# AKARI/IRC Near-Infrared Spectral Atlas of Galactic Planetary Nebulae

Ryou Ohsawa<EMAIL_ADDRESS>Institute of Astronomy, Graduate
School of Science, The University of Tokyo  2-21-1 Osawa, Mitaka, Tokyo
181-0015, Japan  Takashi Onaka, Itsuki Sakon  Department of Astronomy,
Graduate School of Science, The University of Tokyo  7-3-1 Hongo, Bunkyo-ku,
Tokyo 113-0033, Japan  Mikako Matsuura  School of Physics and Astronomy,
Cardiff University  Queen’s Buildings, 5 The Parade, Roath, Cardiff CF24 3AA,
United Kingdom  Hidehiro Kaneda  Division of Particle and Astrophysical
Science, Graduate School of Science, Nagoya University  Furo-cho, Chikusa-ku,
Nagoya, Aichi 464-8602, Japan

###### Abstract

Near-infrared (2.5–5.0$\,\mu$m) low-resolution
($\lambda/\Delta\lambda{\sim}100$) spectra of 72 Galactic planetary nebulae
(PNe) were obtained with the Infrared Camera (IRC) in the post-helium phase.
The IRC, equipped with a $1^{\prime}{\times}1^{\prime}$ window for
spectroscopy of a point source, was capable of obtaining near-infrared spectra
in a slit-less mode without any flux loss due to a slit. The spectra show
emission features including hydrogen recombination lines and the
3.3–3.5$\,\mu$m hydrocarbon features. The intensity and equivalent width of
the emission features were measured by spectral fitting. We made a
catalog111Available at
http://www.ir.isas.jaxa.jp/AKARI/Archive/Catalogues/IRC_PNSPC/ providing
unique information on the investigation of the near-infrared emission of PNe.
In this paper, details of the observations and characteristics of the catalog
are described.

Catalogs — planetary nebulae: general

##  1 Introduction

Planetary nebulae (PNe) are a late evolutionary stage of low- and
intermediate-mass stars (e.g., Schönberner & Blöcker, 1996; Blöcker, 1995).
They are surrounded by rich circumstellar material (CSM) ejected during the
Asymptotic Giant Branch (AGB) phase (Schönberner et al., 2005). The CSM is
eventually incorporated into the interstellar medium and consists of the
ingredients for next-generation star-forming activity.

Infrared spectra are rich in CSM emission features. These features can be used
to investigate mass, temperature and chemical properties of CSMs (e.g.,
Pottasch & Bernard-Salas, 2006; Pottasch et al., 1984; Bernard-Salas &
Tielens, 2005; Phillips & Márquez-Lugo, 2011). In some PNe, far-infrared
emission is dominated by that from dust grains, providing information about
the temperature and the total mass of dust grains. Spectroscopic observations
in the mid-infrared (${\sim}5$–$40\,\mu$m) have been used to identify dust
species (e.g., Volk & Cohen, 1990; Stanghellini et al., 2012). Emission from
stochastically heated dust grains also appears in the mid-infrared (Dwek et
al., 1997; Draine & Li, 2001). The dust features commonly found are PAHs, MgS,
silicate, and some potential cases of SiC. Near-infrared (${\sim}1$–$5\,\mu$m)
continuum emission in PNe involves free-free emission, stellar continuum, and
hot dust emission. Hydrogen recombination lines are prominent in the near-
infrared, such as Brackett-$\alpha$ at 4.051$\,\mu$m. The PAH emission feature
appears at 3.3$\,\mu$m (Beintema et al., 1996; Roche et al., 1996; Tokunaga et
al., 1991), while there is also emission from aliphatic C−H bonds at around
3.4–3.5$\,\mu$m (Joblin et al., 1996; Sloan et al., 1997).

Infrared space telescopes have been instrumental for PNe observations despite
limited spatial resolution. Eliminating the effects of heavy terrestrial
atmospheric absorption provides the critical advantage of continuous infrared
spectroscopic coverage. Volk & Cohen (1990) investigated 7–23$\,\mu$m low-
resolution spectra of 170 Galactic PNe with the Infrared Astronomical
Satellite (IRAS). The Short-Wave Spectrometer (SWS) and the Long-Wave
Spectrometer (LWS) on-board the Infrared Space Observatory (ISO) cover 2.5–45
and 45–197$\,\mu$m. A number of emission lines have been identified and the
physical conditions of circumstellar nebulae have been investigated (e.g.,
Pottasch & Bernard-Salas, 2006; Bernard-Salas & Tielens, 2005). The Infrared
Spectrograph (IRS) on-board the Spitzer space telescope covers 5.5–37$\,\mu$m.
Stanghellini et al. (2012) obtained 157 spectra of compact Galactic PNe and
investigated their dust emission. Spectra of PNe in the Magellanic Clouds were
also obtained with the IRS (Stanghellini & Haywood, 2010; Bernard-Salas et
al., 2009, 2008) thanks to its high sensitivity. The ISO/SWS had obtained
2.5–5.0$\,\mu$m spectra of Galactic PNe. About 85 spectra of Galactic PNe are
available in Sloan et al. (2003). However, only a few PNe have spectra with a
sufficient signal-to-noise ratio at 2.5–5.0$\,\mu$m to investigate weak
features such as the 3.4–3.5$\,\mu$m aliphatic emission. The Infrared Camera
(IRC) on-board AKARI satellite, for the first time, provides near-infrared
(2.5–5.0$\,\mu$m) spectroscopy with a sensitivity of a few mJy (Onaka et al.,
2007).

The present paper reports near-infrared spectroscopy with the AKARI/IRC.
Observations were carried out as part of an Open Time Program for the post-
helium phase, “Near-Infrared Spectroscopy of Planetary Nebulae” (PNSPC). Near-
infrared spectra of 72 PNe were obtained. The data were compiled as a near-
infrared spectral catalog. In this paper, we describe details of the
observations and the characteristics of the catalog. Detailed information
about the observations is given in Section 2. Section 3 describes the
reduction procedures and the method to extract the spectra. The
characteristics of the retrieved spectra and the format of the compiled
catalog are presented in Section 4. The quality of the IRC spectra and the
statistical properties of the catalog are discussed in comparison with the
observations by other facilities in Section 5. We summarize the paper in
Section 6.

##  2 Observations

###  2.1 Target Selection

Figure 1: Distribution of the observed planetary nebulae (the crosses)
overlaid on an extinction map in the Galactic coordinates created from the DSS
(Dobashi et al., 2005a). The gray scale indicates extinction at the $V$-band
from 0.1 to 5 mag.

The observed targets were selected from the Strasbourg-ESO Catalogue of
Galactic Planetary Nebulae (Acker et al., 1992), taking into account their NIR
magnitude and angular size. The spectroscopic sensitivity of the IRC is a few
mJy in the range of 2–5$\,\mu$m, while the saturation limit is about 10 Jy.
With these limits taken into account, objects whose $K$-band magnitude is
between 5 and 13 were selected as targets for this program. The observations
were carried out with the $1\arcmin{\times}1\arcmin$ Np-window (see Section
2.2 and Onaka et al., 2007) in the slit-less mode. Therefore, compact objects
were preferred to avoid degrading the spectral resolution. The candidate list
was then narrowed to objects whose radius in the optical was smaller than
$5\arcsec$, comparable to the full width half maximum of the IRC point spread
function $({\sim}3\arcsec)$, to exclude apparently large objects. Finally, 72
objects were selected and their spectra were successfully obtained. Figure 1
shows the distribution of the targets in the Galactic coordinates. The PNG ID,
the AKARI observation ID, and the coordinates of the PNSPC samples are listed
in Table 1. Table AKARI/IRC Near-Infrared Spectral Atlas of Galactic Planetary
Nebulae summarizes miscellaneous information of the objects, including the
optical (the $V$-band) and infrared (the 2MASS $K_{s}$-band) magnitudes.

The target selection method was independent of the chemistry and dust
compositions of the circumstellar nebula. The catalog is not considered to be
biased, in terms of chemical abundance and the chemistry of dust. However, the
objects were selected based on their sizes. Since PNe expand as they evolve,
the selection could be biased toward young PNe. The potential biases of the
PNSPC samples are discussed in detail in Section 5.

###  2.2 Instruments

Although the AKARI/IRC has three channels (Onaka et al., 2007), only the NIR
channel was available during the post-helium phase. The field of view of the
NIR channel consists of four parts: the N/Nc-window, the Ns-slit, the Np-
window, and the Nh-slit (see, Figure 3 in Onaka et al., 2007). The
observations were performed with the Np-window, which was designed for point
source, slit-less spectroscopy. Spectroscopy with the Np-window allows us to
collect all of the flux from an object. The present spectroscopy was carried
out with the grism, providing 2.5–5.0$\,\mu$m spectra with the spectral
resolution of $\lambda/\Delta\lambda{\sim}100$, for point sources
(${\lesssim}3^{\prime\prime}$). The spectral resolution was degraded for
extended objects.

The observations were carried out with the observation template IRCZ4. This
mode consists of three sequences: the first set is four spectroscopic images,
the second set is a broad band image, and the final set is another sequence of
four spectroscopic images. Thus, each pointing observation involves eight
frames for spectroscopy and one frame for broad-band imaging. Every frame
consists of short (4.58 sec) and long (44.41 sec) exposure images. Due to the
short integration time, the typical signal-to-noise ratio of the short
exposure images is worse than that of the long exposure images. In general, we
used only the long exposure images. The short exposure images were used only
for cases when the long exposure image showed saturated pixels.

Each object was observed either once, or twice. Thus, there were eight or
sixteen frames for each object. However, some frames were not usable due to
cosmic rays or unstable pointing during the exposure. The net integration time
thus depends on the target, listed in the sixth column of Table 1.

Table 1: Summary of Observations

PN G | Obs. ID | RA (J2000) | DEC (J2000) |  $N$(a) |  $t_{\rm int}$(b) | FWHM | Flags
---|---|---|---|---|---|---|---
|  | $hh{:}mm{:}ss$ | $dd{:}mm{:}ss$ |  | ${\rm sec.}$ | ${\rm\mu m}$ |  $\mathcal{S}$(c) |  $\mathcal{D}$(d) |  $\mathcal{C}$(e)
000.3${+}$12.2 | $3460107$ | $17:01:33.6$ | $-21:49:33.5$ | $17$ | $754.97$ | $0.045$ | N | N | N
002.0${-}$13.4 | $3460003$ | $18:45:50.7$ | $-33:20:35.0$ | $16$ | $710.56$ | $0.040$ | N | Y | N
003.1${+}$02.9 | $3460005$ | $17:41:52.8$ | $-24:42:07.7$ | $9$ | $399.69$ | $0.045$ | N | Y | Y
011.0${+}$05.8 | $3460012$ | $17:48:19.8$ | $-16:28:44.0$ | $18$ | $799.38$ | $0.035$ | N | N | N
027.6${-}$09.6 | $3460016$ | $19:16:28.3$ | $-09:02:37.0$ | $9$ | $399.69$ | $0.040$ | N | Y | N
037.8${-}$06.3 | $3460019$ | $19:22:56.9$ | $+01:30:48.0$ | $17$ | $754.97$ | $0.035$ | N | Y | N
038.2${+}$12.0 | $3460020$ | $18:17:34.0$ | $+10:09:05.0$ | $9$ | $399.69$ | $0.040$ | N | N | N
043.1${+}$03.8 | $3460093$ | $18:56:33.6$ | $+10:52:12.0$ | $9$ | $399.69$ | $0.035$ | N | Y | Y
046.4${-}$04.1 | $3460021$ | $19:31:16.4$ | $+10:03:21.7$ | $9$ | $399.69$ | $0.040$ | N | Y | Y
051.4${+}$09.6 | $3460022$ | $18:49:47.6$ | $+20:50:39.5$ | $17$ | $754.97$ | $0.040$ | N | N | N
052.2${-}$04.0 | $3460094$ | $19:42:18.7$ | $+15:09:09.0$ | $18$ | $799.38$ | $0.035$ | N | Y | N
058.3${-}$10.9 | $3460023$ | $20:20:08.8$ | $+16:43:54.0$ | $18$ | $799.38$ | $0.040$ | N | N | N
060.1${-}$07.7 | $3460024$ | $20:12:42.9$ | $+19:59:23.0$ | $14$ | $621.74$ | $0.048$ | N | Y | N
060.5${+}$01.8 | $3460025$ | $19:38:08.4$ | $+25:15:42.0$ | $18$ | $799.38$ | $0.035$ | N | Y | N
064.7${+}$05.0 | $3460026$ | $19:34:45.3$ | $+30:30:59.2$ | $17$ | $\phantom{0}77.86$ | $0.048$ | Y | N | N
071.6${-}$02.3 | $3460027$ | $20:21:03.8$ | $+32:29:24.0$ | $18$ | $799.38$ | $0.035$ | N | N | N
074.5${+}$02.1 | $3460028$ | $20:10:52.5$ | $+37:24:41.0$ | $18$ | $799.38$ | $0.040$ | N | N | N
082.1${+}$07.0 | $3460029$ | $20:10:23.7$ | $+46:27:39.0$ | $18$ | $799.38$ | $0.045$ | N | Y | N
082.5${+}$11.3 | $3460030$ | $19:49:46.6$ | $+48:57:40.0$ | $9$ | $399.69$ | $0.035$ | N | Y | N
086.5${-}$08.8 | $3460114$ | $21:33:08.3$ | $+39:38:09.7$ | $18$ | $799.38$ | $0.045$ | N | Y | N
089.3${-}$02.2 | $3460031$ | $21:19:07.2$ | $+46:18:48.0$ | $18$ | $799.38$ | $0.038$ | N | Y | N
089.8${-}$05.1 | $3460032$ | $21:32:31.0$ | $+44:35:47.7$ | $18$ | $799.38$ | $0.035$ | N | N | N
095.2${+}$00.7 | $3460033$ | $21:31:50.2$ | $+52:33:52.0$ | $18$ | $799.38$ | $0.042$ | N | Y | N
100.6${-}$05.4 | $3460034$ | $22:23:55.7$ | $+50:58:00.0$ | $18$ | $799.38$ | $0.035$ | N | N | N
111.8${-}$02.8 | $3460035$ | $23:26:14.9$ | $+58:10:53.0$ | $8$ | $355.28$ | $0.038$ | N | N | N
118.0${-}$08.6 | $3460096$ | $00:18:42.2$ | $+53:52:20.0$ | $16$ | $710.56$ | $0.035$ | N | Y | N
123.6${+}$34.5 | $3460115$ | $12:33:06.8$ | $+82:33:50.1$ | $18$ | $799.38$ | $0.065$ | N | Y | N
146.7${+}$07.6 | $3460097$ | $04:25:50.8$ | $+60:07:12.7$ | $18$ | $799.38$ | $0.035$ | N | N | N
159.0${-}$15.1 | $3460098$ | $03:47:33.0$ | $+35:02:48.9$ | $9$ | $399.69$ | $0.045$ | N | Y | N
166.1${+}$10.4 | $3460116$ | $05:56:23.9$ | $+46:06:17.2$ | $18$ | $799.38$ | $0.050$ | N | N | N
190.3${-}$17.7 | $3460099$ | $05:05:34.3$ | $+10:42:23.8$ | $9$ | $399.69$ | $0.045$ | N | N | N
194.2${+}$02.5 | $3460117$ | $06:25:57.2$ | $+17:47:27.3$ | $18$ | $799.38$ | $0.045$ | N | N | N
211.2${-}$03.5 | $3460036$ | $06:35:45.1$ | $+00:05:38.0$ | $16$ | $710.56$ | $0.035$ | N | N | N
221.3${-}$12.3 | $3460118$ | $06:21:42.7$ | $-12:59:14.0$ | $15$ | $666.15$ | $0.046$ | N | N | N
226.7${+}$05.6 | $3460100$ | $07:37:18.9$ | $-09:38:50.0$ | $17$ | $754.97$ | $0.040$ | N | Y | N
232.8${-}$04.7 | $3460037$ | $07:11:16.7$ | $-19:51:04.0$ | $14$ | $621.74$ | $0.035$ | N | N | N
235.3${-}$03.9 | $3460038$ | $07:19:21.5$ | $-21:43:54.3$ | $17$ | $754.97$ | $0.035$ | N | N | N
258.1${-}$00.3 | $3460039$ | $08:28:28.0$ | $-39:23:40.0$ | $17$ | $754.97$ | $0.042$ | N | N | N
264.4${-}$12.7 | $3460040$ | $07:47:20.0$ | $-51:15:03.4$ | $17$ | $754.97$ | $0.035$ | N | Y | N
268.4${+}$02.4 | $3460042$ | $09:16:09.6$ | $-45:28:42.8$ | $18$ | $799.38$ | $0.038$ | N | N | N
278.6${-}$06.7 | $3460101$ | $09:19:27.5$ | $-59:12:00.3$ | $18$ | $799.38$ | $0.040$ | N | Y | N
283.8${+}$02.2 | $3460044$ | $10:31:33.4$ | $-55:20:50.5$ | $16$ | $710.56$ | $0.045$ | N | Y | N
285.4${-}$05.3 | $3460120$ | $10:09:20.8$ | $-62:36:48.5$ | $18$ | $799.38$ | $0.050$ | N | Y | N
285.6${-}$02.7 | $3460045$ | $10:23:09.1$ | $-60:32:42.3$ | $17$ | $754.97$ | $0.042$ | N | Y | N
285.7${-}$14.9 | $3460121$ | $09:07:06.3$ | $-69:56:30.6$ | $17$ | $754.97$ | $0.060$ | N | N | N
291.6${-}$04.8 | $3460046$ | $11:00:20.0$ | $-65:14:57.8$ | $18$ | $799.38$ | $0.038$ | N | Y | N
292.8${+}$01.1 | $3460102$ | $11:28:47.4$ | $-60:06:37.3$ | $18$ | $799.38$ | $0.042$ | N | Y | N
294.9${-}$04.3 | $3460047$ | $11:31:45.4$ | $-65:58:13.7$ | $18$ | $799.38$ | $0.035$ | N | N | N
296.3${-}$03.0 | $3460048$ | $11:48:38.2$ | $-65:08:37.3$ | $15$ | $666.15$ | $0.035$ | N | N | N
304.5${-}$04.8 | $3460051$ | $13:08:47.3$ | $-67:38:37.6$ | $16$ | $710.56$ | $0.038$ | N | Y | N
305.1${+}$01.4 | $3460122$ | $13:09:36.4$ | $-61:19:35.6$ | $18$ | $\phantom{0}82.44$ | $0.050$ | Y | N | N
307.2${-}$09.0 | $3460052$ | $13:45:22.4$ | $-71:28:55.7$ | $18$ | $799.38$ | $0.035$ | N | Y | Y
307.5${-}$04.9 | $3460053$ | $13:39:35.1$ | $-67:22:51.7$ | $18$ | $799.38$ | $0.040$ | N | Y | Y
312.6${-}$01.8 | $3460123$ | $14:18:43.3$ | $-63:07:10.1$ | $16$ | $710.56$ | $0.056$ | N | Y | N
315.1${-}$13.0 | $3460054$ | $15:37:11.2$ | $-71:54:52.9$ | $18$ | $\phantom{0}82.44$ | $0.042$ | Y | N | N
320.1${-}$09.6 | $3460103$ | $15:56:01.7$ | $-66:09:09.2$ | $16$ | $710.56$ | $0.045$ | N | Y | N
320.9${+}$02.0 | $3460056$ | $15:05:59.2$ | $-55:59:16.5$ | $9$ | $399.69$ | $0.042$ | N | Y | N
322.5${-}$05.2 | $3460060$ | $15:47:41.2$ | $-61:13:05.6$ | $16$ | $710.56$ | $0.092$ | N | Y | Y
323.9${+}$02.4 | $3460061$ | $15:22:19.4$ | $-54:08:13.1$ | $9$ | $399.69$ | $0.045$ | N | Y | N
324.8${-}$01.1 | $3460062$ | $15:41:58.8$ | $-56:36:25.6$ | $8$ | $355.28$ | $0.036$ | N | Y | Y
325.8${-}$12.8 | $3460063$ | $16:54:35.2$ | $-64:14:28.4$ | $16$ | $710.56$ | $0.035$ | N | Y | N
326.0${-}$06.5 | $3460064$ | $16:15:42.3$ | $-59:54:01.0$ | $14$ | $621.74$ | $0.035$ | N | Y | Y
327.1${-}$01.8 | $3460065$ | $15:58:08.1$ | $-55:41:50.3$ | $9$ | $399.69$ | $0.035$ | N | Y | Y
327.8${-}$01.6 | $3460066$ | $16:00:59.1$ | $-55:05:39.7$ | $8$ | $355.28$ | $0.038$ | N | Y | N
331.1${-}$05.7 | $3460067$ | $16:37:42.7$ | $-55:42:26.5$ | $17$ | $754.97$ | $0.035$ | N | Y | N
331.3${+}$16.8 | $3460068$ | $15:12:50.8$ | $-38:07:32.0$ | $16$ | $710.56$ | $0.048$ | N | Y | N
336.3${-}$05.6 | $3460069$ | $16:59:36.1$ | $-51:42:08.4$ | $18$ | $799.38$ | $0.035$ | N | Y | N
342.1${+}$27.5 | $3460104$ | $15:22:19.3$ | $-23:37:32.0$ | $18$ | $799.38$ | $0.050$ | N | Y | N
349.8${+}$04.4 | $3460105$ | $17:01:06.2$ | $-34:49:38.0$ | $9$ | $399.69$ | $0.040$ | N | Y | N
350.9${+}$04.4 | $3460070$ | $17:04:36.2$ | $-33:59:18.0$ | $18$ | $799.38$ | $0.038$ | N | Y | N
356.1${+}$02.7 | $3460076$ | $17:25:19.2$ | $-30:40:41.0$ | $18$ | $799.38$ | $0.035$ | N | Y | Y
357.6${+}$02.6 | $3460082$ | $17:29:42.7$ | $-29:32:50.0$ | $15$ | $666.15$ | $0.035$ | N | Y | N

Note. — (a) the number of exposures; (b) the net integration time; (c) the
saturation flag, Y: the spectrum is (partly) saturated in long-exposure
spectral images; N: the spectrum is not saturated; (d) the decomposition flag,
Y: the spectral decomposition procedure was used; N: the spectrum was not
affected by any neighbor object; (e) the contamination flag, Y: the
decontamination procedure was used; N: the spectrum was not affected by any
overlapping object.

Table 2: Miscellaneous Information of Objects

PN G | $V^{(a)}$ | $K_{s}^{(b)}$ | $A_{V}({\rm H\beta})$ | $A_{V}({\rm fit.})$ | $T_{\rm eff}$ | Refs. $T_{\rm eff}$
---|---|---|---|---|---|---
| mag. | mag. | mag. | mag. |  $10^{3}\,$K |
000.3${+}$12.2 | $\phantom{0}13.9$ | $\phantom{0}11.4$ | $\phantom{0}\phantom{0}0.90_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.98_{{-}0.05}^{{+}0.15}$ | $\phantom{0}47$ | Ka76,Ph03
002.0${-}$13.4 | $\phantom{0}14.1$ | $\phantom{0}11.1$ | $\phantom{0}\phantom{0}0.31_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}0.38_{{-}0.04}^{{+}0.02}$ | $\phantom{0}60$ | PM89,PM91,Ph03
003.1${+}$02.9 | ${>}17.0$ | $\phantom{0}11.6$ | $\phantom{0}\phantom{0}3.31_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}3.4_{{-}0.1}^{{+}0.6}$ | $\phantom{0}87$ | PM89,Ph03
011.0${+}$05.8 |  $\cdots$ | $\phantom{0}11.8$ | $\phantom{0}\phantom{0}1.81_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}1.79_{{-}0.06}^{{+}0.06}$ | $\phantom{0}93$ | PM91,Ph03
027.6${-}$09.6 | $\phantom{0}15.2$ | $\phantom{0}11.9$ | $\phantom{0}\phantom{0}1.04_{{-}0.05}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}1.0_{{-}0.2}^{{+}0.9}$ | $\phantom{0}58$ | PM91,Ka76,KJ91,Ph03
037.8${-}$06.3 |  $\cdots$ | $\phantom{0}9.47$ | $\phantom{0}\phantom{0}\phantom{0}1.4_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}1.41_{{-}0.02}^{{+}0.08}$ | $\phantom{0}74$ | Ph03
038.2${+}$12.0 | $\phantom{0}12.5$ | $\phantom{0}11.1$ | $\phantom{0}\phantom{0}0.82_{{-}0.05}^{{+}0.05}$ | $\phantom{0}\phantom{0}0.93_{{-}0.07}^{{+}0.07}$ | $\phantom{0}30$ | Ka78,Ph03
043.1${+}$03.8 | $\phantom{0}14.9$ | $\phantom{0}12.1$ | $\phantom{0}\phantom{0}\phantom{0}1.9_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}2.05_{{-}0.05}^{{+}0.46}$ | $\phantom{0}28$ | Ph03
046.4${-}$04.1 | $\phantom{0}15.2$ | $\phantom{0}11.1$ | $\phantom{0}\phantom{0}1.42_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.39_{{-}0.01}^{{+}0.01}$ | $\phantom{0}68$ | Ka76,KJ91,Ph03
051.4${+}$09.6 | $\phantom{0}13.3$ | $\phantom{0}10.4$ | $\phantom{0}\phantom{0}0.88_{{-}0.04}^{{+}0.05}$ | $\phantom{0}\phantom{0}0.98_{{-}0.08}^{{+}0.11}$ | $\phantom{0}37$ | Ka76,Ka78,Ph03

Note. — Table 2.2 is published in its entirety in the electronic edition of
the Astrophysical Journal. A portion is shown here for guidance regarding its
form and content.

References. — (a)Acker et al. (1992); (b) Skrutskie et al. (2006); HF83:
Harrington & Feibelman (1983), Ka76: Kaler (1976), Ka78: Kaler (1978), KJ91:
Kaler & Jacoby (1991), Lu01: Lumsden et al. (2001), Me88: Mendez et al.
(1988), Ph03: Phillips (2003), PM89: Preite-Martinez et al. (1989), PM91:
Preite-Martinez et al. (1991).

##  3 Data Reduction

###  3.1 Bias Subtraction and Flux Calibration

The basic data reduction procedure used here, includes subtraction of dark
frames, linearity correction, saturation masking, flat fielding, and
subtraction of background emission. All steps were carried out with the IRC
Spectroscopy Toolkit for Phase 3 (Version 20111121)222Available at
http://www.ir.isas.jaxa.jp/ASTRO-F/Observation/DataReduction/IRC/. Pixels
affected by cosmic rays were masked by hand. Some pixels were saturated by
bright objects in the long exposure images. The saturated pixels were replaced
by the corresponding pixels from the short exposure images. Objects whose
spectra were saturated in the long exposure images are marked in the eighth
column of Table 1. Spectroscopic images were aligned by maximizing the
correlation among the images. Then, the images were combined by median
stacking, producing a two-dimensional spectrum. Frames that were affected by
unstable pointing during the exposure were excluded from stacking. The toolkit
also produced a two-dimensional noise map, which was given as a standard
deviation of the stacked frames.

###  3.2 Extraction of One-Dimensional Spectrum

Some objects were extended with respect to the point spread function (PSF) of
the IRC. To make a homogeneous data reduction, we assumed that all the sources
were extended. We used a sufficiently wide aperture (${>}10\,$pixels) to
extract a one-dimensional spectrum that included all of the fluxes from the
object, and did not apply any aperture correction. The standard error in the
spectrum was calculated using the noise map produced by the toolkit.

Figure 2: Schematic view of the spectral decomposition procedure. (Left)
Panels A, B, and C represent an original two-dimensional spectrum, estimated
contributions from the neighboring stars, and an isolated target spectrum.
(Right): Spatial profiles of the two-dimensional spectrum (Panel A of Figure
2a). The profiles are decomposed by fitting (see, text). The contributions
from neighboring stars are shown by the blue dashed lines. The component of
the target is shown by the red solid line.

It was difficult to use a wide aperture for objects which were located in
crowded regions. Noble et al. (2013) invented a novel method to extract the
spectrum of a certain object in a crowded region by profile fitting. We used a
similar method to remove the contribution from neighboring objects. Figure 2
shows a schematic view of the method (hereafter, the spectral decomposition
procedure). Panel A of Figure 2a shows an example two-dimensional spectrum of
a target in a crowded region. The horizontal and vertical axes correspond to
the position and wavelength. The spectrum of the target PN runs through the
center of the panel. The spectra of neighboring objects are located to the
right side of the PN spectrum. Figure 2b shows the spatial profiles of the
spectra (Panel A). The spectra were decomposed by fitting with a combination
of Gaussian functions. The red solid line shows the PN profile, and the blue
dashed lines show those of the neighboring objects. The fitting was performed
for every spectral element. The instrumental spatial profile of a spectrum was
not a Gaussian, rather a combination of Gaussian profiles provided the best
fit to the profile. Panel B of Figure 2a shows the estimated contribution from
the neighboring objects. By subtracting Panel B from Panel A, the two-
dimensional spectrum of the target PN was extracted (Panel C). Finally, the
one-dimensional spectrum of the target PN was obtained from Panel C with a
wide aperture, as mentioned above. The uncertainty in the contamination-
corrected spectrum was estimated by taking into account errors in the spectral
decomposition procedure. The targets which are in crowded regions are denoted
in the ninth column of Table 1.

####  3.2.1 Subtraction of Contamination

Figure 3: Schematic view of the decontamination procedure. The upper left
panel shows the locations of a PN and an overlapping star, while the upper
right panel shows the obtained spectrum with contamination from the
overlapping star. The contaminated spectrum is shown by the gray dotted line
in the bottom panel. The red dashed line shows the estimated contamination
from the overlapping star. The decontaminated spectrum of the PN is shown by
the blue solid line.

For some observations, the targets were found to be aligned with neighboring
objects, along the direction of dispersion. In such cases, the spectra of
these objects fully overlapped with each other. This made retrieval of the
target profile spectrum, by profile fitting alone, impossible (see the upper
panels in Figure 3). To remove the contamination from the overlapping objects,
we developed a method to estimate the amount of the contamination (hereafter,
the decontamination procedure). The method basically follows the procedure
used in Sakon et al. (2008). At first, a one-dimensional spectrum was
extracted with a wide aperture. We assumed that overlapping objects were stars
and their spectra did not show any particular spectral features in the
spectral range in question. Their 2.5–5.0$\,\mu$m spectra ($\tilde{f}_{\nu}$)
were estimated from the 2MASS, AKARI, and WISE photometric data by fitting
with a blackbody function. The calibration of the overlapping objects required
correction since the overlapping object was shifted along the direction of
dispersion. The amount of contamination $f^{c}_{\nu}(\lambda)$ was converted
from $\tilde{f}_{\nu}$ using the distance between the target and the
overlapping objects in the direction of the dispersion, $d$, in units of pixel
and the spectral response function of the IRC, $R(\lambda)$, in units of ${\rm
ADU}\,{\rm mJy^{-1}}$. We defined $\delta$ as the pixel scale of the spectrum
in units of $\mu$m$\,{\rm pixel}^{-1}$. The amount of the contamination was
estimated by

$f^{c}_{\nu}(\lambda)=\frac{\tilde{f}_{\nu}(\lambda{-}\delta
d)R(\lambda{-}\delta d)}{R(\lambda)}.$ (1)

We defined $f^{\rm obs}_{\nu}$ as the obtained spectrum, including the
contamination. The decontaminated spectrum was defined by $f^{\rm
obj}_{\nu}=f^{\rm obs}_{\nu}-f^{c}_{\nu}$. A schematic view of the method is
given in Figure 3. The upper left panel shows the location of the target (PN
G123.6+34.5) and overlapping object. The direction of dispersion is
horizontal. The spectrum with the contamination is shown in the upper right
panel. The contaminated one-dimensional spectrum is shown by the gray dotted
line in the bottom panel. The estimated contamination and decontaminated
spectra are shown by the red dashed and blue solid lines. We assume that the
spectrum of the overlapping star does not have any significant features and
that the decontamination procedure does not affect the estimate of emission
feature intensities (although continuum flux could be somewhat affected). The
targets with overlapping objects are flagged as contaminated objects in the
tenth column of Table 1.

##  4 Results

###  4.1 Near-Infrared Spectroscopy of Planetary Nebulae Spectral Atlas

Details of the observations are summarized in Table 1, which includes the PNG
ID, the observation ID, the location, the number of exposures, the total
integration time, the spectral PSF size, and the flags to denote data quality.
The PNSPC catalog contains extracted one-dimensional spectra shown in Figure 7
(plots for all the sources are available in the electric edition). Most of the
spectra cover $2.5$–$5.0\,\mu$m. Some spectra were affected by scattered light
inside the instrument or column-pull-down effects of the detector, which were
not correctable at present. The part of the spectrum severely affected by such
issues has been excluded from the catalog.

Two representative spectra in the PNSPC catalog are shown in Figure 4. The top
panel is the spectrum of PNG 064.7$+$05.0, and the bottom panel is that of PNG
074.5$+$02.1. The spectra showed several emission features: H I and He II
recombination lines, the PAH feature at $3.3\,\mu$m, and the aliphatic feature
complex in $3.4$–$3.5\,\mu$m. Some spectra also showed He II recombination
lines and [Mg IV] at ${\rm 4.49\,\mu m}$ and [Ar VI] at ${\rm 4.53\,\mu m}$
fine-structure lines, indicating that the excitation of the object was high.
Some objects showed molecular hydrogen lines, but they were weak and not
frequently detected. No prominent absorption features were detected in any of
the objects.

Figure 4: Representative spectra in the PNSPC catalog. The top and bottom
panels show the spectra of PNG 064.7$+$05.0 and PNG 074.5$+$02.1 by the blue
solid lines with errors. Series of recombination lines (H I, He I, and He II)
are indicated by the vertical lines. The both spectra show the PAH feature in
3.3$\,\mu$m and the aliphatic feature complex in 3.4–3.5$\,\mu$m. The spectrum
of PNG 074.5$+$02.1 shows fine-structure lines of [Mg IV] at 4.487$\,\mu$m and
[Ar VI] at 4.530$\,\mu$m. Step-like continuum emission is seen in the spectra
of PNG 064.7$+$05.0 (see Section 4.3).

Figure 5: Histograms of the uncertainty in continuum emission at $3.0\,\mu$m.
The top panel shows the histogram of absolute 1$\sigma$ errors. The gray
dashed line indicates the median of the uncertainty
($0.7{\times}10^{-15}\,{\rm W\,m^{-2}\,\mu m^{-1}}$). The data around
30$\mathit{\times}10^{-15}\,{\rm W\,m^{-2}\,\mu m^{-1}}$ are very bright
sources of PNG 064,7${+}$0.5 and 305.1${+}$01.4, for which the spectra were
entirely saturated in the long exposure images. The bottom panel shows the
histogram of fractional 1$\sigma$ errors. The median value (${\sim}$6.7$\%$)
is shown by the gray dashed line.

The top panel of Figure 5 shows a histogram of the uncertainty in continuum
emission at $3.0\,\mu$m. The gray dashed line indicates the median of the
uncertainty, which is about $0.7{\times}10^{-15}\,{\rm W\,m^{-2}\,\mu m^{-1}}$
or $2\,$mJy. When the object is brighter than $2$–$5{\times}10^{-13}\,{\rm
W\,m^{-2}\,\mu m^{-1}}$, the pixels become saturated in the long exposure
image. For moderately bright objects, pixels around emission lines were
saturated. The spectra of extremely bright objects were completely saturated
in the long exposure images. The signal-to-noise ratio of the spectrum depends
on the fraction of saturated pixels. PNG 064.7${+}$05.0 and 305.1${+}$01.4 are
extremely bright, with their spectrum completely saturated in the long
exposure images. Figure 5 (top) indicates that their uncertainties at
$3.0\,\mu$m are about 50 times worse than the others. The fractional
uncertainty at $3.0\,\mu$m is shown in the bottom panel of Figure 5. The
median of the fractional uncertainty is about 6.4%, indicated by the vertical
dashed line. This means that, for half of the PNSPC samples, the continuum
emission at $3.0\,\mu$m was detected with a signal-to-noise ratio larger than
about 15.

The full width half maximum (FWHM) of the spectral PSF of the IRC, equivalent
to the FWHM of an unresolved emission line, is about $0.035\,\mu$m. Thus, the
spectral resolution is about $\lambda/\Delta\lambda\sim 100$. When the object
is extended for the IRC, the spectral resolution is degraded. The FWHM of the
spectral PSF, estimated from spectral fitting (see Section 4.3), is listed in
the seventh column of Table 1. PN G322.5${-}$05.2 is the most extended object
in the PNSPC catalog and its spectral resolution was estimated to be about
$\lambda/\Delta\lambda\sim 40$ at 4$\,\mu$m.

###  4.2 Extinction

Foreground extinction towards the objects was estimated based on an intensity
ratio of H$\beta$ to Brackett-$\alpha$ (Br$\alpha$). The intensities of
H$\beta$ were obtained from literature (Acker et al., 1992, and references
therein). We measured the intensities of Br$\alpha$ from the AKARI spectra by
fitting with a Gaussian function. We defined $I_{\rm H\beta}$ and $I_{\rm
Br\alpha}$ as the intensities of H$\beta$ and Br$\alpha$. The observed
intensity ratio follows the relation:

$\frac{I_{\rm H\beta}^{\rm obs}}{I_{\rm Br\alpha}^{\rm obs}}=\frac{I_{\rm
H\beta}^{0}{\rm e}^{-\tau_{\rm H\beta}}}{I_{\rm Br\alpha}^{0}{\rm
e}^{-\tau_{\rm Br\alpha}}},$ (2)

where $I^{\rm obs}_{X}$ and $I^{0}_{X}$ are the observed and intrinsic
intensities of the line $X$, and $\tau_{X}$ is the extinction of the line $X$.
We assumed that the nebula was totally opaque for Lyman photons (Case B in
Baker & Menzel (1938)). Then, the intrinsic intensity ratio $\left({I_{\rm
H\beta}^{0}}/{I_{\rm Br\alpha}^{0}}\right)$ was assumed to be ${\sim}12.853$,
given by the Case B line ratio calculated for the electron density of
$10^{4}\,{\rm cm^{-3}}$ and the electron temperature of $10^{4}\,$K from
Storey & Hummer (1995). We adopted the extinction curve given by Mathis (1990)
and the extinction at the $V$-band was derived as

${\rm A}_{V}({\rm H\beta})=2.39-0.95\ln\left(\frac{I_{\rm H\beta}^{\rm
obs}}{I_{\rm Br\alpha}^{\rm obs}}\right).$ (3)

The coefficients in Equation (3) depends on the assumed electron temperature
and density. When the assumed electron temperature increases to
$2{\times}10^{4}\,$K, ${\rm A}_{V}$ will increase by about 0.3. The effect of
the electron density on ${\rm A}_{V}$ is much smaller than 0.3 for the range
from $10^{2}$ to $10^{6}\,{\rm cm^{-3}}$. The systematic uncertainty in ${\rm
A}_{V}$, chiefly attributable to the electron temperature uncertainty, was
estimated to be less than $0.3\,$mag. The estimated ${\rm A}_{V}({\rm
H\beta})$ is listed in the fourth colunm of Table AKARI/IRC Near-Infrared
Spectral Atlas of Galactic Planetary Nebulae.

###  4.3 Spectral Fitting

The intensities of the spectral features were measured by spectral fitting.
The fitted function was assumed to be a linear combination of the spectral
features as

$F_{\lambda}(\lambda)=\Bigl{[}f_{\lambda}^{\rm cont}(\lambda)+f_{\lambda}^{\rm
line}(\lambda)+f_{\lambda}^{\rm dust}(\lambda)\Bigr{]}{\rm
e}^{-\tau(\lambda)},$ (4)

where $f_{\lambda}^{\rm cont}$, $f_{\lambda}^{\rm line}$, and
$f_{\lambda}^{\rm dust}$ were the components of continuum, emission lines, and
dust features, and $\tau(\lambda)$ was the optical depth at $\lambda$. The
functional shape of $\tau(\lambda)$ was given by a cubic spline function that
interpolated the extinction curve of Mathis (1990) at every data point of the
IRC spectrum. The amount of the extinction at the $V$-band, ${\rm
A}_{V}=\tau(V)$, was included as a fitting parameter.

The continuum emission, $f_{\lambda}^{\rm cont}$, was given by a polynomial
function, $f_{\lambda}^{\rm cont}=\sum_{l=0}^{N}c_{l}\lambda^{l}$, where
$c_{l}$’s were the fitting parameters. The order $N$ was defined for each
object, usually $N=2$ or $3$. This was sufficient to represent the
contributions from free-free and hot thermal dust emission. Some PNe showed a
sudden increase in the continuum emission around $\lambda\sim 3.6\,\mu$m, for
instance, PN G064.7${+}$05.0 in Figure 4. The existence of this emission was
mentioned in Boulanger et al. (2011), but the carrier of this emission has not
been identified. It was difficult to fit this profile with such a low-order
polynomial function. Thus, for those objects with such an increase, we added a
step-like function in the components of the continuum emission as

$f_{\lambda}^{\rm
cont}(\lambda)=\sum_{l=0}^{N}c_{l}\lambda^{l}+c\left[~{}\frac{1}{2}+\frac{1}{2}{\rm
erf}\left(\frac{\lambda-3.65{\,\rm\mu m}}{\Delta_{\rm step}}\right)\,\right],$
(5)

where $c$ was the fitting parameter, ${\rm erf}(x)$ was the error function,
and $\Delta_{\rm step}$ was the width of the step function, which was
tentatively fixed at 0.135$\,\mu$m. This component strongly appears in PNG
037.8${-}$06.3, 064.7${+}$050, 089.8${-}$05.1, and 268.4${+}$02.4.

The emission line profile was approximated by a Gaussian function. The line
emission component, $f_{\lambda}^{\rm line}$, was approximated by a
combination of Gaussian functions:

$f_{\lambda}^{\rm
line}(\lambda)=\sum_{m}\frac{c_{m}}{\sqrt{2\pi}\sigma}\exp\left[\,-\frac{(\lambda-\lambda_{m0})^{2}}{2\sigma^{2}}\,\,\right],$
(6)

where $\lambda_{m0}$ was the central wavelengths of the $m$-th emission line
and $c_{m}$’s were the parameters to indicate the strength of the lines. The
central wavelengths were fixed in the fitting. The line width of the
Br$\alpha$ line was measured by fitting with a Gaussian function prior to the
fitting and the line widths of other emission lines were assumed to be the
same as Br$\alpha$. The lines included in the fitting are listed in Table 3.
The assignment and central wavelength are shown in the first and second
column. In the fitting, we did not include the lines which were apparently not
detected. Some of the H I and He II recombination lines appear at the same
wavelength and it was impossible to isolate them. Thus, the relative
intensities of the H I and He II recombination lines were fixed, assuming the
Case B condition. The relative intensity was adopted from Storey & Hummer
(1995) for the electron temperature and the electron density of $10^{4}\,$K
and $10^{4}\,{\rm cm^{-2}}$. The variations in the relative intensity with the
electron temperature and density were almost negligible compared to the
uncertainty in the observed spectra.

Table 3: List of Line Features

Name |  $\lambda_{0}$ ($\mu$m)
---|---
Brakett-$\alpha^{\dagger}$ | 4.051
Brakett-$\beta^{\dagger}$ | 2.625
Pfund-$\beta^{\dagger}$ | 4.653
Pfund-$\gamma^{\dagger}$ | 3.740
Pfund-$\delta^{\dagger}$ | 3.296
Pfund-$\epsilon^{\dagger}$ | 3.039
Pfund-$\zeta^{\dagger}$ | 2.873
Pfund-$\eta^{\dagger}$ | 2.758
Humpleys-$\epsilon^{\dagger}$ | 4.671
Humpleys-$\zeta^{\dagger}$ | 4.376
He I(3Po-3D) | 3.704
He I(1Po-1D) | 4.123
He I(3S-3Po) | 4.296
He I(1Po-1S) | 4.607
He I(3Po-3S) | 4.695

Name |  $\lambda_{0}$ ($\mu$m)
---|---
He II(7-6)‡ | 3.092
He II(9-7)‡ | 2.826
He II(8-7)‡ | 4.764
He II(12-8)‡ | 2.625
He II(11-8)‡ | 3.096
He II(10-8)‡ | 4.051
He II(14-9)‡ | 3.145
He II(13-9)‡ | 3.544
He II(12-9)‡ | 4.218
He II(14-10)‡ | 4.652
H2(1-0) | 2.802
H2(1-0) | 3.003
H2(1-0) | 3.234
H2(0-0) | 3.836
H2(0-0) | 4.181
$[$Mg IV$]$ | 4.487
$[$Ar VI$]$ | 4.530

The intrinsic spectral profiles of the PAH emission and the aliphatic feature
complex were assumed to be given by a combination of Lorentzian functions
which need to be convoluted with the resolution given by the instrument. Thus,
their spectral profiles were approximated by the Lorentzian function
convoluted with the spectral PSF of the IRC, which was approximated by a
Gaussian. The component from dust emission, $f_{\lambda}^{\rm dust}$, was
defined by

$f_{\lambda}^{\rm
dust}(\lambda)=\sum_{n}\frac{c_{n}}{\pi\sqrt{2\pi}\sigma}\int{\rm
d}\lambda^{\prime}{\rm
e}^{-\frac{(\lambda-\lambda^{\prime})^{2}}{2\sigma^{2}}}\frac{\Delta_{n}}{\Delta_{n}^{2}+(\lambda^{\prime}-\lambda_{n0})^{2}},$
(7)

where $\Delta_{n}$ and $\lambda_{n0}$ were the width and peak wavelength of
the $n$-th dust emission and $c_{n}$’s were the fitting parameters. The
adopted values of $\Delta_{n}$’s and $\lambda_{n0}$’s were listed in Table 4.
The PAH feature at 3.3$\,\mu$m was mainly composed of the 3.30$\,\mu$m
feature, but the 3.25$\,\mu$m feature was added to account for a slight change
in the spectral profile of the 3.3$\,\mu$m feature. For instance the
3.3$\,\mu$m feature of PNG 320.9${+}$02.0 show an extended blue component,
which cannot be well-fitted without the 3.25$\,\mu$m component. Mori et al.
(2012) used a combination of four Lorentzian functions to describe the
3.4–3.5$\,\mu$m feature complex (C−Hal) in spectra obtained with the IRC. We
used a combination of the four components to describe the C−Hal feature. The
central wavelengths and widths were adopted from Mori et al. (2012).

Table 4: List of Dust Features Name |  $\lambda_{0}$ ($\mu$m) |  $\Delta$ ($\mu$m)
---|---|---
PAH 3.25† | 3.248 | 0.005
PAH 3.30† | 3.296 | 0.021
C−Hal 3.41‡ | 3.410 | 0.030
C−Hal 3.46‡ | 3.460 | 0.013
C−Hal 3.51‡ | 3.512 | 0.013
C−Hal 3.56‡ | 3.560 | 0.013

Define $F_{\lambda}^{\rm obj}(\lambda)$ and $\sigma_{\lambda}(\lambda)$ as the
observed flux and its uncertainty at $\lambda$. We assumed that the residual
$\Delta_{\lambda}(\lambda)=F_{\lambda}^{\rm
obj}(\lambda)-F_{\lambda}(\lambda)$ followed a normal distribution with the
variance of $\sigma^{2}_{\lambda}(\lambda)$. The likelihood function was
defined as

$\mathcal{L}\propto\prod_{i}\exp\left[-\frac{1}{2}\left(\frac{\Delta_{\lambda}(\lambda_{i})}{\sigma_{\lambda}(\lambda_{i})}\right)^{2}\right],$
(8)

where $\lambda_{i}$ was the wavelength of the $i$-th spectral element. The
fitting parameters could be defined by maximizing Equation (8). However, it
was difficult to accurately derive the amount of the extinction, ${\rm
A}_{V}$, only from the near-infrared spectrum (see, Appendix A). To make the
fitting stable, we used the extinction estimated in Section 4.2 to provide a
prior distribution of the extinction

$P({\rm A}_{V})\propto\exp\left[-\frac{1}{2}\left(\frac{{\rm A}_{V}{-}{\rm
A}_{V}({\rm H\beta})}{\sigma^{\prime\prime}}\right)^{2}\right],$ (9)

where ${\rm A}_{V}({\rm H\beta})$ was the extinction estimated from the
H$\beta$ to Br$\alpha$ intensity ratio and $\sigma^{\prime\prime}$ was
tentatively fixed at $0.3\,$mag, estimated from the systematic error. The
fitting parameters were derived by maximizing the product of Equations (8) and
(9) with the constraints that the parameters of ${\rm A}_{V}$, $c$, $c_{m}$
and $c_{n}$ should be non-negative. The uncertainties of the fitting
parameters were estimated based on a Monte Carlo simulation: The spectrum of
the target, $\tilde{F}(\lambda)$ was simulated assuming a normal distribution
of flux with a mean of $F^{\rm obj}_{\lambda}(\lambda)$ and a variance of
$\sigma_{\lambda}(\lambda)$. The fitting parameters were derived for
$\tilde{F}(\lambda)$. This procedure was repeated 1 000 times and the
probability distributions of the fitting parameters were obtained. The
confidence interval of the fitting parameters was defined to account for 68%
of the trials.

Figure 6: The signal-to-noise ratio (${\rm S/N}$) is plotted against the
intensity of the emission features, indicating a typical detection limit of
emission features. The blue circles represent the ${\rm S/N}$ ratio of the
3.3$\,\mu$m PAH feature, while the red squares show that of the
3.4–3.5$\,\mu$m aliphatic feature complex.

The extinction obtained by the fitting (${\rm A}_{V}(\rm fit.)$) is listed in
the fifth column of Table AKARI/IRC Near-Infrared Spectral Atlas of Galactic
Planetary Nebulae. Table 5 lists the extinction-corrected intensities of
Br$\alpha$ at $4.05\,\mu$m, He I at $4.30\,\mu$m, He II at $3.09\,\mu$m, the
PAH feature at $3.3\,\mu$m, the aliphatic feature complex in
$3.4$–$3.5\,\mu$m, [Mg IV] at $4.49\,\mu$m, and [Ar VI] at $4.53\,\mu$m. These
emission features were strong and widely detected among the PNSPC samples.
Other line features were weak or not detected in the majority of the targets
and thus were not included in the table. The equivalent widths of those are
listed in Table 6. Note that [Mg IV] and [Ar VI] are so close that their
spectral profiles are in part overlapping. Their uncertainties are relatively
large compared to other lines, because the effect of overlapping was taken
into account. Figure 6 shows the signal-to-noise ratio against the intensity
of the $3.3\,\mu$m PAH feature and the 3.4–3.5$\,\mu$m aliphatic feature
complex by the blue circles and the red squares. Figure 6 indicates that the
emission feature stronger than ${\sim}2{\times}10^{-16}\,{\rm W\,m^{-2}}$ was
detected with a 3$\sigma$-confidence level.

Table 5: Extinction Corrected Line Intensity

PN G | Bracket-$\alpha$ | He II$(3.09{\rm\mu m})$ | He I$(4.30{\rm\mu m})$ | PAH$(3.3{\rm\mu m})$ | C−Hal$(3.4$-$3.5{\rm\mu m})$ | [Mg IV]$(4.49{\rm\mu m})$ | [Ar VI]$(4.53{\rm\mu m})$
---|---|---|---|---|---|---|---
| $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$
000.3${+}$12.2 | $\phantom{0}\phantom{0}\phantom{0}2.74_{{-}0.04}^{{+}0.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.14_{{-}0.03}^{{+}0.03}$ | ${<}0.11$ |  $\cdots$ |  $\cdots$ |  $\cdots$
002.0${-}$13.4 | $\phantom{0}\phantom{0}\phantom{0}2.05_{{-}0.03}^{{+}0.04}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.31_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.25_{{-}0.05}^{{+}0.05}$ | ${<}0.10$ |  $\cdots$ |  $\cdots$
003.1${+}$02.9 | $\phantom{0}\phantom{0}\phantom{0}3.16_{{-}0.04}^{{+}0.04}$ | ${<}0.53$ | $\phantom{0}\phantom{0}\phantom{0}0.43_{{-}0.04}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.94_{{-}0.16}^{{+}0.25}$ | $\phantom{0}\phantom{0}\phantom{0}0.49_{{-}0.08}^{{+}0.09}$ | $\phantom{0}\phantom{0}\phantom{0}0.35_{{-}0.04}^{{+}0.05}$ |  $\cdots$
011.0${+}$05.8 | $\phantom{0}\phantom{0}\phantom{0}1.09_{{-}0.04}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.13_{{-}0.03}^{{+}0.03}$ | ${<}0.13$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}1.11_{{-}0.08}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.20_{{-}0.05}^{{+}0.04}$
027.6${-}$09.6 | $\phantom{0}\phantom{0}\phantom{0}1.12_{{-}0.02}^{{+}0.04}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.10_{{-}0.01}^{{+}0.01}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
037.8${-}$06.3 | $\phantom{0}\phantom{0}\phantom{0}4.61_{{-}0.10}^{{+}0.24}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}1.80_{{-}0.09}^{{+}0.13}$ | $\phantom{0}\phantom{0}\phantom{0}6.64_{{-}0.21}^{{+}0.40}$ | $\phantom{0}\phantom{0}\phantom{0}2.60_{{-}0.14}^{{+}0.21}$ |  $\cdots$ |  $\cdots$
038.2${+}$12.0 | $\phantom{0}\phantom{0}\phantom{0}2.18_{{-}0.06}^{{+}0.04}$ |  $\cdots$ | ${<}0.13$ | $\phantom{0}\phantom{0}\phantom{0}0.45_{{-}0.05}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.12_{{-}0.02}^{{+}0.03}$ |  $\cdots$ |  $\cdots$
043.1${+}$03.8 | $\phantom{0}\phantom{0}\phantom{0}0.45_{{-}0.01}^{{+}0.01}$ |  $\cdots$ |  $\cdots$ | ${<}0.06$ | ${<}0.01$ |  $\cdots$ |  $\cdots$
046.4${-}$04.1 | $\phantom{0}\phantom{0}\phantom{0}2.43_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.11_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.32_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.40_{{-}0.05}^{{+}0.04}$ | ${<}0.16$ |  $\cdots$ |  $\cdots$
051.4${+}$09.6 | $\phantom{0}\phantom{0}\phantom{0}3.25_{{-}0.02}^{{+}0.06}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.52_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.97_{{-}0.07}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.05}^{{+}0.04}$ |  $\cdots$ |  $\cdots$

Note. — †,‡: relative intensities of these lines are fixed assuming the Case B
condition.

Note. — †: they belong to the PAH feature at 3.3$\,\mu$m. ‡: they belong to
the aliphatic feature complex in 3.4–3.5$\,\mu$m.

Note. — Table 5 is published in its entirety in the electronic edition of the
Astrophysical Journal. A portion is shown here for guidance regarding its form
and content.

Table 6: Extinction Corrected Line Equivalent Width

PN G | Bracket-$\alpha$ | He II$(3.09{\rm\mu m})$ | He I$(4.30{\rm\mu m})$ | PAH$(3.3{\rm\mu m})$ | C−Hal$(3.4$-$3.5{\rm\mu m})$ | [Mg IV]$(4.49{\rm\mu m})$ | [Ar VI]$(4.53{\rm\mu m})$
---|---|---|---|---|---|---|---
| Å | Å | Å | Å | Å | Å | Å
000.3${+}$12.2 | $\phantom{0}2825.6_{{-}38.2}^{{+}47.3}$ |  $\cdots$ | $\phantom{0}\phantom{0}154.5_{{-}32.7}^{{+}35.5}$ | ${<}130.7$ |  $\cdots$ |  $\cdots$ |  $\cdots$
002.0${-}$13.4 | $\phantom{0}2938.4_{{-}39.9}^{{+}64.0}$ |  $\cdots$ | $\phantom{0}\phantom{0}481.9_{{-}27.1}^{{+}42.1}$ | $\phantom{0}\phantom{0}435.3_{{-}84.6}^{{+}86.8}$ | ${<}181.4$ |  $\cdots$ |  $\cdots$
003.1${+}$02.9 | $\phantom{0}2105.7_{{-}25.5}^{{+}26.5}$ | ${<}236.7$ | $\phantom{0}\phantom{0}343.7_{{-}30.2}^{{+}25.6}$ | $\phantom{0}\phantom{0}665.7_{{-}113.7}^{{+}176.0}$ | $\phantom{0}\phantom{0}365.1_{{-}59.5}^{{+}68.0}$ | $\phantom{0}\phantom{0}324.3_{{-}42.0}^{{+}51.4}$ |  $\cdots$
011.0${+}$05.8 | $\phantom{0}2005.1_{{-}68.8}^{{+}61.4}$ | $\phantom{0}\phantom{0}144.8_{{-}34.2}^{{+}32.1}$ | ${<}266.9$ |  $\cdots$ |  $\cdots$ | $\phantom{0}2605.4_{{-}179.7}^{{+}127.9}$ | $\phantom{0}\phantom{0}486.2_{{-}111.4}^{{+}101.8}$
027.6${-}$09.6 | $\phantom{0}3229.6_{{-}44.8}^{{+}128.8}$ |  $\cdots$ | $\phantom{0}\phantom{0}328.8_{{-}27.6}^{{+}35.8}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
037.8${-}$06.3 | $\phantom{0}\phantom{0}482.1_{{-}10.0}^{{+}25.4}$ |  $\cdots$ | $\phantom{0}\phantom{0}182.2_{{-}\phantom{0}8.6}^{{+}13.6}$ | $\phantom{0}1342.1_{{-}42.1}^{{+}80.2}$ | $\phantom{0}\phantom{0}531.1_{{-}29.1}^{{+}42.6}$ |  $\cdots$ |  $\cdots$
038.2${+}$12.0 | $\phantom{0}2863.3_{{-}84.4}^{{+}54.5}$ |  $\cdots$ | ${<}192.5$ | $\phantom{0}\phantom{0}709.0_{{-}75.8}^{{+}55.0}$ | $\phantom{0}\phantom{0}204.3_{{-}38.7}^{{+}47.2}$ |  $\cdots$ |  $\cdots$
043.1${+}$03.8 | $\phantom{0}1316.2_{{-}37.5}^{{+}42.9}$ |  $\cdots$ |  $\cdots$ | ${<}230.0$ |  $\cdots$ |  $\cdots$ |  $\cdots$
046.4${-}$04.1 | $\phantom{0}3171.2_{{-}\phantom{0}5.0}^{{+}29.3}$ | $\phantom{0}\phantom{0}\phantom{0}99.6_{{-}18.0}^{{+}17.8}$ | $\phantom{0}\phantom{0}475.1_{{-}\phantom{0}9.3}^{{+}29.6}$ | $\phantom{0}\phantom{0}595.7_{{-}75.1}^{{+}65.3}$ | ${<}250.8$ |  $\cdots$ |  $\cdots$
051.4${+}$09.6 | $\phantom{0}1882.4_{{-}13.5}^{{+}36.4}$ |  $\cdots$ | $\phantom{0}\phantom{0}315.8_{{-}12.1}^{{+}15.0}$ | $\phantom{0}\phantom{0}740.7_{{-}56.1}^{{+}41.7}$ | $\phantom{0}\phantom{0}180.1_{{-}42.6}^{{+}32.7}$ |  $\cdots$ |  $\cdots$

Note. — Table 6 is published in its entirety in the electronic edition of the
Astrophysical Journal. A portion is shown here for guidance regarding its form
and content.

Figure 7: The AKARI/IRC 2.5–5.0$\,\mu$m spectra. Explanations of the lines are
shown in the bottom of the figures. Plots for all sources are available in the
electronic edition of the journal.

##  5 Discussion

###  5.1 Biases in the PNSPC samples

####  5.1.1 Galactic Coordinates

Figure 8: Histograms of PNe in the Galactic coordinates. The left panel shows
the histogram of the Galactic longitude, while the right panel shows that of
the Galactic latitude. The histograms for the PNSPC objects are shown by the
blue boxes. The gray filled boxes represent the distribution of all the
Galactic PNe in Acker et al. (1992).

We compare the distribution of the PNSPC samples in the Galactic coordinates
with that of the PNe in Acker et al. (1992), which are assumed to represent
the distribution of all the PNe in the Milky Way. The histograms of the
Galactic longitude and latitude are shown in the left and right panels of
Figure 8. The histograms of the PNSPC samples are shown by the blue lines,
while the histograms of PNe in Acker et al. (1992) are shown by the gray
filled bars. The total number of the PNe in Acker et al. (1992) is 1143. The
longitude histogram of the PNSPC samples looks broader than that of the PNe in
Acker et al. (1992), while the latitude histogram of the PNSPC samples does
not show a large deviation from that of the PNe in Acker et al. (1992). We
investigate the differences by Kolmogorov-Smirnov test. The values of
$\chi^{2}_{\nu{=}2}$ are about 16 for the longitude and 4 for the latitude.
The results suggest that the deviation of the longitude is highly significant
and that the PNSPC samples are biased toward PNe in the Galactic disk rather
than those in the bulge. Figure 9 shows the position of the PNSPC samples
projected onto the Galactic plane. The distances to the objects are taken from
literature (Acker, 1978; Pottasch, 1983; Maciel, 1984; Amnuel et al., 1984;
Gathier et al., 1986a, b; Sabbadin, 1986; Cahn et al., 1992; Acker et al.,
1992, and references therein). Figure 9 shows that most of the PNSPC samples
are within $5$ kpc of the Sun, even when accounting for uncertainties in the
distance estimate. This also supports that the PNSPC samples mainly consist of
PNe in the Galactic disk.

Figure 9: Distribution of the PNSPC samples on the Galactic Plane. The red
cross shows the locus of the Sun. The purple circles show the positions of the
PNSPC samples.

####  5.1.2 Effective Temperature and Age

The central star of a PN becomes hot as it evolves. The effective temperature
of the PN can be used as an indicator of the age of the PN. The timescale of
the evolution depends on the mass of the central star (e.g., Blöcker, 1995;
Schönberner, 1983). Although the individual age of the PN is difficult to
accurately derive from the effective temperature, the distribution of the
effective temperature reflects the bias in the age of the PNSPC samples. The
effective temperatures were collected from literature. The temperature and its
references are listed in the sixth and seventh columns of Table AKARI/IRC
Near-Infrared Spectral Atlas of Galactic Planetary Nebulae. The effective
temperature is estimated with several different methods. The effective
temperatures estimated based on a model atmosphere should be the most
reliable. The temperatures estimated in Mendez et al. (1988) and Harrington &
Feibelman (1983) are preferentially used, if available. The typical error for
temperatures measured by this method is about 10% (Mendez et al., 1988).
Otherwise, the effective temperatures estimated with the Zanstra or the Energy
Balance methods are used. The Zanstra temperatures are estimated based on H I,
He I, and He II recombination lines. Since the radiation-bounded condition is
assumed in the Zanstra method, the Zanstra temperature estimated using the
line with the highest ionization potential is most reliable. The Zanstra
temperatures are used with the preferential order of He II, He I, and H I. A
typical uncertainty in the Zanstra temperature is as large as 10,000 K in the
worst case (Phillips, 2003). Preite-Martinez et al. (1991) reported that the
typical uncertainty in the temperature with the Energy Balance method is no
more than 20%. We assume that a typical uncertainty in these methods is about
20%. Finally, the effective temperature was obtained for $67$ of $72$ objects
in the catalog. When multiple references are available, the averaged value is
adopted.

Figure 10 shows the distribution of the effective temperature in the PNSPC
samples. Phillips (2003) collected the effective temperature of 373 Galactic
PNe using the Zanstra method. Their samples were widely collected from
literature without any limitation. Thus, we assume that their samples are not
biased and that the temperature distribution of Phillips’ samples represents
that of the whole Galactic PNe (gray dashed line). The median of the effective
temperature for the PNSPC samples is about $50\,000\,{\rm K}$, while that for
Phillips’ data is about $80\,000\,{\rm K}$. Figure 10 indicates that the PNSPC
samples are biased toward low-temperature or young PNe, possibly due to the
target selection bias: the targets are limited by the apparent size
(${\sim}3^{\prime\prime}$).

Figure 10: Cumulative histogram of the effective temperature of Galactic PNe.
The blue solid line shows the histogram for the PNSPC samples. The gray dashed
line represents the temperature distribution of all the Galactic PNe in
Phillips (2003).

###  5.2 Accuracy of the Absolute Intensity

One of the major characteristics of the PNSPC catalog is slit-less
spectroscopy in the Np-window, which allows us to collect all of the flux from
the target. Since the IRC spectrum totally covers the WISE W1 band, the
accuracy of the absolute flux density is evaluated by comparing the PNSPC
spectra with the WISE W1 photometry from WISE All-Sky Release Catalog (Cutri
et al., 2012). Define $R^{\rm W1}$ as the relative response curve of the WISE
W1 band (per photon; Wright et al., 2010). The flux in the W1 band estimated
from the IRC spectrum is defined as

$F^{\rm IRC}_{\nu}({\rm W1})=\frac{\displaystyle\int F^{\rm
obj}_{\nu}(\nu)R^{\rm W1}(\nu)\frac{{\rm
d}\nu}{\nu}}{\displaystyle\int\left(\frac{\nu_{\rm iso}}{\nu}\right)^{2}R^{\rm
W1}(\nu)\frac{{\rm d}\nu}{\nu}},$ (10)

where $\nu_{\rm iso}$ is the isophotal frequency of the W1 band (3.35$\,\mu$m)
and $F^{\rm obj}_{\nu}$ is the observed flux density in units of Jy. Figure 11
shows the estimated flux density in the W1 band against the WISE W1 catalog
data. It confirms that the W1 flux density estimated from the IRC spectra,
$F^{\rm IRC}_{\nu}({\rm W1})$, is consistent with the WISE W1 data in a wide
range from about $0.01$ to $5\,{\rm Jy}$. The histogram of the AKARI to WISE
W1 flux ratio is shown in Figure 12. Errors in Figure 12 are calculated by a
Monte Carlo simulation with the uncertainty in the flux ratio. The ratios are
distributed with the mean of $1.01{\pm}0.01$ and the standard deviation of
$0.21{\pm}0.02$. Three PNe (PNG 285.7$-$14.9, 324.8$-$01.1, and 305.1$+$01.4)
show significant deviations larger than 50%. For PNG 285.7$-$14.9 and
305.1$+$01.4, their AKARI W1 fluxes are larger than those of WISE. Both
objects are apparently extended in WISE W1 images. The deviations may be
attributed to the loss of the flux in WISE photometry. Furthermore, PNG
305.1$+$01.4 is the brightest object in the PNSPC sample. The WISE detector
starts to saturate in the W1 band at $\sim$0.17$\,{\rm Jy}$ (Wright et al.,
2010). This may also cause an error in WISE photometry of PNG 305.1$+$01.4.
The AKARI W1 flux of PNG 324.8$-$01.1 is smaller than the WISE W1 flux. PNG
324.8$-$01.1 is located in a crowded region, so that the IRC field of view may
not be wide enough to estimate background emission accurately. The loss of the
AKARI W1 flux is attributable to the error in the estimation of the background
emission. Thus, although the absolute continuum intensity of PNG 324.8$-$01.1
may be erroneous, the intensity of emission features is not affected by the
estimation of background emission. The absolute flux of the present catalog is
concluded to be accurate within $20$%.

Figure 11: Flux comparison between the AKARI and WISE observations. The
vertical axis shows the flux in the WISE W1 filter estimated from the
AKARI/IRC spectra, while the horizontal axis shows the flux in the WISE All-
Sky Release Catalog (Cutri et al., 2012). When the deviation between the AKARI
and WISE W1 fluxes is larger than 50%, the data point is labeled with the PNG
ID. Figure 12: Distribution of the flux ratio: the flux in the WISE W1 filter
estimated from the AKARI/IRC spectra to that from the WISE All-Sky Release
Catalog.

###  5.3 Extinction within the Individual Nebula

The PNSPC spectra include Brackett-$\alpha$ (Br$\alpha$), the hydrogen
recombination line at 4.05$\,\mu$m, which enables us to estimate the
extinction towards the objects using the relative intensity of H$\beta$ to
Br$\alpha$ (the intensity of H$\beta$ is from Acker et al. (1992), see Section
4.2). The cumulative histogram of the total extinction towards the PNSPC
samples, $A_{V}({\rm H}\beta)$, is shown by the dotted line in Figure 13. The
extinction toward the PNSPC samples are less than $6\,$mag. at the $V$-band.
About 70% of the PNSPC samples have $A_{\rm V}({\rm H}\beta)<2\,$mag.,
suggesting that most of the PNSPC samples are not heavily obscured. This is
consistent with the Galactic distribution of the PNSPC sample shown in Section
5.1.1.

The extinction values calculated in Section 4.2 include the contribution from
their circumstellar envelope, $A_{V,\,{\rm PN}}$, and the interstellar medium
to the object, $A_{V,\,{\rm ISM}}$. The contribution from the interstellar
medium, $A_{V,\,{\rm ISM}}$, can be estimated using the extinction map based
on the Digitized Sky Survey (Dobashi et al., 2005a, b). The extinction map is
given in the resolution of $2\arcmin{\times}2\arcmin$. We calculate the
averaged extinction values within a $6\arcmin$ radius around the object
$A_{V}({\rm DSS})$ and assumed them as $A_{V,\,{\rm ISM}}$. Dobashi et al.
(2005a) showed that a systematic error in $A_{V}({\rm DSS})$ is typically less
than 0.2 mag for $A_{V}({\rm DSS})<5\,$mag. We estimate the uncertainty in
$A_{V,\,{\rm ISM}}$ from the scatter of $A_{V}({\rm DSS})$ within the
$6\arcmin$ circle taking into account the systematic error. Note that the
extinction $A_{V,\,{\rm ISM}}$ estimated here may have a large uncertainty.
The extinction from the circumstellar envelope, defined by $A_{V}({\rm
H}\beta)-A_{V}({\rm DSS})$, is shown by the solid line in Figure 13. Some
objects show negative extinction values (${\sim}0.5\,$mag.), possibly due to
the overestimation of $A_{V,\,{\rm ISM}}$. Figure 14 shows the dependence of
$A_{V}({\rm H}\beta)-A_{V}({\rm DSS})$ on the distance towards the PN. We find
that PNe with extinction ${>}2\,$mag. frequently appear around 2 kpc. The name
of the constellation is added next to those PNe, indicating that most of them
are in the regions around Cygnus and Norma as indicated by the orange and
green symbols. The extinction $A_{V,\,{\rm ISM}}$ for these PNe may be
underestimated or have large local fluctuations, but this affects only about
10% of the PNSPC samples. Except for the objects in the Cygnus and Norma
regions, Figure 14 does not show any trend with the distance, suggesting that
the $A_{V}({\rm H}\beta)-A_{V}({\rm DSS})$ value is attributable to the
extinction internal to the PN. Figure 13 indicates that the median of the
circumstellar extinction is about 0.8 mag. and about $40\%$ of the PNe show
extinction larger than $1\,$mag. suggesting that the circumstellar envelope of
a PN is generally optically thick in the UV. Ohsawa et al. (2012) investigated
the spatial distribution of mid-infrared dust emission of PN G095.2${+}$00.7,
a young and UV-thick Galactic PN, and suggest that the evolution of a UV-thick
circumstellar envelope may have a significant impact on the appearance of the
mid-infrared spectrum of the PN. The present results suggest that PNe spectra
should be investigated by taking into account the radiation transfer within
the nebula, and the gradient in the dust temperature.

Figure 13: Cumulative histogram of the extinction at the $V$-band. The dotted
line shows the histogram of the total extinction towards the PN. The solid
line shows the histogram of the extinction without the contribution from the
interstellar medium. Figure 14: Net extinction at the $V$-band is plotted
against a distance towards the PN. Errors in the distance are assumed to be
about 20%. The name of the constellation is added next to the symbols for the
PN with the net extinction ${>}2.0\,$mag. The PNe in Cygnus and Vulpecula are
indicated by the orange filled circles, while the PNe in Norma, Lupus and
Circinus are indicated by the green filled circles.

###  5.4 Equivalent Width of Ionized Gas Emission Lines

The spectra in the PNSPC catalog contain several emission lines, including
hydrogen and helium recombination lines and fine-structure lines of [Mg IV] at
4.49$\,\mu$m and [Ar VI] at 4.53$\,\mu$m. These emission lines should reflect
the characteristics of the radiation field of the circumstellar envelope.
Figure 15 shows the equivalent widths of Br$\alpha$, He I at 4.30$\,\mu$m, He
II at 3.09$\,\mu$m, and the summation of [Mg IV] and [Ar VI] against the
effective temperature of the central star. Since the [Mg IV] and [Ar VI] lines
are close to each other, the equivalent width of the summation of these lines
is used. The data whose signal-to-noise ratio of the equivalent width is less
than three are replaced by 3-$\sigma$ upper limits. When the emission is not
detected, the effective temperature is indicated by the crosses. The
equivalent width of Br$\alpha$ is typically about $1$–$3{\times}10^{3}\,$Å and
does not show a clear dependence on the effective temperature. The He I line
is seen from 20 000 to 150 000 K. Its equivalent width is almost constant at
about $2{\times}10^{2}\,$Å. It shows a small increase from 30 000–50 000 K,
possibly explained by the increase in photons with enough energy to ionize
${\rm He}$ with increasing effective temperature. When the effective
temperature exceeds 50 000 K, the He I equivalent width stops increasing and
shows a small decrease. At the same time, the He II lines start to be
detected, suggesting that high-energy photons are in part used to ionize ${\rm
He}^{+}$. The decrease in the He I equivalent width is attributable to the
ionization balance between ${\rm He}^{+}$ and ${\rm He}^{++}$. The He II, [Mg
IV], and [Ar VI] lines are not detected until the effective temperature
exceeds about 50 000 K. The ionization potentials of He II, Mg IV, and Ar VI
are 54.41, 109.27, and 91.00 eV. Although the ionization potential of He II is
about two times lower than those of Mg IV, and Ar VI, the He II, [Mg IV], and
[Ar VI] lines start to appear at almost the same temperature in Figure 15. The
equivalent width of the He II line is typically about $2{\times}10^{2}\,$Å,
not showing a clear trend with the effective temperature. The equivalent width
of the [Mg IV]${+}$[Ar VI] becomes as large as $8{\times}10^{3}\,$Å at a high
temperature of about 100 000 K. Figure 16 shows the intensity ratio of the [Mg
IV]${+}$[Ar VI] to Br$\alpha$. The effective temperature of the PNe with the
ratio larger than unity ranges about 500 000–150 000 K. The [Mg IV] and [Ar
VI] lines are an indicator of high-temperature PNe as expected. But note that
some PNe with high effective temperature show a ratio less than unity. A ratio
less than unity does not necessarily indicate a PN with a low effective
temperature.

Figure 15: Equivalent widths of Brackett-$\alpha$ at 4.05$\,\mu$m (upper
left), He I at 4.30$\,\mu$m (upper right), He II at 3.09$\,\mu$m (lower left),
and [Mg IV] at 4.49$\,\mu$m ${+}$ [Ar VI] at 4.53$\,\mu$m (lower right)
against the effective temperature. The downward arrows indicate a 3-$\sigma$
upper limit. When the emission is not detected, the effective temperature is
indicated by the crosses. Figure 16: Intensity ratio of the summation of [Mg
IV] and [Ar VI] to Brackett-$\alpha$ against the effective temperature. When
the emission of [Mg IV] and [Ar VI] is not detected, the effective temperature
is indicated by the crosses.

###  5.5 PAH Features of Galactic PNe in the Near-Infrared

The PAH features appear both in the near- and mid-infrared, and the PAH
features in the mid-infrared are stronger than those in the near-infrared
(e.g., Schutte et al., 1993; Draine & Li, 2001). The PAH features of PNe in
the mid-infrared have been intensively investigated with Spitzer (e.g.,
Bernard-Salas et al., 2009; Stanghellini et al., 2007, 2012). Surveys of the
3.3$\,\mu$m PAH feature in Galactic PNe were carried out by Roche et al.
(1996) and Smith & McLean (2008). Their samples were, however, biased towards
carbon-rich objects. The PNSPC samples are not selected based on their
chemistry. The PNSPC catalog provides a useful data set to investigate the
near-infrared PAH features in Galactic PNe.

The type of dust features (carbon-rich or oxygen-rich) is thought to be
closely related to the abundance ratio of nebular gas. Several studies have
suggested that the intensities of the PAH features increases with the carbon-
to-oxygen abundance (C/O) ratio (e.g., Cohen et al., 1986; Roche et al., 1996;
Cohen & Barlow, 2005; Smith & McLean, 2008). However, PAH formation both in
carbon-rich and oxygen-rich environments has been suggested recently (Guzman-
Ramirez et al., 2014, 2011). Delgado-Inglada & Rodríguez (2014) measured the
C/O ratio of 51 Galactic PNe and confirmed that the PAH emission can be seen
even in PNe with ${\rm C/O}<1$. The C/O ratios of 11 PNe in the PNSPC catalog
were measured by Delgado-Inglada & Rodríguez (2014). Figure 17 shows the
equivalent width of the 3.3$\,\mu$m PAH feature against the C/O ratio. The C/O
ratio measured by collisionally excited lines (CEL) is indicated by the blue
circles, while that measured by recombination lines (RL) is shown by the red
squares. The downward arrows indicate non-detection of the 3.3$\,\mu$m PAH
features. Figure 17 shows that the 3.3$\,\mu$m PAH emission is detected even
in oxygen-rich environments, consistent with Delgado-Inglada & Rodríguez
(2014). Due to the small number of samples, however, it is difficult to claim
the correlation between the strength of the 3.3$\,\mu$m PAH feature and the
C/O ratio. Extensive measurements of the C/O ratio are encouraged.

Figure 17: Equivalent width of the 3.3$\,\mu$m PAH feature against the carbon-
to-oxygen (C/O) ratio. The C/O ratios are from Delgado-Inglada & Rodríguez
(2014). The C/O ratio measured by collisionally excited lines (CEL) is shown
by the blue circles, while the C/O ratio measured by recombination lines (RL)
is by the red squares. The arrows indicate the non-detection of the
3.3$\,\mu$m PAH feature.

Figure 18 shows a cumulative histogram of the signal-to-noise ratio of the
3.3$\,\mu$m PAH feature (hereafter, ${\rm S/N}(I_{3.3})$). The gray dotted
line shows the 35th percentile, which corresponds to ${\rm S/N}(I_{3.3})=3$.
The result suggests that about 65% of the PNSPC samples show band emission at
3.3$\,\mu$m. The 5–38$\,\mu$m spectra of Galactic PNe with Spitzer/IRS are
available in Stanghellini et al. (2012). We counted the number of PNe with PAH
features, obtaining 40% (60 of 150 PNe). Despite the intrinsic weakness of the
near-infrared PAH features, the PAH detection rate is as high in the near-
infrared as in the mid-infrared. The 3.3$\,\mu$m feature is thought to come
from the smallest PAH populations, which are most fragile, and thus primarily
reflect environment variations (Schutte et al., 1993; Micelotta et al., 2010;
Allain et al., 1996b, a). The PNSPC catalog is useful to investigate the
evolution of the PAH features and the processing of PAHs in circumstellar
environments.

Figure 18: Cumulative histogram of the signal-to-noise ratio of the
3.3$\,\mu$m PAH feature $\left({\rm S/N}(I_{3.3})\right)$. The gray dotted-
line shows the 35th percentile, which is the non-detection rate of the
3.3$\,\mu$m PAH feature when the detection limit is defined as ${\rm
S/N}(I_{3.3})\geq 3$.

##  6 Summary & Conclusion

Near-infrared (2.5–5.0$\,\mu$m) spectra of 72 Galactic PNe were obtained at
high sensitivity using the AKARI/IRC. The PNSPC program provided a set of
near-infrared spectra that collected all of the flux from the objects. The
absolute flux of spectra provided by the PNSPC program is in agreement with
the WISE W1 photometry within ${\sim}20$%. These spectra were compiled into
the PNSPC catalog. The intensity and equivalent width of Brackett-$\alpha$, He
I at 4.30$\,\mu$m, He II at 3.09$\,\mu$m, the $3.3\,\mu$m PAH feature, the
3.4–3.5$\,\mu$m aliphatic feature complex, [Mg IV] at $4.49\,\mu$m, and [Ar
VI] at $4.53\,\mu$m were measured. The detection limit of the emission
features was as faint as $2{\times}10^{-16}\,{\rm W\,m^{-2}}$. The PNSPC
catalog is the largest data set of near-infrared spectra of Galactic PNe. It
provides unique information for the investigation of 2.5–5.0$\,\mu$m emission
of Galactic PNe.

The Galactic coordinates of the PNSPC samples suggest that the objects in the
PNSPC catalog are biased toward PNe in the Galactic disk rather than those in
the Galactic bulge. The median of the effective temperature of the PNSPC
samples is lower than that of the whole Galactic PNe by about 30,000 K. This
indicates that the PNSPC catalog is biased toward young PNe. This bias
possibly originates in the criterion on the apparent size in the target
selection.

The PNSPC catalog also provides the extinction toward the objects. Even after
the contribution from the interstellar medium is taken into account, Figure 13
suggests that 40% of PNe have extinction at the $V$-band larger than unity,
which is attributed to the extinction in the circumstellar envelope. The
present result suggests that for a large fraction of PNe a circumstellar
envelope is optically thick in the UV.

The equivalent width of Brakett-$\alpha$ does not show a clear dependence on
the effective temperature. The variations in the He I and He II equivalent
widths can be attributed to the ionization balance between ${\rm He}^{+}$ and
${\rm He}^{++}$. The [Mg IV] at 4.49$\,\mu$m and [Ar VI] at 4.53$\,\mu$m lines
are only detected when the effective temperature becomes higher than 50 000 K.
The [Mg IV] and [Ar VI] lines are good indicators of PNe with a hot central
star.

The 3.3$\,\mu$m PAH feature is detected in about 65% of the PNSPC samples.
This detection rate is comparable to that reported from mid-infrared
observations (Stanghellini et al., 2012). The present result suggests that the
AKARI/IRC is as sensitive as the Spitzer/IRS in terms of detecting the PAH
features. The PNSPC catalog provides a suitable data set to investigate PAHs
in circumstellar environments. The near-infrared PAH features are attributed
to small-sized PAHs, which are sensitive to harsh environments and processed
faster than larger ones. The processing and evolution of PAHs during the PN
phase will be discussed in the forth-coming paper.

The present results are based on observations with AKARI, a JAXA project with
the participation of ESA. We greatly appreciate all the people who worked in
the operation and maintenance of those instruments. This publication makes use
of data products from the Wide-field Infrared Survey Explorer, which is a
joint project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration. This research has made use of
the SIMBAD database, operated at CDS, Strasbourg, France. This work is
supported in part by Grant-in-Aids for Scientific Research (25-8492, 23244021,
and 26247074) by the Japan Society of Promotion of Science (JSPS).

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Table 2: Miscellaneous Information of Objects

PN G | $V^{(a)}$ | $K_{s}^{(b)}$ | $A_{V}({\rm H\beta})$ | $A_{V}({\rm fit.})$ | $T_{\rm eff}$ | Refs. $T_{\rm eff}$
---|---|---|---|---|---|---
| mag. | mag. | mag. | mag. |  $10^{3}\,$K |
000.3${+}$12.2 | $\phantom{0}13.9$ | $\phantom{0}11.4$ | $\phantom{0}\phantom{0}0.90_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.98_{{-}0.05}^{{+}0.15}$ | $\phantom{0}47$ | Ka76,Ph03
002.0${-}$13.4 | $\phantom{0}14.1$ | $\phantom{0}11.1$ | $\phantom{0}\phantom{0}0.31_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}0.38_{{-}0.04}^{{+}0.02}$ | $\phantom{0}60$ | PM89,PM91,Ph03
003.1${+}$02.9 | ${>}17.0$ | $\phantom{0}11.6$ | $\phantom{0}\phantom{0}3.31_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}3.4_{{-}0.1}^{{+}0.6}$ | $\phantom{0}87$ | PM89,Ph03
011.0${+}$05.8 |  $\cdots$ | $\phantom{0}11.8$ | $\phantom{0}\phantom{0}1.81_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}1.79_{{-}0.06}^{{+}0.06}$ | $\phantom{0}93$ | PM91,Ph03
027.6${-}$09.6 | $\phantom{0}15.2$ | $\phantom{0}11.9$ | $\phantom{0}\phantom{0}1.04_{{-}0.05}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}1.0_{{-}0.2}^{{+}0.9}$ | $\phantom{0}58$ | PM91,Ka76,KJ91,Ph03
037.8${-}$06.3 |  $\cdots$ | $\phantom{0}9.47$ | $\phantom{0}\phantom{0}\phantom{0}1.4_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}1.41_{{-}0.02}^{{+}0.08}$ | $\phantom{0}74$ | Ph03
038.2${+}$12.0 | $\phantom{0}12.5$ | $\phantom{0}11.1$ | $\phantom{0}\phantom{0}0.82_{{-}0.05}^{{+}0.05}$ | $\phantom{0}\phantom{0}0.93_{{-}0.07}^{{+}0.07}$ | $\phantom{0}30$ | Ka78,Ph03
043.1${+}$03.8 | $\phantom{0}14.9$ | $\phantom{0}12.1$ | $\phantom{0}\phantom{0}\phantom{0}1.9_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}2.05_{{-}0.05}^{{+}0.46}$ | $\phantom{0}28$ | Ph03
046.4${-}$04.1 | $\phantom{0}15.2$ | $\phantom{0}11.1$ | $\phantom{0}\phantom{0}1.42_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.39_{{-}0.01}^{{+}0.01}$ | $\phantom{0}68$ | Ka76,KJ91,Ph03
051.4${+}$09.6 | $\phantom{0}13.3$ | $\phantom{0}10.4$ | $\phantom{0}\phantom{0}0.88_{{-}0.04}^{{+}0.05}$ | $\phantom{0}\phantom{0}0.98_{{-}0.08}^{{+}0.11}$ | $\phantom{0}37$ | Ka76,Ka78,Ph03
052.2${-}$04.0 | $\phantom{0}18.1$ | $\phantom{0}12.0$ | $\phantom{0}\phantom{0}1.68_{{-}0.04}^{{+}0.05}$ | $\phantom{0}\phantom{0}1.62_{{-}0.09}^{{+}0.09}$ | $\phantom{0}61$ | Lu01,PM89,KJ91,Ph03
058.3${-}$10.9 | $\phantom{0}14.4$ | $\phantom{0}9.67$ | $\phantom{0}\phantom{0}0.66_{{-}0.05}^{{+}0.05}$ | $\phantom{0}\phantom{0}0.18_{{-}0.04}^{{+}0.08}$ | $\phantom{0}50$ | PM89,Ka76,Ph03
060.1${-}$07.7 | $\phantom{0}18.0$ | $\phantom{0}11.5$ | $\phantom{0}\phantom{0}1.19_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.28_{{-}0.02}^{{+}0.03}$ | $129$ | Ph03
060.5${+}$01.8 |  $\cdots$ | $\phantom{0}11.8$ | $\phantom{0}\phantom{0}\phantom{0}4.1_{{-}0.2}^{{+}0.2}$ | $\phantom{0}\phantom{0}\phantom{0}3.5_{{-}0.4}^{{+}0.5}$ |  $\cdots$ |  $\cdots$
064.7${+}$05.0 | $\phantom{0}12.5$ | $\phantom{0}8.11$ | $\phantom{0}\phantom{0}1.44_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}1.43_{{-}0.04}^{{+}0.05}$ | $\phantom{0}28$ | Lu01,Ka76,Ka78,Ph03
071.6${-}$02.3 | ${>}15.7$ | $\phantom{0}10.1$ | $\phantom{0}\phantom{0}\phantom{0}4.4_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}\phantom{0}5.1_{{-}0.7}^{{+}1.3}$ |  $\cdots$ |  $\cdots$
074.5${+}$02.1 | $\phantom{0}18.4$ | $\phantom{0}11.0$ | $\phantom{0}\phantom{0}3.43_{{-}0.07}^{{+}0.07}$ | $\phantom{0}\phantom{0}3.47_{{-}0.04}^{{+}1.32}$ | $\phantom{0}81$ | Ph03
082.1${+}$07.0 | ${>}15.6$ | $\phantom{0}10.7$ | $\phantom{0}\phantom{0}1.71_{{-}0.08}^{{+}0.07}$ | $\phantom{0}\phantom{0}\phantom{0}1.7_{{-}0.1}^{{+}2.3}$ | $\phantom{0}87$ | Ph03
082.5${+}$11.3 | $\phantom{0}14.5$ | $\phantom{0}12.2$ | $\phantom{0}\phantom{0}0.17_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}0.16_{{-}0.05}^{{+}0.08}$ | $\phantom{0}63$ | Me88
086.5${-}$08.8 | $\phantom{0}17.3$ | $\phantom{0}12.5$ | $\phantom{0}\phantom{0}0.60_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.52_{{-}0.03}^{{+}0.03}$ | $\phantom{0}61$ | Lu01,Ph03
089.3${-}$02.2 | $\phantom{0}12.1$ | $\phantom{0}9.20$ | $\phantom{0}\phantom{0}\phantom{0}2.0_{{-}0.5}^{{+}0.8}$ | $\phantom{0}\phantom{0}1.90_{{-}0.01}^{{+}5.40}$ |  $\cdots$ |  $\cdots$
089.8${-}$05.1 | $\phantom{0}16.7$ | $\phantom{0}9.49$ | $\phantom{0}\phantom{0}1.99_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}2.02_{{-}0.01}^{{+}0.02}$ | $\phantom{0}83$ | Ka78,KJ91,Ph03
095.2${+}$00.7 |  $\cdots$ | $\phantom{0}11.2$ | $\phantom{0}\phantom{0}\phantom{0}5.5_{{-}0.2}^{{+}0.3}$ | $\phantom{0}\phantom{0}\phantom{0}5.4_{{-}0.1}^{{+}0.4}$ | $\phantom{0}58$ | Lu01
100.6${-}$05.4 | $\phantom{0}15.5$ | $\phantom{0}12.0$ | $\phantom{0}\phantom{0}0.52_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.47_{{-}0.07}^{{+}0.05}$ | $\phantom{0}74$ | Ka78,KJ91,Ph03
111.8${-}$02.8 | $\phantom{0}13.8$ | $\phantom{0}8.81$ | $\phantom{0}\phantom{0}1.92_{{-}0.10}^{{+}0.10}$ | $\phantom{0}\phantom{0}2.12_{{-}0.76}^{{+}0.01}$ | $\phantom{0}41$ | Ka76,Ph03
118.0${-}$08.6 | $\phantom{0}14.2$ | $\phantom{0}12.9$ | $\phantom{0}\phantom{0}0.41_{{-}0.10}^{{+}0.10}$ | $\phantom{0}\phantom{0}0.32_{{-}0.03}^{{+}0.02}$ | $\phantom{0}55$ | Lu01,Ka76,KJ91,Ph03
123.6${+}$34.5 | $\phantom{0}13.4$ | $\phantom{0}11.9$ | $\phantom{0}\phantom{0}0.50_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.60_{{-}0.03}^{{+}0.09}$ | $\phantom{0}50$ | HF83
146.7${+}$07.6 | $\phantom{0}14.0$ | $\phantom{0}11.2$ | $\phantom{0}\phantom{0}1.55_{{-}0.09}^{{+}0.09}$ | $\phantom{0}\phantom{0}1.56_{{-}0.02}^{{+}0.29}$ | $\phantom{0}27$ | Ph03
159.0${-}$15.1 | $\phantom{0}15.8$ | $\phantom{0}12.6$ | $\phantom{0}\phantom{0}0.44_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}0.40_{{-}0.06}^{{+}0.02}$ | $\phantom{0}89$ | Ph03
166.1${+}$10.4 | $\phantom{0}11.6$ | $\phantom{0}10.6$ | $\phantom{0}\phantom{0}0.63_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}0.64_{{-}0.03}^{{+}0.02}$ | $\phantom{0}39$ | Ka76,Ka78,Ph03
190.3${-}$17.7 | $\phantom{0}14.4$ | $\phantom{0}13.2$ | $\phantom{0}\phantom{0}0.34_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.36_{{-}0.04}^{{+}0.10}$ | $\phantom{0}61$ | PM89,Ka76,KJ91,Ph03
194.2${+}$02.5 | $\phantom{0}17.8$ | $\phantom{0}10.6$ | $\phantom{0}\phantom{0}1.40_{{-}0.06}^{{+}0.06}$ | $\phantom{0}\phantom{0}1.41_{{-}0.12}^{{+}0.04}$ | $\phantom{0}88$ | PM89,Ph03
211.2${-}$03.5 | $\phantom{0}15.8$ | $\phantom{0}10.6$ | $\phantom{0}\phantom{0}\phantom{0}3.5_{{-}0.2}^{{+}0.2}$ | $\phantom{0}\phantom{0}3.49_{{-}0.02}^{{+}0.03}$ | $\phantom{0}33$ | Lu01,PM89,Ph03
221.3${-}$12.3 | $\phantom{0}17.9$ | $\phantom{0}11.0$ | $\phantom{0}\phantom{0}0.91_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}0.91_{{-}0.02}^{{+}0.10}$ | $111$ | PM91,Ph03
226.7${+}$05.6 | $\phantom{0}16.9$ | $\phantom{0}12.8$ | $\phantom{0}\phantom{0}1.63_{{-}0.03}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.61_{{-}0.05}^{{+}0.11}$ | $\phantom{0}46$ | Ph03
232.8${-}$04.7 | $\phantom{0}13.9$ | $\phantom{0}9.48$ | $\phantom{0}\phantom{0}2.96_{{-}0.06}^{{+}0.06}$ | $\phantom{0}\phantom{0}2.99_{{-}0.09}^{{+}0.39}$ | $\phantom{0}25$ | Lu01,PM89,Ph03
235.3${-}$03.9 | $\phantom{0}14.1$ | $\phantom{0}10.6$ | $\phantom{0}\phantom{0}\phantom{0}1.6_{{-}0.2}^{{+}0.2}$ | $\phantom{0}\phantom{0}1.62_{{-}0.01}^{{+}0.01}$ | $\phantom{0}29$ | Lu01,PM89,Ph03
258.1${-}$00.3 | $\phantom{0}16.2$ | $\phantom{0}10.9$ | $\phantom{0}\phantom{0}4.02_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}4.02_{{-}0.04}^{{+}0.05}$ | $\phantom{0}60$ | PM91,Ph03
264.4${-}$12.7 | $\phantom{0}14.7$ | $\phantom{0}12.2$ | $\phantom{0}\phantom{0}0.72_{{-}0.07}^{{+}0.07}$ | $\phantom{0}\phantom{0}\phantom{0}0.6_{{-}0.1}^{{+}0.1}$ | $\phantom{0}56$ | PM91,KJ91
268.4${+}$02.4 | $\phantom{0}18.7$ | $\phantom{0}10.6$ | $\phantom{0}\phantom{0}3.80_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}3.91_{{-}0.05}^{{+}0.23}$ | $110$ | PM91,Ph03
278.6${-}$06.7 |  $\cdots$ | $\phantom{0}12.3$ | $\phantom{0}\phantom{0}0.73_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.75_{{-}0.05}^{{+}0.10}$ | $\phantom{0}84$ | PM91,Ph03
283.8${+}$02.2 | $\phantom{0}17.2$ | $\phantom{0}12.3$ | $\phantom{0}\phantom{0}1.57_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.35_{{-}0.01}^{{+}0.01}$ | $113$ | Ph03
285.4${-}$05.3 | $\phantom{0}15.5$ | $\phantom{0}11.6$ | $\phantom{0}\phantom{0}0.75_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.68_{{-}0.01}^{{+}0.03}$ | $100$ | PM91,Ph03
285.6${-}$02.7 | $\phantom{0}13.0$ | $\phantom{0}10.2$ | $\phantom{0}\phantom{0}2.11_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}2.16_{{-}0.05}^{{+}0.06}$ | $\phantom{0}34$ | PM89,Ph03
285.7${-}$14.9 | $\phantom{0}14.2$ | $\phantom{0}13.3$ | $\phantom{0}\phantom{0}0.14_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.14_{{-}0.03}^{{+}0.02}$ | $\phantom{0}55$ | Me88
291.6${-}$04.8 | $\phantom{0}15.4$ | $\phantom{0}10.5$ | $\phantom{0}\phantom{0}1.80_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.79_{{-}0.03}^{{+}0.13}$ | $116$ | PM91,Ph03
292.8${+}$01.1 |  $\cdots$ | $\phantom{0}12.5$ | $\phantom{0}\phantom{0}2.03_{{-}0.03}^{{+}0.02}$ | $\phantom{0}\phantom{0}2.16_{{-}0.07}^{{+}0.19}$ | $\phantom{0}95$ | PM91
294.9${-}$04.3 |  $\cdots$ | $\phantom{0}11.5$ | $\phantom{0}\phantom{0}1.80_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.80_{{-}0.05}^{{+}0.08}$ | $\phantom{0}41$ | PM89
296.3${-}$03.0 | $\phantom{0}16.1$ | $\phantom{0}11.6$ | $\phantom{0}\phantom{0}2.32_{{-}0.05}^{{+}0.05}$ | $\phantom{0}\phantom{0}2.38_{{-}0.06}^{{+}0.35}$ | $103$ | PM91,Ph03
304.5${-}$04.8 | $\phantom{0}16.4$ | $\phantom{0}10.8$ | $\phantom{0}\phantom{0}1.34_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}1.34_{{-}0.02}^{{+}0.05}$ | $102$ | PM91,Ph03
305.1${+}$01.4 | $\phantom{0}15.6$ | $\phantom{0}7.93$ | $\phantom{0}\phantom{0}\phantom{0}3.5_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}3.50_{{-}0.05}^{{+}0.02}$ | $\phantom{0}59$ | PM91,KJ91,Ph03
307.2${-}$09.0 | $\phantom{0}15.3$ | $\phantom{0}11.6$ | $\phantom{0}\phantom{0}1.16_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}1.10_{{-}0.03}^{{+}0.05}$ | $\phantom{0}50$ | PM89,KJ91,Ph03
307.5${-}$04.9 |  $\cdots$ | $\phantom{0}10.8$ | $\phantom{0}\phantom{0}\phantom{0}1.6_{{-}0.1}^{{+}0.2}$ | $\phantom{0}\phantom{0}1.64_{{-}0.03}^{{+}0.07}$ | $\phantom{0}38$ | PM89,Ph03
312.6${-}$01.8 | $\phantom{0}15.1$ | $\phantom{0}11.9$ | $\phantom{0}\phantom{0}3.17_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}3.35_{{-}0.08}^{{+}0.47}$ | $\phantom{0}42$ | PM89,KJ91,Ph03
315.1${-}$13.0 | $\phantom{0}11.0$ | $\phantom{0}9.36$ | $\phantom{0}\phantom{0}\phantom{0}0.5_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}\phantom{0}\phantom{0}\phantom{0}9_{{-}5}^{{+}1}$ | $\phantom{0}27$ | PM89,Ka78,Ph03
320.1${-}$09.6 | $\phantom{0}10.9$ | $\phantom{0}10.1$ | $\phantom{0}\phantom{0}0.72_{{-}0.07}^{{+}0.08}$ | $\phantom{0}\phantom{0}0.63_{{-}0.05}^{{+}3.31}$ | $\phantom{0}27$ | Me88
320.9${+}$02.0 | ${>}17.9$ | $\phantom{0}10.2$ | $\phantom{0}\phantom{0}4.96_{{-}0.09}^{{+}0.09}$ | $\phantom{0}\phantom{0}\phantom{0}\phantom{0}\phantom{0}7_{{-}2}^{{+}2}$ | $\phantom{0}44$ | PM89
322.5${-}$05.2 | $\phantom{0}15.3$ | $\phantom{0}12.7$ | $\phantom{0}\phantom{0}0.80_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.89_{{-}0.04}^{{+}0.19}$ | $127$ | Ph03
323.9${+}$02.4 | $\phantom{0}16.8$ | $\phantom{0}11.8$ | $\phantom{0}\phantom{0}3.05_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}3.01_{{-}0.22}^{{+}0.05}$ | $\phantom{0}42$ | PM89,Ph03
324.8${-}$01.1 |  $\cdots$ | $\phantom{0}10.6$ | $\phantom{0}\phantom{0}6.34_{{-}0.03}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}6.5_{{-}0.2}^{{+}0.3}$ |  $\cdots$ |  $\cdots$
325.8${-}$12.8 | $\phantom{0}13.4$ | $\phantom{0}11.1$ | $\phantom{0}\phantom{0}0.50_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.9_{{-}0.1}^{{+}0.5}$ | $\phantom{0}36$ | Me88
326.0${-}$06.5 | $\phantom{0}13.1$ | $\phantom{0}11.8$ | $\phantom{0}\phantom{0}1.23_{{-}0.07}^{{+}0.07}$ | $\phantom{0}\phantom{0}1.16_{{-}0.05}^{{+}0.04}$ | $\phantom{0}25$ | Me88
327.1${-}$01.8 | $\phantom{0}17.2$ | $\phantom{0}11.5$ | $\phantom{0}\phantom{0}3.83_{{-}0.03}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}4.2_{{-}0.3}^{{+}0.2}$ | $\phantom{0}35$ | PM89,Ph03
327.8${-}$01.6 |  $\cdots$ | $\phantom{0}11.0$ | $\phantom{0}\phantom{0}5.10_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}5.7_{{-}0.5}^{{+}0.7}$ |  $\cdots$ |  $\cdots$
331.1${-}$05.7 | $\phantom{0}12.7$ | $\phantom{0}10.3$ | $\phantom{0}\phantom{0}\phantom{0}1.4_{{-}0.1}^{{+}0.1}$ | $\phantom{0}\phantom{0}1.36_{{-}0.03}^{{+}3.35}$ | $\phantom{0}31$ | PM89,Ph03
331.3${+}$16.8 | $\phantom{0}15.5$ | $\phantom{0}12.5$ | $\phantom{0}\phantom{0}0.10_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}0.78_{{-}0.46}^{{+}0.01}$ | $\phantom{0}86$ | PM89,Ph03
336.3${-}$05.6 | $\phantom{0}16.6$ | $\phantom{0}12.2$ | $\phantom{0}\phantom{0}1.32_{{-}0.06}^{{+}0.07}$ | $\phantom{0}\phantom{0}1.36_{{-}0.03}^{{+}0.02}$ | $101$ | PM91,Ph03
342.1${+}$27.5 |  $\cdots$ | $\phantom{0}13.2$ | $\phantom{0}\phantom{0}0.25_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}0.27_{{-}0.04}^{{+}0.47}$ | $119$ | PM89,Ph03
349.8${+}$04.4 | $\phantom{0}17.0$ | $\phantom{0}12.1$ | $\phantom{0}\phantom{0}\phantom{0}1.9_{{-}0.1}^{{+}0.2}$ | $\phantom{0}\phantom{0}\phantom{0}2.1_{{-}0.1}^{{+}0.1}$ | $\phantom{0}76$ | PM89
350.9${+}$04.4 | $\phantom{0}13.3$ | $\phantom{0}10.3$ | $\phantom{0}\phantom{0}1.83_{{-}0.08}^{{+}0.07}$ | $\phantom{0}\phantom{0}1.83_{{-}0.02}^{{+}2.23}$ | $\phantom{0}33$ | Me88
356.1${+}$02.7 |  $\cdots$ | $\phantom{0}11.9$ | $\phantom{0}\phantom{0}\phantom{0}5.8_{{-}0.5}^{{+}1.0}$ | $\phantom{0}\phantom{0}5.54_{{-}0.01}^{{+}0.16}$ | $\phantom{0}73$ | PM89
357.6${+}$02.6 |  $\cdots$ | $\phantom{0}12.2$ | $\phantom{0}\phantom{0}\phantom{0}4.7_{{-}0.6}^{{+}1.8}$ | $\phantom{0}\phantom{0}4.71_{{-}0.45}^{{+}0.06}$ | $107$ | PM91

References. — (a)Acker et al. (1992); (b) Skrutskie et al. (2006); HF83:
Harrington & Feibelman (1983), Ka76: Kaler (1976), Ka78: Kaler (1978), KJ91:
Kaler & Jacoby (1991), Lu01: Lumsden et al. (2001), Me88: Mendez et al.
(1988), Ph03: Phillips (2003), PM89: Preite-Martinez et al. (1989), PM91:
Preite-Martinez et al. (1991).

Table 5: Extinction Corrected Line Intensity  PN G | Bracket-$\alpha$ | He II$(3.09{\rm\mu m})$ | He I$(4.30{\rm\mu m})$ | PAH$(3.3{\rm\mu m})$ | C−Hal$(3.4$-$3.5{\rm\mu m})$ | [Mg IV]$(4.49{\rm\mu m})$ | [Ar VI]$(4.53{\rm\mu m})$
---|---|---|---|---|---|---|---
| $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$ | $10^{-15}\,{\rm W\,m^{-2}}$
000.3${+}$12.2 | $\phantom{0}\phantom{0}\phantom{0}2.74_{{-}0.04}^{{+}0.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.14_{{-}0.03}^{{+}0.03}$ | ${<}0.11$ |  $\cdots$ |  $\cdots$ |  $\cdots$
002.0${-}$13.4 | $\phantom{0}\phantom{0}\phantom{0}2.05_{{-}0.03}^{{+}0.04}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.31_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.25_{{-}0.05}^{{+}0.05}$ | ${<}0.10$ |  $\cdots$ |  $\cdots$
003.1${+}$02.9 | $\phantom{0}\phantom{0}\phantom{0}3.16_{{-}0.04}^{{+}0.04}$ | ${<}0.53$ | $\phantom{0}\phantom{0}\phantom{0}0.43_{{-}0.04}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.94_{{-}0.16}^{{+}0.25}$ | $\phantom{0}\phantom{0}\phantom{0}0.49_{{-}0.08}^{{+}0.09}$ | $\phantom{0}\phantom{0}\phantom{0}0.35_{{-}0.04}^{{+}0.05}$ |  $\cdots$
011.0${+}$05.8 | $\phantom{0}\phantom{0}\phantom{0}1.09_{{-}0.04}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.13_{{-}0.03}^{{+}0.03}$ | ${<}0.13$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}1.11_{{-}0.08}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.20_{{-}0.05}^{{+}0.04}$
027.6${-}$09.6 | $\phantom{0}\phantom{0}\phantom{0}1.12_{{-}0.02}^{{+}0.04}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.10_{{-}0.01}^{{+}0.01}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
037.8${-}$06.3 | $\phantom{0}\phantom{0}\phantom{0}4.61_{{-}0.10}^{{+}0.24}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}1.80_{{-}0.09}^{{+}0.13}$ | $\phantom{0}\phantom{0}\phantom{0}6.64_{{-}0.21}^{{+}0.40}$ | $\phantom{0}\phantom{0}\phantom{0}2.60_{{-}0.14}^{{+}0.21}$ |  $\cdots$ |  $\cdots$
038.2${+}$12.0 | $\phantom{0}\phantom{0}\phantom{0}2.18_{{-}0.06}^{{+}0.04}$ |  $\cdots$ | ${<}0.13$ | $\phantom{0}\phantom{0}\phantom{0}0.45_{{-}0.05}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.12_{{-}0.02}^{{+}0.03}$ |  $\cdots$ |  $\cdots$
043.1${+}$03.8 | $\phantom{0}\phantom{0}\phantom{0}0.45_{{-}0.01}^{{+}0.01}$ |  $\cdots$ |  $\cdots$ | ${<}0.06$ | ${<}0.01$ |  $\cdots$ |  $\cdots$
046.4${-}$04.1 | $\phantom{0}\phantom{0}\phantom{0}2.43_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.11_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.32_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.40_{{-}0.05}^{{+}0.04}$ | ${<}0.16$ |  $\cdots$ |  $\cdots$
051.4${+}$09.6 | $\phantom{0}\phantom{0}\phantom{0}3.25_{{-}0.02}^{{+}0.06}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.52_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.97_{{-}0.07}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.05}^{{+}0.04}$ |  $\cdots$ |  $\cdots$
052.2${-}$04.0 | $\phantom{0}\phantom{0}\phantom{0}0.87_{{-}0.01}^{{+}0.01}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.14_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.05_{{-}0.01}^{{+}0.01}$ | ${<}0.03$ |  $\cdots$ |  $\cdots$
058.3${-}$10.9 | $\phantom{0}\phantom{0}\phantom{0}4.62_{{-}0.07}^{{+}0.10}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.99_{{-}0.04}^{{+}0.07}$ | ${<}0.55$ | ${<}0.26$ |  $\cdots$ |  $\cdots$
060.1${-}$07.7 | $\phantom{0}\phantom{0}\phantom{0}1.41_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.19_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.05_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}2.21_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}1.34_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}5.04_{{-}0.06}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}1.90_{{-}0.03}^{{+}0.04}$
060.5${+}$01.8 | $\phantom{0}\phantom{0}\phantom{0}1.12_{{-}0.01}^{{+}0.03}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.16_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.04}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.07_{{-}0.02}^{{+}0.01}$ |  $\cdots$ |  $\cdots$
064.7${+}$05.0 | $\phantom{0}\phantom{0}34.69_{{-}1.38}^{{+}1.49}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}5.17_{{-}1.38}^{{+}2.18}$ | $\phantom{0}145.36_{{-}4.23}^{{+}4.77}$ | $\phantom{0}\phantom{0}50.92_{{-}1.79}^{{+}2.87}$ |  $\cdots$ |  $\cdots$
071.6${-}$02.3 | $\phantom{0}\phantom{0}\phantom{0}3.50_{{-}0.09}^{{+}0.22}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.75_{{-}0.09}^{{+}0.13}$ | $\phantom{0}\phantom{0}\phantom{0}7.13_{{-}0.58}^{{+}0.37}$ | $\phantom{0}\phantom{0}\phantom{0}2.07_{{-}0.44}^{{+}0.29}$ |  $\cdots$ |  $\cdots$
074.5${+}$02.1 | $\phantom{0}\phantom{0}\phantom{0}1.82_{{-}0.06}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}0.41_{{-}0.03}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}0.12_{{-}0.04}^{{+}0.20}$ | $\phantom{0}\phantom{0}\phantom{0}2.86_{{-}0.22}^{{+}0.25}$ | $\phantom{0}\phantom{0}\phantom{0}1.68_{{-}0.10}^{{+}0.37}$ | $\phantom{0}\phantom{0}\phantom{0}4.43_{{-}0.25}^{{+}0.39}$ | $\phantom{0}\phantom{0}\phantom{0}6.18_{{-}0.34}^{{+}0.30}$
082.1${+}$07.0 | $\phantom{0}\phantom{0}\phantom{0}3.85_{{-}0.04}^{{+}0.40}$ | $\phantom{0}\phantom{0}\phantom{0}0.40_{{-}0.02}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}0.34_{{-}0.02}^{{+}0.06}$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}2.25_{{-}0.06}^{{+}0.09}$ | $\phantom{0}\phantom{0}\phantom{0}0.10_{{-}0.02}^{{+}0.09}$
082.5${+}$11.3 | $\phantom{0}\phantom{0}\phantom{0}0.52_{{-}0.02}^{{+}0.02}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.10_{{-}0.02}^{{+}0.02}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
086.5${-}$08.8 | $\phantom{0}\phantom{0}\phantom{0}0.92_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.49_{{-}0.01}^{{+}0.02}$ |  $\cdots$ | ${<}0.08$ | ${<}0.07$ | $\phantom{0}\phantom{0}\phantom{0}1.40_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}2.75_{{-}0.06}^{{+}0.05}$
089.3${-}$02.2 | $\phantom{0}\phantom{0}\phantom{0}0.79_{{-}0.07}^{{+}0.24}$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}1.96_{{-}0.17}^{{+}0.62}$ | ${<}0.48$ |  $\cdots$ |  $\cdots$
089.8${-}$05.1 | $\phantom{0}\phantom{0}\phantom{0}2.92_{{-}0.03}^{{+}0.15}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.04}^{{+}0.09}$ | $\phantom{0}\phantom{0}\phantom{0}0.92_{{-}0.06}^{{+}0.11}$ | $\phantom{0}\phantom{0}14.75_{{-}0.19}^{{+}0.41}$ | $\phantom{0}\phantom{0}\phantom{0}4.86_{{-}0.09}^{{+}0.22}$ | $\phantom{0}\phantom{0}\phantom{0}2.91_{{-}0.05}^{{+}0.24}$ | $\phantom{0}\phantom{0}\phantom{0}0.43_{{-}0.06}^{{+}0.14}$
095.2${+}$00.7 | $\phantom{0}\phantom{0}\phantom{0}2.52_{{-}0.06}^{{+}0.07}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.53_{{-}0.02}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}0.56_{{-}0.06}^{{+}0.08}$ | ${<}0.18$ |  $\cdots$ |  $\cdots$
100.6${-}$05.4 | $\phantom{0}\phantom{0}\phantom{0}0.93_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.05_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.05_{{-}0.01}^{{+}0.01}$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.06_{{-}0.01}^{{+}0.01}$ |  $\cdots$
111.8${-}$02.8 | $\phantom{0}\phantom{0}\phantom{0}6.18_{{-}0.47}^{{+}0.01}$ |  $\cdots$ | ${<}2.62$ | ${<}3.55$ | $\phantom{0}\phantom{0}\phantom{0}1.65_{{-}0.29}^{{+}0.38}$ |  $\cdots$ |  $\cdots$
118.0${-}$08.6 | $\phantom{0}\phantom{0}\phantom{0}0.35_{{-}0.02}^{{+}0.02}$ |  $\cdots$ | ${<}0.05$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
123.6${+}$34.5 | $\phantom{0}\phantom{0}\phantom{0}2.02_{{-}0.05}^{{+}0.05}$ |  $\cdots$ | ${<}0.15$ | ${<}0.18$ | ${<}0.05$ |  $\cdots$ |  $\cdots$
146.7${+}$07.6 | $\phantom{0}\phantom{0}\phantom{0}0.56_{{-}0.01}^{{+}0.04}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.10_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}4.23_{{-}0.10}^{{+}0.14}$ | $\phantom{0}\phantom{0}\phantom{0}0.79_{{-}0.04}^{{+}0.08}$ |  $\cdots$ |  $\cdots$
159.0${-}$15.1 | $\phantom{0}\phantom{0}\phantom{0}0.48_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.11_{{-}0.01}^{{+}0.01}$ | ${<}0.06$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.86_{{-}0.03}^{{+}0.03}$ |  $\cdots$
166.1${+}$10.4 | $\phantom{0}\phantom{0}\phantom{0}4.34_{{-}0.06}^{{+}0.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.35_{{-}0.06}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.06}^{{+}0.25}$ | ${<}0.16$ |  $\cdots$ |  $\cdots$
190.3${-}$17.7 | $\phantom{0}\phantom{0}\phantom{0}0.46_{{-}0.01}^{{+}0.01}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.04_{{-}0.01}^{{+}0.01}$ | ${<}0.04$ |  $\cdots$ |  $\cdots$ |  $\cdots$
194.2${+}$02.5 | $\phantom{0}\phantom{0}\phantom{0}1.72_{{-}0.08}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.41_{{-}0.04}^{{+}0.06}$ | ${<}0.20$ | $\phantom{0}\phantom{0}\phantom{0}3.70_{{-}0.17}^{{+}0.25}$ | $\phantom{0}\phantom{0}\phantom{0}1.16_{{-}0.14}^{{+}0.17}$ | $\phantom{0}\phantom{0}\phantom{0}2.44_{{-}0.09}^{{+}0.11}$ | $\phantom{0}\phantom{0}\phantom{0}0.34_{{-}0.10}^{{+}0.11}$
211.2${-}$03.5 | $\phantom{0}\phantom{0}\phantom{0}1.82_{{-}0.04}^{{+}0.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.26_{{-}0.05}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.47_{{-}0.07}^{{+}0.23}$ | ${<}0.24$ |  $\cdots$ |  $\cdots$
221.3${-}$12.3 | $\phantom{0}\phantom{0}\phantom{0}2.63_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.70_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.18_{{-}0.03}^{{+}0.04}$ | ${<}0.77$ | ${<}0.30$ | $\phantom{0}\phantom{0}\phantom{0}6.56_{{-}0.09}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}2.17_{{-}0.07}^{{+}0.07}$
226.7${+}$05.6 | $\phantom{0}\phantom{0}\phantom{0}0.47_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.05_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.04_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.84_{{-}0.03}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.52_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.40_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.18_{{-}0.01}^{{+}0.01}$
232.8${-}$04.7 | $\phantom{0}\phantom{0}\phantom{0}2.88_{{-}0.14}^{{+}0.19}$ |  $\cdots$ | ${<}0.59$ | $\phantom{0}\phantom{0}\phantom{0}8.87_{{-}0.61}^{{+}0.69}$ | $\phantom{0}\phantom{0}\phantom{0}2.49_{{-}0.23}^{{+}0.47}$ |  $\cdots$ |  $\cdots$
235.3${-}$03.9 | $\phantom{0}\phantom{0}\phantom{0}1.12_{{-}0.05}^{{+}0.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.16_{{-}0.04}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}0.57_{{-}0.08}^{{+}0.08}$ | ${<}0.21$ |  $\cdots$ |  $\cdots$
258.1${-}$00.3 | $\phantom{0}\phantom{0}\phantom{0}3.70_{{-}0.05}^{{+}0.06}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.56_{{-}0.04}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.35_{{-}0.07}^{{+}0.15}$ | ${<}0.09$ |  $\cdots$ |  $\cdots$
264.4${-}$12.7 | $\phantom{0}\phantom{0}\phantom{0}0.70_{{-}0.01}^{{+}0.02}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.07_{{-}0.01}^{{+}0.01}$ | ${<}0.06$ | ${<}0.04$ |  $\cdots$ |  $\cdots$
268.4${+}$02.4 | $\phantom{0}\phantom{0}\phantom{0}1.52_{{-}0.03}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.29_{{-}0.02}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.27_{{-}0.04}^{{+}0.06}$ | $\phantom{0}\phantom{0}11.23_{{-}0.31}^{{+}0.38}$ | $\phantom{0}\phantom{0}\phantom{0}5.52_{{-}0.13}^{{+}0.19}$ | $\phantom{0}\phantom{0}\phantom{0}5.34_{{-}0.14}^{{+}0.14}$ | $\phantom{0}\phantom{0}\phantom{0}3.69_{{-}0.09}^{{+}0.15}$
278.6${-}$06.7 | $\phantom{0}\phantom{0}\phantom{0}0.59_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.03_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.09_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.10_{{-}0.01}^{{+}0.02}$ | ${<}0.04$ | $\phantom{0}\phantom{0}\phantom{0}0.10_{{-}0.01}^{{+}0.01}$ |  $\cdots$
283.8${+}$02.2 | $\phantom{0}\phantom{0}\phantom{0}0.73_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.34_{{-}0.01}^{{+}0.01}$ | ${<}0.01$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}5.46_{{-}0.01}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}0.96_{{-}0.01}^{{+}0.01}$
285.4${-}$05.3 | $\phantom{0}\phantom{0}\phantom{0}2.68_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.42_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.18_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.21_{{-}0.06}^{{+}0.06}$ | ${<}0.06$ | $\phantom{0}\phantom{0}\phantom{0}2.84_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.29_{{-}0.01}^{{+}0.02}$
285.6${-}$02.7 | $\phantom{0}\phantom{0}\phantom{0}4.92_{{-}0.04}^{{+}0.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.24_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}1.41_{{-}0.04}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}0.21_{{-}0.04}^{{+}0.07}$ |  $\cdots$ |  $\cdots$
285.7${-}$14.9 | $\phantom{0}\phantom{0}\phantom{0}1.28_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.22_{{-}0.03}^{{+}0.03}$ | ${<}0.12$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.65_{{-}0.05}^{{+}0.05}$ | ${<}0.08$
291.6${-}$04.8 | $\phantom{0}\phantom{0}\phantom{0}2.91_{{-}0.03}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}0.55_{{-}0.03}^{{+}0.09}$ | $\phantom{0}\phantom{0}\phantom{0}0.38_{{-}0.01}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}7.18_{{-}0.08}^{{+}0.24}$ | $\phantom{0}\phantom{0}\phantom{0}3.61_{{-}0.04}^{{+}0.18}$ | $\phantom{0}\phantom{0}10.18_{{-}0.05}^{{+}0.40}$ | $\phantom{0}\phantom{0}\phantom{0}7.72_{{-}0.04}^{{+}0.38}$
292.8${+}$01.1 | $\phantom{0}\phantom{0}\phantom{0}0.78_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.08_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.07_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.43_{{-}0.03}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.03}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.06_{{-}0.01}^{{+}0.02}$ |  $\cdots$
294.9${-}$04.3 | $\phantom{0}\phantom{0}\phantom{0}0.92_{{-}0.02}^{{+}0.02}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.14_{{-}0.03}^{{+}0.03}$ | ${<}0.24$ | ${<}0.02$ |  $\cdots$ |  $\cdots$
296.3${-}$03.0 | $\phantom{0}\phantom{0}\phantom{0}1.16_{{-}0.03}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.12_{{-}0.01}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.14_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.49_{{-}0.03}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.02}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.84_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.38_{{-}0.03}^{{+}0.03}$
304.5${-}$04.8 | $\phantom{0}\phantom{0}\phantom{0}3.47_{{-}0.02}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.31_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.48_{{-}0.03}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}1.32_{{-}0.27}^{{+}0.10}$ | $\phantom{0}\phantom{0}\phantom{0}0.49_{{-}0.09}^{{+}0.10}$ | $\phantom{0}\phantom{0}\phantom{0}4.49_{{-}0.03}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}0.85_{{-}0.03}^{{+}0.06}$
305.1${+}$01.4 | $\phantom{0}\phantom{0}12.65_{{-}1.67}^{{+}1.42}$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}7.43_{{-}1.64}^{{+}2.59}$ | $\phantom{0}\phantom{0}10.78_{{-}1.40}^{{+}3.23}$ |  $\cdots$ |  $\cdots$
307.2${-}$09.0 | $\phantom{0}\phantom{0}\phantom{0}0.98_{{-}0.01}^{{+}0.02}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.19_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.20_{{-}0.05}^{{+}0.05}$ | ${<}0.06$ |  $\cdots$ |  $\cdots$
307.5${-}$04.9 | $\phantom{0}\phantom{0}\phantom{0}2.67_{{-}0.03}^{{+}0.03}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.27_{{-}0.02}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}2.06_{{-}0.08}^{{+}0.18}$ | $\phantom{0}\phantom{0}\phantom{0}0.28_{{-}0.09}^{{+}0.12}$ |  $\cdots$ |  $\cdots$
312.6${-}$01.8 | $\phantom{0}\phantom{0}\phantom{0}1.38_{{-}0.02}^{{+}0.03}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.11_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.11_{{-}0.03}^{{+}0.05}$ | ${<}0.04$ |  $\cdots$ |  $\cdots$
315.1${-}$13.0 | $\phantom{0}\phantom{0}11.90_{{-}0.91}^{{+}1.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.78_{{-}0.20}^{{+}0.27}$ | $\phantom{0}\phantom{0}\phantom{0}5.15_{{-}1.02}^{{+}1.08}$ | $\phantom{0}\phantom{0}\phantom{0}1.48_{{-}0.45}^{{+}0.50}$ |  $\cdots$ |  $\cdots$
320.1${-}$09.6 | $\phantom{0}\phantom{0}\phantom{0}3.26_{{-}0.04}^{{+}0.40}$ |  $\cdots$ | ${<}0.13$ | $\phantom{0}\phantom{0}\phantom{0}3.58_{{-}0.08}^{{+}0.33}$ | $\phantom{0}\phantom{0}\phantom{0}0.81_{{-}0.06}^{{+}0.19}$ |  $\cdots$ |  $\cdots$
320.9${+}$02.0 | $\phantom{0}\phantom{0}\phantom{0}5.99_{{-}0.27}^{{+}0.46}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}1.20_{{-}0.09}^{{+}0.31}$ | $\phantom{0}\phantom{0}\phantom{0}3.23_{{-}0.19}^{{+}0.12}$ | $\phantom{0}\phantom{0}\phantom{0}1.31_{{-}0.09}^{{+}0.16}$ |  $\cdots$ |  $\cdots$
322.5${-}$05.2 | $\phantom{0}\phantom{0}\phantom{0}1.12_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.78_{{-}0.03}^{{+}0.04}$ | ${<}0.16$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}13.18_{{-}0.11}^{{+}0.14}$ |  $\cdots$
323.9${+}$02.4 | $\phantom{0}\phantom{0}\phantom{0}2.02_{{-}0.03}^{{+}0.04}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.25_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}2.20_{{-}0.09}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.95_{{-}0.03}^{{+}0.04}$ |  $\cdots$ |  $\cdots$
324.8${-}$01.1 | $\phantom{0}\phantom{0}\phantom{0}4.11_{{-}0.08}^{{+}0.12}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.86_{{-}0.05}^{{+}0.07}$ | $\phantom{0}\phantom{0}\phantom{0}1.06_{{-}0.12}^{{+}0.14}$ | $\phantom{0}\phantom{0}\phantom{0}0.35_{{-}0.08}^{{+}0.11}$ |  $\cdots$ |  $\cdots$
325.8${-}$12.8 | $\phantom{0}\phantom{0}\phantom{0}1.50_{{-}0.03}^{{+}0.06}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.17_{{-}0.01}^{{+}0.03}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
326.0${-}$06.5 | $\phantom{0}\phantom{0}\phantom{0}0.36_{{-}0.01}^{{+}0.01}$ |  $\cdots$ | ${<}0.01$ | $\phantom{0}\phantom{0}\phantom{0}0.07_{{-}0.01}^{{+}0.06}$ | ${<}0.04$ |  $\cdots$ |  $\cdots$
327.1${-}$01.8 | $\phantom{0}\phantom{0}\phantom{0}1.69_{{-}0.07}^{{+}0.07}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.17_{{-}0.01}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}1.20_{{-}0.16}^{{+}0.10}$ | $\phantom{0}\phantom{0}\phantom{0}0.60_{{-}0.02}^{{+}0.03}$ |  $\cdots$ |  $\cdots$
327.8${-}$01.6 | $\phantom{0}\phantom{0}\phantom{0}1.97_{{-}0.03}^{{+}0.07}$ | $\phantom{0}\phantom{0}\phantom{0}0.36_{{-}0.03}^{{+}0.06}$ | $\phantom{0}\phantom{0}\phantom{0}0.28_{{-}0.03}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}2.24_{{-}0.35}^{{+}0.21}$ | $\phantom{0}\phantom{0}\phantom{0}1.33_{{-}0.11}^{{+}0.13}$ | $\phantom{0}\phantom{0}\phantom{0}3.12_{{-}0.14}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}3.68_{{-}0.28}^{{+}0.04}$
331.1${-}$05.7 | $\phantom{0}\phantom{0}\phantom{0}1.13_{{-}0.03}^{{+}0.22}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.29_{{-}0.02}^{{+}0.08}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
331.3${+}$16.8 | $\phantom{0}\phantom{0}\phantom{0}0.74_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.21_{{-}0.02}^{{+}0.03}$ | ${<}0.04$ | $\phantom{0}\phantom{0}\phantom{0}0.16_{{-}0.03}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.05_{{-}0.01}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}1.20_{{-}0.04}^{{+}0.02}$ |  $\cdots$
336.3${-}$05.6 | $\phantom{0}\phantom{0}\phantom{0}0.21_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.06_{{-}0.01}^{{+}0.01}$ | ${<}0.03$ | $\phantom{0}\phantom{0}\phantom{0}0.43_{{-}0.03}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}0.23_{{-}0.02}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.39_{{-}0.02}^{{+}0.02}$ | $\phantom{0}\phantom{0}\phantom{0}0.41_{{-}0.02}^{{+}0.02}$
342.1${+}$27.5 | $\phantom{0}\phantom{0}\phantom{0}0.47_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.25_{{-}0.01}^{{+}0.02}$ | ${<}0.03$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}2.91_{{-}0.05}^{{+}0.05}$ | $\phantom{0}\phantom{0}\phantom{0}0.44_{{-}0.02}^{{+}0.03}$
349.8${+}$04.4 | $\phantom{0}\phantom{0}\phantom{0}0.87_{{-}0.02}^{{+}0.02}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.13_{{-}0.01}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.41_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.19_{{-}0.03}^{{+}0.04}$ |  $\cdots$ |  $\cdots$
350.9${+}$04.4 | $\phantom{0}\phantom{0}\phantom{0}2.03_{{-}0.04}^{{+}0.21}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.14_{{-}0.03}^{{+}0.08}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
356.1${+}$02.7 | $\phantom{0}\phantom{0}\phantom{0}0.74_{{-}0.04}^{{+}0.01}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.22_{{-}0.02}^{{+}0.01}$ | $\phantom{0}\phantom{0}\phantom{0}0.99_{{-}0.02}^{{+}0.03}$ | $\phantom{0}\phantom{0}\phantom{0}0.48_{{-}0.01}^{{+}0.08}$ |  $\cdots$ |  $\cdots$
357.6${+}$02.6 | $\phantom{0}\phantom{0}\phantom{0}0.73_{{-}0.04}^{{+}0.05}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}0.16_{{-}0.04}^{{+}0.04}$ | $\phantom{0}\phantom{0}\phantom{0}0.54_{{-}0.07}^{{+}0.08}$ | $\phantom{0}\phantom{0}\phantom{0}0.15_{{-}0.01}^{{+}0.05}$ |  $\cdots$ |  $\cdots$
Table 6: Extinction Corrected Line Equivalent Width  PN G | Bracket-$\alpha$ | He II$(3.09{\rm\mu m})$ | He I$(4.30{\rm\mu m})$ | PAH$(3.3{\rm\mu m})$ | C−Hal$(3.4$-$3.5{\rm\mu m})$ | [Mg IV]$(4.49{\rm\mu m})$ | [Ar VI]$(4.53{\rm\mu m})$
---|---|---|---|---|---|---|---
| Å | Å | Å | Å | Å | Å | Å
000.3${+}$12.2 | $\phantom{0}2825.6_{{-}38.2}^{{+}47.3}$ |  $\cdots$ | $\phantom{0}\phantom{0}154.5_{{-}32.7}^{{+}35.5}$ | ${<}130.7$ |  $\cdots$ |  $\cdots$ |  $\cdots$
002.0${-}$13.4 | $\phantom{0}2938.4_{{-}39.9}^{{+}64.0}$ |  $\cdots$ | $\phantom{0}\phantom{0}481.9_{{-}27.1}^{{+}42.1}$ | $\phantom{0}\phantom{0}435.3_{{-}84.6}^{{+}86.8}$ | ${<}181.4$ |  $\cdots$ |  $\cdots$
003.1${+}$02.9 | $\phantom{0}2105.7_{{-}25.5}^{{+}26.5}$ | ${<}236.7$ | $\phantom{0}\phantom{0}343.7_{{-}30.2}^{{+}25.6}$ | $\phantom{0}\phantom{0}665.7_{{-}113.7}^{{+}176.0}$ | $\phantom{0}\phantom{0}365.1_{{-}59.5}^{{+}68.0}$ | $\phantom{0}\phantom{0}324.3_{{-}42.0}^{{+}51.4}$ |  $\cdots$
011.0${+}$05.8 | $\phantom{0}2005.1_{{-}68.8}^{{+}61.4}$ | $\phantom{0}\phantom{0}144.8_{{-}34.2}^{{+}32.1}$ | ${<}266.9$ |  $\cdots$ |  $\cdots$ | $\phantom{0}2605.4_{{-}179.7}^{{+}127.9}$ | $\phantom{0}\phantom{0}486.2_{{-}111.4}^{{+}101.8}$
027.6${-}$09.6 | $\phantom{0}3229.6_{{-}44.8}^{{+}128.8}$ |  $\cdots$ | $\phantom{0}\phantom{0}328.8_{{-}27.6}^{{+}35.8}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
037.8${-}$06.3 | $\phantom{0}\phantom{0}482.1_{{-}10.0}^{{+}25.4}$ |  $\cdots$ | $\phantom{0}\phantom{0}182.2_{{-}\phantom{0}8.6}^{{+}13.6}$ | $\phantom{0}1342.1_{{-}42.1}^{{+}80.2}$ | $\phantom{0}\phantom{0}531.1_{{-}29.1}^{{+}42.6}$ |  $\cdots$ |  $\cdots$
038.2${+}$12.0 | $\phantom{0}2863.3_{{-}84.4}^{{+}54.5}$ |  $\cdots$ | ${<}192.5$ | $\phantom{0}\phantom{0}709.0_{{-}75.8}^{{+}55.0}$ | $\phantom{0}\phantom{0}204.3_{{-}38.7}^{{+}47.2}$ |  $\cdots$ |  $\cdots$
043.1${+}$03.8 | $\phantom{0}1316.2_{{-}37.5}^{{+}42.9}$ |  $\cdots$ |  $\cdots$ | ${<}230.0$ |  $\cdots$ |  $\cdots$ |  $\cdots$
046.4${-}$04.1 | $\phantom{0}3171.2_{{-}\phantom{0}5.0}^{{+}29.3}$ | $\phantom{0}\phantom{0}\phantom{0}99.6_{{-}18.0}^{{+}17.8}$ | $\phantom{0}\phantom{0}475.1_{{-}\phantom{0}9.3}^{{+}29.6}$ | $\phantom{0}\phantom{0}595.7_{{-}75.1}^{{+}65.3}$ | ${<}250.8$ |  $\cdots$ |  $\cdots$
051.4${+}$09.6 | $\phantom{0}1882.4_{{-}13.5}^{{+}36.4}$ |  $\cdots$ | $\phantom{0}\phantom{0}315.8_{{-}12.1}^{{+}15.0}$ | $\phantom{0}\phantom{0}740.7_{{-}56.1}^{{+}41.7}$ | $\phantom{0}\phantom{0}180.1_{{-}42.6}^{{+}32.7}$ |  $\cdots$ |  $\cdots$
052.2${-}$04.0 | $\phantom{0}2778.2_{{-}41.1}^{{+}38.8}$ |  $\cdots$ | $\phantom{0}\phantom{0}478.9_{{-}40.3}^{{+}33.0}$ | $\phantom{0}\phantom{0}192.2_{{-}49.9}^{{+}47.2}$ | ${<}138.0$ |  $\cdots$ |  $\cdots$
058.3${-}$10.9 | $\phantom{0}1580.9_{{-}23.7}^{{+}33.7}$ |  $\cdots$ | $\phantom{0}\phantom{0}354.5_{{-}14.5}^{{+}26.0}$ | ${<}252.0$ | ${<}124.7$ |  $\cdots$ |  $\cdots$
060.1${-}$07.7 | $\phantom{0}1489.3_{{-}13.4}^{{+}18.8}$ | $\phantom{0}\phantom{0}179.9_{{-}\phantom{0}9.8}^{{+}\phantom{0}8.4}$ | $\phantom{0}\phantom{0}\phantom{0}50.0_{{-}10.6}^{{+}\phantom{0}9.9}$ | $\phantom{0}3259.8_{{-}47.6}^{{+}47.8}$ | $\phantom{0}2085.7_{{-}43.7}^{{+}46.6}$ | $\phantom{0}5697.5_{{-}65.0}^{{+}71.7}$ | $\phantom{0}2172.0_{{-}39.7}^{{+}47.5}$
060.5${+}$01.8 | $\phantom{0}2334.5_{{-}\phantom{0}7.7}^{{+}54.5}$ |  $\cdots$ | $\phantom{0}\phantom{0}379.5_{{-}13.2}^{{+}\phantom{0}7.7}$ | $\phantom{0}\phantom{0}543.1_{{-}85.9}^{{+}48.1}$ | $\phantom{0}\phantom{0}175.0_{{-}47.2}^{{+}\phantom{0}0.4}$ |  $\cdots$ |  $\cdots$
064.7${+}$05.0 | $\phantom{0}\phantom{0}479.5_{{-}19.0}^{{+}20.6}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}72.0_{{-}19.3}^{{+}30.4}$ | $\phantom{0}5717.7_{{-}166.3}^{{+}187.7}$ | $\phantom{0}1790.1_{{-}62.9}^{{+}100.9}$ |  $\cdots$ |  $\cdots$
071.6${-}$02.3 | $\phantom{0}\phantom{0}623.6_{{-}15.8}^{{+}39.5}$ |  $\cdots$ | $\phantom{0}\phantom{0}139.0_{{-}17.5}^{{+}24.8}$ | $\phantom{0}1853.9_{{-}152.0}^{{+}95.9}$ | $\phantom{0}\phantom{0}559.1_{{-}120.2}^{{+}77.4}$ |  $\cdots$ |  $\cdots$
074.5${+}$02.1 | $\phantom{0}1507.3_{{-}47.9}^{{+}63.7}$ | $\phantom{0}\phantom{0}317.6_{{-}25.1}^{{+}48.7}$ | $\phantom{0}\phantom{0}104.7_{{-}31.3}^{{+}170.7}$ | $\phantom{0}3458.0_{{-}263.3}^{{+}298.1}$ | $\phantom{0}2146.1_{{-}131.8}^{{+}477.7}$ | $\phantom{0}3936.3_{{-}217.8}^{{+}348.3}$ | $\phantom{0}5582.0_{{-}310.8}^{{+}274.4}$
082.1${+}$07.0 | $\phantom{0}2773.7_{{-}27.6}^{{+}291.2}$ | $\phantom{0}\phantom{0}203.6_{{-}\phantom{0}9.5}^{{+}38.5}$ | $\phantom{0}\phantom{0}279.1_{{-}17.6}^{{+}47.0}$ |  $\cdots$ |  $\cdots$ | $\phantom{0}2007.7_{{-}52.5}^{{+}82.0}$ | $\phantom{0}\phantom{0}\phantom{0}93.2_{{-}19.5}^{{+}80.4}$
082.5${+}$11.3 | $\phantom{0}1850.5_{{-}56.8}^{{+}69.2}$ |  $\cdots$ | $\phantom{0}\phantom{0}418.8_{{-}66.7}^{{+}91.3}$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
086.5${-}$08.8 | $\phantom{0}1225.3_{{-}16.8}^{{+}18.4}$ | $\phantom{0}\phantom{0}503.8_{{-}14.4}^{{+}16.0}$ |  $\cdots$ | ${<}140.6$ | ${<}123.9$ | $\phantom{0}2075.1_{{-}47.1}^{{+}45.4}$ | $\phantom{0}4149.5_{{-}88.3}^{{+}73.8}$
089.3${-}$02.2 | $\phantom{0}\phantom{0}\phantom{0}58.2_{{-}\phantom{0}4.8}^{{+}18.0}$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}187.6_{{-}15.8}^{{+}59.6}$ | ${<}48.8$ |  $\cdots$ |  $\cdots$
089.8${-}$05.1 | $\phantom{0}\phantom{0}284.4_{{-}\phantom{0}2.9}^{{+}14.9}$ | $\phantom{0}\phantom{0}\phantom{0}31.3_{{-}\phantom{0}5.1}^{{+}11.7}$ | $\phantom{0}\phantom{0}\phantom{0}88.8_{{-}\phantom{0}5.4}^{{+}10.2}$ | $\phantom{0}2869.5_{{-}36.7}^{{+}79.0}$ | $\phantom{0}\phantom{0}953.0_{{-}17.2}^{{+}44.0}$ | $\phantom{0}\phantom{0}276.9_{{-}\phantom{0}4.9}^{{+}23.1}$ | $\phantom{0}\phantom{0}\phantom{0}40.8_{{-}\phantom{0}5.7}^{{+}13.6}$
095.2${+}$00.7 | $\phantom{0}1430.9_{{-}32.0}^{{+}38.1}$ |  $\cdots$ | $\phantom{0}\phantom{0}316.8_{{-}14.4}^{{+}35.7}$ | $\phantom{0}\phantom{0}415.1_{{-}43.4}^{{+}55.9}$ | ${<}138.7$ |  $\cdots$ |  $\cdots$
100.6${-}$05.4 | $\phantom{0}2648.6_{{-}42.1}^{{+}41.4}$ | $\phantom{0}\phantom{0}\phantom{0}86.8_{{-}17.6}^{{+}23.1}$ | $\phantom{0}\phantom{0}174.4_{{-}36.0}^{{+}32.5}$ |  $\cdots$ |  $\cdots$ | $\phantom{0}\phantom{0}207.7_{{-}41.2}^{{+}40.0}$ |  $\cdots$
111.8${-}$02.8 | $\phantom{0}\phantom{0}422.8_{{-}31.8}^{{+}\phantom{0}0.7}$ |  $\cdots$ | ${<}177.5$ | ${<}376.8$ | $\phantom{0}\phantom{0}179.2_{{-}32.0}^{{+}41.0}$ |  $\cdots$ |  $\cdots$
118.0${-}$08.6 | $\phantom{0}\phantom{0}876.0_{{-}59.9}^{{+}57.3}$ |  $\cdots$ | ${<}124.1$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$
123.6${+}$34.5 | $\phantom{0}3217.8_{{-}71.6}^{{+}77.1}$ |  $\cdots$ | ${<}271.0$ | ${<}321.3$ |  $\cdots$ |  $\cdots$ |  $\cdots$
146.7${+}$07.6 | $\phantom{0}\phantom{0}317.0_{{-}\phantom{0}5.0}^{{+}20.9}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}57.3_{{-}\phantom{0}9.4}^{{+}19.8}$ | $\phantom{0}3562.1_{{-}84.5}^{{+}121.4}$ | $\phantom{0}\phantom{0}676.7_{{-}38.6}^{{+}69.3}$ |  $\cdots$ |  $\cdots$
159.0${-}$15.1 | $\phantom{0}1660.3_{{-}49.9}^{{+}43.4}$ | $\phantom{0}\phantom{0}270.2_{{-}36.4}^{{+}37.1}$ | ${<}234.5$ |  $\cdots$ |  $\cdots$ | $\phantom{0}3545.4_{{-}136.3}^{{+}109.5}$ |  $\cdots$
166.1${+}$10.4 | $\phantom{0}1723.6_{{-}23.4}^{{+}20.6}$ |  $\cdots$ | $\phantom{0}\phantom{0}154.5_{{-}24.6}^{{+}25.5}$ | $\phantom{0}\phantom{0}112.8_{{-}31.5}^{{+}122.4}$ | ${<}84.6$ |  $\cdots$ |  $\cdots$
190.3${-}$17.7 | $\phantom{0}2110.9_{{-}27.2}^{{+}32.7}$ |  $\cdots$ | $\phantom{0}\phantom{0}215.4_{{-}44.8}^{{+}41.2}$ | ${<}202.7$ |  $\cdots$ |  $\cdots$ |  $\cdots$
194.2${+}$02.5 | $\phantom{0}\phantom{0}372.3_{{-}17.7}^{{+}11.4}$ | $\phantom{0}\phantom{0}\phantom{0}85.0_{{-}\phantom{0}9.3}^{{+}12.7}$ | ${<}44.5$ | $\phantom{0}1157.9_{{-}53.9}^{{+}79.8}$ | $\phantom{0}\phantom{0}379.3_{{-}46.7}^{{+}56.9}$ | $\phantom{0}\phantom{0}585.6_{{-}21.7}^{{+}26.1}$ | $\phantom{0}\phantom{0}\phantom{0}82.2_{{-}23.5}^{{+}27.1}$
211.2${-}$03.5 | $\phantom{0}\phantom{0}476.4_{{-}10.3}^{{+}12.3}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}71.3_{{-}12.3}^{{+}12.4}$ | $\phantom{0}\phantom{0}173.7_{{-}25.6}^{{+}84.5}$ | ${<}95.3$ |  $\cdots$ |  $\cdots$
221.3${-}$12.3 | $\phantom{0}1873.6_{{-}18.8}^{{+}23.2}$ | $\phantom{0}\phantom{0}371.5_{{-}21.0}^{{+}22.7}$ | $\phantom{0}\phantom{0}148.6_{{-}28.1}^{{+}30.7}$ | ${<}655.3$ | ${<}273.5$ | $\phantom{0}5881.3_{{-}78.8}^{{+}74.2}$ | $\phantom{0}1983.8_{{-}62.0}^{{+}63.3}$
226.7${+}$05.6 | $\phantom{0}1578.7_{{-}19.0}^{{+}22.1}$ | $\phantom{0}\phantom{0}142.7_{{-}13.3}^{{+}14.8}$ | $\phantom{0}\phantom{0}147.0_{{-}20.4}^{{+}32.7}$ | $\phantom{0}3534.1_{{-}134.5}^{{+}206.2}$ | $\phantom{0}2311.3_{{-}98.9}^{{+}100.0}$ | $\phantom{0}1501.2_{{-}37.7}^{{+}45.9}$ | $\phantom{0}\phantom{0}659.9_{{-}26.9}^{{+}42.4}$
232.8${-}$04.7 | $\phantom{0}\phantom{0}191.3_{{-}\phantom{0}9.0}^{{+}12.9}$ |  $\cdots$ | ${<}40.3$ | $\phantom{0}\phantom{0}865.2_{{-}59.6}^{{+}67.6}$ | $\phantom{0}\phantom{0}250.9_{{-}22.8}^{{+}47.1}$ |  $\cdots$ |  $\cdots$
235.3${-}$03.9 | $\phantom{0}\phantom{0}339.2_{{-}15.4}^{{+}14.4}$ |  $\cdots$ | $\phantom{0}\phantom{0}\phantom{0}50.9_{{-}11.2}^{{+}17.7}$ | $\phantom{0}\phantom{0}243.1_{{-}35.8}^{{+}32.0}$ | ${<}92.8$ |  $\cdots$ |  $\cdots$
258.1${-}$00.3 | $\phantom{0}1577.4_{{-}19.8}^{{+}23.8}$ |  $\cdots$ | $\phantom{0}\phantom{0}248.9_{{-}16.0}^{{+}21.1}$ | $\phantom{0}\phantom{0}195.1_{{-}42.1}^{{+}81.7}$ |  $\cdots$ |  $\cdots$ |  $\cdots$
264.4${-}$12.7 | $\phantom{0}2768.5_{{-}47.2}^{{+}62.1}$ |  $\cdots$ | $\phantom{0}\phantom{0}273.6_{{-}47.5}^{{+}54.6}$ | ${<}289.7$ | ${<}223.4$ |  $\cdots$ |  $\cdots$
268.4${+}$02.4 | $\phantom{0}\phantom{0}354.8_{{-}\phantom{0}7.8}^{{+}\phantom{0}8.2}$ | $\phantom{0}\phantom{0}\phantom{0}86.7_{{-}\phantom{0}6.4}^{{+}13.9}$ | $\phantom{0}\phantom{0}\phantom{0}64.2_{{-}\phantom{0}9.2}^{{+}15.1}$ | $\phantom{0}4927.5_{{-}135.8}^{{+}166.2}$ | $\phantom{0}2485.7_{{-}57.7}^{{+}86.2}$ | $\phantom{0}1292.7_{{-}32.9}^{{+}34.2}$ | $\phantom{0}\phantom{0}894.1_{{-}21.5}^{{+}37.5}$