersion obtainable from the cloud radius and pressure (see Olsen et al 2015).…”

Section: Gas Kinetic Temperaturementioning

confidence: 99%

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

Olsen

Greve

Narayanan

et al. 2017

ApJ

Self Cite

103

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“…In our work we did not take the contribution from ionised regions to the [CII] emission of galaxies into account. Olsen et al (2015b) applied a radiative transfer code to seven modeled main-sequence galaxies at z = 2. The authors compute the contribution to the total [CII] emission from PDRs, atomic, and ionised regions and found that the [CII] emission from ionised regions only accounts for a few percent of the total [CII] luminosity.…”

Section: [Cii] Emission From Ionised Regionsmentioning

confidence: 99%

Sub-mm emission line deep fields: CO and [C ii] luminosity functions out toz= 6

Popping

Kampen

Decarli

et al. 2016

Mon. Not. R. Astron. Soc.

114

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Now that ALMA is reaching its full capabilities, observations of sub-mm emission line deep fields become feasible. We couple a semi-analytic model of galaxy formation with a radiative transfer code to make predictions for the luminosity function of CO J=1-0 out to CO J=6-5 and [CII] at redshifts z=0-6. We find that: 1) our model correctly reproduces the CO and [CII] emission of low-and high-redshift galaxies and reproduces the available constraints on the CO luminosity function at z 2.75; 2) we find that the CO and [CII] luminosity functions of galaxies increase from z = 6 to z = 4, remain relatively constant till z = 1 and rapidly decrease towards z = 0. The galaxies that are brightest in CO and [CII] are found at z ∼ 2; 3) the CO J=3-2 emission line is most favourable to study the CO luminosity and global H 2 mass content of galaxies, because of its brightness and observability with currently available sub-mm and radio instruments; 4) the luminosity functions of high-J CO lines show stronger evolution than the luminosity functions of low-J CO lines; 5) our model barely reproduces the available constraints on the CO and [CII] luminosity function of galaxies at z 1.5 and the CO luminosity of individual galaxies at intermediate redshifts. We argue that this is driven by a lack of cold gas in galaxies at intermediate redshifts as predicted by cosmological simulations of galaxy formation.

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“…From the theoretical side, the issue of non-detections has been studied, e.g., by Vallini et al (2015), Olsen et al (2015), and Narayanan & Krumholz (2016). Both Vallini et al (2015) and Olsen et al (2015) conclude that in high-z galaxies the [C II] emission arises predominately from photodissociation regions.…”

Section: Introductionmentioning

confidence: 99%

ALMA [C ii] 158 μm Detection of a Redshift 7 Lensed Galaxy behind RX J1347.1−1145*

Bradač

Garcia‐Appadoo

Huang

et al. 2017

ApJL

107

129

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We present the results of ALMA spectroscopic follow-up of a z=6.766 Lyα emitting galaxy behind the cluster RX J1347.1−1145. We report the detection of [C II] 158 μm line fully consistent with the Lyα redshift and with the peak of the optical emission. Given the magnification of μ=5.0±0.3, the intrinsic (corrected for lensing) luminosity of the, roughly ∼5 times fainter than other detections of z∼7 galaxies. The result indicates that low L [C II] in z∼7 galaxies compared to the local counterparts might be caused by their low metallicities and/or feedback. ) between the Lyα and [C II] line is unusual, and may be indicative of ionizing photons escaping.

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SIMULATOR OF GALAXY MILLIMETER/SUBMILLIMETER EMISSION (SÍGAME): THE [C ii]–SFR RELATIONSHIP OF MASSIVEz= 2 MAIN SEQUENCE GALAXIES

Cited by 62 publications

References 112 publications

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

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

Sub-mm emission line deep fields: CO and [C ii] luminosity functions out toz= 6

ALMA [C ii] 158 μm Detection of a Redshift 7 Lensed Galaxy behind RX J1347.1−1145*

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