J/ApJS/257/36 ISO supernovae remnants spectra (Millard+, 2021)
A spectroscopic study of supernova remnants with the Infrared Space Observatory.
Millard M.J., Ravi A.P., Rho J., Park S.
<Astrophys. J. Suppl. Ser., 257, 36-36 (2021)>
=2021ApJS..257...36M 2021ApJS..257...36M (SIMBAD/NED BibCode)
ADC_Keywords: Supernova remnants ; Interstellar medium ; Spectra, infrared
Keywords: far infrared astronomy - supernova remnants - interstellar medium -
astrophysical dust processes - shocks
Abstract:
We present far-infrared (FIR) spectroscopy of supernova remnants
(SNRs) based on the archival data of the Infrared Space Observatory
taken with the Long Wavelength Spectrometer (LWS). Our sample includes
previously unpublished profiles of line and continuum spectra for 20
SNRs in the Galaxy and Magellanic Clouds. In several SNRs including
G21.5-0.9, G29.7-0.3, the Crab Nebula, and G320.4-1.2, we find
evidence for broad [OI], [OIII], [NII], and [CII] lines with
velocity dispersions up to a few 103km/s, indicating that they
are associated with high-velocity SN ejecta. Our detection of
Doppler-broadened atomic emission lines and a bright FIR continuum
hints at the presence of newly formed dust in SN ejecta. For
G320.4-1.2, we present the first estimate of an ejecta-dust mass of
0.1-0.2M☉, which spatially coincides with the broad-line
emission, by applying a blackbody model fit with components of the SNR
and background emission. Our sample includes raster maps of 63µm,
145µm [OI], and 158µm [CII] lines toward SNRs Kes 79, CTB
109, and IC 443. Based on these line intensities, we suggest
interacting shock types in these SNRs. Finally, we compare our LWS
spectra of our sample SNRs with the spectra of several HII regions,
and discuss their FIR line intensity ratios and continuum properties.
Follow-up observations with modern instruments (e.g., JWST and SOFIA)
with higher spatial and spectral resolution are encouraged for an
extensive study of the SN ejecta and the SN dust.
Description:
ISO spectroscopy of SNRs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 100 37 ISO LWS observations of our sample of SNRs
and HII regions
list.dat 57 61 List of spectra
sp/* . 61 Individual spectra
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Type Type
6- 17 A12 --- Name Name
19- 40 A22 --- Target Target name (1)
42- 43 I2 h RAh Right ascension (J2000)
45- 46 I2 min RAm Right ascension (J2000)
48- 52 F5.2 s RAs Right ascension (J2000)
54 A1 --- DE- Declination sign (J2000)
55- 56 I2 deg DEd Declination (J2000)
58- 59 I2 arcmin DEm Declination (J2000)
61- 65 F5.2 arcsec DEs Declination (J2000)
67- 77 A11 "date" Date Observation date
79- 82 I4 s ton Exposure time
84- 98 A15 --- Refs References (2)
100 A1 --- Sp [*] indicates spectrum in sp subdirectory
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Note (1): The majority of targets were observed in the L01 mode, which covered
the full range of the LWS detector. A few targets were observed in the L02
mode, which covered only certain wavelength bands specified by the observer.
Note (2): References as follows:
1 = Snell et al. (2005ApJ...620..758S 2005ApJ...620..758S)
2 = Liseau et al. (2006A&A...446..561L 2006A&A...446..561L)
3 = He et al. (2005A&A...434..201H 2005A&A...434..201H, Cat. J/A+A/434/201)
4 = Liu et al. (2001MNRAS.323..343L 2001MNRAS.323..343L)
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 22 A22 --- Target Target name
24- 57 A34 --- FileName Name of the spectrum file in subdirectory sp
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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- 8 F8.4 um lambda Wavelength in micrometer (LSANWAV)
10- 33 E24.17 W/cm2/um Flux Flux in W/cm^2/micrometer (LSANFLX)
35- 56 E22.17 W/cm2/um e_Flux Flux Uncertainty in W/cm^2/micrometer
(LSANFLXU)
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Acknowledgements:
Apazhayath Ravi, apazhayathravi(at)ucdavis.edu
(End) Patricia Vannier [CDS] 14-Feb-2024