J/ApJ/929/144 SNR and HII regions in M83 observed with MUSE (Long+, 2022)
Supernova remnants in M83 as observed with MUSE.
Long K.S., Blair W.P., Winkler P.F., Della Bruna L., Adamo A.,
McLeod A.F., Amram P.
<Astrophys. J., 929, 144 (2022)>
=2022ApJ...929..144L 2022ApJ...929..144L
ADC_Keywords: Supernova remnants ; H II regions ; Spectra, optical ;
Interstellar medium ; Cross identifications ; X-ray sources
Keywords: Supernova remnants ; Interstellar medium
Abstract:
Here we describe a new study of the supernova remnants (SNRs) and SNR
candidates in nearby face-on spiral galaxy M83, based primarily on
MUSE integral field spectroscopy. Our revised catalog of SNR
candidates in M83 has 366 objects, 81 of which are reported here for
the first time. Of these, 229 lie within the MUSE observation region,
160 of which have spectra with [SII]:Hα ratios exceeding 0.4,
the value generally accepted as confirmation that an emission nebula
is shock-heated. Combined with 51 SNR candidates outside the MUSE
region with high [SII]:Hα ratios, there are 211 spectroscopically
confirmed SNRs in M83, the largest number of confirmed SNRs in any
external galaxy. MUSE's combination of relatively high spectral
resolution and broad wavelength coverage has allowed us to explore two
other properties of SNRs that could serve as the basis of future SNR
searches. Specifically, most of the objects identified as SNRs on the
basis of [SII]:Hα ratios exhibit more velocity broadening and
lower ratios of [SIII]:[SII] emission than HII regions. A search for
nebulae with the very broad emission lines expected from young,
rapidly expanding remnants revealed none, except for the previously
identified B12-174a. The SNRs identified in M83 are, with few
exceptions, middle-aged interstellar medium (ISM) dominated ones.
Smaller-diameter candidates show a larger range of velocity broadening
and a larger range of gas densities than the larger-diameter objects,
as expected if the SNRs expanding into denser gas brighten and then
fade from view at smaller diameters than those expanding into a more
tenuous ISM.
Description:
MUSE is an integral field spectrograph mounted on ESO's VLT in Chile.
For the purposes of this paper, we use data obtained from various ESO
programs: 096.B-0057(A), 0101.B-0727(A) (PI Adamo), 097.B-0899(B)
(PI Ibar), and 097.B-0640(A) (PI Gadotti). These data covered the
spectral range 4600-9380Å with a spectral resolution of about
2.3Å, which corresponds to a velocity resolution of about 115km/s
at Hα. Individual exposures cover a field of 1'x1'; each spaxel
is 0.2"x0.2" in extent.
M83 has been well observed previously, and these earlier data sets
complement the MUSE data in several ways. See Section 2.
Objects:
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RA (ICRS) DE Designation(s)
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13 37 00.91 -29 51 56.7 M83 = NAME Southern Pinwheel Galaxy
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 67 366 Supernova remnants and candidates in M83
table2.dat 121 229 MUSE spectra of M83 supernova remnant candidates
table3.dat 34 188 Comparison HII regions in M83
table4.dat 122 188 MUSE spectra of M83 HII regions
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See also:
J/AJ/138/332 : LEDA CMD/tip of the red giant branch (Jacobs+, 2009)
J/ApJS/203/8 : Optical SNR candidates in M83 (Blair+, 2012)
J/ApJ/788/55 : HST/WFC3 SNR discoveries in M83 (NGC5236) (Blair+, 2014)
J/ApJS/212/21 : A deep Chandra ACIS survey of M83 (Long+, 2014)
J/ApJ/839/83 : GMOS spectroscopic obs. of SNR cand. in M83 (Winkler+, 2017)
J/ApJ/855/140 : MMT spectra of SNRs and SNR candidates in M33 (Long+, 2018)
J/ApJ/881/54 : Masses of SNR progenitors in M83 (Williams+, 2019)
J/MNRAS/495/479 : New radio catalog for M83 SNR & HII regions (Russell+, 2020)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- ID Source name (1)
11- 19 F9.5 deg RAdeg [204.16/204.4] Right Ascension (J2000)
21- 29 F9.5 deg DEdeg [-30/-29.7] Declination (J2000)
31- 32 I2 pc Diam [3/97] Estimated diameter
34- 36 F3.1 kpc R [0/9] Distance from the nucleus (2)
38- 41 A4 --- [LKB2014] X-ray source identification (3)
43- 47 A5 --- Origin Discovery origin (4)
49- 52 A4 --- Inst Instrument used to obtain spectra
54- 57 A4 --- Ratio Measured spectroscopic [SII]/Hα>0.4? (5)
59- 67 A9 --- Comm Additional comments (6)
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Note (1): Source names beginning with "B12-", "B14-", and "D10-" are from
Blair+ (2012, J/ApJS/203/8 ; <[BWL2012] NNN> in Simbad),
Blair+ (2014, J/ApJ/788/55 ; <[BCD2014] NN> in Simbad), and
Dopita+ (2010ApJ...710..964D 2010ApJ...710..964D ; <[DBL2010] M83-SNR-1-NN> (nos 1-40) or
<[DBL2010] M83-SNR-N-NN> (nos 01-19) in Simbad), respectively.
Previously unpublished candidates begin with "L22-".
Note (2): The galactocentric distances assume an inclination and position angle
of 24 and 45 degrees, respectively (Talbot+ 1979ApJ...229...91T 1979ApJ...229...91T).
Note (3): X-ray sources in the Long+ (2014, J/ApJS/212/21) list within 1" of
a SNR candidate.
Note (4): Discovery origin as follows:
W19 = the object was included in the list of Williams+ 2019, J/ApJ/881/54 ;
279 occurrences),
MUSE = seen first in the MUSE data (44 occurrences),
New = has been based on further inspection of the HST or Magellan data
(37 occurrences)
Other = Six other objects previously published by
Dopita+ (2010ApJ...710..964D 2010ApJ...710..964D) or Blair+ (2014, J/ApJ/788/55) that
were considered too marginal to be included in the Williams+ (2019)
list have been reinstated here for completeness.
See Section 3.3.
Note (5): Identification as follows:
Both = Observed to have a high ratio with both GMOS and MUSE;
GMOS = Observed to have a high ratio in GMOS;
MUSE = Observed to have a high ratio in MUSE;
no = There are no spectra that show a high enough ratio.
Note (6): Objects with the comment [FeII] were first identified on the basis
of detectable [FeII]1.67um emission.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- ID Source name
11- 16 F6.1 10-20W/m2/arcsec2 HaSB [2.8/9630] Hα surface
brightness; in units of
10-17erg/cm2/s/arcsec2
18- 21 F4.1 10-20W/m2/arcsec2 e_HaSB [0.2/93] Uncertainty in HaSB
23 A1 --- l_Hb 1 sigma upper limit flag on Hb
25- 29 F5.1 --- Hb [1/132] Hβ line flux (1)
31- 34 F4.1 --- e_Hb [0.1/54]? Uncertainty in Hb
36 A1 --- l_O3-5007 1 sigma upper limit flag on O3-5007
38- 42 F5.1 --- O3-5007 [0.3/413] [OIII]5007Å line
flux (1)
44- 47 F4.1 --- e_O3-5007 [0.1/54]? Uncertainty inO3-5007
49 A1 --- l_O1-6300 1 sigma upper limit flag on O1-6300
51- 56 F6.1 --- O1-6300 [1/659] [OI]6300Å line flux (1)
58- 61 F4.1 --- e_O1-6300 [0.1/89]? Uncertainty in O1-6300
63- 65 I3 --- Ha [300] Hα line flux
67- 71 F5.1 --- N2-6584 [68/653] [NII]6584Å line flux (1)
73- 76 F4.1 --- e_N2-6584 [0.4/30] Uncertainty in N2-6584
78- 82 F5.1 --- S2-6716 [25.7/250] [SII]6716Å line
flux (1)
84- 87 F4.1 --- e_S2-6716 [0.2/26] Uncertainty in S2-6716
89- 93 F5.1 --- S2-6731 [22/234.2] [NII]6731Å line
flux (1)
95- 98 F4.1 --- e_S2-6731 [0.2/22] Uncertainty in S2-6731
100 A1 --- l_S3-9069 1 sigma upper limit flag on S3-9069
102-106 F5.1 --- S3-9069 [1/107] [SIII]9069Å line flux (1)
108-111 F4.1 --- e_S3-9069 [0.1/34]? Uncertainty in S3-9069
113-116 F4.2 0.1nm FWHM [2.2/6.6] Hα line full-width
at half-maximum; Angstroms
118-121 F4.2 0.1nm e_FWHM [0/0.4] Uncertainty in FWHM
--------------------------------------------------------------------------------
Note (1): Relative to Hα where, by convention, Hα is
normalized to 300.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Source name
9- 17 F9.5 deg RAdeg [204.2/204.31] Right Ascension (J2000)
19- 27 F9.5 deg DEdeg [-30/-29.8] Declination (J2000)
29- 30 I2 pc Diam [11/86] Estimated diameter
32- 34 F3.1 kpc R [0.3/3.7] Distance from the nucleus (1)
--------------------------------------------------------------------------------
Note (1): The galactocentric distances assume an inclination and position angle
of 24 and 45 degrees, respectively (Talbot+ 1979ApJ...229...91T 1979ApJ...229...91T).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Source name
9- 14 F6.1 10-20W/m2/arcsec2 HaSB [4/1572] Hα surface
brightness in units of
10-17erg/cm2/s/arcsec2
16- 18 F3.1 10-20W/m2/arcsec2 e_HaSB [0.1/5] Uncertainty in HaSB
20 A1 --- l_Hb 1 sigma upper limit flag on Hb
22- 26 F5.1 --- Hb [11.8/451] Hβ line flux (1)
28- 32 F5.1 --- e_Hb [0.1/134]? Uncertainty in Hb
34 A1 --- l_O3-5007 1 sigma upper limit flag on O3-5007
36- 41 F6.1 --- O3-5007 [0.7/1132] [OIII]5007Å line
flux (1)
43- 46 F4.1 --- e_O3-5007 [0.1/40]? Uncertainty inO3-5007
48 A1 --- l_O1-6300 1 sigma upper limit flag on O1-6300
50- 53 F4.1 --- O1-6300 [0.6/92] [OI]6300Å line flux (1)
55- 59 F5.1 --- e_O1-6300 [0.1/130]? Uncertainty in O1-6300
61- 63 I3 --- Ha [300] Hα line flux
65- 69 F5.1 --- N2-6584 [7.8/560] [NII]6584Å line
flux (1)
71- 74 F4.1 --- e_N2-6584 [0.5/32] Uncertainty in N2-6584
76 A1 --- l_S2-6716 1 sigma upper limit flag on S2-6716
78- 82 F5.1 --- S2-6716 [4.9/242] [SII]6716Å line
flux (1)
84- 87 F4.1 --- e_S2-6716 [0.2/30]? Uncertainty in S2-6716
89 A1 --- l_S2-6731 1 sigma upper limit flag on S2-6731
91- 95 F5.1 --- S2-6731 [2.6/151] [NII]6731Å line
flux (1)
97-100 F4.1 --- e_S2-6731 [0.2/26]? Uncertainty in S2-6731
102 A1 --- l_S3-9069 1 sigma upper limit flag on S3-9069
104-107 F4.1 --- S3-9069 [1/81] [SIII]9069Å line flux (1)
109-112 F4.1 --- e_S3-9069 [0.1/15]? Uncertainty in S3-9069
114-117 F4.2 0.1nm FWHM [2/5.4] Hα line full-width at
half-maximum; Angstroms
119-122 F4.2 0.1nm e_FWHM [0/0.3] Uncertainty in FWHM
--------------------------------------------------------------------------------
Note (1): Relative to Hα where, by convention, Hα is
normalized to 300.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 11-Mar-2024