J/ApJS/268/61 Associations between SNRs and molecular clouds (Zhou+, 2023)
A systematic study of associations between supernova remnants and molecular
clouds.
Zhou X., Su Y., Yang Ji, Chen X., Sun Y., Jiang Z., Wang M., Wang H.,
Zhang S., Xu Ye, Yan Q., Yuan L., Chen Z., Ao Y., Ma Y.
<Astrophys. J. Suppl. Ser., 268, 61 (2023)>
=2023ApJS..268...61Z 2023ApJS..268...61Z
ADC_Keywords: Supernova remnants; Molecular clouds; Interstellar medium;
Space velocities;
Keywords: Interstellar medium ; Supernova remnants ; Molecular clouds ;
Galaxy structure
Abstract:
We universally search for evidence of kinematic and spatial
correlation of supernova remnant (SNR) and molecular cloud (MC)
associations for nearly all SNRs in the coverage of the Milky Way
Imaging Scroll Painting CO survey, i.e., 149 SNRs, 170 SNR candidates,
and 18 pure pulsar wind nebulae in 1°<l<230° and
-5.5°<b<5.5°. Based on high-quality and unbiased
12CO/13CO/C18O(J=1-0) survey data, we apply automatic algorithms
to identify broad lines and spatial correlations for molecular gas in
each SNR region. The 91% of SNR-MC associations detected previously
are identified in this paper by CO line emission. Overall, there could
be as high as 80% of SNRs associated with MCs. The proportion of SNRs
associated with MCs is high within the Galactic longitude less than
∼50°. Kinematic distances of all SNRs that are associated with MCs
are estimated based on systemic velocities of associated MCs. The
radii of SNRs associated with MCs follow a lognormal distribution,
which peaks at ∼8.1pc. The progenitor initial mass of these SNRs
follows a power-law distribution with an index of ~-2.3 that is
consistent with the Salpeter index of -2.35. We find that SNR-MC
associations are mainly distributed in a thin disk along the Galactic
plane, while a small number are distributed in a thick disk. With the
height of these SNRs from the Galactic plane below ∼45pc, the
distribution of the average radius relative to the height of them is
roughly flat, and the average radius increases with the height when
above ∼45pc.
Description:
Supernova remnants (SNRs) in the coverage of the MWISP project,
i.e., nearly all SNRs in 1°<l<230° and -5.5°<b<5.5°,
are investigated. The MWISP project is an unbiased survey of
12CO/13CO/C18O(J=1-0) emission lines (see Su+ 2019ApJS..240....9S 2019ApJS..240....9S ;
Sun+ 2020ApJS..246....7S 2020ApJS..246....7S and references therein, for details), using
the Purple Mountain Observatory Delingha 13.7m millimeter wavelength
telescope.
Radio continuum emission data at 200MHz were obtained from the
Galactic and Extragalactic All-sky Murchison Widefield Array (GLEAM)
survey (Wayth+ 2015PASA...32...25W 2015PASA...32...25W & Hurley-Walker+ 2017, VIII/100 and
2019, VIII/102).
1.4GHz radio continuum emission data were obtained from the NRAO Very
Large Array Sky Survey (Condon+ 1998, VIII/65) and the
HI/OH/Recombination line survey (Beuther+ 2016A&A...595A..32B 2016A&A...595A..32B and
Wang+ 2020, J/A+A/634/A83).
4850MHz radio continuum data were also obtained from the Green Bank
6cm/Parkes-MIT-NRAO survey (Condon+ 1991AJ....102.2041C 1991AJ....102.2041C &
1993AJ....106.1095C 1993AJ....106.1095C & 1994AJ....107.1829C 1994AJ....107.1829C).
20cm radio continuum data are from the Multi-Array Galactic Plane
Imaging Survey (Helfand+ 2006, J/AJ/131/2525).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 402 149 SNR-molecular cloud (MC) associations in survey
table2.dat 387 170 SNR candidate-MC associations in survey
table3.dat 700 100 SNR-MC associations studied in previous works
in our coverage
table4.dat 144 18 Pulsar Wind Nebula (PWN)-MC association candidates
in survey
refs.dat 100 172 References
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See also:
B/psr : ATNF Pulsar Catalogue (Manchester+, 2005)
VI/56 : Tests of shock chemistry in IC 443G (Turner+, 1992)
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
VIII/100 : GaLactic and Extragalactic All-sky MWA survey (Hurley-Walker+, 2016)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
VII/284 : A Catalogue of Galactic Supernova Remnants (Green, 2019)
VIII/102 : GLEAM II. Galactic plane (Hurley-Walker+, 2019)
J/A+A/279/541 : Sub-mm observations of SNR IC 443 (van Dishoeck+ 1993)
J/AJ/131/2525 : MAGPIS 20cm survey (Helfand+, 2006)
J/A+A/508/1331 : CO maps of 3 galactic supernova remnants (Liszt, 2009)
J/A+A/569/A81 : CO obs. towards W44E and W44F with APEX (Anderl+, 2014)
J/ApJS/212/1 : The WISE catalog of Galactic HII regions (Anderson+, 2014)
J/ApJ/788/122 : IR photometry of YSO candidates toward SNR IC 443 (Su+, 2014)
J/A+A/580/A51 : SNR G18.8+0.3 data cubes (Paron+, 2015)
J/A+A/587/A71 : SNR G11.0-0.0 1.4GHz radio cont. image (Castelletti+, 2016)
J/A+A/602/A31 : G29.37+0.1 610MHz image (Castelletti+, 2017)
J/A+A/627/A75 : VRO 42.05.01 CO datacubes (Arias+, 2019)
J/ApJ/878/44 : 13CO clumps toward the CasA supernova remnant (Ma+, 2019)
J/ApJ/885/131 : ∼200 high-mass SFR plx & proper motion with VLBI (Reid+, 2019)
J/A+A/644/A64 : CO observations of the IC443 SNR (Dell'Ova+, 2020)
J/A+A/634/A83 : THOR DR2 source list (Wang+, 2020)
J/A+A/651/A86 : GLOSTAR Galactic plane survey. II. SNR. (Dokara+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- SNR SNR name (GLLL.l+B.b)
12- 27 A16 --- OName Other name(s) if any
30- 36 F7.3 deg GLON [1.4/212.4] Galactic longitude
38- 43 F6.3 deg GLAT [-4.7/7] Galactic latitude
45- 47 I3 arcmin Size [7/575] Size of coverage area
49- 50 A2 --- Type Type of source (1)
52- 140 A89 km/s BL-VLSR Detected broad line Local Standard of Rest
velocity (2)
142- 195 A54 km/s SC-VLSR Spatially correlated molecular gas Local
Standard of Rest velocity (3)
197- 218 A22 km/s Vsys Systemic Local Standard of Rest velocity (4)
220- 274 A55 kpc Dist Kinematic distance (5)
276- 402 A127 km/s VHII Local Standard of Rest velocity of overlapped
HII region (6)
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Note (1): S for shell, C for composite, F for filled center (also known as
plerion), and "?" denotes uncertain ones.
Note (2): Those identified only by partial criteria are enclosed by
square brackets.
Note (3): Indicated by the spatial correlation coefficient, and those with
coefficients below 5sigma and less than 0.5 are enclosed by square
brackets. Values inside parentheses are the corresponding coefficients
of the previous value in the column.
Note (4): A "?" denotes possible ones.
Note (5): Estimated by a full distance probability density function, refer to
Reid+ 2016ApJ...823...77R 2016ApJ...823...77R and Reid+ 2019, J/ApJ/885/131
Values inside parentheses are the estimated probabilities of the
previous value in the column.
Note (6): VLSR of 12CO or 13CO is used, if they exist.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name SNR candidate name (GLLL.ll+B.bb)
14- 24 A11 --- OName Other name if any
27- 33 F7.3 deg GLON Galactic longitude
35- 40 F6.3 deg GLAT [-3.2/4] Galactic latitude
42- 44 I3 arcmin Size [7/667] Size of coverage area
46- 47 A2 --- Type Type of source (1)
49- 118 A70 km/s BL-VLSR Detected broad line Local Standard of Rest
velocity (2)
120- 210 A91 km/s SC-VLSR Spatially correlated molecular gas Local
Standard of Rest velocity (3)
212- 241 A30 km/s Vsys Systemic Local Standard of Rest velocity (4)
243- 297 A55 kpc Dist Kinematic distance (5)
299- 387 A89 km/s VHII Local Standard of Rest velocity of overlapped
HII region (6)
--------------------------------------------------------------------------------
Note (1): S for shell, C for composite, F for filled center (also known as
plerion), and "?" denotes uncertain ones.
Note (2): Those identified only by partial criteria are enclosed by
square brackets.
Note (3): Indicated by the spatial correlation coefficient, and those with
coefficients below 5sigma and less than 0.5 are enclosed by square
brackets. Values inside parentheses are the corresponding coefficients
of the previous value in the column.
Note (4): A "?" denotes possible ones.
Note (5): Estimated by a full distance probability density function, refer to
Reid+ 2016ApJ...823...77R 2016ApJ...823...77R and Reid+ 2019, J/ApJ/885/131
Values inside parentheses are the estimated probabilities of the
previous value in the column.
Note (6): VLSR of 12CO or 13CO is used, if they exist.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- SNR SNR name (GLLL.ll+B.bb)
13- 28 A16 --- OName Other name(s) if any
30- 81 A52 km/s OH-VLSR Local Standard of Rest velocity range
associated with OH 1720MHz maser (1)
83- 121 A39 km/s BL-VLSR Local Standard of Rest velocity associated
with broad CO line
123- 151 A29 km/s SC-VLSR Local Standard of Rest velocity of spatially
correlated CO emission (2)
153- 599 A447 km/s Other Local Standard of Rest velocity by other
evidence (3)
601- 700 A100 --- Ref Object reference code(s) (see refs.dat file)
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Note (1): And "D" for a detection of OH 1720MHz line.
Note (2): And "Y" for a detection of spatially correlated CO emission
without velocity information.
Note (3): "SC" represent spatial correlation.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source identifier
12 A1 --- u_Name [?] ?=PWN candidate
14- 57 A44 --- PSR Associated pulsar identifier
58 A1 --- u_PSR [?] ?=PSR candidate
60- 66 F7.3 deg GLON [18/195.2] Galactic longitude
68- 73 F6.3 deg GLAT [-5.8/5.1] Galactic latitude
75- 77 I3 arcmin Size [18/500] Size of coverage area
79-117 A39 km/s VLSR Local Standard of Rest velocity (2)
119-125 A7 --- Det Detection of broad line emission? (3)
127-132 A6 km/s Vsys Systemic Local Standard of Rest velocity (4)
134-144 A11 kpc Dist Kinematic distance (5)
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Note (2): Of spatially correlated molecular gas indicated by the spatial
correlation coefficient, and those with coefficients below 5sigma and
less than 0.5 are enclosed by square brackets. Values inside
parentheses are the corresponding coefficients of the previous value
in the column.
Note (3): Only those related to spatially correlated molecular gas, and those
identified only by partial criteria are enclosed by square brackets.
Note (4): Of candidate MC associated with PWN, and "?" denotes possible ones.
Note (5): Corresponding to Vsys, estimated by a full distance probability
density function, refer to Reid+ 2016ApJ...823...77R 2016ApJ...823...77R and
Reid+ 2019, J/ApJ/885/131, except for CTB 87 and Geminga. Values
inside parentheses are the estimated probabilities of the previous
value in the column.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Ref Reference code
5- 26 A22 --- Auth First author's name(s)
28- 46 A19 --- BibCode Bibcode of the reference
48- 100 A53 --- Comm Comment
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-Jan-2024