J/A+A/679/A131 ISM of galaxies with FIR emission lines (Ramos Padilla+, 2023)
Diagnosing the interstellar medium of galaxies with far-infrared emission lines.
II. [C II], [O I], [O III], [N II], and [N III] up to z=6.
Ramos Padilla A.F., Wang L., van der Tak F.F.S., Trager S.C.
<Astron. Astrophys. 679, A131 (2023)>
=2023A&A...679A.131R 2023A&A...679A.131R (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, IR; Interstellar medium; Spectra, infrared; Models
Keywords: galaxies: ISM - galaxies: star formation - galaxies: high-redshift -
ISM: lines and bands - ISM: structure - methods: numerical
Abstract:
Gas cooling processes in the interstellar medium (ISM) are key to
understanding how star formation occurs in galaxies. Far-infrared
(FIR) fine-structure emission lines can be used to infer gas
conditions and trace different phases of the ISM.
We model eight of the most important FIR emission lines and explore
their variation with star formation rate (SFR) out to z=6 using
cosmological hydrodynamical simulations. In addition, we study how
different physical parameters, such as the interstellar radiation
field (ISRF) and metallicity, impact the FIR lines and line ratios. We
implemented a physically motivated multi-phase model of the ISM by
post-processing the EAGLE cosmological simulation and using Cloudy
look-up tables for line emissivities. In this model we included four
phases of the ISM: dense molecular gas, neutral atomic gas, diffuse
ionised gas (DIG), and Hii regions.
Our model shows reasonable agreement (to ∼0.5dex) with the observed
line luminosity-SFR relations up to z=6 in the FIR lines analysed. For
ease of comparison, we also provide linear fits to our model results.
Our predictions also agree reasonably well with observations in
diagnostic diagrams involving various FIR line ratios. We find that
[CII] is the best SFR tracer of the FIR lines even though it arises
from multiple ISM phases, while [OIII] and [NII] can be used to
understand the DIG-HII balance in the ionised gas. In addition, line
ratios such as [CII]/[OIII] and [NII]/[OI] are useful for deriving
parameters such as ISRF, metallicity, and specific SFR. These results
can help interpret the observations of the FIR lines from the local
Universe to high redshifts.
Description:
We present the estimations of the FIR line luminosities for the
simulated galaxies in EAGLE. These are presented as an example in
tables B1 and B2 of the paper. In addition, we include the
supplementary material of the galaxies and references used to compare
these results with observations from different works. The rest of the
supplementary material are located in the Zenodo repository
(https://doi.org/10.5281/zenodo.6576202).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
dataset.dat 490 8274 Line luminosity estimates and physical parameters
dataset derived from this work (Tables B1 and B2)
sample.dat 393 1702 Galaxies and references used to compare these
results with observations from different works
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See also:
https://doi.org/10.5281/zenodo.6576202 : supplementary data
Byte-by-byte Description of file: dataset.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- ID Group Number in EAGLE simulation
7- 12 A6 --- Sim [Recal Ref100] Name of EAGLE simulation
14 I1 --- z Redshift snapshot
16- 22 F7.5 Lsun L[OIII52] Total luminosity [OIII] at 52um
24- 30 F7.5 Lsun L[OIII52]DIG DIG luminosity [OIII] at 52um
32- 39 F8.5 Lsun L[OIII52]HII ?=- HII luminosity [OIII] at 52um
41- 48 F8.5 Lsun L[OIII52]ato ?=- Atomic luminosity [OIII] at 52um
50- 57 F8.5 Lsun L[OIII52]mol ?=- Molecular luminosity [OIII] at 52um
59- 65 F7.5 Lsun L[NIII57] Total luminosity [NIII] at 57um
67- 73 F7.5 Lsun L[NIII57]DIG DIG luminosity [NIII] at 57um
75- 82 F8.5 Lsun L[NIII57]HII ?=- HII luminosity [NIII] at 57um
84- 91 F8.5 Lsun L[NIII57]ato ?=- Atomic luminosity [NIII] at 57um
93-100 F8.5 Lsun L[NIII57]mol ?=- Molecular luminosity [NIII] at 57um
102-108 F7.5 Lsun L[OI63] Total luminosity [OI] at 63um
110-117 F8.5 Lsun L[OI63]DIG DIG luminosity [OI] at 63um
119-126 F8.5 Lsun L[OI63]HII ?=- HII luminosity [OI] at 63um
128-135 F8.5 Lsun L[OI63]ato ?=- Atomic luminosity [OI] at 63um
137-144 F8.5 Lsun L[OI63]mol ?=- Molecular luminosity [OI] at 63um
146-152 F7.5 Lsun L[OIII88] Total luminosity [OIII] at 88um
154-160 F7.5 Lsun L[OIII88]DIG DIG luminosity [OIII] at 88um
162-169 F8.5 Lsun L[OIII88]HII ?=- HII luminosity [OIII] at 88um
171-178 F8.5 Lsun L[OIII88]ato ?=- Atomic luminosity [OIII] at 88um
180-187 F8.5 Lsun L[OIII88]mol ?=- Molecular luminosity [OIII] at 88um
189-195 F7.5 Lsun L[NII122] Total luminosity [NII] at 122um
197-203 F7.5 Lsun L[NII122]DIG DIG luminosity [NII] at 122um
205-212 F8.5 Lsun L[NII122]HII ?=- HII luminosity [NII] at 122um
214-221 F8.5 Lsun L[NII122]ato ?=- Atomic luminosity [NII] at 122um
223-230 F8.5 Lsun L[NII122]mol ?=- Molecular luminosity [NII] at 122um
232-239 F8.5 Lsun L[OI145] Total luminosity [OI] at 145um
241-248 F8.5 Lsun L[OI145]DIG DIG luminosity [OI] at 145um
250-257 F8.5 Lsun L[OI145]HII ?=- HII luminosity [OI] at 145um
259-266 F8.5 Lsun L[OI145]ato ?=- Atomic luminosity [OI] at 145um
268-275 F8.5 Lsun L[OI145]mol ?=- Molecular luminosity [OI] at 145um
277-283 F7.5 Lsun L[CII] Total luminosity [CII] at 158um
285-291 F7.5 Lsun L[CII]DIG DIG luminosity [CII] at 158um
293-300 F8.5 Lsun L[CII]HII ?=- HII luminosity [CII] at 158um
302-309 F8.5 Lsun L[CII]ato ?=- Atomic luminosity [CII] at 158um
311-318 F8.5 Lsun L[CII]mol ?=- Molecular luminosity [CII] at 158um
320-326 F7.5 Lsun L[NII205] Total luminosity [NII] at 205um
328-334 F7.5 Lsun L[NII205]DIG DIG luminosity [NII] at 205um
336-343 F8.5 Lsun L[NII205]HII ?=- HII luminosity [NII] at 205um
345-352 F8.5 Lsun L[NII205]ato ?=- Atomic luminosity [NII] at 205um
354-361 F8.5 Lsun L[NII205]mol ?=- Molecular luminosity [NII] at 205um
363-370 F8.5 Msun Mstellar Stellar mass
372-379 F8.5 Msun Mgas Gas mass
381-388 F8.5 Msun Mneutral Neutral gas mass
390-397 F8.5 Gyr Agestellar Stellar age
399-406 F8.5 [s-1] logQ ?=- log ionising photon flux
408-416 F9.6 --- ISRF Interstellar radiation field (Habing)
418-425 F8.5 Msun/yr SFR Star formation rate
427-434 F8.5 Sun ZGal Metallicity (Z/Zsun)
436-443 F8.5 K/cm3 Pressure External pressure
445-453 F9.6 cm-3 nHcloud Total hydrogen number density in the
neutral clouds
455-462 F8.6 pc RCI Radius of neutral carbon
464-471 F8.6 pc Rcloud Radius of the neutral clouds
473-481 F9.6 pc RH2 ?=- Radius dense molecular gas
483-490 F8.6 --- fH2 ?=- Molecular H2 fraction
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Byte-by-byte Description of file: sample.dat
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Bytes Format Units Label Explanations
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1- 41 A41 --- Name Name of the galaxy
43- 81 A39 --- SName Name of the galaxy in SIMBAD
83- 84 I2 h RAh Right ascension (J2000)
86- 87 I2 min RAm Right ascension (J2000)
89- 95 F7.4 s RAs Right ascension (J2000)
97 A1 --- DE- Declination sign (J2000)
98- 99 I2 deg DEd Declination (J2000)
101-102 I2 arcmin DEm Declination (J2000)
104-109 F6.3 arcsec DEs Declination (J2000)
111-129 A19 --- Ref Reference bibcode
131-136 F6.4 --- z Redshift
138-151 A14 --- Type SIMBAD Type (Object type)
153-163 F11.6 Msun/yr SFR ?=- Star formation rate
165-169 F5.1 Msun/yr e_SFR ?=- Star formation rate error
171-178 F8.6 --- l_SFR [0/1] Limit in Star formation rate
180-190 E11.6 Msun Mstar ?=- Stellar mass
192-202 E11.6 Msun e_Mstar ?=- Stellar mass error
204 I1 --- l_Mstar [0/1] Limit in stellar mass
206-209 F4.2 [-] Metal ?=- Metallicity
211-215 F5.3 [-] e_Metal ?=- Metallicity error
217 I1 --- l_Metal [0/1] Limit in metallicity
219-223 F5.2 --- mu ?=- Magnification factor
225-230 F6.3 --- e_mu ?=- Magnification factor error
232 I1 --- l_mu [0/1] Limit in magnification factor
234 I1 --- f_mu [0/1] Flag magnification factor
236-246 E11.6 Lsun LOIII52 ?=- Luminosity of [OIII] at 52um
248-250 A3 Lsun e_LOIII52 [-] Luminosity error of [OIII] at 52um
252 I1 --- l_LOIII52 [0/1] Limit in luminosity of [OIII] at 52um
254-264 E11.6 Lsun LNIII57 ?=- Luminosity of [NIII] at 57um
266-268 A3 Lsun e_LNIII57 [-] Luminosity error of [NIII] at 57um
270 I1 --- l_LNIII57 [0/1] Limit in luminosity of [NIII] at 57um
272-282 E11.6 Lsun LOI63 ?=- Luminosity of [OI] at 63um
284-293 I10 Lsun e_LOI63 ?=- Luminosity error of [OI] at 63um
295 I1 --- l_LOI63 [0/1] Limit in luminosity of [OI] at 63um
297-307 E11.6 Lsun LOIII88 ?=- Luminosity of [OIII] at 88um
309-311 A3 Lsun e_LOIII88 [-] Luminosity error of [OIII] at 88um
313 I1 --- l_LOIII88 [0/1] Limit in luminosity of [OIII] at 88um
315-325 E11.6 Lsun LNII122 ?=- Luminosity of [NII] at 122um
327-329 A3 Lsun e_LNII122 [-] Luminosity error of [NII] at 122um
331 I1 --- l_LNII122 [0/1] Limit in luminosity of [NII] at 122um
333-343 E11.6 Lsun LOI145 ?=- Luminosity of [OI] at 145um
345-347 A3 Lsun e_LOI145 [-] Luminosity error of [OI] at 145um
349 I1 --- l_LOI145 [0/1] Limit in luminosity of [OI] at 145um
351-361 E11.6 Lsun LCII ?=- Luminosity of [CII] at 158um
363-373 E11.6 Lsun e_LCII ?=- Luminosity error of [CII] at 158um
375 I1 --- l_LCII [0/1] Limit in luminosity of [CII] at 158um
377-387 E11.6 Lsun LNII205 ?=- Luminosity of [NII] at 205um
389-391 A3 Lsun e_LNII205 [-] Luminosity error of [NII] at 205um
393 I1 --- l_LNII205 [0/1] Limit in luminosity of [NII] at 205um
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Acknowledgements:
Andres Felipe Ramos Padilla, andresrp25(at)gmail.com
References:
Ramos Padilla, Paper I 2021A&A...645A.133R 2021A&A...645A.133R
(End) Patricia Vannier [CDS] 25-Oct-2023