J/ApJ/949/74 Spitzer, WISE & Herschel obs. of the young SNR N132D (Rho+, 2023)
Infrared ejecta and cold dust in the young supernova remnant N132D.
Rho J., Ravi A.P., Slavin J.D., Cha H.
<Astrophys. J., 949, 74 (2023)>
=2023ApJ...949...74R 2023ApJ...949...74R
ADC_Keywords: Magellanic Clouds; Supernova remnants; Spectra, infrared;
Energy distributions
Keywords: Dust continuum emission ; Core-collapse supernovae ;
Type Ib supernovae ; Early universe ; Supernova remnants ;
Large Magellanic Cloud ; Origin of the universe ;
Far infrared astronomy ; Interstellar emissions
Abstract:
We present Spitzer, Wide-field Infrared Survey Explorer (WISE), and
Herschel observations of the young supernova remnant (SNR) N132D in
the Large Magellanic Cloud, including 3-40µm Spitzer Infrared
Spectrograph (IRS) mapping, 12µm WISE and 70, 100, 160, 250, 350,
and 500µm Herschel images. The high-velocity lines of [NeII] at
12.8µm, [NeIII] at 15.5µm, and [OIV] 26µm reveal infrared
ejecta concentrated in a central ring and coincide with the optical
and X-ray ejecta. Herschel images reveal far-IR emission coinciding
with the central ejecta, which suggests that the IR emission is
freshly formed, cold dust in the SN ejecta. The infrared spectra are
remarkably similar to those of another young SNR of 1E0102 with Ne and
O lines. Shock modeling of the Ne ejecta emission suggests a gas
temperature of 300-600K and densities in the range 1000-2x104cm-3
in the postshock photoionized region. The IR continuum from the ejecta
shows an 18µm peak dust feature. We performed spectral fitting to
the IRS dust continuum and Herschel photometry. The dust mass
associated with the central ejecta is 1.25±0.65M☉, while the
18µm dust feature requires forsterite grains. The dust mass of the
central ejecta region in N132D is higher than those of other young
SNRs, which is likely associated with its higher progenitor mass. We
discuss the dust productivity in the ejecta of N132D and infer its
plausible implications for dust in the early universe.
Description:
In this paper, we use archival Herschel, Wide-field Infrared Survey
Explorer (WISE), and Spitzer images and Spitzer Infrared Spectrograph
(IRS) observations of N132D and present maps of infrared emission from
the IR ejecta in the YSNR N132D and the cold dust likely associated
with the IR ejecta. The Herschel and WISE observations of N132D are
presented here for the first time.
Herschel observations of N132D were taken as a part of Herschel LMC
GTO and Key project (Proposal_ID of KPOTmmeixner1 and
SDPmmeixner1) on 2010-Apr-30 to cover the entire LMC with the
Herschel PACS and SPIRE images using the parallel mode. The
observational IDs are 1342187188, 1342195707, 1342195708, 1342202224,
and 1342202225. The spatial resolutions of Herschel images are 8",
12", 18.1", 24.9" and 36.4" at 100, 160, 250, 350, and 500um,
respectively. See Section 2.1.
We used archival WISE images of N132D on 2010-May-4. WISE is a whole
sky mid-IR (MIR) survey that uniquely provides data beyond the
Galactic plane. WISE w1, w2, w3, and w4 images are centered at 3.4,
4.6, 12, and 22um, respectively. WISE w1 and w2 images did not detect
IR emission from N132D. The WISE w3 image of N132D is shown in Figure
3, showing the central ejecta emission as well as the circular shell
emission. The WISE w4 image is similar to Spitzer 24um image but 3
times lower spatial resolution.
We used archival observations (PID of 3483 on 2004-Nov-7 and
2004-Dec-14 and 30372 on 2007-Jun-23) by Spitzer for IRS Long-Low
(IRS-LL) mapping covering the entire SNR, and IRS staring of Short-Low
(SL) observations toward four positions (see Tappe+ 2006ApJ...653..267T 2006ApJ...653..267T).
The staring mode was 12 cycles of 60s exposures for SL. IRS-LL mapping
is two cycles of 30s exposure for 10" stepsize, resulting in 4 minutes
of integration per position. See Section 2.3.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
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05 25 02.30 -69 38 39.0 N132D = LHA 120-N 132D
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 150 4 Comparison of the line widths from different regions
sp/* . 4 Spitzer IRS spectra toward NE Ejecta, Lasker's Bowl,
West Complex and the central ejecta
(Data behind Figure 4)
fig10.dat 30 155 Spectral energy distribution of N132D toward the
central ejecta emission
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See also:
II/328 : AllWISE Data Release (Cutri+ 2013)
VI/139 : Herschel Observation Log (Herschel Science Centre, 2013)
J/A+A/420/763 : Electron impact excitation of NiII (Bautista+, 2004)
J/A+A/475/765 : Fine structure forbidden lines in FeII (Ramsbottom+, 2007)
J/ApJ/656/770 : Mid-IR spectrum of star-forming galaxies (Smith+, 2007)
J/A+A/587/A93 : MeV-GeV counterparts of TeV sources (Rappoldi+, 2016)
J/A+A/625/A122 : CIELO-RGS, soft X-ray ionized emission lines (Mao+, 2019)
J/ApJ/905/55 : Bright-PAH galaxies from AKARI & Spitzer (ASESS) (Lai+, 2020)
J/ApJS/257/36 : ISO supernovae remnants spectra (Millard+, 2021)
J/other/Nat/601.201 : Photometry of SN 2019hgp (Gal-Yam+, 2022)
J/ApJ/948/33 : HST proper motion measurements of SNR N132D (Banovetz+, 2023)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- Region Region identifier
15- 20 F6.3 um lambdaNeIII [15.568/15.595] Wavelength, [NeIII]
22- 26 F5.3 um e_lambdaNeIII [0.001/0.002] lambdaNeIII uncertainty
28- 32 F5.3 um FWHMNeIII [0.15/0.2] FWHM, [NeIII]
34- 38 F5.3 um e_FWHMNeIII [0.001/0.004] FWHMNeIII uncertainty
40- 43 I4 km/s VelNeIII [2982/3620] Velocity, [NeIII]
45- 46 I2 km/s e_VelNeIII [14/60] VelNeIII uncertainty
48- 50 I3 km/s VShiftNeIII [307/781] Velocity shift, [NeIII]
52- 53 I2 km/s e_VShiftNeIII [6/25] VShiftNeIII uncertainty
55- 58 I4 km/s VelTrueNeIII [1265/2411] Velocitytrue, [NeIII]
60- 62 I3 km/s e_VelTrueNeIII [31/136] VelTrueNeIII uncertainty
64- 69 F6.3 um lambdaNeII [12.82/12.85]? Wavelength, [NeII]
71- 75 F5.3 um e_lambdaNeII [0.001/0.001]? lambdaNeII uncertainty
77- 81 F5.3 um FWHMNeII [0.1/0.13]? FWHM, [NeII]
83- 87 F5.3 um e_FWHMNeII [0.001/0.003]? FWHMNeII uncertainty
89- 92 I4 km/s VelNeII [2676/2987]? Velocity, [NeII]
94- 95 I2 km/s e_VelNeII [16/47]? VelNeII uncertainty
97- 99 I3 km/s VShiftNeII [319/806]? Velocity shift, [NeII]
101- 102 I2 km/s e_VShiftNeII [7/16]? VShiftNeII uncertainty
104- 107 I4 km/s VelTrueNeII [726/1513]? Velocitytrue, [NeII]
109- 110 I2 km/s e_VelTrueNeII [57/91]? VelTrueNeII uncertainty
112- 150 A39 --- FileName Name of the spectrum in ASCII format in
subdirectory "sp"; column added by CDS
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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1- 7 F7.4 um lambda [5.2/38.4] Wavelength
9- 20 E12.5 Jy/sr SBFlux [-579890/2.81e+07] Surface brightness flux
22- 32 E11.5 Jy/sr e_SBFlux [40041.8/3.4e+06] Uncertainty in SBFlux
34- 34 I1 --- det [1] det
36- 36 I1 --- line [1] line
38- 38 I1 --- sdir [0/3] sdir
40- 40 I1 --- scnt [1/4] scnt
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Byte-by-byte Description of file: fig10.dat
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Bytes Format Units Label Explanations
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1- 8 F8.4 um lambda [14.26/350] Wavelength
10- 18 F9.7 Jy Flux [0.016/0.6] Flux density
20- 30 F11.9 Jy e_Flux [0.00049/0.07] Standard deviation of flux
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Jul-2025