Issue 
A&A
Volume 564, April 2014



Article Number  A111  
Number of page(s)  5  
Section  Interstellar and circumstellar matter  
DOI  https://doi.org/10.1051/00046361/201322723  
Published online  15 April 2014 
Dust temperature maps of the Galactic plane: The Herschel spectral energy distribution fitting with Cloudy predictions^{⋆,}^{⋆⋆}
^{1}
National Astronomical Observatories,
20A Datun Road, Chaoyang District,
100012
Beijing,
PR China
email:
mhuang@nao.cas.cn
^{2}
University of Chinese Academy of Sciences,
100049
Beijing, PR
China
Received:
21
September
2013
Accepted:
11
February
2014
Context. Dust grains absorb the interstellar far ultraviolet and visible photons and reemit them in farinfrared (FIR) wavebands. The dust FIR continuum can be predicted by a grid of models using various values of the interstellar radiation field.
Aims. We analyze the dust continuum emission in two HiGAL sciencedemonstration phase (SDP) fields using both the radiative transfer code, Cloudy, and the DustEM dust model, to explore the effect of radiative transfer on dust temperature. The 500 μm submillimeter excess emission and the very small grain (VSG) contribution to the 70 μm intensity are investigated by spectral energy distribution (SED) fitting using the Cloudy model.
Methods. By comparing the observation with the model prediction, we derive dust temperature maps of the two SDP fields by fitting the dust SED with 4band data (SPIRE bands plus PACS 160 μm) using both Cloudy and DustEM models. Considering radiative transfer and grain physics simultaneously, we investigate the existence of a 500 μm excess and estimate the VSG contribution to the 70 μm intensity by fitting the dust SED with 3band data (160, 250, and 350 μm) and 5band data (SPIRE and PACS bands), respectively.
Results. We confirm that the field with star formation activities have a higher temperature (18.7 ± 0.9 K) than the quiescent region (15.2 ± 0.6 K). We find that the radiative transfer affects the FIR SED of the SDP fields and results in a higher temperature distribution than the dustonly model fit. There is no significant detection of a 500 μm excess in the two SDP fields. The relative contribution from the VSGs to the 70 μm intensity can be up to 50%.
Key words: ISM: general / dust, extinction / infrared: ISM / methods: data analysis
Herschel is an ESA space observatory with science instruments provided by Europeanled Principal Investigator consortia and with important participation from NASA.
Reduced Herschel maps (FITS) are only available at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsarc.ustrasbg.fr/vizbin/qcat?J/A+A/564/A111
© ESO, 2014
1. Introduction
Interstellar dust particles are size distributed. Mathis et al. (1977) developed a powerlaw grainsize distribution on the basis of the observed interstellar extinction from infrared to ultraviolet wavelengths: n(a) ∝ a^{3.5}, where n(a) is the number density of grains with radius <a (0.005 μm <a< 0.25μm). The emission from dust grains with different sizes dominates farinfrared (FIR) emission in different wavelength ranges. Small grains (≲0.005μm) radiate at λ ≲ 50μm by cooling after they are heated by single starlight photons (Draine 2003). Big grains (BGs; ≳0.01μm) are at thermal equilibrium, emitting FIR continuum at λ ≳ 50μm.
To derive the equilibrium temperature of BGs in the interstellar radiation field (ISRF), there have been mainly two methods to analyze FIR spectral energy distributions (SED) of dust grains. One is fitting the SED with a modified blackbody (i.e., gray body; e.g., Paradis et al. 2010). The other is fitting the SED with FIR continuum emission calculated by dust models, such as DustEM (Compiègne et al. 2010).
In the gray body method, the temperature of big grains is approximated by (1)where F_{ν} is the observed flux, B_{ν} is the blackbody emission, T_{dust} is dust temperature, and β is the emissivity spectral index that modifies the blackbody emission. Boulanger et al. (1996) found that β = 2 for the solar neighborhood derived from diffuse FIR emission, which is measured by Diffuse InfraRed Background Experiment (DIRBE) and Far InfraRed Absolute Spectrophotometer (FIRAS) at high Galactic latitudes, while Paradis et al. (2010) showed variations of the spectral emissivity spectral index in the range 1.8 ~ 2.6 for the Galactic plane. This method assumes that the dust abundance does not vary and dust grains are single size grains.
In the second method, DustEM is used to predict the emission of dust grains with specified grain types and grain size distributions. This method is more physical than using a gray body fit, since it considers the grain size distribution. Bernard et al. (2010) derived dust temperature maps of the Galactic plane using the DustEM code as a modeling tool. The DustEM code does not include any radiative transfer calculation. For dust and gas near hot OB stars, it is more physical to consider both the gas and grain absorption of radiation. To do that, calculation of full radiative transfer is needed.
The Cloudy code (Ferland et al. 2013) includes grain models into selfconsistent radiative transfer calculation, which produces the continuum and line emission of gas and dust in equilibrium condition. In this paper, we compare the predicted dust emission of Cloudy models for various values of ISRF with HiGAL (Molinari et al. 2010) sciencedemonstration phase (SDP) data to derive dust temperature maps of SDP fields. The SDP fields are two 2° × 2° images centered at l = 30°, b = 0°, and l = 59°, b = 0°.
We introduce the observation data and analysis method in Sect. 2. Results of 4band (160, 250, 350, and 500 μm) fits and the comparison between Cloudy and DustEM results are presented in Sect. 3. In Sect. 4, we present the results of 3band (160, 250, and 350 μm) fits for Cloudy models and the calculation of the 500 μm excess. The contribution from very small grains to the 70 μm intensity is estimated in Sect. 5. We summarize in Sect. 6.
2. The observation and analysis method
The Herschel (Pilbratt et al. 2010) HiGAL images provide data with extraordinary spatial, wavelength, and dynamic range coverage for studying the FIR emission of dust grains in the Galactic plane. The HiGAL SDP fields are products of the HiGAL program, which are observed with PACS (Poglitsch et al. 2010) 70 μm and 160 μm channels and SPIRE (Griffin et al. 2010) 250, 350, and 500 μm channels on board Herschel. The HiGAL data processing and map making are described in Molinari et al. (2010). Since the GLS mapmaking technique is known to introduce artifacts in the maps, namely crosses and stripes in correspondence of the brightest sources, a weighted postprocessing of the GLS maps (WGLS, Piazzo et al. 2012) has been applied to finally obtain images in which artifacts are removed or heavily attenuated. The SDP images used in this article are the latest version released to the HiGAL consortium. The data have been absolutely calibrated. For more information of the absolute calibration of the HiGAL pipeline, we refer the reader to Elia et al. (2013).
The very small grains (VSGs, radius <0.005 μm) are stochastically heated. The contribution from the VSGs to the PACS 70 μm channel can be up to ~50% (Compiègne et al. 2010). To focus on equilibrium temperature of BGs, we exclude the 70 μm emission in our SED fitting to derive the temperature maps. The adopted absolute calibration uncertainty is 20% for PACS bands (Bernard et al. 2010) and 15% for SPIRE bands (Paradis et al. 2010). We exclude the higher latitude areas ( b  > 0.9°), where the data could be less reliable. Maps of all five channels are smoothed to the same resolution as SPIRE 500 μm channel with the convolution kernels given by Karl Gordon^{1}.
We adopt the buildin ISM dust grains and ISM gas abundance of Cloudy. This grain set has two components, graphite and silicate. The size distribution of ISM dust grains is given by Mathis et al. (1977). This grain set generally reproduces the observed overall extinction properties for R_{V} = 3.1, or the average Milky Way extinction (Fitzpatrick 2004). The size of adopted ISM grains ranges from 0.005 μm to 0.25 μm with a dusttogas mass ratio, D/G = 6.362 × 10^{3}. PAHs are included in our calculation with a powerlaw size distribution, as described in Abel et al. (2008). The geometry is planeparallel.
With input parameters specified above, we use Cloudy to precalculate the dust FIR SED for the gas column density, N(H) = 10^{20} H cm^{2}, for various values of ISRF. The SED of ISRF is described in Black (1987). The scaling factor U in Cloudy scales the intensity of ISRF. We have U = 1.04 G_{0} in Habing field unit (1.6 × 10^{3} erg cm^{2} s^{1}; Habing 1968). In the calculations, U is set to range from 10^{2} to 10^{2} with 0.02 dex steps. The gas density n is fixed at 10 cm^{3}. We test the effect of gas density by comparing the predicted FIR SED for varying gas density, which ranges from 1 cm^{3} to 10^{3} cm^{3} with 1 dex steps, when the logarithmic value of U is set to range from –2 to 2 with 1 dex steps. For a certain G_{0}, tests show that the difference between the resulted SED of the FIR continuum at n = 10 cm^{3} and at other value of gas density is less than 0.2% when N(H) is fixed to 10^{20} H cm^{2}. Thus, we ignore the effects of gas density. For every map pixel, we compare the observed fluxes with model predictions by computing a chisquare statistic using equation, (2)where F_{obs,i} is the observed flux of waveband i, F_{mod,i} is the model predicted flux of waveband i, and σ_{i} is the calibration uncertainty of waveband i. In this equation, s is the scaling factor chosen to minimize the χ^{2} between observation and model prediction. The value N is the number of band, and the degrees of freedom of χ^{2} distribution is N − M, where M is the number of free parameters determining the model prediction. In our case, G_{0} and s are the varying parameters.
We minimize the χ^{2} to recover the best fit G_{0} for every pixel. The parameter G_{0} determines the SED of dust FIR continuum. We estimate dust temperature using the formula T_{d} = 17.5 K(G_{0})^{1/(4 + β)} (Bernard et al. 2010; Boulanger et al. 1996; Compiègne 2010) with a dust emissivity index β = 2. For both fields, we fit the dust SED with 4band data using Cloudy. When the scaling factor s is held fixed, we estimate the 68% confidence interval of G_{0} by increasing the minimized value of χ^{2} by 1 for every pixel (Avni & Bahcall 1976).
To explore the effect of radiative transfer, we also fit the SED with 4band data using the DustEM model. Following the same procedures as 4band fits for Cloudy models, we first use the DustEM code to precalculate the dust FIR SED for various values of ISRF. The SED of ISRF, the dynamic range and the increment step of G_{0}, and the grain set used in DustEM models are the same as what we adopt in the SED fitting for Cloudy models. The precalculated dust FIR SED is then compared with the observation. We adjust G_{0} and the scaling factor s in Eq. (2) to fit the SED of every map pixel and compute the χ^{2} using Eq. (2). We find the best fit G_{0} by minimizing the χ^{2} of every pixel and then estimate dust temperature using the formula T_{d} = 17.5 K(G_{0})^{1/(4 + β)}.
To investigate the existence of a 500 μm excess, we use the same procedures to fit the SED with 3band data (160, 250, and 350 μm) using the Cloudy code and compare them to results of 4band fits for Cloudy models. We also fit the SED with 5band data using Cloudy to estimate the contribution from the VSGs to the 70 μm intensity by comparing the results of 5band fits with 4band fits for Cloudy models.
3. Results of 4band fits for Cloudy and DustEM models
Fig. 1 Temperature maps and χ^{2} maps of the l = 30° field. Upper panel: the temperature map. Lower panel: χ^{2} map. 

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Fig. 2 Temperature maps and χ^{2} maps of the l = 59° field. Upper panel: the temperature map. Lower panel: χ^{2} map. 

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In this section, we compare the results for Cloudy models with DustEM models to explore the effects of radiative transfer. We present the temperature maps and χ^{2} distribution of 4band fits for Cloudy results in Figs. 1, and 2 and summarize results in Table 1. We show the temperature histograms in Fig. 3. For the l = 30° field, the average temperature is 18.7 K with the root mean square (RMS) value 0.9 K. For the l = 59° field, the average temperature is 15.2 K with the RMS 0.6 K. For both fields, the percentages of pixels with χ^{2}> 2 are both 0.015%.
To explore the effects of radiative transfer, we overlay histograms of Cloudy results on DustEM results and present them in Fig. 4. For both fields, the derived maximum and average temperatures of DustEM results (Table 1) are lower than Cloudy results. Comparing histograms in the upper panels of Fig. 4, we find that the temperature distributions of DustEM results shift toward lower value of temperature. The difference between results for Cloudy and DustEM models is better shown in the lower panels of Fig. 4. We plot the temperature of every pixel for Cloudy and DustEM models in the lower panels of Fig. 4 and overlay the 68% confidence interval of Cloudy results on the two plots. A black dot indicates the temperatures of every pixel for DustEM (T_{DustEM}, the value of y axis) and Cloudy results (T_{Cloudy}, the value of x axis); two red lines indicate the 68% confidence interval of dust temperature for Cloudy results. A black line of y = x is also plotted. If T_{Cloudy} equals to T_{DustEM}, the black dot would fall on the black line; if T_{DustEM} is consistent with T_{Cloudy} within the 68% confidence interval, the black dot would fall between the two red lines. As shown in the lower panels of Fig. 4, most black dots fall outside the area between the two red lines. To find the degree of inconsistency, we count the number of black dots outside the area between the two red lines. For the l = 30° field, 99.9% of all pixels for DustEM results are inconsistent with Cloudy results within the 68% confidence interval. For the l = 59° field, the temperature of all pixels for DustEM results are inconsistent with Cloudy results within the 68% confidence interval. This high degree of inconsistency between DustEM and Cloudy results indicates that 1) the radiative transfer has an effect on FIR SED compared to predictions using the dust model only; 2) the effect is pronounced in both the hotter region and the colder region and makes the temperature distribution shift toward higher value of temperature.
Results of 4band fits.
Fig. 3 Temperature histograms for 4band fits. Black line: the histogram of the l = 30° field. Red line: the histogram of the l = 59° field. 

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Fig. 4 Comparison of DustEM and Cloudy results. Upper panels: the overlay of histograms; black line is the result of Cloudy; red line is the result of DustEM. Lower panels: the function of the black line: y = x; black dot indicates the temperatures of every pixel for DustEM results and for Cloudy results; red lines indicate the 68% confidence interval of Cloudy results. 

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4. Results of 3band fits for Cloudy models
Using Cloudy models, we fit the dust SED using 160, 250, and 350 μm data to investigate the influence of 500 μm data points in the SED fitting and the existence of a 500 μm excess.
To investigate the influence of 500 μm data point in the SED fitting, we compare the results of 3band and 4band fits for Cloudy models. We overlay the temperature histograms of 3band fits on the histograms of 4band fits in Fig. 5. The properties of 3band fits for both fields are listed in Table 2. For both fields, part of histograms of 3band fits and 4band fits are overlapped.
Fig. 5 Comparison of 3band and 4band fits for Cloudy models. Left panel: the histograms of the l = 30° field. Right panel: the histograms of the l = 59° field. Black line is the result of 3band fits for Cloudy models; red line is the result of 4band fits for Cloudy models. 

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Results of 3band fits for the Cloudy model
Fig. 6 500 μm excess. Left panel: excess histograms of the l = 30° field. Right panel: excess histograms of the l = 59° field. 

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For the l = 30° field, 99.5% of all pixels of 3band fits are consistent with 4band fits within the confidence interval of 4band fits. For the l = 59° field, 98.3% of all pixels of 3band fits are consistent with 4band fits within the confidence interval. The high degree of consistency indicates that 500 μm data point has little influence on the results of SED fitting, and there is no significant excess of a 500 μm emission. More specifically, we calculate the 500 μm excess by the equation, (3)where is the observed 500 μm intensity and is the model predicted intensity. Histograms of the 500 μm excess is presented in Fig. 6. The pixel distribution of excess for both fields skew toward positive values, and the average excess with and without negative values is 1% and 2% for both fields. Thus, there is no detection of any notable 500 μm excess in the HiGAL SDP fields.
Our calculation of the 500 μm excess is consistent with the results of Paradis et al. (2012). With respect to the predictions of a modified blackbody model, Paradis et al. (2012) reported that the 500 μm excess in the peripheral parts of the Galactic plane can be up to 16% to 20%. Nevertheless, they found the median value of the 500 μm excess is only 1% and 3% in the l = 30° field and the l = 59° field, respectively.
5. The VSG contribution to the 70 μm intensity
Based on the results of 4band fits for Cloudy models, we include the 70 μm data in the SED fitting to estimate the VSG contribution to the 70 μm intensity. In the 5band fits, the scaling factor s in Eq. (2) is the same as in the 4band fits for Cloudy models, and G_{0} is the only free parameter.
Since the VSG contributes to the 70 μm emission, we should subtract the contribution from the VSG when we fit the SED using 5band data to derive the equilibrium temperature of the BGs. We assume that VSGs contribute x% to the 70 μm intensity. After subtracting x% of the 70 μm intensity coming from the VSGs, we fit the SED using 5band data.
We compare the results of 5band fits with 4band fits for x = 0, 10, 20, 30, 40, 45, 48, 50, and 60, and derive the consistency, or the percentage of pixels whose temperature of 5band fits are consistent with 4band fits within the 68% confidence interval of 4band fits. Since about 10% of all pixels in the l = 59° field have negative values of the 70 μm emission, which might be caused by improper calibration in this waveband, we only analyze the l = 30° field here.
Fig. 7 Consistency of 5band and 4band fits for Cloudy models. 

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The histogram of consistency is presented in Fig. 7. The value of consistency increases from 88% to 98% when the VSG contribution increases from 0% to 30%. When the VSG contribution is more than 30%, the value of consistency decreases with the increasing contribution. The consistency is 52% and 44% when the contribution is 48% and 50%, respectively. Thus, the
VSG contribution to the 70 μm intensity can be from 0% up to 50%. The temperature distributions of the 5band fits are most consistent (consistency >95%) with the 4band fits when the contribution is 20% to 30%. Our estimation of 70 μm contribution from the VSGs is consistent with Compiègne et al. (2010), who found that the VSG contribution goes from 10% up to 50% with a median value of 27% in a diffuse region of the l = 59° field.
6. Summary
We derive temperature maps of the BGs in the fields of l = 30° and l = 59° by considering radiative transfer and grain physics at the same time. The dust temperatures of the l = 30° field range from a minimum 10.9 K in diffuse regions to a maximum 32.8 K with an average value of 18.7 ± 0.9 K. For the l = 59° field, the dust temperatures range from 12.8 K to 29.4 K with an average value of 15.2 ± 0.6 K. Compared to results for dustonly models, we find that the radiative transfer affects the FIR SED and makes the temperature distribution shift toward higher value of temperature.
We explore the 500 μm excess by fitting the dust SED without the 500 μm waveband and find that there is no significant excess of a 500 μm emission in the two SDP fields. The SED fitting of 5band data is performed to estimate the VSG contribution to the 70 μm intensity. The VSGs can contribute up to 50% of the observed 70 μm intensity.
Acknowledgments
We thank the anonymous referee for helpful comments. This study is supported by funding KJCX2YWT20 of Chinese Academy of Science.
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All Tables
All Figures
Fig. 1 Temperature maps and χ^{2} maps of the l = 30° field. Upper panel: the temperature map. Lower panel: χ^{2} map. 

Open with DEXTER  
In the text 
Fig. 2 Temperature maps and χ^{2} maps of the l = 59° field. Upper panel: the temperature map. Lower panel: χ^{2} map. 

Open with DEXTER  
In the text 
Fig. 3 Temperature histograms for 4band fits. Black line: the histogram of the l = 30° field. Red line: the histogram of the l = 59° field. 

Open with DEXTER  
In the text 
Fig. 4 Comparison of DustEM and Cloudy results. Upper panels: the overlay of histograms; black line is the result of Cloudy; red line is the result of DustEM. Lower panels: the function of the black line: y = x; black dot indicates the temperatures of every pixel for DustEM results and for Cloudy results; red lines indicate the 68% confidence interval of Cloudy results. 

Open with DEXTER  
In the text 
Fig. 5 Comparison of 3band and 4band fits for Cloudy models. Left panel: the histograms of the l = 30° field. Right panel: the histograms of the l = 59° field. Black line is the result of 3band fits for Cloudy models; red line is the result of 4band fits for Cloudy models. 

Open with DEXTER  
In the text 
Fig. 6 500 μm excess. Left panel: excess histograms of the l = 30° field. Right panel: excess histograms of the l = 59° field. 

Open with DEXTER  
In the text 
Fig. 7 Consistency of 5band and 4band fits for Cloudy models. 

Open with DEXTER  
In the text 
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