J/ApJ/846/105 [CII], [OI] and [OIII] line emission from z∼6 gal. (Olsen+, 2017)

SIGAME simulations of the [CII], [OI] and [OIII] line emission from star-forming galaxies at z∼6. Olsen K., Greve T.R., Narayanan D., Thompson R., Dave R., Rios L.N., Stawinski S. <Astrophys. J., 846, 105 (2017)> =2017ApJ...846..105O 2017ApJ...846..105O
ADC_Keywords: Galaxies, IR ; Redshifts ; Interstellar medium ; Millimetric/submm sources Keywords: cosmology: theory; galaxies: high-redshift; galaxies: ISM; line: formation; methods: numerical; submillimeter: ISM Abstract: Of the almost 40 star-forming galaxies at z≳5 (not counting quasi-stellar objects) observed in [CII] to date, nearly half are either very faint in [CII] or not detected at all, and fall well below expectations based on locally derived relations between star formation rate and [CII] luminosity. This has raised questions as to how reliable [CII] is as a tracer of star formation activity at these epochs and how factors such as metallicity might affect the [CII] emission. Combining cosmological zoom simulations of galaxies with SIGAME (SImulator of GAlaxy Millimeter/submillimeter Emission), we modeled the multiphased interstellar medium (ISM) and its emission in [CII], as well as in [OI] and [OIII], from 30 main-sequence galaxies at z∼6 with star formation rates ∼3-23M/yr, stellar masses ~(0.7-8)x109M, and metallicities ~(0.1-0.4)xZ. The simulations are able to reproduce the aforementioned [CII] faintness of some normal star-forming galaxy sources at z≥5. In terms of [OI] and [OIII], very few observations are available at z≳5, but our simulations match two of the three existing z≳5 detections of [OIII] and are furthermore roughly consistent with the [OI] and [OIII] luminosity relations with star formation rate observed for local starburst galaxies. We find that the [CII] 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 [CII] than the ionized gas, which makes up ∼85% of the total gas mass. A principal component analysis shows that the [CII] 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 [CII] faintness, and we suggest that these factors may also be responsible for the [CII]-faint normal galaxies observed at these early epochs. Description: We use cosmological zoom simulations of galaxies extracted from the MUFASA cosmological simulation (Dave+ 2016MNRAS.462.3265D 2016MNRAS.462.3265D, 2017MNRAS.467..115D 2017MNRAS.467..115D); see section 2. For the purposes of this paper, we updated SIGAME from the version presented in Olsen+ (2015ApJ...814...76O 2015ApJ...814...76O); see section 3. Throughout, we adopt a flat cold dark matter (ΛCDM) cosmology with cosmological parameters ΩΛ=0.7, ΩM=0.3, and h=0.68. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table3.dat 110 37 All [CII] observations in the literature to date of z>5 -------------------------------------------------------------------------------- See also: J/ApJS/178/280 : Compendium of ISO far-IR extragalactic data (Brauher+, 2008) J/ApJ/774/68 : [CII]157.7um feature in LIRGs (Diaz-Santos+, 2013) J/ApJ/820/83 : ALMA galaxy properties in COSMOS field (Scoville+, 2016) J/ApJ/844/171 : Lyα profile in 43 Green Pea galaxies (Yang+, 2017) J/ApJ/845/96 : [CII] emission in the ISM of nearby galaxies (Croxall+, 2017) Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 20 A20 --- Name Name of object 22- 27 F6.4 --- z [5.1/7.7] Spectroscopic redshift 29 A1 --- l_SFR The 3σ upper limit flag on SFR 30- 35 F6.2 Msun/yr SFR [0.4/750] Star Formation Rate (1) 37- 42 F6.2 Msun/yr hiSFR [0.4/376]? High Star Formation Rate (2) 44 A1 --- l_LCII The 3σ upper limit flag on LCII 45- 53 E9.3 Lsun LCII [300000/16200000000] The [CII]157.7um luminosity (3) 55 A1 --- l_Mag The 3σ upper limit flag on Mag 56- 61 F6.2 --- Mag [1/100] Lensing magnification; 1 where not known 63 I1 --- n_SFR [1/4] Note on SFR (4) 65- 90 A26 --- Ref Reference (Author, year) 92-110 A19 --- BibCode Bibcode -------------------------------------------------------------------------------- Note (1): Converted to Chabrier IMF. Note (2): High SFR in cases where two were derived, see flag "2" in n_SFR. Note (3): Corrected for gravitational magnification. Note (4): Note as follows: 1 = SED-based SFR. 2 = Low SFRs are derived from the UV; high SFRs are from the UV combined with an upper limit in the IR. 3 = UV-based SFR. 4 = IR-based SFR. -------------------------------------------------------------------------------- History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 22-May-2018
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