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 61 publications

(83 citation statements)

References 112 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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%

See 1 more Smart Citation

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

Olsen

Greve

Narayanan

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…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

View full text Add to dashboard Cite

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

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

Cited by 61 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*

Contact Info

Product

Resources

About