Kes 17

# Far-Infrared Luminous Supernova Remnant Kes 17

## Abstract

We present the results of infrared (IR; 2.5–160 m) observations of the supernova remnant (SNR) Kes 17 based on the data obtained with the and satellites. We first detect bright continuum emission of its western shell in the mid- and far-IR wavebands together with its near-IR molecular line emission. We also detect hidden mid-IR emission of its southern shell after subtraction of the background emission in this region. The far-IR luminosity of the western shell is 8100 , which makes Kes 17 one of the few SNRs of significant far-IR emission. The fittings of the spectral energy distribution indicate the existence of two dust components: 79 K (hot) and 27 K (cold) corresponding to the dust mass of 6.2  10 and 6.7 , respectively. We suggest that the hot component represents the dust emission of the material swept up by the SNR to its western and southern boundaries, compatible with the distribution of radio continuum emission overlapping the mid-IR emission in the western and southern shells. The existence of hot ( 2,000 K), shocked dense molecular gas revealed by the near-IR molecular line emission in the western shell, on the other hand, suggests that the cold dust component represents the dust emission related to the interaction between the SNR and nearby molecular gas. The excitation conditions of the molecular gas appear to be consistent with those from shocked, clumpy admixture gas of different temperatures. We discuss three possibilities for the origin of the bright far-IR emission of the cold dust in the western shell: the emission of dust in the inter-clump medium of shocked molecular clouds, the emission of dust in evaporating flows of molecular clouds engulfed by hot gas, and the emission of dust of nearby molecular clouds illuminated by radiative shocks.

ISM: clouds — ISM: individual ( (catalog Kes~17, G304.6$+$0.1)) — infrared: ISM — shock waves — supernova remnants
8

## 1. Introduction

The broad-band infrared (IR) observations are well suited for the study of the evolution of SNRs. Besides the general advantage of suffering less extinction effects, there are diverse important phenomena related to supernova remnants (SNRs) which are bright in the IR wavebands. In the near- and mid-IR regimes, for example, one can study the distributions of dense ejecta from core-collapse supernova explosions (e.g., Koo et al., 2007; Moon et al., 2009), circumstellar material produced by mass loss of the progenitors (e.g., Dwek et al., 2008; Lee et al., 2009a, b), shock interactions between SNRs and nearby molecular clouds (e.g., Burton et al., 1988; Oliva et al., 1990; Reach et al., 2005; Neufeld et al., 2007; Hewitt et al., 2009; Shinn et al., 2009), and hot dust synthesized in ejecta (e.g., Arendt et al., 1999; Rho et al., 2008), along with the emission from the central compact objects (e.g., Moon et al., 2004; Kaplan et al., 2006; Wang et al., 2006).

The far-IR observations of SNRs, on the other hand, are relatively rare but very efficient to investigate cold dust which often contributes to a significant portion of the total mass of the dust in SNRs. First, it is studied that the swept-up dust in SNRs is responsible for the most of cooling of SNRs and plays a critical role in the evolutions of SNRs in dense medium (Dwek et al., 1987). Secondly, the far-IR observations of SNRs appear to provide better means of studying the dust formed during the process of supernova explosion (e.g., Sibthorpe et al., 2010; Barlow et al., 2010). Finally, if an SNR is interacting with a nearby molecular cloud, its far-IR emission is expected to be significantly enhanced by the swept-up, inter-clump medium in the cloud or by the evaporation of dense clumps (e.g., Draine, 1981; Dwek, 1981), although the reality of these processes is yet to be confirmed observationally.

Kes 17, known as G304.60.1, is such an object in which broad-band IR observations can play an important role in our understanding of SNRs. Until recently this SNR has only been studied in radio continuum and OH line observations (Shaver & Goss, 1970; Milne & Dickel, 1975; Whiteoak & Green, 1996; Frail et al., 1996), revealing broken radio shell structures in the west and south. The recent observations, however, detected very bright IR emission in the 3–8 m range (Lee, 2005; Reach et al., 2006), which makes it in fact one of the brightest SNRs in the wavelength range. The follow-up spectroscopic observations in the 5–30 m range also detected many strong H emission lines (Hewitt et al., 2009). Very recently, the XMM-Newton X-ray observations detected centrally filled thermal X-ray emission inside the non-thermal radio shell, listing it as a member of the class of mixed-morphology SNRs (Combi et al., 2010). All these indicate that Kes 17 is interacting with nearby molecular gas and that more IR observations are needed to better understand its nature. In this paper, we present extensive broad-band IR observations of Kes 17 using the satellite, together with new analyses of archival and radio continuum data. For the distance to Kes 17, only a lower limit of 8 kpc, corrected for the distance between the Sun and the Galactic center of 8.5 kpc, is known from the observations of H i line (Caswell et al., 1975). We adopt a distance of 8  kpc where is a scaling factor in this paper.

## 2. Observations and Data

### 2.1. Akari observations

The imaging observations of Kes 17 were carried out covering the mid-IR (13–27 m) and far-IR (50–180 m) bands on 2007 February 5 and 6, respectively. The journal of the observations is given in Table 1. The mid-IR observations were made by the Infrared Camera (IRC) equipped with an Si:As detector array of 256 256 pixels which produced two images of 10′  10′ centered on 15 m (IRC L15) and 24 m (IRC L24) (Onaka et al., 2007). The total on-source integration time was 196 s for both images. The basic calibration and data handling such as dark subtraction, linearity fitting, distortion correction, flat fielding, image combination and astrometric measurement were performed by IRC Imaging Data Reduction Pipeline version 201102259. The far-IR observations, on the other hand, were made by the Far-Infrared Surveyor (FIS) in two round-trip scans in the cross-scan shift mode (Kawada et al., 2007). The scan speed and shift length were 15″ s and 240″, respectively, and the resulting imaging size was 40′  12′ elongated in the scan direction. All the four FIS band (N60, Wide-S, Wide-L, and N160; see Table 2 for the details of the bands) images were obtained simultaneously in a single observing run using Ge:Ga (20 2 pixels for N60; 20 3 pixels for Wide-S) and stressed Ge:Ga (15 3 pixels for Wide-L; 15 2 pixels for N160) detector arrays. The initial calibration and data handling such as glitch detection, dark subtraction, flat fielding and flux calibration were performed by FIS Slow-Scan Toolkit version 2007091410, followed by advanced image construction based on the refined sampling mechanism. A summary of imaging bands used in this paper, including six bands (IRC L15, IRC L24, FIS N60, FIS Wide-S, FIS Wide-L, and FIS N160) and three bands (IRAC 4.5, IRAC 8, and MIPS 24), is given in Table 2.

The spectroscopic observations were carried out in the near-IR slit mode on 2008 August 8 and 2009 February 4–6 (Table 1), which produced grism spectra of R 120 spectral resolving power in the 2.5–5.0 m wavelength range (Ohyama et al., 2007). Spectra of the two bright peaks and the narrow filament in the western shell of Kes 17 previously identified in IRAC images (Lee, 2005; Reach et al., 2006) were obtained. The slit positions and their coordinates are presented in Figure 1 and in Table 3, respectively. The 5″  0″.8 slit was used for the target observations, whereas background spectra, which were subtracted from the target spectra later, were simultaneously obtained using the 3″  1″ slit positioned 1′ apart from the targets. The data calibration and handing were performed by IRC Spectroscopy Toolkit version 2008101511.

### 2.2. Spitzer Infrared and Atca Radio Continuum Data

Previous studies detected bright IR emission of Kes 17 in the IRAC bands between 3.6 and 8.0 m bands (Lee, 2005; Reach et al., 2006). We used the IRAC images of 4.5 and 8.0 m bands in this paper. We analyzed the archival data of MIPS 24 m band12 (Carey et al., 2009) to make an image of size of Kes 17. For the 24 m band image, we used the data in this paper, unless explicitly mentioned otherwise. In addition, we obtained the IRS 8–38 m and MIPS SED 52–97 m spectra available from the data archive13 to estimate contributions of line emission in the wavelength ranges.

We also obtained a high-resolution (9″.17 7″.36) radio-continuum image of Kes 17 using the Australia Telescope Compact Array () archival data provided by the Australia Telescope Online Archive.14. We synthesized the radio-continuum image of Kes 17 from the 12-h exposure 1.4 GHz data obtained with the 1.5A array configuration on 2004 March 24 after calibration of the data with 1329665.

## 3. Infrared Morphology of Kes 17

Figure 1 presents the and near- to far-IR (4.5–160 m) band images of Kes 17, together with the 20 cm radio-continuum image. The most conspicuous feature in the IR images is the bright emission of 5′ in the western shell apparent in all of the IR bands. The emission appears to be clumpy and filamentary in the near- and mid-IR bands up to 24 m, whereas it becomes unresolved in the longer (65–160 m) wavelength images due to increasingly large beam sizes. This IR emission in the western shell partly overlaps that of the radio continuum emission. In addition to the bright western shell, there is relatively weak mid-IR (15 and 24 m) emission in the southern shell overlapping the radio continuum emission in this region.

There exists noticeable background emission in the direction of Kes 17 in all the images longer than 4.5 m (Figure 1), especially in the northeast. In order to identify the southern shell emission in the 15 and 24 m images more clearly, we subtract the background emission from both the images as follows: first, given that both the 4.5 and 8 m emission of Kes 17 is due to the same origin (i.e., emission from shocked H; see § 4 for the details) in the western shell, we obtain a linear correlation with a correlation coefficient 0.86 between the 4.5 and 8 m emission of the shell. Based on the correlation, we scale the 4.5 m emission to 8 m and subtract the scaled emission from the observed 8 m emission to create a background image at 8 m. Next, we obtain a linear correlation of 0.89 between the background 8 m emission and the 24 m emission outside the boundaries of Kes 17, and then scale the 8 m emission to 24 m using the correlation. We subtract the scaled emission from the observed emission at 24 m, which finally gives the background-removed 24 m image of Kes 17 (Figure 2). The peak surface brightnesses of the western shell after the background subtraction are 6.1  1.5 and 6.4  1.5 MJy sr for 15 and 24 m bands, respectively. We apply the same method to obtain the background-removed 15 and 24 m images. In all these processes, we convolved the images of different beam sizes with that of the 24 m images. In Figure 2 we can now easily identify the existence of the southern shell at 15 and 24 m which overlaps that of the radio continuum. For far-IR images of 65, 90, 140, and 160 m, we estimate the background emission by taking the median value in the region between 4 and 6 radius from the center of Kes 17. After background subtraction, the peak surface brightnesses of the western shell are 108  24, 135  45, 173  84, and 117  55 MJy sr for 65, 90, 140 and 160 m bands, respectively.

Table 4 presents the measured (or upper limits) IR fluxes of the western and southern shells between 15 and 160 m, together with the estimation of contributions of line emission in the bands. The errors in the flux measurements are mainly caused by the uncertainties in the background measurements and also by those associated with the calibrations of the and observations. We estimate the line contributions to the observed fluxes of the 15 and 24 m bands using the IRS 8–38 m spectra. We construct the IRS spectra by subtracting the background obtained outside the shell structure and integrate them over the bandpass. The estimated line contributions are 75  21 (15 m) and 38  10 % (24 m for both and ), respectively. The line emission in these bands is dominated by H and ionic lines. We also estimate the contribution of line emission of the 60 and 90 m bands to be 16  8 and 3  2 %, respectively, using MIPS SED 52–97 m spectra. The line contributions in these bands are mostly due to [O i] at 63 m. For the 140 and 160 m bands, we expect the line contributions to be less than 5 % by scaling the flux of the [O i] 63 m line that we obtain above to those of [O i] 145 m and [C ii] 153 m lines in a shocked region (Hollenbach & McKee, 1989; Allen et al., 2008). Figure 3 shows the flux distribution of the western shell excluding the line contributions.

The IR synchrotron flux expected from an extrapolation of the radio fluxes applying synchrotron power-law index of 0.54 (Shaver & Goss, 1970) is less than a few percents of the measured IR values, supporting that the observed continuum is dominated by dust emission. In order to calculate temperatures of the dusts responsible for the mid- and far-IR emission of Kes 17, we perform the spectral energy distribution (SED) fits of the flux distribution (Figure 3) with two modified blackbody components. For the emissivity of the dusts in the SED fits, we adopt a mixture of carbonaceous and silicate interstellar grains (Draine, 2003). As a result, we obtain acceptable fit (reduced chi-square 2) with dust temperature components of 79  6 K and 27  3 K (Figure 3). The mass of the hot (79 K) dust is    and that of the cold (27 K) dust is 6.7  4.0  . The luminosities of the dust emission are (9.5  6.1)  10  and (8.1  5.0)  10  for the hot and cold components, respectively. It is worthwhile to note that the hot dust temperature could have been overestimated if there is any contribution from stochastically heated small grains to the 15 and 24 m continuum fluxes (Dwek, 1986).

## 4. Near-Infrared Spectroscopy and Bright H2 Lines

Figure 4 shows near-IR (2.5–5.0 m) spectra of five points (A, B1, B2, C1, C2 in Figure 1) in the western shell of Kes 17 obtained after subtraction of the background spectrum. (See Table 4 for their coordinates.) We detect several H lines in the spectra including the pure rotational transitions of 0-0 S(9–14) and ro-vibrational transitions of 1-0 O(3, 5, 6). Table 5 lists the observed intensities of the line emission.

Figure 5 presents the excitation diagram of the pure rotational and ro-vibrational H lines of B2 between the upper energy level of 6,000 K and 20,000 K. For this we correct the extinction effect using the H column density of 3.6 10 cm estimated in previous X-ray observations of Kes 17 and the Galactic extinction curve (Hewitt et al., 2009; Draine, 2003). The linear correlation between the upper energy level and the upper column density represented by a straight line in Figure 5 indicates the level population of the local thermodynamic equilibrium at the excitation temperature of 2200  400 K. The spectra of other positions, which have smaller number of detected lines, show similar excitation temperatures to that of B2.

## 5. Discussions

### 5.1. Origin of Bright Infrared Emission of Kes 17

The IR emission of Kes 17 shows the existence of both the western and southern shell structures. The former is visible in all the IR bands, while the latter is visible only in the mid-IR bands of 15 and 24 m. The near-IR emission of the western shell is dominated by H line emission (Figure 4), which suggests that Kes 17 is interacting with molecular gas in this region, consistent with the results of previous observations (e.g., Hewitt et al., 2009). The distribution of the mid-IR emission overlaps that of the radio continuum emission in the western and southern shells (Figure 2), supporting the interpretation that it represents swept-up dust at the boundary of the SNR. On the other hand, the far-IR emission is similar to the near-IR emission with only the western shell being readily identifiable. The coexistence of the far-IR emission from the cold dust and the near-IR line emission form shocked molecular gas in the western shell suggests that the bright far-IR emission of Kes 17 in this region is also related to the interaction of the source with a nearby molecular cloud.

The far-IR luminosity of Kes 17 ( 8100  ; § 3) makes it one of the most luminous SNRs in the far-IR wavebands and the second (after Cassiopeia A) Galactic SNR detected up to 160 m in the IR wavebands (Sibthorpe et al., 2010). For comparison, only eight SNRs were detected by IRAS at 100 m with far-IR luminosity larger than Kes 17 (Saken et al., 1992), five of them interacting with molecular clouds (e.g., Koo & Moon, 1997; Reach et al., 1999; Keohane et al., 2007; Hewitt et al., 2009). Our observations also strongly suggest that the far-IR emission of Kes 17 is originated from the dust in a molecular cloud interacting with the SNR. However, molecular shocks producing strong H lines in a dense molecular cloud cannot directly generate bright far-IR dust continuum emission. This is because, in the non-dissociative molecular shock with shock speeds of 50 km s, the gas temperature does not rise above a few thousand degrees (Draine, 1981). This is inadequate to heat the dust grains sufficiently high enough to emit bright far-IR continuum emission. Instead, if a molecular cloud is clumpy, composed of clumps and inter-clump medium, then the far-IR emission may be produced by faster shocks propagating in the inter-clump medium of lower densities. Even though the density of inter-clump medium is lower than that of the H emitting clumps, it can still be high enough to contain large amount of dusts and reduce shock speeds significantly. In the following we consider these possibilities.

When SNR shocks propagate into a clumpy molecular cloud, hot gas in swept-up inter-clump medium behind shock front collisionally heats dusts to produce the IR emission. The estimated dust mass of the western shell of Kes 17 is  M. If the cloud initially occupies the entire western region with normal dust-to-gas ratio of 1 %, the pre-shock inter-clump density is cm. Assuming that Kes 17 is in a Sedov phase with radius of  7  pc, the shock velocity in the inter-clump medium is , where is the SN explosion energy in the unit of 10 erg and is the density of the inter-clump medium. In this swept-up inter-clump gas, the IR surface brightness of the dust by strong shocks is (Draine, 1981)

 Iν ≃ 90 (nic40 cm−3)(vic200 km s−1)3(λ90 μm)   MJy sr−1

around 90 m, which, for the obtained inter-clump density and velocity of 40 cm and 200 km s, gives comparable surface brightness to the observed value. Note that the calculation by Draine (1981) expects the peak of dust emission power () at the mid-IR wavelength (m), while our observations indicate a somewhat flat peak around the 65–90 m bands. This is suggestive that there may be a significantly increased amount of large dusts contributing effectively in the far-IR regime if the shocked inter-clump medium is responsible for the observed emission of Kes 17.

Alternatively, the bright far-IR emission of Kes 17 may be the emission of dusts injected from an evaporating cloud (Dwek, 1981). If so, the expected IR luminosity of an evaporating cloud in the hot gas of an SNR is (Dwek, 1981)

 LIR ≃ 200 n2h (Rc1 pc)3(Th107 K)1.5   L⊙

where is the radius of the cloud and and are the density and temperature of the hot gas, respectively. The X-ray emitting gas was recently detected inside the radio shell of Kes 17 (Combi et al., 2010), suggesting that the evaporation should occur at the surface of an IR emitting cloud where it is in contact with the hot interior gas. The temperature and density of the hot X-ray gas are  K and  cm, respectively (Combi et al., 2010). We expect the IR luminosity of an evaporating cloud to be 2,000  using the cloud radius of 3  pc () at 90 m (Figure 1). This is somewhat smaller than the observed far-IR luminosity ( 8000 , § 3) of Kes 17, indicating that the dust emission from an evaporating cloud may contribute only a small amount of the far-IR emission of Kes 17, although we cannot rule out the possibility completely given the various uncertainties involved in the measurements.

Another explanation of the bright far-IR emission of Kes 17 may be that the dusts in a pre-shock molecular cloud heated by strong radiation of the SNR shocks in a radiative phase emit the observed emission. The shocks propagating into a molecular cloud at the western shell of Kes 17 can easily become radiative for the pre-shock density of 100 cm if gas cooling is efficient. Taking a power-law temperature dependence of the cooling efficiencies (; Kahn, 1976), Cox et al. (1999) calculated a radiative shell forming at the radius with a shell velocity for a pre-shock density and a radiative shell forming time = 10,000 yrs. This indicates that Kes 17 likely has a radiative shell, if the pre-shock density is 20 cm. Using the shell forming values and a cloud radius of = 3  pc, the luminosity of a radiative shock at the western shell of Kes 17 is expected to be (Hollenbach & McKee, 1989)

 L≃2.6×104(Rc3 pc)2(no20 cm−3)(vs200 km s−1)3   L⊙

which appears to be adequate to explain the observed luminosity of the western shell (§ 3). In this case, we expect the peak of the dust emission power to be at the far-IR ( 60 m) region for the dusts of mixture of carbonaceous and silicate grains (Draine, 2011), consistent with the results of this study. This can also explain the absence of the X-ray emission in the western shell of Kes 17 as the lack of X-ray emitting high temperature gas in the radiative phase (Combi et al., 2010).

### 5.2. Thermal Admixture Model of Molecular Shocks

Our near-IR (2.5–5.0 m) spectra of the western shell of Kes 17 indicate the excitation temperature of 2200  400 K for H gas in this region (Figure 4). This is different from the previous results based on the observations where a mixture of two components of H gas of 300 K and 1200 K was proposed to explain the observed intensity distribution of H lines of the western shell in the 5–28 m range (Hewitt et al., 2009). The discrepancy in the excitation temperature suggests that the H gas in the western shell is in a thermal admixture as found in other H gas interacting with SNRs (Neufeld & Yuan, 2008; Shinn et al., 2009, 2010).

Figure 6 shows the excitation diagram of H lines detected in both the and observations, covering the upper energy level of 1000–17,000 K. (Note that while the results represent the levels of 7,000 K, the results do the levels of higher temperatures.) We fit the observed excitation diagram with a thermal admixture model where the column density of H gas is related to a power of its temperature of 100–4,000 K: (Shinn et al., 2009, 2010). The ortho-to-para ratio is fixed to be 3 in the fit. The best fit gives 3.0  0.1, ( cm, and ( cm for the power index, column density, and number density, respectively. The solid curve in Figure 6 represents the best-fit model to the observed data, where we can identify that the model prediction matches the observed values well. This column density is twice that of the two temperature model of the observations, while the number density is between those obtained for the warm and hot components of the results (Hewitt et al., 2009). The obtained power index of 3.0  0.1 is comparable to what obtained from other sources (Shinn et al., 2009; Neufeld & Yuan, 2009), and is not far from 3.8 obtained for bow shocks (Neufeld & Yuan, 2008). If Kes 17 is indeed interacting with clumpy molecular gas (see § 5.1), it can be easy to develop a group of shocks around dense clumps with various shock velocities, which in turn naturally leads to an admixture of H gas of different temperatures.

## 6. Conclusion

We show in this paper that Kes 17 is one of the most luminous SNRs in the IR wavebands, reaching the far-IR luminosity of 8100 . Its IR emission is concentrated on the western and southern shell structures. The western shell is bright in the mid- and far-IR continuum and the near-IR H line emission, whereas the southern shell is visible only in the mid-IR continuum emission. The far-IR continuum and near-IR H line emission of the western shell is related to its interaction with nearby molecular gas. It is apparent that there exists dense shocked molecular gas, excited to 2,000 K, in this region that produces the observed H line emission. If the molecular gas is clumpy, the observed far-IR emission can be produced by the dust associated with inter-clump molecular gas of lower densities. The far-IR emission may originate from the dust emission of the swept-up inter-clump molecular gas, the dust emission from an evaporating cloud, or the dust emission exposed to strong radiative shocks. The mid-IR emission of Kes 17 is bright in both the western and southern shells and overlaps radio continuum emission which forms a partly-broken circular shell structure. This suggests that the mid-IR and radio continuum emission delineates the boundary of Kes 17 made by the swept-up material.

The SED distribution of the IR emission of Kes 17 indicates the existence of two dust components: hot (79  6 K) component of    and cold (27  3 K) component of 6.7  4.0  . The former is responsible for most of the mid-IR continuum emission, while the latter is for the far-IR emission. The observed flux distribution of the H lines, on the other hand, can be explained with a thermal admixture of the shocked molecular gas of different temperatures in the 100–4,000 K range. This thermal admixture of the shocked molecular gas may be a natural consequence of the interactions between Kes 17 and clumpy molecular gas in which various shock velocities can easily produce thermal admixture of the molecular gas. Overall, it appears that combined far-IR continuum and near-IR spectroscopic observations are very useful to studying SNRs interacting with molecular gas, as was the case for Kes 17 in this paper, providing information for both the gas and dust components associated with the shock interactions.

This work is based on observations with , a JAXA project with the participation of ESA. This work is based in part on observations made with the Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We thank all the members of the project. We also thank an anonymous referee for constructive comments. H.-G.L. was supported by the Early Research Award Program (ERA07-03-270) to D.-S.M. from Ministry of Research and Innovation of the Ontario Provincial Government. D.-S.M. acknowledges the support by NSERC through Discovery program 327277. B.-C.K. was supported by the National Research Foundation of Korea (NRF) Grant (NRF-2010-616-C00020).

Facility: , ,

### Footnotes

1. affiliation: Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada; hglee@astro.utoronto.ca, moon@astro.utoronto.ca
2. affiliation: Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada; hglee@astro.utoronto.ca, moon@astro.utoronto.ca
3. affiliation: Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea; koo@astrohi.snu.ac.kr
4. affiliation: Department of Astronomy, Graduate School of Science, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan; onaka@astron.s.u-tokyo.ac.jp, isakon@astron.s.u-tokyo.ac.jp
5. affiliation: Korea Astronomy and Space Science Institute, 776, Daedeok-daero, Yuseong-gu, Daejeon 305-348, Korea; jeongws@kasi.re.kr, jhshinn@kasi.re.kr
6. affiliation: Korea Astronomy and Space Science Institute, 776, Daedeok-daero, Yuseong-gu, Daejeon 305-348, Korea; jeongws@kasi.re.kr, jhshinn@kasi.re.kr
7. affiliation: Department of Astronomy, Graduate School of Science, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan; onaka@astron.s.u-tokyo.ac.jp, isakon@astron.s.u-tokyo.ac.jp
8. slugcomment: Submitted: August 18, 2019
9. http://www.ir.isas.jaxa.jp/ASTRO-F/Observation/DataReduction/IRC/
10. http://www.ir.isas.jaxa.jp/ASTRO-F/Observation/DataReduction/FIS/
11. http://www.ir.isas.jaxa.jp/ASTRO-F/Observation/DataReduction/IRC/
12. http://data.spitzer.caltech.edu/popular/mipsgal/20080718_enhanced/MIPS_24/
13. http://sha.ipac.caltech.edu/applications/Spitzer/SHA/
14. http://atoa.atnf.csiro.au
15. observational identification number.
16. Detailed characteristics of IRC, FIS IRAC, and MIPS are described in Onaka et al. (2007), Kawada et al. (2007), Fazio et al. (2004), and Rieke et al. (2004), respectively.
17. The slit position angles were fixed to be 127 by the satellite orbit.
18. One of the accompanying slit data was used for the background spectrum.
19. Measured total band flux including continuum and line emission.
20. We estimate the line contribution to the observed band flux using the IRS and MIPS SED spectra
21. Measured total band flux including continuum and line emission.

### References

1. Allen, M. G., Groves, B. A., Dopita, M. A., Sutherland, R. S., & Kewley, L. J. 2008, ApJS, 178, 20
2. Arendt, R. G., Dwek, E., & Moseley, S. H. 1999, ApJ, 521, 234
3. Barlow, M. J. et al. 2010, A&A, 518, 138
4. Burton, M. G., Brand, P. W. J. L., Geballe, T. R., & Webster, A. S. 1988, MNRAS, 235, 161
5. Carey, S. J., et al. 2009, PASP, 121, 76
6. Caswell, J. L., Murray, J. D., Roger, R. S., Cole, D. J., & Cooke, D. J. 1975, A&A, 45, 239
7. Combi, J. A. et al. 2010, A&A, 523, 76
8. Cox, D. P., Shelton, R. L., Maciejewski, W., Smith, R. K., Plewa, T., Pawl, A., Różyczka, M. 1999, ApJ, 524, 179
9. Draine, B. T., 1981, ApJ, 245, 880
10. Draine, B. T., 2003, ARA&A, 41, 241
11. Draine, B. T., 2011, Physics of the Interstellar and Intergalactic Medium, (Princeton, NJ; Princeton University Press)
12. Dwek, E., 1981,ApJ, 430, 433
13. Dwek, E., 1986,ApJ, 302, 363
14. Dwek, E., Petre, R., Szymkowiak, A., & Rice, W. L. 1987,ApJ, 320, L27
15. Dwek, E., et al. 2008, ApJ, 676, 1029
16. Fazio, G. G., et al. 2004, ApJS, 154, 10
17. Frail, D. A., Goss, W. M., Reynoso, E. M., Giacani, E. B., Green, A. J., & Otrupcek, R. 1996, AJ, 111, 1651
18. Hewitt, John W., Rho, J., Andersen, M., & Reach, W. T. 2009, ApJ, 694, 1266
19. Hollenbach, D., & McKee, C. F. 1989, ApJ, 342, 306
20. Kahn, F. D. 1976, A&A, 50, 145
21. Kaplan, D. L., & Moon, D.-S. 2006, ApJ, 644, 1056
22. Kawada, M., Baba, H., Barthel, P. D. et al. 2007, PASJ, 59, 389
23. Keohane, J. W., Reach, W. T., Rho, J., & Jarrett, T. H. 2007, ApJ, 654, 938
24. Koo, B.-C., & Moon, D.-S. 1997, ApJ, 485, 263
25. Koo, B.-C., Moon, D.-S., Lee, H.-G., Lee, J.-J., & Matthews, K. 2007, ApJ, 657, 308
26. Lee, H.-G. 2005, JKAS, 38, 385
27. Lee, H.-G. Moon, D.-S., Koo, B.-C., Lee, J.-J., & Matthews, K. 2009, ApJ, 691, 1042
28. Lee, H.-G. Koo, B.-C., Moon, D.-S., Sakon, I., Onaka, T., Jeong, W.-S., Kaneda, H., Nozawa, T., & Kozasa, T. 2009, ApJ, 706, 441
29. Milne, D. K., & Dickel, J. R. 1975, AuJPh, 28, 209
30. Moon, D.-S., Lee, J.-J., Eikenberry, S. S., Koo, B.-C., Chatterjee, S., Kaplan, D. L., Hester, J. J., Cordes, J. M., Gallant, Y. A., Koch-Miramond, L. 2004, ApJ, 610, 33
31. Moon, D.-S., Koo, B.-C., Lee, H.-G., Matthews, K., Lee, J.-J., Pyo, T.-S., Seok, J. Y., & Hayashi, M. 2009, ApJ, 703, 81
32. Neufeld, D. A., Hollenbach, D. J., Kaufman, M. J., Snell, R. L., Melnick, G. J., Bergin, E. A., & Sonnentrucker, P. 2007, ApJ, 664, 890
33. Neufeld, D. A. & Yuan, Y. 2008, ApJ, 678, 974
34. Neufeld, D. A. Nisini, B, Giannini, T, Melnick, G. J., Bergin, E. A., Yuan, Y, Maret, S, Tolls, V, Güsten, R, & Kaufman, M. J. 2009, ApJ, 706, 170
35. Oliva, E., Moorwood, A. F. M., & Danziger, I. J. 1990, A&A, 240, 453
36. Onaka, T., Matsuhara, H., Wada, T. et al. 2007, PASJ, 59, 401
37. Ohyama, Y., Onaka, T., Matsuhara, H. et al. 2007, PASJ, 59, 411
38. Reach, W. T., & Rho, J. 1999, ApJ, 511, 836
39. Reach, W. T., Rho, J., & Jarrett, T. H. 2005, ApJ, 618, 297
40. Reach, W. T., Rho, J., Tappe, A., Pannuti, T. G., Brogan, C. L., Churchwell, E. B., Meade, M. R., Babler, B., Indebetouw, R., & Whitney, B. A. 2006, AJ, 131, 1479
41. Rho, J., Kozasa, T., Reach, W. T., Smith, J. D., Rudnick, L., DeLaney, T., Ennis, J. A., Gomez, H., & Tappe, A. 2008, ApJ, 673, 271
42. Rieke et al. 2004, ApJS, 154, 25
43. Saken, J. M., Fesen, R. A., & Shull, J. M. 1992, ApJS, 81, 715
44. Shaver, P. A., & Goss, W. M. 1970, AuJPA, 14, 133S
45. Shinn, J.-H., Koo, B.-C., Burton, M. G., Lee, H.-G., & Moon, D.-S. 2009, ApJ, 693, 1883
46. Shinn, J.-H., Koo, B.-C., Burton, M. G., Lee, H.-G., & Moon, D.-S. 2010, AdSpR, 45, 445
47. Sibthorpe, B., et al. 2010, ApJ, 719, 1553
48. Wang, Z., Chakrabarty, D., & Kaplan, D. L. 2006, Nature, 440, 772
49. Whiteoak, J. B. Z., & Green, A. J. 1996, A&AS, 118, 329
You are adding the first comment!
How to quickly get a good reply:
• Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
• Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
• Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters