Star formation in galaxies is traced by the presence of
emission lines, produced by the ionized gas surrounding
young star clusters.
In particular, hydrogen (H) recombination lines intensity is a direct measure
of the number of massive stars still alive. Thus, emission lines are important
tracers of the current star formation rate (SFR).
These regions are often embedded into dusty environments,
and the effects of dust may be significant. Therefore, It is fundamental to model the
nebular emission within a context
that takes into account star-light reprocessing by dust.
For this reason I implemented the modelling of nebular emission by HII regions
into GRASIL that was originally developed
to simulate the spectral energy distribution (SED) of dusty galaxies.
The implementation is based on a pre-computed library of HII region emission models.
The library of HII region emission models provides the emission line luminosities for a given ionizing stellar population. It can be used in other spectrophotometric codes. You can freely download the library and use it in your code. Please acknowledge if you use this library for a publication.
You can find a description of the model in this paper, (2003, A&A, 409, 99). A more detailed description of the HII region model will be aviable in the near future.
The library provides the
emission line luminosities as a function of:
density | filling factor | name | density | filling factor | name |
10 | 1.0 | hii_d10f10.dat.gz | 30 | 1.0 | hii_d30f10.dat.gz |
10 | 0.1 | hii_d10f01.dat.gz | 30 | 0.1 | hii_d30f01.dat.gz |
10 | 0.01 | hii_d10f001.dat.gz | 30 | 0.01 | hii_d30f001.dat.gz |
100 | 1.0 | hii_d100f10.dat.gz | 300 | 1.0 | hii_d300f10.dat.gz |
100 | 0.1 | hii_d100f01.dat.gz | 300 | 0.1 | hii_d300f01.dat.gz |
100 | 0.01 | hii_d100f001.dat.gz | 300 | 0.01 | hii_d300f001.dat.gz |
1000 | 1.0 | hii_d1000f10.dat.gz | 3000 | 0.1 | hii_d3000f01.dat.gz |
1000 | 0.1 | hii_d1000f01.dat.gz | 3000 | 0.01 | hii_d3000f001.dat.gz |
1000 | 0.01 | hii_d1000f001.dat.gz | 3000 | 0.001 | hii_d3000f0001.dat.gz |
10000 | 0.1 | hii_d10000f01.dat.gz | |||
10000 | 0.01 | hii_d10000f001.dat.gz | |||
10000 | 0.001 | hii_d10000f0001.dat.gz |
The HII region models are computed for different values of metallicity, namely:
Zgas=0.0008, 0.004, 0.008, 0.015, 0.02, 0.03, 0.04, 0.05,
where 0.02 means solar metallicity.
The space of Q parameters is divided into two grids, identified by a grid index. In the first grid, with index number equal 1, QHe/QH is > 0.05; in the second (grid index = 2) QHe/QH is < 0.05.
In grid number 1, QHe/QH=0.05+0.05625*i with i=0,...,8; QO/QHe=0.13+0.1*j with j=0,...,5.
In grid 2, QHe/QH=0.05, 0.025, 0.01, 0.005, 0.0025, 0.0001, 0.; while QO/QHe=0.+0.1*j with j=0,...,4.
In both the grids, QH=1046+0.2*k with k=0,...,30.
The first line is an header; each following line correspond to an HII
region model.
This is an example of the first two lines of a library file (namely hii_d10f01.dat):
#density= 10.00 filling= 0.100 1)name 2)numgrid 3)zeta 4)lum 5)shi 6)sx 7)shei 8)so 9-135)intfluxline bZ01H01E01O01 1 .0008 38.622 -2.0000 -2.4590 -3.3010 -4.1871 664505961859289591245900558898587045865964200631....
Bytes | Format | Description |
1 - 13 | A13 | Name of the model: bytes 1-13 are a string that identify the name of the input file for CLOUDY. |
15 | I1 | Grid index |
17 - 21 | F5.4 | Metallicity |
23 - 28 | F6.3 | Log of the luminosity of analytical spectrum in erg/s |
30 - 37 | F8.4 | Log(QH/1050 photons/second) |
39 - 46 | F8.4 | Log(QX/1050): QX is the number of photons per second with a wavelength shorter than 750 Å |
48 - 55 | F8.4 | Log(QHe/1050) |
57 - 64 | F8.4 | Log(QO/1050) |
66 - 636 | 114I5 | Line luminosity |
In the following table there is the list of the computed lines. The order is the same that you can find in the library files.
1: Ly alpha 1216 | 2: Ly beta 1025 | 3: Ly gamma 972 | 4: Ly delta 949 | 5: Ly 937 | 6: Ly 930 | 7: Ly 926 | 8: Ly 922 |
9: H alpha 6563 | 10: H beta 4861 | 11: H gamma 4340 | 12: H delta 4102 | 13: H 3970 | 14: H 3889 | 15: H 3835 | 16: H 3798 |
17: Pa alpha 18752 | 18: Pa beta 12819 | 19: Pa gamma 10939 | 20: Pa delta 10050 | 21: Pa 9546 | 22: Pa 9229 | 23: Pa 9015 | 24: Pa 8863 |
25: Br alpha 40515 | 26: Br beta 26254 | 27: Br gamma 21657 | 28: Br delta 19447 | 29: Br 18175 | 30: Br 17363 | 31: Br 16808 | 32: Br 16408 |
33: Pf alpha 74585 | 34: Pf beta 46529 | 35: Pf gamma 37398 | 36: Pf delta 32964 | 37: Pf 30386 | 38: Pf 28724 | 39: Pf 27577 | 40: Pf 26746 |
41: Hu alpha 12.4µm | 42: Hu beta 75011 | 43: Hu gamma 59071 | 44: Hu delta 51277 | 45: Hu 46716 | 46: Hu 43756 | 47: Hu 41700 | 48: Hu 40201 |
49: HeI 4472 | 50: HeI 5877 | 51: HeI 6680 | 52: HeI 10833 | 53: HeI 3889 | 54: HeI 7065 | 55: [CI]9850 | 56: [CI]8727 |
57: [CI]4621 | 58: [CI]610µm | 59: [CI]369µm | 60: [CII]157.7µm | 61: CII]2326 | 62: [NI]5200 | 63: [NI]3467 | 64: [NI]10405 |
65: [NII]6585 | 66: [NII]6549 | 67: [NII]5756 | 68: [NII]122µm | 69: [NII]205µm | 70: NII]2141 | 71: [NIII]57µm | 72: [OI]6302 |
73: [OI]6365 | 74: [OI]5578 | 75: [OI]63µm | 76: [OI]145µm | 77: [OII]3727 | 78: [OII]7327 | 79: [OII]2471 | 80: OIII]1663 |
81: [OIII]5007 | 82: [OIII]4960 | 83: [OIII]4364 | 84: [OIII]2321 | 85: [OIII]88µm | 86: [OIII]52µm | 87: [NeII]12.8µm | 88: [NeIII]15.5µm |
89: [NeIII]36µm | 90: [NeIII]3870 | 91: [NeIII]3968 | 92: [NeIII]3343 | 93: [NeIII]1815 | 94: MgII 2800 | 95: [SiII]35µm | 96: [SII]10331 |
97: [SII]6732 | 98: [SII]6717 | 99: [SII]4070 | 100: [SII]4078 | 101: [SIII]18.7µm | 102: [SIII]33.5µm | 103: [SIII]9533 | 104: [SIII]9071 |
105: [SIII]6314 | 106: [SIII]3723 | 107: [SIV]10.5µm | 108: [ArII]7µm | 109: [ArIII]7138 | 110: [ArIII]7753 | 111: [ArIII]5193 | 112: [ArIII]3110 |
113: [ArIII]22µm | 114: [ArIII]9µm |
Send me an email at pasquale dot panuzzo at cea dot fr!