PAH emission: Dependence on Starlight Spectrum, Intensity, PAH Size Distribution, and PAH Ionization|天体物理学数据集|多环芳烃数据集

Excitation of PAH Emission: Dependence on Starlight Spectrum, Intensity, PAH Size Distribution, and PAH Ionizations The emission spectra provided here are from the paper \"Excitation of PAH Emission: Dependence on Starlight Spectrum, Intensity, PAH Size Distribution, and PAH Ionization\" (Draine, Li, Hensley, Hunt, Sandstrom, & Smith 2021, Astrophysical Journal, in press). Please cite that paper if you use these data. Preprint available at https://arxiv.org/abs/2011.07046 We consider 14 different radiation spectra: mmpisrf : mMMP spectrum (see Draine, Li, Hensley et al 2021) bc03_z0.02_3e6 : BC03 3 Myr old stellar population with Z=0.02 bc03_z0.0004_1e7 : BC03 10 Myr old stellar population with Z=0.0004 bc03_z0.02_1e7 : BC03 10 Myr old stellar population with Z=0.02 bc03_z0.02_1e8 : BC03 100 Myr old stellar population with Z=0.02 bc03_z0.02_3e8 : BC03 300 Myr old stellar population with Z=0.02 bc03_z0.02_1e9 : BC03 1 Gyr old stellar population with Z=0.02 bpass_z0.02_3e6 : BPASS 3 Myr old stellar population with Z=0.02 bpass_z0.001_1e7 : BPASS 10 Myr old stellar population with Z=0.001 bpass_z0.02_1e7 : BPASS 10 Myr old stellar population with Z=0.02 bpass_z0.02_1e8 : BPASS 100 Myr old stellar population with Z=0.02 bpass_z0.02_3e8 : BPASS 300 Myr old stellar population with Z=0.02 bpass_z0.02_1e9 : BPASS 1 Gyr old stellar population with Z=0.02 m31blge : M31 bulge spectrum Note: The mMMP (\"modified Mathis, Mezger & Panagia\") spectrum is based on Mathis, Mezger & Panagia (1983), with parameters modified as described in Draine (2011). The BC03 model spectra for single-age stellar populations are from Bruzual & Charlot (2003) The BPASS model spectra for single-age stellar populations with binary evolution are from Eldridge et al. (2017) and Stanway & Eldridge (2018) The M31 bulge spectrum uses the spectrum obtained by Groves et al. (2012) for the bulge of M31. The above spectra are all shown in Figure 1 of Draine, Li, Hensley et al (2021). Each spectrum (for intensity parameter U=1) is included in a file in the appropriate library (see below). We calculate heating of dust grains, and resulting infrared emission, for each of the above radiation fields, for selected values of the dimensionless intensity scaling parameter U, where U=1 corresponds to an intensity such that a \"standard grain\" (taken to be an 1.6:1 oblate spheroid of \"astrodust\" with a_eff=0.10um, b/a=1.6, and porosity P=0.2) is heated at the same rate as in the modified MMP estimate for the starlight intensity in the solar neighborhood [see Draine (2011) or Draine, Li, Hensley et al (2021) for discussion of the mMMP spectrum]. The PAH properties are almost identical to the model of Draine & Li (2007), but with some small adjusts in bandstrengths for features at 14.19um, 17.04um, 17.375um, and 17.87um (see Draine, Li, Hensley et al (2021). For the properties of \"astrodust\", see Draine & Hensley (2021). We also calculate heating of dust grains, and resulting infrared emission, for dust distributed in a \"slab\" of total thickness A_V = 2 mag. The radiation incident on the cloud surface is assumed to be from one of the above-listed spectra, with an intensity at the cloud surface characterized by the scaling parameter U. The cloud is illuminated on one side only. The dust slab is divided into 20 zones, with the radiation attenuated and reddened as it propagates into the cloud, as described in Draine, Li, Hensley et al (2021). Results are presented for values of lgU = log10(U) = 0.00, 0.50, 1.00, ..., 6.50, 7.00 The results for each of the different spectra are located in different libraries. We provide gzipped tarfiles containing complete results for each of the starlight models: mMMP.tgz BC03_Z0.02_3Myr.tgz BC03_Z0.0004_10Myr.tgz BC03_Z0.02_10Myr.tgz BC03_Z0.02_100Myr.tgz BC03_Z0.02_300Myr.tgz BC03_Z0.02_1Gyr.tgz BPASS_Z0.02_3Myr.tgz BPASS_Z0.001_10Myr.tgz BPASS_Z0.02_10Myr.tgz BPASS_Z0.02_100Myr.tgz BPASS_Z0.02_300Myr.tgz BPASS_Z0.02_1Gyr.tgz m31bulge.tgz We also provide libraries for models with starlight incident on a cloud with A_V=2mag of extinction: mMMP_slab.tgz BC03_Z0.02_3Myr_slab.tgz BC03_Z0.0004_10Myr_slab.tgz BC03_Z0.02_10Myr_slab.tgz BC03_Z0.02_100Myr_slab.tgz BC03_Z0.02_300Myr_slab.tgz BC03_Z0.02_1Gyr_slab.tgz BPASS_Z0.02_3Myr_slab.tgz BPASS_Z0.001_10Myr_slab.tgz BPASS_Z0.02_10Myr_slab.tgz BPASS_Z0.02_100Myr_slab.tgz BPASS_Z0.02_300Myr_slab.tgz BPASS_Z0.02_1Gyr_slab.tgz m31bulge_slab.tgz Each library contains files of four different types: Emission spectra for selected radiation fields, PAH size distributions, and PAH ionizations, e.g., the mMMP library includes pahspec.out_mmpisrf_0.00_st_std.gz : mMMP starlight with lgU=0.00, \"standard\" PAH ionization (\"st\"), and \"standard\" PAH size distribution (\"std\") pahspec.out_mmpisrf_0.00_st_sma.gz : mMMP starlight with lgU=0.00, standard PAH ionization (\"st\"), and \"small\" PAH size distribution (\"sma\") pahspec.out_mmpisrf_0.00_st_lrg.gz : mMMP starlight with lgU=0.00, standard PAH ionization (\"st\"), and \"large\" PAH size distribution (\"lrg\") pahspec.out_mmpisrf_0.00_hi_std.gz : mMMP starlight with lgU=0.00, \"high\" PAH ionization (\"hi\"), and \"standard\" PAH size distribution (\"std\") pahspec.out_mmpisrf_0.00_hi_sma.gz : mMMP starlight with lgU=0.00, \"high\" PAH ionization (\"hi\"), and \"small\" PAH size distribution (\"sma\") pahspec.out_mmpisrf_0.00_hi_lrg.gz : mMMP starlight with lgU=0.00, \"high\" PAH ionization (\"hi\"), and \"large\" PAH size distribution (\"lrg\") pahspec.out_mmpisrf_0.00_lo_std.gz : mMMP starlight with lgU=0.00, \"low\" PAH ionization (\"lo\"), and \"standard\" PAH size distribution (\"std\") pahspec.out_mmpisrf_0.00_lo_sma.gz : mMMP starlight with lgU=0.00, \"low\" PAH ionization (\"lo\"), and \"small\" PAH size distribution (\"sma\") pahspec.out_mmpisrf_0.00_lo_lrg.gz : mMMP starlight with lgU=0.00, \"low\" PAH ionization (\"lo\"), and \"large\" PAH size distribution (\"lrg\") Emission spectra for individual dust grains, heated by selected radiation fields and intensities, e.g., iout_graD16emtPAHib_mmpisrf_0.00.gz : PAH^+ particles of different sizes, heated by mMMP radiation spectrum with lgU=0.00 iout_graD16emtPAHnb_mmpisrf_0.00.gz : PAH^0 particles of different sizes, heated by mMMP radiation spectrum with lgU=0.00 iout_DH21Ad_P0.20_0.00_mmpisrf_0.00.gz : DH21 astrodust with porosity 0.20, oblate spheroids with b/a=1.6: particles of different sizes, heated by mMMP radiation spectrum with lgU=0.00 Starlight spectra used in the calculations, e.g., isrf_mmpisrf_0.00.gz : mMMP starlight spectrum with lgU=0.00 Grain sizes, and abundance for each size, for Astrodust, PAH+, and PAH0 used in the calculations, e.g., pahspec_dnda.out_st_std : \"standard\" ionization and \"standard\" PAH size distribution pahspec_dnda.out_st_sma : \"standard\" ionization and \"small\" PAH size distribution pahspec_dnda.out_st_lrg : \"standard\" ionization and \"large\" PAH size distribution pahspec_dnda.out_hi_std : \"high\" ionization and \"standard\" PAH size distribution pahspec_dnda.out_hi_sma : \"high\" ionization and \"small\" PAH size distribution pahspec_dnda.out_hi_lrg : \"high\" ionization and \"large\" PAH size distribution pahspec_dnda.out_lo_std : \"low\" ionization and \"standard\" PAH size distribution pahspec_dnda.out_lo_sma : \"low\" ionization and \"small\" PAH size distribution pahspec_dnda.out_lo_lrg : \"low\" ionization and \"large\" PAH size distribution References: Bruzual, G, & Charlot, S. 2003, MNRAS, 344, 1000 Draine, B.T. 2011, Physics of the Interstellar and Intergalactic Medium (Princeton: Princeton University Press) Draine, B.T., & Hensley, B.S. 2021, ApJ, 909:94 Draine, B.T., & Li, A. 2007, ApJ, 657, 810 Draine, B.T., Li, A., Hensley, B.S., Hunt, L.K., Sandstrom, K., and Smith, J.-D.T 2021, ApJ, in press, https://ui.adsabs.harvard.edu/abs/2020arXiv201107046D/abstract Eldridge, J.J., Stanway, E.R., Xiao, L., et al. 2017, PASA, 34, e058 Groves, B., Krause, O., Sandstrom, K. et al. 2012, MNRAS, 426, 892 Mathis, J.S., Mezger, P.G., & Panagia, N. 1983, A&A, 128, 212 Stanway, E.R., & Eldridge, J.J. 2018, MNRAS, 479, 75 Description of files: 1. Emission Spectra for Individual Grain sizes: Filenames: iout_dusttype_startype_lgU.gz iout_dusttype_startype_lgU_slab.gz where dusttype = graD16emtPAHib for PAH ions graD16emtPAHnb for PAH neutrals DH21Ad_P0.20_0.00 for DH21 Astrodust, P=0.20, f_Fe=0 startype = mmpisrf : mMMP spectrum (see Draine, Li, Hensley et al 2021) bc03_z0.02_3e6 : BC03 3 Myr old stellar population with Z=0.02 bc03_z0.0004_1e7 : BC03 10 Myr old stellar population with Z=0.0004 bc03_z0.02_1e7 : BC03 10 Myr old stellar population with Z=0.02 bc03_z0.02_1e8 : BC03 100 Myr old stellar population with Z=0.02 bc03_z0.02_3e8 : BC03 300 Myr old stellar population with Z=0.02 bc03_z0.02_1e9 : BC03 1 Gyr old stellar population with Z=0.02 bpass_z0.02_3e6 : BPASS 3 Myr old stellar population with Z=0.02 bpass_z0.001_1e7 : BPASS 10 Myr old stellar population with Z=0.001 bpass_z0.02_1e7 : BPASS 10 Myr old stellar population with Z=0.02 bpass_z0.02_1e8 : BPASS 100 Myr old stellar population with Z=0.02 bpass_z0.02_3e8 : BPASS 300 Myr old stellar population with Z=0.02 bpass_z0.02_1e9 : BPASS 1 Gyr old stellar population with Z=0.02 m31blge : M31 bulge spectrum lgU = log_10(U) = 0.00 0.50 1.00 1.50 2.00 2.50 3.00 3.50 4.00 4.50 5.00 5.50 6.00 6.50 7.00 file structure for N = 1 - 167 [a = 3.548e-8 cm to 5.012e-4 cm] in 40 steps per decade in particle radius: lines 1-3 : comments line 4 + (N-1)*2511 : description of starlight spectrum line 5: (N-1)*2511 :blank line 6 + (N-1)*2511 : a(cm) = 10.**(-7.45+0.025*(N-1)) lines 7-14 + (N-1)*2511 : comments lines 15-2514 + (N-1)*2511: column 1: lambda (um) column 2: nu * P_nu (erg s-1) [P_nu = time-averaged power per unit frequency for one particle] column 3: C_abs (cm2) [absorption cross section for one particle] 2. Emission Spectra Summed over Simple Dust Model for a Single U, for Dust Abundance per H Appropriate for the Local Diffuse ISM: Filenames: pahspec.out_startype_lgU_fion_fsize.gz pahspec.out_startype_lgU_slab_fion_fsize.gz where startype is as above fion = lo, st, hi for low, standard, high f_ion fsize = sma, std, lrg for small, standard, large size distribution file structure: line 1: description of radiation field line 2: TIR power radiated by Astrodust (erg s-1 per H) line 3: TIR power radiated by PAH^+ (erg s-1 per H) line 4: TIR power radiated by PAH^0 (erg s-1 per H) line 5: total TIR power radiated (erg s-1 per H) lines 6-7: comments lines 8-1980: (1973 wavelengths from 1.0056 um to 8000um) column 1: wave (um) column 2: nu*P_nu (total) (erg s-1 per H) [P_nu=power radiated per unit frquency per H] column 3: nu*P_nu (Astrodust only) (erg s-1 per H) column 4: nu*P_nu (PAH^+ only) (erg s-1 per H) column 5: nu*P_nu (PAH^- only) (erg s-1 per H) 3. PAH Ionization and Size Distributions Used in Computing pahspec.out: Filenames: pahspec_dnda.out_fion_fsize where fion = lo, st, hi for low, standard, or high PAH ionization fsize = sma, std, lrg for small, standard, large PAH size distribution file structure: lines 1-3: comments lines 4-170: column 1: a_eff (um) column 2: dn_Ad = astrodust number per H in this bin column 3: dn_PAH+ = PAH^+ number per H in this bin column 4: dn_PAH0 = PAH^0 number per H in this bin 4. Unreddened Starlight Spectra Used in Calculations for U = 1 : Filenames: isrf_startype_0.00.gz where startype is as above file structure: line 1: comments line 2: U line 3: u = u_starlight+u_CMB = photon energy density (erg cm-3) line 4: u_starlight = starlight energy density (erg cm-3) line 5: < h nu > = mean photon energy (eV) [including CMB photons] line 6-7: comments lines 8-2507: column 1: lambda (um) column 2: lambda*u_lambda (erg cm-3)